FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Aller, J
Swain, N
Baber, M
Tatar, G
Jacobson, N
Gannon, P
AF Aller, Josh
Swain, Nolan
Baber, Michael
Tatar, Greg
Jacobson, Nathan
Gannon, Paul
TI Influence of silicon on high-temperature (600 degrees C) chlorosilane
interactions with iron
SO SOLAR ENERGY MATERIALS AND SOLAR CELLS
LA English
DT Article
DE Iron; Chlorosilane; Silicon; Silicon tetrachloride; Iron silicide;
Corrosion
ID CHEMICAL-VAPOR-DEPOSITION; HYDROGEN-CHLORIDE; DIFFUSION COUPLES;
TETRACHLORIDE; SILICIDES; CORROSION; MIXTURES; TRICHLOROSILANE;
KINETICS; ALLOYS
AB High-temperature ( > 500 degrees C) chlorosilane gas streams are prevalent in the manufacture of polycrystalline silicon, the feedstock for silicon-based solar panels and electronics. This study investigated the influence of metallurgical grade silicon on the corrosion behavior of pure iron in these types of environments. The experiment included exposing pure iron samples at 600 degrees C to a silicon tetrachloride/hydrogen input gas mixture with and without embedding the samples in silicon. The samples in a packed bed of silicon had significantly higher mass gains compared to samples not in a packed bed. Comparison to diffusion studies suggest that the increase in mass gain of embedded samples is due to a higher silicon activity from the gas phase reaction with silicon. The experimental results were supported by chemical equilibrium calculationswhich showed that more active trichlorosilane and dichlorosilane species are formed from silicon tetrachloride in silicon packed bed conditions.
C1 [Aller, Josh; Baber, Michael] Montana State Univ, Mech & Ind Engn, Bozeman, MT 59717 USA.
[Swain, Nolan; Tatar, Greg; Gannon, Paul] Montana State Univ, Chem & Biol Engn, Bozeman, MT 59717 USA.
[Jacobson, Nathan] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Aller, J (reprint author), Montana State Univ, 306 Cobleigh Hall, Bozeman, MT 59717 USA.
EM Josh.aller@yahoo.com
FU Montana State University College of Engineering
FX We would like to acknowledge the Montana State University College of
Engineering for providing funding for this project. Additionally, we
would like to acknowledge Montana State University's Imaging and
Chemical Analysis Laboratory (ICAL) for their assistance with surface
analysis.
NR 30
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U1 7
U2 7
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0927-0248
EI 1879-3398
J9 SOL ENERG MAT SOL C
JI Sol. Energy Mater. Sol. Cells
PD FEB
PY 2017
VL 160
BP 410
EP 417
DI 10.1016/j.solmat.2016.11.002
PG 8
WC Energy & Fuels; Materials Science, Multidisciplinary; Physics, Applied
SC Energy & Fuels; Materials Science; Physics
GA EF1GG
UT WOS:000390072700050
ER
PT J
AU Carvalho, D
Rocha, A
Gomez-Gesteira, M
Santos, CS
AF Carvalho, D.
Rocha, A.
Gomez-Gesteira, M.
Santos, C. Silva
TI Potential impacts of climate change on European wind energy resource
under the CMIP5 future climate projections
SO RENEWABLE ENERGY
LA English
DT Article
DE Wind energy; Climate change; CMIP5; IPCC; Global models; Europe
ID MULTIMODEL ENSEMBLE; MODEL; NETHERLANDS; TRENDS
AB Climate change impact on future European large-scale wind energy resource under the latest IPCC CMIP5 future climate projections were analysed. After assessing the models that best reproduce contemporary near-surface wind speeds over Europe, their data was used to assess future changes in the wind energetic resource in Europe.
Using a multi-model ensemble composed by the models that showed the best ability to represent contemporary near-surface wind speeds over Europe, the future European large-scale wind energetic resource is projected to increase in Northern-Central Europe (Baltic Sea and surrounding areas), and decrease in the Mediterranean region, mainly by the end of the current century and under stronger radiative forcing scenarios. It is also projected an increase of the intra-annual variability in the Baltic Sea and surrounding areas and a decrease in Mediterranean areas, but no significant changes in the inter annual variability are expected over Europe.
Despite the large uncertainty associated to future climate projections, the findings of this work can serve as background for future downscaling of CMIP5 data to regional-local scales focused on climate change impacts on wind energy, and should be seen as a preliminary warning that a continuous increase of greenhouse gases emissions are expected to impact European wind energy production. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Carvalho, D.; Rocha, A.] Univ Aveiro, CESAM Dept Phys, Campus Univ Santiago, P-3810193 Aveiro, Portugal.
[Gomez-Gesteira, M.] Univ Vigo, Fac Ciencias, EPHYSLAB Environm Phys Lab, Orense 32004, Spain.
[Santos, C. Silva] Inst Super Engn Porto, Rua Dr Antonio Bernardino de Almeida 341, P-4200072 Oporto, Portugal.
[Carvalho, D.] NASA, Global Modeling & Assimilat Off GMAO, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Carvalho, D.] Univ Space Res Assoc USRA, Goddard Earth Sci Technol & Res GESTAR, Columbia, MD 21046 USA.
RP Carvalho, D (reprint author), Univ Aveiro, CESAM Dept Phys, Campus Univ Santiago, P-3810193 Aveiro, Portugal.; Carvalho, D (reprint author), NASA, Global Modeling & Assimilat Off GMAO, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Carvalho, D (reprint author), Univ Space Res Assoc USRA, Goddard Earth Sci Technol & Res GESTAR, Columbia, MD 21046 USA.
EM david.carvalho@ua.pt; alfredo.rocha@ua.pt; mggesteira@uvigo.es;
cmi@isep.ipp.pt
FU project CLICURB - Urban atmospheric quality, climate change and
resilience [EXCL/AAG-MAA/0383/2012]; FCT; Xunta de Galicia under the
project "Programa de Consolidacion e Estructuracion de Unidades de
Investigacion Competitivas (Grupos de Referencia Competitiva)"; European
Regional Development Fund (FEDER)
FX This work was supported by the project CLICURB - Urban atmospheric
quality, climate change and resilience (EXCL/AAG-MAA/0383/2012), funded
by FCT, and partially financed by Xunta de Galicia under the project
"Programa de Consolidacion e Estructuracion de Unidades de Investigacion
Competitivas (Grupos de Referencia Competitiva)", co-funded by the
European Regional Development Fund (FEDER). The authors would like to
express their gratitude to all the CMIP5 community and institutions
involved for providing the GCM data used in this work.
NR 38
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0960-1481
J9 RENEW ENERG
JI Renew. Energy
PD FEB
PY 2017
VL 101
BP 29
EP 40
DI 10.1016/j.renene.2016.08.036
PG 12
WC GREEN & SUSTAINABLE SCIENCE & TECHNOLOGY; Energy & Fuels
SC Science & Technology - Other Topics; Energy & Fuels
GA ED3VD
UT WOS:000388775700004
ER
PT J
AU Graydon, PJ
Holloway, CM
AF Graydon, Patrick J.
Holloway, C. Michael
TI An investigation of proposed techniques for quantifying confidence in
assurance arguments
SO SAFETY SCIENCE
LA English
DT Review
DE Safety case; Assurance argument; Confidence; Uncertainty
AB The use of safety cases in certification raises the question of assurance argument sufficiency and the issue of confidence (or uncertainty) in the argument's claims. Some researchers propose to model confidence quantitatively and to calculate confidence in argument conclusions. We know of little evidence to suggest that any proposed technique would deliver trustworthy results when implemented by system safety practitioners. Proponents do not usually assess the efficacy of their techniques through controlled experiment or historical study. Instead, they present an illustrative example where the calculation delivers a plausible result. In this paper, we review current proposals, claims made about them, and evidence advanced in favor of them. We then show that proposed techniques can deliver implausible results in some cases. We conclude that quantitative confidence techniques require further validation before they should be recommended as part of the basis for deciding whether an assurance argument justifies fielding a critical system.
C1 [Graydon, Patrick J.; Holloway, C. Michael] NASA, Langley Res Ctr, Mail Stop 130, Hampton, VA 23681 USA.
RP Graydon, PJ (reprint author), NASA, Langley Res Ctr, Mail Stop 130, Hampton, VA 23681 USA.
EM patrick.j.graydon@nasa.gov
FU National Aeronautics and Space Administration (NASA)
FX We thank Lian Duan, Janusz Gorski, and Sunil Nair for their assistance
in understanding and replicating their work. We thank John McDermid,
Andrew Rae, and the branch and directorate reviewers for their feedback
on this work. This work was funded by the National Aeronautics and Space
Administration (NASA).
NR 52
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U1 1
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0925-7535
EI 1879-1042
J9 SAFETY SCI
JI Saf. Sci.
PD FEB
PY 2017
VL 92
BP 53
EP 65
DI 10.1016/j.ssci.2016.09.014
PG 13
WC Engineering, Industrial; Operations Research & Management Science
SC Engineering; Operations Research & Management Science
GA EE0QT
UT WOS:000389284700007
ER
PT J
AU Desconnets, JC
Giuliani, G
Guigoz, Y
Lacroix, P
Mlisa, A
Noort, M
Ray, N
Searby, ND
AF Desconnets, Jean-Christophe
Giuliani, Gregory
Guigoz, Yaniss
Lacroix, Pierre
Mlisa, Andiswa
Noort, Mark
Ray, Nicolas
Searby, Nancy D.
TI GEOCAB Portal: A gateway for discovering and accessing capacity building
resources in Earth Observation
SO INTERNATIONAL JOURNAL OF APPLIED EARTH OBSERVATION AND GEOINFORMATION
LA English
DT Article
DE Capacity building; Earth observations; User needs; Discovery service;
Semantic search; Resource facility
ID INTEROPERABILITY; ARCHITECTURE; FRAMEWORK
AB The discovery of and access to capacity building resources are often essential to conduct environmental projects based on Earth Observation (EO) resources, whether they are Earth Observation products, methodological tools, techniques, organizations that impart training in these techniques or even projects that have shown practical achievements. Recognizing this opportunity and need, the European Commission through two FP7 projects jointly with the Group on Earth Observations (GEO) teamed up with the Committee on Earth observation Satellites (CEOS). The Global Earth Observation CApacity Building (GEOCAB) portal aims at compiling all current capacity building efforts on the use of EO data for societal benefits into an easily updateable and user-friendly portal. GEOCAB offers a faceted search to improve user discovery experience with a fully interactive world map with all inventoried projects and activities. This paper focuses on the conceptual framework used to implement the underlying platform. An ISO19115 metadata model associated with a terminological repository are the core elements that provide a semantic search application and an interoperable discovery service. The organization and the contribution of different user communities to ensure the management and the update of the content of GEOCAB are addressed. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Desconnets, Jean-Christophe] IRD, ESPACE, DEV, Montpellier, France.
[Noort, Mark] HCP Int, Wageningen, Netherlands.
[Searby, Nancy D.] NASA Headquarters, CEOS WGCapD Liaison GEOCAB, Div Earth Sci, 300 E St SW, Washington, DC 20546 USA.
[Mlisa, Andiswa] GEO Secretariat, Geneva, Switzerland.
[Giuliani, Gregory; Guigoz, Yaniss; Lacroix, Pierre; Ray, Nicolas] Univ Geneva, Inst Environm Sci, EnviroSPACE Lab, Bd Carl Vogt 66, CH-1211 Geneva, Switzerland.
[Giuliani, Gregory; Guigoz, Yaniss; Lacroix, Pierre; Ray, Nicolas] GRID Geneva, Bd Carl Vogt 66, CH-1211 Geneva, Switzerland.
RP Desconnets, JC (reprint author), IRD, ESPACE, DEV, Montpellier, France.
EM jean-christophe.Desconnets@ird.fr; amlisa@geosec.org;
m.noort@hcpinternational.com; nancy.d.searby@nasa.gov
FU European Commission FP7 Program [244172, 603500, 603534]
FX The authors would like to acknowledge the European Commission FP7
Program that funded GEONetCab (Grant agreement no 244172), EOPOWER
(Grant Agreement no 603500), and IASON (Grant Agreement no 603534)
projects.
NR 41
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U1 6
U2 6
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0303-2434
J9 INT J APPL EARTH OBS
JI Int. J. Appl. Earth Obs. Geoinf.
PD FEB
PY 2017
VL 54
BP 95
EP 104
DI 10.1016/j.jag.2016.09.010
PG 10
WC Remote Sensing
SC Remote Sensing
GA ED3VH
UT WOS:000388776100009
ER
PT J
AU Fujiwara, M
Wright, JS
Manney, GL
Gray, LJ
Anstey, J
Birner, T
Davis, S
Gerber, EP
Harvey, VL
Hegglin, MI
Homeyer, CR
Knox, JA
Kruger, K
Lambert, A
Long, CS
Martineau, P
Molod, A
Monge-Sanz, BM
Santee, ML
Tegtmeier, S
Chabrillat, S
Tan, DGH
Jackson, DR
Polavarapu, S
Compo, GP
Dragani, R
Ebisuzaki, W
Harada, Y
Kobayashi, C
McCarty, W
Onogi, K
Pawson, S
Simmons, A
Wargan, K
Whitaker, JS
Zou, CZ
AF Fujiwara, Masatomo
Wright, Jonathon S.
Manney, Gloria L.
Gray, Lesley J.
Anstey, James
Birner, Thomas
Davis, Sean
Gerber, Edwin P.
Harvey, V. Lynn
Hegglin, Michaela I.
Homeyer, Cameron R.
Knox, John A.
Kruger, Kirstin
Lambert, Alyn
Long, Craig S.
Martineau, Patrick
Molod, Andrea
Monge-Sanz, Beatriz M.
Santee, Michelle L.
Tegtmeier, Susann
Chabrillat, Simon
Tan, David G. H.
Jackson, David R.
Polavarapu, Saroja
Compo, Gilbert P.
Dragani, Rossana
Ebisuzaki, Wesley
Harada, Yayoi
Kobayashi, Chiaki
McCarty, Will
Onogi, Kazutoshi
Pawson, Steven
Simmons, Adrian
Wargan, Krzysztof
Whitaker, Jeffrey S.
Zou, Cheng-Zhi
TI Introduction to the SPARC Reanalysis Intercomparison Project (S-RIP) and
overview of the reanalysis systems
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID SEA-SURFACE TEMPERATURE; GENERAL-CIRCULATION MODELS; GRAVITY-WAVE DRAG;
VARIATIONAL DATA ASSIMILATION; ENSEMBLE KALMAN FILTER; LARGE-SCALE
MODELS; OZONE PHOTOCHEMISTRY PARAMETERIZATION; DIFFERENT VERTICAL
PARTITIONINGS; NUMERICAL WEATHER PREDICTION; TROPOPAUSE INVERSION LAYER
AB The climate research community uses atmospheric reanalysis data sets to understand a wide range of processes and variability in the atmosphere, yet different reanalyses may give very different results for the same diagnostics. The Stratosphere-troposphere Processes And their Role in Climate (SPARC) Reanalysis Intercomparison Project (S-RIP) is a coordinated activity to compare reanalysis data sets using a variety of key diagnostics. The objectives of this project are to identify differences among reanalyses and understand their underlying causes, to provide guidance on appropriate usage of various reanalysis products in scientific studies, particularly those of relevance to SPARC, and to contribute to future improvements in the reanalysis products by establishing collaborative links between reanalysis centres and data users. The project focuses predominantly on differences among reanalyses, although studies that include operational analyses and studies comparing reanalyses with observations are also included when appropriate. The emphasis is on diagnostics of the upper troposphere, stratosphere, and lower mesosphere. This paper summarizes the motivation and goals of the S-RIP activity and extensively reviews key technical aspects of the reanalysis data sets that are the focus of this activity. The special issue "The SPARC Reanalysis Intercomparison Project (S-RIP)" in this journal serves to collect research with relevance to the S-RIP in preparation for the publication of the planned two (interim and full) S-RIP reports.
C1 [Fujiwara, Masatomo] Hokkaido Univ, Fac Environm Earth Sci, Sapporo, Hokkaido 0600810, Japan.
[Wright, Jonathon S.] Tsinghua Univ, Ctr Earth Syst Sci, Beijing 100084, Peoples R China.
[Manney, Gloria L.] NorthWest Res Associates, Socorro, NM 87801 USA.
[Manney, Gloria L.] New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA.
[Gray, Lesley J.] Univ Oxford, Atmospher Ocean & Planetary Phys, Oxford OX1 3PU, England.
[Gray, Lesley J.] NERC, Natl Ctr Atmospher Sci, Leeds LS2 9JT, W Yorkshire, England.
[Anstey, James] Univ Victoria, Environm & Climate Change Canada, Canadian Ctr Climate Modelling & Anal, Victoria, BC V8W 2Y2, Canada.
[Birner, Thomas] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Davis, Sean] NOAA, Earth Syst Res Lab, Boulder, CO 80305 USA.
[Davis, Sean; Compo, Gilbert P.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Gerber, Edwin P.] NYU, Courant Inst Math Sci, 251 Mercer St, New York, NY 10012 USA.
[Harvey, V. Lynn] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80303 USA.
[Hegglin, Michaela I.] Univ Reading, Dept Meteorol, Reading RG6 6BB, Berks, England.
[Homeyer, Cameron R.] Univ Oklahoma, Sch Meteorol, Norman, OK 73072 USA.
[Knox, John A.] Univ Georgia, Dept Geog, Athens, GA 30602 USA.
[Kruger, Kirstin] Univ Oslo, Dept Geosci, N-0315 Oslo, Norway.
[Lambert, Alyn; Santee, Michelle L.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Long, Craig S.; Ebisuzaki, Wesley] NOAA, Climate Predict Ctr, Natl Ctr Environm Predict, College Pk, MD 20740 USA.
[Martineau, Patrick] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA.
[Molod, Andrea; McCarty, Will; Pawson, Steven; Wargan, Krzysztof] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610-1, Greenbelt, MD 20771 USA.
[Monge-Sanz, Beatriz M.; Tan, David G. H.; Dragani, Rossana; Simmons, Adrian] European Ctr Medium Range Weather Forecasts, Shinfield Pk, Reading RG2 9AX, Berks, England.
[Tegtmeier, Susann] GEOMAR Helmholtz Ctr Ocean Res Kiel, D-24105 Kiel, Germany.
[Chabrillat, Simon] Royal Belgian Inst Space Aeron BIRA IASB, B-1180 Brussels, Belgium.
[Jackson, David R.] Met Off, FitzRoy Rd, Exeter EX1 3PB, Devon, England.
[Polavarapu, Saroja] Environm & Climate Change Canada, Climate Res Div, Toronto, ON M3H 5T4, Canada.
[Compo, Gilbert P.; Whitaker, Jeffrey S.] NOAA, Div Phys Sci, Earth Syst Res Lab, Boulder, CO 80305 USA.
[Harada, Yayoi; Onogi, Kazutoshi] Japan Meteorol Agcy, Tokyo 1008122, Japan.
[Harada, Yayoi; Kobayashi, Chiaki] JMA, Meteorol Res Inst, Climate Res Dept, Tsukuba, Ibaraki 3050052, Japan.
[Wargan, Krzysztof] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Zou, Cheng-Zhi] NOAA, Ctr Satellite Applicat & Res, NESDIS, College Pk, MD 20740 USA.
RP Fujiwara, M (reprint author), Hokkaido Univ, Fac Environm Earth Sci, Sapporo, Hokkaido 0600810, Japan.; Wright, JS (reprint author), Tsinghua Univ, Ctr Earth Syst Sci, Beijing 100084, Peoples R China.
EM fuji@ees.hokudai.ac.jp; jswright@tsinghua.edu.cn
RI Homeyer, Cameron/D-5034-2013; Manager, CSD Publications/B-2789-2015;
Birner, Thomas/A-2108-2008
OI Homeyer, Cameron/0000-0002-4883-6670; Birner, Thomas/0000-0002-2966-3428
FU US Department of Energy, Office of Science Innovative and Novel
Computational Impact on Theory and Experiment (DOE INCITE) program;
Office of Biological and Environmental Research (BER); National Oceanic
and Atmospheric Administration Climate Program Office; Japanese Ministry
of Education, Culture, Sports, Science and Technology (MEXT) [26287117,
16K05548]; National Aeronautics and Space Administration; US NSF; NSF
CEDAR [1343056]; NASA LWS [NNX14AH54G]
FX We acknowledge the scientific guidance and sponsorship of the World
Climate Research Programme, coordinated in the framework of SPARC. We
are grateful to Ted Shepherd and Greg Bodeker (past SPARC co-chairs) for
strong encouragement and valuable advice during the proposal phase of
the project during 2011-2012 and Joan Alexander (serving SPARC co-chair
during 2013-2015) and Neil Harris (serving SPARC co-chair since 2014)
for continued support and encouragement. The Information Initiative
Center of Hokkaido University, Japan, has hosted the S-RIP web server
since 2014. We thank the reanalysis centres for providing their support
and data products. The British Atmospheric Data Centre (BADC) of the UK
Centre for Environmental Data Analysis (CEDA) has provided a virtual
machine for data processing and a group workspace for data storage. We
thank Yulia Zyulyaeva for contributions to the S-RIP as an original
member of the working group, as a chapter co-lead through October 2014,
and as the designer of the S-RIP logo. We thank Diane Pendlebury for
contributions to the S-RIP as a chapter co-lead through August 2015. We
thank Quentin Errera, the lead of the SPARC Data Assimilation working
group, for co-organizing the 2014, 2015, and 2016 S-RIP workshops.
Travel support for some participants of the 2013 planning meeting and
the 2014, 2015, and 2016 workshops was provided by SPARC. We thank Peter
Haynes, Gabriele Stiller, and William Lahoz for serving as the editors
for the special issue "The SPARC Reanalysis Intercomparison Project
(S-RIP)" in this journal. The materials contained in the tables and
figures for the technical aspects of the reanalysis data sets have been
compiled from a variety of sources, for which we acknowledge the
contributions of Santha Akella, Michael Bosilovich, Dick Dee, John
Derber, Ron Gelaro, Yu-Tai Hou, Robert Kistler, Daryl Kleist, Shinya
Kobayashi, Shrinivas Moorthi, Eric Nielsen, Paul Poli, Bill Putman,
Suranjana Saha, Jack Woollen, Fanglin Yang, and Valery Yudin. We thank
Kazuyuki Miyazaki and Karen Rosenlof for valuable comments and
suggestions on this paper. Support for the Twentieth Century Reanalysis
Project data set is provided by the US Department of Energy, Office of
Science Innovative and Novel Computational Impact on Theory and
Experiment (DOE INCITE) program and the Office of Biological and
Environmental Research (BER) and by the National Oceanic and Atmospheric
Administration Climate Program Office. Masatomo Fujiwara's contribution
was financially supported in part by the Japanese Ministry of Education,
Culture, Sports, Science and Technology (MEXT) through Grants-in-Aid for
Scientific Research (26287117 and 16K05548). Work at the Jet Propulsion
Laboratory, California Institute of Technology, was carried out under a
contract with the National Aeronautics and Space Administration. Edwin
P. Gerber acknowledges support from the US NSF. V. Lynn Harvey was
supported by NSF CEDAR grant 1343056 and NASA LWS grant NNX14AH54G.
NR 194
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PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PD JAN 31
PY 2017
VL 17
IS 2
BP 1417
EP 1452
DI 10.5194/acp-17-1417-2017
PG 36
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EL4SH
UT WOS:000394610700002
ER
PT J
AU Quintana, CM
Chen, Y
Sank, D
Petukhov, AG
White, TC
Kafri, D
Chiaro, B
Megrant, A
Barends, R
Campbell, B
Chen, Z
Dunsworth, A
Fowler, AG
Graff, R
Jeffrey, E
Kelly, J
Lucero, E
Mutus, JY
Neeley, M
Neill, C
O'Malley, PJJ
Roushan, P
Shabani, A
Smelyanskiy, VN
Vainsencher, A
Wenner, J
Neven, H
Martinis, JM
AF Quintana, C. M.
Chen, Yu
Sank, D.
Petukhov, A. G.
White, T. C.
Kafri, Dvir
Chiaro, B.
Megrant, A.
Barends, R.
Campbell, B.
Chen, Z.
Dunsworth, A.
Fowler, A. G.
Graff, R.
Jeffrey, E.
Kelly, J.
Lucero, E.
Mutus, J. Y.
Neeley, M.
Neill, C.
O'Malley, P. J. J.
Roushan, P.
Shabani, A.
Smelyanskiy, V. N.
Vainsencher, A.
Wenner, J.
Neven, H.
Martinis, John M.
TI Observation of Classical-Quantum Crossover of 1/f Flux Noise and Its
Paramagnetic Temperature Dependence
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID JOSEPHSON-JUNCTION; SUPERCONDUCTING QUBIT; DECOHERENCE; DISSIPATION;
CIRCUITS
AB By analyzing the dissipative dynamics of a tunable gap flux qubit, we extract both sides of its two-sided environmental flux noise spectral density over a range of frequencies around 2kBT/h approximate to 1 GHz, allowing for the observation of a classical-quantum crossover. Below the crossover point, the symmetric noise component follows a 1/f power law that matches the magnitude of the 1/f noise near 1 Hz. The antisymmetric component displays a 1/T dependence below 100 mK, providing dynamical evidence for a paramagnetic environment. Extrapolating the two-sided spectrum predicts the linewidth and reorganization energy of incoherent resonant tunneling between flux qubit wells.
C1 [Quintana, C. M.; Chiaro, B.; Campbell, B.; Chen, Z.; Dunsworth, A.; Neill, C.; O'Malley, P. J. J.; Wenner, J.; Martinis, John M.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Chen, Yu; Sank, D.; White, T. C.; Megrant, A.; Barends, R.; Fowler, A. G.; Graff, R.; Jeffrey, E.; Kelly, J.; Lucero, E.; Mutus, J. Y.; Neeley, M.; Roushan, P.; Vainsencher, A.; Martinis, John M.] Google Inc, Santa Barbara, CA 93117 USA.
[Petukhov, A. G.] NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kafri, Dvir; Shabani, A.; Smelyanskiy, V. N.; Neven, H.] Google Inc, Venice, CA 90291 USA.
RP Quintana, CM (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
FU National Science Foundation Graduate Research Fellowship [DGE-1144085];
Air Force Research Laboratory (AFRL) [F4HBKC4162G001]; NSF
FX We thank Sergio Boixo, Robert McDermott, Fedir Vasko, Mostafa Khezri,
Fei Yan, and Sebastian de Graaf for insightful discussions. This work
was supported by Google. C.Q. and Z. C. acknowledge support from the
National Science Foundation Graduate Research Fellowship under Grant No.
DGE-1144085. A. P. acknowledges support from the Air Force Research
Laboratory (AFRL) Information Directorate under Grant No.
F4HBKC4162G001. Devices were made at the UC Santa Barbara
Nanofabrication Facility, a part of the NSF-funded National
Nanotechnology Infrastructure Network.
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PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
EI 1079-7114
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD JAN 31
PY 2017
VL 118
IS 5
AR 057702
DI 10.1103/PhysRevLett.118.057702
PG 6
WC Physics, Multidisciplinary
SC Physics
GA EO0UQ
UT WOS:000396414200013
PM 28211704
ER
PT J
AU Kempes, CP
van Bodegom, PM
Wolpert, D
Libby, E
Amend, J
Hoehler, T
AF Kempes, Christopher P.
van Bodegom, Peter M.
Wolpert, David
Libby, Eric
Amend, Jan
Hoehler, Tori
TI Drivers of Bacterial Maintenance and Minimal Energy Requirements
SO FRONTIERS IN MICROBIOLOGY
LA English
DT Article
DE maintenance metabolism; basal power requirement; metabolic ecology
ID ESCHERICHIA-COLI; MESSENGER-RNAS; RIBOSOMAL-RNA; GROWTH; ENERGETICS;
BIOSPHERE; CELLS; SIZE; LIFE; FERMENTATION
AB Microbes maintain themselves through a variety of processes. Several of these processes can be reduced or shut down entirely when resource availability declines. In pure culture conditions with ample substrate supply, a relationship between the maximum growth rate and the energy invested in maintenance has been reported widely. However, at the other end of the resources spectrum, bacteria are so extremely limited by energy that no growth occurs and metabolism is constrained to the most essential functions only. These minimum energy requirements have been called the basal power requirement. While seemingly different from each other, both aspects are likely components of a continuum of regulated maintenance processes. Here, we analyze cross-species tradeoffs in cellular physiology over the range of bacterial size and energy expenditure and determine the contributions to maintenance metabolism at each point along the size-energy spectrum. Furthermore, by exploring the simplest bacteria within this framework which are most affected by maintenance constraints we uncover which processes become most limiting. For the smallest species, maintenance metabolism converges on total metabolism, where we predict that maintenance is dominated by the repair of proteins. For larger species the relative costs of protein repair decrease and maintenance metabolism is predicted to be dominated by the repair of RNA components. These results provide new insights into which processes are likely to be regulated in environments that are extremely limited by energy.
C1 [Kempes, Christopher P.; Wolpert, David; Libby, Eric] Santa Fe Inst, Santa Fe, NM 87501 USA.
[van Bodegom, Peter M.] Leiden Univ, Inst Environm Sci, Leiden, Netherlands.
[Amend, Jan] Univ Southern Calif, Dept Earth Sci, Los Angeles, CA USA.
[Amend, Jan] Univ Southern Calif, Dept Biol Sci, Los Angeles, CA 90089 USA.
[Hoehler, Tori] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Kempes, CP (reprint author), Santa Fe Inst, Santa Fe, NM 87501 USA.
EM ckempes@santafe.edu
FU Omidyar Fellowship at the Santa Fe Institute; Life Underground NASA
Astrobiology Institute [NNA13AA92A]; NASA Exobiology Program
[NNX16AJ59G]; Gordon and Betty Moore Foundation
FX CK acknowledges the support of the Omidyar Fellowship at the Santa Fe
Institute, the Life Underground NASA Astrobiology Institute
(NNA13AA92A), the NASA Exobiology Program (NNX16AJ59G), and the Gordon
and Betty Moore Foundation. EL thanks the Omidyar Fellowship at the
Santa Fe Institute for support.
NR 48
TC 0
Z9 0
U1 4
U2 4
PU FRONTIERS MEDIA SA
PI LAUSANNE
PA PO BOX 110, EPFL INNOVATION PARK, BUILDING I, LAUSANNE, 1015,
SWITZERLAND
SN 1664-302X
J9 FRONT MICROBIOL
JI Front. Microbiol.
PD JAN 31
PY 2017
VL 8
AR 31
DI 10.3389/fmicb.2017.00031
PG 10
WC Microbiology
SC Microbiology
GA EJ1IR
UT WOS:000392964300001
PM 28197128
ER
PT J
AU Kipp, MA
Stueken, EE
Bekker, A
Buick, R
AF Kipp, Michael A.
Stueken, Eva E.
Bekker, Andrey
Buick, Roger
TI Selenium isotopes record extensive marine suboxia during the Great
Oxidation Event
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE Paleoproterozoic; trace metals; oxygen; eukaryote evolution
ID MASS-DEPENDENT FRACTIONATION; ATMOSPHERIC OXYGEN; ARCHEAN ATMOSPHERE;
RICH SHALES; RISE; EVOLUTION; CARBON; CYCLE; EXCURSION; OCEAN
AB It has been proposed that an "oxygen overshoot" occurred during the early Paleoproterozoic Great Oxidation Event (GOE) in association with the extreme positive carbon isotopic excursion known as the Lomagundi Event. Moreover, it has also been suggested that environmental oxygen levels then crashed to very low levels during the subsequent extremely negative Shunga-Francevillian carbon isotopic anomaly. These redox fluctuations could have profoundly influenced the course of eukaryotic evolution, as eukaryotes have several metabolic processes that are obligately aerobic. Here we investigate the magnitude of these proposed oxygen perturbations using selenium (Se) geochemistry, which is sensitive to redox transitions across suboxic conditions. We find that delta Se-82/78 values in offshore shales show a positive excursion from 2.32 Ga until 2.1 Ga (mean + 1.03 +/- 0.67%). Selenium abundances and Se/TOC (total organic carbon) ratios similarly show a peak during this interval. Together these data suggest that during the GOE there was pervasive suboxia in near-shore environments, allowing nonquantitative Se reduction to drive the residual Se oxyanions isotopically heavy. This implies O-2 levels of >0.4 mu M in these settings. Unlike in the late Neoproterozoic and Phanerozoic, when negative delta Se-82/78 values are observed in offshore environments, only a single formation, evidently the shallowest, shows evidence of negative delta Se-82/78. This suggests that there was no upwelling of Se oxyanions from an oxic deep-ocean reservoir, which is consistent with previous estimates that the deep ocean remained anoxic throughout the GOE. The abrupt decline in delta Se-82/78 and Se/TOC values during the subsequent Shunga-Francevillian anomaly indicates a widespread decrease in surface oxygenation.
C1 [Kipp, Michael A.; Stueken, Eva E.; Buick, Roger] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA.
[Kipp, Michael A.; Stueken, Eva E.; Buick, Roger] Univ Washington, Astrobiol Program, Seattle, WA 98195 USA.
[Kipp, Michael A.; Stueken, Eva E.; Buick, Roger] NASA, Virtual Planetary Lab, Seattle, WA 98195 USA.
[Stueken, Eva E.; Bekker, Andrey] Univ Calif Riverside, Dept Earth Sci, Riverside, CA 92521 USA.
[Stueken, Eva E.] Univ St Andrews, Dept Earth & Environm Sci, St Andrews KY16 9AL, Fife, Scotland.
RP Kipp, MA (reprint author), Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA.; Kipp, MA (reprint author), Univ Washington, Astrobiol Program, Seattle, WA 98195 USA.; Kipp, MA (reprint author), NASA, Virtual Planetary Lab, Seattle, WA 98195 USA.
EM kipp@uw.edu
FU National Science Foundation (NSF) [EAR-0921580]; NSF Frontiers in Earth
System Dynamics Grant [1338810]; NASA [NNX16AI37G]; NSF [EAR-05-45484];
NASA Astrobiology Institute Award [NNA04CC09A]; Natural Sciences and
Engineering Research Council of Canada; NSF Graduate Research
Fellowship; NASA Postdoctoral Fellowship; NASA Astrobiology Institute
Virtual Planetary Laboratory [NNA13AA93A]
FX We thank Aivo Lepland, Chris Reinhard, PavelMedvedev, Luke Ootes, Frantz
Ossa-Ossa, New Millennium Iron, Cliffs Natural Resources, and the
Geological Survey of Botswana for access to samples critical to this
work. We thank the University of Washington Isotope Geochemistry Lab for
technical support. Funding for this work was provided by National
Science Foundation (NSF) Grant EAR-0921580, NSF Frontiers in Earth
System Dynamics Grant 1338810, and NASA Grant NNX16AI37G to R.B., as
well as NSF Grant EAR-05-45484, NASA Astrobiology Institute Award
NNA04CC09A, and an Natural Sciences and Engineering Research Council of
Canada Discovery and Accelerator Grant (to A.B.). M.A.K. acknowledges
support from an NSF Graduate Research Fellowship. E.E.S. is supported by
a NASA Postdoctoral Fellowship. Additional support was provided by the
NASA Astrobiology Institute Virtual Planetary Laboratory team Grant
NNA13AA93A.
NR 58
TC 0
Z9 0
U1 4
U2 4
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD JAN 31
PY 2017
VL 114
IS 5
BP 875
EP 880
DI 10.1073/pnas.1615867114
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EJ4OI
UT WOS:000393196300048
PM 28096405
ER
PT J
AU Garfinkel, CI
Aquila, V
Waugh, DW
Oman, LD
AF Garfinkel, Chaim I.
Aquila, Valentina
Waugh, Darryn W.
Oman, Luke D.
TI Time-varying changes in the simulated structure of the Brewer-Dobson
Circulation
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID CHEMISTRY-CLIMATE MODEL; STRATOSPHERIC AIR; TEMPERATURE TRENDS; MEAN
AGE; IN-SITU; TROPOSPHERE; VARIABILITY; UNCERTAINTIES; ACCELERATION;
EVOLUTION
AB A series of simulations using the NASA Goddard Earth Observing System Chemistry Climate Model are analyzed in order to assess changes in the Brewer-Dobson Circulation (BDC) over the past 55 years. When trends are computed over the past 55 years, the BDC accelerates throughout the stratosphere, consistent with previous modeling results. However, over the second half of the simulations (i.e., since the late 1980s), the model simulates structural changes in the BDC as the temporal evolution of the BDC varies between regions in the stratosphere. In the mid-stratosphere in the midlatitude Northern Hemisphere, the BDC does not accelerate in the ensemble mean of our simulations despite increases in greenhouse gas concentrations and warming sea surface temperatures, and it even decelerates in one ensemble member. This deceleration is reminiscent of changes inferred from satellite instruments and in situ measurements. In contrast, the BDC in the lower stratosphere continues to accelerate. The main forcing agents for the recent slowdown in the mid-stratosphere appear to be declining ozone-depleting substance (ODS) concentrations and the timing of volcanic eruptions. Changes in both mean age of air and the tropical upwelling of the residual circulation indicate a lack of recent acceleration. We therefore clarify that the statement that is often made that climate models simulate a decreasing age throughout the stratosphere only applies over long time periods and is not necessarily the case for the past 25 years, when most tracer measurements were taken.
C1 [Garfinkel, Chaim I.] Hebrew Univ Jerusalem, Fredy & Nadine Herrmann Inst Earth Sci, Jerusalem, Israel.
[Aquila, Valentina; Waugh, Darryn W.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[Aquila, Valentina] Goddard Earth Sci Technol & Res, Greenbelt, MD USA.
[Aquila, Valentina; Oman, Luke D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Garfinkel, CI (reprint author), Hebrew Univ Jerusalem, Fredy & Nadine Herrmann Inst Earth Sci, Jerusalem, Israel.
EM chaim.garfinkel@mail.huji.ac.il
FU Israel Science Foundation [1558/14]; European Research Council [677756];
US National Science Foundation; NASA MAP program
FX The work of Chaim I. Garfinkel was supported by the Israel Science
Foundation (grant number 1558/14) and by a European Research Council
starting grant under the European Union's Horizon 2020 research and
innovation program (grant agreement no. 677756). The work of Darryn W.
Waugh is supported, in part, by grants of the US National Science
Foundation to Johns Hopkins University. Valentina Aquila and Luke D.
Oman thank the NASA MAP program for their support. We also thank Eric
Ray for providing data from Figs. 7 and 8 of Ray et al. (2014) and for
help in interpreting balloon data and their uncertainties, and the four
anonymous reviewers for their constructive criticism. We also thanks
those involved in model development at GSFC-GMAO and Steven Pawson for
initially suggesting the suite of GEOSCCM simulations analyzed here.
High-performance computing resources were provided by the NASA Center
for Climate Simulation (NCCS). Correspondence and requests for data
should be addressed to Chaim I. Garfinkel (email:
chaim.garfinkel@mail.huji.ac.il).
NR 63
TC 0
Z9 0
U1 0
U2 0
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PD JAN 30
PY 2017
VL 17
IS 2
BP 1313
EP 1327
DI 10.5194/acp-17-1313-2017
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EL4QP
UT WOS:000394606200001
ER
PT J
AU Bhatt, R
Doelling, DR
Angal, A
Xiong, XX
Scarino, B
Gopalan, A
Haney, C
Wu, AS
AF Bhatt, Rajendra
Doelling, David R.
Angal, Amit
Xiong, Xiaoxiong
Scarino, Benjamin
Gopalan, Arun
Haney, Conor
Wu, Aisheng
TI Characterizing response versus scan-angle for MODIS reflective solar
bands using deep convective clouds
SO JOURNAL OF APPLIED REMOTE SENSING
LA English
DT Article
DE moderate resolution imaging spectroradiometer; reflective solar bands;
response versus scan-angle; scan mirror; Aqua
ID PART I; CALIBRATION; AVHRR; STABILITY; CHANNELS; DESERT; RECORD
AB MODIS consists of a cross-track, two-sided scan mirror, whose reflectance is not uniform but is a function of angle of incidence (AOI). This feature, known as response versus scan-angle (RVS), was characterized for all reflective solar bands of both MODIS instruments prior to launch. The RVS characteristic has changed on orbit, which must be tracked precisely over time to ensure the quality of MODIS products. The MODIS characterization support team utilizes the onboard calibrators and the earth view responses from multiple pseudoinvariant desert sites to track the RVS changes at different AOIs. The drawback of using deserts is the assumption that these sites are radiometrically stable during the monitoring period. In addition, the 16-day orbit repeat cycle of MODIS allows for only a limited set of AOIs over a given desert. We propose a novel and robust approach of characterizing the MODIS RVS using tropical deep convective clouds (DCC). The method tracks the monthly DCC response at specified sets of AOIs to compute the temporal RVS changes. Initial results have shown that the Aqua-MODIS collection 6 band 1 level 1B radiances show considerable residual RVS dependencies, with long-term drifts up to 2.3% at certain AOIs. (C) 2017 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Bhatt, Rajendra; Scarino, Benjamin; Gopalan, Arun; Haney, Conor] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
[Doelling, David R.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Angal, Amit; Wu, Aisheng] Sci Syst & Applicat Inc, Lanham, MD USA.
[Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Bhatt, R (reprint author), Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
EM rajendra.bhatt@nasa.gov
FU National Aeronautics and Space Administration Earth Science Enterprise
Office through the CERES Project
FX This work was supported by the National Aeronautics and Space
Administration Earth Science Enterprise Office through the CERES
Project. The MODIS data were obtained from the NASA Langley Atmospheric
Science Data Center Distributed Active Archive Center (ASDC DAAC).
NR 26
TC 0
Z9 0
U1 0
U2 0
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 1931-3195
J9 J APPL REMOTE SENS
JI J. Appl. Remote Sens.
PD JAN 28
PY 2017
VL 11
AR 016014
DI 10.1117/1.JRS.11.016014
PG 14
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA EP8SZ
UT WOS:000397646400001
ER
PT J
AU Dai, L
Wang, C
Zhang, YC
Lavraud, B
Burch, J
Pollock, C
Torbert, RB
AF Dai, Lei
Wang, Chi
Zhang, Yongcun
Lavraud, Benoit
Burch, James
Pollock, Craig
Torbert, Roy B.
TI Kinetic Alfven wave explanation of the Hall fields in magnetic
reconnection
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE kinetic Alfven wave; Hall fields; magnetic reconnection; Hall current
ID MAGNETOSPHERIC MULTISCALE; ELECTRIC-FIELD; SMALL-SCALE; X-LINE; PLASMA;
MAGNETOPAUSE; MODEL; MAGNETOTAIL; TRANSPORT; REGION
AB Magnetic reconnection is initiated in a small diffusion region but can drive global-scale dynamics in Earth's magnetosphere, solar flares, and astrophysical systems. Understanding the processes at work in the diffusion region remains a main challenge in space plasma physics. Recent in situ observations from Magnetospheric Multiscale and Time History of Events and Macroscale Interactions during Substorms reveal that the electric field normal to the reconnection current layer, often called the Hall electric field (E-n), is mainly balanced by the ion pressure gradient. Here we present theoretical explanations indicating that this observation fact is a manifestation of kinetic Alfven waves (KAWs) physics. The ion pressure gradient represents the finite gyroradius effect of KAW, leading to ion intrusion across the magnetic field lines. Electrons stream along the magnetic field lines to track ions, resulting in field-aligned currents and the associated pattern of the out-of-plane Hall magnetic field (B-m). The ratio E-n/B-m is on the order of the Alfven speed, as predicted by the KAW theory. The KAW physics further provides new perspectives on how ion intrusion may trigger electric fields suitable for reconnection to occur.
C1 [Dai, Lei; Wang, Chi; Zhang, Yongcun] Chinese Acad Sci, Natl Space Sci Ctr, State Key Lab Space Weather, Beijing, Peoples R China.
[Lavraud, Benoit] Univ Toulouse, Inst Rech Astrophys & Planetol, Toulouse, France.
[Burch, James] Southwest Res Inst, San Antonio, TX USA.
[Pollock, Craig] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Torbert, Roy B.] Univ New Hampshire, Durham, NH 03824 USA.
RP Dai, L (reprint author), Chinese Acad Sci, Natl Space Sci Ctr, State Key Lab Space Weather, Beijing, Peoples R China.
EM ldai@spaceweather.ac.cn
OI Zhang, Yongcun/0000-0001-5721-8164
FU NNSFC [41574161, 41231067]; Specialized Research Fund for State Key
Laboratories of China
FX This work was supported by NNSFC grants 41574161 and 41231067 and in
part by the Specialized Research Fund for State Key Laboratories of
China.
NR 46
TC 0
Z9 0
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN 28
PY 2017
VL 44
IS 2
BP 634
EP 640
DI 10.1002/2016GL071044
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA EM9SY
UT WOS:000395652600004
ER
PT J
AU Khazanov, GV
Sibeck, DG
Zesta, E
AF Khazanov, G. V.
Sibeck, D. G.
Zesta, E.
TI Is diffuse aurora driven from above or below?
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE diffuse aurora; magnetosphere-ionosphere coupling; electron
precipitation
ID ELECTRON-TRANSPORT; MAGNETOSPHERE; PRECIPITATION; WAVES; PLASMASPHERE;
ATMOSPHERE; EMISSIONS; REGIONS; MODEL
AB In the diffuse aurora, magnetospheric electrons, initially precipitated from the inner plasma sheet via wave-particle interaction processes, degrade in the atmosphere toward lower energies, and produce secondary electrons via impact ionization of the neutral atmosphere. These initially precipitating electrons of magnetospheric origin can also be additionally reflected back into the magnetosphere, leading to a series of multiple reflections by the two magnetically conjugate atmospheres that can greatly impact the initially precipitating flux at the upper ionospheric boundary (700-800km). The resultant population of secondary and primary electrons cascades toward lower energies and escape back to the magnetosphere. Escaping upward electrons traveling from the ionosphere can be trapped in the magnetosphere, as they travel inside the loss cone, via Coulomb collisions with the cold plasma, or by interactions with various plasma waves. Even though this scenario is intuitively transparent, this magnetosphere-ionosphere coupling element is not considered in any of the existing diffuse aurora research. Nevertheless, as we demonstrate in this letter, this process has the potential to dramatically affect the formation of electron precipitated fluxes in the regions of diffuse auroras.
C1 [Khazanov, G. V.; Sibeck, D. G.; Zesta, E.] NASA, GSFC, Greenbelt, MD 20771 USA.
RP Khazanov, GV (reprint author), NASA, GSFC, Greenbelt, MD 20771 USA.
EM george.v.khazanov@nasa.gov
FU NASA [NNH13ZDA001N-HSR]
FX Funding support for this study was provided by NASA Van Allen Probes
Project, and the NASA LWS Program and NASA grant NNH13ZDA001N-HSR. The
data for this paper are available from George V. Khazanov at
george.v.khazanov@nasa.gov.
NR 32
TC 0
Z9 0
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN 28
PY 2017
VL 44
IS 2
BP 641
EP 647
DI 10.1002/2016GL072063
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA EM9SY
UT WOS:000395652600005
ER
PT J
AU Wordsworth, R
Kalugina, Y
Lokshtanov, S
Vigasin, A
Ehlmann, B
Head, J
Sanders, C
Wang, H
AF Wordsworth, R.
Kalugina, Y.
Lokshtanov, S.
Vigasin, A.
Ehlmann, B.
Head, J.
Sanders, C.
Wang, H.
TI Transient reducing greenhouse warming on early Mars
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Mars; valley networks; astrobiology; methane; hydrogen; paleoclimate
ID COLLISION-INDUCED ABSORPTION; EARTHS EARLY ATMOSPHERE; TITANS
ATMOSPHERE; MARTIAN CLIMATE; GALE CRATER; METHANE; CO2; WATER;
PLANETARY; CARBON
AB The evidence for abundant liquid water on early Mars despite the faint young Sun is a long-standing problem in planetary research. Here we present new ab initio spectroscopic and line-by-line climate calculations of the warming potential of reduced atmospheres on early Mars. We show that the strength of both CO2-H-2 and CO2-CH4 collision-induced absorption (CIA) has previously been significantly underestimated. Contrary to previous expectations, methane could have acted as a powerful greenhouse gas on early Mars due to CO2-CH4 CIA in the critical 250-500cm(-1) spectral window region. In atmospheres of 0.5bar CO2 or more, percent levels of H-2 or CH4 raise annual mean surface temperatures by tens of degrees, with temperatures reaching 273K for pressures of 1.25-2bars and 2-10% of H-2 and CH4. Methane and hydrogen produced following aqueous alteration of Mars' crust could have combined with volcanically outgassed CO2 to form transient atmospheres of this composition 4.5-3.5Ga. Our results also suggest that inhabited exoplanets could retain surface liquid water at significant distances from their host stars.
C1 [Wordsworth, R.; Wang, H.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Wordsworth, R.; Sanders, C.] Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA.
[Kalugina, Y.] Tomsk State Univ, Dept Opt & Spect, Tomsk 634050, Russia.
[Lokshtanov, S.] Lomonosov Moscow State Univ, Dept Chem, Moscow, Russia.
[Lokshtanov, S.; Vigasin, A.] Russian Acad Sci, Obukhov Inst Atmospher Phys, Moscow, Russia.
[Ehlmann, B.; Sanders, C.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Ehlmann, B.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Head, J.] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA.
RP Wordsworth, R (reprint author), Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.; Wordsworth, R (reprint author), Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA.
EM rwordsworth@seas.harvard.edu
OI Ehlmann, Bethany/0000-0002-2745-3240
FU Kavli Foundation; RFBR [15-03-03302, 15-05-00736]; Russian Academy of
Sciences [9]
FX R.W. acknowledges financial support from the Kavli Foundation and
discussions with T. Robinson and F. Ding on line-by-line radiative
calculations and K. Zahnle on atmospheric chemistry. S.L., Y.K., and
A.V. gratefully acknowledge partial support of this work from RFBR
grants 15-03-03302 and 15-05-00736 and the Russian Academy of Sciences
Program 9. B.L.E. thanks B. Sherwood-Lollar and G. Etiope for discussion
of H2/CH4 observed in terrestrial serpentinizing
systems. The ab initio calculations were performed using the HPC
resources of the FAS Research Computing Cluster (Harvard University) and
the "Lomonosov" (Moscow State University) supercomputer. The CIA data
produced from our spectroscopic calculations and the line-by-line and
temperature data produced from our climate model are available from the
lead author on request (rwordsworth@seas.harvard.edu).
NR 61
TC 0
Z9 0
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN 28
PY 2017
VL 44
IS 2
BP 665
EP 671
DI 10.1002/2016GL071766
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA EM9SY
UT WOS:000395652600008
ER
PT J
AU Poh, G
Slavin, JA
Jia, XZ
Raines, JM
Imber, SM
Sun, WJ
Gershman, DJ
DiBraccio, GA
Genestreti, KJ
Smith, AW
AF Poh, Gangkai
Slavin, James A.
Jia, Xianzhe
Raines, Jim M.
Imber, Suzanne M.
Sun, Wei-Jie
Gershman, Daniel J.
DiBraccio, Gina A.
Genestreti, Kevin J.
Smith, Andy W.
TI Mercury's cross-tail current sheet: Structure, X-line location and
stress balance
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Mercury; cross-tail current sheet; stress balance; Near-Mercury Neutral
Line; magnetotail structure
ID LARGE-SCALE STRUCTURE; MESSENGER OBSERVATIONS; MAGNETIC-FIELD; PLASMA
SHEET; MAGNETOTAIL; RECONNECTION; MAGNETOPAUSE; MAGNETOSPHERE;
INSTRUMENT; DYNAMICS
AB The structure, X-line location, and magnetohydrodynamic (MHD) stress balance of Mercury's magnetotail were examined between -2.68mm). The period of subsidence is delayed by 1-2months over areas where smaller seasonal movements are observed, suggesting an unsaturated soil where water occurs in the deeper part of the active layer.
C1 [Daout, Simon; Doin, Marie-Pierre; Socquet, Anne; Lasserre, Cecile] Univ Grenoble Alpes, CNRS, ISTerre, Grenoble, France.
[Peltzer, Gilles] Univ Calif Los Angeles, Dept Earth Sci, Los Angeles, CA USA.
[Peltzer, Gilles] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Daout, S (reprint author), Univ Grenoble Alpes, CNRS, ISTerre, Grenoble, France.
EM simon.daout@univ-grenoble-alpes.fr
RI Lasserre, Cecile/D-7073-2017;
OI Lasserre, Cecile/0000-0002-0582-0775; Socquet, Anne/0000-0002-9208-7136
FU European Space Agency (ESA) [10686]; CNES TOSCA; CNRS Mastodons; Young
Scientist Dragon 3; French Appel a project Grenoble Innovation Recherche
(AGIR) fellowship
FX The SAR data set was provided by the European Space Agency (ESA) in the
framework of the Dragon 3 program (project ID 10686). The NSBAS
development and computing facilities were funded through the CNES TOSCA
program (SAR-ready and TeraSAR projects) and the CNRS Mastodons. S.
Daout's work is supported through the Young Scientist Dragon 3 and the
French Appel a project Grenoble Innovation Recherche (AGIR) fellowship.
We are grateful to Matthieu Volat for his contribution to the
development and the optimization of the NSBAS processing chain. We thank
Gerhard Krinner and Peter van der Beek for simulating discussions about
permafrost deformation mechanisms. The paper benefited from the detailed
reviews and constructive suggestions of two anonymous reviewers.
NR 46
TC 0
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U1 4
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN 28
PY 2017
VL 44
IS 2
BP 901
EP 909
DI 10.1002/2016GL070781
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA EM9SY
UT WOS:000395652600036
ER
PT J
AU Volkov, DL
Lee, SK
Landerer, FW
Lumpkin, R
AF Volkov, Denis L.
Lee, Sang-Ki
Landerer, Felix W.
Lumpkin, Rick
TI Decade-long deep-ocean warming detected in the subtropical South Pacific
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE ocean warming; sea level; South Pacific; heat content; subtropical
convergence; ENSO
ID SEA-LEVEL RISE; EARTHS ENERGY IMBALANCE; HEAT-CONTENT; SATELLITE
ALTIMETRY; GLOBAL HEAT; GRACE; REANALYSIS; GRAVITY; SURFACE; VARIABILITY
AB The persistent energy imbalance at the top of the atmosphere, inferred from satellite measurements, indicates that the Earth's climate system continues to accumulate excess heat. As only sparse and irregular measurements of ocean heat below 2000m depth exist, one of the most challenging questions in global climate change studies is whether the excess heat has already penetrated into the deep ocean. Here we perform a comprehensive analysis of satellite and in situ measurements to report that a significant deep-ocean warming occurred in the subtropical South Pacific Ocean over the past decade (2005-2014). The local accumulation of heat accounted for up to a quarter of the global ocean heat increase, with directly and indirectly inferred deep ocean (below 2000m) contribution of 2.41.4 and 6.1-10.14.4%, respectively. We further demonstrate that this heat accumulation is consistent with a decade-long intensification of the subtropical convergence, possibly linked to the persistent La Nina-like state.
C1 [Volkov, Denis L.] Univ Miami, Cooperat Inst Marine & Atmospher Studies, Miami, FL 33136 USA.
[Volkov, Denis L.; Lee, Sang-Ki; Lumpkin, Rick] NOAA, Atlantic Oceanog & Meteorol Lab, Miami, FL 33149 USA.
[Landerer, Felix W.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Volkov, DL (reprint author), Univ Miami, Cooperat Inst Marine & Atmospher Studies, Miami, FL 33136 USA.; Volkov, DL (reprint author), NOAA, Atlantic Oceanog & Meteorol Lab, Miami, FL 33149 USA.
EM denis.volkov@noaa.gov
OI Lee, Sang-Ki/0000-0002-4047-3545
FU NASA Ocean Surface Topography Science Team program; NOAA-AOML; NASA
FX This research was supported by the NASA Ocean Surface Topography Science
Team program and by the base funds of NOAA-AOML. The work of F.W.
Landerer was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with NASA. The authors thank
two anonymous reviewers and Don Chambers for their constructive comments
and helpful suggestions. All data for this paper are publicly available,
properly cited, and referred to in the reference list.
NR 46
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN 28
PY 2017
VL 44
IS 2
BP 927
EP 936
DI 10.1002/2016GL071661
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA EM9SY
UT WOS:000395652600039
ER
PT J
AU Orbe, C
Waugh, DW
Yang, H
Lamarque, JF
Tilmes, S
Kinnison, DE
AF Orbe, Clara
Waugh, Darryn W.
Yang, Huang
Lamarque, Jean-Francois
Tilmes, Simone
Kinnison, Douglas E.
TI Tropospheric transport differences between models using the same
large-scale meteorological fields
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE large-scale tropospheric transport; idealized tracers; specified
meteorology simulations
ID GENERAL-CIRCULATION MODEL; CHEMISTRY-CLIMATE MODEL; AIR-MASS ORIGIN;
CUMULUS CONVECTION; MOIST CONVECTION; PARAMETERIZATION; SIMULATIONS;
STRATOSPHERE; VARIABILITY; EMISSIONS
AB The transport of chemicals is a major uncertainty in the modeling of tropospheric composition. A common approach is to transport gases using the winds from meteorological analyses, either using them directly in a chemical transport model or by constraining the flow in a general circulation model. Here we compare the transport of idealized tracers in several different models that use the same meteorological fields taken from Modern-Era Retrospective analysis for Research and Applications (MERRA). We show that, even though the models use the same meteorological fields, there are substantial differences in their global-scale tropospheric transport related to large differences in parameterized convection between the simulations. Furthermore, we find that the transport differences between simulations constrained with the same-large scale flow are larger than differences between free-running simulations, which have differing large-scale flow but much more similar convective mass fluxes. Our results indicate that more attention needs to be paid to convective parameterizations in order to understand large-scale tropospheric transport in models, particularly in simulations constrained with analyzed winds.
C1 [Orbe, Clara] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Orbe, Clara; Waugh, Darryn W.; Yang, Huang] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[Lamarque, Jean-Francois; Tilmes, Simone; Kinnison, Douglas E.] Natl Ctr Atmospher Res, Atmospher Chem Observat & Modeling Lab, POB 3000, Boulder, CO 80307 USA.
RP Orbe, C (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.; Orbe, C (reprint author), Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
EM clara.orbe@nasa.gov
OI Kinnison, Douglas/0000-0002-3418-0834
FU NASA's Advanced Supercomputing (NAS) Division; NASA Center for Climate
Simulation (NCCS); NSF [AGS-1403676]; NASA [NNX14AP58G]; U.S. National
Science Foundation; National Science Foundation (NSF); Office of Science
of the U.S. Department of Energy; NSF
FX The authors thanks useful discussions with Andrea Molod and the
high-performance computing resources provided by NASA's Advanced
Supercomputing (NAS) Division and the NASA Center for Climate Simulation
(NCCS). D.W. acknowledges support from NSF grant AGS-1403676 and NASA
grant NNX14AP58G. The National Center for Atmospheric Research (NCAR) is
sponsored by the U.S. National Science Foundation. WACCM is a component
of the Community Earth System Model (CESM), which is supported by the
National Science Foundation (NSF) and the Office of Science of the U.S.
Department of Energy. Computing resources were provided by NCAR's
Climate Simulation Laboratory, sponsored by NSF and other agencies. This
research was enabled by the computational and storage resources of
NCAROs Computational and Information Systems Laboratory (CISL). All data
and model output used in this study are available by contacting the
corresponding author (clara.orbe@nasa.gov/).
NR 39
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U1 1
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN 28
PY 2017
VL 44
IS 2
BP 1068
EP 1078
DI 10.1002/2016GL071339
PG 11
WC Geosciences, Multidisciplinary
SC Geology
GA EM9SY
UT WOS:000395652600055
ER
PT J
AU Schwarz, JP
Weinzierl, B
Samset, BH
Dollner, M
Heimerl, K
Markovic, MZ
Perring, AE
Ziemba, L
AF Schwarz, Joshua P.
Weinzierl, Bernadett
Samset, Bjorn H.
Dollner, Maximilian
Heimerl, Katharina
Markovic, Milos Z.
Perring, Anne E.
Ziemba, Luke
TI Aircraft measurements of black carbon vertical profiles show upper
tropospheric variability and stability
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE black carbon; AeroCom; SP2; aerosol; global models; measurements
ID LIGHT-ABSORPTION; MIXING STATE; AEROSOL; EMISSIONS; MODEL;
RECOMMENDATIONS; EUROPE; AREA
AB We present new data sets of black carbon (BC) aerosol mass mixing ratio (MMR) obtained from aircraft missions over North America, Europe, the Arctic, and the outflow region of Saharan Africa before and after trans-Atlantic transport. The data, collected from 2011 to 2013 with single-particle soot photometers, provide new insight into the variability and distribution of BC over global scales and refine understanding of AeroCom global model ensemble performance. The results indicate extensive global-scale longitudinal mixing of BC above altitude pressures as low as 400hPa. They also constrain the absolute and temporal variability of upper tropospheric BC MMR and point to opportunities for new tests of global aerosol models in the upper troposphere. A comparison to the AeroCom Phase II results generally reinforces previous estimates of the ensemble performance, except that it also strengthens confidence that the ensemble actually is biased high in the Arctic in all seasons.
C1 [Schwarz, Joshua P.; Perring, Anne E.] NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO 80305 USA.
[Weinzierl, Bernadett; Dollner, Maximilian; Heimerl, Katharina] Deutsch Zentrum Luft & Raumfahrt, Oberpfaffenhofen, Germany.
[Weinzierl, Bernadett; Dollner, Maximilian; Heimerl, Katharina] Ludwig Maximilians Univ Munchen, Fac Phys, Inst Meteorol, Munich, Germany.
[Weinzierl, Bernadett; Dollner, Maximilian] Univ Vienna, Aerosol Phys & Environm Phys, Vienna, Austria.
[Samset, Bjorn H.] Ctr Int Climate & Environm Res Oslo, Oslo, Norway.
[Markovic, Milos Z.] Piccaro Inc, Santa Clara, CA USA.
[Perring, Anne E.] Cooperat Inst Res Environm Sci, Boulder, CO USA.
[Ziemba, Luke] NASA, Goddard Flight Ctr, Greenbelt, MD USA.
RP Schwarz, JP (reprint author), NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO 80305 USA.
EM joshua.p.schwarz@noaa.gov
RI Perring, Anne/G-4597-2013; Manager, CSD Publications/B-2789-2015
OI Perring, Anne/0000-0003-2231-7503;
FU NOAA Atmospheric Composition and Climate Program; NASA Radiation
Sciences Program; NASA Upper Atmosphere Research Program; Helmholtz
Association [VH-NG-606]; DLR project CATS; DLR project VolcATS; European
Union project ACCESS [265863]; Center for Advanced Studies at LMU; LMU
Munich's Institutional Strategy LMUexcellent; European Research Council
under the European Community/ERC [640458A-LIFE]; Research Council of
Norway [AEROCOM-P3]; AC/BC [240372]; NetBC [244141]
FX The NOAA SP2 data were obtained and analyzed with the support of the
NOAA Atmospheric Composition and Climate Program, the NASA Radiation
Sciences Program, and the NASA Upper Atmosphere Research Program. The
DLR SP2 data were obtained and analyzed with the support of the
Helmholtz Association under grant VH-NG-606
(Helmholtz-Hochschul-Nachwuchsforschergruppe AerCARE), the DLR projects
CATS and VolcATS, and the European Union project ACCESS under grant
agreement 265863. Additional analysis was supported in part by the
Center for Advanced Studies at LMU, LMU Munich's Institutional Strategy
LMUexcellent within the framework of the German Excellence Initiative,
and by the European Research Council under the European Community's
Horizon 2020 research and innovation framework program/ERC grant
agreement 640458A-LIFE. Data are available at
http://wwwair.larc.nasa.gov/missions/seac4rs/index.html for the SEAC4RS
mission, http://www-air.larc.nasa.gov/cgi-bin/ArcView/dc3 for the DC3
mission (both DLR Falcon and NASA DC8 data), and by request to the DLR
for the CONCERT, ACCESS, and SALTRACE missions; the PI for the Falcon BC
data can be reached at Bernadett.Weinzierl@univie.ac.at. AeroCom model
data are freely available upon application, see aerocom. met. no for
details. We thank the modeling groups for use of their results. B.H.S.
acknowledges funding by the Research Council of Norway through the
grants AEROCOM-P3, AC/BC (240372), and NetBC (244141).
NR 27
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U1 2
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN 28
PY 2017
VL 44
IS 2
BP 1132
EP 1140
DI 10.1002/2016GL071241
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA EM9SY
UT WOS:000395652600062
ER
PT J
AU de Wit, RJ
Janches, D
Fritts, DC
Stockwell, RG
Coy, L
AF de Wit, R. J.
Janches, D.
Fritts, D. C.
Stockwell, R. G.
Coy, L.
TI Unexpected climatological behavior of MLT gravity wave momentum flux in
the lee of the Southern Andes hot spot
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE middle atmosphere dynamics; gravity waves
ID GENERAL-CIRCULATION MODEL; METEOR RADAR MEASUREMENTS; LOWER
STRATOSPHERE; SUMMER MESOPAUSE; AUCKLAND ISLANDS; MOUNTAIN WAVES; POKER
FLAT; MESOSPHERE; ATMOSPHERE; TURBULENCE
AB The Southern Argentina Agile MEteor Radar (SAAMER), located at Tierra del Fuego (53.7 degrees S, 67.7 degrees W), has been providing near-continuous high-resolution measurements of winds and high-frequency gravity wave (GW) momentum fluxes of the mesopause region since May 2008. As SAAMER is located in the lee of the largest seasonal GW hot spot on Earth, this is a key location to study GWs and their interaction with large-scale motions. GW momentum flux climatologies are shown for the first time for this location and discussed in light of these unique dynamics. Particularly, the large eastward GW momentum fluxes during local winter are surprising, as these observations cannot be explained by the direct upward propagation of expected large-amplitude mountain waves (MWs) through the eastward stratospheric jet. Instead, these results are interpreted as secondary GWs propagating away from stratospheric sources over the Andes accompanying MW breaking over the Southern Andes.
C1 [de Wit, R. J.; Janches, D.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA.
[de Wit, R. J.] Zentralanstalt Meteorol & Geodynam ZAMG, Vienna, Austria.
[Fritts, D. C.; Stockwell, R. G.] GATS Inc, Boulder, CO USA.
[Coy, L.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD USA.
RP de Wit, RJ (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA.; de Wit, RJ (reprint author), Zentralanstalt Meteorol & Geodynam ZAMG, Vienna, Austria.
EM rosmarie.dewit@zamg.ac.at
RI Janches, Diego/D-4674-2012
OI Janches, Diego/0000-0001-8615-5166
FU NSF [AGS-1112830]; NASA Postdoctoral Program
FX We wish to thank the Estacion Astronomica Rio Grande (EARG) personnel
for their invaluable help with the operation of SAAMER. Useful
discussions with Benedikt Ehard, Andreas Dornbrack, and Corwin Wright
are gratefully acknowledged. SAAMER is supported by NSF under grant
AGS-1112830. This work was supported by RJW's appointment to the NASA
Postdoctoral Program, administered by the Universities Space Research
Association through a contract with NASA. MERRA-2 results are freely
available from , meteor radar data are available from the authors upon
request.
NR 61
TC 0
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U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN 28
PY 2017
VL 44
IS 2
BP 1182
EP 1191
DI 10.1002/2016GL072311
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA EM9SY
UT WOS:000395652600068
ER
PT J
AU Vasilkov, A
Qin, WH
Krotkov, N
Lamsal, L
Spurr, R
Haffner, D
Joiner, J
Yang, ES
Marchenko, S
AF Vasilkov, Alexander
Qin, Wenhan
Krotkov, Nickolay
Lamsal, Lok
Spurr, Robert
Haffner, David
Joiner, Joanna
Yang, Eun-Su
Marchenko, Sergey
TI Accounting for the effects of surface BRDF on satellite cloud and
trace-gas retrievals: a new approach based on geometry-dependent
Lambertian equivalent reflectivity applied to OMI algorithms
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID OZONE MONITORING INSTRUMENT; SPACE-BASED MEASUREMENTS; TROPOSPHERIC NO2;
RAMAN-SCATTERING; REFLECTANCE ANISOTROPY; NITROGEN-DIOXIDE; TRANSPORT
MODEL; PRESSURE; WATERS; OCEAN
AB Most satellite nadir ultraviolet and visible cloud, aerosol, and trace-gas algorithms make use of climatological surface reflectivity databases. For example, cloud and NO2 retrievals for the Ozone Monitoring Instrument (OMI) use monthly gridded surface reflectivity climatologies that do not depend upon the observation geometry. In reality, reflection of incoming direct and diffuse solar light from land or ocean surfaces is sensitive to the sun-sensor geometry. This dependence is described by the bidirectional reflectance distribution function (BRDF). To account for the BRDF, we propose to use a new concept of geometry-dependent Lambertian equivalent reflectivity (LER). Implementation within the existing OMI cloud and NO2 retrieval infrastructure requires changes only to the input surface reflectivity database. The geometry-dependent LER is calculated using a vector radiative transfer model with high spatial resolution BRDF information from the Moderate Resolution Imaging Spectro-radiometer (MODIS) over land and the Cox-Munk slope distribution over ocean with a contribution from water-leaving radiance. We compare the geometry-dependent and climatological LERs for two wavelengths, 354 and 466 nm, that are used in OMI cloud algorithms to derive cloud fractions. A detailed comparison of the cloud fractions and pressures derived with climatological and geometry-dependent LERs is carried out. Geometry-dependent LER and corresponding retrieved cloud products are then used as inputs to our OMI NO2 algorithm. We find that replacing the climatological OMI-based LERs with geometry-dependent LERs can increase NO2 vertical columns by up to 50% in highly polluted areas; the differences include both BRDF effects and biases between the MODIS and OMI-based surface reflectance data sets. Only minor changes to NO2 columns (within 5 %) are found over unpolluted and overcast areas.
C1 [Vasilkov, Alexander; Qin, Wenhan; Haffner, David; Yang, Eun-Su; Marchenko, Sergey] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Krotkov, Nickolay; Joiner, Joanna] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Lamsal, Lok] Univ Space Res Assoc, Columbia, MD USA.
[Spurr, Robert] RT Solut, Cambridge, MA USA.
RP Vasilkov, A (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
EM alexander.vasilkov@ssaihq.com
FU NASA
FX Funding for this work was provided in part by the NASA through the Aura
science team program. We thank Pawan K. Bhartia for helpful discussions,
Ziauddin Ahmad for providing data for comparisons, Andrew Sayer for
provision of an updated ocean optics model used in the water-leaving
supplement of the VLIDORT code, and Crystel B. Schaaf for consultation
on the use of the MODIS BRDF product.
NR 51
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U1 0
U2 0
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1867-1381
EI 1867-8548
J9 ATMOS MEAS TECH
JI Atmos. Meas. Tech.
PD JAN 27
PY 2017
VL 10
IS 1
BP 333
EP 349
DI 10.5194/amt-10-333-2017
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EM2VK
UT WOS:000395173700002
ER
PT J
AU Scarino, BR
Minnis, P
Chee, T
Bedka, KM
Yost, CR
Palikonda, R
AF Scarino, Benjamin R.
Minnis, Patrick
Chee, Thad
Bedka, Kristopher M.
Yost, Christopher R.
Palikonda, Rabindra
TI Global clear-sky surface skin temperature from multiple satellites using
a single-channel algorithm with angular anisotropy corrections
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID DATA ASSIMILATION SYSTEM; THERMAL INFRARED EMISSIVITY; REFLECTION
RADIOMETER ASTER; HIGH-RESOLUTION RADIOMETER; SPLIT-WINDOW ALGORITHM;
SUITE VIIRS; MODIS DATA; LAND; VALIDATION; PRODUCTS
AB Surface skin temperature (T-s) is an important parameter for characterizing the energy exchange at the ground/water-atmosphere interface. The Satellite ClOud and Radiation Property retrieval System (SatCORPS) employs a single-channel thermal-infrared (TIR) method to retrieve T-s over clear-sky land and ocean surfaces from data taken by geostationary Earth orbit (GEO) and low Earth orbit (LEO) satellite imagers. GEO satellites can provide somewhat continuous estimates of T-s over the diurnal cycle in non-polar regions, while polar T-s retrievals from LEO imagers, such as the Advanced Very High Resolution Radiometer (AVHRR), can complement the GEO measurements. The combined global coverage of remotely sensed T-s, along with accompanying cloud and surface radiation parameters, produced in near-realtime and from historical satellite data, should be beneficial for both weather and climate applications. For example, near-realtime hourly T-s observations can be assimilated in high-temporal-resolution numerical weather prediction models and historical observations can be used for validation or assimilation of climate models. Key drawbacks to the utility of TIR-derived T-s data include the limitation to clear-sky conditions, the reliance on a particular set of analyses/reanalyses necessary for atmospheric corrections, and the dependence on viewing and illumination angles. Therefore, T-s validation with established references is essential, as is proper evaluation of T-s sensitivity to atmospheric correction source.
This article presents improvements on the NASA Langley GEO satellite and AVHRR TIR-based T-s product that is derived using a single-channel technique. The resulting clear-sky skin temperature values are validated with surface references and independent Satellite products. Furthermore, an empirically adjusted theoretical model of satellite land surface temperature (LST) angular anisotropy is tested to improve satellite LST retrievals. Application of the anisotropic correction yields reduced mean bias and improved precision of GOES-13 LST relative to independent Moderateresolution Imaging Spectroradiometer (MYD11_L2) LST and Atmospheric Radiation Measurement Program ground station measurements. It also significantly reduces inter-satellite differences between LSTs retrieved simultaneously from two different imagers. The implementation of these universal corrections into the SatCORPS product can yield significant improvement in near-global-scale, near-realtime, satellite-based LST measurements. The immediate availability and broad coverage of these skin temperature observations should prove valuable to modelers and climate researchers looking for improved forecasts and better understanding of the global climate model.
C1 [Scarino, Benjamin R.; Chee, Thad; Yost, Christopher R.; Palikonda, Rabindra] Sci Syst & Applicat Inc, 1 Enterprise Pkwy,Suite 200, Hampton, VA 23666 USA.
[Minnis, Patrick; Bedka, Kristopher M.] NASA, Langley Res Ctr, 21 Langley Blvd MS 420, Hampton, VA 23681 USA.
RP Scarino, BR (reprint author), Sci Syst & Applicat Inc, 1 Enterprise Pkwy,Suite 200, Hampton, VA 23666 USA.
EM benjamin.r.scarino@nasa.gov
FU NASA Modeling, Analysis, and Prediction Program; NOAA CDR Program
FX This research was supported by the NASA Modeling, Analysis, and
Prediction Program and the NOAA CDR Program. Computing was supported by
the NASA High End Computing Program. The authors would like to thank
Sarah Bedka and Doug Spangenberg for their generous assistance with
SatCORPS processing.
NR 79
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U1 2
U2 2
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1867-1381
EI 1867-8548
J9 ATMOS MEAS TECH
JI Atmos. Meas. Tech.
PD JAN 27
PY 2017
VL 10
IS 1
BP 351
EP 371
DI 10.5194/amt-10-351-2017
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EM2VK
UT WOS:000395173700003
ER
PT J
AU Herold, N
Behrangi, A
Alexander, LV
AF Herold, Nicholas
Behrangi, Ali
Alexander, Lisa V.
TI Large uncertainties in observed daily precipitation extremes over land
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID UNITED-STATES; CLIMATE; SATELLITE; INDEXES; RAIN; TEMPERATURE;
RESOLUTION; MODEL
AB We explore uncertainties in observed daily precipitation extremes over the terrestrial tropics and subtropics (50 degrees S-50 degrees N) based on five commonly used products: the Climate Hazards Group InfraRed Precipitation with Stations (CHIRPS) dataset, the Global Precipitation Climatology Centre-Full Data Daily (GPCC-FDD) dataset, the Tropical Rainfall Measuring Mission (TRMM) multi-satellite research product (T3B42 v7), the Precipitation Estimation from Remotely Sensed Information using Artificial Neural Networks-Climate Data Record (PERSIANN-CDR), and the Global Precipitation Climatology Project's One-Degree Daily (GPCP-1DD) dataset. We use the precipitation indices R10mm and Rx1day, developed by the Expert Team on Climate Change Detection and Indices, to explore the behavior of "moderate" and "extreme" extremes, respectively. In order to assess the sensitivity of extreme precipitation to different grid sizes we perform our calculations on four common spatial resolutions (0.25 degrees x 0.25 degrees, 1 degrees x1 degrees, 2.5 degrees x 2.5 degrees, and 3.75 degrees x 2.5 degrees). The impact of the chosen "order of operation" in calculating these indices is also determined. Our results show that moderate extremes are relatively insensitive to product and resolution choice, while extreme extremes can be very sensitive. For example, at 0.25 degrees x 0.25 degrees quasi-global mean Rx1day values vary from 37 mm in PERSIANN-CDR to 62 mm in T3B42. We find that the interproduct spread becomes prominent at resolutions of 1 degrees x 1 degrees and finer, thus establishing a minimum effective resolution at which observational products agree. Without improvements in interproduct spread, these exceedingly large observational uncertainties at high spatial resolution may limit the usefulness of model evaluations. As has been found previously, resolution sensitivity can be largely eliminated by applying an order of operation where indices are calculated prior to regridding. However, this approach is not appropriate when true area averages are desired (e.g., for model evaluations).
C1 [Herold, Nicholas; Alexander, Lisa V.] Univ New South Wales, Climate Change Res Ctr, Sydney, NSW, Australia.
[Herold, Nicholas; Alexander, Lisa V.] Univ New South Wales, ARC Ctr Excellence Climate Syst Sci, Sydney, NSW, Australia.
[Behrangi, Ali] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Herold, N (reprint author), Univ New South Wales, Climate Change Res Ctr, Sydney, NSW, Australia.; Herold, N (reprint author), Univ New South Wales, ARC Ctr Excellence Climate Syst Sci, Sydney, NSW, Australia.
EM nicholas.herold@unsw.edu.au
FU ARC [CE110001028]; NASA Energy and Water Cycle Study (NEWS); NASA
WEATHER awards
FX This work contributes to the WCRP Grand Challenge on Extremes. N.H. and
L.V.A. are supported by ARC grant CE110001028. L.V.A. is also supported
by ARC grant DP160103439. Part of the research was carried out at the
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. A.B.
was supported by NASA Energy and Water Cycle Study (NEWS) and NASA
WEATHER awards. The authors would like to thank the anonymous reviewers
for their insightful comments and suggestions that have contributed to
improve this paper. Data were processed and plots were created by using
the National Center for Atmospheric Research Command Language
[UCAR/NCAR/CISL/VETS, 2016] and the R statistical language [Team, R. C.,
2015]. ETCCDI indices were calculated by using the climdex.pcic R
software package [Consortium, D. B. for the P. C. I., 2015], which
represents the official implementation of the ETCCDI indices. GPCP-1DD
was downloaded from Climate and Global Dynamics
(ftp://ftp.cgd.ucar.edu/archive/PRECIP/, accessed 24 March 2015).
GPCC-FDD was downloaded from Deutscher Wetterdienst
(ftp://ftp.dwd.de/pub/data/gpcc/full_data_daily_V1/, accessed 15 July
2015). PERSIANN-CDR was downloaded from the National Center for
Environmental Information
[ftp://eclipse.ncdc.noaa.gov/pub/cdr/persiann/files/, accessed 10 August
2015]. CHIRPS was downloaded from the Climate Hazards Group
(ftp://ftp.chg.ucsb.edu/pub/org/chg/products/CHIRPS-2.0/global_daily/net
cdf/p25/, accessed 10 August 2015). T3B42 was downloaded from Goddard
Earth Sciences Data and Information Services Center
(http://disc.sci.gsfc.nasa.gov/TRMM, accessed 10 August 2015).
NR 48
TC 0
Z9 0
U1 1
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 27
PY 2017
VL 122
IS 2
BP 668
EP 681
DI 10.1002/2016JD025842
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EN6MA
UT WOS:000396116900006
ER
PT J
AU Jiang, XN
AF Jiang, Xianan
TI Key processes for the eastward propagation of the Madden-Julian
Oscillation based on multimodel simulations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID STATIC ENERGY BUDGET; TROPICAL INTRASEASONAL OSCILLATION; MARITIME
CONTINENT; INTERIM REANALYSIS; VERTICAL STRUCTURE; PHYSICAL PROCESSES;
MOISTURE MODES; MJO; CLIMATE; ATMOSPHERE
AB As a prominent climate variability mode with widespread influences on global weather extremes, the Madden-Julian Oscillation (MJO) remains poorly represented in the latest generation of general circulation models (GCMs), with a particular challenge in simulating its eastward propagating convective signals. In this study, by analyzing multimodel simulations from a recent global MJO model evaluation project, an effort is made to identify key processes for the eastward propagation of the MJO through analyses of moisture entropy (ME) processes under a "moisture mode" framework for the MJO. The column-integrated horizontal ME advection is found to play a critical role for the eastward propagation of the MJO in both observations and good MJO models, with a primary contribution through advection of the lower tropospheric seasonal mean ME by the MJO anomalous circulations. By contrast, the horizontal ME advection effect for the eastward propagation is greatly underestimated in poor MJO GCMs, due to model deficiencies in simulating both the seasonal mean ME pattern and MJO circulations, leading to a largely stationary MJO mode in these GCMs. These results thus pinpoint an important guidance toward improved representation of the MJO in climate and weather forecast models. While this study mainly focuses on fundamental physics for the MJO propagation over the Indian Ocean, complex influences by the Maritime Continent on the MJO and also ME processes associated with the MJO over the western Pacific warrant further investigations.
C1 [Jiang, Xianan] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
[Jiang, Xianan] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
RP Jiang, XN (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.; Jiang, XN (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM xianan@ucla.edu
FU National Science Foundation (NSF) [AGS-1228302]; NOAA Climate Program
Office MAPP program [NA12OAR4310075, NA15OAR4310098]; CVP program
[NA15OAR4310177]
FX We thank modeling groups for making available their model output through
the MJOTF/GASS MJO project. The multimodel output collected by this
project and analyzed in this study is available for free download from
https://earthsystemcog.org/projects/gassyotc-mip/. We acknowledge the
insightful comments from the Editor, C. Zhang, and two anonymous
reviewers. The author is indebted to E. Maloney, M. Zhao, D. Waliser, B.
Wang, M. Pritchard, and WGNE MJO Task Force members for stimulating
discussions during the course of this study. X. Jiang acknowledges
support by the National Science Foundation (NSF) Climate and Large-Scale
Dynamics Program under award AGS-1228302 and NOAA Climate Program Office
MAPP program under awards NA12OAR4310075, NA15OAR4310098, and CVP
program under award NA15OAR4310177.
NR 63
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U1 2
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 27
PY 2017
VL 122
IS 2
BP 755
EP 770
DI 10.1002/2016JD025955
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EN6MA
UT WOS:000396116900012
ER
PT J
AU Chiacchio, M
Pausata, FSR
Messori, G
Hannachi, A
Chin, M
Onskog, T
Ekman, AML
Barrie, L
AF Chiacchio, Marc
Pausata, Francesco S. R.
Messori, Gabriele
Hannachi, Abdel
Chin, Mian
Onskog, Thomas
Ekman, Annica M. L.
Barrie, Leonard
TI On the links between meteorological variables, aerosols, and tropical
cyclone frequency in individual ocean basins
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID WESTERN NORTH PACIFIC; SEA-SURFACE-TEMPERATURE; SEASONAL HURRICANE
FREQUENCY; QUASI-BIENNIAL OSCILLATION; R-SQUARED MEASURES; POTENTIAL
INTENSITY; EL-NINO; SOUTHERN-OSCILLATION; INTERANNUAL VARIABILITY;
ATLANTIC HURRICANES
AB A generalized linear model based on Poisson regression has been used to assess the impact of environmental variables modulating tropical cyclone frequency in six main cyclone development areas: the East Pacific, West Pacific, North Atlantic, North Indian, South Indian, and South Pacific. The analysis covers the period 1980-2009 and focuses on widely used meteorological parameters including wind shear, sea surface temperature, and relative humidity from different reanalyses as well as aerosol optical depth for different compounds simulated by the Goddard Chemistry Aerosol Radiation and Transport model. Circulation indices are also included. Cyclone frequency is obtained from the International Best Track Archive for Climate Stewardship. A strong link is found between cyclone frequency and the relative sea surface temperature, Atlantic Meridional Mode, and wind shear with significant explained log likelihoods in the North Atlantic of 37%, 27%, and 28%, respectively. A significant impact of black carbon and organic aerosols on cyclone frequency is found over the North Indian Ocean, with explained log likelihoods of 27%. A weaker but still significant impact is found for observed dust aerosols in the North Atlantic with an explained log likelihood of 11%. Changes in lower stratospheric temperatures explain 28% of the log likelihood in the North Atlantic. Lower stratospheric temperatures from a subset of Coupled Model Intercomparison Project Phase 5 models properly simulate the warming and subsequent cooling of the lower stratosphere that follows a volcanic eruption but underestimates the cooling by about 0.5 degrees C.
C1 [Chiacchio, Marc; Pausata, Francesco S. R.; Messori, Gabriele; Hannachi, Abdel; Ekman, Annica M. L.; Barrie, Leonard] Stockholm Univ, Dept Meteorol, Stockholm, Sweden.
[Chiacchio, Marc; Pausata, Francesco S. R.; Messori, Gabriele; Ekman, Annica M. L.; Barrie, Leonard] Bert Bolin Ctr Climate Res, Stockholm, Sweden.
[Chin, Mian] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Onskog, Thomas] KTH, Dept Math, Stockholm, Sweden.
RP Chiacchio, M (reprint author), Stockholm Univ, Dept Meteorol, Stockholm, Sweden.; Chiacchio, M (reprint author), Bert Bolin Ctr Climate Res, Stockholm, Sweden.
EM marc.chiacchio@misu.su.se
OI Hannachi, Abdelwaheb/0000-0002-8255-5186; Onskog,
Thomas/0000-0003-2716-3195
FU Bolin Centre for Climate Research; Department of Meteorology at the
University of Stockholm; Swedish Vetenskapsradet (MILEX project)
FX This study was financially supported by the Bolin Centre for Climate
Research, the Department of Meteorology at the University of Stockholm,
and the Swedish Vetenskapsradet (MILEX project). The IBTrACS data set
was obtained from the NOAA National Climatic Data Center
(https://www.ncdc.noaa.gov/ibtracs/). NCEP reanalysis data were
retrieved from the NOAA Earth Systems Research Laboratory
(http://www.esrl.noaa.gov/psd/data/gridded/data.ncep.reanalysis. html).
ERA-Interim data were taken from the European Centre for Medium-Range
Weather Forecasts (http://apps.ecmwf.int/datasets/). MERRA data were
obtained from the Modeling and the Assimilation Data and Information
Services Center (MDISC) at NASA Goddard
(http://disc.sci.gsfc.nasa.gov/daac-bin/DataHoldings.pl). All
circulation indices were obtained from the NOAA Earth Systems Research
Laboratory (http://www.esrl.noaa.gov/psd/data/climateindices/list/).
Observed dust AOD was obtained from the Atlantic Aerosol Products on
http://evan.ucsd.edu/Data.html.
NR 114
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U1 2
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 27
PY 2017
VL 122
IS 2
BP 802
EP 822
DI 10.1002/2015JD024593
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EN6MA
UT WOS:000396116900015
ER
PT J
AU Yue, Q
Kahn, BH
Fetzer, EJ
Wong, S
Frey, R
Meyer, KG
AF Yue, Qing
Kahn, Brian H.
Fetzer, Eric J.
Wong, Sun
Frey, Richard
Meyer, Kerry G.
TI On the response of MODIS cloud coverage to global mean surface air
temperature
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID CLIMATE FEEDBACKS; RADIATIVE KERNELS; OPTICAL-THICKNESS; PART II;
TRENDS; TERRA; ISCCP; INSTRUMENT; SATELLITE; MODELS
AB The global surface temperature change (Delta T-s) mediated cloud cover response is directly related to cloud-climate feedback. Using satellite remote sensing data to relate cloud and climate requires a well-calibrated, stable, and consistent long-term cloud data record. The Collection 5.1 (C5) Moderate Resolution Imaging Spectroradiometer (MODIS) cloud observations have been widely used for this purpose. However, the MODIS data quality varies greatly with the surface type, spectral region, cloud type, and time periods of study, which calls for additional caution when applying such data to studies on cloud cover temporal trends and variability. Using 15 years of cloud observations made by Terra and Aqua MODIS, we analyze the Delta T-s-mediated cloud cover response for different cloud types by linearly regressing the monthly anomaly of cloud cover (Delta C) with the monthly anomaly of global T-s. The Collection 6 (C6) Aqua data exhibit a similar cloud response to the long-term counterpart simulated by advanced climate models. A robust increase in altitude with increasing Delta T-s is found for high clouds, while a robust decrease of Delta C is noticed for optically thick low clouds. The large differences between C5 and C6 results are from improvements in calibration and cloud retrieval algorithms. The large positive cloud cover responses with data after 2010 and the strong sensitivity to time period obtained from the Terra (C5 and C6) data are likely due to calibration drift that has not been corrected, suggesting that the previous estimate of the short-term cloud cover response from the these data should be revisited.
C1 [Yue, Qing; Kahn, Brian H.; Fetzer, Eric J.; Wong, Sun] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
[Frey, Richard] Univ Wisconsin Madison, Cooperat Inst Meteorol Satellite Studies, Madison, WI USA.
[Meyer, Kerry G.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA.
RP Yue, Q (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM Qing.Yue@jpl.nasa.gov
RI Yue, Qing/F-4619-2017; Meyer, Kerry/E-8095-2016
OI Yue, Qing/0000-0002-3559-6508; Meyer, Kerry/0000-0001-5361-9200
FU NASA [NNH15ZDA001N-CCST, NNN13D455T, NNX14AN48G]; AIRS Project at JPL
FX The authors would like to thank Chen Zhou and Mark Zelinka from the
Lawrence Livermore National Laboratory and Steve Ackerman and Steve
Platnick from the MODIS team for the helpful discussions. The research
described in this paper was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration. Q.Y., E.J.F., and
S.W. were supported by the NASA's Making Earth Science Data Records for
Use in Research Environments Program. Q.Y. was supported by the NASA
CloudSat and CALIPSO Science Team Recompete NNH15ZDA001N-CCST grant.
B.H.K. was partially supported by the NASA Science of Terra and Aqua
program under grant NNN13D455T. Q.Y., E.J.F., S.W., and B.H.K.
acknowledge the support of the AIRS Project at JPL. R.F. was supported
by NASA NNX14AN48G (MODIS maintenance). MODIS data were obtained through
the Level-1 Atmosphere Archive and Distribution System
(http://ladsweb.nascom.nasa.gov/) and the CERES SSF-Level2 ordering page
(http://ceres.larc.nasa.gov/products-info.php?product= SSF-Level2).
NR 47
TC 1
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U1 1
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 27
PY 2017
VL 122
IS 2
BP 966
EP 979
DI 10.1002/2016JD025174
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EN6MA
UT WOS:000396116900024
ER
PT J
AU Guzman, R
Chepfer, H
Noel, V
de Guelis, TV
Kay, JE
Raberanto, P
Cesana, G
Vaughan, MA
Winker, DM
AF Guzman, R.
Chepfer, H.
Noel, V.
de Guelis, T. Vaillant
Kay, J. E.
Raberanto, P.
Cesana, G.
Vaughan, M. A.
Winker, D. M.
TI Direct atmosphere opacity observations from CALIPSO provide new
constraints on cloud-radiation interactions
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SATELLITE-OBSERVATIONS; MODEL; BIASES; PHASE
AB The spaceborne lidar CALIPSO (Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observation) directly measures atmospheric opacity. In 8 years of CALIPSO observations, we find that 69% of vertical profiles penetrate through the complete atmosphere. The remaining 31% do not reach the surface, due to opaque clouds. The global mean altitude of full attenuation of the lidar beam (z_opaque) is 3.2 km, but there are large regional variations in this altitude. Of relevance to cloud-climate studies, the annual zonal mean longwave cloud radiative effect and annual zonal mean z_opaque weighted by opaque cloud cover are highly correlated (0.94). The annual zonal mean shortwave cloud radiative effect and annual zonal mean opaque cloud cover are also correlated (-0.95). The new diagnostics introduced here are implemented within a simulator framework to enable scale-aware and definition-aware evaluation of the LMDZ5B global climate model. The evaluation shows that the model overestimates opaque cloud cover (31% obs. versus 38% model) and z_opaque (3.2 km obs. versus 5.1 km model). In contrast, the model underestimates thin cloud cover (35% obs. versus 14% model). Further assessment shows that reasonable agreement between modeled and observed longwave cloud radiative effects results from compensating errors between insufficient warming by thin clouds and excessive warming due to overestimating both z_opaque and opaque cloud cover. This work shows the power of spaceborne lidar observations to directly constrain cloud-radiation interactions in both observations and models.
C1 [Guzman, R.; Raberanto, P.] CNRS, Ecole Polytechn, LMD IPSL, Palaiseau, France.
[Chepfer, H.; de Guelis, T. Vaillant] Univ Paris 06, LMD IPSL, Paris, France.
[Noel, V.] LA CNRS, Toulouse, France.
[Kay, J. E.] Univ Colorado Boulder, CIRES ATOC, Boulder, CO USA.
[Cesana, G.] CALTECH, JPL, Pasadena, CA USA.
[Vaughan, M. A.; Winker, D. M.] NASA Langley Res Ctr, Hampton, VA USA.
RP Guzman, R (reprint author), CNRS, Ecole Polytechn, LMD IPSL, Palaiseau, France.
EM rodrigo.guzman@lmd.polytechnique.fr
OI Guzman, Rodrigo/0000-0002-7653-1276
FU CNES; NASA [12-CCST10-0095]
FX The authors would like to thank NASA, CNES, Icare, and Climserv for
giving access to the CALIOP data. Special thanks are due to Climserv for
computing resources which let us perform all the data analysis and to
produce this new version of the GOCCP product. This work was supported
by CNES and NASA grant 12-CCST10-0095. The GOCCP v3.0 products presented
in this article are available online through the GOCCP website
(http://climserv.ipsl.polytechnique.fr/cfmip-obs/Calipso_goccp.html).
The new diagnostics will be available in COSP V2. Thanks are due to the
two anonymous reviewers who helped to significantly improve this
manuscript.
NR 33
TC 0
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U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 27
PY 2017
VL 122
IS 2
BP 1066
EP 1085
DI 10.1002/2016JD025946
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EN6MA
UT WOS:000396116900030
ER
PT J
AU Perring, AE
Schwarz, JP
Markovic, MZ
Fahey, DW
Jimenez, JL
Campuzano-Jost, P
Palm, BD
Wisthaler, A
Mikoviny, T
Diskin, G
Sachse, G
Ziemba, L
Anderson, B
Shingler, T
Crosbie, E
Sorooshian, A
Yokelson, R
Gao, RS
AF Perring, Anne E.
Schwarz, Joshua P.
Markovic, Milos Z.
Fahey, David W.
Jimenez, Jose L.
Campuzano-Jost, Pedro
Palm, Brett D.
Wisthaler, Armin
Mikoviny, Tomas
Diskin, Glenn
Sachse, Glen
Ziemba, Luke
Anderson, Bruce
Shingler, Taylor
Crosbie, Ewan
Sorooshian, Armin
Yokelson, Robert
Gao, Ru-Shan
TI In situ measurements of water uptake by black carbon-containing aerosol
in wildfire plumes
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID PARTICLE SOOT PHOTOMETER; CONDENSATION NUCLEUS ACTIVITY; LONG-RANGE
TRANSPORT; ORGANIC AEROSOL; OPTICAL-PROPERTIES; HYGROSCOPIC PROPERTIES;
MIXING STATE; ATMOSPHERIC LIFETIME; SMOKE; EVOLUTION
AB Water uptake by black carbon (BC)-containing aerosol was quantified in North American wildfire plumes of varying age (1 to similar to 40 h old) sampled during the SEAC(4)RS mission (2013). A Humidified Dual SP2 (HD-SP2) is used to optically size BC-containing particles under dry and humid conditions from which we extract the hygroscopicity parameter, kappa , of materials internally mixed with BC. Instrumental variability and the uncertainty of the technique are briefly discussed. An ensemble average kappa of 0.04 is found for the set of plumes sampled, consistent with previous estimates of bulk aerosol hygroscopicity from biomass burning sources. The temporal evolution of kappa in the Yosemite Rim Fire plume is explored to constrain the rate of conversion of BC-containing aerosol from hydrophobic to more hydrophilic modes in these emissions. A BC-specific kappa increase of similar to 0.06 over 40 h is found, fit well with an exponential curve corresponding to a transition from a kappa of 0 to a kappa of similar to 0.09 with an e-folding time of 29 h. Although only a few percent of wildfire particles contain BC, a similar kappa increase is estimated for bulk aerosol and the measured aerosol composition is used to infer that the observed kappa change is driven by a combination of incorporation of ammonium sulfate and oxidation of existing organic materials. Finally, a substantial fraction of wildfire-generated BC-containing aerosol is calculated to be active as cloud condensation nuclei shortly after emission likely indicating efficient wet removal. These results can constrain model treatment of BC from wildfire sources.
C1 [Perring, Anne E.; Schwarz, Joshua P.; Markovic, Milos Z.; Fahey, David W.; Gao, Ru-Shan] NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO 80305 USA.
[Perring, Anne E.; Markovic, Milos Z.; Jimenez, Jose L.; Campuzano-Jost, Pedro; Palm, Brett D.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Markovic, Milos Z.] Picarro Inc, Toronto, ON, Canada.
[Jimenez, Jose L.; Campuzano-Jost, Pedro; Palm, Brett D.] Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA.
[Wisthaler, Armin; Mikoviny, Tomas] Univ Oslo, Dept Chem, Oslo, Norway.
[Wisthaler, Armin] Univ Innsbruck, Inst Ion Phys & Appl Phys, Innsbruck, Austria.
[Diskin, Glenn; Sachse, Glen; Ziemba, Luke; Anderson, Bruce; Crosbie, Ewan] NASA, Langley Res Ctr, Hampton, VA USA.
[Shingler, Taylor; Crosbie, Ewan; Sorooshian, Armin] Univ Arizona, Dept Chem & Environm Engn, Tucson, AZ USA.
[Sorooshian, Armin] Univ Arizona, Dept Hydrol & Atmospher Sci, Tucson, AZ USA.
[Yokelson, Robert] Univ Montana, Dept Chem, Missoula, MT 59812 USA.
RP Perring, AE (reprint author), NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO 80305 USA.
EM Anne.Perring@noaa.gov
RI Yokelson, Robert/C-9971-2011;
OI Yokelson, Robert/0000-0002-8415-6808; PERRING, ANNE/0000-0003-2231-7503;
Jimenez, Jose L/0000-0001-6203-1847; Fahey, David/0000-0003-1720-0634
FU NOAA Atmospheric Composition and Climate Program; NASA Radiation
Sciences Program; NASA Upper Atmosphere Research Program; NASA
[NNX12AC10G, NNX14AP75G, NNX14AK79H, NNX12AC03G, NNX15AT96G]; NASA Earth
Science Division [NNX12AC20G, NNX14AP45G]
FX All data for the SEAC4RS project are publicly available at DOI
10.5067/Aircraft/SEAC4RS/Aerosol-TraceGas-Cloud. NOAA SP2 research
conducted by A.P., M.M., J.S., R.S.G., and D.F. was supported by the
NOAA Atmospheric Composition and Climate Program, the NASA Radiation
Sciences Program, and the NASA Upper Atmosphere Research Program. A.S.
and T.S. were funded by NASA grants NNX12AC10G, NNX14AP75G, and
NNX14AK79H. P.C.J., B.D.P., and J.L.J. were supported by NASA grants
NNX12AC03G and NNX15AT96G. R.Y. was supported by NASA Earth Science
Division Awards NNX12AC20G and NNX14AP45G.
NR 63
TC 0
Z9 0
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 27
PY 2017
VL 122
IS 2
BP 1086
EP 1097
DI 10.1002/2016JD025688
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EN6MA
UT WOS:000396116900031
ER
PT J
AU Kim, MH
Omar, AH
Vaughan, MA
Winker, DM
Trepte, CR
Hu, YX
Liu, ZY
Kim, SW
AF Kim, Man-Hae
Omar, Ali H.
Vaughan, Mark A.
Winker, David M.
Trepte, Charles R.
Hu, Yongxiang
Liu, Zhaoyan
Kim, Sang-Woo
TI Quantifying the low bias of CALIPSO's column aerosol optical depth due
to undetected aerosol layers
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID GROUND-BASED LIDAR; SPECTRAL-RESOLUTION LIDAR; REMOTE-SENSING DATA;
RAMAN LIDAR; AIRBORNE MEASUREMENTS; DUST AEROSOL; BORNE LIDAR;
MODIS-AQUA; CALIOP; AERONET
AB The Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) data processing scheme only retrieves extinction profiles in those portions of the return signal where cloud or aerosol layers have been identified by the CALIOP layer detection scheme. In this study we use 2 years of CALIOP and Moderate Resolution Imaging Spectroradiometer (MODIS) data to quantify the aerosol optical depth of undetected weakly backscattering layers. Aerosol extinction and column-averaged lidar ratio is retrieved from CALIOP level 1B (version 4) profile using MODIS aerosol optical depth (AOD) as a constraint over oceans from March 2013 to February 2015. To quantify the undetected layer AOD (ULA), an unconstrained retrieval is applied globally using a lidar ratio of 28.75 sr estimated from constrained retrievals during the daytime over the ocean. We find a global mean ULA of 0.031 +/- 0.052. There is no significant difference in ULA between land and ocean. However, the fraction of undetected aerosol layers rises considerably during daytime, when the large amount of solar background noise lowers the signal-to-noise ratio. For this reason, there is a difference in ULA between day (0.036 +/- 0.066) and night (0.025 +/- 0.021). ULA is larger in the northern hemisphere and relatively larger at high latitudes. Large ULA for the polar regions is strongly related to the cases where the CALIOP level 2 product reports zero AOD. This study provides an estimate of the complement of AOD that is not detected by lidar and bounds the CALIOP AOD uncertainty to provide corrections for science studies that employ the CALIOP level 2 AOD.
C1 [Kim, Man-Hae; Omar, Ali H.; Vaughan, Mark A.; Winker, David M.; Trepte, Charles R.; Hu, Yongxiang; Liu, Zhaoyan] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Kim, Man-Hae] Univ Space Res Assoc, Columbia, MD USA.
[Liu, Zhaoyan] Sci Syst & Applicat Inc, Hampton, VA USA.
[Kim, Sang-Woo] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul, South Korea.
RP Kim, MH (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
EM man-hae.kim@nasa.gov
RI Hu, Yongxiang/K-4426-2012
FU NASA; KMA R&D program under grant KMIPA
FX The CALIPSO data used in this study were obtained from the NASA Langley
Atmospheric Science Data Center
(https://eosweb.larc.nasa.gov/project/calipso/calipso_table). The MODIS
data were obtained through the NASA Goddard Space and Flight Center Data
Center Atmosphere Archive and Distribution System
(https://ladsweb.nascom.nasa.gov/). Man-Hae Kim was supported by a NASA
Postdoctoral Program Fellowship. Sang-Woo Kim was supported by the KMA
R&D program under grant KMIPA 2015-2011.
NR 68
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PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 27
PY 2017
VL 122
IS 2
BP 1098
EP 1113
DI 10.1002/2016JD025797
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EN6MA
UT WOS:000396116900032
ER
PT J
AU Gogoi, MM
Babu, SS
Moorthy, KK
Bhuyan, PK
Pathak, B
Subba, T
Chutia, L
Kundu, SS
Bharali, C
Borgohain, A
Guha, A
De, BK
Singh, B
Chin, M
AF Gogoi, Mukunda M.
Babu, S. Suresh
Moorthy, K. Krishna
Bhuyan, Pradip Kumar
Pathak, Binita
Subba, Tamanna
Chutia, Lakhima
Kundu, Shyam Sundar
Bharali, Chandrakala
Borgohain, Arup
Guha, Anirban
De, Barin Kumar
Singh, Brajamani
Chin, Mian
TI Radiative effects of absorbing aerosols over northeastern India:
Observations and model simulations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID BIOMASS BURNING AEROSOLS; BLACK CARBON CONCENTRATION; FOSSIL-FUEL
COMBUSTION; REAL-TIME MEASUREMENT; LIGHT-ABSORPTION; OPTICAL-PROPERTIES;
TIBETAN PLATEAU; BROWN CARBON; SOUTH-ASIA; SEASONAL-VARIATION
AB Multiyear measurements of spectral properties of aerosol absorption are examined over four geographically distinct locations of northeastern India. Results indicated significant spatiotemporal variation in aerosol absorption coefficients (sigma(abs)) with highest values in winter and lowest in monsoon. The western parts of the region, close to the outflow of Indo-Gangetic Plains, showed higher values of sigma(abs) and black carbon (BC) concentration-mostly associated with fossil fuel combustion. But, the eastern parts showed higher contributions from biomass-burning aerosols, as much as 20-25% to the total aerosol absorption, conspicuously during premonsoon season. This is attributed to a large number of burning activities over the Southeast Asian region, as depicted from Moderate Resolution Imaging Spectroradiometer fire count maps, whose spatial extent and magnitude peaks during March/April. The nearly consistent high values of aerosol index (AI) and layer height from Ozone Monitoring Instrument indicate the presence of absorbing aerosols in the upper atmosphere. The observed seasonality has been captured fairly well by Goddard Chemistry Aerosol Radiation and Transport (GOCART) as well as Weather Research and Forecasting-Chemistry (WRF-Chem) model simulations. The ratio of column-integrated optical depths due to particulate organic matter and BC from GOCART showed good coincidence with satellite-based observations, indicating the increased vertical dispersion of absorbing aerosols, probably by the additional local convection due to higher fire radiative power caused by the intense biomass-burning activities. In the WRF-Chem though underperformed by different magnitude in winter, the values are closer or overestimated near the burnt areas. Atmospheric forcing due to BC was highest (similar to 30 Wm(-2)) over the western part associated with the fossil fuel combustion.
C1 [Gogoi, Mukunda M.; Babu, S. Suresh] ISRO, Vikram Sarabhai Space Ctr, Space Phys Lab, Trivandrum, Kerala, India.
[Moorthy, K. Krishna] Indian Inst Sci, CAOS, Bangalore, Karnataka, India.
[Bhuyan, Pradip Kumar; Pathak, Binita; Subba, Tamanna; Chutia, Lakhima; Bharali, Chandrakala] Dibrugarh Univ, Ctr Atmospher Studies, Dibrugarh, Assam, India.
[Kundu, Shyam Sundar; Borgohain, Arup] North Eastern Space Applicat Ctr, Shillong, Meghalaya, India.
[Guha, Anirban; De, Barin Kumar] Tripura Univ, Dept Phys, Agartala, India.
[Singh, Brajamani] Manipur Univ, Dept Phys, Imphal, Manipur, India.
[Chin, Mian] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Gogoi, MM (reprint author), ISRO, Vikram Sarabhai Space Ctr, Space Phys Lab, Trivandrum, Kerala, India.
EM dr_mukunda@vssc.gov.in
OI Kundu, Shyam S/0000-0003-2386-4912
NR 111
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PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 27
PY 2017
VL 122
IS 2
BP 1132
EP 1157
DI 10.1002/2016JD025592
PG 26
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EN6MA
UT WOS:000396116900034
ER
PT J
AU Zhu, YQ
Toon, OB
Pitts, MC
Lambert, A
Bardeen, C
Kinnison, DE
AF Zhu, Yunqian
Toon, Owen B.
Pitts, Michael C.
Lambert, Alyn
Bardeen, Charles
Kinnison, Douglas E.
TI Comparing simulated PSC optical properties with CALIPSO observations
during the 2010 Antarctic winter
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID POLAR STRATOSPHERIC CLOUDS; NITRIC-ACID TRIHYDRATE; COMMUNITY CLIMATE
MODEL; ARCTIC STRATOSPHERE; OZONE DEPLETION; HETEROGENEOUS FORMATION;
LIDAR OBSERVATIONS; UPPER TROPOSPHERE; NUCLEATION; DENITRIFICATION
AB We simulate polar stratospheric clouds (PSCs) during the Antarctic winter of 2010 using the Specified Dynamics version of the Whole Atmosphere Community Climate Model/Community Aerosol and Radiation Model for Atmospheres (SD-WACCM/CARMA) model. The current PSC model contains microphysical schemes for supercooled ternary solutions (STS) and nitric acid trihydrate (NAT) particles, as well as a prognostic treatment for PSC ice particles and dehydration. Our simulations and CALIPSO satellite data suggest two major NAT particle formation mechanisms. The first mechanism is the nucleation of NAT from STS. Our model, with homogeneous nucleation rates of NAT from STS constrained by observations from the Arctic winter of 2010-2011, reproduces optical properties observed by CALIPSO over Antarctica in May and the timing of denitrification observed by the Microwave Limb Sounder within their uncertainties. On the other hand, the CALIPSO data indicate that our simulations are missing clouds containing small NAT particles with large number densities. We suggest these particles are most likely to form from ice clouds or STS in gravity waves, as found by previous investigations. The simulated cloud coverage agrees with the CALIPSO cloud coverage within a few percent on average with a correlation coefficient of 0.83. However, using the CALIPSO classification algorithm, simulated ice clouds often fall into Mix categories under the denitrified and dehydrated conditions. The model needs an improved ice microphysical representation, not only to allow ice particles to be a source of NAT but also to provide information on ice cloud particle number and size so that ice cloud optical properties can be more precisely calculated for comparison with CALIPSO data.
C1 [Zhu, Yunqian; Toon, Owen B.] Univ Colorado Boulder, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[Toon, Owen B.] Univ Colorado Boulder, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
[Pitts, Michael C.] Langley Res Ctr, Hampton, VA USA.
[Lambert, Alyn] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Bardeen, Charles; Kinnison, Douglas E.] Natl Ctr Atmospher Res, Boulder, CO USA.
RP Zhu, YQ (reprint author), Univ Colorado Boulder, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
EM yunqian.zhu@colorado.edu
OI Kinnison, Douglas/0000-0002-3418-0834
FU NASA [NNX09AK71G]; National Science Foundation
FX The work at the University of Colorado was supported by NASA grant
NNX09AK71G from the AURA satellite project. The work at the Jet
Propulsion Laboratory, California Institute of Technology, was carried
out under a contract with the National Aeronautics and Space
Administration. We thank Lamont Poole at NASA Langley Research Center
for his help with the CALIPSO classification algorithm. We thank A.T.J.
de Laat from Royal Netherlands Meteorological Institute for his help
with MLS data. We thank Jens-Uwe Grooss and Ines Tritscher from
Forschungszentrum Juelich for their help with the noise uncertainty
estimation for the CALIPSO algorithm. We would like to acknowledge
high-performance computing support from Yellowstone
(ark:/85065/d7wd3xhc) provided by NCAR's Computational and Information
Systems Laboratory, sponsored by the National Science Foundation. The
source code for WACCM/CARMA model used in this study is freely available
at http://www2.cesm.ucar.edu/ upon registration. The developing version
of this model, the data, and input files necessary to reproduce the
experiments are available from the authors upon request
(yunqian.zhu@colorado.edu). The data are archived at the Toon Aerosol
Research Group computers.
NR 62
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PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 27
PY 2017
VL 122
IS 2
BP 1175
EP 1202
DI 10.1002/2016JD025191
PG 28
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EN6MA
UT WOS:000396116900036
ER
PT J
AU Stauffer, RM
Thompson, AM
Oltmans, SJ
Johnson, BJ
AF Stauffer, Ryan M.
Thompson, Anne M.
Oltmans, Samuel J.
Johnson, Bryan J.
TI Tropospheric ozonesonde profiles at long-term US monitoring sites: 2.
Links between Trinidad Head, CA, profile clusters and inland surface
ozone measurements
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID TRANSPORTED BACKGROUND OZONE; AIR-QUALITY; STRATOSPHERIC INTRUSIONS;
UNITED-STATES; NORTH-AMERICA; LIGHTNING NOX; SUMMERTIME; EXCHANGE;
IMPACT; CLIMATOLOGY
AB Much attention has been focused on the transport of ozone (O-3) to the western U.S., particularly given the latest revision of the National Ambient Air Quality Standard to 70 parts per billion by volume (ppbv) of O-3. This makes quantifying the contributions of stratosphere-to-troposphere exchange, local pollution, and pollution transport to this region essential. To evaluate free-tropospheric and surface O-3 in the western U.S., we use self-organizing maps to cluster 18 years of ozonesonde profiles from Trinidad Head, CA. Three of nine O-3 mixing ratio profile clusters exhibit thin laminae of high O-3 above Trinidad Head. The high O-3 layers are located between 1 and 6 km above mean sea level and reside above an inversion associated with a northern location of the Pacific subtropical high. Ancillary data (reanalyses, trajectories, and remotely sensed carbon monoxide) help identify the high O-3 sources in one cluster, but distinguishing mixed influences on the elevated O-3 in other clusters is difficult. Correlations between the elevated tropospheric O-3 and surface O-3 at high-altitude monitors at Lassen Volcanic and Yosemite National Parks, and Truckee, CA, are marked and long lasting. The temporal correlations likely result from a combination of transport of baseline O-3 and covarying meteorological parameters. Days corresponding to the high O-3 clusters exhibit hourly surface O-3 anomalies of +5-10 ppbv compared to a climatology; the positive anomalies can last up to 3 days after the ozonesonde profile. The profile and surface O-3 links demonstrate the importance of regular ozonesonde profiling at Trinidad Head.
C1 [Stauffer, Ryan M.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Stauffer, Ryan M.; Thompson, Anne M.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
[Stauffer, Ryan M.] NASA, Univ Space Res Assoc, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD USA.
[Thompson, Anne M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Oltmans, Samuel J.] Univ Colorado Boulder, Cooperat Inst Res Environm Sci, Boulder, CO USA.
[Oltmans, Samuel J.; Johnson, Bryan J.] NOAA Earth Syst Res Lab, Global Monitoring Div, Boulder, CO USA.
RP Stauffer, RM (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
EM ryan.m.stauffer@nasa.gov
FU NASA [NNG05G062G, NNX10AR39G, NNX11AQ44G, NNX12AF05G]; NASA
FX Funding for this project was provided by the following NASA grants
NNG05G062G, NNX10AR39G, NNX11AQ44G, and NNX12AF05G. Funding for R.
Stauffer was also provided through the NASA Postdoctoral Program at NASA
GSFC administered by the Universities Space Research Association. This
paper is the basis for a chapter in the first author's PhD dissertation.
NOAA ESRL GMD data (Trinidad Head ozonesondes) can be accessed at
ftp://ftp.cmdl.noaa.gov/data/ozwv/Ozonesonde/. ERA-Interim reanalysis
data can be accessed at http://rda.ucar.edu/datasets/ds627.0/.NCEP/NCAR
reanalysis data can accessed at ftp://ftp.cdc.noaa.gov/. AIRS CO and
O3 data can be accessed at
http://acdisc.sci.gsfc.nasa.gov/open-dap/Aqua_AIRS_Level3/AIRX3STD.006/.
Surface O3 data can be accessed at
http://java.epa.gov/castnet/clearsession. do (Lassen and Yosemite) and
https://aqs.epa.gov/api (Truckee). Thanks to George Young and William
Brune (Penn State) for their valuable comments and suggestions for
meteorological analyses. We thank the Editor and three anonymous
reviewers whose suggestions improved the manuscript.
NR 47
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PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 27
PY 2017
VL 122
IS 2
BP 1261
EP 1280
DI 10.1002/2016JD025254
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EN6MA
UT WOS:000396116900040
ER
PT J
AU Kuang, S
Newchurch, MJ
Johnson, MS
Wang, LH
Burris, J
Pierce, RB
Eloranta, EW
Pollack, IB
Graus, M
de Gouw, J
Warneke, C
Ryerson, TB
Markovic, MZ
Holloway, JS
Pour-Biazar, A
Huang, GY
Liu, X
Feng, N
AF Kuang, Shi
Newchurch, Michael J.
Johnson, Matthew S.
Wang, Lihua
Burris, John
Pierce, Robert B.
Eloranta, Edwin W.
Pollack, Ilana B.
Graus, Martin
de Gouw, Joost
Warneke, Carsten
Ryerson, Thomas B.
Markovic, Milos Z.
Holloway, John S.
Pour-Biazar, Arastoo
Huang, Guanyu
Liu, Xiong
Feng, Nan
TI Summertime tropospheric ozone enhancement associated with a cold front
passage due to stratosphere-to-troposphere transport and biomass
burning: Simultaneous ground-based lidar and airborne measurements
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID CROSS-TROPOPAUSE EXCHANGE; SPECTRAL-RESOLUTION LIDAR; SOUTHEAST
UNITED-STATES; US ANTHROPOGENIC AEROSOLS; EXTRATROPICAL TROPOPAUSE;
POTENTIAL VORTICITY; CARBON-MONOXIDE; MONITORING INSTRUMENT;
NORTH-AMERICA; TRACE GASES
AB Stratosphere-to-troposphere transport (STT) and biomass burning (BB) are two important natural sources for tropospheric ozone that can result in elevated ozone and air-quality episode events. High-resolution observations of multiple related species are critical for complex ozone source attribution. In this article, we present an analysis of coinciding ground-based and airborne observations, including ozone lidar, ozonesonde, high spectral resolution lidar (HSRL), and multiple airborne in situ measurements, made on 28 and 29 June 2013 during the Southeast Nexus field campaign. The ozone lidar and HSRL reveal detailed ozone and aerosol structures as well as the temporal evolution associated with a cold front passage. The observations also captured two enhanced (+30 ppbv) ozone layers in the free troposphere (FT), which were determined from this study to be caused by a mixture of BB and stratospheric sources. The mechanism for this STT is tropopause folding associated with a cutoff upper level low-pressure system according to the analysis of its potential vorticity structure. The depth of the tropopause fold appears to be shallow for this case compared to events observed in other seasons; however, the impact on lower tropospheric ozone was clearly observed. This event suggests that strong STT may occur in the southeast United States during the summer and can potentially impact lower troposphere during these times. Statistical analysis of the airborne observations of trace gases suggests a coincident influence of BB transport in the FT impacting the vertical structure of ozone during this case study.
C1 [Kuang, Shi; Wang, Lihua; Pour-Biazar, Arastoo] Univ Alabama, Earth Syst Sci Ctr, Huntsville, AL 35899 USA.
[Newchurch, Michael J.; Huang, Guanyu; Feng, Nan] Univ Alabama, Atmospher Sci Dept, Huntsville, AL 35899 USA.
[Johnson, Matthew S.] NASA, Ames Res Ctr, Earth Sci Div, Moffett Field, CA 94035 USA.
[Burris, John] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Pierce, Robert B.] NOAA NESDIS Ctr Satellite Applicat & Res, Madison, WI USA.
[Eloranta, Edwin W.] Univ Wisconsin, Space Sci & Engn Ctr, Madison, WI 53705 USA.
[Pollack, Ilana B.; Graus, Martin; de Gouw, Joost; Warneke, Carsten; Ryerson, Thomas B.; Markovic, Milos Z.; Holloway, John S.] NOAA Earth Syst Res Iaboratory, Chem Sci Div, Boulder, CO USA.
[Pollack, Ilana B.; Graus, Martin; de Gouw, Joost; Warneke, Carsten; Holloway, John S.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Pollack, Ilana B.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Graus, Martin] Univ Innsbruck, Inst Atmospher & Cryospher Sci, A-6020 Innsbruck, Austria.
[Markovic, Milos Z.] Environm & Climate Change Canada, Air Qual Res Div, Toronto, ON, Canada.
[Huang, Guanyu; Liu, Xiong] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA USA.
RP Kuang, S (reprint author), Univ Alabama, Earth Syst Sci Ctr, Huntsville, AL 35899 USA.
EM kuang@nsstc.uah.edu
RI de Gouw, Joost/A-9675-2008;
OI de Gouw, Joost/0000-0002-0385-1826; Kuang, Shi/0000-0003-2423-6088
FU TOLNet program
FX The authors thank Whitney G. Jewett for editing the manuscript. The
authors are grateful to Joshua P. Schwarz of NOAA/ESRL for providing the
BC data. The authors thank the SENEX science team, instrument team, and
pilot crew for managing and coordinating the intercomparison
measurements. The authors also thank the MODIS team for providing the
AOD, radiance, and fire data (AOD MOD04 10 km, Radiance MOD021KM 1 km,
and Fires MOD14 1 km) and thank the NOAA Air Resources Laboratory (ARL)
for the provision of the HYSPLIT model and READY website
(http://www.ready.noaa.gov) used in this publication. The authors thank
three anonymous reviewers for providing constructive comments. The ozone
lidar data are available at
http://www-air.larc.nasa.gov/missions/TOLNet/. This work is supported by
the TOLNet program developed by National Aeronautics and Space
Administration (NASA)'s Science Mission Directorate. The views,
opinions, and findings contained in this report are those of the authors
and should not be construed as an official NOAA, NASA, or the U.S.
Government position, policy, or decision.
NR 113
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U1 2
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 27
PY 2017
VL 122
IS 2
BP 1293
EP 1311
DI 10.1002/2016JD026078
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EN6MA
UT WOS:000396116900042
ER
PT J
AU Terrer, C
Vicca, S
Hungate, BA
Phillips, RP
Reich, PB
Franklin, O
Stocker, BD
Fisher, JB
Prentice, IC
AF Terrer, Cesar
Vicca, Sara
Hungate, Bruce A.
Phillips, Richard P.
Reich, Peter B.
Franklin, Oskar
Stocker, Benjamin D.
Fisher, Joshua B.
Prentice, I. Colin
TI Response to Comment on "Mycorrhizal association as a primary control of
the CO2 fertilization effect"
SO SCIENCE
LA English
DT Editorial Material
ID ELEVATED CO2; TERRESTRIAL BIOSPHERE; CARBON; PRODUCTIVITY; AVAILABILITY;
TEMPERATURE; IMPACT; FUNGI
AB Norby et al. center their critique on the design of the data set and the response variable used. We address these criticisms and reinforce the conclusion that plants that associate with ectomycorrhizal fungi exhibit larger biomass and growth responses to elevated CO2 compared with plants that associate with arbuscular mycorrhizae.
C1 [Terrer, Cesar; Stocker, Benjamin D.; Prentice, I. Colin] Imperial Coll London, Dept Life Sci, AXA Chair Programme Biosphere & Climate Impacts, Silwood Pk Campus,Buckhurst Rd, Ascot SL5 7PY, Berks, England.
[Vicca, Sara] Univ Antwerp, Dept Biol, Ctr Excellence PLECO Plant & Vegetat Ecol, B-2610 Antwerp, Belgium.
[Hungate, Bruce A.] No Arizona Univ, Ctr Ecosyst Sci & Soc, Flagstaff, AZ 86011 USA.
[Hungate, Bruce A.] No Arizona Univ, Dept Biol Sci, Flagstaff, AZ 86011 USA.
[Phillips, Richard P.] Indiana Univ, Dept Biol, Bloomington, IN 47405 USA.
[Reich, Peter B.] Univ Minnesota, Dept Forest Resources, St Paul, MN 55108 USA.
[Reich, Peter B.] Univ Western Sydney, Hawkesbury Inst Environm, Penrith, NSW 2751, Australia.
[Franklin, Oskar] Int Inst Appl Syst Anal, Ecosyst Serv & Management Program, Laxenburg, Austria.
[Franklin, Oskar] Swedish Univ Agr Sci, Dept Forest Ecol & Management, S-90183 Umea, Sweden.
[Fisher, Joshua B.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Fisher, Joshua B.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
RP Terrer, C (reprint author), Imperial Coll London, Dept Life Sci, AXA Chair Programme Biosphere & Climate Impacts, Silwood Pk Campus,Buckhurst Rd, Ascot SL5 7PY, Berks, England.
EM c.terrer@imperial.ac.uk
FU Imperial College Ph.D. studentship; International Institute for Applied
System Analysis (IIASA); Climate Change Manipulation Experiments in
Terrestrial Ecosystems (ClimMani) European Cooperation in Science and
Technology (COST) Action [ES1308]; NSF (Ecosystem Studies Program)
[1153401]; DOE (Environmental System Science Program); Royal Netherlands
Academy of Arts and Sciences; DOE; INTERFACE; New Phytologist trust;
European Research Council [ERC-SyG-610028 IMBALANCE-P]; Swiss National
Science Foundation
FX We thank D. Blumenthal, M. Hovenden, A. Talhelm, A. Finzi, P. Newton, N.
Chiariello, C. Kammann, C. Muller, C. Field, and M. Schneider, who
provided data and advice. This research is a contribution to the
Imperial College initiative Grand Challenges in Ecosystems and the
Environment and the AXA Chair Programme in Biosphere and Climate
Impacts. C.T. was supported by an Imperial College Ph.D. studentship
within this program and the International Institute for Applied System
Analysis (IIASA). S.V. is a postdoctoral fellow of the Research
Foundation-Flanders (FWO). C.T. and S.V. acknowledge support from
Climate Change Manipulation Experiments in Terrestrial Ecosystems
(ClimMani) European Cooperation in Science and Technology (COST) Action
(ES1308). R.P.P. acknowledges support from NSF (Ecosystem Studies
Program 1153401) and DOE (Environmental System Science Program). R.P.P.
and C.T. thank the Royal Netherlands Academy of Arts and Sciences, DOE,
INTERFACE, and the New Phytologist trust for funding the workshop
"Climate models revisited: The biogeochemical consequences of
mycorrhizal dynamics." S.V. and O.F. acknowledge support from the
European Research Council grant ERC-SyG-610028 IMBALANCE-P. Part of
J.B.F.'s contribution was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. B.D.S. is funded by the Swiss
National Science Foundation. All authors contributed to the development
of the conceptual framework and to the writing of this Response.
NR 17
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U1 2
U2 2
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD JAN 27
PY 2017
VL 355
IS 6323
DI 10.1126/science.aai8242
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EJ4FR
UT WOS:000393172800029
ER
PT J
AU Miyazaki, K
Eskes, H
Sudo, K
Boersma, KF
Bowman, K
Kanaya, Y
AF Miyazaki, Kazuyuki
Eskes, Henk
Sudo, Kengo
Boersma, K. Folkert
Bowman, Kevin
Kanaya, Yugo
TI Decadal changes in global surface NOx emissions from multi-constituent
satellite data assimilation
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID OZONE MONITORING INSTRUMENT; VERTICAL COLUMN DENSITIES; TROPOSPHERIC
NO2; NITROGEN-OXIDES; UNITED-STATES; EAST-ASIA; SEASONAL-VARIATIONS;
ERROR ANALYSIS; LIGHTNING NOX; AIR-QUALITY
AB Global surface emissions of nitrogen oxides (NOx) over a 10-year period (20052014) are estimated from an assimilation of multiple satellite data sets: tropospheric NO2 columns from Ozone Monitoring Instrument (OMI), Global Ozone Monitoring Experiment-2 (GOME-2), and Scanning Imaging Absorption Spectrometer for Atmospheric Chartography (SCIAMACHY), O-3 profiles from Tropospheric Emission Spectrometer (TES), CO profiles from Measurement of Pollution in the Troposphere (MOPITT), and O-3 and HNO3 profiles from Microwave Limb Sounder (MLS) using an ensemble Kalman filter technique. Chemical concentrations of various species and emission sources of several precursors are simultaneously optimized. This is expected to improve the emission inversion because the emission estimates are influenced by biases in the modelled tropospheric chemistry, which can be partly corrected by also optimizing the concentrations. We present detailed distributions of the estimated emission distributions for all major regions, the diurnal and seasonal variability, and the evolution of these emissions over the 10-year period. The estimated regional total emissions show a strong positive trend over India (+29 % decade(-1)), China (+26 % decade(-1)), and the Middle East (+20 % decade(-1)), and a negative trend over the USA (-38 % decade(-1)), southern Africa (-8.2 % decade(-1)), and western Europe (-8.8 % decade(-1)). The negative trends in the USA and western Europe are larger during 2005-2010 relative to 2011-2014, whereas the trend in China becomes negative after 2011. The data assimilation also suggests a large uncertainty in anthropogenic and fire-related emission factors and an important underestimation of soil NOx sources in the emission inventories. Despite the large trends observed for individual regions, the global total emission is almost constant between 2005 (47.9 Tg N yr(-1)) and 2014 (47.5 Tg N yr(-1)).
C1 [Miyazaki, Kazuyuki; Kanaya, Yugo] Japan Agcy Marine Earth Sci & Technol, Yokohama, Kanagawa 2360001, Japan.
[Eskes, Henk; Boersma, K. Folkert] Royal Netherlands Meteorol Inst KNMI, Wilhelminalaan 10, NL-3732 GK De Bilt, Netherlands.
[Sudo, Kengo] Nagoya Univ, Grad Sch Environm Studies, Nagoya, Aichi, Japan.
[Boersma, K. Folkert] Wageningen Univ, Meteorol & Air Qual Dept, Wageningen, Netherlands.
[Miyazaki, Kazuyuki; Bowman, Kevin] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Miyazaki, K (reprint author), Japan Agcy Marine Earth Sci & Technol, Yokohama, Kanagawa 2360001, Japan.; Miyazaki, K (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM kmiyazaki@jamstec.go.jp
RI Boersma, Klaas/H-4559-2012
OI Boersma, Klaas/0000-0002-4591-7635
FU JSPS KAKENHI [15K05296, 26220101]; MEXT, JAPAN
FX We acknowledge the free use of tropospheric NO2 column data
from the SCIAMACHY, GOME-2, and OMI sensors from http://www.temis.nl. We
also acknowledge the use of data products from the NASA AURA and EOS
Terra satellite missions. We would also like to thank the editor and two
anonymous reviewers for their valuable comments. This work was supported
through JSPS KAKENHI grant numbers 15K05296 and 26220101 and
Coordination Funds for Promoting AeroSpace Utilization by MEXT, JAPAN.
NR 106
TC 0
Z9 0
U1 9
U2 9
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PD JAN 27
PY 2017
VL 17
IS 2
BP 807
EP 837
DI 10.5194/acp-17-807-2017
PG 31
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EL4MD
UT WOS:000394594400001
ER
PT J
AU Jung, M
Reichstein, M
Schwalm, CR
Huntingford, C
Sitch, S
Ahlstrom, A
Arneth, A
Camps-Valls, G
Ciais, P
Friedlingstein, P
Gans, F
Ichii, K
Ain, AKJ
Kato, E
Papale, D
Poulter, B
Raduly, B
Rodenbeck, C
Tramontana, G
Viovy, N
Wang, YP
Weber, U
Zaehle, S
Zeng, N
AF Jung, Martin
Reichstein, Markus
Schwalm, Christopher R.
Huntingford, Chris
Sitch, Stephen
Ahlstrom, Anders
Arneth, Almut
Camps-Valls, Gustau
Ciais, Philippe
Friedlingstein, Pierre
Gans, Fabian
Ichii, Kazuhito
Ain, Atul K. J.
Kato, Etsushi
Papale, Dario
Poulter, Ben
Raduly, Botond
Rodenbeck, Christian
Tramontana, Gianluca
Viovy, Nicolas
Wang, Ying-Ping
Weber, Ulrich
Zaehle, Sonke
Zeng, Ning
TI Compensatory water effects link yearly global land CO2 sink changes to
temperature
SO NATURE
LA English
DT Article
ID NET ECOSYSTEM EXCHANGE; CARBON-DIOXIDE; TERRESTRIAL ECOSYSTEMS;
INTERANNUAL VARIABILITY; TROPICAL TEMPERATURE; SEMIARID ECOSYSTEMS;
CLIMATE; CYCLE; FLUXES; SPACE
AB Large interannual variations in the measured growth rate of atmospheric carbon dioxide (CO2) originate primarily from fluctuations in carbon uptake by land ecosystems(1-3). It remains uncertain, however, to what extent temperature and water availability control the carbon balance of land ecosystems across spatial and temporal scales(3-14). Here we use empirical models based on eddy covariance data(15) and process-based models(16,17) to investigate the effect of changes in temperature and water availability on gross primary productivity (GPP), terrestrial ecosystem respiration (TER) and net ecosystem exchange (NEE) at local and global scales. We find that water availability is the dominant driver of the local interannual variability in GPP and TER. To a lesser extent this is true also for NEE at the local scale, but when integrated globally, temporal NEE variability is mostly driven by temperature fluctuations. We suggest that this apparent paradox can be explained by two compensatory water effects. Temporal water-driven GPP and TER variations compensate locally, dampening water-driven NEE variability. Spatial water availability anomalies also compensate, leaving a dominant temperature signal in the year-to-year fluctuations of the land carbon sink. These findings help to reconcile seemingly contradictory reports regarding the importance of temperature and water in controlling the interannual variability of the terrestrial carbon balance(3-6,9,11,12,14). Our study indicates that spatial climate covariation drives the global carbon cycle response.
C1 [Jung, Martin; Reichstein, Markus; Gans, Fabian; Weber, Ulrich; Zaehle, Sonke] Max Planck Inst Biogeochem, Dept Biogeochem Integrat, D-07745 Jena, Germany.
[Reichstein, Markus; Zaehle, Sonke] Friedrich Schiller Univ Jena, Michael Stifel Ctr Jena Data Driven & Simulat Sci, D-07743 Jena, Germany.
[Schwalm, Christopher R.] Woods Hole Res Ctr, Falmouth, MA 02540 USA.
[Huntingford, Chris] Ctr Ecol & Hydrol, Wallingford OX10 8BB, Oxon, England.
[Sitch, Stephen] Univ Exeter, Coll Life & Environm Sci, Exeter EX4 4QF, Devon, England.
[Ahlstrom, Anders] Stanford Univ, Sch Earth Energy & Environm Sci, Dept Earth Syst Sci, Stanford, CA 94305 USA.
[Ahlstrom, Anders] Lund Univ, Dept Phys Geog & Ecosyst Sci, S-22362 Lund, Sweden.
[Arneth, Almut] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, D-82467 Garmisch Partenkirchen, Germany.
[Camps-Valls, Gustau] Univ Valencia, Image Proc Lab, Catedrat Jose Beltran, Valencia 46980, Spain.
[Ciais, Philippe; Viovy, Nicolas] UVSQ, CNRS, CEA, Lab Sci Climat & Environm, F-91191 Gif Sur Yvette, France.
[Friedlingstein, Pierre] Univ Exeter, Coll Engn Math & Phys Sci, Exeter EX4 4QE, Devon, England.
[Ichii, Kazuhito] Japan Agcy Marine Earth Sci & Technol, Dept Environm Geochem Cycle Res, Kanazawa Ku, Yokohama, Kanagawa 2360001, Japan.
[Ichii, Kazuhito] Natl Inst Environm Studies, Ctr Global Environm Res, Tsukuba, Ibaraki 3058506, Japan.
[Ain, Atul K. J.] Univ Illinois, Dept Atmospher Sci, Urbana, IL 61801 USA.
[Kato, Etsushi] Inst Appl Energy, Global Environm Program, Tokyo 1050003, Japan.
[Papale, Dario; Raduly, Botond; Tramontana, Gianluca] Univ Tuscia, Dept Innovat Biol Agrofood & Forest Syst, I-01100 Viterbo, Italy.
[Poulter, Ben] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Raduly, Botond] Sapientia Hungarian Univ Transylvania, Dept Bioengn, M Ciuc 530104, Romania.
[Rodenbeck, Christian] Max Planck Inst Biogeochem, Dept Biogeochem Syst, D-07745 Jena, Germany.
[Wang, Ying-Ping] CSIRO Oceans & Atmosphere, Aspendale, Vic 3195, Australia.
[Zeng, Ning] Chinese Acad Sci, Inst Atmospher Phys, Beijing 100029, Peoples R China.
[Zeng, Ning] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
RP Jung, M (reprint author), Max Planck Inst Biogeochem, Dept Biogeochem Integrat, D-07745 Jena, Germany.
EM mjung@bgc-jena.mpg.de
RI Zeng, Ning/A-3130-2008; Jain, Atul/D-2851-2016; Ahlstrom,
Anders/F-3215-2017; Huntingford, Chris/A-4307-2008
OI Zeng, Ning/0000-0002-7489-7629; Jain, Atul/0000-0002-4051-3228;
Ahlstrom, Anders/0000-0003-1642-0037;
FU European Union (EU) [283080]; EU [640176, 603542]; European Space
Agency; European Research Council (ERC) under the EU [647204]; National
Aeronautics and Space Administration (NASA) [NNX12AK12G, NNX12AP74G,
NNX10AG01A, NNX11AO08A]; ERC [ERC-2013-SyG-610028 IMBALANCE-P]; Ministry
of the Environment of Japan [2-1401]; Natural Environment Research
Council (NERC) [NE/J010057/1]; NERC CEH National Capability fund; Royal
Physiographic Society in Lund (Birgit and Hellmuth Hertz' Foundation);
Swedish Research Council [637-2014-6895]; EU under ERC [SEDAL-647423]
FX We thank P. Peylin for providing RECCAP inversion results. We also thank
P. Bodesheim for help with the mathematical notations, J. Nelson for
proofreading the Supplementary Information, S. Schott for help with
artwork, and G. Boenisch, L. Maack and P. Koch for help archiving the
FLUXCOM data. M.J., M.R. and D.P. acknowledge funding from the European
Union (EU) FP7 project GEOCARBON (grant number 283080) and the EU H2020
BACI project (grant number 640176). F.G. and M.R. acknowledge the
European Space Agency for funding the 'Coupled Biosphere-Atmosphere
virtual LABoratory' (CAB-LAB). S.Z. acknowledges support from the
European Research Council (ERC) under the EU's Horizon 2020 research and
innovation programme (QUINCY; grant number 647204). A. Arneth
acknowledges support from the EU FP7 project LUC4C (grant number
603542). C.R.S. was supported by National Aeronautics and Space
Administration (NASA) grants NNX12AK12G, NNX12AP74G, NNX10AG01A and
NNX11AO08A. P.C. acknowledges support from the ERC Synergy grant
ERC-2013-SyG-610028 IMBALANCE-P. K.I. acknowledges support from the
Environment Research and Technology Development Funds (2-1401) from the
Ministry of the Environment of Japan. S.S. acknowledges the support of
the Natural Environment Research Council (NERC) South AMerican Biomass
Burning Analysis (SAMBBA) project (grant code NE/J010057/1). C.H. is
grateful for support from the NERC CEH National Capability fund. A.
Ahlstrom acknowledges support from The Royal Physiographic Society in
Lund (Birgit and Hellmuth Hertz' Foundation) and the Swedish Research
Council (637-2014-6895). G.C.-V. was supported by the EU under ERC
consolidator grant SEDAL-647423.
NR 44
TC 0
Z9 0
U1 13
U2 13
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD JAN 26
PY 2017
VL 541
IS 7638
DI 10.1038/nature20780
PG 11
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EN6LX
UT WOS:000396116600047
PM 28092919
ER
PT J
AU Webb, MJ
Andrews, T
Bodas-Salcedo, A
Bony, S
Bretherton, CS
Chadwick, R
Chepfer, H
Douville, H
Good, P
Kay, JE
Klein, SA
Marchand, R
Medeiros, B
Siebesma, AP
Skinner, CB
Stevens, B
Tselioudis, G
Tsushima, Y
Watanabe, M
AF Webb, Mark J.
Andrews, Timothy
Bodas-Salcedo, Alejandro
Bony, Sandrine
Bretherton, Christopher S.
Chadwick, Robin
Chepfer, Helene
Douville, Herve
Good, Peter
Kay, Jennifer E.
Klein, Stephen A.
Marchand, Roger
Medeiros, Brian
Siebesma, A. Pier
Skinner, Christopher B.
Stevens, Bjorn
Tselioudis, George
Tsushima, Yoko
Watanabe, Masahiro
TI The Cloud Feedback Model Intercomparison Project (CFMIP) contribution to
CMIP6
SO GEOSCIENTIFIC MODEL DEVELOPMENT
LA English
DT Article
ID GENERAL-CIRCULATION MODEL; SURFACE-TEMPERATURE-CHANGE; COMMUNITY
ATMOSPHERE MODEL; MADDEN-JULIAN OSCILLATION; CLIMATE SENSITIVITY;
SOUTHERN-OCEAN; TROPICAL RAINFALL; SATELLITE-OBSERVATIONS; COUPLED
MODEL; TROPOSPHERIC ADJUSTMENT
AB The primary objective of CFMIP is to inform future assessments of cloud feedbacks through improved understanding of cloud-climate feedback mechanisms and better evaluation of cloud processes and cloud feedbacks in climate models. However, the CFMIP approach is also increasingly being used to understand other aspects of climate change, and so a second objective has now been introduced, to improve understanding of circulation, regional-scale precipitation, and non-linear changes. CFMIP is supporting ongoing model inter-comparison activities by coordinating a hierarchy of targeted experiments for CMIP6, along with a set of cloud-related output diagnostics. CFMIP contributes primarily to addressing the CMIP6 questions "How does the Earth system respond to forcing?" and "What are the origins and consequences of systematic model biases?" and supports the activities of the WCRP Grand Challenge on Clouds, Circulation and Climate Sensitivity.
A compact set of Tier 1 experiments is proposed for CMIP6 to address this question: (1) what are the physical mechanisms underlying the range of cloud feedbacks and cloud adjustments predicted by climate models, and which models have the most credible cloud feedbacks? Additional Tier 2 experiments are proposed to address the following questions. (2) Are cloud feedbacks consistent for climate cooling and warming, and if not, why? (3) How do cloudradiative effects impact the structure, the strength and the variability of the general atmospheric circulation in present and future climates? (4) How do responses in the climate system due to changes in solar forcing differ from changes due to CO2, and is the response sensitive to the sign of the forcing? (5) To what extent is regional climate change per CO2 doubling state-dependent (non-linear), and why? (6) Are climate feedbacks during the 20th century different to those acting on long-term climate change and climate sensitivity? (7) How do regional climate responses (e.g. in precipitation) and their uncertainties in coupled models arise from the combination of different aspects of CO2 forcing and sea surface warming?
CFMIP also proposes a number of additional model outputs in the CMIP DECK, CMIP6 Historical and CMIP6 CFMIP experiments, including COSP simulator outputs and process diagnostics to address the following questions.
1. How well do clouds and other relevant variables simulated by models agree with observations?
2. What physical processes and mechanisms are important for a credible simulation of clouds, cloud feedbacks and cloud adjustments in climate models?
3. Which models have the most credible representations of processes relevant to the simulation of clouds?
4. How do clouds and their changes interact with other elements of the climate system?
C1 [Webb, Mark J.; Andrews, Timothy; Bodas-Salcedo, Alejandro; Chadwick, Robin; Good, Peter; Tsushima, Yoko] Met Off Hadley Ctr, Exeter, Devon, England.
[Bony, Sandrine; Chepfer, Helene] Univ Paris 06, CNRS, LMD IPSL, Paris, France.
[Bretherton, Christopher S.; Marchand, Roger] Univ Washington, Seattle, WA 98195 USA.
[Douville, Herve] Ctr Natl Rech Meteorol, Toulouse, France.
[Kay, Jennifer E.] Univ Colorado, Boulder, CO 80309 USA.
[Klein, Stephen A.] Lawrence Livermore Natl Lab, Livermore, CA USA.
[Medeiros, Brian] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
[Siebesma, A. Pier] Royal Netherlands Meteorol Inst, De Bilt, Netherlands.
[Skinner, Christopher B.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Stevens, Bjorn] Max Planck Inst Meteorol, Hamburg, Germany.
[Tselioudis, George] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Watanabe, Masahiro] Atmosphere & Ocean Res Inst, Tokyo, Japan.
RP Webb, MJ (reprint author), Met Off Hadley Ctr, Exeter, Devon, England.
EM mark.webb@metoffice.gov.uk
FU Regional and Global Climate Modeling program of the United States
Department of Energy's Office of Science; U.S. Department of Energy by
Lawrence Livermore National Laboratory [DEAC5207NA27344]; UK BEIS
DECC/Defra Met Office Hadley Centre Climate Programme [GA01101]
FX We are grateful to Florent Brient, Hideo Shiogama, Aiko Voigt, Mark
Ringer and two anonymous referees for helpful comments on the
manuscript. We thank the modelling groups and the wider CFMIP community
for reviewing and supporting the CFMIP contribution to CMIP6, the CMIP
Panel for their coordination of CMIP6, the WGCM Infrastructure Panel
(WIP) overseeing the CMIP6 infrastructure, and Martin Juckes for taking
the lead in preparing the CMIP6 data request. We are also grateful to
Robert Pincus and Yuying Zhang for their contributions to COSP and to
CFMIP-OBS, to Dustin Swales for his development work for COSP-2, and to
Gregory Cesana and Mathieu Reverdy for their contributions to CFMIP-OBS.
We are grateful to Brian Soden for producing the CMIP3 composite pattern
dataset used for the CMIP5 amipFuture and CMIP6 amip-future4K
experiments, and to PMIP representatives Pascale Braconnot, Masa
Kageyama, and Masakazu Yoshimori for discussions relating to the
amip-m4K experiment. The efforts of S. A. Klein are supported by the
Regional and Global Climate Modeling program of the United States
Department of Energy's Office of Science and were performed under the
auspices of the U.S. Department of Energy by Lawrence Livermore National
Laboratory under contract DEAC5207NA27344. Met Office Hadley Centre
authors are supported by the Joint UK BEIS DECC/Defra Met Office Hadley
Centre Climate Programme (GA01101).
NR 177
TC 0
Z9 0
U1 1
U2 1
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1991-959X
EI 1991-9603
J9 GEOSCI MODEL DEV
JI Geosci. Model Dev.
PD JAN 25
PY 2017
VL 10
IS 1
BP 359
EP 384
DI 10.5194/gmd-10-359-2017
PG 26
WC Geosciences, Multidisciplinary
SC Geology
GA EM3AS
UT WOS:000395187500001
ER
PT J
AU Brattich, E
Liu, HY
Tositti, L
Considine, DB
Crawford, JH
AF Brattich, Erika
Liu, Hongyu
Tositti, Laura
Considine, David B.
Crawford, James H.
TI Processes controlling the seasonal variations in Pb-210 and Be-7 at the
Mt. Cimone WMO-GAW global station, Italy: a model analysis
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID GROUND LEVEL AIR; STRATOSPHERE-TROPOSPHERE EXCHANGE; INITIATIVE
ASSESSMENT MODEL; CROSS-TROPOPAUSE TRANSPORT; CHEMICAL TRACER MODEL;
SURFACE AIR; TEMPORAL VARIATIONS; IBERIAN PENINSULA; METEOROLOGICAL
PARAMETERS; 3-DIMENSIONAL SIMULATION
AB We apply the Global Modeling Initiative (GMI) chemistry and transport model driven by NASA's MERRA assimilated meteorological data to simulate the seasonal variations in two radionuclide aerosol tracers (terrigenous Pb-210 and cosmogenic Be-7) at the WMO-GAW station of Mt. Cimone (44 degrees 12'N, 10 degrees 42'E; 2165 m a.s.l.; Italy), which is representative of free-tropospheric conditions most of the year, during 2005 with an aim to understand the roles of transport and precipitation scavenging processes in controlling their seasonality. The total precipitation field in the MERRA data set is evaluated with the Global Precipitation Climatology Project (GPCP) observations, and generally good agreement is found. The model reproduces reasonably the observed seasonal pattern of Pb-210 concentrations, characterized by a wintertime minimum due to lower Rn-222 emissions and weaker uplift from the boundary layer and summertime maxima resulting from strong convection over the continent. The observed seasonal behavior of Be-7 concentrations shows a winter minimum, a summer maximum, and a secondary spring maximum. The model captures the observed Be-7 pattern in winter-spring, which is linked to the larger stratospheric influence during spring. However, the model tends to underestimate the observed Be-7 concentrations in summer, partially due to the sensitivity to spatial sampling in the model. Model sensitivity experiments indicate a dominant role of precipitation scavenging (vs. dry deposition and convection) in controlling the seasonality of Pb-210 and Be-7 concentrations at Mt. Cimone.
C1 [Brattich, Erika; Tositti, Laura] Alma Mater Studiorum Univ Bologna, Dept Chem G Ciamician, I-40126 Bologna, BO, Italy.
[Liu, Hongyu] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Considine, David B.] NASA Headquarters, Washington, DC 20546 USA.
[Crawford, James H.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Liu, HY (reprint author), Natl Inst Aerosp, Hampton, VA 23666 USA.
EM hongyu.liu-1@nasa.gov
FU MIUR; DTA-CNR throughout Project of National Interest "NextData";
Department of Biological, Geological and Earth Sciences of the
University of Bologna; NASA Modeling and Analysis Program (MAP); NASA
Atmospheric Composition Modeling and Analysis Program (ACMAP); NASA
Atmospheric Composition Campaign Data Analysis and Modeling (ACCDAM)
program
FX Italian Air Force Meteorological Office (IAFMS) and ISAC-CNR are
gratefully acknowledged for their precious technical support at the Mt.
Cimone station. In particular, ISAC-CNR is gratefully acknowledged for
providing infrastructural access at the WMO-GAW Global Station Italian
Climate Observatory "O. Vittori" at Mt. Cimone. IAFMS is gratefully
acknowledged for providing meteorological observations at Mt. Cimone
station. The Italian Climate Observatory "O. Vittori" is supported by
MIUR and DTA-CNR throughout the Project of National Interest "NextData".
Erika Brattich thanks the National Institute of Aerospace (NIA) Visitor
Program for hosting her one-month visit, and the Department of
Biological, Geological and Earth Sciences of the University of Bologna
for grant support during her PhD study. Hongyu Liu is supported by NASA
Modeling and Analysis Program (MAP), NASA Atmospheric Composition
Modeling and Analysis Program (ACMAP), and NASA Atmospheric Composition
Campaign Data Analysis and Modeling (ACCDAM) program. The GMI activity
is managed by Jose Rodriguez and Susan Strahan (NASA GSFC). Stephen
Steenrod, Megan Damon, and Jules Kouatchou (GSFC) are acknowledged for
programming support. NASA Center for Computational Sciences (NCCS)
provided supercomputing resources. We thank the two anonymous reviewers
for their comments, which improved the quality of our work.
NR 114
TC 0
Z9 0
U1 0
U2 0
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PD JAN 24
PY 2017
VL 17
IS 2
BP 1061
EP 1080
DI 10.5194/acp-17-1061-2017
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EL4NJ
UT WOS:000394597600001
ER
PT J
AU Kutepov, AA
Rezac, L
Feofilov, AG
AF Kutepov, Alexander A.
Rezac, Ladislav
Feofilov, Artem G.
TI Evidence of a significant rotational non-LTE effect in the CO2 4.3 mu m
PFS-MEX limb spectra
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID ACCELERATED LAMBDA ITERATION; RADIATION-DRIVEN WINDS; MARS EXPRESS
MISSION; HOT LUMINOUS STARS; PLANETARY-ATMOSPHERES; MARTIAN ATMOSPHERE;
RETRIEVAL APPROACH; DAYTIME; MESOSPHERE; EMISSION
AB Since January 2004, the planetary Fourier spectrometer (PFS) on board the Mars Express satellite has been recording near-infrared limb spectra of high quality up to the tangent altitudes approximate to 150 km, with potential information on density and thermal structure of the upper Martian atmosphere. We present first results of our modeling of the PFS short wavelength channel (SWC) daytime limb spectra for the altitude region above 90 km. We applied a ro-vibrational non-LTE model based on the stellar astrophysics technique of accelerated lambda iteration (ALI) to solve the multispecies and multi-level CO2 problem in the Martian atmosphere. We show that the long-standing discrepancy between observed and calculated spectra in the cores and wings of 4.3 mu m region is explained by the non-thermal rotational distribution of molecules in the upper vibrational states 10011 and 10012 of the CO2 main isotope second hot (SH) bands above 90 km altitude. The redistribution of SH band intensities from band branch cores into their wings is caused (a) by intensive production of the CO2 molecules in rotational states with j > 30 due to the absorption of solar radiation in optically thin wings of 2.7 mu m bands and (b) by a short radiative lifetime of excited molecules, which is insufficient at altitudes above 90 km for collisions to maintain rotation of excited molecules thermalized. Implications for developing operational algorithms for massive processing of PFS and other instrument limb observations are discussed.
C1 [Kutepov, Alexander A.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA.
[Kutepov, Alexander A.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Rezac, Ladislav] Max Planck Inst Sonnensyst Forsch, Dept Planets & Comets, Justus von Liebig Weg 3, D-37077 Gottingen, Germany.
[Feofilov, Artem G.] Ecole Polytech, Lab Meteorol Dynam, IPSL CNRS, UMR8539, Paris, France.
RP Kutepov, AA (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA.; Kutepov, AA (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
EM kutepov@cua.edu
FU NASA [NNX08AL12G]; NSF [AGS-1301762]; DFG [HA3261/7-1]; project "Towards
a better interpretation of atmospheric phenomena" of the French National
Program LEFE/INSU
FX The authors cordially thank Marco Giuranna, the PI of PFS/MEX for
providing us samples of PFS limb spectra with the emission features
unexplained by the nominal non-LTE models, and for a very helpful
discussion on the data quality and the general performance of the
instrument. The work of AAK was supported by the NASA grant NNX08AL12G
and the NSF grant AGS-1301762. The work of LR was partly supported by
the DFG grant HA3261/7-1. The work of AGF was supported during his
employment in the USA by the NASA grant NNX08AL12G and in France by the
project "Towards a better interpretation of atmospheric phenomena" of
the French National Program LEFE/INSU.
NR 38
TC 0
Z9 0
U1 1
U2 1
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1867-1381
EI 1867-8548
J9 ATMOS MEAS TECH
JI Atmos. Meas. Tech.
PD JAN 24
PY 2017
VL 10
IS 1
BP 265
EP 271
DI 10.5194/amt-10-265-2017
PG 7
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EL7BI
UT WOS:000394775700001
ER
PT J
AU Anisimov, A
Tao, WC
Stenchikov, G
Kalenderski, S
Prakash, PJ
Yang, ZL
Shi, MJ
AF Anisimov, Anatolii
Tao, Weichun
Stenchikov, Georgiy
Kalenderski, Stoitchko
Prakash, P. Jish
Yang, Zong-Liang
Shi, Mingjie
TI Quantifying local-scale dust emission from the Arabian Red Sea coastal
plain
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID AEROSOL OPTICAL DEPTH; MINERAL DUST; ATMOSPHERIC DUST; MIDDLE-EAST;
NORTHERN AFRICA; SURFACE OBSERVATIONS; GLOBAL DISTRIBUTION; RETRIEVAL
PRODUCTS; MACC REANALYSIS; CLIMATE SYSTEM
AB Dust plumes emitted from the narrow Arabian Red Sea coastal plain are often observed on satellite images and felt in local population centers. Despite its relatively small area, the coastal plain could be a significant dust source; however, its effect is not well quantified as it is not well approximated in global or even regional models. In addition, because of close proximity to the Red Sea, a significant amount of dust from the coastal areas could be deposited into the Red Sea and serve as a vital component of the nutrient balance of marine ecosystems.
In the current study, we apply the offline Community Land Model version 4 (CLM4) to better quantify dust emission from the coastal plain during the period of 2009-2011. We verify the spatial and temporal variability in model results using independent weather station reports. We also compare the results with the MERRA Aerosol Reanalysis (MERRAero). We show that the best results are obtained with 1 km model spatial resolution and dust source function based on Meteosat Second Generation Spinning Enhanced Visible and InfraRed Imager (SEVIRI) measurements. We present the dust emission spatial pattern, as well as estimates of seasonal and diurnal variability in dust event frequency and intensity, and discuss the emission regime in the major dust generation hot spot areas. We demonstrate the contrasting seasonal dust cycles in the northern and southern parts of the coastal plain and discuss the physical mechanisms responsible for dust generation.
This study provides the first estimates of the fine-scale spatial and temporal distribution of dust emissions from the Arabian Red Sea coastal plain constrained by MERRAero and short-term WRF-Chem simulations. The estimate of total dust emission from the coastal plain, tuned to fit emissions in MERRAero, is 7.5 +/- 0.5 Mt a(-1). Small interannual variability indicates that the study area is a stable dust source. The mineralogical composition analysis shows that the coastal plain generates around 76 +/- 5 kt of iron oxides and 6 +/- 0.4 kt of phosphorus annually. Over 65% of dust is emitted from the northern part of the coastal plain.
C1 [Anisimov, Anatolii; Tao, Weichun; Stenchikov, Georgiy; Kalenderski, Stoitchko; Prakash, P. Jish] KAUST, Phys Sci & Engn Div PSE, Thuwal 239556900, Saudi Arabia.
[Yang, Zong-Liang; Shi, Mingjie] Univ Texas Austin, Jackson Sch Geosci, Dept Geol Sci, Austin, TX 78712 USA.
[Tao, Weichun] Minist Environm Protect, Policy Res Ctr Environm & Econ, Beijing 100029, Peoples R China.
[Shi, Mingjie] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Stenchikov, G (reprint author), KAUST, Phys Sci & Engn Div PSE, Thuwal 239556900, Saudi Arabia.
EM georgiy.stenchikov@kaust.edu.sa
FU King Abdullah University of Science and Technology (KAUST)
FX We thank V. Ramaswamy and Paul A. Ginoux of GFDL for valuable
discussions. We also thank Johann Engelbrecht and Linda Everett for
proofreading the article. The research reported in this publication was
supported by the King Abdullah University of Science and Technology
(KAUST). For computer time, this research used the resources of the
Supercomputing Laboratory at KAUST in Thuwal, Saudi Arabia.
NR 120
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U2 2
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PD JAN 23
PY 2017
VL 17
IS 2
BP 993
EP 1015
DI 10.5194/acp-17-993-2017
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EL4MM
UT WOS:000394595300003
ER
PT J
AU Halls, BR
Radke, CD
Reuter, BJ
Kastengren, AL
Gord, JR
Meyer, TR
AF Halls, Benjamin R.
Radke, Christopher D.
Reuter, Benjamin J.
Kastengren, Alan L.
Gord, James R.
Meyer, Terrence R.
TI High-speed, two-dimensional synchrotron white-beam x-ray radiography of
spray breakup and atomization
SO OPTICS EXPRESS
LA English
DT Article
ID DENSE SPRAYS; FUEL SPRAYS; STRUCTURED ILLUMINATION; ATOMIZING SPRAYS;
FLUID-DYNAMICS; DISTRIBUTIONS; FLUORESCENCE; JET; LIGHT; SHADOWGRAPHY
AB High-speed, two-dimensional synchrotron x-ray radiography and phase-contrast imaging are demonstrated in propulsion sprays. Measurements are performed at the 7-BM beamline at the Advanced Photon Source user facility at Argonne National Laboratory using a recently developed broadband x-ray white beam. This novel enhancement allows for high speed, high fidelity x-ray imaging for the community at large. Quantitative path-integrated liquid distributions and spatio-temporal dynamics of the sprays were imaged with a LuAG:Ce scintillator optically coupled to a high-speed CMOS camera. Images are collected with a microscope objective at frame rates of 20 kHz and with a macro lens at 120 kHz, achieving spatial resolutions of 12 mu m and 65 mu m, respectively. Imaging with and without potassium iodide (KI) as a contrast-enhancing agent is compared, and the effects of broadband attenuation and spatial beam characteristics are determined through modeling and experimental calibration. In addition, phase contrast is used to differentiate liquid streams with varying concentrations of KI. The experimental approach is applied to different spray conditions, including quantitative measurements of mass distribution during primary atomization and qualitative visualization of turbulent binary fluid mixing. (C) 2017 Optical Society of America
C1 [Halls, Benjamin R.; Gord, James R.] Air Force Res Lab, Aerosp Syst Directorate, Wright Patterson AFB, OH 45433 USA.
[Radke, Christopher D.] NASA, Prop & Power Div, Johnson Space Ctr, Houston, TX 77058 USA.
[Radke, Christopher D.; Reuter, Benjamin J.] Iowa State Univ, Dept Mech Engn, Ames, IA 50011 USA.
[Reuter, Benjamin J.] Spectral Energies LLC, Dayton, OH 45431 USA.
[Kastengren, Alan L.] Argonne Natl Lab, Xray Sci Div, Lemont, IL 60439 USA.
[Meyer, Terrence R.] Purdue Univ, Sch Mech Engn, W Lafayette, IN 47907 USA.
RP Halls, BR (reprint author), Air Force Res Lab, Aerosp Syst Directorate, Wright Patterson AFB, OH 45433 USA.
EM hallsbenjamin@gmail.com
FU National Research Council Post-doctoral Research Associateship award at
the Air Force Research Laboratory, Aerospace Systems Directorate,
Wright-Patterson AFB; U.S. Department of Energy [DE-AC02-06CH11357]
FX National Research Council Post-doctoral Research Associateship award at
the Air Force Research Laboratory, Aerospace Systems Directorate,
Wright-Patterson AFB; U.S. Department of Energy under Contract No.
DE-AC02-06CH11357.
NR 54
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U1 2
U2 2
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD JAN 23
PY 2017
VL 25
IS 2
BP 1605
EP 1617
DI 10.1364/OE.25.001605
PG 13
WC Optics
SC Optics
GA EO2HY
UT WOS:000396518400100
PM 28158042
ER
PT J
AU Sahai, R
Vlemmings, WHT
Gledhill, T
Contreras, CS
Lagadec, E
Nyman, LA
Quintana-Lacaci, G
AF Sahai, R.
Vlemmings, W. H. T.
Gledhill, T.
Sanchez Contreras, C.
Lagadec, E.
Nyman, L-A
Quintana-Lacaci, G.
TI ALMA Observations of the Water Fountain Pre-planetary Nebula IRAS
16342-3814: High-velocity Bipolar Jets and an Expanding Torus
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE circumstellar matter; stars: AGB and post-AGB; stars: mass-loss; stars:
winds, outflows; techniques: interferometric
ID YOUNG PLANETARY-NEBULAE; CIRCUMSTELLAR ENVELOPES; EVOLVED STARS; DUST
SHELL; IK TAURI; AGB; PROTOPLANETARY; (CO)-C-12; EMISSION; SYSTEM
AB We have mapped (CO)-C-12 J = 3-2 and other molecular lines from the "water fountain" bipolar pre-planetary nebula (PPN) IRAS 16342-3814 with similar to 0 ''. 35 resolution using Atacama Large Millimeter/submillimeter Array. We find (i) two very high-speed knotty, jet-like molecular outflows; (ii) a central high-density (> few x 10(6) cm(-3)), expanding torus of diameter 1300 au; and (iii) the circumstellar envelope of the progenitor AGB, generated by a sudden, very large increase in the mass-loss rate to > 3.5 x 10(-4) Me-circle dot yr(-1) in the past similar to 455 years. Strong continuum emission at 0.89 mm from a central source (690 mJy), if due to thermally emitting dust, implies a substantial mass (0.017M(circle dot)) of very large (similar to millimeter-sized) grains. The measured expansion ages of the above structural components imply that the torus (age similar to 160 years) and the younger high-velocity outflow (age similar to 110 years) were formed soon after the sharp increase in the AGB mass-loss rate. Assuming a binary model for the jets in IRAS 16342, the high momentum rate for the dominant jet-outflow in IRAS 16342 implies a high minimum accretion rate, ruling out standard Bondi-Hoyle-Lyttleton wind accretion and wind Roche-lobe overflow (RLOF) models with white-dwarf or main-sequence companions. Most likely, enhanced RLOF from the primary or accretion modes operating within common-envelope evolution are needed.
C1 [Sahai, R.] CALTECH, Jet Prop Lab, MS 183-900, Pasadena, CA 91109 USA.
[Vlemmings, W. H. T.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden.
[Gledhill, T.] Univ Hertfordshire, Ctr Astrophys Res, Coll Lane, Hatfield AL10 9AB, Herts, England.
[Sanchez Contreras, C.] INTA, CSIC, Astrobiol Ctr, ESAC Campus, E-28691 Madrid, Spain.
[Lagadec, E.] Univ Cote Azur, Observ Cote Azur, CNRS, Lagrange, France.
[Nyman, L-A] JAO, Alonso Cordova 3107, Santiago, Chile.
[Nyman, L-A] European Southern Observ, Alonso Cordova 3107, Santiago, Chile.
[Quintana-Lacaci, G.] Inst Ciencia Mat Madrid, Sor Juana Ines Cruz 3, E-28049 Madrid, Spain.
RP Sahai, R (reprint author), CALTECH, Jet Prop Lab, MS 183-900, Pasadena, CA 91109 USA.
EM raghvendra.sahai@jpl.nasa.gov
OI /0000-0002-2700-9916; Gledhill, Tim/0000-0002-2859-4600;
Quintana-Lacaci, Guillermo/0000-0002-5417-1943
FU NASA; ERC consolidator grant [614264]; Spanish MINECO [AYA2012-32032];
ERC [610256]
FX We are grateful to the late Patrick Huggins, who helped in defining the
proposal that led to this study. We thank an anonymous referee for
helpful comments. R.S.'s contribution to this research was carried out
at JPL, California Institute of Technology, under a contract with NASA.
W.V., C.S.C., and G.Q.-L. acknowledge support from ERC consolidator
grant 614264, Spanish MINECO grant AYA2012-32032, and ERC Grant
Agreement 610256 (NANOCOSMOS), respectively. This Letter uses ALMA data
set ADS/JAO. ALMA#2012.1.00678.S. ALMA is a partnership of ESO
(representing its member states), NSF (USA) and NINS (Japan), together
with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea),
in cooperation with the Republic of Chile. The Joint ALMA Observatory is
operated by ESO, AUI/NRAO and NAOJ.
NR 30
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JAN 20
PY 2017
VL 835
IS 1
AR L13
DI 10.3847/2041-8213/835/1/L13
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EL3SV
UT WOS:000394540500005
ER
PT J
AU Wakeford, HR
Stevenson, KB
Lewis, NK
Sing, DK
Lopez-Morales, M
Marley, M
Kataria, T
Mandell, A
Ballester, GE
Barstow, J
Ben-Jaffel, L
Bourrier, V
Buchhave, LA
Ehrenreich, D
Evans, T
Munoz, AG
Henry, G
Knutson, H
Lavvas, P
Etangs, ALD
Nikolov, N
Sanz-Forcada, J
AF Wakeford, H. R.
Stevenson, K. B.
Lewis, N. K.
Sing, D. K.
Lopez-Morales, M.
Marley, M.
Kataria, T.
Mandell, A.
Ballester, G. E.
Barstow, J.
Ben-Jaffel, L.
Bourrier, V.
Buchhave, L. A.
Ehrenreich, D.
Evans, T.
Munoz, A. Garcia
Henry, G.
Knutson, H.
Lavvas, P.
Etangs, A. Lecavelier des
Nikolov, N.
Sanz-Forcada, J.
TI HST PanCET Program: A Cloudy Atmosphere for the Promising JWST Target
WASP-101b
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planets and satellites: atmospheres; planets and satellites: individual
(WASP-101b); techniques: spectroscopic
ID MASS DWARF STARS; HUBBLE-SPACE-TELESCOPE; HOT-JUPITER EXOPLANETS;
TRANSMISSION SPECTRUM; GIANT PLANETS; BROWN DWARFS; CHEMISTRY;
SPECTROSCOPY; WATER; EMISSION
AB We present results from the first observations of the Hubble Space Telescope (HST) Panchromatic Comparative Exoplanet Treasury program for WASP-101b, a highly inflated hot Jupiter and one of the community targets proposed for the James Webb Space Telescope (JWST) Early Release Science (ERS) program. From a single HST Wide Field Camera 3 observation, we find that the near-infrared transmission spectrum of WASP-101b contains no significant H2O absorption features and we rule out a clear atmosphere at 13 sigma. Therefore, WASP-101b is not an optimum target for a JWST ERS program aimed at observing strong molecular transmission features. We compare WASP-101b to the well-studied and nearly identical hot Jupiter WASP-31b. These twin planets show similar temperature-pressure profiles and atmospheric features in the near-infrared. We suggest exoplanets in the same parameter space as WASP-101b and WASP-31b will also exhibit cloudy transmission spectral features. For future HST exoplanet studies, our analysis also suggests that a lower count limit needs to be exceeded per pixel on the detector in order to avoid unwanted instrumental systematics.
C1 [Wakeford, H. R.; Mandell, A.] NASA, Planetary Syst Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Stevenson, K. B.; Lewis, N. K.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Sing, D. K.; Evans, T.; Nikolov, N.] Univ Exeter, Astrophys Grp, Phys Bldg,Stocker Rd, Exeter EX4 4QL, Devon, England.
[Lopez-Morales, M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Marley, M.] NASA, Ames Res Ctr, MS 245-5, Moffett Field, CA 94035 USA.
[Kataria, T.] NASA, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Ballester, G. E.] Univ Arizona, Dept Planetary Sci, 1541 E Univ Blvd, Tucson, AZ 85721 USA.
[Ballester, G. E.] Univ Arizona, Lunar & Planetary Lab, 1541 E Univ Blvd, Tucson, AZ 85721 USA.
[Barstow, J.] UCL, Phys & Astron, London, England.
[Ben-Jaffel, L.; Etangs, A. Lecavelier des] CNRS, UMR 7095, Inst Astrophys Paris, 98 Bis Bd Arago, F-75014 Paris, France.
[Ben-Jaffel, L.; Etangs, A. Lecavelier des] UPMC Paris 6, Sorbonne Univ, 98 Bis Bd Arago, F-75014 Paris, France.
[Bourrier, V.; Ehrenreich, D.] Observ Univ Geneve, 51 Chemin Maillettes, CH-1290 Sauverny, Switzerland.
[Buchhave, L. A.] Univ Copenhagen, Niels Bohr Inst, Ctr Star & Planet Format, Oster Voldgade 5-7, DK-1350 Copenhagen K, Denmark.
[Buchhave, L. A.] Univ Copenhagen, Nat Hist Museum, Oster Voldgade 5-7, DK-1350 Copenhagen K, Denmark.
[Munoz, A. Garcia] Tech Univ Berlin, Zentrum Astron & Astrophys, D-10623 Berlin, Germany.
[Henry, G.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA.
[Knutson, H.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Lavvas, P.] Univ Reims, CNRS, UMR 7331, Grp Spect Mol & Atmospher, Reims, France.
[Sanz-Forcada, J.] INTA, CSIC, Ctr Astrobiol, ESAC Campus,POB 78, E-28691 Madrid, Spain.
RP Wakeford, HR (reprint author), NASA, Planetary Syst Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM hannah.wakeford@nasa.gov
OI Wakeford, Hannah/0000-0003-4328-3867
FU NASA [NAS 5-26555]; NASA Postdoctoral Program at Goddard Space Flight
Center; European Research Council under the European Unions Seventh
Framework Programme/ERC [336792]; Royal Astronomical Society Research
Fellowship; National Centre for Competence in Research "PlanetS" - Swiss
National Science Foundation (SNSF); CNES (France) under project PACES;
[GO-14767]
FX This research has made use of NASA's Astrophysics Data System and
components of the IDL astronomy library. Based on observations made with
the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at
the Space Telescope Science Institute, which is operated by the
Association of Universities for Research in Astronomy, Inc., under NASA
contract NAS 5-26555. These observations are associated with program
GO-14767. H.R.W. acknowledges support by an appointment to the NASA
Postdoctoral Program at Goddard Space Flight Center, administered by
USRA through a contract with NASA. D.K.S., N.N., and T.E. acknowledge
funding from the European Research Council under the European Unions
Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No.
336792. J.K.B. is supported by a Royal Astronomical Society Research
Fellowship. D.E. acknowledges the financial support of the National
Centre for Competence in Research "PlanetS" supported by the Swiss
National Science Foundation (SNSF). L.B.-J., P.L., and A.L. acknowledge
support from CNES (France) under project PACES. The authors would like
to thank the referee for their careful examination of this Letter.
NR 35
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JAN 20
PY 2017
VL 835
IS 1
AR L12
DI 10.3847/2041-8213/835/1/L12
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EL3SV
UT WOS:000394540500004
ER
PT J
AU Way, MJ
Georgakarakos, N
AF Way, M. J.
Georgakarakos, Nikolaos
TI Effects of Variable Eccentricity on the Climate of an Earth-like World
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE astrobiology; planets and satellites: atmospheres; planets and
satellites: terrestrial planets
ID LONG-TERM EVOLUTION; PLANETARY SYSTEMS; OBLIQUITY; HABITABILITY; MARS;
EXOPLANETS; MODEL
AB The Kepler era of exoplanetary discovery has presented the astronomical community with a cornucopia of planetary systems that are very different from the one that we inhabit. It has long been known that Jupiter plays a major role in the orbital parameters of Mars and its climate, but there is also a long-standing belief that Jupiter would play a similar role for Earth if not for the Moon. Using a three-dimensional general circulation model (3D GCM) with a fully coupled ocean, we simulate what would happen to the climate of an Earth-like world if Mars did not exist, but a Jupiter-like planet was much closer to Earth's orbit. We investigate two scenarios that involve the evolution of the Earth-like planet's orbital eccentricity from 0 to 0.283 over 6500 years, and from 0 to 0.066 on a timescale of 4500 years. In both cases we discover that they would maintain relatively temperate climates over the timescales simulated. More Earth-like planets in multi-planet systems will be discovered as we continue to survey the skies and the results herein show that the proximity of large gas giant planets may play an important role in the habitability of these worlds. These are the first such 3D GCM simulations using a fully coupled ocean with a planetary orbit that evolves over time due to the presence of a giant planet.
C1 [Way, M. J.] NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
[Georgakarakos, Nikolaos] New York Univ Abu Dhabi, POB 129188, Abu Dhabi, U Arab Emirates.
[Way, M. J.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
RP Way, MJ (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.; Way, MJ (reprint author), Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
EM Michael.J.Way@nasa.gov
OI Georgakarakos, Nikolaos/0000-0002-7071-5437; Way,
Michael/0000-0003-3728-0475
FU NASAs Science Mission Directorate; NASA Goddard Space Flight Center
ROCKE-3D Science Task Group
FX We thank Thomas P. Clune for his help in getting the ROCKE-3D model to
handle variable eccentricity worlds and Tony Del Genio and the GISS
ROCKE-3D NExSS team for comments and suggestions. Special thanks goes to
the referee Dorian Abbott for suggestions that improved the manuscript.
The results reported herein benefited from participation in NASA's Nexus
for Exoplanet System Science research coordination network sponsored by
NASAs Science Mission Directorate. This work was also supported by NASA
Goddard Space Flight Center ROCKE-3D Science Task Group funding.
Resources supporting this work were provided by the NASA High-End
Computing (HEC) Program through the NASA Center for Climate Simulation
(NCCS) at Goddard Space Flight Center.
NR 29
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JAN 20
PY 2017
VL 835
IS 1
AR L1
DI 10.3847/2041-8213/835/1/L1
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EK5NV
UT WOS:000393974000001
ER
PT J
AU De Young, R
Carrion, W
Ganoe, R
Pliutau, D
Gronoff, G
Berkoff, T
Kuang, S
AF De Young, Russell
Carrion, William
Ganoe, Rene
Pliutau, Denis
Gronoff, Guillaume
Berkoff, Timothy
Kuang, Shi
TI Langley mobile ozone lidar: ozone and aerosol atmospheric profiling for
air quality research
SO APPLIED OPTICS
LA English
DT Article
ID ABSORPTION CROSS-SECTIONS; UV SPECTROSCOPY; TEMPERATURE; REGION
AB The Langley mobile ozone lidar (LMOL) is a mobile ground-based ozone lidar system that consists of a pulsed UV laser producing two UV wavelengths of 286 and 291 nm with energy of approximately 0.2 mJ/pulse and repetition rate of 1 kHz. The 527 nm pump laser is also transmitted for aerosol measurements. The receiver consists of a 40 cm parabolic telescope, which is used for both backscattered analog and photon counting. The lidar is very compact and highly mobile. This demonstrates the utility of very small lidar systems eventually leading to spacebased ozone lidars. The lidar has been validated by numerous ozonesonde launches and has provided ozone curtain profiles from ground to approximately 4 km in support of air quality field missions.
C1 [De Young, Russell; Berkoff, Timothy] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Carrion, William] Coherent Technol, Hampton, VA 23681 USA.
[Ganoe, Rene; Pliutau, Denis; Gronoff, Guillaume] Sci Syst & Applicat Inc, Hampton, VA 23681 USA.
[Kuang, Shi] Ctr Earth Syst Sci, Huntsville, AL 35805 USA.
RP De Young, R (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM Russell.j.deyoung@nasa.gov
OI Kuang, Shi/0000-0003-2423-6088
FU National Aeronautics and Space Administration (NASA) Earth Sciences
Division
FX National Aeronautics and Space Administration (NASA) Earth Sciences
Division.
NR 26
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U2 1
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD JAN 20
PY 2017
VL 56
IS 3
BP 721
EP 730
DI 10.1364/AO.56.000721
PG 10
WC Optics
SC Optics
GA EJ6SA
UT WOS:000393347900080
PM 28157936
ER
PT J
AU Murrill, SR
Franck, CC
Jacobs, EL
Petkie, DT
De Lucia, FC
AF Murrill, Steven R.
Franck, Charmaine C.
Jacobs, Eddie L.
Petkie, Douglas T.
De Lucia, Frank C.
TI Enhanced MMW and SMMW/THz imaging system performance prediction and
analysis tool for concealed weapon detection and pilotage obstacle
avoidance
SO APPLIED OPTICS
LA English
DT Review
AB The U.S. Army Research Laboratory has continued to develop and enhance a millimeter- wave (MMW) and submillimeter-wave (SMMW)/terahertz (THz)-band imaging system performance prediction and analysis tool for both the detection and identification of concealed weaponry and for pilotage obstacle avoidance. The details of the MATLAB-based model that accounts for the effects of all critical sensor and display components, for the effects of atmospheric attenuation, concealment material attenuation, active illumination, target and background orientation, target and background thermal emission, and various imaging system architectures have been reported on in 2005, 2007, and 2011. This paper provides a comprehensive review of a newly enhanced MMW and SMMW/THz imaging system analysis and design tool that now includes an improved noise submodel for more accurate and reliable performance predictions, the capability to account for postcapture image contrast enhancement, and the capability to account for concealment material backscatter with active-illumination-based systems. Present plans for additional expansion of the model's predictive capabilities are also outlined. (C) 2017 Optical Society of America
C1 [Murrill, Steven R.] US Army Res Lab, Adelphi, MD 20783 USA.
[Franck, Charmaine C.] NASA Langley, Hampton, VA 23692 USA.
[Jacobs, Eddie L.] Univ Memphis, Dept Elect & Comp Engn, Memphis, TN 38152 USA.
[Petkie, Douglas T.] Wright State Univ, Dept Phys, Dayton, OH 45435 USA.
[De Lucia, Frank C.] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA.
RP Murrill, SR (reprint author), US Army Res Lab, Adelphi, MD 20783 USA.
EM steven.r.murrill2.civ@mail.mil
NR 6
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U1 3
U2 3
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD JAN 20
PY 2017
VL 56
IS 3
BP B231
EP B239
DI 10.1364/AO.56.00B231
PG 9
WC Optics
SC Optics
GA EJ6SA
UT WOS:000393347900030
PM 28157942
ER
PT J
AU Aartsen, MG
Abraham, K
Ackermann, M
Adams, J
Aguilar, JA
Ahlers, M
Ahrens, M
Altmann, D
Andeen, K
Anderson, T
Ansseau, I
Anton, G
Archinger, M
Arguelles, C
Arlen, TC
Auffenberg, J
Axani, S
Bai, X
Barwick, SW
Baum, V
Bay, R
Beatty, JJ
Tjus, JB
Becker, KH
BenZvi, S
Berghaus, P
Berley, D
Bernardini, E
Bernhard, A
Besson, DZ
Binder, G
Bindig, D
Bissok, M
Blaufuss, E
Blot, S
Boersma, DJ
Bohm, C
Borner, M
Bos, F
Bose, D
Boser, S
Botner, O
Braun, J
Brayeur, L
Bretz, HP
Burgman, A
Casey, J
Casier, M
Cheung, E
Chirkin, D
Christov, A
Clark, K
Classen, L
Coenders, S
Collin, GH
Conrad, JM
Cowen, DF
Silva, AHC
Daughhetee, J
Davis, JC
Day, M
de Andre, JPAM
De Clercq, C
Rosendo, ED
Dembinski, H
De Ridder, S
Desiati, P
de Vries, KD
de Wasseige, G
de With, M
DeYoung, T
Diaz-Velez, JC
di Lorenzo, V
Dujmovic, H
Dumm, JP
Dunkman, M
Eberhardt, B
Ehrhardt, T
Eichmann, B
Euler, S
Evenson, PA
Fahey, S
Fazely, AR
Feintzeig, J
Felde, J
Filimonov, K
Finley, C
Flis, S
Fosig, CC
Franckowiak, A
Fuchs, T
Gaisser, TK
Gaior, R
Gallagher, J
Gerhardt, L
Ghorbani, K
Giang, W
Gladstone, L
Glagla, M
Glusenkamp, T
Goldschmidt, A
Golup, G
Gonzalez, JG
Gora, D
Grant, D
Griffith, Z
Haack, C
Ismail, AH
Hallgren, A
Halzen, F
Hansen, E
Hansmann, B
Hansmann, T
Hanson, K
Hebecker, D
Heereman, D
Helbing, K
Hellauer, R
Hickford, S
Hignight, J
Hill, GC
Hoffman, KD
Hoffmann, R
Holzapfel, K
Homeier, A
Hoshina, K
Huang, F
Huber, M
Huelsnitz, W
Hultqvist, K
In, S
Ishihara, A
Jacobi, E
Japaridze, GS
Jeong, M
Jero, K
Jones, BJP
Jurkovic, M
Kappes, A
Karg, T
Karle, A
Katz, U
Kauer, M
Keivani, A
Kelley, JL
Kemp, J
Kheirandish, A
Kim, M
Kintscher, T
Kiryluk, J
Kittler, T
Klein, SR
Kohnen, G
Koirala, R
Kolanoski, H
Konietz, R
Kopke, L
Kopper, C
Kopper, S
Koskinen, DJ
Kowalski, M
Krings, K
Kroll, M
Kruckl, G
Kruger, C
Kunnen, J
Kunwar, S
Kurahashi, N
Kuwabara, T
Labare, M
Lanfranchi, JL
Larson, MJ
Lennarz, D
Lesiak-Bzdak, M
Leuermann, M
Leuner, J
Lu, L
Lunemann, J
Madsen, J
Maggi, G
Mahn, KBM
Mancina, S
Mandelartz, M
Maruyama, R
Mase, K
Maunu, R
McNally, F
Meagher, K
Medici, M
Meier, M
Meli, A
Menne, T
Merino, G
Meures, T
Miarecki, S
Middell, E
Mohrmann, L
Montaruli, T
Moulai, M
Nahnhauer, R
Naumann, U
Neer, G
Niederhausen, H
Nowicki, SC
Nygren, DR
Pollmann, AO
Olivas, A
Omairat, A
O'Murchadha, A
Palczewski, T
Pandya, H
Pankova, DV
Penek, O
Pepper, JA
de los Heros, CP
Pfendner, C
Pieloth, D
Pinat, E
Posselt, J
Price, PB
Przybylski, GT
Quinnan, M
Raab, C
Radel, L
Rameez, M
Rawlins, K
Reimann, R
Relich, M
Resconi, E
Rhode, W
Richman, M
Riedel, B
Robertson, S
Rongen, M
Rott, C
Ruhe, T
Ryckbosch, D
Rysewyk, D
Sabbatini, L
Herrera, SES
Sandrock, A
Sandroos, J
Sarkar, S
Satalecka, K
Schimp, M
Schlunder, P
Schmidt, T
Schoenen, S
Schoneberg, S
Schonwald, A
Schumacher, L
Seckel, D
Seunarine, S
Soldin, D
Song, M
Spiczak, GM
Spiering, C
Stahlberg, M
Stamatikos, M
Stanev, T
Stasik, A
Steuer, A
Stezelberger, T
Stokstad, RG
Stossl, A
Strom, R
Strotjohann, NL
Sullivan, GW
Sutherland, M
Taavola, H
Taboada, I
Tatar, J
Ter-Antonyan, S
Terliuk, A
Tesic, G
Tilav, S
Toale, PA
Tobin, MN
Toscano, S
Tosi, D
Tselengidou, M
Turcati, A
Unger, E
Usner, M
Vallecorsa, S
Vandenbroucke, J
van Eijndhoven, N
Vanheule, S
van Rossem, M
van Santen, J
Veenkamp, J
Vehring, M
Voge, M
Vraeghe, M
Walck, C
Wallace, A
Wallraff, M
Wandkowsky, N
Weaver, C
Wendt, C
Westerhoff, S
Whelan, BJ
Wickmann, S
Wiebe, K
Wiebusch, CH
Wille, L
Williams, DR
Wills, L
Wissing, H
Wolf, M
Wood, TR
Woolsey, E
Woschnagg, K
Xu, DL
Xu, XW
Xu, Y
Yanez, JP
Yodh, G
Yoshida, S
Zoll, M
AF Aartsen, M. G.
Abraham, K.
Ackermann, M.
Adams, J.
Aguilar, J. A.
Ahlers, M.
Ahrens, M.
Altmann, D.
Andeen, K.
Anderson, T.
Ansseau, I.
Anton, G.
Archinger, M.
Arguelles, C.
Arlen, T. C.
Auffenberg, J.
Axani, S.
Bai, X.
Barwick, S. W.
Baum, V.
Bay, R.
Beatty, J. J.
Tjus, J. Becker
Becker, K. -H.
BenZvi, S.
Berghaus, P.
Berley, D.
Bernardini, E.
Bernhard, A.
Besson, D. Z.
Binder, G.
Bindig, D.
Bissok, M.
Blaufuss, E.
Blot, S.
Boersma, D. J.
Bohm, C.
Boerner, M.
Bos, F.
Bose, D.
Boeser, S.
Botner, O.
Braun, J.
Brayeur, L.
Bretz, H. -P.
Burgman, A.
Casey, J.
Casier, M.
Cheung, E.
Chirkin, D.
Christov, A.
Clark, K.
Classen, L.
Coenders, S.
Collin, G. H.
Conrad, J. M.
Cowen, D. F.
Silva, A. H. Cruz
Daughhetee, J.
Davis, J. C.
Day, M.
de Andre, J. P. A. M.
De Clercq, C.
Rosendo, E. del Pino
Dembinski, H.
De Ridder, S.
Desiati, P.
de Vries, K. D.
de Wasseige, G.
de With, M.
DeYoung, T.
Diaz-Velez, J. C.
di Lorenzo, V.
Dujmovic, H.
Dumm, J. P.
Dunkman, M.
Eberhardt, B.
Ehrhardt, T.
Eichmann, B.
Euler, S.
Evenson, P. A.
Fahey, S.
Fazely, A. R.
Feintzeig, J.
Felde, J.
Filimonov, K.
Finley, C.
Flis, S.
Foesig, C. -C.
Franckowiak, A.
Fuchs, T.
Gaisser, T. K.
Gaior, R.
Gallagher, J.
Gerhardt, L.
Ghorbani, K.
Giang, W.
Gladstone, L.
Glagla, M.
Gluesenkamp, T.
Goldschmidt, A.
Golup, G.
Gonzalez, J. G.
Gora, D.
Grant, D.
Griffith, Z.
Haack, C.
Ismail, A. Haj
Hallgren, A.
Halzen, F.
Hansen, E.
Hansmann, B.
Hansmann, T.
Hanson, K.
Hebecker, D.
Heereman, D.
Helbing, K.
Hellauer, R.
Hickford, S.
Hignight, J.
Hill, G. C.
Hoffman, K. D.
Hoffmann, R.
Holzapfel, K.
Homeier, A.
Hoshina, K.
Huang, F.
Huber, M.
Huelsnitz, W.
Hultqvist, K.
In, S.
Ishihara, A.
Jacobi, E.
Japaridze, G. S.
Jeong, M.
Jero, K.
Jones, B. J. P.
Jurkovic, M.
Kappes, A.
Karg, T.
Karle, A.
Katz, U.
Kauer, M.
Keivani, A.
Kelley, J. L.
Kemp, J.
Kheirandish, A.
Kim, M.
Kintscher, T.
Kiryluk, J.
Kittler, T.
Klein, S. R.
Kohnen, G.
Koirala, R.
Kolanoski, H.
Konietz, R.
Koepke, L.
Kopper, C.
Kopper, S.
Koskinen, D. J.
Kowalski, M.
Krings, K.
Kroll, M.
Krueckl, G.
Krueger, C.
Kunnen, J.
Kunwar, S.
Kurahashi, N.
Kuwabara, T.
Labare, M.
Lanfranchi, J. L.
Larson, M. J.
Lennarz, D.
Lesiak-Bzdak, M.
Leuermann, M.
Leuner, J.
Lu, L.
Lunemann, J.
Madsen, J.
Maggi, G.
Mahn, K. B. M.
Mancina, S.
Mandelartz, M.
Maruyama, R.
Mase, K.
Maunu, R.
McNally, F.
Meagher, K.
Medici, M.
Meier, M.
Meli, A.
Menne, T.
Merino, G.
Meures, T.
Miarecki, S.
Middell, E.
Mohrmann, L.
Montaruli, T.
Moulai, M.
Nahnhauer, R.
Naumann, U.
Neer, G.
Niederhausen, H.
Nowicki, S. C.
Nygren, D. R.
Pollmann, A. Obertacke
Olivas, A.
Omairat, A.
O'Murchadha, A.
Palczewski, T.
Pandya, H.
Pankova, D. V.
Penek, Oe.
Pepper, J. A.
de los Heros, C. Perez
Pfendner, C.
Pieloth, D.
Pinat, E.
Posselt, J.
Price, P. B.
Przybylski, G. T.
Quinnan, M.
Raab, C.
Raedel, L.
Rameez, M.
Rawlins, K.
Reimann, R.
Relich, M.
Resconi, E.
Rhode, W.
Richman, M.
Riedel, B.
Robertson, S.
Rongen, M.
Rott, C.
Ruhe, T.
Ryckbosch, D.
Rysewyk, D.
Sabbatini, L.
Herrera, S. E. Sanchez
Sandrock, A.
Sandroos, J.
Sarkar, S.
Satalecka, K.
Schimp, M.
Schlunder, P.
Schmidt, T.
Schoenen, S.
Schoeneberg, S.
Schoenwald, A.
Schumacher, L.
Seckel, D.
Seunarine, S.
Soldin, D.
Song, M.
Spiczak, G. M.
Spiering, C.
Stahlberg, M.
Stamatikos, M.
Stanev, T.
Stasik, A.
Steuer, A.
Stezelberger, T.
Stokstad, R. G.
Stoessl, A.
Strom, R.
Strotjohann, N. L.
Sullivan, G. W.
Sutherland, M.
Taavola, H.
Taboada, I.
Tatar, J.
Ter-Antonyan, S.
Terliuk, A.
Tesic, G.
Tilav, S.
Toale, P. A.
Tobin, M. N.
Toscano, S.
Tosi, D.
Tselengidou, M.
Turcati, A.
Unger, E.
Usner, M.
Vallecorsa, S.
Vandenbroucke, J.
van Eijndhoven, N.
Vanheule, S.
van Rossem, M.
van Santen, J.
Veenkamp, J.
Vehring, M.
Voge, M.
Vraeghe, M.
Walck, C.
Wallace, A.
Wallraff, M.
Wandkowsky, N.
Weaver, Ch.
Wendt, C.
Westerhoff, S.
Whelan, B. J.
Wickmann, S.
Wiebe, K.
Wiebusch, C. H.
Wille, L.
Williams, D. R.
Wills, L.
Wissing, H.
Wolf, M.
Wood, T. R.
Woolsey, E.
Woschnagg, K.
Xu, D. L.
Xu, X. W.
Xu, Y.
Yanez, J. P.
Yodh, G.
Yoshida, S.
Zoll, M.
CA IceCube Collaboration
TI THE CONTRIBUTION OF FERMI-2LAC BLAZARS TO DIFFUSE TEV-PEV NEUTRINO FLUX
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astroparticle physics; BL Lacertae objects: general; gamma rays:
galaxies; methods: data analysis; neutrinos; quasars: general
ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; BL-LACERTAE OBJECTS;
HIGH-ENERGY NEUTRINOS; ICECUBE DATA; LIKELIHOOD ANALYSIS;
MAXIMUM-LIKELIHOOD; SIMPLIFIED VIEW; SOURCE CATALOG; LAC OBJECTS
AB The recent discovery of a diffuse cosmic neutrino flux extending up to PeV energies raises the question of which astrophysical sources generate this signal. Blazars are one class of extragalactic sources which may produce such high-energy neutrinos. We present a likelihood analysis searching for cumulative neutrino emission from blazars in the 2nd Fermi-LAT AGN catalog (2LAC) using IceCube neutrino data set 2009-12, which was optimized for the detection of individual sources. In contrast to those in previous searches with IceCube, the populations investigated contain up to hundreds of sources, the largest one being the entire blazar sample in the 2LAC catalog. No significant excess is observed, and upper limits for the cumulative flux from these populations are obtained. These constrain the maximum contribution of 2LAC blazars to the observed astrophysical neutrino flux to 27% or less between around 10 TeV and 2 PeV, assuming the equipartition of flavors on Earth and a single power-law spectrum with a spectral index of -2.5. We can still exclude the fact that 2LAC blazars (and their subpopulations) emit more than 50% of the observed neutrinos up to a spectral index as hard as -2.2 in the same energy range. Our result takes into account the fact that the neutrino source count distribution is unknown, and it does not assume strict proportionality of the neutrino flux to the measured 2LAC gamma-ray signal for each source. Additionally, we constrain recent models for neutrino emission by blazars.
C1 [Aartsen, M. G.; Hill, G. C.; Robertson, S.; Wallace, A.; Whelan, B. J.] Univ Adelaide, Dept Phys, Adelaide, SA 5005, Australia.
[Abraham, K.; Bernhard, A.; Coenders, S.; Holzapfel, K.; Huber, M.; Jurkovic, M.; Krings, K.; Resconi, E.; Turcati, A.; Veenkamp, J.] Tech Univ Munich, Dept Phys, D-85748 Garching, Germany.
[Ackermann, M.; Bernardini, E.; Blot, S.; Bretz, H. -P.; Silva, A. H. Cruz; Franckowiak, A.; Gluesenkamp, T.; Gora, D.; Jacobi, E.; Karg, T.; Kintscher, T.; Kowalski, M.; Kunwar, S.; Middell, E.; Mohrmann, L.; Nahnhauer, R.; Satalecka, K.; Schoenwald, A.; Spiering, C.; Stasik, A.; Stoessl, A.; Strotjohann, N. L.; Terliuk, A.; Usner, M.; van Santen, J.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany.
[Adams, J.] Univ Canterbury, Dept Phys & Astron, Private Bag 4800, Christchurch, New Zealand.
[Aguilar, J. A.; Ansseau, I.; Heereman, D.; Meagher, K.; Meures, T.; O'Murchadha, A.; Pinat, E.; Raab, C.] Univ Libre Bruxelles, Fac Sci, CP230, B-1050 Brussels, Belgium.
[Ahlers, M.; Braun, J.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Fahey, S.; Feintzeig, J.; Ghorbani, K.; Gladstone, L.; Griffith, Z.; Halzen, F.; Hanson, K.; Hoshina, K.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kheirandish, A.; Krueger, C.; Mancina, S.; McNally, F.; Merino, G.; Sabbatini, L.; Tobin, M. N.; Tosi, D.; Vandenbroucke, J.; van Rossem, M.; Wandkowsky, N.; Wendt, C.; Westerhoff, S.; Wille, L.; Xu, D. L.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Ahlers, M.; Braun, J.; Chirkin, D.; Day, M.; Desiati, P.; Diaz-Velez, J. C.; Fahey, S.; Feintzeig, J.; Ghorbani, K.; Gladstone, L.; Griffith, Z.; Halzen, F.; Hanson, K.; Hoshina, K.; Jero, K.; Karle, A.; Kauer, M.; Kelley, J. L.; Kheirandish, A.; Krueger, C.; Mancina, S.; McNally, F.; Merino, G.; Sabbatini, L.; Tobin, M. N.; Tosi, D.; Vandenbroucke, J.; van Rossem, M.; Wandkowsky, N.; Wendt, C.; Westerhoff, S.; Wille, L.; Xu, D. L.] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA.
[Ahrens, M.; Bohm, C.; Dumm, J. P.; Finley, C.; Flis, S.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Ahrens, M.; Bohm, C.; Dumm, J. P.; Finley, C.; Flis, S.; Hultqvist, K.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Altmann, D.; Anton, G.; Katz, U.; Kittler, T.; Tselengidou, M.] Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany.
[Andeen, K.] Marquette Univ, Dept Phys, Milwaukee, WI 53201 USA.
[Anderson, T.; Arlen, T. C.; Cowen, D. F.; Dunkman, M.; Huang, F.; Keivani, A.; Lanfranchi, J. L.; Pankova, D. V.; Quinnan, M.; Tesic, G.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Archinger, M.; Baum, V.; Boeser, S.; Rosendo, E. del Pino; di Lorenzo, V.; Eberhardt, B.; Ehrhardt, T.; Foesig, C. -C.; Koepke, L.; Krueckl, G.; Sandroos, J.; Steuer, A.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, Staudinger Weg 7, D-55099 Mainz, Germany.
[Arguelles, C.; Axani, S.; Collin, G. H.; Conrad, J. M.; Jones, B. J. P.; Moulai, M.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Auffenberg, J.; Bissok, M.; Glagla, M.; Haack, C.; Hansmann, B.; Hansmann, T.; Kemp, J.; Konietz, R.; Leuermann, M.; Leuner, J.; Penek, Oe.; Raedel, L.; Reimann, R.; Rongen, M.; Schimp, M.; Schoenen, S.; Schumacher, L.; Stahlberg, M.; Vehring, M.; Wallraff, M.; Wickmann, S.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany.
[Bai, X.] South Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA.
[Barwick, S. W.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Bay, R.; Binder, G.; Filimonov, K.; Gerhardt, L.; Klein, S. R.; Miarecki, S.; Price, P. B.; Tatar, J.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.; Sutherland, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Beatty, J. J.; Davis, J. C.; Pfendner, C.; Stamatikos, M.; Sutherland, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Tjus, J. Becker; Bos, F.; Eichmann, B.; Kroll, M.; Mandelartz, M.; Schoeneberg, S.] Ruhr Univ Bochum, Fac Phys & Astron, D-44780 Bochum, Germany.
[Becker, K. -H.; Bindig, D.; Helbing, K.; Hickford, S.; Hoffmann, R.; Kopper, S.; Naumann, U.; Pollmann, A. Obertacke; Omairat, A.; Posselt, J.; Soldin, D.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
[BenZvi, S.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
[Berghaus, P.] Natl Res Nucl Univ MEPhI, Moscow Engn Phys Inst, Moscow, Russia.
[Berley, D.; Blaufuss, E.; Cheung, E.; Felde, J.; Hellauer, R.; Hoffman, K. D.; Huelsnitz, W.; Maunu, R.; Olivas, A.; Schmidt, T.; Song, M.; Sullivan, G. W.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Binder, G.; Gerhardt, L.; Goldschmidt, A.; Klein, S. R.; Miarecki, S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.; Tatar, J.] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Boersma, D. J.; Botner, O.; Burgman, A.; Euler, S.; Hallgren, A.; de los Heros, C. Perez; Strom, R.; Taavola, H.; Unger, E.] Uppsala Univ, Dept Phys & Astron, Box 516, SE-75120 Uppsala, Sweden.
[Boerner, M.; Fuchs, T.; Meier, M.; Menne, T.; Pieloth, D.; Rhode, W.; Ruhe, T.; Sandrock, A.; Schlunder, P.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany.
[Bose, D.; Dujmovic, H.; Jeong, M.; Kim, M.; Rott, C.; Tobin, M. N.] Sungkyunkwan Univ, Dept Phys, Suwon 440746, South Korea.
[Brayeur, L.; Casier, M.; De Clercq, C.; de Vries, K. D.; de Wasseige, G.; Golup, G.; Kunnen, J.; Lunemann, J.; Maggi, G.; Toscano, S.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
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[Classen, L.; Kappes, A.] Westfalische Wilhelms Univ Munster, Inst Kernphys, D-48149 Munster, Germany.
[Cowen, D. F.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
[de Andre, J. P. A. M.; DeYoung, T.; Hignight, J.; Lennarz, D.; Mahn, K. B. M.; Neer, G.; Rysewyk, D.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Dembinski, H.; Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Koirala, R.; Pandya, H.; Seckel, D.; Stanev, T.; Tilav, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Dembinski, H.; Evenson, P. A.; Gaisser, T. K.; Gonzalez, J. G.; Koirala, R.; Pandya, H.; Seckel, D.; Stanev, T.; Tilav, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[De Ridder, S.; Ismail, A. Haj; Labare, M.; Meli, A.; Ryckbosch, D.; Vanheule, S.; Vraeghe, M.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium.
[de With, M.; Hebecker, D.; Kolanoski, H.; Kowalski, M.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA.
[Gaior, R.; Ishihara, A.; Kuwabara, T.; Lu, L.; Mase, K.; Relich, M.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan.
[Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Giang, W.; Grant, D.; Kopper, C.; Nowicki, S. C.; Riedel, B.; Herrera, S. E. Sanchez; Weaver, Ch.; Wood, T. R.; Woolsey, E.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada.
[Hansen, E.; Koskinen, D. J.; Larson, M. J.; Medici, M.; Sarkar, S.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Homeier, A.; Voge, M.] Univ Bonn, Inst Phys, Nussallee 12, D-53115 Bonn, Germany.
[Hoshina, K.] Univ Tokyo, Earthquake Res Inst, Bunkyo Ku, Tokyo 1130032, Japan.
[Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA.
[Kauer, M.; Maruyama, R.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Kiryluk, J.; Lesiak-Bzdak, M.; Niederhausen, H.; Xu, Y.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Kohnen, G.] Univ Mons, B-7000 Mons, Belgium.
[Kurahashi, N.; Richman, M.; Wills, L.] Drexel Univ, Dept Phys, 3141 Chestnut St, Philadelphia, PA 19104 USA.
[Madsen, J.; Seunarine, S.; Spiczak, G. M.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA.
[Palczewski, T.; Pepper, J. A.; Toale, P. A.; Williams, D. R.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, 3211 Providence Dr, Anchorage, AK 99508 USA.
[Sarkar, S.] Univ Oxford, Dept Phys, 1 Keble Rd, Oxford OX1 3NP, England.
[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Glusenkamp, T (reprint author), DESY, D-15735 Zeuthen, Germany.
EM thorsten.gluesenkamp@fau.de
RI Beatty, James/D-9310-2011; Maruyama, Reina/A-1064-2013
OI Beatty, James/0000-0003-0481-4952; Maruyama, Reina/0000-0003-2794-512X
FU U.S. National Science Foundation-Office of Polar Programs; U.S. National
Science Foundation-Physics Division; University of Wisconsin Alumni
Research Foundation; Grid Laboratory of Wisconsin's grid infrastructure
at the University of Wisconsin-Madison; Open Science Grid's grid
infrastructure; U.S. Department of Energy's National Energy Research
Scientific Computing Center; Louisiana Optical Network Initiative's grid
computing resources; Natural Sciences and Engineering Research Council
of Canada; WestGrid; Compute/Calcul Canada; Swedish Research Council,
Sweden; Swedish Polar Research Secretariat, Sweden; Swedish National
Infrastructure for Computing, Sweden; Knut and Alice Wallenberg
Foundation, Sweden; German Ministry for Education and Research (Bochum),
Germany; Deutsche Forschungsgemeinschaft (Bochum), Germany; Helmholtz
Alliance for Astroparticle Physics (Bochum), Germany; Research
Department of Plasmas with Complex Interactions (Bochum), Germany; Fund
for Scientific Research, FWO Odysseus program; Flanders Institute;
Belgian Federal Science Policy Office; University of Oxford, United
Kingdom; Marsden Fund, New Zealand; Australian Research Council; Japan
Society for Promotion of Science; Swiss National Science Foundation,
Switzerland; National Research Foundation of Korea (NRF); Villum Fonden,
Danish National Research Foundation, Denmark
FX We acknowledge support from the following agencies: the U.S. National
Science Foundation-Office of Polar Programs, the U.S. National Science
Foundation-Physics Division, the University of Wisconsin Alumni Research
Foundation, the Grid Laboratory of Wisconsin's grid infrastructure at
the University of Wisconsin-Madison, and the Open Science Grid's grid
infrastructure; the U.S. Department of Energy's National Energy Research
Scientific Computing Center and the Louisiana Optical Network
Initiative's grid computing resources; the Natural Sciences and
Engineering Research Council of Canada, WestGrid, and Compute/Calcul
Canada; the Swedish Research Council, the Swedish Polar Research
Secretariat, the Swedish National Infrastructure for Computing, and the
Knut and Alice Wallenberg Foundation, Sweden; the German Ministry for
Education and Research, Deutsche Forschungsgemeinschaft, the Helmholtz
Alliance for Astroparticle Physics, and the Research Department of
Plasmas with Complex Interactions (Bochum), Germany; the Fund for
Scientific Research, FWO Odysseus program, Flanders Institute (to
encourage scientific and technological research in industry) and the
Belgian Federal Science Policy Office; the University of Oxford, United
Kingdom; the Marsden Fund, New Zealand; the Australian Research Council;
Japan Society for Promotion of Science; the Swiss National Science
Foundation, Switzerland; the National Research Foundation of Korea
(NRF); and Villum Fonden, Danish National Research Foundation, Denmark.
NR 61
TC 0
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U1 6
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2017
VL 835
IS 1
AR 45
DI 10.3847/1538-4357/835/1/45
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EJ8DO
UT WOS:000393455400045
ER
PT J
AU Borovikov, D
Tenishev, V
Gombosi, TI
Guidoni, SE
DeVore, CR
Karpen, JT
Antiochos, SK
AF Borovikov, D.
Tenishev, V.
Gombosi, T. I.
Guidoni, S. E.
DeVore, C. R.
Karpen, J. T.
Antiochos, S. K.
TI ELECTRON ACCELERATION IN CONTRACTING MAGNETIC ISLANDS DURING SOLAR
FLARES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; magnetic reconnection; Sun: flares
ID CORONAL MASS EJECTIONS; X-RAY OBSERVATIONS; PARTICLE-ACCELERATION;
RECONNECTION; SPECTRA; MODEL
AB Electron acceleration in solar flares is well known to be efficient at generating energetic particles that produce the observed bremsstrahlung X-ray spectra. One mechanism proposed to explain the observations is electron acceleration within contracting magnetic islands formed by magnetic reconnection in the flare current sheet. In a previous study, a numerical magnetohydrodynamic simulation of an eruptive solar flare was analyzed to estimate the associated electron acceleration due to island contraction. That analysis used a simple analytical model for the island structure and assumed conservation of the adiabatic invariants of particle motion. In this paper, we perform the first-ever rigorous integration of the guiding-center orbits of electrons in a modeled flare. An initially isotropic distribution of particles is seeded in a contracting island from the simulated eruption, and the subsequent evolution of these particles is followed using guiding-center theory. We find that the distribution function becomes increasingly anisotropic over time as the electrons' energy increases by up to a factor of five, in general agreement with the previous study. In addition, we show that the energized particles are concentrated on the Sunward side of the island, adjacent to the reconnection X-point in the flare current sheet. Furthermore, our analysis demonstrates that the electron energy gain is dominated by betatron acceleration in the compressed, strengthened magnetic field of the contracting island. Fermi acceleration by the shortened field lines of the island also contributes to the energy gain, but it is less effective than the betatron process.
C1 [Borovikov, D.; Tenishev, V.; Gombosi, T. I.] Univ Michigan, Dept Climate & Space Sci & Engn, 2455 Hayward St, Ann Arbor, MI 48104 USA.
[Guidoni, S. E.] Catholic Univ Amer, 620 Michigan Ave Northeast, Washington, DC 20064 USA.
[Guidoni, S. E.; DeVore, C. R.; Karpen, J. T.; Antiochos, S. K.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
RP Borovikov, D (reprint author), Univ Michigan, Dept Climate & Space Sci & Engn, 2455 Hayward St, Ann Arbor, MI 48104 USA.
RI Gombosi, Tamas/G-4238-2011;
OI Gombosi, Tamas/0000-0001-9360-4951; Borovikov,
Dmitry/0000-0002-0151-7437
FU National Science Foundation [AGS-1322543, PHY-1513379]; NASA
[NNX13AG25G]; European Union [637302]
FX The work performed at the University of Michigan was partially supported
by National Science Foundation grants AGS-1322543 and PHY-1513379, NASA
grant NNX13AG25G, the European Union's Horizon 2020 research and
innovation program under grant agreement No 637302 PROGRESS. We would
also like to acknowledge high-performance computing support from
Pleiades operated by NASA's Advanced Super-computing Division.
NR 25
TC 0
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U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2017
VL 835
IS 1
AR 48
DI 10.3847/1538-4357/835/1/48
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EJ8DO
UT WOS:000393455400048
ER
PT J
AU Knizhnik, KJ
Antiochos, SK
DeVore, CR
AF Knizhnik, K. J.
Antiochos, S. K.
DeVore, C. R.
TI THE ROLE OF MAGNETIC HELICITY IN STRUCTURING THE SOLAR CORONA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona; Sun: filaments; prominences; Sun: magnetic fields
ID DRIVEN VORTEX FLOWS; ACTIVE REGIONS; FILAMENT CHANNEL; QUIET-SUN;
FIELDS; CONDENSATION; ENERGY; LOOPS; RECONNECTION; ATMOSPHERE
AB Two of the most widely observed and striking features of the Sun 's magnetic field are coronal loops, which are smooth and laminar, and prominences or filaments, which are strongly sheared. Loops are puzzling because they show little evidence of tangling or braiding, at least on the quiet Sun, despite the chaotic nature of the solar surface convection. Prominences are mysterious because the origin of their underlying magnetic structure-filament channels-is poorly understood at best. These two types of features would seem to be quite unrelated and wholly distinct. We argue that, on the contrary, they are inextricably linked and result from a single process: the injection of magnetic helicity into the corona by photospheric motions and the subsequent evolution of this helicity by coronal reconnection. In this paper, we present numerical simulations of the response of a Parker (1972) corona to photospheric driving motions that have varying degrees of helicity preference. We obtain four main conclusions: (1) in agreement with the helicity condensation model of Antiochos (2013), the inverse cascade of helicity by magnetic reconnection in the corona results in the formation of filament channels localized about polarity inversion lines; (2) this same process removes most complex fine structure from the rest of the corona, resulting in smooth and laminar coronal loops; (3) the amount of remnant tangling in coronal loops is inversely dependent on the net helicity injected by the driving motions; and (4) the structure of the solar corona depends only on the helicity preference of the driving motions and not on their detailed time dependence. We discuss the implications of our results for high-resolution observations of the corona.
C1 [Knizhnik, K. J.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21287 USA.
[Knizhnik, K. J.; Antiochos, S. K.; DeVore, C. R.] NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Knizhnik, KJ (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21287 USA.; Knizhnik, KJ (reprint author), NASA, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
FU NASA Earth and Space Science Fellowship; NASA's Center for Climate
Simulation; NASA's Living With a Star and Heliophysics Supporting
Research programs
FX K.J.K. acknowledges the use of post-processing codes originally written
by Benjamin Lynch and Peter Wyper. K.J.K. received funding for this work
through a NASA Earth and Space Science Fellowship. The numerical
simulations were performed under a grant of High-End Computing resources
to C.R.D. at NASA's Center for Climate Simulation. S.K.A. and C.R.D.
were supported, in part, by grants from NASA's Living With a Star and
Heliophysics Supporting Research programs.
NR 50
TC 0
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U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2017
VL 835
IS 1
AR 85
DI 10.3847/1538-4357/835/1/85
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EJ8DO
UT WOS:000393455400085
ER
PT J
AU Kuhar, M
Krucker, S
Hannah, IG
Glesener, L
Saint-Hilaire, P
Grefenstette, BW
Hudson, HS
White, SM
Smith, DM
Marsh, AJ
Wright, PJ
Boggs, SE
Christensen, FE
Craig, WW
Hailey, CJ
Harrison, FA
Stern, D
Zhang, WW
AF Kuhar, Matej
Krucker, Sam
Hannah, Iain G.
Glesener, Lindsay
Saint-Hilaire, Pascal
Grefenstette, Brian W.
Hudson, Hugh S.
White, Stephen M.
Smith, David M.
Marsh, Andrew J.
Wright, Paul J.
Boggs, Steven E.
Christensen, Finn E.
Craig, William W.
Hailey, Charles J.
Harrison, Fiona A.
Stern, Daniel
Zhang, William W.
TI EVIDENCE OF SIGNIFICANT ENERGY INPUT IN THE LATE PHASE OF A SOLAR FLARE
FROM NuSTAR X-RAY OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: flares; Sun: particle emission; Sun: X-rays; gamma rays
ID ACTIVE CORONAL PHENOMENA; ULTRAVIOLET LATE-PHASE; YOHKOH SXT IMAGES;
GIANT ARCHES; ATOMIC DATABASE; MASS EJECTION; EMISSION; REGIONS; RHESSI;
RECONNECTION
AB We present observations of the occulted active region AR 12222 during the third Nuclear Spectroscopic Telescope ARray (NuSTAR) solar campaign on 2014 December 11, with concurrent Solar Dynamics Observatory (SDO)/AIA and FOXSI-2 sounding rocket observations. The active region produced a medium-size solar flare 1 day before the observations, at similar to 18 UT on 2014 December 10, with the post-flare loops still visible at the time of NuSTAR observations. The time evolution of the source emission in the SDO/AIA 335 angstrom channel reveals the characteristics of an extreme-ultraviolet late-phase event, caused by the continuous formation of new post-flare loops that arch higher and higher in the solar corona. The spectral fitting of NuSTAR observations yields an isothermal source, with temperature 3.8-4.6 MK, emission measure (0.3-1.8)x 10(46) cm(-3), and density estimated at (2.5-6.0) x 10(8) cm(-3). The observed AIA fluxes are consistent with the derived NuSTAR temperature range, favoring temperature values in the range of 4.0-4.3 MK. By examining the post-flare loops' cooling times and energy content, we estimate that at least 12 sets of post-flare loops were formed and subsequently cooled between the onset of the flare and NuSTAR observations, with their total thermal energy content an order of magnitude larger than the energy content at flare peak time. This indicates that the standard approach of using only the flare peak time to derive the total thermal energy content of a flare can lead to a large underestimation of its value.
C1 [Kuhar, Matej; Krucker, Sam] Univ Appl Sci & Arts Northwestern Switzerland, Bahnhofstr 6, CH-5210 Windisch, Switzerland.
[Kuhar, Matej] ETH, Inst Particle Phys, CH-8093 Zurich, Switzerland.
[Krucker, Sam; Saint-Hilaire, Pascal; Hudson, Hugh S.; Boggs, Steven E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Hannah, Iain G.; Wright, Paul J.] Univ Glasgow, SUPA Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland.
[Glesener, Lindsay] Univ Minnesota Twin Cities, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Grefenstette, Brian W.; Harrison, Fiona A.] CALTECH, Cahill Ctr Astrophys, 1216 E Calif Blvd, Pasadena, CA 91125 USA.
[Hudson, Hugh S.] Univ Glasgow, Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland.
[White, Stephen M.] Air Force Res Lab, Albuquerque, NM USA.
[Smith, David M.; Marsh, Andrew J.] Univ Calif Santa Cruz, Dept Phys, 1156 High St, Santa Cruz, CA 95064 USA.
[Smith, David M.; Marsh, Andrew J.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, 1156 High St, Santa Cruz, CA 95064 USA.
[Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, Elektrovej 327, DK-2800 Lyngby, Denmark.
[Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Kuhar, M (reprint author), Univ Appl Sci & Arts Northwestern Switzerland, Bahnhofstr 6, CH-5210 Windisch, Switzerland.; Kuhar, M (reprint author), ETH, Inst Particle Phys, CH-8093 Zurich, Switzerland.
RI Hannah, Iain/F-1972-2011;
OI Hannah, Iain/0000-0003-1193-8603; Hudson, Hugh/0000-0001-5685-1283;
Glesener, Lindsay/0000-0001-7092-2703; Wright, Paul/0000-0001-9021-611X;
White, Stephen/0000-0002-8574-8629; Kuhar, Matej/0000-0002-7210-180X
FU NASA [NNX12AJ36G, NNX14AG07G]; Swiss National Science Foundation
[200021-140308]; NASA Earth and Space Science Fellowship [NNX13AM41H];
Royal Society University Research Fellowship; EPSRC-Royal Society
fellowship engagement grant; NASA LCAS grant [NNX11AB75G]
FX This work made use of data from the NuSTAR mission, a project led by the
California Institute of Technology, managed by the Jet Propulsion
Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software
and Calibration teams for support with the execution and analysis of
these observations. This research made use of the NuSTAR Data Analysis
Software (NuSTARDAS), jointly developed by the ASI Science Data Center
(ASDC, Italy) and the California Institute of Technology (USA). M.K. and
S.K. acknowledge funding from the Swiss National Science Foundation
(200021-140308). Funding for this work was also provided under NASA
grants NNX12AJ36G and NNX14AG07G. A.J.M.'s participation was supported
by NASA Earth and Space Science Fellowship award NNX13AM41H. I.G.H. is
supported by a Royal Society University Research Fellowship. P.J.W. is
supported by an EPSRC-Royal Society fellowship engagement grant. FOXSI
was funded by NASA LCAS grant NNX11AB75G. We would also like to thank
the anonymous referee for the helpful comments.
NR 37
TC 0
Z9 0
U1 2
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2017
VL 835
IS 1
AR 6
DI 10.3847/1538-4357/835/1/6
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EJ8DO
UT WOS:000393455400006
ER
PT J
AU LaMassa, SM
Yaqoob, T
Levenson, NA
Boorman, P
Heckman, TM
Gandhi, P
Rigby, JR
Urry, CM
Ptak, AF
AF LaMassa, Stephanie M.
Yaqoob, Tahir
Levenson, N. A.
Boorman, Peter
Heckman, Timothy M.
Gandhi, Poshak
Rigby, Jane R.
Urry, C. Megan
Ptak, Andrew F.
TI CHANDRA REVEALS HEAVY OBSCURATION AND CIRCUMNUCLEAR STAR FORMATION IN
SEYFERT 2 GALAXY NGC 4968
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (NGC 4968); galaxies: Seyfert;
galaxies: star formation; X-rays: galaxies; X-rays: individual (NGC
4968)
ID ACTIVE GALACTIC NUCLEI; ULTRALUMINOUS INFRARED GALAXIES; X-RAY
LUMINOSITY; AGN DUSTY TORI; SILICATE ABSORPTION; STARBURST DISKS; LOCAL
UNIVERSE; EVOLUTION; EMISSION; SAMPLE
AB We present the Chandra imaging and spectral analysis of NGC 4968, a nearby (z = 0.00986) Seyfert 2 galaxy. We discover extended (similar to 1 kpc) X-ray emission in the soft band (0.5 - 2 keV) that is neither coincident with the narrow line region nor the extended radio emission. Based on spectral modeling, it is linked to on-going star formation (similar to 2.6-4 M-circle dot yr(-1)). The soft emission at circumnuclear scales (inner similar to 400 pc) originates from hot gas, with kT similar to 0.7 keV, while the most extended thermal emission is cooler (kT similar to 0.3 keV). We refine previous measurements of the extreme Fe K alpha equivalent width in this source (EW = 2.5(-1.0)(+2.6) keV), which suggests the central engine is completely embedded within Compton-thick levels of obscuration. Using physically motivated models fit to the Chandra spectrum, we derive a Compton-thick column density (N-H>1.25x10(24) cm(-2)) and an intrinsic hard (2-10 keV) X-ray luminosity of similar to 3-8x10(42) erg s(-1) (depending on the presumed geometry of the obscurer), which is over two orders of magnitude larger than that observed. The large Fe K alpha EW suggests a spherical covering geometry, which could be confirmed with X-ray measurements above 10 keV. NGC 4968 is similar to other active galaxies that exhibit extreme Fe K alpha EWs (i.e., >2 keV) in that they also contain ongoing star formation. This work supports the idea that gas associated with nuclear star formation may increase the covering factor of the enshrouding gas and play a role in obscuring AGN
C1 [LaMassa, Stephanie M.; Rigby, Jane R.; Ptak, Andrew F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yaqoob, Tahir] Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
[Levenson, N. A.] Gemini Observ, Casilla 603, La Serena, Chile.
[Boorman, Peter; Gandhi, Poshak] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Heckman, Timothy M.] Johns Hopkins Univ, Dept Phys & Astron, 3400 North Chales St, Baltimore, MD 21218 USA.
[Urry, C. Megan] Yale Ctr Astron & Astrophys, Dept Phys, POB 208120, New Haven, CT 06520 USA.
RP LaMassa, SM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
OI Levenson, Nancy A./0000-0003-4209-639X; Urry, Meg/0000-0002-0745-9792
FU National Aeronautics and Space Administration through Chandra Award
[GO5-16112X]; National Aeronautics Space Administration [NAS8-03060];
Gemini Observatory; STFC [ST/J003697/2]
FX We thank the referee for a thorough reading of this manuscript and for
providing constructive comments. Support for this work was provided by
the National Aeronautics and Space Administration through Chandra Award
Number GO5-16112X issued by the Smithsonian Astrophysical Observatory
for and on behalf of the National Aeronautics Space Administration under
contract NAS8-03060. S.M.L. is supported by an appointment to the NASA
Postdoctoral Program at the NASA Goddard Space Flight Center,
administered by Universities Space Research Association under contract
with NASA. N.A.L.. is supported by the Gemini Observatory, which is
operated by the Association of Universities for Research in Astronomy,
Inc., on behalf of the international Gemini partnership of Argentina,
Brazil, Canada, Chile, and the United States of America. P.B. and P.G.
thank STFC for support (trant reference ST/J003697/2).
NR 67
TC 0
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U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2017
VL 835
IS 1
AR 91
DI 10.3847/1538-4357/835/1/91
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EJ8DO
UT WOS:000393455400091
ER
PT J
AU Lindberg, JE
Charnley, SB
Jorgensen, JK
Cordiner, MA
Bjerkeli, P
AF Lindberg, Johan E.
Charnley, Steven B.
Jorgensen, Jes K.
Cordiner, Martin A.
Bjerkeli, Per
TI EXTERNALLY HEATED PROTOSTELLAR CORES IN THE OPHIUCHUS STAR-FORMING
REGION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; ISM: individual objects (Ophiuchus); ISM: molecules;
radiative transfer; stars: formation
ID LOW-MASS PROTOSTARS; MOLECULAR CLOUDS; DARK CLOUD; COMPARATIVE
CHEMISTRY; CORONA AUSTRALIS; SUBMILLIMETER; ENVELOPES; CH3OH; H2CO;
DESORPTION
AB We present APEX 218. GHz observations of molecular emission in a complete sample of embedded protostars in the Ophiuchus star-forming region. To study the physical properties of the cores, we calculate H2CO and c-C3H2 rotational temperatures, both of which are good tracers of the kinetic temperature of the molecular gas. We find that the H2CO temperatures range between 16. K and 124. K, with the highest H2CO temperatures toward the hot corino source IRAS. 16293-2422 (69-124 K) and the sources in the.. Oph. A cloud (23-49 K) located close to the luminous Herbig. Be star S1, which externally irradiates the.. Oph. A cores. On the other hand, the c-C3H2 rotational temperature is consistently low (7-17 K) in all sources. Our results indicate that the c-C3H2 emission is primarily tracing more shielded parts of the envelope whereas the H2CO emission (at the angular scale of the APEX beam; 3600 au in Ophiuchus) mainly traces the outer irradiated envelopes, apart from in IRAS. 16293-2422, where the hot corino emission dominates. In some sources, a secondary velocity component is also seen, possibly tracing the molecular outflow.
C1 [Lindberg, Johan E.; Charnley, Steven B.; Cordiner, Martin A.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Mail Code 691,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Jorgensen, Jes K.; Bjerkeli, Per] Univ Copenhagen, Ctr Star & Planet Format, Niels Bohr Inst, Oster Voldgade 5-7, DK-1350 Copenhagen, Denmark.
[Jorgensen, Jes K.; Bjerkeli, Per] Univ Copenhagen, Nat Hist Museum Denmark, Oster Voldgade 5-7, DK-1350 Copenhagen, Denmark.
[Cordiner, Martin A.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Bjerkeli, Per] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden.
RP Lindberg, JE (reprint author), NASA, Goddard Space Flight Ctr, Astrochem Lab, Mail Code 691,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM johan.lindberg@nasa.gov
OI Jorgensen, Jes Kristian/0000-0001-9133-8047
FU NASA's Emerging Worlds Program; NASA
FX This research was supported by NASA's Emerging Worlds Program and by an
appointment to the NASA Postdoctoral Program at the NASA Goddard Space
Flight Center to J.E.L., administered by the Universities Space Research
Association through a contract with NASA. We thank the anonymous referee
for insightful comments and suggestions, which helped us improve the
manuscript.
NR 45
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2017
VL 835
IS 1
AR 3
DI 10.3847/1538-4357/835/1/3
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EJ8DO
UT WOS:000393455400003
ER
PT J
AU Malhotra, S
Rhoads, JE
Finkelstein, K
Yang, H
Carilli, C
Combes, F
Dassas, K
Finkelstein, S
Frye, B
Gerin, M
Guillard, P
Nesvadba, N
Rigby, J
Shin, MS
Spaans, M
Strauss, MA
Papovich, C
AF Malhotra, Sangeeta
Rhoads, James E.
Finkelstein, K.
Yang, Huan
Carilli, Chris
Combes, Francoise
Dassas, Karine
Finkelstein, Steven
Frye, Brenda
Gerin, Maryvonne
Guillard, Pierre
Nesvadba, Nicole
Rigby, Jane
Shin, Min-Su
Spaans, Marco
Strauss, Michael A.
Papovich, Casey
TI HERSCHEL EXTREME LENSING LINE OBSERVATIONS: [C II] VARIATIONS IN
GALAXIES AT REDSHIFTS z=1-3
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: ISM; ISM: atoms; galaxies: high-redshift; radiation
mechanisms: thermal
ID STAR-FORMING GALAXIES; 158 MU-M; POLYCYCLIC AROMATIC-HYDROCARBONS;
ULTRALUMINOUS INFRARED GALAXIES; SIMILAR-TO 2.5; PHOTODISSOCIATION
REGIONS; INTERSTELLAR-MEDIUM; MOLECULAR GAS; VIRGO CLUSTER; MIDINFRARED
SPECTROSCOPY
AB We observed the [C II] line in 15 lensed galaxies at redshifts 1 < z <. 3 using HIFI on the Herschel Space Observatory and detected 14/15 galaxies at 3 sigma or better. High magnifications enable even modestly luminous galaxies to be detected in [C II] with Herschel. The [C II] luminosity in this sample ranges from 8x10(7) L-circle dot to 3.7x10(9) L-circle dot (after correcting for magnification), confirming that [C II] is a strong tracer of the ISM at high redshifts. The ratio of the [C II] line to the total far-infrared (FIR) luminosity serves as a measure of the ratio of gas to dust cooling and thus the efficiency of the grain photoelectric heating process. It varies between 3.3% and 0.09%. We compare the [C II]/FIR ratio to that of galaxies at z = 0 and at high redshifts and find that they follow similar trends. The [C II]/FIR ratio is lower for galaxies with higher dust temperatures. This is best explained if increased UV intensity leads to higher FIR luminosity and dust temperatures, but gas heating does not rise due to lower photoelectric heating efficiency. The [C II]/FIR ratio shows weaker correlation with FIR luminosity. At low redshifts highly luminous galaxies tend to have warm dust, so the effects of dust temperature and luminosity are degenerate. Luminous galaxies at high redshifts show a range of dust temperatures, showing that [C II]/FIR correlates most strongly with dust temperature. The [C II] to mid-IR ratio for the HELLO sample is similar to the values seen for low-redshift galaxies, indicating that small grains and PAHs dominate the heating in the neutral ISM, although some of the high [CII]/FIR ratios may be due to turbulent heating.
C1 [Malhotra, Sangeeta; Rhoads, James E.; Yang, Huan] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Finkelstein, K.; Finkelstein, Steven] Univ Texas Austin, Austin, TX 78712 USA.
[Carilli, Chris] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Combes, Francoise] CNRS, LERMA, Observ Paris, 61 Ave Observ, F-75014 Paris, France.
[Dassas, Karine; Guillard, Pierre; Nesvadba, Nicole] Ctr Univ Orsay, Inst Astrophys Spatiale, Orsay, France.
[Frye, Brenda] Univ Arizona, Steward Observ, Tucson, AZ USA.
[Gerin, Maryvonne] LERMA, 24 Rue Lhomond, F-75231 Paris 05, France.
[Rigby, Jane] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Shin, Min-Su] Univ Oxford, Oxford OX1 3PA, England.
[Spaans, Marco] Univ Groningen, Kapteyn Astron Inst, Groningen, Netherlands.
[Strauss, Michael A.] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA.
[Papovich, Casey] Texas A&M Univ, Dept Phys, George P & Cynthia W Mitchell Inst Fundamental Ph, College Stn, TX 77843 USA.
RP Malhotra, S (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
EM malhotra@asu.edu
OI Combes, Francoise/0000-0003-2658-7893
FU NASA through Herschel GO funding
FX Herschel is an ESA space observatory with science instruments provided
by European-led Principal Investigator consortia and with important
participation from NASA. We are grateful to the DARK Cosmology Centre in
Copenhagen, Denmark; Nordea Fonden in Copenhagen; the Institute for
Advanced Study in Princeton, NJ; and Princeton University's Department
of Astrophysical Sciences for their hospitality during the completion of
this work. We thank the staff at the NASA Herschel Science Center, and
Adwin Boogert in particular, for their assistance and guidance with HIFI
data. The authors would like to thank Gordon Stacey for discussions, the
referee for careful readings of the manuscript, and the editor for their
patience. This work has been supported by NASA through Herschel GO
funding.
NR 83
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2017
VL 835
IS 1
AR 110
DI 10.3847/1538-4357/835/1/110
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EJ8DO
UT WOS:000393455400110
ER
PT J
AU Posselt, B
Pavlov, GG
Slane, PO
Romani, R
Bucciantini, N
Bykov, AM
Kargaltsev, O
Weisskopf, MC
Ng, CY
AF Posselt, B.
Pavlov, G. G.
Slane, P. O.
Romani, R.
Bucciantini, N.
Bykov, A. M.
Kargaltsev, O.
Weisskopf, M. C.
Ng, C-Y
TI GEMINGA'S PUZZLING PULSAR WIND NEBULA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: individual (Geminga); stars: neutron
ID SPIN-VELOCITY ALIGNMENT; GAMMA-RAY PULSAR; GALACTIC PLANE IPHAS; BAND
X-RAY; BOW-SHOCK; PARTICLE-ACCELERATION; INTERSTELLAR-MEDIUM;
CROSS-SECTIONS; PSR J1741-2054; DATA RELEASE
AB We report on six new Chandra observations of the Geminga pulsar wind nebula (PWN). The PWN consists of three distinct elongated structures-two approximate to 0.2d(250) pc long lateral tails and a segmented axial tail of approximate to 0.05d(250) pc length, where d(250) = d/(250 pc). The photon indices of the power-law spectra of the lateral tails, Gamma approximate to 1, are lsignificantly harder than those of the pulsar (Gamma approximate to 1.5) and the axial tail (Gamma approximate to 1.6). There is no significant diffuse X-ray emission between the lateral tails-the ratio of the X-ray surface brightness between the south tail and this sky area is at least 12. The lateral tails apparently connect directly to the pulsar and show indications of moving footpoints. The axial tail comprises time-variable emission blobs. However, there is no evidence for constant or decelerated outward motion of these blobs. Different physical models are consistent with the observed morphology and spectra of the Geminga PWN. In one scenario, the lateral tails could represent an azimuthally asymmetric shell whose hard emission is caused by the Fermi acceleration mechanism of colliding winds. In another scenario, the lateral tails could be luminous, bent polar outflows, while the blobs in the axial tail could represent a crushed torus. In a resemblance to planetary magnetotails, the blobs of the axial tail might also represent short-lived plasmoids, which are formed by magnetic field reconnection in the relativistic plasma of the pulsar wind tail.
C1 [Posselt, B.; Pavlov, G. G.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
[Slane, P. O.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Romani, R.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Bucciantini, N.] INAF Osservatorio Astrofis Arcetri, Lgo E Fermi 5, I-50125 Florence, Italy.
[Bucciantini, N.] INFN Sez Firenze, Via G Sansone 1, I-50019 Florence, Italy.
[Bykov, A. M.] St Petersburg State Politech Univ, AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia.
[Bykov, A. M.] Int Space Sci Inst, Bern, Switzerland.
[Kargaltsev, O.] George Washington Univ, Dept Phys, 725 21st St NW, Washington, DC 20052 USA.
[Weisskopf, M. C.] NASA, Marshall Space Flight Ctr, ZP12,320 Sparkman Dr, Huntsville, AL 35805 USA.
[Ng, C-Y] Univ Hong Kong, Dept Phys, Pokfulam Rd, Hong Kong, Hong Kong, Peoples R China.
RP Posselt, B (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
EM posselt@psu.edu
OI /0000-0002-5847-2612; Posselt, Bettina/0000-0003-2317-9747
FU National Aeronautics and Space Administration through Chandra Award
[G03-14057]; National Aeronautics Space Administration [NAS8-03060];
National Aeronautics and Space Administration [NNX15AF10G]; RSF grant
[16-12-10225]
FX Support for this work was provided by the National Aeronautics and Space
Administration through Chandra Award Number G03-14057 issued by the
Chandra X-ray Observatory Center, which is operated by the Smithsonian
Astrophysical Observatory for and on behalf of the National Aeronautics
Space Administration under contract NAS8-03060. This work was also
partly supported by the National Aeronautics and Space Administration
under Grant Number NNX15AF10G issued through the Astrophysics Data
Analysis Program. A.M.B. acknowledges support from RSF grant
16-12-10225.
NR 68
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U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2017
VL 835
IS 1
AR 66
DI 10.3847/1538-4357/835/1/66
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EJ8DO
UT WOS:000393455400066
ER
PT J
AU Racusin, JL
Burns, E
Goldstein, A
Connaughton, V
Wilson-Hodge, CA
Jenke, P
Blackburn, L
Briggs, MS
Broida, J
Camp, J
Christensen, N
Hui, CM
Littenberg, T
Shawhan, P
Singer, L
Veitch, J
Bhat, PN
Cleveland, W
Fitzpatrick, G
Gibby, MH
von Kienlin, A
McBreen, S
Mailyan, B
Meegan, CA
Paciesas, WS
Preece, RD
Roberts, OJ
Stanbro, M
Veres, P
Zhang, BB
Ackermann, M
Albert, A
Atwood, WB
Axelsson, M
Baldini, L
Ballet, J
Barbiellini, G
Baring, MG
Bastieri, D
Bellazzini, R
Bissaldi, E
Blandford, RD
Bloom, ED
Bonino, R
Bregeon, J
Bruel, P
Buson, S
Caliandro, GA
Cameron, RA
Caputo, R
Caragiulo, M
Caraveo, PA
Cavazzuti, E
Charles, E
Chiang, J
Ciprini, S
Costanza, F
Cuoco, A
Cutini, S
D'Ammando, F
de Palma, F
Desiante, R
Digel, SW
Di Lalla, N
Di Mauro, M
Di Venere, L
Drell, PS
Favuzzi, C
Ferrara, EC
Focke, WB
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Giglietto, N
Gill, R
Giroletti, M
Glanzman, T
Granot, J
Green, D
Grove, JE
Guillemot, L
Guiriec, S
Harding, AK
Jogler, T
Johannesson, G
Kamae, T
Kensei, S
Kocevski, D
Kuss, M
Larsson, S
Latronico, L
Li, J
Longo, F
Loparco, F
Lubrano, P
Magill, JD
Maldera, S
Malyshev, D
Mazziotta, MN
McEnery, JE
Michelson, PF
Mizuno, T
Monzani, ME
Morselli, A
Moskalenko, IV
Negro, M
Nuss, E
Omodei, N
Orienti, M
Orlando, E
Ormes, JF
Paneque, D
Perkins, JS
Pesce-Rollins, M
Piron, F
Pivato, G
Porter, TA
Principe, G
Raino, S
Rando, R
Razzano, M
Razzaque, S
Reimer, A
Reimer, O
Parkinson, PMS
Scargle, JD
Sgro, C
Simone, D
Siskind, EJ
Smith, DA
Spada, F
Spinelli, P
Suson, DJ
Tajima, H
Thayer, JB
Torres, DF
Troja, E
Uchiyama, Y
Vianello, G
Wood, KS
Wood, M
AF Racusin, J. L.
Burns, E.
Goldstein, A.
Connaughton, V.
Wilson-Hodge, C. A.
Jenke, P.
Blackburn, L.
Briggs, M. S.
Broida, J.
Camp, J.
Christensen, N.
Hui, C. M.
Littenberg, T.
Shawhan, P.
Singer, L.
Veitch, J.
Bhat, P. N.
Cleveland, W.
Fitzpatrick, G.
Gibby, M. H.
von Kienlin, A.
McBreen, S.
Mailyan, B.
Meegan, C. A.
Paciesas, W. S.
Preece, R. D.
Roberts, O. J.
Stanbro, M.
Veres, P.
Zhang, B. -B.
Ackermann, M.
Albert, A.
Atwood, W. B.
Axelsson, M.
Baldini, L.
Ballet, J.
Barbiellini, G.
Baring, M. G.
Bastieri, D.
Bellazzini, R.
Bissaldi, E.
Blandford, R. D.
Bloom, E. D.
Bonino, R.
Bregeon, J.
Bruel, P.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caputo, R.
Caragiulo, M.
Caraveo, P. A.
Cavazzuti, E.
Charles, E.
Chiang, J.
Ciprini, S.
Costanza, F.
Cuoco, A.
Cutini, S.
D'Ammando, F.
de Palma, F.
Desiante, R.
Digel, S. W.
Di Lalla, N.
Di Mauro, M.
Di Venere, L.
Drell, P. S.
Favuzzi, C.
Ferrara, E. C.
Focke, W. B.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Giglietto, N.
Gill, R.
Giroletti, M.
Glanzman, T.
Granot, J.
Green, D.
Grove, J. E.
Guillemot, L.
Guiriec, S.
Harding, A. K.
Jogler, T.
Johannesson, G.
Kamae, T.
Kensei, S.
Kocevski, D.
Kuss, M.
Larsson, S.
Latronico, L.
Li, J.
Longo, F.
Loparco, F.
Lubrano, P.
Magill, J. D.
Maldera, S.
Malyshev, D.
Mazziotta, M. N.
McEnery, J. E.
Michelson, P. F.
Mizuno, T.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Negro, M.
Nuss, E.
Omodei, N.
Orienti, M.
Orlando, E.
Ormes, J. F.
Paneque, D.
Perkins, J. S.
Pesce-Rollins, M.
Piron, F.
Pivato, G.
Porter, T. A.
Principe, G.
Raino, S.
Rando, R.
Razzano, M.
Razzaque, S.
Reimer, A.
Reimer, O.
Parkinson, P. M. Saz
Scargle, J. D.
Sgro, C.
Simone, D.
Siskind, E. J.
Smith, D. A.
Spada, F.
Spinelli, P.
Suson, D. J.
Tajima, H.
Thayer, J. B.
Torres, D. F.
Troja, E.
Uchiyama, Y.
Vianello, G.
Wood, K. S.
Wood, M.
CA LAT Collaboration
TI SEARCHING THE GAMMA-RAY SKY FOR COUNTERPARTS TO GRAVITATIONAL WAVE
SOURCES: FERMI GAMMA-RAY BURST MONITOR. AND LARGE AREA TELESCOPE
OBSERVATIONS OF LVT151012 AND GW151226
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma rays: general; gravitational waves; methods: observational
ID EVENT GW150914; ELECTROMAGNETIC COUNTERPARTS; SPECTRAL CATALOG;
NEUTRON-STAR; GEV EMISSION; FOLLOW-UP; LIGO; TRANSIENTS; AFTERGLOW;
MERGERS
AB We present the Fermi Gamma-ray Burst Monitor (GBM) and Large Area Telescope (LAT) observations of the LIGO binary black hole merger event GW151226 and candidate LVT151012. At the time of the LIGO triggers on LVT151012 and GW151226, GBM was observing 68% and 83% of the localization regions, and LAT was observing 47% and 32%, respectively. No candidate electromagnetic counterparts were detected by either the GBM or LAT. We present a detailed analysis of the GBM and LAT data over a range of timescales from seconds to years, using automated pipelines and new techniques for characterizing the flux upper bounds across large areas of the sky. Due to the partial GBM and LAT coverage of the large LIGO localization regions at the trigger times for both events, differences in source distances and masses, as well as the uncertain degree to which emission from these sources could be beamed, these non-detections cannot be used to constrain the variety of theoretical models recently applied to explain the candidate GBM counterpart to GW150914.
C1 [Racusin, J. L.; Camp, J.; Singer, L.; Buson, S.; Ferrara, E. C.; Green, D.; Guiriec, S.; Harding, A. K.; Kocevski, D.; McEnery, J. E.; Perkins, J. S.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Burns, E.] Univ Alabama, Dept Phys, 320 Sparkman Dr, Huntsville, AL 35805 USA.
[Goldstein, A.; Connaughton, V.; Littenberg, T.; Cleveland, W.; Paciesas, W. S.] Univ Space Res Assoc, 320 Sparkman Dr, Huntsville, AL 35806 USA.
[Wilson-Hodge, C. A.; Hui, C. M.] NASA, Astrophys Off, Marshall Space Flight Ctr, ZP12, Huntsville, AL 35812 USA.
[Jenke, P.; Briggs, M. S.; Bhat, P. N.; Mailyan, B.; Meegan, C. A.; Veres, P.; Zhang, B. -B.] Univ Alabama, CSPAR, 320 Sparkman Dr, Huntsville, AL 35805 USA.
[Blackburn, L.] MIT, LIGO, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Briggs, M. S.; Preece, R. D.; Stanbro, M.] Univ Alabama, Dept Space Sci, 320 Sparkman Dr, Huntsville, AL 35805 USA.
[Broida, J.; Christensen, N.] Carleton Coll, Phys & Astron, Northfield, MN 55057 USA.
[Shawhan, P.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Veitch, J.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England.
[Fitzpatrick, G.; McBreen, S.; Roberts, O. J.] Univ Coll Dublin, Sch Phys, Stillorgan Rd, Dublin 4, Ireland.
[Gibby, M. H.] Jacobs Technol Inc, Huntsville, AL USA.
[von Kienlin, A.] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany.
[Zhang, B. -B.] CSIC, Inst Astrofis Andalucia, POB 03004, E-18080 Granada, Spain.
[Ackermann, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Albert, A.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Atwood, W. B.; Caputo, R.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Atwood, W. B.; Caputo, R.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Axelsson, M.; Larsson, S.] KTH Royal Inst Technol, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Axelsson, M.] Tokyo Metropolitan Univ, Dept Phys, Minami Osawa 1-1, Hachioji, Tokyo 1920397, Japan.
[Baldini, L.] Univ Pisa, I-56127 Pisa, Italy.
[Baldini, L.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Ballet, J.] Univ Paris Diderot, CNRS, Lab AIM, CEA,IRFU,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France.
[Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Baring, M. G.] Rice Univ, Dept Phys & Astron, MS-108,POB 1892, Houston, TX 77251 USA.
[Bastieri, D.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy.
[Bellazzini, R.; Di Lalla, N.; Kuss, M.; Pesce-Rollins, M.; Pivato, G.; Razzano, M.; Sgro, C.; Spada, F.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Bissaldi, E.; Caragiulo, M.; Costanza, F.; de Palma, F.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Simone, D.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Blandford, R. D.; Bloom, E. D.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Digel, S. W.; Di Mauro, M.; Drell, P. S.; Focke, W. B.; Glanzman, T.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Omodei, N.; Orlando, E.; Porter, T. A.; Reimer, A.; Reimer, O.; Tajima, H.; Thayer, J. B.; Vianello, G.; Wood, M.] Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Blandford, R. D.; Bloom, E. D.; Caliandro, G. A.; Cameron, R. A.; Charles, E.; Chiang, J.; Digel, S. W.; Di Mauro, M.; Drell, P. S.; Focke, W. B.; Glanzman, T.; Michelson, P. F.; Monzani, M. E.; Moskalenko, I. V.; Omodei, N.; Orlando, E.; Porter, T. A.; Reimer, A.; Reimer, O.; Tajima, H.; Thayer, J. B.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Bonino, R.; Cuoco, A.; Desiante, R.; Latronico, L.; Maldera, S.; Negro, M.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Bonino, R.; Negro, M.] Univ Turin, Dipartimento Fis, I-10125 Turin, Italy.
[Bregeon, J.; Nuss, E.; Piron, F.] Univ Montpellier, CNRS, IN2P3, Lab Univers & Particules Montpellier, F-34095 Montpellier, France.
[Bruel, P.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Caliandro, G. A.] CIFS, I-10133 Turin, Italy.
[Caragiulo, M.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Loparco, F.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Caragiulo, M.; Di Venere, L.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Loparco, F.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy.
[Caraveo, P. A.] Ist Astrofis Spaziale & Fis Cosm Milano, INAF, Via E Bassini 15, I-20133 Milan, Italy.
[Cavazzuti, E.; Ciprini, S.; Cutini, S.; Gasparrini, D.] ASI, Sci Data Ctr, I-00133 Rome, Italy.
[Ciprini, S.; Cutini, S.; Gasparrini, D.; Lubrano, P.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Cuoco, A.] Rhein Westfal TH Aachen, Inst Theoret Particle Phys & Cosmol TTK, D-52056 Aachen, Germany.
[D'Ammando, F.; Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[D'Ammando, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[de Palma, F.] Univ Telemat Pegaso, Piazza Trieste & Trento 48, I-80132 Naples, Italy.
[Desiante, R.] Univ Udine, I-33100 Udine, Italy.
[Fukazawa, Y.; Kensei, S.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Funk, S.; Malyshev, D.; Principe, G.] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany.
[Gill, R.; Granot, J.] Open Univ Israel, Dept Nat Sci, 1 Univ Rd,POB 808, IL-43537 Raanana, Israel.
[Green, D.; Magill, J. D.; McEnery, J. E.; Troja, E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Green, D.; Magill, J. D.; McEnery, J. E.; Troja, E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Grove, J. E.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Guillemot, L.] Univ Orleans, CNRS, Lab Phys & Chim Environm & Espace, F-45071 Orleans 02, France.
[Guillemot, L.] Observ Paris, CNRS, INSU, Stn Radioastron Nancay, F-18330 Nancay, France.
[Jogler, T.] Friedrich Alexander Univ, Schlosspl 4, D-91054 Erlangen, Germany.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Kamae, T.] Univ Tokyo, Grad Sch Sci, Dept Phys, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan.
[Larsson, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Li, J.; Torres, D. F.] CSIC, Inst Space Sci, IEEC, Campus UAB, E-08193 Barcelona, Spain.
[Mizuno, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Razzaque, S.] Univ Johannesburg, Dept Phys, POB 524, ZA-2006 Auckland Pk, South Africa.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Parkinson, P. M. Saz] Univ Hong Kong, Dept Phys, Pokfulam Rd, Hong Kong, Hong Kong, Peoples R China.
[Parkinson, P. M. Saz] Univ Hong Kong, Lab Space Res, Hong Kong, Hong Kong, Peoples R China.
[Scargle, J. D.] NASA, Div Space Sci, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Smith, D. A.] Univ Bordeaux 1, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, CNRS, BP120, F-33175 Gradignan, France.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Tajima, H.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Uchiyama, Y.] Rikkyo Univ, Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan.
[Wood, K. S.] Praxis Inc, Alexandria, VA 22303 USA.
[Wood, K. S.] Naval Res Lab, Washington, DC 20375 USA.
RP Racusin, JL (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Burns, E (reprint author), Univ Alabama, Dept Phys, 320 Sparkman Dr, Huntsville, AL 35805 USA.; Goldstein, A (reprint author), Univ Space Res Assoc, 320 Sparkman Dr, Huntsville, AL 35806 USA.; Omodei, N; Vianello, G (reprint author), Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.; Omodei, N; Vianello, G (reprint author), Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
EM judith.racusin@nasa.gov; EricKayserBurns@gmail.com;
adam.m.goldstein@nasa.gov; nicola.omodei@stanford.edu;
giacomov@stanford.edu
OI Mazziotta, Mario Nicola/0000-0001-9325-4672
FU NASA; Bundesministerium fur Bildung und Forschung (BMBF) via the
Deutsches Zentrum fur Luft und Raumfahrt (DLR) [50 QV 0301]; NASA
Postdoctoral Fellowship Program; NSF [PHY-1505373]
FX The GBM project is supported by NASA. Support for the German
contribution to GBM was provided by the Bundesministerium fur Bildung
und Forschung (BMBF) via the Deutsches Zentrum fur Luft und Raumfahrt
(DLR) under contract number 50 QV 0301. AG is funded through the NASA
Postdoctoral Fellowship Program.; NC and JB are supported by NSF grant
PHY-1505373.
NR 62
TC 0
Z9 0
U1 5
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2017
VL 835
IS 1
AR 82
DI 10.3847/1538-4357/835/1/82
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EJ8DO
UT WOS:000393455400082
ER
PT J
AU Ricci, C
Assef, RJ
Stern, D
Nikutta, R
Alexander, DM
Asmus, D
Ballantyne, DR
Bauer, FE
Blain, AW
Boggs, S
Boorman, PG
Brandt, WN
Brightman, M
Chang, CS
Chen, CTJ
Christensen, FE
Comastri, A
Craig, WW
Diaz-Santos, T
Eisenhardt, PR
Farrah, D
Gandhi, P
Hailey, CJ
Harrison, FA
Jun, HD
Koss, MJ
LaMassa, S
Lansbury, GB
Markwardt, CB
Stalevski, M
Stanley, F
Treister, E
Tsai, CW
Walton, DJ
Wu, JW
Zappacosta, L
Zhang, WW
AF Ricci, C.
Assef, R. J.
Stern, D.
Nikutta, R.
Alexander, D. M.
Asmus, D.
Ballantyne, D. R.
Bauer, F. E.
Blain, A. W.
Boggs, S.
Boorman, P. G.
Brandt, W. N.
Brightman, M.
Chang, C. S.
Chen, C. -T. J.
Christensen, F. E.
Comastri, A.
Craig, W. W.
Diaz-Santos, T.
Eisenhardt, P. R.
Farrah, D.
Gandhi, P.
Hailey, C. J.
Harrison, F. A.
Jun, H. D.
Koss, M. J.
LaMassa, S.
Lansbury, G. B.
Markwardt, C. B.
Stalevski, M.
Stanley, F.
Treister, E.
Tsai, C. -W.
Walton, D. J.
Wu, J. W.
Zappacosta, L.
Zhang, W. W.
TI NuSTAR OBSERVATIONS OF WISE J1036+0449, A GALAXY AT z similar to 1
OBSCURED BY HOT DUST
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: galaxies; galaxies: active; galaxies: evolution; galaxies:
high-redshift; quasars: general; quasars: individual (WISE J1036+0449)
ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; ULTRALUMINOUS INFRARED
GALAXIES; X-RAY-EMISSION; SPECTRAL ENERGY-DISTRIBUTIONS; DIGITAL SKY
SURVEY; SEYFERT-GALAXIES; XMM-NEWTON; HOST GALAXIES; HIGH-REDSHIFT
AB Hot dust-obscured galaxies (hot DOGs), selected from Wide-Field Infrared Survey Explorer's all-sky infrared survey, host some of the most powerful active galactic nuclei known and may represent an important stage in the evolution of galaxies. Most known hot DOGs are located at z > 1.5, due in part to a strong bias against identifying them at lower redshift related to the selection criteria. We present a new selection method that identifies 153 hot DOG candidates at z similar to 1, where they are significantly brighter and easier to study. We validate this approach by measuring a redshift z = 1.009 and finding a spectral energy distribution similar to that of higher-redshift hot DOGs for one of these objects, WISE J1036+ 0449 (L-Bol similar or equal to 8 x 10(46) erg s(-1)). We find evidence of a broadened component in Mg II, which would imply a black hole mass of M-BH similar or equal to 2 x 10(8) M-circle dot and an Eddington ratio of lambda(Edd) similar or equal to 2.7. WISE J1036+ 0449 is the first hot DOG detected by the Nuclear Spectroscopic Telescope Array, and observations show that the source is heavily obscured, with a column density of N-II similar or equal to (2-15) x 10(23)cm(-2). The source has an intrinsic 2-10 keV luminosity of similar to 6 x 10(44)erg s(-1), a value significantly lower than that expected from the mid-infrared/X-ray correlation. We also find that other hot DOGs observed by X-ray facilities show a similar deficiency of X-ray flux. We discuss the origin of the X-ray weakness and the absorption properties of hot DOGs. Hot DOGs at z <= 1 could be excellent laboratories to probe the characteristics of the accretion flow and of the X-ray emitting plasma at extreme values of the Eddington ratio.
C1 [Ricci, C.; Nikutta, R.; Bauer, F. E.; Treister, E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Casilla 306, Santiago 22, Chile.
[Ricci, C.; Bauer, F. E.; Treister, E.] EMBIGGEN Anillo, Concepcion, Chile.
[Ricci, C.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China.
[Assef, R. J.; Diaz-Santos, T.] Univ Diego Portales, Fac Ingn, Nucleo Astron, Av Ejercito Libertador 441, Santiago, Chile.
[Stern, D.; Eisenhardt, P. R.; Jun, H. D.; Tsai, C. -W.; Walton, D. J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Nikutta, R.] Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85719 USA.
[Alexander, D. M.; Lansbury, G. B.; Stanley, F.] Univ Durham, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England.
[Asmus, D.] European So Observ, Casilla 19001, Santiago 19, Chile.
[Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, 837 State St, Atlanta, GA 30332 USA.
[Bauer, F. E.] Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA.
[Bauer, F. E.] Millennium Inst Astrophys, Santiago, Chile.
[Blain, A. W.] Univ Leicester, Phys & Astron, 1 Univ Rd, Leicester LE1 7RH, Leics, England.
[Boggs, S.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Boorman, P. G.; Gandhi, P.] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Brandt, W. N.; Chen, C. -T. J.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Brandt, W. N.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Brandt, W. N.] Penn State Univ, Dept Phys, 104 Davey Lab, University Pk, PA 16802 USA.
[Brightman, M.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Chang, C. S.] Joint ALMA Observ, Alonso de Cordova 3107, Santiago, Chile.
[Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, Elektronvej 327, DK-2800 Lyngby, Denmark.
[Comastri, A.] INAF Osservatorio Astron Bologna, Via Ranzani 1, I-40127 Bologna, Italy.
[Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Koss, M. J.] ETH, Dept Phys, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.
[LaMassa, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Markwardt, C. B.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Markwardt, C. B.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Mail Code 661, Greenbelt, MD 20771 USA.
[Stalevski, M.] Univ Chile, Dept Astron, Camino El Observ 1515,Casilla 36-D, Santiago, Chile.
[Stalevski, M.] Astron Observ, Volgina 7, Belgrade 11060, Serbia.
[Stalevski, M.] Univ Ghent, Sterrenkundig Observ, Krijgslaan 281-S9, B-9000 Ghent, Belgium.
[Walton, D. J.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA.
[Wu, J. W.] Chinese Acad Sci, Natl Astron Observ, 20A Datun Rd, Beijing 100012, Peoples R China.
[Zappacosta, L.] INAF Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, RM, Italy.
RP Ricci, C (reprint author), Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Casilla 306, Santiago 22, Chile.; Ricci, C (reprint author), EMBIGGEN Anillo, Concepcion, Chile.; Ricci, C (reprint author), Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China.
EM cricci@astro.puc.cl
OI Stalevski, Marko/0000-0001-5146-8330
FU National Aeronautics and Space Administration (NASA); W.M. Keck
Foundation; NASA through Astrophysics Data Analysis Program
[13ADAP13-0092]; CONICYT-Chile grants "EMBIGGEN" Anillo ACT; FONDECYT
[1141218, 3140436, 1151408, 1151239]; Basal-CATA [PFB-06/2007]; Ministry
of Economy, Development, and Tourism's Millennium Science Initiative
[IC120009]; China-CONICYT fund; STFC [ST/J003697/2]; NuSTAR
[44A-1092750]; STFC studentship; ASI/INAF grant [I/037/12/0011/13];
Caltech Kingsley visitor program; ALMA-CONICYT project [31130005]
FX We thank the referee for a very prompt report that helped to improve the
article. This work makes use of data products from the Wide-Field
Infrared Survey Explorer, which is a joint project of the University of
California, Los Angeles, and the Jet Propulsion Laboratory/California
Institute of Technology (Caltech). WISE is funded by the National
Aeronautics and Space Administration (NASA). Some of the data presented
herein were obtained at the W.M. Keck Observatory, which is operated as
a scientific partnership between Caltech, the University of California,
and NASA. Use of the observatory was made possible by the generous
financial support of the W.M. Keck Foundation. This work makes use of
data from the NuSTAR mission, a project led by Caltech, managed by the
Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR
Operations, Software, and Calibration teams for their support with the
execution and analysis of these observations. This research has made use
of the NuSTAR Data Analysis Software, jointly developed by the ASI
Science Data Center (Italy) and Caltech. This work has made use of the
NASA/IPAC Infrared Science Archive and NASA/IPAC Extragalactic Database,
which are operated by the Jet Propulsion Laboratory, Caltech, under
contract with NASA. This material is based upon work supported by NASA
under Proposal No. 13ADAP13-0092, issued through the Astrophysics Data
Analysis Program. We thank M. Karouzos and C.S. Chang for their comments
on the manuscript. We acknowledge financial support from CONICYT-Chile
grants "EMBIGGEN" Anillo ACT1101 (C.R., E.T., F.E.B.); FONDECYT 1141218
(C.R., F.E.B.), 3140436 (R.N.), and 1151408 (R.A.); and Basal-CATA
PFB-06/2007 (C.R., F.E.B., E.T.) and from the Ministry of Economy,
Development, and Tourism's Millennium Science Initiative through grant
IC120009, awarded to the Millennium Institute of Astrophysics (F.E.B.).
C.R. acknowledges support from the China-CONICYT fund. P.G. thanks the
STFC for their support [grant reference ST/J003697/2], and W.N.B.
acknowledges financial support from NuSTAR subcontract 44A-1092750. P.B.
is supported by an STFC studentship. A.C. acknowledges support from
ASI/INAF grant I/037/12/0011/13 and the Caltech Kingsley visitor
program. T.D.-S. acknowledges support from ALMA-CONICYT project 31130005
and FONDECYT 1151239. S.M.L. is supported by an appointment to the NASA
Postdoctoral Program at the NASA Goddard Space Flight Center,
administered by the Universities Space Research Association under
contract with NASA.
NR 134
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2017
VL 835
IS 1
AR 105
DI 10.3847/1538-4357/835/1/105
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EJ8DO
UT WOS:000393455400105
ER
PT J
AU Saigo, K
Onishi, T
Nayak, O
Meixner, M
Tokuda, K
Harada, R
Morioka, Y
Sewilo, M
Indebetouw, R
Torii, K
Kawamura, A
Ohama, A
Hattori, Y
Yamamoto, H
Tachihara, K
Minamidani, T
Inoue, T
Madden, S
Galametz, M
Lebouteiller, V
Chen, CHR
Mizuno, N
Fukui, Y
AF Saigo, Kazuya
Onishi, Toshikazu
Nayak, Omnarayani
Meixner, Margaret
Tokuda, Kazuki
Harada, Ryohei
Morioka, Yuuki
Sewilo, Marta
Indebetouw, Remy
Torii, Kazufumi
Kawamura, Akiko
Ohama, Akio
Hattori, Yusuke
Yamamoto, Hiroaki
Tachihara, Kengo
Minamidani, Tetsuhiro
Inoue, Tsuyoshi
Madden, Suzanne
Galametz, Maud
Lebouteiller, Vianney
Chen, C. -H. Rosie
Mizuno, Norikazu
Fukui, Yasuo
TI KINEMATIC STRUCTURE OF MOLECULAR GAS AROUND HIGH-MASS YSO, PAPILLON
NEBULA, IN N159 EAST IN THE LARGE MAGELLANIC CLOUD: A NEW PERSPECTIVE
WITH ALMA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: clouds; ISM: kinematics and dynamics; ISM: molecules; stars:
formation
ID YOUNG STELLAR OBJECTS; SUPER STAR CLUSTER; H-II REGIONS; CO SURVEY;
GALAXY EVOLUTION; WESTERLUND 2; KEY PROGRAM; N 159; COLLISION; LMC
AB We present the ALMA Band 3 and Band 6 results of 12CO(2-1), (CO)-C-13(2-1), H30 alpha recombination line, free-free emission around 98 GHz, and the dust thermal emission around 230 GHz toward the N159 East Giant Molecular Cloud (N159E) in the Large Magellanic Cloud (LMC). LMC is the nearest active high-mass star-forming face-on galaxy at a distance of. 50 kpc and is the best target for studing high-mass star formation. ALMA observations show that N159E is the complex of filamentary clouds with the width and length of similar to 1 pc and several parsecs. The total molecular mass is 0.92 x 10(5)M(circle dot) from the (CO)-C-13(2-1) intensity. N159E harbors the well-known Papillon Nebula, a compact high-excitation H II region. We found that a YSO associated with the Papillon Nebula has the mass of 35M(circle dot) and is located at the intersection of three filamentary clouds. It indicates that the formation of the high-mass YSO was induced by the collision of filamentary clouds. Fukui et al. reported a similar kinematic structure toward two YSOs in the N159 West region, which are the other YSOs that have the mass of >= 35M(circle dot). This suggests that the collision of filamentary clouds is a primary mechanism of high-mass star formation. We found a small molecular hole around the YSO in Papillon Nebula with a sub-parsec scale. It is filled by free-free and H30 alpha emission. The temperature of the molecular gas around the hole reaches similar to 80 K. It indicates that this YSO has just started the distruction of parental molecular cloud.
C1 [Saigo, Kazuya; Harada, Ryohei; Kawamura, Akiko; Mizuno, Norikazu] Natl Inst Nat Sci, Natl Astron Observ Japan, Chile Observ, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Onishi, Toshikazu; Tokuda, Kazuki; Morioka, Yuuki] Osaka Prefecture Univ, Dept Phys Sci, Grad Sch Sci, Naka Ku, 1-1 Gakuen Cho, Sakai, Osaka 5998531, Japan.
[Nayak, Omnarayani; Meixner, Margaret] Johns Hopkins Univ, Dept Phys & Astron, 366 Bloomberg Ctr,3400 N Charles St, Baltimore, MD 21218 USA.
[Meixner, Margaret] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Sewilo, Marta] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Indebetouw, Remy] Univ Virginia, Dept Astron, POB 400325, Charlottesville, VA 22904 USA.
[Indebetouw, Remy] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA.
[Torii, Kazufumi; Ohama, Akio; Hattori, Yusuke; Yamamoto, Hiroaki; Tachihara, Kengo; Fukui, Yasuo] Nagoya Univ, Dept Phys, Chikusa Ku, Nagoya, Aichi 4648602, Japan.
[Minamidani, Tetsuhiro] Nobeyama Radio Observ, 462-2 Nobeyama, Minamimaki, Nagano 3841305, Japan.
[Inoue, Tsuyoshi] Natl Astron Observ, Div Theoret Astron, Mitaka, Tokyo, Japan.
[Madden, Suzanne; Lebouteiller, Vianney] Univ Paris VII, IRFU, Serv Astrophys, CEA,Lab AIM, Bat 709, F-91191 Gif Sur Yvette, France.
[Galametz, Maud] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Galametz, Maud] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Chen, C. -H. Rosie] Max Planck Inst Radio Astron, Huegel 69, D-53121 Bonn, Germany.
[Mizuno, Norikazu] Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1330033, Japan.
RP Saigo, K (reprint author), Natl Inst Nat Sci, Natl Astron Observ Japan, Chile Observ, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
FU JSPS KAKENHI [16743612, 22244014, 22540250, 22740127, 23403001,
24224005, 26247026]; Mitsubishi Foundation; NSF [1313276]
FX The authors thank the anonymous referee for helpful comments. This paper
makes use of the following ALMA data: ADS/JAO.ALMA #2012.1.00554.S. ALMA
is a partnership of ESO (representing its member states), NSF (USA) and
NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and
KASI (Republic of Korea), in cooperation with the Republic of Chile. The
Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. This work
was supported by JSPS KAKENHI grant numbers of 16743612, 22244014,
22540250, 22740127, 23403001, 24224005, and 26247026. This work was also
supported by the Mitsubishi Foundation and by NSF award 1313276.
NR 55
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U1 0
U2 0
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2017
VL 835
IS 1
AR 108
DI 10.3847/1538-4357/835/1/108
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EJ8DO
UT WOS:000393455400108
ER
PT J
AU Sharon, K
Bayliss, MB
Dahle, H
Florian, MK
Gladders, MD
Johnson, TL
Paterno-Mahler, R
Rigby, JR
Whitaker, KE
Wuyts, E
AF Sharon, Keren
Bayliss, Matthew B.
Dahle, Hakon
Florian, Michael K.
Gladders, Michael D.
Johnson, Traci L.
Paterno-Mahler, Rachel
Rigby, Jane R.
Whitaker, Katherine E.
Wuyts, Eva
TI LENS MODEL AND TIME DELAY PREDICTIONS FOR THE SEXTUPLY LENSED QUASAR
SDSS J2222+2745
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: clusters: individual (SDSS
J2222+2745); gravitational lensing: strong
ID DIGITAL SKY SURVEY; GIANT ARCS SURVEY; GALAXY CLUSTERS;
MASS-DISTRIBUTION; IMAGE SEPARATION; REDSHIFT; SPECTROSCOPY; SPECTRA;
GROWTH
AB SDSS J2222+2745 is a galaxy cluster at z - 0.49, strongly lensing a quasar at z - 2.805 into six widely separated images. In recent Hubble Space Telescope imaging of the field, we identify additional multiply lensed galaxies and confirm the sixth quasar image that was identified by Dahle et al. We used the Gemini-North telescope to measure a spectroscopic redshift of z - 4.56 of one of the lensed galaxies. These data are used to refine the lens model of SDSS J2222+2745, compute the time delay and magnifications of the lensed quasar images, and reconstruct the source image of the quasar host and a lensed galaxy at z = 2.3. This galaxy also appears in absorption in our Gemini spectra of the lensed quasar, at a projected distance of 34 kpc. Our model is in agreement with the recent time delay measurements of Dahle et al., who found T-AB =. 47.7 +/- 6.0 days and T-AC = -722 +/- 24 days. We use the observed time delays to further constrain the model, and find that the model-predicted time delays of the three faint images of the quasar are T-AD =502 +/- 68 days, T-AE = 611 +/- 75 days, and T-AF = 415 +/- 72 days. We have initiated a follow-up campaign to measure these time delays with Gemini North. Finally, we present initial results from an X-ray monitoring program with Swift, indicating the presence of hard X-ray emission from the lensed quasar, as well as extended X-ray emission from the cluster itself, which is consistent with the lensing mass measurement and the cluster velocity dispersion.
C1 [Sharon, Keren; Johnson, Traci L.; Paterno-Mahler, Rachel] Univ Michigan, Dept Astron, 1085 S Univ Ave, Ann Arbor, MI 48109 USA.
[Bayliss, Matthew B.] Colby Coll, 5800 Mayflower Hill, Waterville, ME 04901 USA.
[Bayliss, Matthew B.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Bayliss, Matthew B.] Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA.
[Dahle, Hakon] Univ Oslo, Inst Theoret Astrophys, POB 1029, NO-0315 Oslo, Norway.
[Florian, Michael K.; Gladders, Michael D.] Univ Chicago, Dept Astron & Astrophys, 5640 South Ellis Ave, Chicago, IL 60637 USA.
[Gladders, Michael D.] Univ Chicago, Kavli Inst Cosmol Phys, 5640 South Ellis Ave, Chicago, IL 60637 USA.
[Rigby, Jane R.] Goddard Space Flight Ctr, Astrophys Sci Div, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Whitaker, Katherine E.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Wuyts, Eva] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85741 Garching, Germany.
RP Sharon, K (reprint author), Univ Michigan, Dept Astron, 1085 S Univ Ave, Ann Arbor, MI 48109 USA.
EM kerens@umich.edu
OI Florian, Michael/0000-0001-5097-6755; Johnson, Traci/0000-0002-8829-5303
FU NASA through a grant from Space Telescope Science Institute [GO-13337];
NASA [NAS 5-26555]; NASA through Hubble Fellowship - Space Telescope
Science Institute [HF2-51368]
FX We thank the anonymous referee for useful comments, which improved this
manuscript. Support for program GO-13337 was provided by NASA through a
grant from the Space Telescope Science Institute, which is operated by
the Association of Universities for Research in Astronomy, Inc., under
NASA contract NAS 5-26555. K.E.W. gratefully acknowledges support by
NASA through Hubble Fellowship grant #HF2-51368 awarded by the Space
Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., for NASA. Based on
observations obtained at the Gemini Observatory, which is operated by
the Association of Universities for Research in Astronomy, Inc., under a
cooperative agreement with the NSF on behalf of the Gemini partnership:
the National Science Foundation (United States), the National Research
Council (Canada), CONICYT (Chile), the Australian Research Council
(Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil) and
Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina).
This work made use of data supplied by the UK Swift Science Data Centre
at the University of Leicester. This work makes use of the Matlab
Astronomy Package (Ofek 2014).
NR 43
TC 0
Z9 0
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2017
VL 835
IS 1
AR 5
DI 10.3847/1538-4357/835/1/5
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EJ8DO
UT WOS:000393455400005
ER
PT J
AU Starkey, D
Horne, K
Fausnaugh, MM
Peterson, BM
Bentz, MC
Kochanek, CS
Denney, KD
Edelson, R
Goad, MR
De Rosa, G
Anderson, MD
Arevalo, P
Barth, AJ
Bazhaw, C
Borman, GA
Boroson, TA
Bottorff, MC
Brandt, WN
Breeveld, AA
Cackett, EM
Carini, MT
Croxall, KV
Crenshaw, DM
Dalla Bonta, E
De Lorenzo-Caceres, A
Dietrich, M
Efimova, NV
Ely, J
Evans, PA
Filippenko, AV
Flatland, K
Gehrels, N
Geier, S
Gelbord, JM
Gonzalez, L
Gorjian, V
Grier, CJ
Grupe, D
Hall, PB
Hicks, S
Horenstein, D
Hutchison, T
Im, M
Jensen, JJ
Joner, MD
Jones, J
Kaastra, J
Kaspi, S
Kelly, BC
Kennea, JA
Kim, SC
Kim, M
Klimanov, SA
Korista, KT
Kriss, GA
Lee, JC
Leonard, DC
Lira, P
MacInnis, F
Manne-Nicholas, ER
Mathur, S
McHardy, IM
Montouri, C
Musso, R
Nazarov, SV
Norris, RP
Nousek, JA
Okhmat, DN
Pancoast, A
Parks, JR
Pei, L
Pogge, RW
Pott, JU
Rafter, SE
Rix, HW
Saylor, DA
Schimoia, JS
Schnulle, K
Sergeev, SG
Siegel, MH
Spencer, M
Sung, HI
Teems, KG
Turner, CS
Uttley, P
Vestergaard, M
Villforth, C
Weiss, Y
Woo, JH
Yan, H
Young, S
Zheng, W
Zu, Y
AF Starkey, D.
Horne, Keith
Fausnaugh, M. M.
Peterson, B. M.
Bentz, M. C.
Kochanek, C. S.
Denney, K. D.
Edelson, R.
Goad, M. R.
De Rosa, G.
Anderson, M. D.
Arevalo, P.
Barth, A. J.
Bazhaw, C.
Borman, G. A.
Boroson, T. A.
Bottorff, M. C.
Brandt, W. N.
Breeveld, A. A.
Cackett, E. M.
Carini, M. T.
Croxall, K. V.
Crenshaw, D. M.
Dalla Bonta, E.
De Lorenzo-Caceres, A.
Dietrich, M.
Efimova, N. V.
Ely, J.
Evans, P. A.
Filippenko, A. V.
Flatland, K.
Gehrels, N.
Geier, S.
Gelbord, J. M.
Gonzalez, L.
Gorjian, V.
Grier, C. J.
Grupe, D.
Hall, P. B.
Hicks, S.
Horenstein, D.
Hutchison, T.
Im, M.
Jensen, J. J.
Joner, M. D.
Jones, J.
Kaastra, J.
Kaspi, S.
Kelly, B. C.
Kennea, J. A.
Kim, S. C.
Kim, M.
Klimanov, S. A.
Korista, K. T.
Kriss, G. A.
Lee, J. C.
Leonard, D. C.
Lira, P.
MacInnis, F.
Manne-Nicholas, E. R.
Mathur, S.
McHardy, I. M.
Montouri, C.
Musso, R.
Nazarov, S. V.
Norris, R. P.
Nousek, J. A.
Okhmat, D. N.
Pancoast, A.
Parks, J. R.
Pei, L.
Pogge, R. W.
Pott, J-U
Rafter, S. E.
Rix, H-W
Saylor, D. A.
Schimoia, J. S.
Schnuelle, K.
Sergeev, S. G.
Siegel, M. H.
Spencer, M.
Sung, H-I
Teems, K. G.
Turner, C. S.
Uttley, P.
Vestergaard, M.
Villforth, C.
Weiss, Y.
Woo, J-H
Yan, H.
Young, S.
Zheng, W.
Zu, Y.
TI SPACE TELESCOPE AND OPTICAL REVERBERATION MAPPING PROJECT. VI.
REVERBERATING DISK MODELS FOR NGC 5548
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; galaxies: active; galaxies: individual (NGC
5548); galaxies: nuclei; galaxies: Seyfert
ID ACTIVE GALACTIC NUCLEI; QUASAR ACCRETION DISKS; SUPERMASSIVE BLACK-HOLE;
BROAD-LINE REGION; X-RAY; CONTINUUM EMISSION; EMITTING REGIONS;
SEYFERT-GALAXIES; VARIABILITY; SIZE
AB We conduct a multiwavelength continuum variability study of the Seyfert 1 galaxy NGC 5548 to investigate the temperature structure of its accretion disk. The 19 overlapping continuum light curves (1158 angstrom to 9157 angstrom) combine simultaneous Hubble Space Telescope, Swift, and ground-based observations over a 180 day period from 2014 January to July. Light-curve variability is interpreted as the reverberation response of the accretion disk to irradiation by a central time-varying point source. Our model yields the disk inclination i = 36 degrees +/- 10 degrees, temperature T-1= (44 +/- 6) x 10(3) K at 1 light day from the black hole, and a temperature-radius slope (T proportional to r(-alpha)) of alpha = 0.99 +/- 0.03. We also infer the driving light curve and find that it correlates poorly with both the hard and soft X-ray light curves, suggesting that the X-rays alone may not drive the ultraviolet and optical variability over the observing period. We also decompose the light curves into bright, faint, and mean accretion-disk spectra. These spectra lie below that expected for a standard blackbody accretion disk accreting at L/L-Edd = 0.1.
C1 [Starkey, D.; Horne, Keith; De Lorenzo-Caceres, A.] Univ St Andrews, SUPA Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Fausnaugh, M. M.; Peterson, B. M.; Kochanek, C. S.; Denney, K. D.; De Rosa, G.; Croxall, K. V.; Grier, C. J.; Mathur, S.; Pogge, R. W.; Zu, Y.] Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA.
[Peterson, B. M.; Kochanek, C. S.; Denney, K. D.; De Rosa, G.; Croxall, K. V.; Mathur, S.; Pogge, R. W.; Schimoia, J. S.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, 191 West Woodruff Ave, Columbus, OH 43210 USA.
[Peterson, B. M.; De Rosa, G.; Ely, J.; Kriss, G. A.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Bentz, M. C.; Anderson, M. D.; Bazhaw, C.; Crenshaw, D. M.; Horenstein, D.; Jones, J.; Manne-Nicholas, E. R.; Norris, R. P.; Parks, J. R.; Saylor, D. A.; Teems, K. G.; Turner, C. S.] Georgia State Univ, Dept Phys & Astron, 25 Pk Pl,Suite 605, Atlanta, GA 30303 USA.
[Edelson, R.; Young, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Goad, M. R.; Evans, P. A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Gran Bretana N 1111, Valparaiso, Chile.
[Barth, A. J.; Pei, L.] Univ Calif Irvine, Dept Phys & Astron, 4129 Frederick Reines Hall, Irvine, CA 92697 USA.
[Borman, G. A.; Nazarov, S. V.; Okhmat, D. N.; Sergeev, S. G.] Crimean Astrophys Observ, Crimea 298409, Russia.
[Boroson, T. A.; Kennea, J. A.; Siegel, M. H.] Las Cumbres Global Telescope Network, 6740 Cortona Dr,Suite 102, Santa Barbara, CA 93117 USA.
[Bottorff, M. C.; Hutchison, T.; MacInnis, F.; Musso, R.] Southwestern Univ, Dept Phys FJS 149, Fountainwood Observ, 1011 E Univ Ave, Georgetown, TX 78626 USA.
[Brandt, W. N.; Grier, C. J.; Nousek, J. A.] Penn State Univ, Eberly Coll Sci, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Brandt, W. N.; Grier, C. J.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Brandt, W. N.] Penn State Univ, Dept Phys, Davey Lab 104, University Pk, PA 16802 USA.
[Breeveld, A. A.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Cackett, E. M.] Wayne State Univ, Dept Phys & Astron, 666 W Hancock St, Detroit, MI 48201 USA.
[Carini, M. T.; Hicks, S.] Western Kentucky Univ, Dept Phys & Astron, 1906 Coll Hts Blvd 11077, Bowling Green, KY 42101 USA.
[Dalla Bonta, E.] Univ Padua, Dipartimento Fis & Astron G Galilei, Vicolo Osservatorio 3, I-35122 Padua, Italy.
[Dalla Bonta, E.] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy.
[Dietrich, M.] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA.
[Dietrich, M.] Worcester State Univ, Dept Earth Environm & Phys, 486 Chandler St, Worcester, MA 01602 USA.
[Efimova, N. V.; Klimanov, S. A.] Pulkovo Observ, St Petersburg 196140, Russia.
[Filippenko, A. V.; Zheng, W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Flatland, K.; Gonzalez, L.; Leonard, D. C.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Gehrels, N.] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Geier, S.] Inst Astrofis Canarias, Tenerife 38200, Spain.
[Geier, S.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Geier, S.] Gran Telescopio Canarias GRANTECAN, Tenerife 38205, Spain.
[Gelbord, J. M.] Spectral Sci Inc, 4 Fourth Ave, Burlington, MA 01803 USA.
[Gelbord, J. M.] Eureka Sci Inc, 2452 Delmer St,Suite 100, Oakland, CA 94602 USA.
[Gorjian, V.] CALTECH, Jet Prop Lab, MS 169-327,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Grupe, D.] Morehead State Univ, Ctr Space Sci, 235 Martindale Dr, Morehead, KY 40351 USA.
[Hall, P. B.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada.
[Im, M.; Woo, J-H] Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul, South Korea.
[Jensen, J. J.; Vestergaard, M.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark.
[Joner, M. D.; Spencer, M.] Brigham Young Univ, Dept Phys & Astron, N283 ESC, Provo, UT 84602 USA.
[Kaastra, J.] SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands.
[Kaastra, J.] Univ Utrecht, Dept Phys & Astron, POB 80000, NL-3508 Utrecht, Netherlands.
[Kaastra, J.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
[Kaspi, S.] Tel Aviv Univ, Sch Phys & Astron, Raymond & Beverly Sackler Fac Exact Sci, IL-69978 Tel Aviv, Israel.
[Kaspi, S.; Rafter, S. E.; Weiss, Y.] Technion, Dept Phys, IL-32000 Haifa, Israel.
[Kelly, B. C.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Kim, S. C.; Kim, M.; Lee, J. C.; Sung, H-I] Korea Astron & Space Sci Inst, Daejeon, South Korea.
[Korista, K. T.] Western Michigan Univ, Dept Phys, 1120 Everett Tower, Kalamazoo, MI 49008 USA.
[Kriss, G. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Lira, P.] Univ Chile, Dept Astron, Camino Observ 1515, Santiago, Chile.
[McHardy, I. M.] Univ Southampton, Southampton SO17 1BJ, Hants, England.
[Montouri, C.] Univ Insubria, DiSAT, Via Valleggio 11, I-22100 Como, Italy.
[Pancoast, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Pancoast, A.; Schimoia, J. S.] Univ Fed Rio Sul, Inst Fis, Campus Vale, Porto Alegre, RS, Brazil.
[Pott, J-U; Rix, H-W; Schnuelle, K.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Rafter, S. E.] Univ Haifa, Fac Nat Sci, Dept Phys, IL-31905 Haifa, Israel.
[Uttley, P.] Univ Amsterdam, Astron Inst Anton Pannekoek, Postbus 94249, NL-1090 GE Amsterdam, Netherlands.
[Vestergaard, M.] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.
[Villforth, C.] Univ Bath, Dept Phys, Bath BA2 7AY, Avon, England.
[Yan, H.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA.
[Zu, Y.] Carnegie Mellon Univ, Dept Phys, 5000 Forbes Ave, Pittsburgh, PA 15213 USA.
RP Starkey, D (reprint author), Univ St Andrews, SUPA Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
FU NASA through a grant from the Space Telescope Science Institute
[GO-13330]; NASA [NAS5-26555, NNX13AC26G, NNX13AC63G, NNX13AE99G,
NNX15AH49G]; UK Science and Technology Facilities Council [ST/K502339/1,
ST/J001651/1]; National Science Foundation (NSF) [AST-1008882]; NSF
[AST-1412693, AST-1211916, AST-1302093, AST-0618209, AST-1009571,
AST-1210311, AST-1412315]; TABASGO Foundation; Christopher R. Redlich
Fund; NSF CAREER grant [AST-1253702]; HHMI; NSERC; Creative Initiative
program of the National Research Foundation of Korea (NRFK) - Korean
government (MSIP) [20080060544]; NWO, the Netherlands Organization for
Scientific Research; UC Center for Galaxy Evolution; Fondecyt [1120328];
NSF graduate fellowship; UCSB Deans Fellowship; CNPq, National Council
for Scientific and Technological Development (Brazil); Packard
Foundation; Danish National Research Foundation; Danish Council for
Independent Research [DFF 4002-00275]; National Research Foundation of
Korea (NRF) - Korean government [2010-0027910]
FX Support for HST program number GO-13330 was provided by NASA through a
grant from the Space Telescope Science Institute, which is operated by
the Association of Universities for Research in Astronomy, Inc., under
NASA contract NAS5-26555. D.A.S. and K.D.H. acknowledge support from the
UK Science and Technology Facilities Council through grant ST/K502339/1
and ST/J001651/1. M.M.F., G.D.R., B.M.P., C.J.G., and R.W.P. are
grateful for the support of the National Science Foundation (NSF)
through grant AST-1008882 to The Ohio State University. A.J.B. and L.P.
have been supported by NSF grant AST-1412693. A.V.F. and W.Z. are
grateful for financial assistance from NSF grant AST-1211916, the
TABASGO Foundation, and the Christopher R. Redlich Fund. M.C. Bentz
gratefully acknowledges support through NSF CAREER grant AST-1253702 to
Georgia State University. M.C.B. acknowledges HHMI for support through
an undergraduate science education grant to Southwestern University.
K.D.D. is supported by an NSF Fellowship awarded under grant
AST-1302093. R.E. gratefully acknowledges support from NASA under awards
NNX13AC26G, NNX13AC63G, and NNX13AE99G. J.M.G. gratefully acknowledges
support from NASA under award NNX15AH49G. P.B.H. is supported by NSERC.
M.I. acknowledges support from the Creative Initiative program, No.
20080060544, of the National Research Foundation of Korea (NRFK) funded
by the Korean government (MSIP). M.D.J. acknowledges NSF grant
AST-0618209. S.R.O.N. is financially supported by NWO, the Netherlands
Organization for Scientific Research. B.C.K. is partially supported by
the UC Center for Galaxy Evolution. C.S.K. acknowledges the support of
NSF grant AST-1515876. D.C.L. acknowledges support from NSF grants
AST-1009571 and AST-1210311. P.L. acknowledges support from Fondecyt
grant 1120328. A.P. acknowledges support from an NSF graduate fellowship
and a UCSB Deans Fellowship. J.S.S. acknowledges CNPq, National Council
for Scientific and Technological Development (Brazil) for partial
support and The Ohio State University for warm hospitality. T.T. has
been supported by NSF grant AST-1412315. T.T. and B.C.K. acknowledge
support from the Packard Foundation in the form of a Packard Research
Fellowship to T.T.; also, T.T. thanks the American Academy in Rome and
the Observatory of Monteporzio Catone for kind hospitality. The Dark
Cosmology Centre is funded by the Danish National Research Foundation.
M.V. gratefully acknowledges support from the Danish Council for
Independent Research via grant no. DFF 4002-00275. J.-H.W. acknowledges
support by the National Research Foundation of Korea (NRF) grant funded
by the Korean government (No. 2010-0027910). This research has made use
of the NASA/IPAC Extragalactic Database (NED), which is operated by the
Jet Propulsion Laboratory, California Institute of Technology, under
contract with NASA. The authors acknowledge the support of the referee
for their helpful input during the review process.
NR 45
TC 0
Z9 0
U1 2
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2017
VL 835
IS 1
AR 65
DI 10.3847/1538-4357/835/1/65
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EJ8DO
UT WOS:000393455400065
ER
PT J
AU Vreeswijk, PM
Leloudas, G
Gal-Yam, A
De Cia, A
Perley, DA
Quimby, RM
Waldman, R
Sullivan, M
Yan, L
Ofek, EO
Fremling, C
Taddia, F
Sollerman, J
Valenti, S
Arcavi, I
Howell, DA
Filippenko, AV
Cenko, SB
Yaron, O
Kasliwal, MM
Cao, Y
Ben-Ami, S
Horesh, A
Rubin, A
Lunnan, R
Nugent, PE
Laher, R
Rebbapragada, UD
Wozniak, P
Kulkarni, SR
AF Vreeswijk, Paul M.
Leloudas, Giorgos
Gal-Yam, Avishay
De Cia, Annalisa
Perley, Daniel A.
Quimby, Robert M.
Waldman, Roni
Sullivan, Mark
Yan, Lin
Ofek, Eran O.
Fremling, Christoffer
Taddia, Francesco
Sollerman, Jesper
Valenti, Stefano
Arcavi, Iair
Howell, D. Andrew
Filippenko, Alexei V.
Cenko, S. Bradley
Yaron, Ofer
Kasliwal, Mansi M.
Cao, Yi
Ben-Ami, Sagi
Horesh, Assaf
Rubin, Adam
Lunnan, Ragnhild
Nugent, Peter E.
Laher, Russ
Rebbapragada, Umaa D.
Wozniak, Przemyslaw
Kulkarni, Shrinivas R.
TI ON THE EARLY-TIME EXCESS EMISSION IN HYDROGEN-POOR SUPERLUMINOUS
SUPERNOVAE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE supernovae: general; supernovae: individual (PTF 12dam, iPTF 13dcc)
ID LIGHT CURVES; LUMINOUS SUPERNOVAE; SHOCK-BREAKOUT; IC SUPERNOVAE; HOST
GALAXY; ANALYTIC SOLUTIONS; MASS-LOSS; EXPLOSIONS; TRANSIENT; MAGNETAR
AB We present the light curves of the hydrogen-poor superluminous supernovae (SLSNe I) PTF 12dam and iPTF 13dcc, discovered by the (intermediate) Palomar Transient Factory. Both show excess emission at early times and a slowly declining light curve at late times. The early bump in PTF 12dam is very similar in duration (similar to 10 days) and brightness relative to the main peak (2-3 mag fainter) compared to that observed in other SLSNe I. In contrast, the long-duration (>30 days) early excess emission in iPTF 13dcc, whose brightness competes with that of the main peak, appears to be of a different nature. We construct bolometric light curves for both targets, and fit a variety of light-curve models to both the early bump and main peak in an attempt to understand the nature of these explosions. Even though the slope of the late-time decline in the light curves of both SLSNe is suggestively close to that expected from the radioactive decay of Ni-56 and Co-56, the amount of nickel required to power the full light curves is too large considering the estimated ejecta mass. The magnetar model including an increasing escape fraction provides a reasonable description of the PTF 12dam observations. However, neither the basic nor the double-peaked magnetar model is capable of reproducing the light curve of iPTF 13dcc. A model combining a shock breakout in an extended envelope with late-time magnetar energy injection provides a reasonable fit to the iPTF 13dcc observations. Finally, we find that the light curves of both PTF 12dam and iPTF 13dcc can be adequately fit with the model involving interaction with the circumstellar medium.
C1 [Vreeswijk, Paul M.; Leloudas, Giorgos; Gal-Yam, Avishay; De Cia, Annalisa; Waldman, Roni; Ofek, Eran O.; Yaron, Ofer; Ben-Ami, Sagi; Horesh, Assaf; Rubin, Adam] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-7610001 Rehovot, Israel.
[Leloudas, Giorgos; Perley, Daniel A.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark.
[De Cia, Annalisa] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Perley, Daniel A.; Kasliwal, Mansi M.; Cao, Yi; Lunnan, Ragnhild; Kulkarni, Shrinivas R.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Quimby, Robert M.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Quimby, Robert M.] Univ Tokyo, UTIAS, Kavli IPMU WPI, Kashiwa, Chiba 2778583, Japan.
[Waldman, Roni] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel.
[Sullivan, Mark] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Yan, Lin] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Fremling, Christoffer; Taddia, Francesco; Sollerman, Jesper] Stockholm Univ, AlbaNova, Dept Astron, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Valenti, Stefano] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Arcavi, Iair; Howell, D. Andrew] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Arcavi, Iair; Howell, D. Andrew] Las Cumbres Observ Global Telescope, 6740 Cortona Dr,Suite 102, Goleta, CA 93111 USA.
[Filippenko, Alexei V.; Nugent, Peter E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Cenko, S. Bradley] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Mail Code 661, Greenbelt, MD 20771 USA.
[Cenko, S. Bradley] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Ben-Ami, Sagi] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
[Nugent, Peter E.] Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, 1 Cyclotron Rd, Berkeley, CA 94720 USA.
[Laher, Russ] CALTECH, Spitzer Sci Ctr, MS 314-6, Pasadena, CA 91125 USA.
[Rebbapragada, Umaa D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Wozniak, Przemyslaw] Los Alamos Natl Lab, MS D436, Los Alamos, NM 87545 USA.
RP Vreeswijk, PM (reprint author), Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-7610001 Rehovot, Israel.
EM paul.vreeswijk@weizmann.ac.il
OI Sullivan, Mark/0000-0001-9053-4820; Gal-Yam, Avishay/0000-0002-3653-5598
FU W. M. Keck Foundation; National Science Foundation [AST-1005313]; DNRF;
EU/FP7 via ERC grant [307260]; Quantum Universe I-Core program by the
Israeli Committee for planning; ISF; GIF; Minerva; NASA through Hubble
Fellowship - Space Telescope Science Institute [HST-HF-51296.01-A]; NASA
[NAS 5-26555]; EU/FP7-ERC grant [615929]; Willner Family Leadership
Institute Ilan Gluzman (Secaucus NJ); Israel Science Foundation; I-CORE
Program of the Planning and Budgeting Committee; NASA through the
Einstein Fellowship Program [PF6-170148]; NSF grant [AST-1211916];
TABASGO Foundation; Christopher R. Redlich Fund; Office of Science of
the U.S. Department of Energy [DE-AC02-05CH11231]
FX It is a pleasure to acknowledge the help of Manos Chatzopoulos with the
implementation of the semianalytical light-curve models developed by him
and his colleagues in our light-curve fitting program. We are grateful
to Nir Sapir for enlightening discussions, and to WeiKang Zheng, Kelsey
Clubb, and Patrick Kelly for their contribution to the 2013 December 3
Keck/LRIS observations of iPTF 13dcc. We thank the staffs at Palomar and
Lick Observatories for their expert assistance. The intermediate Palomar
Transient Factory project is a scientific collaboration among the
California Institute of Technology, Los Alamos National Laboratory, the
University of Wisconsin at Milwaukee, the Oskar Klein Center, the
Weizmann Institute of Science, the TANGO Program of the University
System of Taiwan, and the Kavli Institute for the Physics and
Mathematics of the Universe. This paper is based in part on observations
made with the NASA/ESA Hubble Space Telescope. Some of the data
presented herein were obtained at the W.M. Keck Observatory, which is
operated as a scientific partnership among the California Institute of
Technology, the University of California, and NASA; the observatory was
made possible by the generous financial support of the W. M. Keck
Foundation. Research at Lick Observatory is partially supported by a
generous gift from Google. These results also made use of the Discovery
Channel Telescope at Lowell Observatory. Lowell is a private, non-profit
institution dedicated to astrophysical research and public appreciation
of astronomy and operates the DCT in partnership with Boston University,
the University of Maryland, the University of Toledo, Northern Arizona
University, and Yale University. LMI construction was supported by a
grant AST-1005313 from the National Science Foundation.; The Dark
Cosmology Centre is funded by the DNRF. A.G.-Y. is supported by the
EU/FP7 via ERC grant No. 307260, the Quantum Universe I-Core program by
the Israeli Committee for planning and funding, and the ISF, GIF,
Minerva, and ISF grants, WIS-UK "making connections," and Kimmel and
ARCHES awards. Support for D.A.P. was provided by NASA through Hubble
Fellowship grant HST-HF-51296.01-A awarded by the Space Telescope
Science Institute, which is operated by the Association of Universities
for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555.
M.S. acknowledges support from EU/FP7-ERC grant 615929. E.O.O. is
incumbent of the Arye Dissentshik career development chair and is
grateful to support by grants from the Willner Family Leadership
Institute Ilan Gluzman (Secaucus NJ), Israel Science Foundation,
Minerva, and the I-CORE Program of the Planning and Budgeting Committee
and The Israel Science Foundation. Support for I. A. was provided by
NASA through the Einstein Fellowship Program, grant PF6-170148. A.V.F.'s
supernova group at UC Berkeley is supported through NSF grant
AST-1211916, the TABASGO Foundation, and the Christopher R. Redlich
Fund. The National Energy Research Scientific Computing Center, which is
supported by the Office of Science of the U.S. Department of Energy
under Contract No. DE-AC02-05CH11231, provided staff, computational
resources, and data storage for this project. Part of this research was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration.
NR 91
TC 0
Z9 0
U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2017
VL 835
IS 1
AR 58
DI 10.3847/1538-4357/835/1/58
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EJ8DO
UT WOS:000393455400058
ER
PT J
AU Williams, JC
Nguyen, BN
McCorkle, L
Scheiman, D
Griffin, JS
Steiner, SA
Meador, MAB
AF Williams, Jarrod C.
Nguyen, Baochau N.
McCorkle, Linda
Scheiman, Daniel
Griffin, Justin S.
Steiner, Stephen A., III
Meador, Mary Ann B.
TI Highly Porous, Rigid-Rod Polyamide Aerogels with Superior Mechanical
Properties and Unusually High Thermal Conductivity
SO ACS APPLIED MATERIALS & INTERFACES
LA English
DT Article
DE polyamide; porous polymers; aerogels; mesoporous; thermal conductivity
ID FLEXIBLE POLYIMIDE AEROGELS; COHERENT EXPANDED AEROGELS; POLYSTYRENE
AEROGELS; ORGANIC AEROGELS
AB We report here the fabrication of polyamide aerogels composed of poly-p-phenylene-terephthalamide, the same backbone chemistry as DuPonts Kevlar. The all-para-substituted polymers gel without the use of cross-linker and maintain their shape during processing-an improvement over the meta-substituted cross-linked polyamide aerogels reported previously. Solutions containing calcium chloride (CaCl2) and para-phenylenediamine (pPDA) in N-methylpyrrolidinone (NMP) at low temperature are reacted with terephthaloyl chloride (TPC). Polymerization proceeds over the course of 5 min resulting in gelation. Removal of the reaction solvent via solvent exchange followed by extraction with supercritical carbon dioxide provides aerogels with densities ranging from 0.1 to 0.3 g/cm(3), depending on the concentration of calcium chloride, the formulated number of repeat units, n, and the concentration of polymer in the reaction mixture. These variables were assessed in a statistical experimental study to understand their effects on the properties of the aerogels. Aerogels made using at least 30 wt % CaCl2 had the best strength when compared to aerogels of similar density. Furthermore, aerogels made using 30 wt % CaCl2 exhibited the lowest shrinkage when aged at elevated temperatures. Notably, whereas most aerogel materials are highly insulating (thermal conductivities of 10-30 mW/m K), the polyamide aerogels produced here exhibit remarkably high thermal conductivities (50-80 mW/(m K)) at the same densities as other inorganic and polymer aerogels. These high thermal conductivities are attributed to efficient phonon transport by the rigid-rod polymer backbone. In conjunction with their low cost, ease of fabrication with respect to other polymer aerogels, low densities, and high mass-normalized strength and stiffness properties, these aerogels are uniquely valuable for applications such as lightweighting in consumer electronics, automobiles, and aerospace where weight reduction is desirable but trapping of heat may be undesirable-applications where other polymer aerogels have to date otherwise been unsuitable-creating new opportunities for commercialization of aerogels.
C1 [Williams, Jarrod C.; Meador, Mary Ann B.] NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
[Nguyen, Baochau N.; McCorkle, Linda; Scheiman, Daniel] Ohio Aerosp Inst, 22800 Cedar Point Rd, Cleveland, OH 44142 USA.
[Griffin, Justin S.; Steiner, Stephen A., III] Aerogel Technol LLC, 270 Dorchester Ave, Boston, MA 02127 USA.
RP Meador, MAB (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM maryann.meador@nasa.gov
FU NASA Glenn's Director's Discretionary Fund
FX The authors thank NASA Glenn's Director's Discretionary Fund for support
of this work.
NR 34
TC 0
Z9 0
U1 29
U2 29
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1944-8244
J9 ACS APPL MATER INTER
JI ACS Appl. Mater. Interfaces
PD JAN 18
PY 2017
VL 9
IS 2
BP 1801
EP 1809
DI 10.1021/acsami.6b13100
PG 9
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary
SC Science & Technology - Other Topics; Materials Science
GA EI4IZ
UT WOS:000392458300069
PM 28060486
ER
PT J
AU Price, SF
Hoffman, MJ
Bonin, JA
Howat, IM
Neumann, T
Saba, J
Tezaur, I
Guerber, J
Chambers, DP
Evans, KJ
Kennedy, JH
Lenaerts, J
Lipscomb, WH
Perego, M
Salinger, AG
Tuminaro, RS
van den Broeke, MR
Nowicki, SMJ
AF Price, Stephen F.
Hoffman, Matthew J.
Bonin, Jennifer A.
Howat, Ian M.
Neumann, Thomas
Saba, Jack
Tezaur, Irina
Guerber, Jeffrey
Chambers, Don P.
Evans, Katherine J.
Kennedy, Joseph H.
Lenaerts, Jan
Lipscomb, William H.
Perego, Mauro
Salinger, Andrew G.
Tuminaro, Raymond S.
van den Broeke, Michiel R.
Nowicki, Sophie M. J.
TI An ice sheet model validation framework for the Greenland ice sheet
SO GEOSCIENTIFIC MODEL DEVELOPMENT
LA English
DT Article
ID FUTURE SEA-LEVEL; SURFACE MASS-BALANCE; GLACIERS; GRACE; VARIABILITY;
DYNAMICS; PROJECT; RISE; SENSITIVITIES; ALBANY/FELIX
AB We propose a new ice sheet model validation framework - the Cryospheric Model Comparison Tool (CmCt) - that takes advantage of ice sheet altimetry and gravimetry observations collected over the past several decades and is applied here to modeling of the Greenland ice sheet. We use realistic simulations performed with the Community Ice Sheet Model (CISM) along with two idealized, non-dynamic models to demonstrate the framework and its use. Dynamic simulations with CISM are forced from 1991 to 2013, using combinations of reanalysis-based surface mass balance and observations of outlet glacier flux change. We propose and demonstrate qualitative and quantitative metrics for use in evaluating the different model simulations against the observations. We find that the altimetry observations used here are largely ambiguous in terms of their ability to distinguish one simulation from another. Based on basin-scale and whole-ice-sheet-scale metrics, we find that simulations using both idealized conceptual models and dynamic, numerical models provide an equally reasonable representation of the ice sheet surface (mean elevation differences of <1 m). This is likely due to their short period of record, biases inherent to digital elevation models used for model initial conditions, and biases resulting from firn dynamics, which are not explicitly accounted for in the models or observations. On the other hand, we find that the gravimetry observations used here are able to unambiguously distinguish between simulations of varying complexity, and along with the CmCt, can provide a quantitative score for assessing a particular model and/or simulation. The new framework demonstrates that our proposed metrics can distinguish relatively better from relatively worse simulations and that dynamic ice sheet models, when appropriately initialized and forced with the right boundary conditions, demonstrate a predictive skill with respect to observed dynamic changes that have occurred on Greenland over the past few decades. An extensible design will allow for continued use of the CmCt as future altimetry, gravimetry, and other remotely sensed data become available for use in ice sheet model validation.
C1 [Price, Stephen F.; Hoffman, Matthew J.; Lipscomb, William H.] Los Alamos Natl Lab, Fluid Dynam & Solid Mech Grp, MS B216, Los Alamos, NM 87545 USA.
[Bonin, Jennifer A.; Chambers, Don P.] Univ S Florida, Coll Marine Sci, St Petersburg, FL 33701 USA.
[Howat, Ian M.] Ohio State Univ, Sch Earth Sci, Columbus, OH 43210 USA.
[Howat, Ian M.] Ohio State Univ, Byrd Polar Res Ctr, Columbus, OH 43210 USA.
[Neumann, Thomas; Saba, Jack; Guerber, Jeffrey; Nowicki, Sophie M. J.] NASA, Cryospher Sci, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Tezaur, Irina] Sandia Natl Labs, Extreme Scale Data Sci & Analyt Dept, POB 969,MS 9159, Livermore, CA 94551 USA.
[Saba, Jack] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Guerber, Jeffrey] Sigma Space Corp, Lanham, MD 20706 USA.
[Evans, Katherine J.; Kennedy, Joseph H.] Oak Ridge Natl Lab, Computat Earth Sci Grp, MS 6301, Oak Ridge, TN 37831 USA.
[Lenaerts, Jan; van den Broeke, Michiel R.] Univ Utrecht, Inst Marine & Atmospher Res Utrecht, Utrecht, Netherlands.
[Perego, Mauro; Salinger, Andrew G.; Tuminaro, Raymond S.] Sandia Natl Labs, Computat Math Dept, POB 5800,MS 1320, Albuquerque, NM 87185 USA.
RP Price, SF (reprint author), Los Alamos Natl Lab, Fluid Dynam & Solid Mech Grp, MS B216, Los Alamos, NM 87545 USA.
EM sprice@lanl.gov
RI Van den Broeke, Michiel/F-7867-2011; Howat, Ian/A-3474-2008;
OI Van den Broeke, Michiel/0000-0003-4662-7565; Howat,
Ian/0000-0002-8072-6260; Evans, Katherine/0000-0001-8174-6450
FU Scientific Discovery through Advanced Computing (SciDAC) program - US
Department of Energy (DOE), Office of Science, Advanced Scientific
Computing Research and Biological and Environmental Research Programs;
NASA Cryospheric Sciences grant [NNX11AR47G]; NASA Cryospheric Sciences;
National Science Foundation [ANT-0424589]; Polar Program of the
Netherlands Organization for Scientific Research (NWO/NPP); Netherlands
Earth System Science Center (NESSC); Water, Climate, Ecosystems research
theme of Utrecht University; NWO ALW through a Veni postdoctoral grant;
Office of Science of the US Department of Energy [DE-AC02-05CH11231]
FX The authors thank the editor, Philip Huybrechts, and three anonymous
reviewers for comments that helped improve the clarity and focus of the
paper. Support for Stephen F. Price, Matthew J. Hoffman, Irina Tezaur,
Katherine J. Evans, Joseph H. Kennedy, William H. Lipscomb, Mauro
Perego, Andrew G. Salinger, and Raymond S. Tuminaro was provided through
the Scientific Discovery through Advanced Computing (SciDAC) program
funded by the US Department of Energy (DOE), Office of Science, Advanced
Scientific Computing Research and Biological and Environmental Research
Programs. Support for Ian M. Howat was provided by NASA Cryospheric
Sciences grant NNX11AR47G. Stephen F. Price was also partially supported
by NASA Cryospheric Sciences, and Stephen F. Price and Matthew J.
Hoffman were partially supported by the National Science Foundation,
under grant ANT-0424589 to the Center for Remote Sensing of Ice Sheets
(CReSIS). Jan Lenaerts and Michiel R. van den Broeke acknowledge funding
from the Polar Program of the Netherlands Organization for Scientific
Research (NWO/NPP), the Netherlands Earth System Science Center (NESSC)
and Water, Climate, Ecosystems research theme of Utrecht University. Jan
Lenaerts is supported by NWO ALW through a Veni postdoctoral grant. This
research used resources of the National Energy Research Scientific
Computing Center (NERSC; supported by the Office of Science of the US
Department of Energy under contract DE-AC02-05CH11231).
NR 48
TC 0
Z9 0
U1 2
U2 2
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1991-959X
EI 1991-9603
J9 GEOSCI MODEL DEV
JI Geosci. Model Dev.
PD JAN 17
PY 2017
VL 10
IS 1
BP 255
EP 270
DI 10.5194/gmd-10-255-2017
PG 16
WC Geosciences, Multidisciplinary
SC Geology
GA EK1LC
UT WOS:000393685800001
ER
PT J
AU Creamer, JS
Mora, MF
Willis, PA
AF Creamer, Jessica S.
Mora, Maria F.
Willis, Peter A.
TI Enhanced Resolution of Chiral Amino Acids with Capillary Electrophoresis
for Biosignature Detection in Extraterrestrial Samples
SO ANALYTICAL CHEMISTRY
LA English
DT Article
ID LASER-INDUCED FLUORESCENCE; MARS ORGANIC ANALYZER; IN-SITU ANALYSIS;
BETA-CYCLODEXTRIN; ZONE ELECTROPHORESIS; MONO LAKE; SEPARATION;
EXPLORATION; SELECTORS; SURFACE
AB Amino acids are fundamental building blocks of terrestrial life as well as ubiquitous byproducts of abiotic reactions. In order to distinguish between amino acids formed by abiotic versus biotic processes it is possible to use chemical distributions to identify patterns unique to life. This article describes two capillary electrophoresis methods capable of resolving 17 amino acids found in high abundance in both biotic and abiotic samples (seven enantiomer pairs d/l-Ala, -Asp, -Glu, -His, -Leu, -Ser, -Val and the three achiral amino acids Gly, beta-Ala, and GABA). To resolve the 13 neutral amino acids one method utilizes a background electrolyte containing gamma-cyclodextrin and sodium taurocholate micelles. The acidic amino acid enantiomers were resolved with gamma-cyclodextrin alone. These methods allow detection limits down to 5 nM for the neutral amino acids and 500 nM for acidic amino acids and were used to analyze samples collected from Mono Lake with minimal sample preparation.
C1 [Creamer, Jessica S.; Mora, Maria F.; Willis, Peter A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Willis, PA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM peter.a.willis@jpl.nasa.gov
FU Planetary Instrument Concepts for the Advancement of Solar System
Observations (PICASSO) Program; NASA Postdoctoral Program (NPP) at the
Jet Propulsion Laboratory
FX The work done in this article was done at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. Financial support was provided by
The Planetary Instrument Concepts for the Advancement of Solar System
Observations (PICASSO) Program and the NASA Postdoctoral Program (NPP)
at the Jet Propulsion Laboratory, administered by Universities Space
Research Association through a contract with NASA. U.S. Government
sponsor is acknowledged. The image of Europa in the table of contents
and abstract graphics appears courtesy of NASA/JPL-Caltech/SETI
Institute.
NR 66
TC 0
Z9 0
U1 23
U2 23
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0003-2700
EI 1520-6882
J9 ANAL CHEM
JI Anal. Chem.
PD JAN 17
PY 2017
VL 89
IS 2
BP 1329
EP 1337
DI 10.1021/acs.analchem.6b04338
PG 9
WC Chemistry, Analytical
SC Chemistry
GA EI4IX
UT WOS:000392458100042
PM 28194989
ER
PT J
AU Richardson, JA
Wilson, JA
Connor, CB
Bleacher, JE
Kiyosugi, K
AF Richardson, Jacob A.
Wilson, James A.
Connor, Charles B.
Bleacher, Jacob E.
Kiyosugi, Koji
TI Recurrence rate and magma effusion rate for the latest volcanism on
Arsia Mons, Mars
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Mars; lava flows; recurrence rate estimation; magma flux; Monte Carlo
ID MOUNTAIN GLACIER DEPOSITS; THARSIS PROVINCE; PAVONIS MONS; LAVA FLOWS;
RHEOLOGIES; MODEL; FIELD; AGES; ICE
AB Magmatism and volcanism have evolved the Martian lithosphere, surface, and climate throughout the history of Mars. Constraining the rates of magma generation and timing of volcanism on the surface clarifies the ways in which magma and volcanic activity have shaped these Martian systems. The ages of lava flows on other planets are often estimated using impact crater counts, assuming that the number and size-distribution of impact craters per unit area reflect the time the lava flow has been on the surface and exposed to potential impacts. Here we show that impact crater age model uncertainty is reduced by adding stratigraphic information observed at locations where neighboring lavas abut each other, and demonstrate the significance of this reduction in age uncertainty for understanding the history of a volcanic field comprising 29 vents in the 110-km-diameter caldera of Arsia Mons, Mars. Each vent within this caldera produced lava flows several to tens of kilometers in length; these vents are likely among the youngest on Mars, since no impact craters in their lava flows are larger than 1 km in diameter. First, we modeled the age of each vent with impact crater counts performed on their corresponding lava flows and found very large age uncertainties for the ages of individual vents, often spanning the estimated age for the entire volcanic field. The age model derived from impact crater counts alone is broad and unimodal, with estimated peak activity in the field around 130 Ma. Next we applied our volcano event age model (VEAM), which uses a directed graph of stratigraphic relationships and random sampling of the impact crater age determinations to create alternative age models. Monte Carlo simulation was used to create 10,000 possible vent age sets. The recurrence rate of volcanism is calculated for each possible age set, and these rates are combined to calculate the median recurrence rate of all simulations. Applying this approach to the 29 volcanic vents, volcanism likely began around 200-300 Ma then first peaked around 150 Ma, with an average production rate of 0.4 vents per Myr. The recurrence rate estimated including stratigraphic data is distinctly bimodal, with a second, lower peak in activity around 100 Ma. Volcanism then waned until the final vents were produced 10-90 Ma. Based on this model, volume flux is also bimodal, reached a peak rate of 1-8 km(3) Myr(-1) by 150 Ma and remained above half this rate until about 90 Ma, after which the volume flux diminished greatly. The onset of effusive volcanism from 200-150 Ma might be due to a transition of volcanic style away from explosive volcanism that emplaced tephra on the western flank of Arsia Mons, while the waning of volcanism after the 150 Ma peak might represent a larger-scale diminishing of volcanic activity at Arsia Mons related to the emplacement of flank apron lavas. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Richardson, Jacob A.; Wilson, James A.; Connor, Charles B.] Univ S Florida, Sch Geosci, Tampa, FL USA.
[Richardson, Jacob A.; Bleacher, Jacob E.] NASA, Planetary Geol Geophys & Geochem Lab, Goddard Space Flight Ctr, Code 698, Greenbelt, MD 20771 USA.
[Kiyosugi, Koji] Kobe Univ, Org Adv & Integrated Res, Nada Ku, 1-1 Rokkodai Cho, Kobe, Hyogo 6578501, Japan.
EM jacob.a.richardson@nasa.gov
FU NASA Mars Data Analysis Program [NNX14AN02G, 13-MDAP13-0026]; NSF [ACI
1339768]; NASA Postdoctoral Program
FX Mapping and data analysis were funded through the NASA Mars Data
Analysis Program, grant #NNX14AN02G, 13-MDAP13-0026. The VEAM code was
developed with funding from the NSF (ACI 1339768). J. Richardson's
research was supported by the NASA Postdoctoral Program administered by
Universities Space Research Association under contract with NASA. J.
Richardson would like to thank Susan Conway for an invaluable CTX
projection code. We also thank Lionel Wilson and an anonymous reviewer
for valuable feedback that helped improve this manuscript.
NR 40
TC 0
Z9 0
U1 2
U2 2
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
EI 1385-013X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD JAN 15
PY 2017
VL 458
BP 170
EP 178
DI 10.1016/j.epsl.2016.10.040
PG 9
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EI7NO
UT WOS:000392685100016
ER
PT J
AU Yokoyama, T
Misawa, K
Okano, O
Shih, CY
Nyquist, LE
Simon, JI
Tappa, MJ
Yoneda, S
AF Yokoyama, Tatsunori
Misawa, Keiji
Okano, Osamu
Shih, Chi-Yu
Nyquist, Laurence E.
Simon, Justin I.
Tappa, Michael J.
Yoneda, Shigekazu
TI Extreme early solar system chemical fractionation recorded by
alkali-rich clasts contained in ordinary chondrite breccias
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE chondritic breccias; moderately volatile elements; K-Ca and Rb-Sr dating
ID RB-SR CHRONOLOGY; K-CA; REFRACTORY INCLUSIONS; DECAY CONSTANTS; LUNAR
GRANITES; IRON METEORITE; ALLENDE; EARTH; GEOCHEMISTRY; ABUNDANCES
AB New K-Ca and Rb-Sr isotopic analyses have been performed on alkali-rich igneous rock fragments in the Yamato (Y)-74442 and Bhola LL-chondritic breccias to better understand the extent and timing of alkali enrichments in the early solar system. The Y-74442 fragments yield a K-Ca age of 4.41 +/- 0.28 Ga for lambda(K-40 =) 0.5543 Ga-1 with an initial Ca-40/Ca-44 ratio of 47.1618 +/- 0.0032. Studying the same fragments with the Rb-Sr isotope system yields an age of 4.420 +/- 0.031 Ga for lambda(Rb-87) = 0.01402 Ga-1 with an initial ratio of Sr-87/Sr-86 = 0.7203 +/- 0.0044. An igneous rock fragment contained in Bhola shows a similar alkali fractionation pattern to those of Y-74442 fragments but does not plot on the K-Ca or Rb-Sr isochron of the Y-74442 fragments. Calcium isotopic compositions of whole-rock samples of angrite and chondrites are primordial, indistinguishable from mantle-derived terrestrial rocks, and here considered to represent the initial composition of bulk silicate Earth. The initial epsilon Ca-40 value determined for the source of the alkali clasts in Y-74442 that is similar to 0.5 epsilon-units higher than the solar system value implies an early alkali enrichment.
Multi-isotopic studies on these alkali-rich fragments reveal that the source material of Y-74442 fragments had elemental ratios of K/Ca = 0.43 +/- 0.18, Rb/Sr = 3.45 +/- 0.66 and K/Rb similar to 170, that may have formed from mixtures of an alkali-rich component (possibly an alkali-enriched gaseous reservoir produced by fractionation of early nebular condensates) and chondritic components that were flash-heated during an impact event on the LL-chondrite parent body similar to 4.42 Ga ago. Further enrichments of potassium and rubidium relative to calcium and strontium as well as a mutual alkali-fractionation (K/Rb similar to 50 and heavier alkali-enrichment) would have likely occurred during subsequent cooling and differentiation of this melt. Alkali fragments in Bhola might have undergone similar solid-vapor fractionation processes to those of Y-74442 fragments but appear to have formed via a distinct impact melting event. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Yokoyama, Tatsunori; Misawa, Keiji] SOKENDAI, Dept Polar Sci, 10-3 Midoricho, Tachikawa, Tokyo 1908518, Japan.
[Yokoyama, Tatsunori; Misawa, Keiji] Univ Space Res Assoc, Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77058 USA.
[Yokoyama, Tatsunori; Yoneda, Shigekazu] Natl Museum Nat & Sci, 4-1-1 Amakubo, Tsukuba, Ibaraki 3050005, Japan.
[Misawa, Keiji] Natl Inst Polar Res, 10-3 Midoricho, Tachikawa, Tokyo 1908518, Japan.
[Okano, Osamu] Okayama Univ, Grad Sch Nat Sci & Technol, 3-1-1 Tsushimanaka, Okayama 7008530, Japan.
[Shih, Chi-Yu] NASA, Johnson Space Ctr, Jacobs, Mail Code XI3, Houston, TX 77058 USA.
[Nyquist, Laurence E.; Simon, Justin I.; Tappa, Michael J.] NASA, Ctr Isotope Cosmochem & Geochronol, Astromat Res & Explorat Sci, Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA.
[Tappa, Michael J.] NASA, Aerodyne Ind, Jacobs JETS Contract, Johnson Space Ctr, Houston, TX 77058 USA.
[Yokoyama, Tatsunori] Japan Atom Energy Agcy, Tono Geosci Ctr, 959-31 Izumichojorinji, Toki, Gifu 5095102, Japan.
[Tappa, Michael J.] Boston Coll, Earth & Environm Sci, Devlin Hall 213,140 Commonwealth Ave, Chestnut Hill, MA 02467 USA.
EM yokoyama.tatsunori@jaea.go.jp
FU JSPS (KAKENHI Grant) [15H03754]; NIPR; Lunar and Planetary Institute
(LPI); NASA [10-LASER10-0077]
FX We are grateful to the National Institute of Polar Research and the
Smithsonian National Museum of Natural History for allocating the
meteorite specimens of Yamato-74442 and Bhola (USNM 1806), respectively.
We also thank K. Yamashita for supply of the D'Orbigny sample. TY wants
to thank H. Minowa and T. Fukuoka for their help during the course of
Imaging Plate experiments. Constructive comments from a reviewer
improved and clarified the manuscript. This work was partly supported by
funds from the JSPS (KAKENHI Grant Number 15H03754 to KM), NIPR Research
Program (KP-6), Lunar and Planetary Institute (LPI) and NASA
(10-LASER10-0077 to JIS). This is LPI contribution 001979.
NR 34
TC 0
Z9 0
U1 2
U2 2
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
EI 1385-013X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD JAN 15
PY 2017
VL 458
BP 233
EP 240
DI 10.1016/j.epsl.2016.10.037
PG 8
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EI7NO
UT WOS:000392685100022
ER
PT J
AU Jiang, NB
Mance, JG
Slipchenko, MN
Felver, JJ
Stauffer, HU
Yi, TX
Danehy, PM
Roy, S
AF Jiang, Naibo
Mance, Jason G.
Slipchenko, Mikhail N.
Felver, Josef J.
Stauffer, Hans U.
Yi, Tongxun
Danehy, Paul M.
Roy, Sukesh
TI Seedless velocimetry at 100 kHz with picosecond-laser
electronic-excitation tagging
SO OPTICS LETTERS
LA English
DT Article
ID VELOCITY-MEASUREMENTS; AIR
AB Picosecond-laser electronic-excitation tagging (PLEET), a seedless picosecond-laser-based velocimetry technique, is demonstrated in non-reactive flows at a repetition rate of 100 kHz with a 1064 nm, 100 ps burst-mode laser. The fluorescence lifetime of the PLEET signal was measured in nitrogen, and the laser heating effects were analyzed. PLEET experiments with a free jet of nitrogen show the ability to measure multi-point flow velocity fluctuations at a 100 kHz detection rate or higher. Both spectral and dynamic mode decomposition analyses of velocity on a Ma = 0.8 free jet show two dominant Strouhal numbers around 0.24 and 0.48, respectively, well within the shear-layer flapping frequencies of the free jets. This technique increases the laser-tagging repetition rate for velocimetry to hundreds of kilohertz. PLEET is suitable for subsonic through supersonic laminar- and turbulent-flow velocity measurements. (C) 2017 Optical Society of America
C1 [Jiang, Naibo; Mance, Jason G.; Slipchenko, Mikhail N.; Felver, Josef J.; Stauffer, Hans U.; Yi, Tongxun; Roy, Sukesh] Spectral Energies LLC, 5100 Springfield St, Dayton, OH 45431 USA.
[Slipchenko, Mikhail N.] Purdue Univ, Sch Mech Engn, W Lafayette, IN 47907 USA.
[Danehy, Paul M.] NASA, Adv Measurements & Data Syst Branch, Langley Res Ctr, Hampton, VA 23681 USA.
RP Roy, S (reprint author), Spectral Energies LLC, 5100 Springfield St, Dayton, OH 45431 USA.
EM roy.sukesh@gmail.com
FU Stennis Space Center [NNX15CL24C]
FX Stennis Space Center (NNX15CL24C).
NR 19
TC 0
Z9 0
U1 0
U2 0
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 0146-9592
EI 1539-4794
J9 OPT LETT
JI Opt. Lett.
PD JAN 15
PY 2017
VL 42
IS 2
BP 239
EP 242
DI 10.1364/OL.42.000239
PG 4
WC Optics
SC Optics
GA EI0VN
UT WOS:000392193100017
PM 28081082
ER
PT J
AU Sehlke, A
Whittington, AG
AF Sehlke, Alexander
Whittington, Alan G.
TI The viscosity of planetary tholeiitic melts: A configurational entropy
model (vol 191, pg 277, 2016)
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Correction
C1 [Sehlke, Alexander] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Whittington, Alan G.] Univ Missouri, Dept Geol Sci, Columbia, MO USA.
RP Sehlke, A (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
OI Sehlke, Alexander/0000-0001-7929-1776
NR 1
TC 0
Z9 0
U1 2
U2 2
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
EI 1872-9533
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JAN 15
PY 2017
VL 197
BP 474
EP 475
DI 10.1016/j.gca.2016.10.041
PG 2
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EG4BF
UT WOS:000390987700029
ER
PT J
AU Kharuk, VI
Im, ST
Petrov, IA
Golyukov, AS
Ranson, KJ
Yagunov, MN
AF Kharuk, Viacheslav I.
Im, Sergei T.
Petrov, Ilya A.
Golyukov, Alexei S.
Ranson, Kenneth J.
Yagunov, Mikhail N.
TI Climate-induced mortality of Siberian pine and fir in the Lake Baikal
Watershed, Siberia
SO FOREST ECOLOGY AND MANAGEMENT
LA English
DT Article
DE Water stress; Conifer mortality; Lake Baikal Region; Drought; Aridity
increase; Forest health
ID DYNAMICS; DECLINE; IMPACTS; DROUGHT; REGION
AB Siberian pine (Pinus sibirica) and fir (Abies sibirica) (so called "dark needle conifers", DNC) showed decreased radial growth increment within the Lake Baikal watershed since the 1980s with increasing mortality recorded since the year 2000. Tree ring width was strongly correlated with vapor pressure deficit, aridity and root zone moisture. Water stress from droughts made trees more susceptible to insect attacks causing mortality in about 10% of DNC stands within the Lake Baikal watershed. Within Siberia DNC mortality increased in the southern part of the DNC range. Biogeographically, tree mortality was located within the DNC - forest-steppes transition. Tree mortality was significantly correlated with drought and soil moisture anomalies.
Within the interior of the DNC range mortality occurred within relief features with high water stress risk (i.e., steep convex south facing slopes with shallow well drained soils). In general, DNC mortality in Siberia was induced by increased aridity and severe drought (inciting factors) in synergy with biotic attacks (contributing factor). In future climate scenarios with predicted increase in aridity DNC could be eliminated from the southern part of its current range and will be replaced by drought-resistant conifers and broadleaf species (e.g., Larix sibirica, Pinus silvestris, and Betula pubescence). (C) 2016 Elsevier B.V. All rights reserved.
C1 [Kharuk, Viacheslav I.; Im, Sergei T.; Petrov, Ilya A.; Golyukov, Alexei S.] Sukachev Inst Forest, Acad 50-28, Krasnoyarsk 660036, Russia.
[Kharuk, Viacheslav I.; Im, Sergei T.; Golyukov, Alexei S.] Siberian Fed Univ, Krasnoyarsk 660041, Russia.
[Im, Sergei T.] Siberian State Aerosp Univ, Krasnoyarsk 660014, Russia.
[Ranson, Kenneth J.] NASAs Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Yagunov, Mikhail N.] Russian Ctr Forest Protect, Krasnoyarsk 660036, Russia.
RP Kharuk, VI (reprint author), Sukachev Inst Forest, Acad 50-28, Krasnoyarsk 660036, Russia.
EM kharuk@ksc.krasn.ru
FU Russian Science Fund (RNF) [14-24-00112]; NASA's Terrestrial Ecology
Program; Ministry of Education and Science of the Russian Federation
[2.914.2014/K]
FX This research was supported by Russian Science Fund (RNF) [Grant No.
14-24-00112] and by NASA's Terrestrial Ecology Program. The Landsat data
processing was supported by the Ministry of Education and Science of the
Russian Federation (No. 2.914.2014/K).
NR 36
TC 1
Z9 1
U1 13
U2 13
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0378-1127
EI 1872-7042
J9 FOREST ECOL MANAG
JI For. Ecol. Manage.
PD JAN 15
PY 2017
VL 384
BP 191
EP 199
DI 10.1016/j.foreco.2016.10.050
PG 9
WC Forestry
SC Forestry
GA EG0MT
UT WOS:000390727600021
ER
PT J
AU Birch, SPD
Hayes, AG
Dietrich, WE
Howard, AD
Bristow, CS
Malaska, MJ
Moore, JM
Mastrogiuseppe, M
Hofgartner, JD
Williams, DA
White, OL
Soderblom, JM
Barnes, JW
Turtle, EP
Lunine, JI
Wood, CA
Neish, CD
Kirk, RL
Stofan, ER
Lorenz, RD
Lopes, RMC
AF Birch, S. P. D.
Hayes, A. G.
Dietrich, W. E.
Howard, A. D.
Bristow, C. S.
Malaska, M. J.
Moore, J. M.
Mastrogiuseppe, M.
Hofgartner, J. D.
Williams, D. A.
White, O. L.
Soderblom, J. M.
Barnes, J. W.
Turtle, E. P.
Lunine, J. I.
Wood, C. A.
Neish, C. D.
Kirk, R. L.
Stofan, E. R.
Lorenz, R. D.
Lopes, R. M. C.
TI Geomorphologic mapping of titan's polar terrains: Constraining surface
processes and landscape evolution
SO ICARUS
LA English
DT Article
DE Titan; Geological processes; Titan hydrology; Titan surface
ID CASSINI RADAR; FLUVIAL EROSION; SALINITY CRISIS; SEAS; TOPOGRAPHY;
LAKES; SHORELINES; EVAPORITES; MORPHOLOGY; FEATURES
AB We present a geomorphologic map of Titan's polar terrains. The map was generated from a combination of Cassini Synthetic Aperture Radar (SAR) and Imaging Science Subsystem imaging products, as well as altimetry, SARTopo and radargrammetry topographic datasets. In combining imagery with topographic data, our geomorphologic map reveals a stratigraphic sequence from which we infer process interactions between units. In mapping both polar regions with the same geomorphologic units, we conclude that processes that formed the terrains of the north polar region also acted to form the landscape we observe at the south. Uniform, SAR-dark plains are interpreted as sedimentary deposits, and are bounded by moderately dissected uplands. These plains contain the highest density of filled and empty lake depressions, and canyons. These units unconformably overlay a basement rock that outcrops as mountains and SARbright dissected terrains at various elevations across both poles. All these units are then superposed by surficial units that slope towards the seas, suggestive of subsequent overland transport of sediment. From estimates of the depths of the embedded empty depressions and canyons that drain into the seas, the SAR-dark plains must be >600 m thick in places, though the thickness may vary across the poles. At the lowest elevations of each polar region, there are large seas, which are currently liquid methane/ethane filled at the north and empty at the south. The large plains deposits and the surrounding hillslopes may represent remnant landforms that are a result of previously vast polar oceans, where larger liquid bodies may have allowed for a sustained accumulation of soluble and insoluble sediments, potentially forming layered sedimentary deposits. Coupled with vertical crustal movements, the resulting layers would be of varying solubilities and erosional resistances, allowing formation of the complex landscape that we observe today. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Birch, S. P. D.; Hayes, A. G.] Cornell Univ, Dept Earth & Atmospher Sci, Ithaca, NY 14853 USA.
[Hayes, A. G.; Mastrogiuseppe, M.; Hofgartner, J. D.; Lunine, J. I.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Dietrich, W. E.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
[Howard, A. D.] Univ Virginia, Dept Environm Sci, Clark Hall, Charlottesville, VA 22903 USA.
[Bristow, C. S.] Birkbeck Univ London, Dept Earth & Planetary Sci, London, England.
[Malaska, M. J.; Hofgartner, J. D.; Lopes, R. M. C.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Moore, J. M.] NASA Ames Res Facil, Div Space Sci, Moffett Field, CA USA.
[Williams, D. A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA.
[Soderblom, J. M.] MIT, Dept Earth Atmospher & Planetary Sci, Boston, MA USA.
[Barnes, J. W.] Univ Idaho, Dept Phys, Moscow, ID USA.
[Turtle, E. P.; Lorenz, R. D.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Wood, C. A.] Planetary Sci Inst Tucson, Tucson, AZ USA.
[Neish, C. D.] Univ Western Ontario, London, ON, Canada.
[Kirk, R. L.] US Geol Survey, Astrogeol Div, Flagstaff, AZ 86001 USA.
[Stofan, E. R.] UCL, Dept Earth & Planetary Sci, London WC1E 6BT, England.
RP Birch, SPD (reprint author), Cornell Univ, Dept Earth & Atmospher Sci, Ithaca, NY 14853 USA.
EM sb2222@cornell.edu
OI Birch, Samuel/0000-0002-4578-1694
FU NASA Cassini Data Analysis Program [NNX13AG03G]; NASA Earth and Space
Science Fellowship [5-PLANET5F-0011]; Outer Planets Research Program
[NNX14AT29G]; NASA; ESA; ASI
FX All data for this mapping project are located at the following webpage:
http://www.geomorph-sbirch.com/data-products/. SPDB, AGH, WED, JWB, EPT,
and RLK were funded by a NASA Cassini Data Analysis Program: Grant
NNX13AG03G, and SPDB by the NASA Earth and Space Science Fellowship
Program: Grant 5-PLANET5F-0011. DAW was funded for Titan geologic
mapping under grant NNX14AT29G from the Outer Planets Research Program.
This research was also supported by the Cassini-Huygens mission, a
cooperative endeavor of NASA, ESA, and ASI managed by JPL/Caltech under
a contract with NASA. We would like to thank two reviewers for their
comments on the manuscript. We would especially like to thank Thomas
Cornet for a very thorough and thoughtful review that significantly
improved the manuscript. Finally, we would also like to acknowledge the
entire Cassini RADAR team for the acquisition of the radar data, and
Paul Corlies for comments and revisions of earlier versions of this
manuscript.
NR 94
TC 0
Z9 0
U1 20
U2 20
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JAN 15
PY 2017
VL 282
BP 214
EP 236
DI 10.1016/j.icarus.2016.08.003
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA ED0PX
UT WOS:000388545500018
ER
PT J
AU Yu, Y
Michel, P
Schwartz, SR
Naidu, SP
Benner, LAM
AF Yu, Yang
Michel, Patrick
Schwartz, Stephen R.
Naidu, Shantanu P.
Benner, Lance A. M.
TI Ejecta cloud from the AIDA space project kinetic impact on the secondary
of a binary asteroid: I. mechanical environment and dynamical model
SO ICARUS
LA English
DT Article
DE Asteroids dynamics; Accretion; Collisional physics; Interplanetary dust;
Cratering
ID MOMENTUM-TRANSFER; DENSITY; PARTICLES; EVOLUTION; REGOLITH; ORIGIN
AB An understanding of the post-impact dynamics of ejecta clouds are crucial to the planning of a kinetic impact mission to an asteroid, and also has great implications for the history of planetary formation. The purpose of this article is to track the evolution of ejecta produced by AIDA mission, which targets for kinetic impact the secondary of near-Earth binary asteroid (65803) Didymos on 2022, and to feedback essential informations to AIDA's ongoing phase-A study. We present a detailed dynamic model for the simulation of an ejecta cloud from a binary asteroid that synthesizes all relevant forces based on a previous analysis of the mechanical environment. We apply our method to gain insight into the expected response of Didymos to the AIDA impact, including the subsequent evolution of debris and dust. The crater scaling relations from laboratory experiments are employed to approximate the distributions of ejecta mass and launching speed. The size distribution of fragments is modeled with a power law fitted from observations of real asteroid surface. A full-scale demonstration is simulated using parameters specified by the mission. We report the results of the simulation, which include the computed spread of the ejecta cloud and the recorded history of ejecta accretion and escape. The violent period of the ejecta evolution is found to be short, and is followed by a stage where the remaining ejecta is gradually cleared. Solar radiation pressure proves to be efficient in cleaning dust-size ejecta, and the simulation results after two weeks shows that large debris on polar orbits (perpendicular to the binary orbital plane) has a survival advantage over smaller ejecta and ejecta that keeps to low latitudes. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Yu, Yang; Michel, Patrick; Schwartz, Stephen R.] Univ Cote dAzur, CNRS, Lab Lagrange, Observ Cote dAzur, F-06304 Nice, France.
[Naidu, Shantanu P.; Benner, Lance A. M.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Yu, Yang] Observ Cote Azur, CNRS, UMR Lagrange 7293, Blvd Observ,CS 34229, F-06304 Nice 4, France.
RP Yu, Y (reprint author), Univ Cote dAzur, CNRS, Lab Lagrange, Observ Cote dAzur, F-06304 Nice, France.; Yu, Y (reprint author), Observ Cote Azur, CNRS, UMR Lagrange 7293, Blvd Observ,CS 34229, F-06304 Nice 4, France.
EM yuyang.thu@gmail.com
OI Schwartz, Stephen/0000-0001-5475-9379; Yu, Yang/0000-0001-9329-7015
FU ESA; NASA; European Commission [282703]; European Union [640351]
FX Y.Y., P.M., and S.R.S. acknowledge the support of ESA and NASA, and from
the NEOShield and NEOShield-2 projects, funded under the European
Commission's FP7 programme (2007-2013) under grant agreement No. 282703,
and the European Union's Horizon 2020 research and innovation programme
under grant agreement No. 640351, respectively. The reference parameters
of binary NEA 65803 Didymos are taken from the ESA AIM Team. The
simulations were performed using the Beowulf computing cluster licallo,
run by l'Observatoire de la Cote d'Azur, CNRS. For data visualization,
the authors made use of the freeware, multi-platform ray tracing
package, Persistence of Vision Raytracer (POV-Ray).
NR 40
TC 0
Z9 0
U1 10
U2 10
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JAN 15
PY 2017
VL 282
BP 313
EP 325
DI 10.1016/j.icarus.2016.09.008
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA ED0PX
UT WOS:000388545500023
ER
PT J
AU Libourel, G
Michel, P
Delbo, M
Ganino, C
Recio-Blanco, A
de Laverny, P
Zolensky, ME
Krot, AN
AF Libourel, Guy
Michel, Patrick
Delbo, Marco
Ganino, Clement
Recio-Blanco, Alejandra
de Laverny, Patrick
Zolensky, Michael E.
Krot, Alexander N.
TI Search for primitive matter in the Solar System
SO ICARUS
LA English
DT Article
DE Solar system formation; Solar system evolution
ID PARIS METEORITE; CORE FORMATION; PARENT BODY; CHONDRULES; ACCRETION;
CHONDRITE; DISK; PROTOPLANETS; CHRONOLOGY; EVOLUTION
AB In this note, we show that neither the age of an object, nor its mineralogy is discriminant enough for revealing its primitiveness, and propose a new parameterization scheme based on the processes the matter underwent since its delivery to the Solar System. By ranking celestial objects and their constituents, two antagonistic sources of primitive materials in the protoplanetary disk emerge, one close to the Sun resulting from evaporation, condensation and melting of the protosolar molecular cloud dust followed by accretion into asteroidal bodies, and the other at large heliocentric distances resulting from agglomeration of the protosolar and solar dust into cometary bodies, the latter reservoir remaining poorly sampled so far. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Libourel, Guy; Michel, Patrick; Delbo, Marco; Recio-Blanco, Alejandra; de Laverny, Patrick] Univ Cote dAzur, OCA, CNRS, Blvd Observ,CS 34229, F-06304 Nice 4, France.
[Ganino, Clement] Univ Cote dAzur, OCA, CNRS, Geoazur, 250 Rue Albert Einstein, F-06560 Valbonne, France.
[Libourel, Guy; Krot, Alexander N.] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Sch Ocean Earth Sci & Technol, Honolulu, HI 96821 USA.
[Zolensky, Michael E.] NASA JSC, Astromat Res & Explorat Sci, 2101 NASA Pkwy, Houston, TX 77058 USA.
RP Libourel, G (reprint author), Univ Cote dAzur, OCA, CNRS, Blvd Observ,CS 34229, F-06304 Nice 4, France.; Libourel, G (reprint author), Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Sch Ocean Earth Sci & Technol, Honolulu, HI 96821 USA.
EM guy.libourel@oca.eu
FU BQR OCA; CNES BCU5 grant; CNES BCU70 grant
FX We are grateful to several colleagues from OCA and elsewhere for useful
discussions and suggestions. Editorial handling by Giovanna Tinetti and
constructive reviews by two anonymous reviewers are all gratefully
acknowledged. This work was inspired by some of the outcomes of the 2014
workshop on "Primitive material in the Solar System I" organized in
Villefranche sur Mer
(https://www-n.oca.eu/michel/WorkshopPrimitive2014/), and was supported
by the BQR OCA and CNES BCU5 grant to G. Libourel, and CNES BCU70 grant
to P. Michel and M. Delbo.
NR 35
TC 0
Z9 0
U1 8
U2 8
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JAN 15
PY 2017
VL 282
BP 375
EP 379
DI 10.1016/j.icarus.2016.09.014
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA ED0PX
UT WOS:000388545500028
ER
PT J
AU Hudson, RL
Loeffler, MJ
Gerakines, PA
AF Hudson, R. L.
Loeffler, M. J.
Gerakines, P. A.
TI Infrared spectra and band strengths of amorphous and crystalline N2O
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
ID SOLID NITROUS-OXIDE; CARBON-DIOXIDE; OPTICAL-CONSTANTS; ICES RELEVANT;
VIBRATIONAL-SPECTRA; REFRACTIVE-INDEX; SPECTROSCOPY; ABSORPTION;
MOLECULES; CO2
AB Infrared transmission spectra from 4000 to 400 cm(-1), and associated band strengths and absorption coefficients, are presented for the first time for both amorphous and crystalline N2O. Changes in the spectra as a function of ice thickness and ice temperature are shown. New measurements of density, refractive index, and specific refraction are reported for amorphous and crystalline N2O. Comparisons are made to published results, and the most-likely reason for some recent disagreements in the literature is discussed. As with CO2, its isoelectronic congener, the formation of amorphous N2O is found to require greater care than the formation of amorphous solids from more-polar molecules.
C1 [Hudson, R. L.; Loeffler, M. J.; Gerakines, P. A.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA.
RP Hudson, RL (reprint author), NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA.
EM reggie.hudson@nasa.gov
FU NASA's Astrophysics Research and Analysis program; NASA Astrobiology
Institute
FX This work was supported by NASA's Astrophysics Research and Analysis
program and assisted by a grant to the Goddard Center for Astrobiology
from the NASA Astrobiology Institute.
NR 51
TC 0
Z9 0
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0021-9606
EI 1089-7690
J9 J CHEM PHYS
JI J. Chem. Phys.
PD JAN 14
PY 2017
VL 146
IS 2
AR 024304
DI 10.1063/1.4973548
PG 9
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA EK5PN
UT WOS:000393978400016
PM 28088158
ER
PT J
AU Freitas, SR
Panetta, J
Longo, KM
Rodrigues, LF
Moreira, DS
Rosario, NE
Dias, PLS
Dias, MAFS
Souza, EP
Freitas, ED
Longo, M
Frassoni, A
Fazenda, AL
Silva, CMSE
Pavani, CAB
Eiras, D
Franca, DA
Massaru, D
Silva, FB
Santos, FC
Pereira, G
Camponogara, G
Ferrada, GA
Campos, HF
Velho, HFC
Menezes, I
Freire, JL
Alonso, MF
Gacita, MS
Zarzur, M
Fonseca, RM
Lima, RS
Siqueira, RA
Braz, R
Tomita, S
Oliveira, V
Martins, LD
AF Freitas, Saulo R.
Panetta, Jairo
Longo, Karla M.
Rodrigues, Luiz F.
Moreira, Demerval S.
Rosario, Nilton E.
Silva Dias, Pedro L.
Silva Dias, Maria A. F.
Souza, Enio P.
Freitas, Edmilson D.
Longo, Marcos
Frassoni, Ariane
Fazenda, Alvaro L.
Santos e Silva, Claudio M.
Pavani, Claudio A. B.
Eiras, Denis
Franca, Daniela A.
Massaru, Daniel
Silva, Fernanda B.
Santos, Fernando C.
Pereira, Gabriel
Camponogara, Glauber
Ferrada, Gonzalo A.
Campos, Haroldo F.
Campos Velho, Haroldo F.
Menezes, Isilda
Freire, Julliana L.
Alonso, Marcelo F.
Gacita, Madeleine S.
Zarzur, Mauricio
Fonseca, Rafael M.
Lima, Rafael S.
Siqueira, Ricardo A.
Braz, Rodrigo
Tomita, Simone
Oliveira, Valter
Martins, Leila D.
TI The Brazilian developments on the Regional Atmospheric Modeling System
(BRAMS 5.2): an integrated environmental model tuned for tropical areas
SO GEOSCIENTIFIC MODEL DEVELOPMENT
LA English
DT Article
ID WAVE OPTICAL-PROPERTIES; CLOUD MICROPHYSICS PARAMETERIZATION; CONVECTIVE
TRIGGER FUNCTION; TRACER TRANSPORT MODEL; YAMADA LEVEL-3 MODEL;
BOUNDARY-LAYER; AIR-QUALITY; NUMERICAL-SIMULATION; CLIMATE MODELS;
SOUTH-AMERICA
AB We present a new version of the Brazilian developments on the Regional Atmospheric Modeling System (BRAMS), in which different previous versions for weather, chemistry, and carbon cycle were unified in a single integrated modeling system software. This new version also has a new set of state-of-the-art physical parameterizations and greater computational parallel and memory usage efficiency. The description of the main model features includes several examples illustrating the quality of the transport scheme for scalars, radiative fluxes on surface, and model simulation of rainfall systems over South America at different spatial resolutions using a scale aware convective parameterization. Additionally, the simulation of the diurnal cycle of the convection and carbon dioxide concentration over the Amazon Basin, as well as carbon dioxide fluxes from biogenic processes over a large portion of South America, are shown. Atmospheric chemistry examples show the model performance in simulating near-surface carbon monoxide and ozone in the Amazon Basin and the megacity of Rio de Janeiro. For tracer transport and dispersion, the model capabilities to simulate the volcanic ash 3-D redistribution associated with the eruption of a Chilean volcano are demonstrated. The gain of computational efficiency is described in some detail. BRAMS has been applied for research and operational forecasting mainly in South America. Model results from the operational weather forecast of BRAMS on 5 km grid spacing in the Center for Weather Forecasting and Climate Studies, INPE/Brazil, since 2013 are used to quantify the model skill of near-surface variables and rainfall. The scores show the reliability of BRAMS for the tropical and subtropical areas of South America. Requirements for keeping this modeling system competitive regarding both its functionalities and skills are discussed. Finally, we highlight the relevant contribution of this work to building a South American community of model developers.
C1 [Freitas, Saulo R.; Longo, Karla M.; Rodrigues, Luiz F.; Frassoni, Ariane; Pavani, Claudio A. B.; Eiras, Denis; Franca, Daniela A.; Massaru, Daniel; Silva, Fernanda B.; Ferrada, Gonzalo A.; Freire, Julliana L.; Gacita, Madeleine S.; Fonseca, Rafael M.; Lima, Rafael S.; Siqueira, Ricardo A.; Braz, Rodrigo; Tomita, Simone; Oliveira, Valter] Inst Nacl Pesquisas Espaciais, Ctr Previsao Tempo & Estudos Climat, Cachoeira Paulista, SP, Brazil.
[Panetta, Jairo] Inst Tecnol Aeronaut, Div Ciencia Computacao, Sao Jose Dos Campos, SP, Brazil.
[Moreira, Demerval S.] Univ Estadual Paulista Unesp, Fac Ciencias, Bauru, SP, Brazil.
[Moreira, Demerval S.] Ctr Meteorol Bauru IPMet, Bauru, SP, Brazil.
[Rosario, Nilton E.] Univ Fed Sao Paulo, Dept Ciencias Ambientais, Diadema, SP, Brazil.
[Silva Dias, Pedro L.; Silva Dias, Maria A. F.; Freitas, Edmilson D.; Camponogara, Glauber] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Sao Paulo, SP, Brazil.
[Souza, Enio P.] Univ Fed Campina Grande, Dept Ciencias Atmosfer, Campina Grande, PB, Brazil.
[Longo, Marcos] Embrapa Informat Agr, Campinas, SP, Brazil.
[Fazenda, Alvaro L.] Univ Fed Sao Paulo, Inst Ciencia & Tecnol, Sao Jose Dos Campos, SP, Brazil.
[Santos e Silva, Claudio M.] Univ Fed Rio Grande do Norte, Dept Ciencias Atmosfer & Climat, Programa Pos Grad Ciencias Climat, Natal, RN, Brazil.
[Santos, Fernando C.] Inst Nacl Pesquisas Espaciais, Ctr Ciencias Sistema, Sao Jose Dos Campos, SP, Brazil.
[Pereira, Gabriel] Univ Fed Sao Joao Del Rei, Dept Geociencias, Sao Joao Del Rei, MG, Brazil.
[Campos Velho, Haroldo F.] Inst Nacl Pesquisas Espaciais, Lab Associado Computacao & Matemat Aplica, Sao Jose Dos Campos, Brazil.
[Menezes, Isilda] Univ Evora, Inst Ciencias Agr & Ambientais Mediterr, Evora, Portugal.
[Menezes, Isilda] Univ Lusofona Humanidades & Tecnol, Ctr Interdisciplinar Desenvolvimento Ambient Gest, Lisbon, Portugal.
[Alonso, Marcelo F.] Univ Fed Pelotas, Fac Meteorol, Pelotas, RS, Brazil.
[Martins, Leila D.] Unive Tecnol Fed Parana, Londrina, PR, Brazil.
[Freitas, Saulo R.; Longo, Karla M.] NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Goddard Earth Sci Technol & Res Global Modeling &, Greenbelt, MD USA.
RP Freitas, SR (reprint author), Inst Nacl Pesquisas Espaciais, Ctr Previsao Tempo & Estudos Climat, Cachoeira Paulista, SP, Brazil.; Freitas, SR (reprint author), NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Goddard Earth Sci Technol & Res Global Modeling &, Greenbelt, MD USA.
EM saulo.r.freitas@nasa.gov
RI Camponogara, Glauber/F-1312-2017; Freitas, Saulo/A-2279-2012;
OI Camponogara, Glauber/0000-0001-9171-8402; Freitas,
Saulo/0000-0002-9879-646X; Freitas, Edmilson/0000-0001-8783-2747
FU CNPq [306340/2011-9]; FAPESP [2014/01563-1, 2015/10206-0, 2014/01564-8];
Earth System Research Laboratory at the National Oceanic and Atmospheric
Administration (ESRL/NOAA), Boulder, USA
FX S. R. Freitas acknowledges partial support of this work by CNPq
(306340/2011-9) and FAPESP (2014/01563-1 and 2015/10206-0) and K. M.
Longo acknowledges partial support of this work by FAPESP
(2014/01564-8). This work was partially carried out during the
sabbatical year of S. R. Freitas and K. M. Longo at the Earth System
Research Laboratory at the National Oceanic and Atmospheric
Administration (ESRL/NOAA), Boulder, USA. Both authors acknowledge the
partial support by this institution. The authors acknowledge Georg Grell
from ESRL/NOAA and Michael Baldauf from Deutscher Wetterdienst (DWD),
Germany, for their collaboration on key aspects of this modeling system.
NR 165
TC 0
Z9 0
U1 1
U2 1
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1991-959X
EI 1991-9603
J9 GEOSCI MODEL DEV
JI Geosci. Model Dev.
PD JAN 13
PY 2017
VL 10
IS 1
BP 189
EP 222
DI 10.5194/gmd-10-189-2017
PG 34
WC Geosciences, Multidisciplinary
SC Geology
GA EK1KV
UT WOS:000393685100002
ER
PT J
AU Bocchini, PJ
Sudbrack, CK
Noebe, RD
Dunand, DC
Seidman, DN
AF Bocchini, Peter J.
Sudbrack, Chantal K.
Noebe, Ronald D.
Dunand, David C.
Seidman, David N.
TI Microstructural and creep properties of boron- and zirconium-containing
cobalt-based superalloys
SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES
MICROSTRUCTURE AND PROCESSING
LA English
DT Article
DE Cobalt-base superalloys; Gamma prime; Atom-probe tomography (APT); Grain
boundaries; Creep
ID GRAIN-BOUNDARY SEGREGATION; ATOM-PROBE TOMOGRAPHY; HIGH-TEMPERATURE
OXIDATION; SINGLE-CRYSTALS; GAMMA'-CO-3(AL,W) PHASE; INTERNAL
INTERFACES; SUPER-ALLOY; GAMMA'; DEFORMATION; NICKEL
AB The effects of micro-additions of boron and zirconium on grain-boundary (GB) structure and strength in polycrystalline y(f.c.c.) plus y'(L1(2)) strengthened Co-9.5A1-7.5W-X at% alloys (X=0-Ternary, 0.05B, 0.01B, 0.05Zr, and 0.005B-0.05Zr at%) are studied. Creep tests performed at 850 degrees C demonstrate that GB strength and cohesion limit the creep resistance and ductility of the ternary B- and Zr-free alloy due to intergranular fracture. Alloys with 0.05B and 0.005B-0.05Zr both exhibit improved creep strength due to enhanced GB cohesion, compared to the baseline ternary Co-9.5A1-7.5W alloy, but alloys containing 0.01B or 0.05Zr additions display no benefit. Atom-probe tomography (APT) is utilized to measure GB segregation, where B and Zr are demonstrated to segregate at GBs. A Gibbsian interfacial excess of 5.57 +/- 1.04 atoms nm(-2) was found for B at a GB in the 0.01B alloy and 2.88 +/- 0.81 and 2.40 +/- 0.84 atoms nm(-2) for B and Zr, respectively, for the 0.005B-0.05Zr alloy. The GBs in the highest B-containing (0.05B) alloy exhibit micrometer-sized boride precipitates with adjacent precipitate denuded-zones (PDZs), whereas secondary precipitation at the GBs is absent in the other four alloys. The 0.05B alloy has the smallest room temperature yield strength, by 6%, which is attributed to the PDZs, but it exhibits the largest increase in creep strength (with an similar to 2.5 order of magnitude decrease in the minimum strain rate for a given stress at 850 degrees C) over the baseline Co-9.5A1-7.5W alloy.
C1 [Bocchini, Peter J.; Dunand, David C.; Seidman, David N.] Northwestern Univ, Dept Mat Sci & Engn, 2220 Campus Dr, Evanston, IL 60208 USA.
[Sudbrack, Chantal K.; Noebe, Ronald D.; Dunand, David C.] NASA, Glenn Res Ctr, Mat & Struct Div, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
[Seidman, David N.] Northwestern Univ, Ctr Atom Probe Tomog, 2220 Campus Dr, Evanston, IL 60208 USA.
RP Bocchini, PJ (reprint author), Northwestern Univ, Dept Mat Sci & Engn, 2220 Campus Dr, Evanston, IL 60208 USA.
EM pbocchin@gmail.com
FU US Department of Energy, Office of Basic Energy Sciences
[DE-FG02-98ER45721]; NASA [NNX14AF45H]; NSF-MRI [DMR-0420532]; ONR-DURIP
[N00014-0400798, N00014-0610539, N00014-0910781]; National Science
Foundation MRSEC Program [DMR-1121262]; NSF MRSEC program [DMR-112162];
Fixed Wing project; Initiative for Sustainability and Energy at
Northwestern (ISEN)
FX This research was supported by the US Department of Energy, Office of
Basic Energy Sciences (Dr. John Vetrano, grant monitor) through grant
DE-FG02-98ER45721. P.J.B. received partial support from the NASA
Aeronautics Scholarship Program (Grant No. NNX14AF45H) and Fixed Wing
project. APT measurements were performed at the Northwestern University
Center for Atom-Probe Tomography (NUCAPT). The APT system was purchased
and upgraded with funding from NSF-MRI (DMR-0420532) and ONR-DURIP
(N00014-0400798, N00014-0610539 and N00014-0910781) grants. NUCAPT is a
shared facility of the Materials Research Center of NU, supported by the
National Science Foundation MRSEC Program (DMR-1121262). The authors
also gratefully acknowledge the Initiative for Sustainability and Energy
at Northwestern (ISEN) for grants to upgrade the capabilities of NUCAPT.
This work made use of Northwestern's Materials Research Center's core
facilities funded by the NSF MRSEC program (DMR-112162). TEM research
was performed at the Northwestern University Atomic and Nanoscale
Characterization Experimental (NUANCE) Center. The authors would like to
thank research associate professor D. Isheim for managing NUCAPT, Dr.
S.-I. Baik (Northwestern University) for assistance with transmission
electron microscopy, Drs. Dave Ellis and Cheryl Bowman (NASA Glenn
Research) for assistance with creep experiments, Mr. Grant Feichter and
Jesse Bierer for arc melting and heat treating (NASA Glenn Research),
and Dr. Tim Gabb (NASA Glenn Research) for helpful discussions.
NR 55
TC 0
Z9 0
U1 1
U2 1
PU ELSEVIER SCIENCE SA
PI LAUSANNE
PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND
SN 0921-5093
EI 1873-4936
J9 MAT SCI ENG A-STRUCT
JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process.
PD JAN 13
PY 2017
VL 682
BP 260
EP 269
DI 10.1016/j.msea.2016.10.124
PG 10
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Metallurgy & Metallurgical Engineering
SC Science & Technology - Other Topics; Materials Science; Metallurgy &
Metallurgical Engineering
GA EJ1XM
UT WOS:000393003800030
ER
PT J
AU Zhuravleva, TB
Kabanov, DM
Nasrtdinov, IM
Russkova, TV
Sakerin, SM
Smirnov, A
Holben, BN
AF Zhuravleva, Tatiana B.
Kabanov, Dmitriy M.
Nasrtdinov, Ilmir M.
Russkova, Tatiana V.
Sakerin, Sergey M.
Smirnov, Alexander
Holben, Brent N.
TI Radiative characteristics of aerosol during extreme fire event over
Siberia in summer 2012
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID BIOMASS BURNING PARTICLES; SKY RADIANCE MEASUREMENTS; LIGHT-ABSORPTION;
OPTICAL-PROPERTIES; MICROPHYSICAL PROPERTIES; ORGANIC-CARBON; SPECTRAL
DEPENDENCE; SOLAR-RADIATION; SMOKE AEROSOL; BROWN CARBON
AB Microphysical and optical properties of aerosol were studied during a mega-fire event in summer 2012 over Siberia using ground-based measurements of spectral solar radiation at the AERONET site in Tomsk and satellite observations. The data were analysed using multi-year (2003-2013) measurements of aerosol characteristics under background conditions and for less intense fires, differing in burning biomass type, stage of fire, remoteness from observation site, etc. ("ordinary" smoke). In June-August 2012, the average aerosol optical depth (AOD, 500 nm) had been 0.95 +/- 0.86, about a factor of 6 larger than background values (0.16 +/- 0.08), and a factor of 2.5 larger than in ordinary smoke. The AOD values were extremely high on 2428 July and reached 3-5. A comparison with satellite observations showed that ground-based measurements in the region of Tomsk not only reflect the local AOD features, but are also characteristic for the territory of Western Siberia as a whole. Single scattering albedo (SSA, 440 nm) in this period ranged from 0.91 to 0.99 with an average of similar to 0.96 in the entire wavelength range of 440-1020 nm. The increase in absorptance of aerosol particles (SSA(440 nm) = 0.92) and decrease in SSA with wavelength observed in ordinary smoke agree with the data from multi-year observations in analogous situations in the boreal zone of USA and Canada. Volume aerosol size distribution in extreme and ordinary smoke had a bimodal character with significant prevalence of fine-mode particles, but in summer 2012 the mean median radius and the width of the fine-mode distribution somewhat increased. In contrast to data from multi-year observations, in summer 2012 an increase in the volume concentration and median radius of the coarse mode was observed with growing AOD.
The calculations of the average radiative effects of smoke and background aerosol are presented. Compared to background conditions and ordinary smoke, under the extreme smoke conditions the cooling effect of aerosol considerably intensifies: direct radiative effects (DRE) at the bottom (BOA) and at the top of the atmosphere (TOA) are -13, -35, and -60 W m(-2) and -5, -14, and -35 W m(-2) respectively. The maximal values of DRE were observed on 27 July (AOD(500 nm) = 3.5), when DRE(BOA) reached -150 W m(-2), while DRE(TOA) and DRE of the atmosphere were -75 W m(-2). During the fire event in summer 2012 the direct radiative effect efficiency varied in range: at the BOA it was -80- -40 W m(-2), at the TOA it was -50- -20 W m(-2) and in the atmosphere it was -35- -20 W m(-2).
C1 [Zhuravleva, Tatiana B.; Kabanov, Dmitriy M.; Nasrtdinov, Ilmir M.; Russkova, Tatiana V.; Sakerin, Sergey M.] VE Zuev Inst Atmospher Opt SB RAS, Div Radiat Components Climate & Opt Diagnost Envi, Tomsk, Russia.
[Smirnov, Alexander] Sci Syst & Applicat Inc, Lanham, MD USA.
[Smirnov, Alexander; Holben, Brent N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Zhuravleva, TB (reprint author), VE Zuev Inst Atmospher Opt SB RAS, Div Radiat Components Climate & Opt Diagnost Envi, Tomsk, Russia.
EM ztb@iao.ru
RI Smirnov, Alexander/C-2121-2009
OI Smirnov, Alexander/0000-0002-8208-1304
NR 74
TC 0
Z9 0
U1 4
U2 4
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1867-1381
EI 1867-8548
J9 ATMOS MEAS TECH
JI Atmos. Meas. Tech.
PD JAN 13
PY 2017
VL 10
IS 1
BP 179
EP 198
DI 10.5194/amt-10-179-2017
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EK1JT
UT WOS:000393682300001
ER
PT J
AU Alwood, JS
Ronca, AE
Mains, RC
Shelhamer, MJ
Smith, JD
Goodwin, TJ
AF Alwood, Joshua S.
Ronca, April E.
Mains, Richard C.
Shelhamer, Mark J.
Smith, Jeffrey D.
Goodwin, Thomas J.
TI From the bench to exploration medicine: NASA life sciences translational
research for human exploration and habitation missions
SO NPJ MICROGRAVITY
LA English
DT Article
ID LONG-DURATION SPACEFLIGHT; SPACE-FLIGHT; HUMAN CATALASE; IN-VIVO; MICE;
MICROGRAVITY; BONE; VIRULENCE; ASTRONAUTS; INCREASES
AB NASA's Space Biology and Human Research Program entities have recently spearheaded communications both internally and externally to coordinate the agency's translational research efforts. In this paper, we strongly advocate for translational research at NASA, provide recent examples of NASA sponsored early-stage translational research, and discuss options for a path forward. Our overall objective is to help in stimulating a collaborative research across multiple disciplines and entities that, working together, will more effectively and more rapidly achieve NASA's goals for human spaceflight.
C1 [Alwood, Joshua S.; Ronca, April E.; Smith, Jeffrey D.] NASA, Ames Res Ctr, Space BioSci Div, Moffett Field, CA 94035 USA.
[Ronca, April E.] Wake Forest Sch Med, Winston Salem, NC USA.
[Mains, Richard C.] Mains Associates, Berkeley, CA USA.
[Shelhamer, Mark J.] NASA, Human Res Program, Johnson Space Ctr, Houston, TX USA.
[Goodwin, Thomas J.] NASA, Biomed Res & Environm Sci Div, Johnson Space Ctr, Houston, TX USA.
RP Alwood, JS (reprint author), NASA, Ames Res Ctr, Space BioSci Div, Moffett Field, CA 94035 USA.
FU Human Health Countermeasures element of the HRP at NASA
FX Many of the ideas and concepts reflected in this perspective were
prepared by and presented at recent NASA Workshops by our colleagues:
William Paloski (Director, NASA JSC HRP), David Tomko (NASA HQ, Program
Executive, Space Biology Program), and Barbara Corbin (NASA JSC, Deputy
Manager, HRP). We wish to thank them for guiding the groundwork and
facilitating continuing work on this effort. Additionally, we thank
David Tomko for providing expert consultation and the initial draft of
Fig. 1. We thank Sidney Sun, Chris Maese, Ruth Globus, Ken Souza, and
Marianne Sowa at NASA ARC and John Charles, David Baumann, and Craig
Kundrot at NASA JSC for expert consultation. The Human Health
Countermeasures element of the HRP at NASA provided funding for this
paper.
NR 79
TC 0
Z9 0
U1 0
U2 0
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 2373-8065
J9 NPJ MICROGRAVITY
JI NPJ Microgravity
PD JAN 12
PY 2017
VL 3
AR 5
DI 10.1038/s41526-016-0002-8
PG 9
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EL3XZ
UT WOS:000394553900003
ER
PT J
AU Nadir, AJ
Sato, K
AF Nadir, Andrei James
Sato, Kevin
TI A hitchhiker's guide to an ISS experiment in under 9 months
SO NPJ MICROGRAVITY
LA English
DT Article
AB The International Space Station National Laboratory gives students a platform to conduct space-flight science experiments. To successfully take advantage of this opportunity, students and their mentors must have an understanding of how to develop and then conduct a science project on international space station within a school year. Many factors influence the speed in which a project progresses. The first step is to develop a science plan, including defining a hypothesis, developing science objectives, and defining a concept of operation for conducting the flight experiment. The next step is to translate the plan into well-defined requirements for payload development. The last step is a rapid development process. Included in this step is identifying problems early and negotiating appropriate trade-offs between science and implementation complexity. Organizing the team and keeping players motivated is an equally important task, as is employing the right mentors. The project team must understand the flight experiment infrastructure, which includes the international space station environment, payload resource requirements and available components, fail-safe operations, system logs, and payload data. Without this understanding, project development can be impacted, resulting in schedule delays, added costs, undiagnosed problems, and data misinterpretation. The information and processes for conducting low-cost, rapidly developed student-based international space station experiments are presented, including insight into the system operations, the development environment, effective team organization, and data analysis. The details are based on the Valley Christian Schools (VCS, San Jose, CA) fluidic density experiment and penicillin experiment, which were developed by 13- and 14-year-old students and flown on ISS.
C1 [Nadir, Andrei James; Sato, Kevin] NASA, Ames Res Ctr, NASA Biosci & Space Biol, FILMSS,Wyle Sci Technol & Engn, Mountain View, CA 94035 USA.
RP Nadir, AJ (reprint author), NASA, Ames Res Ctr, NASA Biosci & Space Biol, FILMSS,Wyle Sci Technol & Engn, Mountain View, CA 94035 USA.
EM andrei.nadir@warriorlife.net
NR 3
TC 0
Z9 0
U1 0
U2 0
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 2373-8065
J9 NPJ MICROGRAVITY
JI NPJ Microgravity
PD JAN 12
PY 2017
VL 3
AR 6
DI 10.1038/s41526-016-0003-7
PG 11
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EL3XZ
UT WOS:000394553900004
ER
PT J
AU Moores, JE
Smith, CL
Toigo, AD
Guzewich, SD
AF Moores, John E.
Smith, Christina L.
Toigo, Anthony D.
Guzewich, Scott D.
TI Penitentes as the origin of the bladed terrain of Tartarus Dorsa on
Pluto
SO NATURE
LA English
DT Article
ID CONVECTION; HORIZONS; METHANE
AB Penitentes are snow and ice features formed by erosion that, on Earth, are characterized by bowl-shaped depressions several tens of centimetres across, whose edges grade into spires up to several metres tall(1-3). Penitentes have been suggested as an explanation for anomalous radar data on Europa(4), but until now no penitentes have been identified conclusively on planetary bodies other than Earth. Regular ridges with spacings of 3,000 to 5,000 metres and depths of about 500 metres with morphologies that resemble penitentes have been observed by the New Horizons spacecraft(5-8) in the Tartarus Dorsa region of Pluto (220 degrees-250 degrees E, 0 degrees-20 degrees N). Here we report simulations, based upon a recent model(3) representing conditions on Pluto(7,9), in which deepening penitentes reproduce both the tri-modal (north-south, east-west and northeast-southwest) orientation and the spacing of the ridges of this bladed terrain. At present, these penitentes deepen by approximately one centimetre per orbital cycle and grow only during periods of relatively high atmospheric pressure, suggesting a formation timescale of several tens of millions of years, consistent with crater ages. This timescale implies that the penitentes formed from initial topographic variations of no more than a few tens of metres, consistent with Pluto's youngest terrains.
C1 [Moores, John E.; Smith, Christina L.] York Univ, Ctr Res Earth & Space Sci, Dept Earth & Space Sci & Engn, 4700 Keele St, N York, ON M3J 1P3, Canada.
[Toigo, Anthony D.] Johns Hopkins Univ, Appl Phys Lab, Baltimore, MD 21218 USA.
[Guzewich, Scott D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Moores, JE (reprint author), York Univ, Ctr Res Earth & Space Sci, Dept Earth & Space Sci & Engn, 4700 Keele St, N York, ON M3J 1P3, Canada.
EM jmoores@yorku.ca
FU Natural Sciences and Engineering Research Council of Canada (NSERC)
[436252-2013]; Integrating Atmospheric Chemistry and Physics from the
Earth to Space (IACPES) Collaborative Research and Training Experience
(CREATE) programme of NSERC
FX J.E.M. was supported in this work by a Discovery Grant (436252-2013)
from the Natural Sciences and Engineering Research Council of Canada
(NSERC) and C.L.S. was supported by a fellowship under the Integrating
Atmospheric Chemistry and Physics from the Earth to Space (IACPES)
Collaborative Research and Training Experience (CREATE) programme of
NSERC. We thank the New Horizons team for their efforts to plan, develop
and operate a mission to explore Pluto. The successful fly-by of 2015
provided publicly available data and peer-reviewed analysis of the
surface and atmosphere that enabled the research presented in this
paper.
NR 27
TC 0
Z9 0
U1 2
U2 2
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD JAN 12
PY 2017
VL 541
IS 7636
BP 188
EP +
DI 10.1038/nature20779
PG 9
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EN6PI
UT WOS:000396125500034
PM 28052055
ER
PT J
AU Moy, L
Bhartia, PK
Jaross, G
Loughman, R
Kramarova, N
Chen, Z
Taha, G
Chen, G
Xu, P
AF Moy, Leslie
Bhartia, Pawan K.
Jaross, Glen
Loughman, Robert
Kramarova, Natalya
Chen, Zhong
Taha, Ghassan
Chen, Grace
Xu, Philippe
TI Altitude registration of limb-scattered radiation
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID RETRIEVAL; INSTRUMENT; SATELLITE; PROFILES; MISSION
AB One of the largest constraints to the retrieval of accurate ozone profiles from UV backscatter limb sounding sensors is altitude registration. Two methods, the Rayleigh scattering attitude sensing (RSAS) and absolute radiance residual method (ARRM), are able to determine altitude registration to the accuracy necessary for long-term ozone monitoring. The methods compare model calculations of radiances to measured radiances and are independent of onboard tracking devices. RSAS determines absolute altitude errors, but, because the method is susceptible to aerosol interference, it is limited to latitudes and time periods with minimal aerosol contamination. ARRM, a new technique introduced in this paper, can be applied across all seasons and altitudes. However, it is only appropriate for relative altitude error estimates. The application of RSAS to Limb Profiler (LP) measurements from the Ozone Mapping and Profiler Suite (OMPS) on board the Suomi NPP (SNPP) satellite indicates tangent height (TH) errors greater than 1 km with an absolute accuracy of +/- 200 m. Results using ARRM indicate a similar to 300 to 400m intra-orbital TH change varying seasonally +/- 100 m, likely due to either errors in the spacecraft pointing or in the geopotential height (GPH) data that we use in our analysis. ARRM shows a change of similar to 200m over similar to 5 years with a relative accuracy (a long-term accuracy) of +/- 100m outside the polar regions.
C1 [Moy, Leslie; Kramarova, Natalya; Chen, Zhong; Chen, Grace] SSAI, 10210 Greenbelt Rd,Suite 600, Lanham, MD 20706 USA.
[Bhartia, Pawan K.; Jaross, Glen] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Loughman, Robert] Hampton Univ, Hampton, VA 23668 USA.
[Taha, Ghassan] GESTAR, Columbia, MD USA.
[Xu, Philippe] Sci Applicat Int Corp, Lanham, MD USA.
RP Moy, L (reprint author), SSAI, 10210 Greenbelt Rd,Suite 600, Lanham, MD 20706 USA.
EM leslie.moy@ssaihq.com
NR 14
TC 0
Z9 0
U1 1
U2 1
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1867-1381
EI 1867-8548
J9 ATMOS MEAS TECH
JI Atmos. Meas. Tech.
PD JAN 12
PY 2017
VL 10
IS 1
BP 167
EP 178
DI 10.5194/amt-10-167-2017
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EK1JR
UT WOS:000393682100001
ER
PT J
AU Garcia, EV
Currie, T
Guyon, O
Stassun, KG
Jovanovic, N
Lozi, J
Kudo, T
Doughty, D
Schlieder, J
Kwon, J
Uyama, T
Kuzuhara, M
Carson, JC
Nakagawa, T
Hashimoto, J
Kusakabe, N
Abe, L
Brandner, W
Brandt, TD
Feldt, M
Goto, M
Grady, CA
Hayano, Y
Hayashi, M
Hayashi, SS
Henning, T
Hodapp, KW
Ishii, M
Iye, M
Janson, M
Kandori, R
Knapp, GR
Matsuo, T
McElwain, MW
Miyama, S
Morino, JI
Moro-Martin, A
Nishimura, T
Pyo, TS
Serabyn, E
Suenaga, T
Suto, H
Suzuki, R
Takahashi, YH
Takami, H
Takami, M
Takato, N
Terada, H
Thalmann, C
Turner, EL
Watanabe, M
Wisniewski, J
Yamada, T
Usuda, T
Tamura, M
AF Garcia, E. Victor
Currie, Thayne
Guyon, Olivier
Stassun, Keivan G.
Jovanovic, Nemanja
Lozi, Julien
Kudo, Tomoyuki
Doughty, Danielle
Schlieder, Josh
Kwon, J.
Uyama, T.
Kuzuhara, M.
Carson, J. C.
Nakagawa, T.
Hashimoto, J.
Kusakabe, N.
Abe, L.
Brandner, W.
Brandt, T. D.
Feldt, M.
Goto, M.
Grady, C. A.
Hayano, Y.
Hayashi, M.
Hayashi, S. S.
Henning, T.
Hodapp, K. W.
Ishii, M.
Iye, M.
Janson, M.
Kandori, R.
Knapp, G. R.
Matsuo, T.
McElwain, M. W.
Miyama, S.
Morino, J. -I.
Moro-Martin, A.
Nishimura, T.
Pyo, T. -S.
Serabyn, E.
Suenaga, T.
Suto, H.
Suzuki, R.
Takahashi, Y. H.
Takami, H.
Takami, M.
Takato, N.
Terada, H.
Thalmann, C.
Turner, E. L.
Watanabe, M.
Wisniewski, J.
Yamada, T.
Usuda, T.
Tamura, M.
TI SCExAO AND GPI Y JH BAND PHOTOMETRY AND INTEGRAL FIELD SPECTROSCOPY OF
THE YOUNG BROWN DWARF COMPANION TO HD 1160
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE instrumentation: adaptive optics; planetary systems; stars: low-mass;
techniques: imaging spectroscopy
ID LOW-MASS STARS; PRE-MAIN-SEQUENCE; FINDING CAMPAIGN DISCOVERY; STELLAR
ASTROPHYSICS MESA; HYDROGEN-BURNING LIMIT; DIRECTLY IMAGED PLANET;
BETA-PICTORIS B; UPPER SCORPIUS; DYNAMICAL MASSES; HR 8799
AB We present high signal-to-noise ratio, precise Y JH photometry and Y band (0.957-1.120 mu m) spectroscopy of HD 1160 B, a young substellar companion discovered from the Gemini NICI Planet Finding Campaign using the Subaru Coronagraphic Extreme Adaptive Optics instrument and the Gemini Planet Imager. HD 1160 B has typical mid-M dwarf-like infrared colors and a spectral type of M5.5(-0.5)(+1.0), where the blue edge of our Y band spectrum rules out earlier spectral types. Atmospheric modeling suggests HD 1160 B has an effective temperature of 3000-3100 K, a surface gravity of log g - 4-4.5, a radius of. 1.55 +/- 0.10 R-J, and a luminosity of log L/L circle dot - 2.76 +/- 0.05. Neither the primary's Hertzspring-Russell diagram position nor atmospheric modeling of HD 1160 B show evidence for a subsolar metallicity. Interpretation of the HD 1160 B spectroscopy depends on which stellar system components are used to estimate the age. Considering HD 1160 A, B and C jointly, we derive an age of 80-125 Myr, implying that HD 1160 B straddles the hydrogen-burning limit (70-90 M-J) If we consider HD 1160 A alone, younger ages (20-125 Myr) and a brown dwarf-like mass (35-90 M-J) are possible. Interferometric measurements of the primary, a precise Gaia parallax, and moderate-resolution spectroscopy can better constrain the system's age and how HD 1160 B fits within the context of (sub) stellar evolution.
C1 [Garcia, E. Victor] Lowell Observ, Flagstaff, AZ 86001 USA.
[Garcia, E. Victor; Stassun, Keivan G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
[Garcia, E. Victor] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Currie, Thayne; Guyon, Olivier; Jovanovic, Nemanja; Lozi, Julien; Kudo, Tomoyuki; Hayano, Y.; Hayashi, S. S.; Nishimura, T.; Pyo, T. -S.; Takato, N.] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Guyon, Olivier; Kuzuhara, M.; Hashimoto, J.; Kusakabe, N.; Suto, H.; Tamura, M.] Astrobiol Ctr NINS, Mitaka, Tokyo 1818588, Japan.
[Guyon, Olivier] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Stassun, Keivan G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA.
[Doughty, Danielle] Univ Arizona, Coll Opt Sci, Tucson, AZ 85721 USA.
[Schlieder, Josh] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kwon, J.; Nakagawa, T.; Yamada, T.] Japan Aerosp Explorat Agcy JAXA, ISAS, Dept Space Astron & Astrophys, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Uyama, T.; Suenaga, T.; Tamura, M.] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
[Kuzuhara, M.; Hashimoto, J.; Kusakabe, N.; Hayashi, M.; Ishii, M.; Iye, M.; Kandori, R.; Morino, J. -I.; Moro-Martin, A.; Suto, H.; Suzuki, R.; Takahashi, Y. H.; Terada, H.; Usuda, T.; Tamura, M.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Kuzuhara, M.] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan.
[Carson, J. C.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
[Abe, L.; Henning, T.] Univ Nice Sophia Antipolis, Lab Lagrange UMR 7293, CNRS, Observ Cote Azur, F-06108 Nice 2, France.
[Brandner, W.; Feldt, M.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Brandt, T. D.] Inst Adv Study, Dept Astrophys, Princeton, NJ 08540 USA.
[Goto, M.; McElwain, M. W.] Ludwig Maximilians Univ Scheinerstr, Univ Sternwarte Munchen, D-81679 Munich, Germany.
[Grady, C. A.] Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Grady, C. A.] Eureka Sci, Oakland, CA 96002 USA.
[Grady, C. A.] Goddard Ctr Astrobiol, Greenbelt, MD USA.
[Hayashi, S. S.; Suenaga, T.] SOKENDAI Grad Univ Adv Studies, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan.
[Hodapp, K. W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
[Janson, M.] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, SE-10691 Stockholm, Sweden.
[Knapp, G. R.; Turner, E. L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Matsuo, T.] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan.
[Miyama, S.] Hiroshima Univ, Higashihiroshima, Hiroshima 7398511, Japan.
[Moro-Martin, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Moro-Martin, A.] Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA.
[Serabyn, E.; Takahashi, Y. H.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Takami, H.; Takami, M.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Thalmann, C.] Swiss Fed Inst Technol, ETH Zurich, Inst Astron, CH-8093 Zurich, Switzerland.
[Turner, E. L.] Univ Tokyo, Kavli Inst Phys & Math Univ, Kashiwa, Chiba 2778568, Japan.
[Watanabe, M.] Hokkaido Univ, Dept Cosmosci, Kita Ku, Sapporo, Hokkaido 0600810, Japan.
[Wisniewski, J.] Univ Oklahoma, HL Dodge Dept Phys & Astron, St Norman, OK 73019 USA.
RP Garcia, EV (reprint author), Lowell Observ, Flagstaff, AZ 86001 USA.
EM eugenio.v.garcia@gmail.com
OI Stassun, Keivan/0000-0002-3481-9052
FU BF foundation; Fisk-Vanderbilt Bridge Program; JSPS [23103002, 23340051,
26220704, 25-8826]; U.S. Department of Energy by Lawrence Livermore
National Laboratory [DE-AC52-07NA27344, LLNL-JRNL-701012-DRAFT]; U.S.
National Science Foundation [1009203]
FX We thank Anna-Lise Marie for detailed, helpful discussions about and
access to SPHERE HD 1160 B spectra. We thank Eric Mamajek for
discussions about the metallicity of nearby, young stars. We thank Davy
Kirkpatrick for providing NIR spectra of M-dwarf spectral standards. We
thank Federico Spada for discussions and tests of the Yonsei-Yale
models. EVG would like to acknowledge the gracious support of his Lowell
Predoctoral Fellowship by the BF foundation and the excellent support of
Fisk-Vanderbilt Bridge Program. This research has made use of the SIMBAD
database, operated at CDS, Strasbourg, France. This research has made
use of the Keck Observatory Archive (KOA), which is operated by the W.
M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI),
under contract with the National Aeronautics and Space Administration.
The authors acknowledge support from the JSPS (Grant-in-Aid for Research
#23103002, #23340051, and #26220704). This work was partially supported
by the Grant-in-Aid for JSPS fellows (Grant Number 25-8826). M.J.
acknowledges support of the U.S. National Science Foundation, under
Award No. 1009203. This work performed under the auspices of the U.S.
Department of Energy by Lawrence Livermore National Laboratory under
Contract DE-AC52-07NA27344 with document release number
LLNL-JRNL-701012-DRAFT. We wish to acknowledge the pivotal cultural role
and reverence that the summit of Maunakea has always had within the
indigenous Hawaiian community. We are most fortunate to have the
privilege to conduct scientific observations from this mountain.
NR 90
TC 0
Z9 0
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2017
VL 834
IS 2
AR 162
DI 10.3847/1538-4357/834/2/162
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EK2LQ
UT WOS:000393759200024
ER
PT J
AU Choquet, E
Milli, J
Wahhaj, Z
Soummer, R
Roberge, A
Augereau, JC
Booth, M
Absil, O
Boccaletti, A
Chen, CH
Debes, JH
del Burgo, C
Dent, WRF
Ertel, S
Girard, JH
Gofas-Salas, E
Golimowski, DA
Gonzalez, CAG
Hagan, JB
Hibon, P
Hines, DC
Kennedy, GM
Lagrange, AM
Matra, L
Mawet, D
Mouillet, D
N'Diaye, M
Perrin, MD
Pinte, C
Pueyo, L
Rajan, A
Schneider, G
Wolff, S
Wyatt, M
AF Choquet, Elodie
Milli, Julien
Wahhaj, Zahed
Soummer, Remi
Roberge, Aki
Augereau, Jean-Charles
Booth, Mark
Absil, Olivier
Boccaletti, Anthony
Chen, Christine H.
Debes, John H.
del Burgo, Carlos
Dent, William R. F.
Ertel, Steve
Girard, Julien H.
Gofas-Salas, Elena
Golimowski, David A.
Gonzalez, Carlos A. Gomez
Hagan, J. Brendan
Hibon, Pascale
Hines, Dean C.
Kennedy, Grant M.
Lagrange, Anne-Marie
Matra, Luca
Mawet, Dimitri
Mouillet, David
N'Diaye, Mamadou
Perrin, Marshall D.
Pinte, Christophe
Pueyo, Laurent
Rajan, Abhijith
Schneider, Glenn
Wolff, Schuyler
Wyatt, Mark
TI First Scattered-light Images of the Gas-rich Debris Disk around 49 Ceti
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE circumstellar matter; stars: individual (49 Ceti); techniques: image
processing
ID A-TYPE STARS; CENTAURUS OB ASSOCIATION; CIRCUMSTELLAR DISK; MOLECULAR
GAS; BETA-PICTORIS; EXOCOMETARY GAS; HD 181327; EXOPLANETS; DUST;
EVOLUTION
AB We present the first scattered-light images of the debris disk around 49 Ceti, a similar to 40 Myr A1 main-sequence star at 59 pc, famous for hosting two massive dust belts as well as large quantities of atomic and molecular gas. The outer disk is revealed in reprocessed archival Hubble Space Telescope NICMOS-F110W images, as well as new coronagraphic H-band images from the Very Large Telescope SPHERE instrument. The disk extends from 1 1 (65 au) to 4.'' 6 (250 au) and is seen at an inclination of 73 degrees, which refines previous measurements at lower angular resolution. We also report no companion detection larger than 3 M-Jup at projected separations beyond 20 au from the star (0.'' 34). Comparison between the F110W and H-band images is consistent with a gray color of 49 Ceti's dust, indicating grains larger than greater than or similar to 2 mu m. Our photometric measurements indicate a scattering efficiency/infrared excess ratio of 0.2-0.4, relatively low compared to other characterized debris disks. We find that 49 Ceti presents morphological and scattering properties very similar to the gas-rich HD 131835 system. From our constraint on the disk inclination we find that the atomic gas previously detected in absorption must extend to the inner disk, and that the latter must be depleted of CO gas. Building on previous studies, we propose a schematic view of the system describing the dust and gas structure around 49 Ceti and hypothetical scenarios for the gas nature and origin.
C1 [Choquet, Elodie; Mawet, Dimitri] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Milli, Julien; Wahhaj, Zahed; Girard, Julien H.; Hibon, Pascale] European Southern Observ, Alonso de Cordova 3107, Santiago 19001, Chile.
[Soummer, Remi; Chen, Christine H.; Debes, John H.; Golimowski, David A.; Hagan, J. Brendan; Hines, Dean C.; N'Diaye, Mamadou; Perrin, Marshall D.; Pueyo, Laurent] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Roberge, Aki] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 20771 USA.
[Augereau, Jean-Charles; Lagrange, Anne-Marie; Mouillet, David; Pinte, Christophe] Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France.
[Booth, Mark] Friedrich Schiller Univ Jena, Astrophys Inst, Schillergasschen 2-3, D-07745 Jena, Germany.
[Booth, Mark] Friedrich Schiller Univ Jena, Univ Sternwarte, Schillergasschen 2-3, D-07745 Jena, Germany.
[Booth, Mark] Pontificia Univ Catolica Chile, Inst Astrofis, Vicuna Mackenna 4860, Santiago, Chile.
[Absil, Olivier; Gonzalez, Carlos A. Gomez] Univ Liege, Space Sci Technol & Astrophys Res STAR Inst, 19 Allee Six Aout, B-4000 Cointe Ougree, Belgium.
[Boccaletti, Anthony] UPMC Univ Paris 06, Univ Paris Diderot, Sorbonne Paris Cite, Sorbonne Univ,CNRS,PSL Res Univ,LESIA,Observ Pari, 5 Pl Jules Janssen, F-92195 Meudon, France.
[del Burgo, Carlos] Inst Nacl Astrofis Opt & Electr, Luis Enrique Erro 1, Puebla, Mexico.
[Dent, William R. F.] Atacama Large Millimeter Submillimeter Array ALMA, Santiago Cent Off, Alonso de Cordova 3107, Santiago 7630355, Chile.
[Ertel, Steve; Schneider, Glenn] Univ Arizona, Dept Astron, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA.
[Gofas-Salas, Elena] Off Natl Etud & Rech Aerosp, 29 Ave Div Leclerc, F-92320 Paris, France.
[Kennedy, Grant M.; Matra, Luca; Wyatt, Mark] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Mawet, Dimitri] CALTECH, Dept Astron, 1200 E Calif Blvd,MC 249-17, Pasadena, CA 91125 USA.
[N'Diaye, Mamadou] Univ Cote Azur, Lab Lagrange, Observ Cote Azur, CNRS, Parc Valrose,Bat H Fizeau, F-06108 Nice, France.
[Rajan, Abhijith] Arizona State Univ, Phoenix, AZ 85004 USA.
[Wolff, Schuyler] Johns Hopkins Univ, 3400 North Charles St, Baltimore, MD 21218 USA.
RP Choquet, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM echoquet@jpl.nasa.gov
OI Absil, Olivier/0000-0002-4006-6237
FU NASA through Hubble Fellowship - STScI [HST-HF2-51355]; AURA, Inc.
[NAS5-26555]; ESO through the ESO fellowship program; DFG [Kr
2164/15-1]; Mexican CONACyT [CB-2012-183007]; STFC; Programme National
de Plane-tologie; European Union through ERC [337569, 279973];
[HST-AR-12652]
FX E.C. acknowledges support from NASA through Hubble Fellowship grant
HST-HF2-51355 awarded by STScI, operated by AURA, Inc. under contract
NAS5-26555, and support from HST-AR-12652, for research carried out at
the Jet Propulsion Laboratory, California Institute of Technology. J.M.
acknowledges ESO through the ESO fellowship program. M.B. acknowledges
support from DFG project Kr 2164/15-1. G.M.K. is supported by the Royal
Society as a Royal Society University Research Fellow. C.d.B. is
supported by Mexican CONACyT research grant CB-2012-183007. L.M.
acknowledges support by STFC through a graduate studentship. J.C.A.
acknowledges support by the Programme National de Plane-tologie. We
acknowledge support by the European Union through ERC grant 337569 for
O.A. and C.A.G.G. and grant 279973 for M.W. and L.M.
NR 47
TC 0
Z9 0
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JAN 10
PY 2017
VL 834
IS 2
AR L12
DI 10.3847/2041-8213/834/2/L12
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EK4IL
UT WOS:000393890200004
ER
PT J
AU Schumann, U
Baumann, R
Baumgardner, D
Bedka, ST
Duda, DP
Freudenthaler, V
Gayet, JF
Heymsfield, AJ
Minnis, P
Quante, M
Raschke, E
Schlager, H
Vazquez-Navarro, M
Voigt, C
Wang, ZE
AF Schumann, Ulrich
Baumann, Robert
Baumgardner, Darrel
Bedka, Sarah T.
Duda, David P.
Freudenthaler, Volker
Gayet, Jean-Francois
Heymsfield, Andrew J.
Minnis, Patrick
Quante, Markus
Raschke, Ehrhard
Schlager, Hans
Vazquez-Navarro, Margarita
Voigt, Christiane
Wang, Zhien
TI Properties of individual contrails: a compilation of observations and
some comparisons
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID IN-SITU MEASUREMENTS; AIRCRAFT EXHAUST PLUMES; TO-CIRRUS TRANSITION;
DIFFERENT SULFUR CONTENTS; WATER-VAPOR MEASUREMENTS; RADIATIVE
PROPERTIES; OPTICAL-PROPERTIES; YOUNG CONTRAILS; ICE PARTICLES;
NUMERICAL SIMULATIONS
AB Mean properties of individual contrails are characterized for a wide range of jet aircraft as a function of age during their life cycle from seconds to 11.5 h (7.4-18.7 km altitude, -88 to -31 degrees C ambient temperature), based on a compilation of about 230 previous in situ and remote sensing measurements. The airborne, satellite, and ground-based observations encompass exhaust contrails from jet aircraft from 1972 onwards, as well as a few older data for propeller aircraft. The contrails are characterized by mean ice particle sizes and concentrations, extinction, ice water content, optical depth, geometrical depth, and contrail width. Integral contrail properties include the cross-section area and total number of ice particles, total ice water content, and total extinction (area integral of extinction) per contrail length. When known, the contrail-causing aircraft and ambient conditions are characterized. The individual datasets are briefly described, including a few new analyses performed for this study, and compiled together to form a "contrail library" (COLI). The data are compared with results of the Contrail Cirrus Prediction (CoCiP) model. The observations confirm that the number of ice particles in contrails is controlled by the engine exhaust and the formation process in the jet phase, with some particle losses in the wake vortex phase, followed later by weak decreases with time. Contrail cross sections grow more quickly than expected from exhaust dilution. The cross-section-integrated extinction follows an algebraic approximation. The ratio of volume to effective mean radius decreases with time. The ice water content increases with increasing temperature, similar to non-contrail cirrus, while the equivalent relative humidity over ice saturation of the contrail ice mass increases at lower temperatures in the data. Several contrails were observed in warm air above the Schmidt-Appleman threshold temperature. The "emission index" of ice particles, i.e., the number of ice particles formed in the young contrail per burnt fuel mass, is estimated from the measured concentrations for estimated dilution; maximum values exceed 10(15) kg(-1). The dependence of the data on the observation methods is discussed. We find no obvious indication for significant contributions from spurious particles resulting from shattering of ice crystals on the microphysical probes.
C1 [Schumann, Ulrich; Baumann, Robert; Schlager, Hans; Vazquez-Navarro, Margarita; Voigt, Christiane] Deutsch Zentrum Luft & Raumfahrt, Inst Phys Atmosphare, D-82234 Oberpfaffenhofen, Germany.
[Baumgardner, Darrel] Droplet Measurement Technol Inc, Boulder, CO USA.
[Bedka, Sarah T.; Duda, David P.] Sci Syst & Applicat Inc, Hampton, VA USA.
[Freudenthaler, Volker] Ludwig Maximilians Univ Munchen, Meteorolog Inst, Munich, Germany.
[Gayet, Jean-Francois] CNRS, Lab Meteorol Phys, Clermont Ferrand, France.
[Heymsfield, Andrew J.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
[Minnis, Patrick] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Quante, Markus] Helmholtz Zentrum Geesthacht, Inst Coastal Res, Geesthacht, Germany.
[Raschke, Ehrhard] Max Planck Inst Meteorol, Hamburg, Germany.
[Raschke, Ehrhard] Univ Hamburg, Hamburg, Germany.
[Voigt, Christiane] Johannes Gutenberg Univ Mainz, Inst Phys Atmosphare, Mainz, Germany.
[Wang, Zhien] Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82071 USA.
RP Schumann, U (reprint author), Deutsch Zentrum Luft & Raumfahrt, Inst Phys Atmosphare, D-82234 Oberpfaffenhofen, Germany.
EM ulrich.schumann@dlr.de
FU FAA ACCRI Program
FX We are grateful for input and comments from William A. Cooper, Ru-Shan
Gao, Timothy Garrett, Kaspar Graf, Christian Kiemle, Andreas Minikin,
Andrew Roberts, and Simon Unterstrasser. S. Bedka, D. Duda, and P.
Minnis were supported by the FAA ACCRI Program. We gratefully
acknowledge the wide set of data sources as explained in the text. The
first author dedicates this work to his former colleague, Manfred E.
Reinhardt (26 January 1927 to 1 October 2015), a reliable partner, for
fruitful cooperation between 1982 and 1991, and for early contrail
research with research aircraft.
NR 194
TC 2
Z9 2
U1 1
U2 1
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PD JAN 10
PY 2017
VL 17
IS 1
BP 403
EP 438
DI 10.5194/acp-17-403-2017
PG 36
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EK2KL
UT WOS:000393756100002
ER
PT J
AU Habbal, F
Larour, E
Morlighem, M
Seroussi, H
Borstad, CP
Rignot, E
AF Habbal, Feras
Larour, Eric
Morlighem, Mathieu
Seroussi, Helene
Borstad, Christopher P.
Rignot, Eric
TI Optimal numerical solvers for transient simulations of ice flow using
the Ice Sheet System Model (ISSM versions 4.2.5 and 4.11)
SO GEOSCIENTIFIC MODEL DEVELOPMENT
LA English
DT Article
ID GREENLAND; ANTARCTICA; DYNAMICS; MESHES; ORDER
AB Identifying fast and robust numerical solvers is a critical issue that needs to be addressed in order to improve projections of polar ice sheets evolving in a changing climate. This work evaluates the impact of using advanced numerical solvers for transient ice-flow simulations conducted with the JPL-UCI Ice Sheet System Model (ISSM). We identify optimal numerical solvers by testing a broad suite of readily available solvers, ranging from direct sparse solvers to preconditioned iterative methods, on the commonly used Ice Sheet Model Intercomparison Project for Higher-Order ice sheet Models benchmark tests. Three types of analyses are considered: mass transport, horizontal stress balance, and incompressibility. The results of the fastest solvers for each analysis type are ranked based on their scalability across mesh size and basal boundary conditions. We find that the fastest iterative solvers are similar to 1.5-100 times faster than the default direct solver used in ISSM, with speed-ups improving rapidly with increased mesh resolution. We provide a set of recommendations for users in search of efficient solvers to use for transient ice-flow simulations, enabling higher-resolution meshes and faster turnaround time. The end result will be improved transient simulations for short-term, highly resolved forward projections (10-100 year time scale) and also improved long-term paleo-reconstructions using higher-order representations of stresses in the ice. This analysis will also enable a new generation of comprehensive uncertainty quantification assessments of forward sea-level rise projections, which rely heavily on ensemble or sampling approaches that are inherently expensive.
C1 [Habbal, Feras] Univ Texas Austin, Inst Geophys, JJ Pickle Res Campus,Bldg 196,10100 Burnet Rd, Austin, TX 78758 USA.
[Larour, Eric; Seroussi, Helene; Rignot, Eric] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr MS 300-323, Pasadena, CA 91109 USA.
[Morlighem, Mathieu; Rignot, Eric] Univ Calif Irvine, Dept Earth Syst Sci, Croul Hall, Irvine, CA 92697 USA.
[Borstad, Christopher P.] Univ Ctr Svalbard, Dept Arctic Geophys, Longyearbyen, Norway.
RP Habbal, F (reprint author), Univ Texas Austin, Inst Geophys, JJ Pickle Res Campus,Bldg 196,10100 Burnet Rd, Austin, TX 78758 USA.
EM ferashabbal@utexas.edu
FU National Science Foundation (NSF) [ANT-1155885]; Cryospheric Sciences
Program; Modeling Analysis and Prediction Program
FX This work was performed at the Jet Propulsion Laboratory, California
Institute of Technology, and at the Department of Earth System Science,
University of California Irvine, under two contracts: one a grant from
the National Science Foundation (NSF) (award ANT-1155885) and the other
a contract with the National Aeronautics and Space Administration
(NASA), funded by the Cryospheric Sciences Program and the Modeling
Analysis and Prediction Program. Resources supporting the numerical
simulations were provided by the NASA High-End Computing (HEC) Program
through the NASA Advanced Supercomputing (NAS) Division at Ames Research
Center. We would like to acknowledge the insights and help from Jed
Brown, as well as helpful feedback from the anonymous reviewers. This is
UTIG contribution 3033.
NR 30
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U1 2
U2 2
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1991-959X
EI 1991-9603
J9 GEOSCI MODEL DEV
JI Geosci. Model Dev.
PD JAN 10
PY 2017
VL 10
IS 1
BP 155
EP 168
DI 10.5194/gmd-10-155-2017
PG 14
WC Geosciences, Multidisciplinary
SC Geology
GA EK1KU
UT WOS:000393685000001
ER
PT J
AU Prasad, SK
Jess, DB
Klimchuk, JA
Banerjee, D
AF Prasad, S. Krishna
Jess, D. B.
Klimchuk, J. A.
Banerjee, D.
TI UNRAVELLING THE COMPONENTS OF A MULTI-THERMAL CORONAL LOOP USING
MAGNETOHYDRODYNAMIC SEISMOLOGY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetohydrodynamics (MHD); Sun: corona; Sun: fundamental parameters;
Sun: oscillations; sunspots
ID SOLAR CORONA; TRACE OBSERVATIONS; MAGNETIC-FIELD; ACTIVE REGIONS; WAVES;
OSCILLATIONS; DISTURBANCES; AIA/SDO; SDO
AB Coronal loops, constituting the basic building blocks of the active Sun, serve as primary targets to help understand the mechanisms responsible for maintaining multi-million Kelvin temperatures in the solar and stellar coronae. Despite significant advances in observations and theory, our knowledge on the fundamental properties of these structures is limited. Here, we present unprecedented observations of accelerating slow magnetoacoustic waves along a coronal loop that show differential propagation speeds in two distinct temperature channels, revealing the multi-stranded and multithermal nature of the loop. Utilizing the observed speeds and employing nonlinear force-free magnetic field extrapolations, we derive the actual temperature variation along the loop in both channels, and thus are able to resolve two individual components of the multithermal loop for the first time. The obtained positive temperature gradients indicate uniform heating along the loop, rather than isolated footpoint heating.
C1 [Prasad, S. Krishna; Jess, D. B.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Jess, D. B.] Calif State Univ Northridge, Dept Phys & Astron, Northridge, CA 91330 USA.
[Klimchuk, J. A.] NASA, Heliophys Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Banerjee, D.] Indian Inst Astrophys, 2 Block Koramangala, Bengaluru 560034, India.
RP Prasad, SK (reprint author), Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
EM krishna.prasad@qub.ac.uk
OI Banerjee, Dipankar/0000-0003-4653-6823
FU UK Science and Technology Facilities Council (STFC); NASA Supporting
Research and Technology Program
FX The authors thank the anonymous referees for useful comments. S.K.P.
wishes to thank S. Tomczyk for sharing his speed estimation software.
D.B.J. wishes to thank the UK Science and Technology Facilities Council
(STFC) for the award of an Ernest Rutherford Fellowship in addition to a
dedicated research grant. J.A.K. would like to thank the NASA Supporting
Research and Technology Program for support.
NR 43
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U1 3
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2017
VL 834
IS 2
AR 103
DI 10.3847/1538-4357/834/2/103
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EI3KJ
UT WOS:000392389100006
ER
PT J
AU Xie, YS
Fan, X
Chen, YP
Wilson, JD
Simons, RN
Xiao, JQ
AF Xie, Yunsong
Fan, Xin
Chen, Yunpeng
Wilson, Jeffrey D.
Simons, Rainee N.
Xiao, John Q.
TI A subwavelength resolution microwave/6.3 GHz camera based on a
metamaterial absorber
SO SCIENTIFIC REPORTS
LA English
DT Article
ID SENSOR
AB The design, fabrication and characterization of a novel metamaterial absorber based camera with subwavelength spatial resolution are investigated. The proposed camera is featured with simple and lightweight design, easy portability, low cost, high resolution and sensitivity, and minimal image interference or distortion to the original field distribution. The imaging capability of the proposed camera was characterized in both near field and far field ranges. The experimental and simulated near field images both reveal that the camera produces qualitatively accurate images with negligible distortion to the original field distribution. The far field demonstration was done by coupling the designed camera with a microwave convex lens. The far field results further demonstrate that the camera can capture quantitatively accurate electromagnetic wave distribution in the diffraction limit. The proposed camera can be used in application such as non-destructive image and beam direction tracer.
C1 [Xie, Yunsong; Chen, Yunpeng; Xiao, John Q.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Fan, Xin] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Wilson, Jeffrey D.; Simons, Rainee N.] Natl Aeronaut & Space Adm, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Xiao, JQ (reprint author), Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
EM jqx@udel.edu
FU NASA EPSCoR program [NNX11AQ29A]
FX The work is supported from the NASA EPSCoR program under grant No.
NNX11AQ29A.
NR 41
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U1 14
U2 14
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2045-2322
J9 SCI REP-UK
JI Sci Rep
PD JAN 10
PY 2017
VL 7
AR 40490
DI 10.1038/srep40490
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EH5TU
UT WOS:000391836600001
PM 28071734
ER
PT J
AU McKibben, SM
Peterson, W
Wood, M
Trainer, VL
Hunter, M
White, AE
AF McKibben, S. Morgaine
Peterson, William
Wood, Michelle
Trainer, Vera L.
Hunter, Matthew
White, Angelicque E.
TI Climatic regulation of the neurotoxin domoic acid
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE domoic acid; Pacific Decadal Oscillation; El Nino; Northern California
Current; Pseudo-nitzschia
ID NORTHERN CALIFORNIA CURRENT; HARMFUL ALGAL BLOOMS; PSEUDO-NITZSCHIA;
ENSO TELECONNECTIONS; UPWELLING SYSTEMS; RAZOR CLAMS; EL-NINO; IMPACTS;
ECOSYSTEM; PACIFIC
AB Domoic acid is a potent neurotoxin produced by certain marine microalgae that can accumulate in the foodweb, posing a health threat to human seafood consumers and wildlife in coastal regions worldwide. Evidence of climatic regulation of domoic acid in shellfish over the past 20 y in the Northern California Current regime is shown. The timing of elevated domoic acid is strongly related to warm phases of the Pacific Decadal Oscillation and the Oceanic Nino Index, an indicator of El Nino events. Ocean conditions in the northeast Pacific that are associated with warm phases of these indices, including changes in prevailing currents and advection of anomalously warm water masses onto the continental shelf, are hypothesized to contribute to increases in this toxin. We present an applied domoic acid risk assessment model for the US West Coast based on combined climatic and local variables. Evidence of regional-to basin-scale controls on domoic acid has not previously been presented. Our findings have implications in coastal zones worldwide that are affected by this toxin and are particularly relevant given the increased frequency of anomalously warm ocean conditions.
C1 [McKibben, S. Morgaine; White, Angelicque E.] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA.
[Peterson, William] Hatfield Marine Sci Ctr, NOAA, Natl Marine Fisheries Serv, Northwest Fisheries Sci Ctr, Newport, OR 97365 USA.
[Wood, Michelle] Univ Oregon, Inst Ecol & Evolut, Eugene, OR 97403 USA.
[Trainer, Vera L.] NOAA, Natl Marine Fisheries Serv, Northwest Fisheries Sci Ctr, Seattle, WA 98112 USA.
[Hunter, Matthew] Oregon Dept Fish & Wildlife, Astoria, OR 97103 USA.
RP McKibben, SM (reprint author), Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA.
EM mmckibben@coas.oregonstate.edu
FU NOAA from the Monitoring and Event Response for Harmful Algal Blooms
(MERHAB) program [NA07NOS4780195]; National Science Foundation
[1459480-OCE]
FX We thank Dr. Stephen Pierce for the upwelling data and Dan Ayres for
providing the WA shellfish data. This study was supported by NOAA Grant
NA07NOS4780195 (to A.E.W., W.P., A.M.W., and M.H.) from the Monitoring
and Event Response for Harmful Algal Blooms (MERHAB) program. Additional
support was provided by the National Science Foundation Grant
1459480-OCE (to A.E.W.). This is MERHAB Publication 190. The statements,
findings, conclusions, and recommendations are those of the authors and
do not necessarily reflect the views of NOAA or the Department of
Commerce.
NR 44
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U1 32
U2 32
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD JAN 10
PY 2017
VL 114
IS 2
BP 239
EP 244
DI 10.1073/pnas.1606798114
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EH0FR
UT WOS:000391439300032
PM 28069959
ER
PT J
AU Cherry, JE
Knapp, C
Trainor, S
Ray, AJ
Tedesche, M
Walker, S
AF Cherry, Jessica E.
Knapp, Corrie
Trainor, Sarah
Ray, Andrea J.
Tedesche, Molly
Walker, Susan
TI Planning for climate change impacts on hydropower in the Far North
SO HYDROLOGY AND EARTH SYSTEM SCIENCES
LA English
DT Article
ID EARTH SYSTEM MODELS; ARCTIC SNOW COVER; WATER-RESOURCES; POTENTIAL
IMPACTS; RIVER-BASIN; BOUNDARY ORGANIZATIONS; SOLID PRECIPITATION;
LAND-SURFACE; ECMWF MODEL; TIEN-SHAN
AB Unlike much of the contiguous United States, new hydropower development continues in the Far North, where climate models project precipitation will likely increase over the next century. Regional complexities in the Arctic and sub-Arctic, such as glacier recession and permafrost thaw, however, introduce uncertainties about the hydrologic responses to climate change that impact water resource management. This work reviews hydroclimate changes in the Far North and their impacts on hydropower; it provides a template for application of current techniques for prediction and estimating uncertainty, and it describes best practices for integrating science into management and decision-making. The growing number of studies on hydrologic impacts suggests that information resulting from climate change science has matured enough that it can and should be integrated into hydropower scoping, design, and management. Continuing to ignore the best available information in lieu of status quo planning is likely to prove costly to society in the long term.
C1 [Cherry, Jessica E.; Tedesche, Molly] Univ Alaska Fairbanks, Int Arctic Res Ctr, Fairbanks, AK 99775 USA.
[Cherry, Jessica E.] Univ Alaska Fairbanks, Inst Northern Engn, Fairbanks, AK 99775 USA.
[Knapp, Corrie] Western State Colorado Univ, Dept Environm & Sustainabil, Gunnison, CO 81231 USA.
[Trainor, Sarah] Univ Alaska Fairbanks, Alaska Ctr Climate Assessment & Policy, Fairbanks, AK 99775 USA.
[Ray, Andrea J.] NOAA, Earth Syst Res Lab, Div Phys Sci, Boulder, CO 80305 USA.
[Walker, Susan] NOAA, Natl Marine Fisheries Serv, Juneau, AK 99801 USA.
RP Cherry, JE (reprint author), Univ Alaska Fairbanks, Int Arctic Res Ctr, Fairbanks, AK 99775 USA.; Cherry, JE (reprint author), Univ Alaska Fairbanks, Inst Northern Engn, Fairbanks, AK 99775 USA.
EM jessica.cherry@alaska.edu
FU National Oceanic and Atmospheric Administration-National Marine
Fisheries Service (NOAA-NMFS) [HA-133F-12-SE-2460]; NOAA-NMFS; NOAA
Climate Program Office through the Alaska Center for Climate Assessment
and Policy at UAF [NA11OAR4310141]; Alaska EPSCoR NSF [OIA-1208927];
state of Alaska
FX Cherry wishes to thank the National Oceanic and Atmospheric
Administration-National Marine Fisheries Service (NOAA-NMFS) for
financial support of this effort (award no. HA-133F-12-SE-2460) and Lily
Cohen at the University of Alaska Fairbanks (UAF) for helping organize
the references. Molly Tedesche, Corrie Knapp, and Sarah Trainor
acknowledge financial support from NOAA-NMFS under that same award
number. Sarah Trainor also acknowledges support from NOAA Climate
Program Office grant NA11OAR4310141 through the Alaska Center for
Climate Assessment and Policy at UAF, Alaska EPSCoR NSF award no.
OIA-1208927, and the state of Alaska. Ray's participation in this effort
was supported in-kind by the NOAA/ESRL Physical Sciences Division and
Walker was supported in-kind by NOAA-NMFS. The authors wish to thank
ACCAP and IARC for covering the cost of page charges.
NR 174
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U1 2
U2 2
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1027-5606
EI 1607-7938
J9 HYDROL EARTH SYST SC
JI Hydrol. Earth Syst. Sci.
PD JAN 9
PY 2017
VL 21
IS 1
BP 133
EP 151
DI 10.5194/hess-21-133-2017
PG 19
WC Geosciences, Multidisciplinary; Water Resources
SC Geology; Water Resources
GA EK1JN
UT WOS:000393681700002
ER
PT J
AU Stone, RP
Malecha, PW
Masuda, MM
AF Stone, Robert P.
Malecha, Patrick W.
Masuda, Michele M.
TI A Five-Year, In Situ Growth Study on Shallow-Water Populations of the
Gorgonian Octocoral Calcigorgia spiculifera in the Gulf of Alaska
SO PLOS ONE
LA English
DT Article
ID CORALLIUM-RUBRUM; DEEP-SEA; HABITAT; AGE; ASSOCIATIONS; RATES
AB Gorgonian octocorals are the most abundant corals in Alaska where they provide important structural habitat for managed species of demersal fish and invertebrates. Fifty-nine gorgonian species have been reported from Alaska waters but little is known about their life history characteristics to help us gauge their ability to recover from seafloor disturbance. Colonies of the holaxonian Calcigorgia spiculifera were tagged beginning in 1999 at three sites in Chatham Strait, Southeast Alaska, using scuba and their growth measured annually for up to 5 years. Colonies were video recorded, and computer image analysis tools provided calibration of video images for measuring the length of several branches. Growth data indicate that C. spiculifera grows much slower (6.0 mm yr(-1)) than other gorgonians in Alaska for which there are data and that intraspecific growth is highly variable. We fit a Bayesian linear mixed-effects model that showed that average colony growth was significantly reduced with warmer temperature and presence of necrosis. The model further indicated that growth may slow among larger (older) colonies. Based on these results and previous studies, we propose that gorgonian growth rates are taxonomically constrained at the Suborder level and that holaxonians grow the slowest followed by scleraxonians and calcaxonians (2-3 times as fast). Findings of this study indicate that it would take approximately 60 years for C. spiculifera to grow to its maximum size and depending on the location and size of the parental standing stock, at least one and possibly 10 additional years for recruitment to occur. Our results further indicate that colonies that are injured, perhaps chronically in areas of frequent disturbance, grow at slower rates and if the current trend of ocean warming continues then we can expect these corals to grow more slowly, and the habitats they form will require more time to recover from disturbance.
C1 [Stone, Robert P.; Malecha, Patrick W.; Masuda, Michele M.] NOAA, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Juneau, AK 99801 USA.
RP Stone, RP (reprint author), NOAA, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Juneau, AK 99801 USA.
EM bob.stone@noaa.gov
FU Alaska Fisheries Science Center of NOAA Fisheries
FX We thank Ken Krieger, Linc Freese, Alex Wertheimer, Chuck O'Clair,
Strydr Nutting, and Chris Lunsford for their assistance in the field,
Jeff Regelin for performing the initial computer image analyses, Lou
Barr for sharing his vast knowledge about the distribution of shallow
water corals in Southeast Alaska, and Bruce Wing for help conceiving the
original concept of this project. We thank Sandra Brooke (Florida State
University Coastal and Marine Laboratory) for examining the reproductive
biology of the coral specimens. We thank the captains and crew of the
NOAA ship John N. Cobb for their assistance and support. This project
was funded by the Alaska Fisheries Science Center of NOAA Fisheries. The
findings and conclusions in this manuscript are those of the authors and
do not necessarily represent the views of the National Marine Fisheries
Service, NOAA.
NR 41
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U1 4
U2 4
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD JAN 9
PY 2017
VL 12
IS 1
AR e0169470
DI 10.1371/journal.pone.0169470
PG 16
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EH5WO
UT WOS:000391843900037
PM 28068374
ER
PT J
AU Qiu, B
Nakano, T
Chen, SM
Klein, P
AF Qiu, Bo
Nakano, Toshiya
Chen, Shuiming
Klein, Patrice
TI Submesoscale transition from geostrophic flows to internal waves in the
northwestern Pacific upper ocean
SO NATURE COMMUNICATIONS
LA English
DT Article
ID EQUATORIAL UNDERCURRENT JETS; WESTERN NORTH PACIFIC; SUBTROPICAL
COUNTERCURRENT; SATELLITE ALTIMETRY; PART I; MESOSCALE; TURBULENCE;
CIRCULATION; DYNAMICS; IMPACT
AB With radar interferometry, the next-generation Surface Water and Ocean Topography satellite mission will improve the measured sea surface height resolution down to 15 km, allowing us to investigate for the first time the global upper ocean variability at the submesoscale range. Here, by analysing shipboard Acoustic Doppler Current Profiler measurements along 137 degrees E in the northwest Pacific of 2004-2016, we show that the observed upper ocean velocities are comprised of balanced geostrophic flows and unbalanced internal waves. The transition length scale, L-t, separating these two motions, is found to depend strongly on the energy level of local mesoscale eddy variability. In the eddy-abundant western boundary current region of Kuroshio, L-t can be shorter than 15 km, whereas L-t exceeds 200 km along the path of relatively stable North Equatorial Current. Judicious separation between the geostrophic and internal wave signals represents both a challenge and an opportunity for the Surface Water and Ocean Topography mission.
C1 [Qiu, Bo; Chen, Shuiming] Univ Hawaii Manoa, Dept Oceanog, 1000 Pope Rd, Honolulu, HI 96822 USA.
[Nakano, Toshiya] Japan Meteorol Agcy, Global Environm & Marine Dept, Chiyoda Ku, 1-3-4 Otemachi, Tokyo 1008122, Japan.
[Klein, Patrice] IFREMER, Lab Oceanog Phys & Spatiale, CNRS, UBO,IRD, F-29280 Plouzane, France.
[Klein, Patrice] CALTECH, Environm Sci & Engn, Pasadena, CA 91125 USA.
[Klein, Patrice] NASA, JPL, Pasadena, CA USA.
RP Qiu, B (reprint author), Univ Hawaii Manoa, Dept Oceanog, 1000 Pope Rd, Honolulu, HI 96822 USA.
EM bo@soest.hawaii.edu
RI Qiu, Bo/D-9569-2017
FU NASA [NNX16AH66G, NNX13AE51E]; CNRS (France); LabexMer
[ANR-10-LABX-19-01]; NASA-CNES SWOT mission
FX We are grateful to the past and present captains and crews of R/V Ryofu
Maru and Keifu Maru, and staff of the Marine Division, Japan
Meteorological Agency, for their laudable long-term observational
efforts. We thank Jules Hummon and Eric Firing for help with the
processing and deciphering of the shipboard ADCP data, and Lee Fu and
Jinbo Wang for their in-depth discussions. B.Q. and S.C. acknowledge
support from NASA SWOT and OSTST missions (NNX16AH66G and NNX13AE51E).
P.K. acknowledges support of CNRS (France), LabexMer
(ANR-10-LABX-19-01), as well as of the NASA-CNES SWOT mission.
NR 48
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U1 12
U2 12
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2041-1723
J9 NAT COMMUN
JI Nat. Commun.
PD JAN 9
PY 2017
VL 8
AR 14055
DI 10.1038/ncomms14055
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EG9GD
UT WOS:000391366000001
PM 28067242
ER
PT J
AU Albert, A
Anderson, B
Bechtol, K
Drlica-Wagner, A
Meyer, M
Sanchez-Conde, M
Strigari, L
Wood, M
Abbott, TMC
Abdalla, FB
Benoit-Levy, A
Bernstein, GM
Bernstein, RA
Bertin, E
Brooks, D
Burke, DL
Rosell, AC
Kind, MC
Carretero, J
Crocce, M
Cunha, CE
D'Andrea, CB
da Costa, LN
Desai, S
Diehl, HT
Dietrich, JP
Doel, P
Eifler, TF
Evrard, AE
Neto, AF
Finley, DA
Flaugher, B
Fosalba, P
Frieman, J
Gerdes, DW
Goldstein, DA
Gruen, D
Gruendl, RA
Honscheid, K
James, DJ
Kent, S
Kuehn, K
Kuropatkin, N
Lahav, O
Li, TS
Maia, MAG
March, M
Marshall, JL
Martini, P
Miller, CJ
Miquel, R
Neilsen, E
Nord, B
Ogando, R
Plazas, AA
Reil, K
Romer, AK
Rykoff, ES
Sanchez, E
Santiago, B
Schubnell, M
Sevilla-Noarbe, I
Smith, RC
Soares-Santos, M
Sobreira, F
Suchyta, E
Swanson, MEC
Tarle, G
Vikram, V
Walker, AR
Wechsler, RH
AF Albert, A.
Anderson, B.
Bechtol, K.
Drlica-Wagner, A.
Meyer, M.
Sanchez-Conde, M.
Strigari, L.
Wood, M.
Abbott, T. M. C.
Abdalla, F. B.
Benoit-Levy, A.
Bernstein, G. M.
Bernstein, R. A.
Bertin, E.
Brooks, D.
Burke, D. L.
Rosell, A. Carnero
Kind, M. Carrasco
Carretero, J.
Crocce, M.
Cunha, C. E.
D'Andrea, C. B.
da Costa, L. N.
Desai, S.
Diehl, H. T.
Dietrich, J. P.
Doel, P.
Eifler, T. F.
Evrard, A. E.
Fausti Neto, A.
Finley, D. A.
Flaugher, B.
Fosalba, P.
Frieman, J.
Gerdes, D. W.
Goldstein, D. A.
Gruen, D.
Gruendl, R. A.
Honscheid, K.
James, D. J.
Kent, S.
Kuehn, K.
Kuropatkin, N.
Lahav, O.
Li, T. S.
Maia, M. A. G.
March, M.
Marshall, J. L.
Martini, P.
Miller, C. J.
Miquel, R.
Neilsen, E.
Nord, B.
Ogando, R.
Plazas, A. A.
Reil, K.
Romer, A. K.
Rykoff, E. S.
Sanchez, E.
Santiago, B.
Schubnell, M.
Sevilla-Noarbe, I.
Smith, R. C.
Soares-Santos, M.
Sobreira, F.
Suchyta, E.
Swanson, M. E. C.
Tarle, G.
Vikram, V.
Walker, A. R.
Wechsler, R. H.
CA FERMI-LAT Collaboration
DES Collaboration
TI SEARCHING FOR DARK MATTER ANNIHILATION IN RECENTLY DISCOVERED MILKY WAY
SATELLITES WITH FERMI-LAT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dark matter; galaxies: dwarf; gamma rays: galaxies
ID LARGE-AREA TELESCOPE; DWARF SPHEROIDAL GALAXY; PAN-STARRS1 3-PI SURVEY;
GAMMA-RAY EMISSION; ENERGY SURVEY DATA; ALL-SKY SURVEY;
GLOBULAR-CLUSTER; SOURCE CATALOG; TRIANGULUM II; RETICULUM II
AB We search for excess gamma-ray emission coincident with the positions of confirmed and candidate Milky Way satellite galaxies using six years of data from the Fermi Large Area Telescope (LAT). Our sample of 45 stellar systems includes 28 kinematically confirmed dark-matter-dominated dwarf spheroidal galaxies (dSphs) and 17 recently discovered systems that have photometric characteristics consistent with the population of known dSphs. For each of these targets, the relative predicted gamma-ray flux due to dark matter annihilation is taken from kinematic analysis if available, and estimated from a distance-based scaling relation otherwise, assuming that the stellar systems are DM-dominated dSphs. LAT data coincident with four of the newly discovered targets show a slight preference (each similar to 2 sigma local) for gamma-ray emission in excess of the background. However, the ensemble of derived gamma-ray flux upper limits for individual targets is consistent with the expectation from analyzing random blank-sky regions, and a combined analysis of the population of stellar systems yields no globally significant excess (global significance < 1 sigma). Our analysis has increased sensitivity compared to the analysis of 15 confirmed dSphs by Ackermann et al. The observed constraints on the DM annihilation cross section are statistically consistent with the background expectation, improving by a factor of similar to 2 for large DM masses (m(DM, b<(b)over bar>) greater than or similar to 1 TeV and m(DM, tau+tau-) greater than or similar to 70 GeV) and weakening by a factor of similar to 1.5 at lower masses relative to previously observed limits.
C1 [Albert, A.; Wood, M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Anderson, B.; Meyer, M.; Sanchez-Conde, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Anderson, B.; Meyer, M.; Sanchez-Conde, M.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Bechtol, K.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Bechtol, K.] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA.
[Drlica-Wagner, A.; Diehl, H. T.; Finley, D. A.; Flaugher, B.; Frieman, J.; Kent, S.; Kuropatkin, N.; Neilsen, E.; Nord, B.; Soares-Santos, M.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA.
[Strigari, L.; Li, T. S.; Marshall, J. L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
[Strigari, L.; Li, T. S.; Marshall, J. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
[Abbott, T. M. C.; James, D. J.; Smith, R. C.; Walker, A. R.] Cerro Tololo Interamer Observ, Natl Opt Astron Observ, Casilla 603, La Serena, Chile.
[Abdalla, F. B.; Benoit-Levy, A.; Brooks, D.; Doel, P.; Lahav, O.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Abdalla, F. B.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa.
[Benoit-Levy, A.; Bertin, E.] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Benoit-Levy, A.; Bertin, E.] Univ Paris 06, Sorbonne Univ, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Bernstein, G. M.; Eifler, T. F.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Bernstein, R. A.] Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA.
[Burke, D. L.; Cunha, C. E.; Gruen, D.; Rykoff, E. S.; Wechsler, R. H.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA.
[Burke, D. L.; Gruen, D.; Reil, K.; Rykoff, E. S.; Wechsler, R. H.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA.
[Rosell, A. Carnero; Fausti Neto, A.; Maia, M. A. G.; Ogando, R.; Santiago, B.; Sobreira, F.] Lab Interinst eAstron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, Brazil.
[Rosell, A. Carnero; da Costa, L. N.; Maia, M. A. G.; Ogando, R.] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, Brazil.
[Kind, M. Carrasco; Gruendl, R. A.; Sevilla-Noarbe, I.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA.
[Kind, M. Carrasco; Gruendl, R. A.; Swanson, M. E. C.] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA.
[Carretero, J.; Crocce, M.; Fosalba, P.] IEEC CSIC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain.
[Carretero, J.; Miquel, R.] Barcelona Inst Sci & Technol, Inst Fisica Altes Energies, Campus UAB, E-08193 Barcelona, Spain.
[D'Andrea, C. B.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[D'Andrea, C. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Desai, S.; Dietrich, J. P.] Excellence Cluster Univ, Boltzmannstr 2, D-85748 Garching, Germany.
[Desai, S.; Dietrich, J. P.] Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany.
[Eifler, T. F.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Evrard, A. E.; Miller, C. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Evrard, A. E.; Miller, C. J.; Schubnell, M.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Frieman, J.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Goldstein, D. A.] Univ Calif Berkeley, Dept Astron, 501 Campbell Hall, Berkeley, CA 94720 USA.
[Goldstein, D. A.] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA.
[Honscheid, K.; Martini, P.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Honscheid, K.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia.
[Martini, P.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Miquel, R.] Inst Catalana Rec & Estud Avancats, E-08010 Barcelona, Spain.
[Romer, A. K.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England.
[Sanchez, E.; Sevilla-Noarbe, I.] CIEMAT, Madrid, Spain.
[Santiago, B.] Univ Fed Rio Grande do Sul, Inst Fis, Caixa Postal 15051, BR-91501970 Porto Alegre, RS, Brazil.
[Vikram, V.] Argonne Natl Lab, 9700 South Cass Ave, Lemont, IL 60439 USA.
[Wechsler, R. H.] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA.
RP Albert, A; Wood, M (reprint author), Los Alamos Natl Lab, Los Alamos, NM 87545 USA.; Bechtol, K (reprint author), Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.; Bechtol, K (reprint author), Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA.; Drlica-Wagner, A (reprint author), Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA.; Strigari, L (reprint author), Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.; Strigari, L (reprint author), Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
EM amalbert@lanl.gov; keith.bechtol@icecube.wisc.edu; kadrlica@fnal.gov;
strigari@physics.tamu.edu; mdwood@slac.stanford.edu
RI Ogando, Ricardo/A-1747-2010;
OI Ogando, Ricardo/0000-0003-2120-1154; Abdalla,
Filipe/0000-0003-2063-4345; Sobreira, Flavia/0000-0002-7822-0658
FU U.S. Department of Energy; U.S. National Science Foundation; Ministry of
Science and Education of Spain; Science and Technology Facilities
Council of the United Kingdom; Higher Education Funding Council for
England; National Center for Supercomputing Applications at the
University of Illinois at Urbana-Champaign; Kavli Institute of
Cosmological Physics at the University of Chicago; Center for Cosmology
and Astro-Particle Physics at the Ohio State University; Mitchell
Institute for Fundamental Physics and Astronomy at Texas AM University;
Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de
Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de
Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia,
Tecnologia e Inovacao; Deutsche Forschungsgemeinschaft; National Science
Foundation [AST-1138766]; MINECO [AYA2012-39559, ESP2013-48274,
FPA2013-47986]; Centro de Excelencia Severo Ochoa [SEV-2012-0234]; ERDF
funds from the European Union; Argonne National Laboratory; University
of California at Santa Cruz; University of Cambridge; Centro de
Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid;
University of Chicago; University College London; DES-Brazil Consortium;
University of Edinburgh; Eidgenossische Technische Hochschule (ETH)
Zurich; Fermi National Accelerator Laboratory; University of Illinois at
Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC); Institut
de Fisica d'Altes Energies; Lawrence Berkeley National Laboratory;
Ludwig-Maximilians Universitat Munchen and the associated Excellence
Cluster universe; University of Michigan; National Optical Astronomy
Observatory; University of Nottingham; Ohio State University; University
of Pennsylvania; University of Portsmouth; SLAC National Accelerator
Laboratory; Stanford University; University of Sussex; Texas AM
University
FX Funding for the DES Projects has been provided by the U.S. Department of
Energy, the U.S. National Science Foundation, the Ministry of Science
and Education of Spain, the Science and Technology Facilities Council of
the United Kingdom, the Higher Education Funding Council for England,
the National Center for Supercomputing Applications at the University of
Illinois at Urbana-Champaign, the Kavli Institute of Cosmological
Physics at the University of Chicago, the Center for Cosmology and
Astro-Particle Physics at the Ohio State University, the Mitchell
Institute for Fundamental Physics and Astronomy at Texas A&M University,
Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de
Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de
Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia,
Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft and the
Collaborating Institutions in the DES. The DES data management system is
supported by the National Science Foundation under Grant Number
AST-1138766. The DES participants from Spanish institutions are
partially supported by MINECO under grants AYA2012-39559, ESP2013-48274,
FPA2013-47986, and Centro de Excelencia Severo Ochoa SEV-2012-0234, some
of which include ERDF funds from the European Union.; The Collaborating
Institutions are Argonne National Laboratory, the University of
California at Santa Cruz, the University of Cambridge, Centro de
Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the
University of Chicago, University College London, the DES-Brazil
Consortium, the University of Edinburgh, the Eidgenossische Technische
Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the
University of Illinois at Urbana-Champaign, the Institut de Ciencies de
l'Espai (IEEC/CSIC), the Institut de Fisica d'Altes Energies, Lawrence
Berkeley National Laboratory, the Ludwig-Maximilians Universitat Munchen
and the associated Excellence Cluster universe, the University of
Michigan, the National Optical Astronomy Observatory, the University of
Nottingham, The Ohio State University, the University of Pennsylvania,
the University of Portsmouth, SLAC National Accelerator Laboratory,
Stanford University, the University of Sussex, and Texas A&M University.
NR 82
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 6
PY 2017
VL 834
IS 2
AR 110
DI 10.3847/1538-4357/834/2/110
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EK1HZ
UT WOS:000393677700004
ER
PT J
AU Blagorodnova, N
Kotak, R
Polshaw, J
Kasliwal, MM
Cao, Y
Cody, AM
Doran, GB
Elias-Rosa, N
Fraser, M
Fremling, C
Gonzalez-Fernandez, C
Harmanen, J
Jencson, J
Kankare, E
Kudritzki, RP
Kulkarni, SR
Magnier, E
Manulis, I
Masci, FJ
Mattila, S
Nugent, P
Ochner, P
Pastorello, A
Reynolds, T
Smith, K
Sollerman, J
Taddia, F
Terreran, G
Tomasella, L
Turatto, M
Vreeswijk, PM
Wozniak, P
Zaggia, S
AF Blagorodnova, N.
Kotak, R.
Polshaw, J.
Kasliwal, M. M.
Cao, Y.
Cody, A. M.
Doran, G. B.
Elias-Rosa, N.
Fraser, M.
Fremling, C.
Gonzalez-Fernandez, C.
Harmanen, J.
Jencson, J.
Kankare, E.
Kudritzki, R. -P.
Kulkarni, S. R.
Magnier, E.
Manulis, I.
Masci, F. J.
Mattila, S.
Nugent, P.
Ochner, P.
Pastorello, A.
Reynolds, T.
Smith, K.
Sollerman, J.
Taddia, F.
Terreran, G.
Tomasella, L.
Turatto, M.
Vreeswijk, P. M.
Wozniak, P.
Zaggia, S.
TI COMMON ENVELOPE EJECTION FOR A LUMINOUS RED NOVA IN M101
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: close; novae, cataclysmic variables; stars: individual (M101
OT2015-1, PSN J14021678+5426205); stars: massive; stars: winds, outflows
ID V838 MONOCEROTIS; SN 2008S; NGC 300; PHOTOMETRIC CALIBRATION; OPTICAL
TRANSIENTS; V4332 SAGITTARII; SPACE-TELESCOPE; BLUE VARIABLES;
CORE-COLLAPSE; UGC 2773-OT
AB We present the results of optical, near-infrared, and mid-infrared observations of M101 OT2015-1 (PSN J14021678+ 5426205), a luminous red transient in the Pinwheel galaxy (M101), spanning a total of 16 years. The light curve showed two distinct peaks with absolute magnitudes M-r <= -12.4 and M-r similar or equal to -12, on 2014 November 11 and 2015 February 17, respectively. The spectral energy distributions during the second maximum show a cool outburst temperature of approximate to 3700 K and low expansion velocities (approximate to -300 km s(-1)) for the H I, Ca II, Ba II, and K I lines. From archival data spanning 15-8 years before the outburst, we find a single source consistent with the optically discovered transient, which we attribute to being the progenitor; it has properties consistent with being an F-type yellow supergiant with L similar to 8.7 x 10(4) L-circle dot, T-eff approximate to 7000. K, and an estimated mass of M1= 18 +/- 1 M-circle dot. This star has likely just finished the H-burning phase in the core, started expanding, and is now crossing the Hertzsprung gap. Based on the combination of observed properties, we argue that the progenitor is a binary system, with the more evolved system overfilling the Roche lobe. Comparison with binary evolution models suggests that the outburst was an extremely rare phenomenon, likely associated with the ejection of the common envelope of a massive star. The initial mass of the primary fills the gap between the merger candidates V838 Mon (5-10 M-circle dot) and NGC. 4490-OT. (30M(circle dot)).
C1 [Blagorodnova, N.; Kasliwal, M. M.; Cao, Y.; Jencson, J.; Kulkarni, S. R.; Masci, F. J.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Blagorodnova, N.; Fraser, M.; Gonzalez-Fernandez, C.; Mattila, S.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Kotak, R.; Polshaw, J.; Kankare, E.; Smith, K.; Terreran, G.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Cody, A. M.] CALTECH, Spitzer Sci Ctr, 1200 East Calif Blvd, Pasadena, CA 91125 USA.
[Doran, G. B.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
[Elias-Rosa, N.; Ochner, P.; Pastorello, A.; Terreran, G.; Tomasella, L.; Turatto, M.; Zaggia, S.] INAF, Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy.
[Fremling, C.; Sollerman, J.; Taddia, F.] Stockholm Univ, Dept Astron, Oskar Klein Ctr, AlbaNova, SE-10691 Stockholm, Sweden.
[Harmanen, J.; Mattila, S.; Reynolds, T.] Univ Turku, Dept Phys & Astron, Tuorla Observ, Vaisalantie 20, FI-21500 Piikkio, Finland.
[Kudritzki, R. -P.; Magnier, E.] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
[Manulis, I.; Vreeswijk, P. M.] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-7610001 Rehovot, Israel.
[Nugent, P.] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Reynolds, T.] Nord Opt Telescope, Apartado 474, E-38700 Santa Cruz De La Palma, Spain.
[Wozniak, P.] Los Alamos Natl Lab, MS-D466, Los Alamos, NM 87545 USA.
RP Blagorodnova, N (reprint author), CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
OI Fraser, Morgan/0000-0003-2191-1674; Kotak, Rubina/0000-0001-5455-3653;
Fremling, Christoffer/0000-0002-4223-103X
FU European Union [264895]; European Union FP7 programme through ERC grant
[320360]; European Science Foundation under the GREAT ESF RNP programme;
GROWTH project - National Science Foundation [1545949]; US Department of
Energy as part of the Laboratory Directed Research and Development
program; PRIN-INAF
FX The research leading to these results has received funding from the
European Union Seventh Framework Programme ([FP7/2007-2013] under grant
agreement no. 264895. This work was partly supported by the European
Union FP7 programme through ERC grant no. 320360. This work was
supported, in whole or in part, by the European Science Foundation under
the GREAT ESF RNP programme. This work was supported by the GROWTH
project funded by the National Science Foundation under grant no.
1545949. LANL participation in iPTF was funded by the US Department of
Energy as part of the Laboratory Directed Research and Development
program. Part of this research was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration. Based on observations
obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/IRFU,
at the Canada-France-Hawaii Telescope (CFHT), which is operated by the
National Research Council (NRC) of Canada, the Institut National des
Science de l'Univers of the Centre National de la Recherche Scientifique
(CNRS) of France, and the University of Hawaii. This work is based in
part on data products produced at Terapix available at the Canadian
Astronomy Data Centre as part of the Canada-France-Hawaii Telescope
Legacy Survey, a collaborative project of NRC and CNRS. This paper makes
use of data obtained from the Isaac Newton Group Archive, which is
maintained as part of the CASU Astronomical Data Centre at the Institute
of Astronomy, Cambridge. This work is partly based on observations
obtained with the Nordic Optical Telescope, operated by the Nordic
Optical Telescope Scientific Association at the Observatorio del Roque
de los Muchachos, La Palma, Spain. This work is partly based on
observations made with the William Hershell Telescope operated on the
island of La Palma by the Isaac Newton Group in the Spanish Observatorio
del Roque de los Muchachos of the Instituto de Astrofsica de Canarias.
The Gran Telescopio Canarias (GTC) operated on the island of La Palma at
the Spanish Observatorio del Roque de los Muchachos of the Instituto de
Astrofisica de Canarias. This work is partly based on data from
Copernico 1.82 m telescope operated by INAF Osservatorio Astronomico di
Padova. NER, AP, GT, and MT are partially supported by the PRIN-INAF
2014 with the project "Transient universe: unveiling new types of
stellar explosions with PESSTO." Finally, NBM would like to thank the
anonymous referee, who helped to improve the manuscript, Robert G.
Izzard, Philipp Podsiadlowski, Lars Bildsten, E. Sterl Phinney, and Noam
Soker for helpful discussions, and Pablo and Lucia Solis, and Israel
Zenteno for the motivation.
NR 85
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 6
PY 2017
VL 834
IS 2
AR 107
DI 10.3847/1538-4357/834/2/107
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EK1HZ
UT WOS:000393677700001
ER
PT J
AU Prettyman, TH
Yamashita, N
Toplis, MJ
McSween, HY
Schorghofer, N
Marchi, S
Feldman, WC
Castillo-Rogez, J
Forni, O
Lawrence, DJ
Ammannito, E
Ehlmann, BL
Sizemore, HG
Joy, SP
Polanskey, CA
Rayman, MD
Raymond, CA
Russell, CT
AF Prettyman, T. H.
Yamashita, N.
Toplis, M. J.
McSween, H. Y.
Schorghofer, N.
Marchi, S.
Feldman, W. C.
Castillo-Rogez, J.
Forni, O.
Lawrence, D. J.
Ammannito, E.
Ehlmann, B. L.
Sizemore, H. G.
Joy, S. P.
Polanskey, C. A.
Rayman, M. D.
Raymond, C. A.
Russell, C. T.
TI Extensive water ice within Ceres' aqueously altered regolith: Evidence
from nuclear spectroscopy
SO SCIENCE
LA English
DT Article
ID METEORITE; ASTEROIDS; MODEL
AB The surface elemental composition of dwarf planet Ceres constrains its regolith ice content, aqueous alteration processes, and interior evolution. Using nuclear spectroscopy data acquired by NASA's Dawn mission, we determined the concentrations of elemental hydrogen, iron, and potassium on Ceres. The data show that surface materials were processed by the action of water within the interior. The non-icy portion of Ceres' carbon-bearing regolith contains similar amounts of hydrogen to those present in aqueously altered carbonaceous chondrites; however, the concentration of iron on Ceres is lower than in the aforementioned chondrites. This allows for the possibility that Ceres experienced modest ice-rock fractionation, resulting in differences between surface and bulk composition. At mid-to-high latitudes, the regolith contains high concentrations of hydrogen, consistent with broad expanses of water ice, confirming theoretical predictions that ice can survive for billions of years just beneath the surface.
C1 [Prettyman, T. H.; Yamashita, N.; Feldman, W. C.; Sizemore, H. G.] Planetary Sci Inst, 1700 East Ft Lowell,Suite 106, Tucson, AZ 85719 USA.
[Toplis, M. J.; Forni, O.] Univ Paul Sabatier, CNRS, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France.
[McSween, H. Y.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Schorghofer, N.] Univ Hawaii, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
[Marchi, S.] Southwest Res Inst, Boulder, CO 80302 USA.
[Castillo-Rogez, J.; Ehlmann, B. L.; Polanskey, C. A.; Rayman, M. D.; Raymond, C. A.] CALTECH, JPL, Pasadena, CA 91109 USA.
[Lawrence, D. J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Ammannito, E.; Joy, S. P.; Russell, C. T.] Univ Calif Los Angeles, Earth Planetary & Space Sci, Los Angeles, CA 90095 USA.
[Ehlmann, B. L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Prettyman, TH (reprint author), Planetary Sci Inst, 1700 East Ft Lowell,Suite 106, Tucson, AZ 85719 USA.
EM prettyman@psi.edu
FU JPL, California Institute of Technology; NASA; NASA Dawn at Ceres Guest
Investigator Program; NASA Discovery Program Office
FX Portions of this work were performed by the Planetary Science Institute
under contract with JPL, California Institute of Technology; by JPL
under contract with NASA; and by the NASA Dawn at Ceres Guest
Investigator Program. The Dawn mission is led by the University of
California, Los Angeles, and is managed by JPL under the auspices of the
NASA Discovery Program Office. The Dawn data are archived with the NASA
Planetary Data System (http://sbn.psi.edu/pds/archive/dawn.html).
NR 25
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PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD JAN 6
PY 2017
VL 355
IS 6320
BP 55
EP 58
DI 10.1126/science.aah6765
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EH4KK
UT WOS:000391739900041
PM 27980087
ER
PT J
AU Afsar, MZ
Leib, SJ
Bozak, RF
AF Afsar, M. Z.
Leib, S. J.
Bozak, R. F.
TI Effect of de-correlating turbulence on the low frequency decay of
jet-surface interaction noise in sub-sonic unheated air jets using a
CFD-based approach
SO JOURNAL OF SOUND AND VIBRATION
LA English
DT Article
DE Jet-surface interaction; Trailing edge noise; Rapid-distortion theory
ID SHEARED MEAN FLOWS; CONTRACTING STREAM; AERODYNAMIC SOUND; UNSTEADY
MOTION; SCATTERING; AEROACOUSTICS; DISTORTION; VICINITY; PLATE
AB In this paper we extend the Rapid-distortion theory (RDT)-based model derived by Goldstein, Afsar & Leib (J. Fluid Mech., vol. 736, pp. 532-569, 2013) for the sound generated by the interaction of a large-aspect-ratio rectangular jet with the trailing edge of a flat plate to include a more realistic upstream turbulence spectrum that possess a de correlation (i.e. negative dip) in its space-time structure and use results from three-dimensional Reynolds-Averaged Navier-Stokes (RANS) solutions to determine the mean flow, turbulent kinetic energy and turbulence length & time scales. Since the interaction noise dominates the low-frequency portion of the spectrum, we use an appropriate asymptotic approximation for the Rayleigh equation Green's function, which enters the analysis, based on a two-dimensional mean flow representation for the jet. We use the model to predict jet-surface interaction noise for a range of subsonic acoustic Mach number jets, nozzle aspect ratios, streamwise and transverse trailing-edge locations and compare them with experimental data. The RANS meanflow computations are also compared with flow data for selected cases to assess their validity. We find that finite de correlation in the turbulence spectrum increases the low-frequency algebraic decay (the low-frequency "roll-off") of the acoustic spectrum with angular frequency to give a model that has a pure dipole frequency scaling. This gives better agreement with noise data compared to Goldstein et al. (2013) for Strouhal numbers less than the peak jet-surface interaction noise. For example, through sensitivity analysis we find that there is a difference of 10 dB at the lowest frequency for which data exists (relative to a model without de-correlation effects included) for the highest acoustic Mach number case. Secondly, our results for the planar flow theory provide a first estimate of the low-frequency amplification due to the jet-surface interaction for moderate aspect ratio nozzles when RANS meanflow quantities are used appropriately. This work will hopefully add to noise prediction efforts for aircraft configurations in which the exhaust systems are tightly integrated with the airframe. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Afsar, M. Z.] Univ Strathclyde, Dept Mech & Aerosp Engn, 75 Montrose St, Glasgow G1 1XJ, Lanark, Scotland.
[Leib, S. J.] Ohio Aerosp Inst, 22800 Cedar Point Rd, Cleveland, OH 44142 USA.
[Bozak, R. F.] Glenn Res Ctr, Natl Aeronaut & Space Adm, Cleveland, OH 44135 USA.
RP Afsar, MZ (reprint author), Univ Strathclyde, Dept Mech & Aerosp Engn, 75 Montrose St, Glasgow G1 1XJ, Lanark, Scotland.
EM mohammed.afsar@strath.ac.uk
FU Chapman Fellowship at Imperial College London, Department of
Mathematics; NASA Fundamental Aeronautics Program, High Speed Project
FX MZA would like to thank financial support from Chapman Fellowship
(2013-2014) at Imperial College London, Department of Mathematics and
would like to thank Professor J. T. Stuart of Imperial College for his
most insightful comments. The work was also supported by the NASA
Fundamental Aeronautics Program, High Speed Project. The authors would
like to thank Drs. Khairul Zaman, James Bridges and Clifford Brown for
providing their experimental data.
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U1 7
U2 7
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0022-460X
EI 1095-8568
J9 J SOUND VIB
JI J. Sound Vibr.
PD JAN 6
PY 2017
VL 386
BP 177
EP 207
DI 10.1016/j.jsv.2016.08.021
PG 31
WC Acoustics; Engineering, Mechanical; Mechanics
SC Acoustics; Engineering; Mechanics
GA EC5DD
UT WOS:000388152400012
ER
PT J
AU Chatterjee, S
Law, CJ
Wharton, RS
Burke-Spolaor, S
Hessels, JWT
Bower, GC
Cordes, JM
Tendulkar, SP
Bassa, CG
Demorest, P
Butler, BJ
Seymour, A
Scholz, P
Abruzzo, MW
Bogdanov, S
Kaspi, VM
Keimpema, A
Lazio, TJW
Marcote, B
McLaughlin, MA
Paragi, Z
Ransom, SM
Rupen, M
Spitler, LG
van Langevelde, HJ
AF Chatterjee, S.
Law, C. J. .
Wharton, R. S.
Burke-Spolaor, S.
Hessels, J. W. T.
Bower, G. C.
Cordes, J. M.
Tendulkar, S. P.
Bassa, C. G.
Demorest, P.
Butler, B. J.
Seymour, A.
Scholz, P.
Abruzzo, M. W.
Bogdanov, S.
Kaspi, V. M.
Keimpema, A.
Lazio, T. J. . W.
Marcote, B.
McLaughlin, M. A.
Paragi, Z.
Ransom, S. M.
Rupen, M.
Spitler, L. G.
van Langevelde, H. J. .
TI A direct localization of a fast radio burst and its host
SO NATURE
LA English
DT Article
ID GAMMA-RAY BURSTS; PHOTOMETRIC SYSTEM; DISPERSION MEASURE; ALPHA SURVEY;
MILKY-WAY; GALAXIES; PULSES; STARS; EMISSION; REDSHIFT
AB Fast radio bursts(1,2) are astronomical radio flashes of unknown physical nature with durations of milliseconds. Their dispersive arrival times suggest an extragalactic origin and imply radio luminosities that are orders of magnitude larger than those of all known short-duration radio transients(3). So far all fast radio bursts have been detected with large single-dish telescopes with arcminute localizations, and attempts to identify their counterparts (source or host galaxy) have relied on the contemporaneous variability of field sources(4) or the presence of peculiar field stars(5) or galaxies(4). These attempts have not resulted in an unambiguous association(6,7) with a host or multi-wavelength counterpart. Here we report the subarcsecond localization of the fast radio burst FRB 121102, the only known repeating burst source(8-11), using high-time-resolution radio interferometric observations that directly image the bursts. Our precise localization reveals that FRB 121102 originates within 100 milliarcseconds of a faint 180-microJansky persistent radio source with a continuum spectrum that is consistent with non-thermal emission, and a faint (twenty-fifth magnitude) optical counterpart. The flux density of the persistent radio source varies by around ten per cent on day timescales, and very long baseline radio interferometry yields an angular size of less than 1.7 milliarcseconds. Our observations are inconsistent with the fast radio burst having a Galactic origin or its source being located within a prominent star-forming galaxy. Instead, the source appears to be co-located with a low-luminosity active galactic nucleus or a previously unknown type of extragalactic source. Localization and identification of a host or counterpart has been essential to understanding the origins and physics of other kinds of transient events, including gamma-ray bursts(12,13) and tidal disruption events(14). However, if other fast radio bursts have similarly faint radio and optical counterparts, our findings imply that direct subarcsecond localizations may be the only way to provide reliable associations.
C1 [Chatterjee, S.; Wharton, R. S.; Cordes, J. M.] Cornell Univ, Cornell Ctr Astrophys & Planetary Sci, Ithaca, NY 14853 USA.
[Chatterjee, S.; Wharton, R. S.; Cordes, J. M.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Law, C. J. .] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Law, C. J. .] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA.
[Burke-Spolaor, S.; Demorest, P.; Butler, B. J.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Burke-Spolaor, S.; McLaughlin, M. A.] West Virginia Univ, Dept Phys & Astron, Morgantown, WV 26506 USA.
[Burke-Spolaor, S.; McLaughlin, M. A.] West Virginia Univ, Ctr Gravitat Waves & Cosmol, Chestnut Ridge Res Bldg, Morgantown, WV 26505 USA.
[Hessels, J. W. T.; Bassa, C. G.] Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands.
[Hessels, J. W. T.] Univ Amsterdam, Anton Pannekoek Inst Astron, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.
[Bower, G. C.] Acad Sinica, Inst Astron & Astrophys, 645 N Aohoku Pl, Hilo, HI 96720 USA.
[Tendulkar, S. P.; Kaspi, V. M.] McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada.
[Tendulkar, S. P.; Kaspi, V. M.] McGill Univ, McGill Space Inst, 3600 Univ St, Montreal, PQ H3A 2T8, Canada.
[Seymour, A.] Arecibo Observ, HC3 Box 53995, Arecibo, PR 00612 USA.
[Scholz, P.; Rupen, M.] Natl Res Council Canada, Herzberg Astron & Astrophys, Domin Radio Astrophys Observ, POB 248, Penticton, BC V2A 6J9, Canada.
[Abruzzo, M. W.] Haverford Coll, 370 Lancaster Ave, Haverford, PA 19041 USA.
[Bogdanov, S.] Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA.
[Keimpema, A.; Marcote, B.; Paragi, Z.; van Langevelde, H. J. .] Joint Inst VLBI ERIC, Postbus 2, NL-7990 AA Dwingeloo, Netherlands.
[Lazio, T. J. . W.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Ransom, S. M.] Natl Radio Astron Observ, Edgemont Rd, Charlottesville, VA 22903 USA.
[Spitler, L. G.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[van Langevelde, H. J. .] Leiden Univ, Sterrewacht Leiden, Postbus 9513, NL-2300 RA Leiden, Netherlands.
RP Chatterjee, S (reprint author), Cornell Univ, Cornell Ctr Astrophys & Planetary Sci, Ithaca, NY 14853 USA.
EM shami.chatterjee@cornell.edu
NR 47
TC 3
Z9 3
U1 2
U2 2
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD JAN 5
PY 2017
VL 541
IS 7635
BP 58
EP +
DI 10.1038/nature20797
PG 12
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EN6NA
UT WOS:000396119500028
PM 28054614
ER
PT J
AU Smith, JA
Ndersen, TJA
Shortt, M
Gaffney, AM
Truffer, M
Stanton, TP
Bindschadler, R
Dutrieux, P
Enkins, AJ
Hillenbrand, CD
Ehrmann, W
Corr, HFJ
Farley, N
Crowhurst, S
Vaughan, DG
AF Smith, J. A.
Ndersen, T. J. A.
Shortt, M.
Gaffney, A. M.
Truffer, M.
Stanton, T. P.
Bindschadler, R.
Dutrieux, P.
Enkins, A. J.
Hillenbrand, C. -D.
Ehrmann, W.
Corr, H. F. J.
Farley, N.
Crowhurst, S.
Vaughan, D. G.
TI Sub-ice-shelf sediments record history of twentieth-century retreat of
Pine Island Glacier
SO NATURE
LA English
DT Article
ID AMUNDSEN SEA EMBAYMENT; WEST ANTARCTICA; GROUNDING-LINE; ROSS SEA;
SHEET; OCEAN; CORES; BAY; ACCUMULATION; VARIABILITY
AB The West Antarctic Ice Sheet is one of the largest potential sources of rising sea levels(1). Over the past 40 years, glaciers flowing into the Amundsen Sea sector of the ice sheet have thinned at an accelerating rate(2), and several numerical models suggest that unstable and irreversible retreat of the grounding line-which marks the boundary between grounded ice and floating ice shelf- is underway(3). Understanding this recent retreat requires a detailed knowledge of grounding-line history(4), but the locations of the grounding line before the advent of satellite monitoring in the 1990s are poorly dated. In particular, a history of grounding-line retreat is required to understand the relative roles of contemporaneous ocean-forced change and of ongoing glacier response to an earlier perturbation in driving ice-sheet loss. Here we show that the present thinning and retreat of Pine Island Glacier in West Antarctica is part of a climatically forced trend that was triggered in the 1940s. Our conclusions arise from analysis of sediment cores recovered beneath the floating Pine Island Glacier ice shelf, and constrain the date at which the grounding line retreated from a prominent seafloor ridge. We find that incursion of marine water beyond the crest of this ridge, forming an ocean cavity beneath the ice shelf, occurred in 1945 (+/- 12 years); final ungrounding of the ice shelf from the ridge occurred in 1970 (+/- 4 years). The initial opening of this ocean cavity followed a period of strong warming of West Antarctica, associated with El Nino activity. Thus our results suggest that, even when climate forcing weakened, ice-sheet retreat continued.
C1 [Smith, J. A.; Shortt, M.; Enkins, A. J.; Hillenbrand, C. -D.; Corr, H. F. J.; Farley, N.; Vaughan, D. G.] British Antarctic Survey, High Cross,Madingley Rd, Cambridge CB3 0ET, England.
[Ndersen, T. J. A.] Univ Copenhagen, Ctr Permafrost CENPERM, Dept Geosci & Nat Resource Management, DK-1350 Copenhagen K, Denmark.
[Gaffney, A. M.] Lawrence Livermore Natl Lab, Nucl & Chem Sci Div, Livermore, CA 94550 USA.
[Truffer, M.] Univ Alaska, Inst Geophys, Fairbanks, AK 99775 USA.
[Stanton, T. P.] Naval Postgrad Sch, Dept Oceanog, Monterey, CA 93943 USA.
[Bindschadler, R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Dutrieux, P.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Ehrmann, W.] Univ Leipzig, Inst Geophys & Geol, Talstr 35, D-04103 Leipzig, Germany.
[Farley, N.] Univ Geneva, Dept Earth Sci, 13 Rue Maraichers, CH-1205 Geneva, Switzerland.
[Crowhurst, S.] Univ Cambridge, Dept Earth Sci, Godwin Lab Palaeoclimate Res, Downing St, Cambridge CB2 3EQ, England.
RP Smith, JA (reprint author), British Antarctic Survey, High Cross,Madingley Rd, Cambridge CB3 0ET, England.
EM jaas@bas.ac.uk
OI Andersen, Thorbjorn Joest/0000-0001-5032-9945; Dutrieux,
Pierre/0000-0002-8066-934X
FU NSF's Office of Polar Programs under NSF [ANT-0732926, ANT 0732730];
NASA's Cryospheric Sciences Program; New York University Abhu Dabi
[1204]; Natural Environment Research Council-British Antarctic Survey
Polar Science for Planet Earth Programme; [DE-AC52-07NA27344];
[LLNL-JRNL-697878]
FX We thank D. Pomraning for help with designing and manning the hot-water
drill equipment. Logistic and safety support was provided by K. Gibbon,
D. Einerson, E. Steinarsson, F. McCarthy, S. Consalvi, S. King, the PIG
support camp personnel, and the National Science Foundation (NSF)
Antarctic support team. We particularly thank E. Steinarsson for his
help with sediment coring. This research project was supported by NSF's
Office of Polar Programs under NSF grants including ANT-0732926 and ANT
0732730; by funding from NASA's Cryospheric Sciences Program; by New
York University Abhu Dabi grant 1204; and by the Natural Environment
Research Council-British Antarctic Survey Polar Science for Planet Earth
Programme. Work at the Lawrence Livermore National Laboratory (LLNL) was
performed under contract DE-AC52-07NA27344; LLNL-JRNL-697878.
NR 45
TC 1
Z9 1
U1 4
U2 4
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD JAN 5
PY 2017
VL 541
IS 7635
BP 77
EP +
DI 10.1038/nature20136
PG 12
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EN6NA
UT WOS:000396119500032
PM 27880756
ER
PT J
AU Mosier-Boss, PA
Gordon, FE
Forsley, LP
Zhou, DZ
AF Mosier-Boss, P. A.
Gordon, F. E.
Forsley, L. P.
Zhou, Dazhuang
TI Detection of high energy particles using CR-39 detectors part 1: Results
of microscopic examination, scanning, and LET analysis
SO INTERNATIONAL JOURNAL OF HYDROGEN ENERGY
LA English
DT Article
DE Palladium; Nuclear particles; CR-39; LET spectrum; Energy distribution
ID NUCLEAR TRACK DETECTORS; HEAVY-WATER; NEUTRON EMISSION; DIFFERENT
DOSIMETERS; PALLADIUM CATHODES; TRITIUM PRODUCTION; CHARGED-PARTICLES;
D2O ELECTROLYSIS; D2SO4-D2O SOLUTION; HELIUM PRODUCTION
AB CR-39 detectors were used to detect high energy particles produced during Pd/D co-deposition. Upon completion of the experiments, the detectors were subjected to either microscopic examination, scanning using an automated scanner to obtain quantitative information on the tracks, sequential etching, or linear energy transfer (LET) spectrum analysis. Both the sequential etching and LET analysis allowed speciation of the particles that caused the tracks as well as estimating their energies. In these experiments it was shown that the tracks coincide with the placement of the Pd deposit. The average number of tracks obtained as a result of Pd/D co-deposition is more than 133 times greater than that found in the background. In this communication, the results of microscopic examination, scanning, and LET analysis are discussed. (C) 2016 Hydrogen Energy Publications LLC. Published by Elsevier Ltd. All rights reserved.
C1 [Mosier-Boss, P. A.] GEC, 5101B Backlick Rd, Annandale, VA 22003 USA.
[Gordon, F. E.] SPAWAR Syst Ctr Pacific, San Diego, CA 92122 USA.
[Forsley, L. P.] JWK Int Corp, Annandale, VA 22003 USA.
[Zhou, Dazhuang] Chinese Acad Sci, Natl Space Sci Ctr, Beijing 100190, Peoples R China.
[Zhou, Dazhuang] NASA, Johnson Space Ctr, 2101 Nasa Pkwy, Houston, TX 77058 USA.
[Zhou, Dazhuang] Univ Space Res Assoc, 3600 Bay Area Blvd, Houston, TX 77058 USA.
RP Mosier-Boss, PA (reprint author), GEC, 5101B Backlick Rd, Annandale, VA 22003 USA.; Zhou, DZ (reprint author), NASA, Johnson Space Ctr, 2101 Nasa Pkwy, Houston, TX 77058 USA.
EM pboss@san.rr.com; dazhuang.zhou@gmail.com
OI Forsley, Lawrence/0000-0002-0349-3096
FU Defense Threat Reduction Agency (DTRA); JWK Corporation
FX This effort was funded by the Defense Threat Reduction Agency (DTRA),
and JWK Corporation. The authors would like to thank Dr. Gary Phillips,
nuclear physicist, retired from the Naval Research Laboratory, US Navy,
Radiation Effects Branch for valuable discussions in interpreting the
optical data. The authors thank Steve Krivit of New Energy Times for
initiating the SRI replication of the Pd/D co-deposition CR-39 results.
We also thank Dr. Fran Tanzella, of SRI, for conducting the experiments
irradiating CR-39 under the Pd/D co-deposition protocol described in US
Patent 8,419,919. We wish to thank NASA-JSC-SRAG and USRA (Universities
Space Research Association) for the use of research facilities for LENR
data analysis.
NR 68
TC 0
Z9 0
U1 0
U2 0
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0360-3199
EI 1879-3487
J9 INT J HYDROGEN ENERG
JI Int. J. Hydrog. Energy
PD JAN 5
PY 2017
VL 42
IS 1
BP 416
EP 428
DI 10.1016/j.ijhydene.2016.09.223
PG 13
WC Chemistry, Physical; Electrochemistry; Energy & Fuels
SC Chemistry; Electrochemistry; Energy & Fuels
GA EL5AW
UT WOS:000394634900038
ER
PT J
AU Gurgiolo, C
Goldstein, ML
AF Gurgiolo, Chris
Goldstein, Melvyn L.
TI Absence of the strahl during times of slow wind
SO ANNALES GEOPHYSICAE
LA English
DT Article
DE Interplanetary physics (solar wind plasma)
ID ELECTRON-DISTRIBUTION FUNCTIONS; VELOCITY DISTRIBUTION-FUNCTIONS; HELIOS
PLASMA-EXPERIMENT; FAST SOLAR-WIND; CLUSTER MISSION; FIELD; TRANSPORT;
CORONA; HALO; AU
AB It is not uncommon during periods when the solar wind speed is less than 425 km s(-1) to observe near 1 AU no evidence of a strahl population in either the electron solar wind or within the foreshock. Estimating the fluid flow within each energy step returned from the Plasma Electron And Current Experiment (PEACE) on board Cluster-2 often finds that in slow wind the GSE spherical flow angles in energies above where there is a clear core/halo signature are often close to radial with no evidence of a field-aligned flow. This signifies the lack of a strahl presence in the electron velocity distribution function (eVDF). When there is no obvious strahl signature in the data, the electrons above the core/halo in energy appear to be unstructured and smeared in angle. This can either be interpreted as due to statistical noise in low counting rate situations or the result of intense scattering. Regions where the strahl is seen and not seen are often separated by a very thin boundary layer. These transitions in the spacecraft frame of reference can be quite rapid, generally occurring within one to two spins (4-8 s).
C1 [Gurgiolo, Chris] Bitterroot Basic Res, Hamilton, MT 59880 USA.
[Goldstein, Melvyn L.] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Code 672, Greenbelt, MD USA.
RP Gurgiolo, C (reprint author), Bitterroot Basic Res, Hamilton, MT 59880 USA.
EM chris@gurgiolo.com
FU NASA [NNX15AI88G]
FX The authors would like to acknowledge the work and role of the Cluster
Science Archive (CSA) and thank the EFW and FGM teams for providing the
data used in this study. We would also like to acknowledge the PEACE
team at MSSL who worked on and are constantly improving the instrument
calibration. We thank the ACE SWEPAM instrument team and the ACE Science
Center for providing the ACE data. We would like to acknowledge support
from NASA Grant NNX15AI88G.
NR 41
TC 0
Z9 0
U1 0
U2 0
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 0992-7689
EI 1432-0576
J9 ANN GEOPHYS-GERMANY
JI Ann. Geophys.
PD JAN 5
PY 2017
VL 35
IS 1
BP 71
EP 85
DI 10.5194/angeo-35-71-2017
PG 15
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA EI3PV
UT WOS:000392404600002
ER
PT J
AU Crisp, D
Pollock, HR
Rosenberg, R
Chapsky, L
Lee, RAM
Oyafuso, FA
Frankenberg, C
O'Dell, CW
Bruegge, CJ
Doran, GB
Eldering, A
Fisher, BM
Fu, DJ
Gunson, MR
Mandrake, L
Osterman, GB
Schwandner, FM
Sun, K
Taylor, TE
Wennberg, PO
Wunch, D
AF Crisp, David
Pollock, Harold R.
Rosenberg, Robert
Chapsky, Lars
Lee, Richard A. M.
Oyafuso, Fabiano A.
Frankenberg, Christian
O'Dell, Christopher W.
Bruegge, Carol J.
Doran, Gary B.
Eldering, Annmarie
Fisher, Brendan M.
Fu, Dejian
Gunson, Michael R.
Mandrake, Lukas
Osterman, Gregory B.
Schwandner, Florian M.
Sun, Kang
Taylor, Tommy E.
Wennberg, Paul O.
Wunch, Debra
TI The on-orbit performance of the Orbiting Carbon Observatory-2 (OCO-2)
instrument and its radiometrically calibrated products
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID CO2 RETRIEVAL ALGORITHM; VALIDATION; DESIGN; SPACE
AB The Orbiting Carbon Observatory-2 (OCO-2) carries and points a three-channel imaging grating spectrometer designed to collect high-resolution, co-boresighted spectra of reflected sunlight within the molecular oxygen (O-2) A-band at 0.765 microns and the carbon dioxide (CO2) bands at 1.61 and 2.06 microns. These measurements are calibrated and then combined into soundings that are analyzed to retrieve spatially resolved estimates of the column-averaged CO2 dry-air mole fraction, XCO2. Variations of XCO2 in space and time are then analyzed in the context of the atmospheric transport to quantify surface sources and sinks of CO2. This is a particularly challenging remote-sensing observation because all but the largest emission sources and natural absorbers produce only small (< 0.25 %) changes in the background XCO2 field. High measurement precision is therefore essential to resolve these small variations, and high accuracy is needed because small biases in the retrieved XCO2 distribution could be misinterpreted as evidence for CO2 fluxes.
To meet its demanding measurement requirements, each OCO-2 spectrometer channel collects 24 spectra s(-1) across a narrow (< 10 km) swath as the observatory flies over the sunlit hemisphere, yielding almost 1 million soundings each day. On monthly timescales, between 7 and 12% of these soundings pass the cloud screens and other data quality filters to yield full-column estimates of XCO2. Each of these soundings has an unprecedented combination of spatial resolution (< 3 km(2)/sounding), spectral resolving power (lambda /Delta lambda > 17 000), dynamic range (similar to 10(4)), and sensitivity (continuum signal-to-noise ratio > 400).
The OCO-2 instrument performance was extensively characterized and calibrated prior to launch. In general, the instrument has performed as expected during its first 18 months in orbit. However, ongoing calibration and science analysis activities have revealed a number of subtle radiometric and spectroscopic challenges that affect the yield and quality of the OCO-2 data products. These issues include increased numbers of bad pixels, transient artifacts introduced by cosmic rays, radiance discontinuities for spatially non-uniform scenes, a misunderstanding of the instrument polarization orientation, and time-dependent changes in the throughput of the oxygen A-band channel. Here, we describe the OCO-2 instrument, its data products, and its on-orbit performance. We then summarize calibration challenges encountered during its first 18 months in orbit and the methods used to mitigate their impact on the calibrated radiance spectra distributed to the science community.
Copyright statement
The author's copyright for this publication is transferred to the California Institute of Technology.
C1 [Crisp, David; Pollock, Harold R.; Rosenberg, Robert; Chapsky, Lars; Lee, Richard A. M.; Oyafuso, Fabiano A.; Frankenberg, Christian; Bruegge, Carol J.; Doran, Gary B.; Eldering, Annmarie; Fisher, Brendan M.; Fu, Dejian; Gunson, Michael R.; Mandrake, Lukas; Osterman, Gregory B.; Schwandner, Florian M.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Frankenberg, Christian; Taylor, Tommy E.; Wennberg, Paul O.; Wunch, Debra] CALTECH, Pasadena, CA 91125 USA.
[O'Dell, Christopher W.] Colorado State Univ, Ft Collins, CO 80523 USA.
[Schwandner, Florian M.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Sun, Kang] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Wunch, Debra] Univ Toronto, Dept Phys, Toronto, ON, Canada.
RP Crisp, D (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM david.crisp@jpl.nasa.gov
FU National Aeronautics and Space Administration; JPL [1439002]
FX Part of the research described in this paper was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. The
CSU/CIRA contribution to this work was supported by JPL subcontract
1439002. Government sponsorship is acknowledged.
NR 29
TC 2
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U1 8
U2 8
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1867-1381
EI 1867-8548
J9 ATMOS MEAS TECH
JI Atmos. Meas. Tech.
PD JAN 5
PY 2017
VL 10
IS 1
BP 59
EP 81
DI 10.5194/amt-10-59-2017
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EG8BW
UT WOS:000391281700001
ER
PT J
AU D'Incao, JP
Krutzik, M
Elliott, E
Williams, JR
AF D'Incao, J. P.
Krutzik, M.
Elliott, E.
Williams, J. R.
TI Enhanced association and dissociation of heteronuclear Feshbach
molecules in a microgravity environment
SO PHYSICAL REVIEW A
LA English
DT Article
ID BOSE-EINSTEIN CONDENSATION; INTERACTING FERMI GAS; FEW-BODY SYSTEMS;
ULTRACOLD MOLECULES; ATOM-INTERFEROMETER; COOLING ATOMS; SPACE;
RESONANCES
AB We study the association and dissociation dynamics of weakly bound heteronuclear Feshbach molecules using transverse radio-frequency fields for expected parameters accessible through the microgravity environment of NASA's Cold Atom Laboratory (CAL) aboard the International Space Station, including subnanokelvin temperatures and atomic densities as low as 108/cm(3). We show that under such conditions, thermal and loss effects can be greatly suppressed, resulting in a high efficiency of both association and dissociation of Feshbach molecules with a mean size exceeding 10(4)a(0) and allowing for the coherence in atom-molecule transitions to be clearly observable. Our theoretical model for heteronuclear mixtures includes thermal, loss, and density effects in a simple and conceptually clear manner. We derive the temperature, density, and scattering length regimes of K-41-Rb-87 that allow optimal association or dissociation efficiency with minimal heating and loss to guide upcoming experiments with ultracold atomic gases in space.
C1 [D'Incao, J. P.] Univ Colorado, JILA, Boulder, CO 80309 USA.
[D'Incao, J. P.] NIST, 440 UCB, Boulder, CO 80309 USA.
[D'Incao, J. P.] Univ Colorado, Dept Phys, Boulder, CO 80302 USA.
[Krutzik, M.] Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany.
[Krutzik, M.; Elliott, E.; Williams, J. R.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91011 USA.
RP D'Incao, JP (reprint author), Univ Colorado, JILA, Boulder, CO 80309 USA.; D'Incao, JP (reprint author), NIST, 440 UCB, Boulder, CO 80309 USA.; D'Incao, JP (reprint author), Univ Colorado, Dept Phys, Boulder, CO 80302 USA.
FU German space agency; Federal Ministry of Economics and Technology
[50WP1432, 50WM1132, 1237]; U.S. National Science Foundation
[PHY-1307380]
FX This research was carried out under a contract with the National
Aeronautics and Space Administration. M.K. acknowledges support by the
German space agency with funds provided by the Federal Ministry of
Economics and Technology under Grants No. 50WP1432, No. 50WM1132, and
No. 1237. J.P.D. also acknowledges partial support from U.S. National
Science Foundation Grant No. PHY-1307380.
NR 97
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U1 2
U2 2
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-9926
EI 2469-9934
J9 PHYS REV A
JI Phys. Rev. A
PD JAN 3
PY 2017
VL 95
IS 1
AR 012701
DI 10.1103/PhysRevA.95.012701
PG 10
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA EG8JU
UT WOS:000391303800007
ER
PT J
AU Pahlevan, N
Sarkar, S
Devadiga, S
Wolfe, RE
Roman, M
Vermote, E
Lin, GQ
Xiong, XX
AF Pahlevan, Nima
Sarkar, Sudipta
Devadiga, Sadashiva
Wolfe, Robert E.
Roman, Miguel
Vermote, Eric
Lin, Guoqing
Xiong, Xiaoxiong
TI Impact of Spatial Sampling on Continuity of MODIS-VIIRS Land Surface
Reflectance Products: A Simulation Approach
SO IEEE GEOSCIENCE AND REMOTE SENSING MAGAZINE
LA English
DT Article
DE Biosphere; consistency; geometry; land surface; spatial resolution
ID DIFFERENCE VEGETATION INDEX; RESOLUTION; PERFORMANCE; VALIDATION;
SATELLITE; SCIENCE; SENSORS; COVER
AB With the increasing need to construct long-term climate-quality data records to understand, monitor, and predict climate variability and change, it is vital to continue systematic satellite measurements along with the development of new technology for more quantitative and accurate observations. The Suomi National Polar-orbiting Partnership mission provides continuity in monitoring the Earth's surface and its atmosphere in a similar fashion as the heritage MODIS instruments onboard the National Aeronautics and Space Administration's Terra and Aqua satellites. In this paper, we aim at quantifying the consistency of Aqua MODIS and Suomi-NPP Visible Infrared Imaging Radiometer Suite (VIIRS) Land Surface Reflectance (LSR) and NDVI products as related to their inherent spatial sampling characteristics. To avoid interferences from sources of measurement and/or processing errors other than spatial sampling, including calibration, atmospheric correction, and the effects of the bidirectional reflectance distribution function, the MODIS and VIIRS LSR products were simulated using the Landsat-8's Operational Land Imager (OLI) LSR products. The simulations were performed using the instruments' point spread functions on a daily basis for various OLI scenes over a 16-day orbit cycle. It was found that the daily mean differences due to discrepancies in spatial sampling remain below 0.0015 (1%) in absolute surface reflectance at subgranule scale (i.e., OLI scene size). We also found that the MODIS-VIIRS product intercomparisons appear to be minimally impacted when differences in the corresponding view zenith angles (VZAs) are within the range of -15. to -35. (VZA(V) - VZA(M)), where VIIRS and MODIS footprints resemble in size. In general, depending on the spatial heterogeneity of the OLI scene contents, per-grid-cell differences can reach up to 20%. Further spatial analysis of the simulated NDVI and LSR products revealed that, depending on the user accuracy requirements for product intercomparisons, spatial aggregations may be used. It was found that if per-grid-cell differences on the order of 10% (in LSR or NDVI) are tolerated, the product intercomparisons are expected to be immune from differences in spatial sampling.
C1 [Pahlevan, Nima; Sarkar, Sudipta; Devadiga, Sadashiva; Wolfe, Robert E.; Roman, Miguel; Lin, Guoqing; Xiong, Xiaoxiong] Natl Aero & Space Adm, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Pahlevan, Nima; Sarkar, Sudipta; Devadiga, Sadashiva; Lin, Guoqing] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
RP Pahlevan, N (reprint author), Natl Aero & Space Adm, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Pahlevan, N (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
EM nima.pahlevan@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2168-6831
J9 IEEE GEOSC REM SEN M
JI IEEE Geosci. Remote Sens. Mag.
PD JAN
PY 2017
VL 55
IS 1
BP 183
EP 196
DI 10.1109/TGRS.2016.2604214
PG 14
WC Geochemistry & Geophysics; Remote Sensing; Imaging Science &
Photographic Technology
SC Geochemistry & Geophysics; Remote Sensing; Imaging Science &
Photographic Technology
GA EP3IQ
UT WOS:000397276400015
ER
PT B
AU Morgan, MA
AF Morgan, Matthew A.
BA Morgan, MA
BF Morgan, MA
TI Passive Microwave Networks
SO REFLECTIONLESS FILTERS
SE Artech House Microwave Library
LA English
DT Article; Book Chapter
C1 [Morgan, Matthew A.] Lockheed Martin Fed Syst, Manassas, VA 20110 USA.
[Morgan, Matthew A.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Morgan, Matthew A.] Natl Radio Astron Observ, Cent Dev Lab, Charlottesville, VA 22903 USA.
[Morgan, Matthew A.] Green Bank Telescope, K Band Focal Plane Array Dev Project, Green Bank, WV 24944 USA.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band GHz Cryogen IF Amplifier Prod 6 211 275, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band Receiver Cartridge Testing 6, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band GHz 3 84 116, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band Orthomode Transducer OMT Prod 6, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] CDL, Integrated Receiver Dev Program, Charlottesville, VA 22903 USA.
RP Morgan, MA (reprint author), Lockheed Martin Fed Syst, Manassas, VA 20110 USA.; Morgan, MA (reprint author), NASA, Jet Prop Lab, Pasadena, CA 91109 USA.; Morgan, MA (reprint author), Natl Radio Astron Observ, Cent Dev Lab, Charlottesville, VA 22903 USA.; Morgan, MA (reprint author), Green Bank Telescope, K Band Focal Plane Array Dev Project, Green Bank, WV 24944 USA.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band GHz Cryogen IF Amplifier Prod 6 211 275, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band Receiver Cartridge Testing 6, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band GHz 3 84 116, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band Orthomode Transducer OMT Prod 6, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), CDL, Integrated Receiver Dev Program, Charlottesville, VA 22903 USA.
NR 13
TC 0
Z9 0
U1 0
U2 0
PU ARTECH HOUSE
PI NORWOOD
PA 685 CANTON ST, NORWOOD, MA 02062 USA
BN 978-1-63081-327-7
J9 ARTECH HSE MICROW LI
PY 2017
BP 1
EP 34
PG 34
WC Engineering, Electrical & Electronic; Physics, Applied;
Telecommunications
SC Engineering; Physics; Telecommunications
GA BH0XR
UT WOS:000396947600001
ER
PT J
AU Kim, KS
Kim, MJ
Park, C
Fay, CC
Chu, SH
Kingston, CT
Simard, B
AF Kim, Keun Su
Kim, Myung Jong
Park, Cheol
Fay, Catharine C.
Chu, Sang-Hyon
Kingston, Christopher T.
Simard, Benoit
TI Scalable manufacturing of boron nitride nanotubes and their assemblies:
a review
SO SEMICONDUCTOR SCIENCE AND TECHNOLOGY
LA English
DT Review
DE boron nitride nanotubes; macroscopic assemblies of boron nitride
nanotubes; scalable manufacturing
ID CHEMICAL-VAPOR-DEPOSITION; WALLED CARBON NANOTUBES; INDUCTION THERMAL
PLASMA; LASER VAPORIZATION; SCALE PRODUCTION; BN NANOTUBES; GROWTH;
CHEMISTRY; PRECURSOR; CATALYST
AB Boron nitride nanotubes (BNNTs) are wide bandgap semiconducting materials with a quasiparticle energy gap larger than 6.0 eV. Since their first synthesis in 1995, there have been considerable attempts to develop novel BNNT-based applications in semiconductor science and technology. Inspired by carbon nanotube synthesis methods, many BNNT synthesis methods have been developed so far; however, it has been very challenging to produce BNNTs at a large scale with the structural quality high enough for exploring practical applications. Very recently there has been significant progress in the scalable manufacturing of high-quality BNNTs. In this article, we will review those particular breakthroughs and discuss their impact on semiconductor industries. Freestanding BNNT assemblies such as transparent thin films, yarns or buckypapers are highly advantageous in the development of novel BNNT-based semiconductor devices. The latest achievements in their manufacturing processes will be also presented along with their potential applications.
C1 [Kim, Keun Su; Kingston, Christopher T.; Simard, Benoit] Natl Res Council Canada, Secur & Disrupt Technol Portfolio, Emerging Technol Div, Ottawa, ON K1A 0R6, Canada.
[Kim, Myung Jong] Korea Inst Sci & Technol, Appl Quantum Composites Res Ctr, Wonju 55324, South Korea.
[Park, Cheol; Fay, Catharine C.] NASA, Adv Mat & Proc Branch, Langley Res Ctr, Hampton, VA 23681 USA.
[Chu, Sang-Hyon] Natl Inst Aerosp, Hampton, VA 23666 USA.
RP Kim, KS (reprint author), Natl Res Council Canada, Secur & Disrupt Technol Portfolio, Emerging Technol Div, Ottawa, ON K1A 0R6, Canada.
EM KeunSu.Kim@nrc-cnrc.gc.ca
FU NRC-Security Materials Technology Program; Korea Institute of Science
and Technology (KIST) institutional program
FX KSK, CTK, and BS are grateful for the support from the NRC-Security
Materials Technology Program. MJK acknowledges this work was supported
by a grant from Korea Institute of Science and Technology (KIST)
institutional program.
NR 98
TC 0
Z9 0
U1 3
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0268-1242
EI 1361-6641
J9 SEMICOND SCI TECH
JI Semicond. Sci. Technol.
PD JAN
PY 2017
VL 32
IS 1
AR 013003
DI 10.1088/0268-1242/32/1/013003
PG 18
WC Engineering, Electrical & Electronic; Materials Science,
Multidisciplinary; Physics, Condensed Matter
SC Engineering; Materials Science; Physics
GA EO2UF
UT WOS:000396550800001
ER
PT J
AU Hofmann, DC
Andersen, LM
Kolodziejska, J
Roberts, SN
Borgonia, JP
Johnson, WL
Vecchio, KS
Kennett, A
AF Hofmann, Douglas C.
Andersen, Laura M.
Kolodziejska, Joanna
Roberts, Scott N.
Borgonia, John-Paul
Johnson, William L.
Vecchio, Kenneth S.
Kennett, Andrew
TI Optimizing Bulk Metallic Glasses for Robust, Highly Wear-Resistant Gears
SO ADVANCED ENGINEERING MATERIALS
LA English
DT Article
ID AMORPHOUS-ALLOYS; THERMAL-STABILITY; CU-ZR; PLASTICITY; BEHAVIOR;
COMPOSITES; TOUGHNESS; CRYSTALLIZATION; DUCTILITY
AB Despite their promising mechanical properties and ability to be manufactured like plastics, bulk metallic glasses ( BMGs) are slow to emerge as a structural engineering material. Because BMGs properties are highly correlated with processing, it is necessary to test them in a relevant engineering application. In the current work, CuZr-based BMGs are developed with excellent wear performance when used as gears. It is shown that in order to optimize the wear performance of these gears, toughness should be maximized. This contrasts the conventional design strategy, where wear performance increases with increasing hardness. Finally, a new low-cost manufacturing method for casting net- shaped macroscale gears is developed.
C1 [Hofmann, Douglas C.; Kolodziejska, Joanna; Roberts, Scott N.; Borgonia, John-Paul; Vecchio, Kenneth S.] CALTECH, Jet Prop Lab, Mat Dev & Mfg Technol Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Hofmann, Douglas C.; Kolodziejska, Joanna; Roberts, Scott N.] CALTECH, Keck Lab Engn Sci, 1200 E. Calif Blvd, Pasadena, CA 91125 USA.
[Andersen, Laura M.; Vecchio, Kenneth S.] Univ Calif San Diego, Dept NanoEngn, 9500 Gilman Dr, La Jolla, CA 92093 USA.
RP Hofmann, DC (reprint author), CALTECH, Jet Prop Lab, Mat Dev & Mfg Technol Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.; Hofmann, DC (reprint author), CALTECH, Keck Lab Engn Sci, 1200 E. Calif Blvd, Pasadena, CA 91125 USA.
EM dch@jpl.nasa.gov
FU NASA's Science Mission Directorate and Space Technology Mission
Directorate through the Game Changing Development program [NAS7-03001];
NASA's Center Innovation Funds; Presidential Early Career Award;
Achievement Rewards for College Scientists ( ARCS) Foundation; Jet
Propulsion Laboratory Summer Internship Program
FX The JPL authors acknowledge financial support from NASA's Science
Mission Directorate and Space Technology Mission Directorate through the
Game Changing Development program under Prime Contract #NAS7-03001 and
from NASA's Center Innovation Funds. D. C. Hofmann also acknowledges
support from the Presidential Early Career Award. Part of this research
was done at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with NASA. L. M. Andersen acknowledges
financial support from the Achievement Rewards for College Scientists (
ARCS) Foundation and the Jet Propulsion Laboratory Summer Internship
Program. The authors would like to thank Nicolo Valigi for his
invaluable contributions in performing hardness and elastic constant
measurements and running gear-on-gear testing. The authors acknowledge
useful discussions with K. Boykins, B. Wilcox, D. Bickler, G. Davis, and
M. Knopp. Patents related to the current technology have been filed with
the California Institute of Technology.
NR 43
TC 0
Z9 0
U1 0
U2 0
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA POSTFACH 101161, 69451 WEINHEIM, GERMANY
SN 1438-1656
EI 1527-2648
J9 ADV ENG MATER
JI Adv. Eng. Mater.
PD JAN
PY 2017
VL 19
IS 1
AR UNSP 1600541
DI 10.1002/adem.201600541
PG 10
WC Materials Science, Multidisciplinary
SC Materials Science
GA EO2VZ
UT WOS:000396555400014
ER
PT S
AU Beran, P
Stanford, B
Schrock, C
AF Beran, Philip
Stanford, Bret
Schrock, Christopher
BE Davis, SH
Moin, P
TI Uncertainty Quantification in Aeroelasticity
SO ANNUAL REVIEW OF FLUID MECHANICS, VOL 49
SE Annual Review of Fluid Mechanics
LA English
DT Review; Book Chapter
DE uncertainty quantification; aeroelasticity; polynomial chaos; flutter;
limit-cycle oscillation; reliability; design under uncertainty
ID LIMIT-CYCLE OSCILLATIONS; RELIABILITY-BASED DESIGN; COMPUTATIONAL
FLUID-DYNAMICS; POLYNOMIAL CHAOS; NONLINEAR AEROELASTICITY; STOCHASTIC
PROJECTION; BIFURCATION BEHAVIOR; FLUTTER; OPTIMIZATION; AIRFOIL
AB Physical interactions between a fluid and structure, potentially manifested as self-sustained or divergent oscillations, can be sensitive to many parameters whose values are uncertain. Of interest here are aircraft aeroelastic interactions, which must be accounted for in aircraft certification and design. Deterministic prediction of these aeroelastic behaviors can be difficult owing to physical and computational complexity. New challenges are introduced when physical parameters and elements of the modeling process are uncertain. By viewing aeroelasticity through a nondeterministic prism, where key quantities are assumed stochastic, one may gain insights into how to reduce system uncertainty, increase system robustness, and maintain aeroelastic safety. This article reviews uncertainty quantification in aeroelasticity using traditional analytical techniques not reliant on computational fluid dynamics; compares and contrasts this work with emerging methods based on computational fluid dynamics, which target richer physics; and reviews the state of the art in aeroelastic optimization under uncertainty. Barriers to continued progress, for example, the so-called curse of dimensionality, are discussed.
C1 [Beran, Philip] Air Force Res Lab, Multidisciplinary Sci & Technol Ctr, Wright Patterson AFB, OH 45433 USA.
[Stanford, Bret] NASA, Langley Res Ctr, Aeroelast Branch, Hampton, VA 23681 USA.
[Schrock, Christopher] Air Force Res Lab, Computat Sci Ctr, Wright Patterson AFB, OH 45433 USA.
RP Beran, P (reprint author), Air Force Res Lab, Multidisciplinary Sci & Technol Ctr, Wright Patterson AFB, OH 45433 USA.
EM philip.beran@us.af.mil; bret.k.stanford@nasa.gov;
christopher.schrock@us.af.mil
NR 106
TC 0
Z9 0
U1 0
U2 0
PU ANNUAL REVIEWS
PI PALO ALTO
PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0897 USA
SN 0066-4189
BN 978-0-8243-0749-3
J9 ANNU REV FLUID MECH
JI Annu. Rev. Fluid Mech.
PY 2017
VL 49
BP 361
EP 386
DI 10.1146/annurev-fluid-122414-034441
PG 26
WC Mechanics; Physics, Fluids & Plasmas
SC Mechanics; Physics
GA BH0QM
UT WOS:000396042600015
ER
PT J
AU Luo, B
Brandt, WN
Xue, YQ
Lehmer, B
Alexander, DM
Bauer, FE
Vito, F
Yang, G
Basu-Zych, AR
Comastri, A
Gilli, R
Gu, QS
Hornschemeier, AE
Koekemoer, A
Liu, T
Mainieri, V
Paolillo, M
Ranalli, P
Rosati, P
Schneider, DP
Shemmer, O
Smail, I
Sun, M
Tozzi, P
Vignali, C
Wang, JX
AF Luo, B.
Brandt, W. N.
Xue, Y. Q.
Lehmer, B.
Alexander, D. M.
Bauer, F. E.
Vito, F.
Yang, G.
Basu-Zych, A. R.
Comastri, A.
Gilli, R.
Gu, Q. -S.
Hornschemeier, A. E.
Koekemoer, A.
Liu, T.
Mainieri, V.
Paolillo, M.
Ranalli, P.
Rosati, P.
Schneider, D. P.
Shemmer, O.
Smail, I.
Sun, M.
Tozzi, P.
Vignali, C.
Wang, J. -X.
TI THE CHANDRA DEEP FIELD-SOUTH SURVEY: 7 MS SOURCE CATALOGS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; cosmology: observations; diffuse radiation; galaxies: active;
surveys; X-rays: galaxies
ID X-RAY SOURCES; POINT-SOURCE CATALOGS; CCD IMAGING SPECTROMETER; ACTIVE
GALACTIC NUCLEI; STAR-FORMING GALAXIES; CHARGE-TRANSFER INEFFICIENCY;
EXTRAGALACTIC LEGACY SURVEY; NUMBER COUNTS; GOODS-SOUTH; OPTICAL
SPECTROSCOPY
AB We present X-ray source catalogs for the approximate to 7 Ms exposure of the Chandra Deep Field-South (CDF-S), which covers a total area of 484.2. arcmin(2). Utilizing WAVDETECT for initial source detection and ACIS Extract for photometric extraction and significance assessment, we create a main source catalog containing 1008 sources that are detected in up to three X-ray bands: 0.5-7.0. keV, 0.5-2.0. keV, and 2-7. keV. A supplementary source catalog is also provided,. including 47 lower-significance sources that have bright (K-s <= 23) near-infrared counterparts. We identify multiwavelength counterparts for 992 (98.4%) of the main-catalog sources, and we collect redshifts for 986 of these sources, including 653 spectroscopic redshifts and 333 photometric redshifts. Based on the X-ray and multiwavelength properties, we identify 711 active galactic nuclei (AGNs) from the main-catalog sources. Compared to the previous approximate to 4 Ms CDF-S catalogs, 291 of the main-catalog sources are new detections. We have achieved unprecedented X-ray sensitivity with average flux limits over the central approximate to 1 arcmin(2) region of approximate to 1.9. x. 10(-17), 6.4 x 10(-18), and 2.7 x 10(-17) erg cm(-2) s(-1) in the three X-ray bands, respectively. We provide cumulative number-count measurements observing, for the first time, that normal galaxies start to dominate the X-ray source population at the faintest 0.5-2.0. keV flux levels. The highest X-ray source density reaches approximate to 50,500 deg(-2), and 47% +/- 4% of these sources are AGNs (approximate to 23,900 deg(-2)).
C1 [Luo, B.; Gu, Q. -S.] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China.
[Luo, B.; Gu, Q. -S.] Nanjing Univ, Key Lab Modern Astron & Astrophys, Nanjing 210093, Jiangsu, Peoples R China.
[Luo, B.; Gu, Q. -S.] Collaborat Innovat Ctr Modern Astron & Space Expl, Nanjing 210093, Jiangsu, Peoples R China.
[Luo, B.; Brandt, W. N.; Vito, F.; Yang, G.; Schneider, D. P.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
[Brandt, W. N.; Vito, F.; Yang, G.; Schneider, D. P.; Wang, J. -X.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Brandt, W. N.] Penn State Univ, Dept Phys, 104 Davey Lab, University Pk, PA 16802 USA.
[Xue, Y. Q.; Liu, T.; Sun, M.; Wang, J. -X.] Univ Sci & Technol China, Dept Astron, CAS Key Lab Res Galaxies & Cosmol, Hefei 230026, Peoples R China.
[Lehmer, B.] Univ Arkansas, Dept Phys, 226 Phys Bldg,835 W Dickson St, Fayetteville, AR 72701 USA.
[Alexander, D. M.; Smail, I.] Univ Durham, Ctr Extragalact Astron, Dept Phys, Durham DH1 3LE, England.
[Bauer, F. E.] Pontificia Univ Catolica Chile, Fac Fis, Casilla 6177, Santiago 22, Chile.
[Bauer, F. E.] Millennium Inst Astrophys, Nuncio Monsenor Soero Sanz 100, Santiago, Chile.
[Bauer, F. E.] Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA.
[Basu-Zych, A. R.; Hornschemeier, A. E.] NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA.
[Basu-Zych, A. R.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Comastri, A.; Gilli, R.; Vignali, C.] INAF Osserv Astronom Bologna, Via Ranzani 1, I-40127 Bologna, Italy.
[Koekemoer, A.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Mainieri, V.] European Sourthern Observ, Karl Schwarzschild Str 2, D-85748 Munich, Germany.
[Paolillo, M.] Univ Naples Federico II, Dip Fis Ettore Pancini, Federico II,C Monte S, I-80126 Naples, Italy.
[Paolillo, M.] INFN Sez Napoli, I-80126 Naples, Italy.
[Paolillo, M.] Agenzia Spaziale Italiana Sci Data Ctr, Via Politecn snc, I-00133 Rome, Italy.
[Rosati, P.] Lund Univ, Lund Observ Dept Astron & Theoret Phys, Box 43, SE-22100 Lund, Sweden.
[Rosati, P.] Univ Ferrara, Dipartimento Fis & Sci Terra, Via Saragat 1, I-44122 Ferrara, Italy.
[Shemmer, O.] Univ North Texas, Dept Phys, Denton, TX 76203 USA.
[Tozzi, P.] INAF Osserv Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy.
[Vignali, C.] Univ Bologna, Dipartimento Fis & Atron, Viale Berti Pichat 6-2, I-40127 Bologna, Italy.
RP Luo, B (reprint author), Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China.; Luo, B (reprint author), Nanjing Univ, Key Lab Modern Astron & Astrophys, Nanjing 210093, Jiangsu, Peoples R China.; Luo, B (reprint author), Collaborat Innovat Ctr Modern Astron & Space Expl, Nanjing 210093, Jiangsu, Peoples R China.; Luo, B (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
OI Paolillo, Maurizio/0000-0003-4210-7693; Luo, Bin/0000-0002-9036-0063;
Comastri, Andrea/0000-0003-3451-9970; Koekemoer,
Anton/0000-0002-6610-2048
FU National Thousand Young Talents program of China; National Natural
Science Foundation of China [11673010]; Ministry of Science and
Technology of China [2016YFA0400702]; CXC [GO4-15130A]; 973 Program
[2015CB857004, 2015CB857005]; Strategic Priority Research Program of CAS
[XDB09000000]; Fundamental Research Funds for the Central Universities;
CAS Frontier Science Key Research Program [QYZDJ-SSW-SLH006]; STFC
[ST/L00075X/1]; CONICYT-Chile [Basal-CATA PFB-06/2007]; FONDECYT
[1141218]; "EMBIGGEN" Anillo [ACT1101]; Ministry of Economy,
Development, and Tourism's Millennium Science Initiative [IC120009]; ERC
[DUSTYGAL 321334]; Royal Society/Wolfson Merit Award; [NSFC-11473026];
[NSFC-11421303]
FX We acknowledge financial support from the National Thousand Young
Talents program of China (B.L., Y.Q.X.), National Natural Science
Foundation of China grant 11673010 (B.L.), Ministry of Science and
Technology of China grant 2016YFA0400702 (B.L.), CXC grant GO4-15130A
(B.L., W.N.B., F.V., G.Y.), 973 Program 2015CB857004 (Y.Q.X., M.S.) and
2015CB857005 (J.X.W.), NSFC-11473026 (Y.Q.X., M.S.), NSFC-11421303
(Y.Q.X., M.S., J.X.W.), Strategic Priority Research Program of CAS grant
XDB09000000 (Y.Q.X., M.S., J.X.W.), Fundamental Research Funds for the
Central Universities (Y.Q.X., M.S.), CAS Frontier Science Key Research
Program QYZDJ-SSW-SLH006 (Y.Q.X., M.S., J.X.W.), STFC grant ST/L00075X/1
(D.M.A., I.S.), CONICYT-Chile grants Basal-CATA PFB-06/2007 (F.E.B.),
FONDECYT Regular 1141218 (F.E.B.), "EMBIGGEN" Anillo ACT1101 (F.E.B.),
the Ministry of Economy, Development, and Tourism's Millennium Science
Initiative through grant IC120009, awarded to the Millennium Institute
of Astrophysics, MAS (F.E.B.), ERC Advanced grant DUSTYGAL 321334
(I.S.), and the Royal Society/Wolfson Merit Award (I.S.).
NR 108
TC 0
Z9 0
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD JAN
PY 2017
VL 228
IS 1
AR 2
DI 10.3847/1538-4365/228/1/2
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EP3VN
UT WOS:000397309900002
ER
PT J
AU Nayyeri, H
Hemmati, S
Mobasher, B
Ferguson, HC
Cooray, A
Barro, G
Faber, SM
Dickinson, M
Koekemoer, AM
Peth, M
Salvato, M
Ashby, MLN
Darvish, B
Donley, J
Durbin, M
Finkelstein, S
Fontana, A
Grogin, NA
Gruetzbauch, R
Huang, K
Khostovan, AA
Kocevski, D
Kodra, D
Lee, B
Newman, J
Pacifici, C
Pforr, J
Stefanon, M
Wiklind, T
Willner, SP
Wuyts, S
Castellano, M
Conselice, C
Dolch, T
Dunlop, JS
Galametz, A
Hathi, NP
Lucas, RA
Yan, H
AF Nayyeri, H.
Hemmati, S.
Mobasher, B.
Ferguson, H. C.
Cooray, A.
Barro, G.
Faber, S. M.
Dickinson, M.
Koekemoer, A. M.
Peth, M.
Salvato, M.
Ashby, M. L. N.
Darvish, B.
Donley, J.
Durbin, M.
Finkelstein, S.
Fontana, A.
Grogin, N. A.
Gruetzbauch, R.
Huang, K.
Khostovan, A. A.
Kocevski, D.
Kodra, D.
Lee, B.
Newman, J.
Pacifici, C.
Pforr, J.
Stefanon, M.
Wiklind, T.
Willner, S. P.
Wuyts, S.
Castellano, M.
Conselice, C.
Dolch, T.
Dunlop, J. S.
Galametz, A.
Hathi, N. P.
Lucas, R. A.
Yan, H.
TI CANDELS MULTI-WAVELENGTH CATALOGS: SOURCE IDENTIFICATION AND PHOTOMETRY
IN THE CANDELS COSMOS SURVEY FIELD
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; galaxies: high-redshift; galaxies: photometry; methods: data
analysis; techniques: image processing
ID ACTIVE GALACTIC NUCLEI; SIMILAR-TO 2; LYMAN-BREAK GALAXIES;
HIGH-REDSHIFT GALAXIES; STAR-FORMING GALAXIES; ULTRA-DEEP-FIELD;
ULTRAVIOLET LUMINOSITY DENSITY; SPECTRAL ENERGY-DISTRIBUTIONS;
EXTRAGALACTIC LEGACY SURVEY; SPITZER-SPACE-TELESCOPE
AB We present a multi-wavelength photometric catalog in the COSMOS field as part of the observations by the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey. The catalog is based on Hubble Space Telescope Wide Field Camera 3 (HST/WFC3) and Advanced Camera for Surveys observations of the COSMOS field (centered at R. A.: 10(h)00(m)28(s), Decl.: + 02 degrees 12'21 ''). The final catalog has 38671 sources with photometric data in 42 bands from UV to the infrared (similar to 0.3-8 mu m). This includes broadband photometry from HST, CFHT, Subaru, the Visible and Infrared Survey Telescope for Astronomy, and Spitzer Space Telescope in the visible, near-infrared, and infrared bands along with intermediate-and narrowband photometry from Subaru and medium-band data from Mayall NEWFIRM. Source detection was conducted in the WFC3 F160W band (at 1.6 mu m) and photometry is generated using the Template FITting algorithm. We further present a catalog of the physical properties of sources as identified in the HST F160W band and measured from the multi-band photometry by fitting the observed spectral energy distributions of sources against templates.
C1 [Nayyeri, H.; Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Nayyeri, H.; Hemmati, S.; Mobasher, B.; Darvish, B.; Khostovan, A. A.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[Hemmati, S.] CALTECH, Infrared Proc & Anal Ctr, MS 100-22, Pasadena, CA 91125 USA.
[Ferguson, H. C.; Koekemoer, A. M.; Lucas, R. A.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Barro, G.; Faber, S. M.] Univ Calif Santa Cruz, UCO Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Barro, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Dickinson, M.] Natl Optic Astron Observ, Tucson, AZ 85719 USA.
[Peth, M.] Johns Hopkins Univ, Dept Phys & Astron, 366 Bloomberg Ctr, Baltimore, MD 21218 USA.
[Salvato, M.; Galametz, A.] Max Planck Inst Extraterr Phys, Giessenbachstrasse 1, D-85748 Munich, Germany.
[Ashby, M. L. N.; Willner, S. P.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Darvish, B.] CALTECH, Cahill Ctr Astrophys, 1216 E Calif Blvd, Pasadena, CA 91125 USA.
[Donley, J.] Los Alamos Natl Lab, Los Alamos, NM 87544 USA.
[Finkelstein, S.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Fontana, A.; Castellano, M.] INAF Osservat Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, Italy.
[Gruetzbauch, R.] Obser Astron Lisboa, Ctr Astron & Astrophys, PL-1349018 Lisbon, Portugal.
[Huang, K.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Kocevski, D.] Colby Coll, 4000 Mayflower Hill, Waterville, ME 04901 USA.
[Kodra, D.; Newman, J.] Univ Pittsburgh, Dept Phys & Astron & PITT PACC, Pittsburgh, PA 15260 USA.
[Lee, B.] Univ Massachusetts, Dept Astron, 710 N Plesant St, Amherst, MA 01003 USA.
[Pacifici, C.] Goddard Space Flight Ctr, Code 665, Greenbelt, MD USA.
[Pforr, J.; Hathi, N. P.] Aix Marseille Univ, CNRS LAM, UMR 7326, F-13388 Marseille, France.
[Pforr, J.] ESA ESTEC SCI S, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands.
[Stefanon, M.] Huygens Lab Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands.
[Wiklind, T.] Cathol Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Wuyts, S.] Univ Bath, Dept Phys, Claverton Down, Bath BA1 1RL, Avon, England.
[Conselice, C.] Univ Nottingham, Sch Phys & Astron, Nottingham, England.
[Dolch, T.] Hillsdale Coll, Dept Phys, 33 E Coll St, Hillsdale, MI 49242 USA.
[Dunlop, J. S.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Yan, H.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA.
OI Hathi, Nimish/0000-0001-6145-5090; Koekemoer, Anton/0000-0002-6610-2048;
Ferguson, Henry/0000-0001-7113-2738
FU NASA [NAS5-26555, NNX16AF39G]; NSF [AST-1313319]; ESO programme
[179.A-2005]
FX We wish to thank the anonymous referee for carefully reading the
original manuscript and providing very useful suggestions. We also thank
S. Fleming for his help with the MAST archive. This work is based on
observations taken by the CANDELS Multi-Cycle Treasury Program with the
NASA/ESA HST, which is operated by the Association of Universities for
Research in Astronomy, Inc., under NASA contract NAS5-26555. This work
is based in part on observations made with the Spitzer Space Telescope,
which is operated by the Jet Propulsion Laboratory, California Institute
of Technology under a contract with NASA. Financial support for this
work was provided by NSF through AST-1313319 for H.N. and A.C. H.N.
further acknowledges support from NASA (grant No. NNX16AF39G). This work
is based in part on data products from observations made with ESO
Telescopes at the La Silla Paranal Observatories under ESO programme ID
179.A-2005 and on data products produced by TER-APIX and the Cambridge
Astronomy survey Unit on behalf of the UltraVISTA consortium. This study
was based in part on observations obtained with MegaPrime/MegaCam, a
joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii
Telescope (CFHT), which is operated by the National Research Council
(NRC) of Canada, the Institut National des Science de l'Univers of the
Centre National de la Recherche Scienti que (CNRS) of France, and the
University of Hawaii. This work is based in part on data products
produced at TERAPIX and the Canadian Astronomy Data Centre as part of
the Canada-France-Hawaii Telescope Legacy Survey, a collaborative
project of NRC and CNRS.
NR 174
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U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD JAN
PY 2017
VL 228
IS 1
AR 7
DI 10.3847/1538-4365/228/1/7
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EP3VQ
UT WOS:000397310200002
ER
PT J
AU Norris, TA
Littnan, CL
Gulland, FMD
Baker, JD
Harvey, JT
AF Norris, Tenaya A.
Littnan, Charles L.
Gulland, Frances M. D.
Baker, Jason D.
Harvey, James T.
TI An integrated approach for assessing translocation as an effective
conservation tool for Hawaiian monk seals
SO ENDANGERED SPECIES RESEARCH
LA English
DT Article
DE Translocation; Post-release monitoring; Health assessment; Foraging
conditions; First-year survival; Hawaiian monk seal
ID SOUTHERN ELEPHANT SEALS; MONACHUS-SCHAUINSLANDI; DIVE DURATION;
CALLORHINUS-URSINUS; FORAGING HABITAT; MIROUNGA-LEONINA; BODY-SIZE;
SURVIVAL; ISLANDS; WILDLIFE
AB For threatened and endangered species, translocations have been widely used to mitigate multiple sources of mortality that threaten population recovery. Although numerous Hawaiian monk seals Neomonachus schauinslandi have been translocated for a variety of purposes, few monk seal translocations have addressed the problem of prey limitation. To assess the efficacy of using translocations to mitigate reduced prey availability, 12 weanling monk seals were translocated with pre-release health screening and post-release monitoring. Specifically, the health, foraging behavior, habitat use, and survival of translocated seals were compared with those of 17 monk seals resident to the release site. There was little evidence of infectious diseases in translocated and resident seals, although Chlamydophila abortus antibodies and enteric bacteria were detected in many individuals. Translocated and resident weanling seals also demonstrated similar diving, movements, and habitat use, whereas resident adult seals had greater variability in foraging patterns. First-year survival for translocated weanlings (50%, n = 12) and non-translocated weanlings at the donor (31%, n = 36) and recipient sites (69%, n = 16) was related to weaning body size, with larger individuals having greater survivorship. These results supported 3 main conclusions that have important consequences for future translocation and population recovery efforts: (1) there was minimal risk of exposing seals to novel infectious diseases as a result of translocation; (2) individuals translocated with limited foraging experience rapidly adapted to their post-release environment; and (3) translocation for the purpose of mitigating prey limitation is a viable and important conservation tool for Hawaiian monk seals.
C1 [Norris, Tenaya A.; Gulland, Frances M. D.] Marine Mammal Ctr, Sausalito, CA 94965 USA.
[Norris, Tenaya A.; Harvey, James T.] Moss Landing Marine Labs, Moss Landing, CA 95039 USA.
[Littnan, Charles L.; Baker, Jason D.] NOAA, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, Honolulu, HI 96818 USA.
RP Norris, TA (reprint author), Marine Mammal Ctr, Sausalito, CA 94965 USA.; Norris, TA (reprint author), Moss Landing Marine Labs, Moss Landing, CA 95039 USA.
EM norrist@tmmc.org
FU National Marine Fisheries Service; Marine Mammal Center
FX Funding for this study was provided by National Marine Fisheries Service
and The Marine Mammal Center. We thank the many field researchers and
the officers and crews of the NOAA Ship 'Oscar Elton Sette' and M/V
'Searcher' who were critical to the translocation, seal capture, and
habitat assessment efforts and who provided additional project support,
especially B. Braun, C. Yoshinaga, S. Guerin, M. Sullivan, S. Farry, J.
Jones, L. Kashinsky, and T. Johanos-Kam. This project was conducted
under Marine Mammal Protection Act Research and Enhancement Permit
10137. All activities were permitted by the Papahanaumokuakea Marine
National Monument Management Board (PMNM-2008-016, PMNM-2009-001, PMNM-
20100-30, and PMNM-2011-001), and activities involving monk seals were
approved by the San Jose State University Institutional Animal Care and
Use Committee Protocol 917.
NR 74
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U1 0
U2 0
PU INTER-RESEARCH
PI OLDENDORF LUHE
PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY
SN 1863-5407
EI 1613-4796
J9 ENDANGER SPECIES RES
JI Endanger. Species Res.
PY 2017
VL 32
BP 103
EP 115
DI 10.3354/esr00788
PG 13
WC Biodiversity Conservation
SC Biodiversity & Conservation
GA EN0ED
UT WOS:000395682200009
ER
PT J
AU Yazawa, K
Shakouri, A
Hendricks, TJ
AF Yazawa, Kazuaki
Shakouri, Ali
Hendricks, Terry J.
TI Thermoelectric heat recovery from glass melt processes
SO ENERGY
LA English
DT Article
DE High temperature thermoelectrk; Glass process; Industrial heat recovery
ID WASTE HEAT; EFFICIENCY; FURNACE; STRESS
AB Thermoelectric energy recovery from waste heat in glass melting process is investigated without any detrimental design or process changes. Melting glass pellets require a furnace with temperature over 1500 degrees C for downstream glass shaping processes and hence a large amount of exergy is available but currently destroyed. Due to high temperature gradients, parasitic losses are investigated in conjunction with the optimum thermoelectric design for maximum power output and the lowest cost. Among variations of thermal paths, the fireports are identified as the best potential for lowest cost. By partially replacing the refractory wall in thickness with a thermoelectric generator, heat loss is kept at the current 9 kW/m(2). High temperature gradients across the thermoelectric generator requires a water cooling heat sink. The cost of the heat sink is included in the overall energy and cost analysis. Based on a typical thermoelectric figure-of-merit (ZT = 1), optimally designed thermoelectric integrated system generates 55.6 kW of electricity with efficiency of over 15% from a 500 ton/day (5.8 kg/s) scale glass production at an additional cost of $ 1-2/W. This technology can provide 1.37 billion kWh of primary energy savings annually, if it is implemented throughout the whole glass industry in U.S. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Yazawa, Kazuaki; Shakouri, Ali] Purdue Univ, Birck Nanotechnol Ctr, 1205 W State St, W Lafayette, IN 47907 USA.
[Hendricks, Terry J.] CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Yazawa, K (reprint author), Purdue Univ, Birck Nanotechnol Ctr, 1205 W State St, W Lafayette, IN 47907 USA.
EM kyazawa@purdue.edu
FU Jet Propulsion Laboratory, California Institute of Technology
[NNN12AAO1C]
FX Terry J. Hendricks acknowledges the support from the Jet Propulsion
Laboratory, California Institute of Technology, under a contract
#NNN12AAO1C to the National Aeronautics and Space Administration.
NR 37
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U1 0
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0360-5442
EI 1873-6785
J9 ENERGY
JI Energy
PD JAN 1
PY 2017
VL 118
BP 1035
EP 1043
DI 10.1016/j.energy.2016.10.136
PG 9
WC Thermodynamics; Energy & Fuels
SC Thermodynamics; Energy & Fuels
GA EM1AF
UT WOS:000395048900088
ER
PT J
AU Pons, M
Branch, TA
Melnychuk, MC
Jensen, OP
Brodziak, J
Fromentin, JM
Harley, SJ
Haynie, AC
Kell, LT
Maunder, MN
Parma, AM
Restrepo, VR
Sharma, R
Ahrens, R
Hilborn, R
AF Pons, Maite
Branch, Trevor A.
Melnychuk, Michael C.
Jensen, Olaf P.
Brodziak, Jon
Fromentin, Jean M.
Harley, Shelton J.
Haynie, Alan C.
Kell, Laurie T.
Maunder, Mark N.
Parma, Ana M.
Restrepo, Victor R.
Sharma, Rishi
Ahrens, Robert
Hilborn, Ray
TI Effects of biological, economic and management factors on tuna and
billfish stock status
SO FISH AND FISHERIES
LA English
DT Article
DE Fisheries management; marine conservation; stock assessment; stock
status; tuna fisheries
ID ATLANTIC BLUEFIN TUNA; FISHERIES; UNCERTAINTY; POPULATIONS; ASSESSMENTS;
PATTERNS; DECLINE; OCEAN
AB Commercial tunas and billfishes (swordfish, marlins and sailfish) provide considerable catches and income in both developed and developing countries. These stocks vary in status from lightly exploited to rebuilding to severely depleted. Previous studies suggested that this variability could result from differences in life-history characteristics and economic incentives, but differences in exploitation histories and management measures also have a strong effect on current stock status. Although the status (bio-mass and fishing mortality rate) of major tuna and billfish stocks is well documented, the effect of these diverse factors on current stock status and the effect of management measures in rebuilding stocks have not been analysed at the global level. Here, we show that, particularly for tunas, stocks were more depleted if they had high commercial value, were long-lived species, had small pre-fishing biomass and were subject to intense fishing pressure for a long time. In addition, implementing and enforcing total allowable catches (TACs) had the strongest positive influence on rebuilding overfished tuna and billfish stocks. Other control rules such as minimum size regulations or seasonal closures were also important in reducing fishing pressure, but stocks under TAC implementations showed the fastest increase of biomass. Lessons learned from this study can be applied in managing large industrial fisheries around the world. In particular, tuna regional fisheries management organizations should consider the relative effectiveness of management measures observed in this study for rebuilding depleted large pelagic stocks.
C1 [Pons, Maite; Branch, Trevor A.; Melnychuk, Michael C.; Hilborn, Ray] Univ Washington, Sch Aquat & Fishery Sci, Box 355020, Seattle, WA 98195 USA.
[Jensen, Olaf P.] Rutgers State Univ, Dept Marine & Coastal Sci, 71 Dudley Rd, New Brunswick, NJ 08901 USA.
[Brodziak, Jon] NOAA Fisheries, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, 1845 Wasp Blvd, Honolulu, HI 96818 USA.
[Fromentin, Jean M.] IFREMER, UMR MARBEC Marine Biodivers Exploitat & Conservat, Blvd Jean Monnet,CS 30171, F-34203 Sete, France.
[Harley, Shelton J.] Secretariat Pacific Community, Fisheries Aquaculture & Marine Ecosyst Div, BP D5, Noumea 98848, New Caledonia.
[Haynie, Alan C.] NOAA Fisheries, Alaska Fisheries Sci Ctr, Bldg 4,7600 Sand Point Way NE, Seattle, WA 98115 USA.
[Kell, Laurie T.] ICCAT Int Commiss Conservat Atlantic Tunas Secret, Corazon de Maria 8, Madrid 28002, Spain.
[Maunder, Mark N.] IATTC, 8901 La Jolla Shores Dr, San Diego, CA 92037 USA.
[Parma, Ana M.] Consejo Nacl Invest Cient & Tecn, Ctr Nacl Patagon, Blvd Brown 2915,U9120ACD, Puerto Madryn, Chubut, Argentina.
[Restrepo, Victor R.] ISSF, 805 15th St NW,Suite 708, Washington, DC 20005 USA.
[Sharma, Rishi] IOTC, Le Chantier Mall,2nd Floor,POB 1011, Victoria, Mahe, Seychelles.
[Ahrens, Robert] Univ Florida, Program Fisheries & Aquat Sci, Sch Forest Resources & Conservat, POB 110410, Gainesville, FL 32653 USA.
[Sharma, Rishi] NOAA Fisheries, Southeast Fisheries Sci Ctr, 75 Virginia Beach Dr, Miami, FL 33149 USA.
RP Pons, M (reprint author), Univ Washington, Sch Aquat & Fishery Sci, Box 355020, Seattle, WA 98195 USA.
EM mpons@uw.edu
FU Pelagic Fisheries Research Program of the Joint Institute for Marine and
Atmospheric Research; Walton Family Foundation; Fulbright Fellowship
FX This project was funded by the Pelagic Fisheries Research Program of the
Joint Institute for Marine and Atmospheric Research, and the Walton
Family Foundation. MP was supported by a Fulbright Fellowship.
NR 82
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U1 1
U2 1
PU WILEY
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1467-2960
EI 1467-2979
J9 FISH FISH
JI Fish. Fish.
PD JAN
PY 2017
VL 18
IS 1
BP 1
EP 21
DI 10.1111/faf.12163
PG 21
WC Fisheries
SC Fisheries
GA EO0SC
UT WOS:000396407200001
ER
PT J
AU Driggers, WB
Campbell, MD
Hannan, KM
Hoffmayer, ER
Jones, CM
Jones, LM
Pollack, AG
AF Driggers, William B., III
Campbell, Matthew D.
Hannan, Kristin M.
Hoffmayer, Eric R.
Jones, Christian M.
Jones, Lisa M.
Pollack, Adam G.
TI Influence of bait type on catch rates of predatory fish species on
bottom longline gear in the northern Gulf of Mexico
SO FISHERY BULLETIN
LA English
DT Article
ID STANDARDIZED DIET COMPOSITIONS; FEEDING-BEHAVIOR; SHARK BYCATCH; RED
DRUM; LOPHOLATILUS-CHAMAELEONTICEPS; SCIAENOPS-OCELLATA; TROPHIC LEVELS;
HOOK; SEA; MORTALITY
AB Identifying effective methods of reducing shark bycatch in hook-based fisheries has received little attention despite reports of declines in some shark populations. Previously proposed shark bycatch mitigation measures include gear modifications, time and area closures, avoidance of areas with high shark abundance, use of repellents, and use of specific bait types. Regardless of the method of shark bycatch reduction, knowledge of the effects of the chosen method on the catch rates of targeted fish species should be understood. To examine the effects of bait type on catch rates of sharks and teleosts on bottom longline gear, standardized gear was deployed with bait alternating between Atlantic mackerel (Scomber scombrus) and northern shortfin squid (Illex illecebrosus). For all shark species examined, except the scalloped hammerhead (Sphyrna lewini), a preference for hooks baited with Atlantic mackerel was observed. Commercially and recreationally important teleosts had no significant preference for a specific bait, with the exception of the red drum (Sciaenops ocellatus), which had a significant preference for hooks baited with northern shortfin squid. Bait preference decreased as total catch rate increased on individual longline sets. Our results point to the use of specific baits as a viable method to reduce shark catch rates without decreasing catches of targeted teleosts.
C1 [Driggers, William B., III; Campbell, Matthew D.; Hoffmayer, Eric R.; Jones, Christian M.; Jones, Lisa M.] NOAA, Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Mississippi Labs, PO Drawer 1207, Pascagoula, MS 39567 USA.
[Hannan, Kristin M.; Pollack, Adam G.] NOAA, Natl Marine Fisheries Serv, Riverside Technol Inc, Southeast Fisheries Sci Ctr,Mississippi Labs, PO Drawer 1207, Pascagoula, MS 39567 USA.
RP Driggers, WB (reprint author), NOAA, Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Mississippi Labs, PO Drawer 1207, Pascagoula, MS 39567 USA.
EM william.driggers@noaa.gov
NR 45
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Z9 0
U1 0
U2 0
PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE
PI SEATTLE
PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA
SN 0090-0656
EI 1937-4518
J9 FISH B-NOAA
JI Fish. Bull.
PY 2017
VL 115
IS 1
BP 50
EP 59
DI 10.7755/FB.115.1.5
PG 10
WC Fisheries
SC Fisheries
GA EO2LN
UT WOS:000396528100005
ER
PT J
AU Bradford, AL
Forney, KA
Oleson, EM
Barlow, J
AF Bradford, Amanda L.
Forney, Karin A.
Oleson, Erin M.
Barlow, Jay
TI Abundance estimates of cetaceans from a line-transect survey within the
US Hawaiian Islands Exclusive Economic Zone
SO FISHERY BULLETIN
LA English
DT Article
ID SPINNER DOLPHIN; SITE FIDELITY; PACIFIC
AB A ship-based line-transect survey was conducted during the summer and fall of 2010 to obtain abundance estimates of cetaceans in the U.S. Hawaiian Islands Exclusive Economic Zone (EEZ). Given the low sighting rates for cetaceans in the study area, sightings from 2010 were pooled with sightings made during previous line-transect surveys within the central Pacific for calculating detection functions, which were estimated by using a multiple-covariate approach. The trackline detection probabilities used in this study are the first to reflect the effect of sighting conditions in the central Pacific and are markedly lower than estimates used in previous studies. During the survey, 23 cetacean species (17 odontocetes and 6 mysticetes) were seen, and abundance was estimated for 19 of them (15 odontocetes and 4 mysticetes). Group size and Beaufort sea state were the most important factors affecting the detectability of cetacean groups. Across all species, abundance estimates and coefficients of variation range from 133 to 72,528 and from 0.29 to 1.13, respectively. Estimated abundance is highest for delphinid species and lowest for the killer whale (Orcinus orca) and rorqual species. Overall, cetacean density in the Hawaiian Islands EEZ is low in comparison with highly productive oceanic regions.
C1 [Bradford, Amanda L.; Oleson, Erin M.] NOAA, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, 1845 Wasp Blvd,Bldg 176, Honolulu, HI 96818 USA.
[Forney, Karin A.] NOAA, Southwest Fisheries Sci Ctr, Natl Marine Fisheries Serv, 110 Shaffer Rd, Santa Cruz, CA 95060 USA.
[Barlow, Jay] NOAA, Southwest Fisheries Sci Ctr, Natl Marine Fisheries Serv, 8901 La Jolla Shores Dr, La Jolla, CA 92037 USA.
RP Bradford, AL (reprint author), NOAA, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, 1845 Wasp Blvd,Bldg 176, Honolulu, HI 96818 USA.
EM amanda.bradford@noaa.gov
NR 35
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U1 0
U2 0
PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE
PI SEATTLE
PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA
SN 0090-0656
EI 1937-4518
J9 FISH B-NOAA
JI Fish. Bull.
PY 2017
VL 115
IS 2
BP 129
EP 142
DI 10.7755/FB.115.2.1
PG 14
WC Fisheries
SC Fisheries
GA EO2LQ
UT WOS:000396528400001
ER
PT J
AU Stehlik, LL
Manderson, JP
Pessutti, J
AF Stehlik, Linda L.
Manderson, John P.
Pessutti, Jeffrey
TI Use of gill nets and telemetry in tracking movements and feeding of
striped bass (Morone saxatilis), bluefish (Pomatomus saltatrix), and
weakfish (Cynoscion regalis) at a salinity front in a small estuary
SO FISHERY BULLETIN
LA English
DT Article
ID THE-YEAR BLUEFISH; JUVENILE WINTER FLOUNDER; SOUTHERN NEW-JERSEY;
CHESAPEAKE BAY; HABITAT USE; ACOUSTIC TELEMETRY; TURBIDITY MAXIMUM;
CONTINENTAL-SHELF; ATLANTIC MENHADEN; SPATIAL-PATTERNS
AB The hypothesis that striped bass (Morone saxatilis), bluefish (Pomatomus saltatrix), weakfish (Cynoscion regalis), and species of forage fish would be associated closely with a salinity transition front was tested through sampling and tagging efforts. In a small New Jersey estuary, a station at a salinity front and another in a nearby channel were sampled weekly with gill nets. Abundance of bluefish was significantly greater at the front, and abundance of weakfish was significantly greater at the channel. Forage fish were collected at both stations, and the diets of bluefish and weakfish overlapped in all seasons. Ultrasonically tagged striped bass, weakfish, and bluefish were tracked concurrently, and their home ranges, or the 95% probability of their occurrences were computed. Home ranges of tagged striped bass occurred upriver and also near river kilometer 1. Home ranges of weakfish were located in the midriver channels, and those of bluefish were located midriver and upriver at river kilometers 5-12. Home ranges for these 3 species were not limited to the area of the salinity front, contrary to the initial hypothesis.
C1 [Stehlik, Linda L.; Manderson, John P.; Pessutti, Jeffrey] NOAA, Northeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Ecosyst & Aquaculture Div,James J Howard Marin Sc, 74 Magruder Rd, Highlands, NJ 07732 USA.
RP Stehlik, LL (reprint author), NOAA, Northeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Ecosyst & Aquaculture Div,James J Howard Marin Sc, 74 Magruder Rd, Highlands, NJ 07732 USA.
EM linda.stehlik@noaa.gov
NR 43
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U1 0
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PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE
PI SEATTLE
PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA
SN 0090-0656
EI 1937-4518
J9 FISH B-NOAA
JI Fish. Bull.
PY 2017
VL 115
IS 2
BP 143
EP 154
DI 10.7755/FB.115.2.2
PG 12
WC Fisheries
SC Fisheries
GA EO2LQ
UT WOS:000396528400002
ER
PT J
AU Berezin, IA
Timofeyev, YM
Virolainen, YA
Frantsuzova, IS
Volkova, KA
Poberovsky, AV
Holben, BN
Smirnov, A
Slutsker, I
AF Berezin, I. A.
Timofeyev, Yu. M.
Virolainen, Ya. A.
Frantsuzova, I. S.
Volkova, K. A.
Poberovsky, A. V.
Holben, B. N.
Smirnov, A.
Slutsker, I.
TI Error analysis of integrated water vapor measured by CIMEL photometer
SO IZVESTIYA ATMOSPHERIC AND OCEANIC PHYSICS
LA English
DT Article
DE Integrated water vapor; AERONET; CIMEL; MW radiometer; FTIR spectrometer
ID VARIABILITY
AB Water vapor plays a key role in weather and climate forming, which leads to the need for continuous monitoring of its content in different parts of the Earth. Intercomparison and validation of different methods for integrated water vapor (IWV) measurements are essential for determining the real accuracies of these methods. CIMEL photometers measure IWV at hundreds of ground-based stations of the AERONET network. We analyze simultaneous IWV measurements performed by a CIMEL photometer, an RPG-HATPRO MW radiometer, and a FTIR Bruker 125-HR spectrometer at the Peterhof station of St. Petersburg State University. We show that the CIMEL photometer calibrated by the manufacturer significantly underestimates the IWV obtained by other devices. We may conclude from this intercomparison that it is necessary to perform an additional calibration of the CIMEL photometer, as well as a possible correction of the interpretation technique for CIMEL measurements at the Peterhof site.
C1 [Berezin, I. A.; Timofeyev, Yu. M.; Virolainen, Ya. A.; Frantsuzova, I. S.; Volkova, K. A.; Poberovsky, A. V.] St Petersburg State Univ, St Petersburg 199034, Russia.
[Holben, B. N.; Smirnov, A.; Slutsker, I.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Virolainen, YA (reprint author), St Petersburg State Univ, St Petersburg 199034, Russia.
EM yana.virolainen@spbu.ru
RI Smirnov, Alexander/C-2121-2009
OI Smirnov, Alexander/0000-0002-8208-1304
FU Russian Foundation for Basic Research [15-05-07524]; Russian Scientific
Foundation [14-17-00096]
FX The experimental part of the research was carried out using the RC
Geomodel equipment of St. Petersburg State University, and was funded by
the by the Russian Foundation for Basic Research (grant no.
15-05-07524). Primary and secondary processing and analysis was carried
out at the expense of the Russian Scientific Foundation (grant no.
14-17-00096). The article was discussed and performed in the frame of
research activity at SPbU, no. 11.42.1380.2015. The work was performed
at St. Petersburg State University.
NR 24
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U2 0
PU MAIK NAUKA/INTERPERIODICA/SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013-1578 USA
SN 0001-4338
EI 1555-628X
J9 IZV ATMOS OCEAN PHY+
JI Izv. Atmos. Ocean. Phys.
PD JAN
PY 2017
VL 53
IS 1
BP 58
EP 64
DI 10.1134/S0001433817010030
PG 7
WC Meteorology & Atmospheric Sciences; Oceanography
SC Meteorology & Atmospheric Sciences; Oceanography
GA EN9GC
UT WOS:000396307700007
ER
PT J
AU Reginald, NL
Gopalswamy, N
Yashiro, S
Gong, Q
Guhathakurta, M
AF Reginald, Nelson L.
Gopalswamy, Natchimuthuk
Yashiro, Seiji
Gong, Qian
Guhathakurta, Madhulika
TI Replacing the polarizer wheel with a polarization camera to increase the
temporal resolution and reduce the overall complexity of a solar
coronagraph
SO JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS
LA English
DT Article
DE solar corona; linearly polarized brightness; linear polarizer;
polarization camera
ID ECLIPSE; MACS
AB Experiments that require linearly polarized brightness measurements, traditionally have obtained three successive images through a linear polarizer that is rotated through three well-defined angles and the images are combined to get the linearly polarized brightness. This technique requires a mechanism to hold the linear polarizer in place and to precisely turn it through the three angles. Obviously, the temporal resolution is lost in such a scenario, since the three images that are used to derive the linearly polarized brightness are taken at three different times. Specifically, in a dynamic corona that is in constant reshaping of its structures, the linearly polarized brightness image produced in this manner may not yield true values all around the corona. In this regard, with the advent of the polarization camera, the linearly polarized brightness can be measured from a single image. This also eliminates the need for a linear polarizer and the associated rotator mechanisms and can contribute toward lower weight, size, power requirements, overall risk of the instrument, and most importantly, increase the temporal resolution. We evaluate the capabilities of a selected polarization camera and how these capabilities could be tested in a ground experiment conducted in conjunction with a total solar eclipse. The ground experiment requires the measurement of the linearly polarized brightness, also known as K-corona, in a corona that also contains unpolarized brightness, known as F-corona, in order to measure three important physical properties pertaining to coronal electrons, namely, the electron density, electron temperature, and the electron speed. (C) The Authors.
C1 [Reginald, Nelson L.; Yashiro, Seiji] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Reginald, Nelson L.; Gopalswamy, Natchimuthuk; Yashiro, Seiji] NASA Goddard Space Flight Ctr, Solar Phys Div, Greenbelt, MD 20771 USA.
[Gong, Qian] NASA Goddard Space Flight Ctr, Opt Sci Div, Greenbelt, MD USA.
[Guhathakurta, Madhulika] NASA HQ, Heliophys Sci Div, Washington, DC USA.
RP Reginald, NL (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.; Reginald, NL (reprint author), NASA Goddard Space Flight Ctr, Solar Phys Div, Greenbelt, MD 20771 USA.
EM Nelson.L.Reginald@nasa.gov
FU NASA [CAN-NNG11PL10A2-Task125]
FX The eclipse team to the total solar eclipse of March 9, 2016, thanks the
Indonesian National Institute of Aeronautics and Space (LAPAN) for all
the help rendered in transporting our equipment between Jakarta,
Indonesia, and the eclipse observation site in Maba, Indonesia, in
selecting an observing site and for providing all the other necessary
logistics such as lodging and meals. We also thank the staff at the
American Embassy in Indonesia for receiving and clearing customs of our
eclipse equipment and for organizing public seminars to present our
effort to the Indonesian audience. Nelson L. Reginald also acknowledges
support from NASA grant CAN-NNG11PL10A2-Task125. Natchimuthuk
Gopalswamy, PI of the eclipse task force, acknowledges the travel
support provided by NASA HQ.
NR 23
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PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 2329-4124
EI 2329-4221
J9 J ASTRON TELESC INST
JI J. Astron. Telesc. Instrum. Syst.
PD JAN
PY 2017
VL 3
IS 1
AR 014001
DI 10.1117/1.JATIS.3.1.014001
PG 17
WC Engineering, Aerospace; Instruments & Instrumentation; Optics
SC Engineering; Instruments & Instrumentation; Optics
GA EO0DY
UT WOS:000396369700001
ER
PT J
AU Pagnutti, M
Ryan, RE
Cazenavette, G
Gold, M
Harlan, R
Leggett, E
Pagnutti, J
AF Pagnutti, Mary
Ryan, Robert E.
Cazenavette, George
Gold, Maxwell
Harlan, Ryan
Leggett, Edward
Pagnutti, James
TI Laying the foundation to use Raspberry Pi 3 V2 camera module imagery for
scientific and engineering purposes
SO JOURNAL OF ELECTRONIC IMAGING
LA English
DT Article
DE imaging; radiometric calibration; Raspberry Pi camera
AB A comprehensive radiometric characterization of raw-data format imagery acquired with the Raspberry Pi 3 and V2.1 camera module is presented. The Raspberry Pi is a high-performance single-board computer designed to educate and solve real-world problems. This small computer supports a camera module that uses a Sony IMX219 8 megapixel CMOS sensor. This paper shows that scientific and engineering-grade imagery can be produced with the Raspberry Pi 3 and its V2.1 camera module. Raw imagery is shown to be linear with exposure and gain (ISO), which is essential for scientific and engineering applications. Dark frame, noise, and exposure stability assessments along with flat fielding results, spectral response measurements, and absolute radiometric calibration results are described. This low-cost imaging sensor, when calibrated to produce scientific quality data, can be used in computer vision, biophotonics, remote sensing, astronomy, high dynamic range imaging, and security applications, to name a few. (C) The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its
C1 [Pagnutti, Mary; Ryan, Robert E.; Cazenavette, George; Gold, Maxwell; Harlan, Ryan; Leggett, Edward; Pagnutti, James] Stennis Space Ctr, Innovat Imaging & Res, Mississippi State, MS USA.
RP Pagnutti, M (reprint author), Stennis Space Ctr, Innovat Imaging & Res, Mississippi State, MS USA.
EM mpagnutti@i2rcorp.com
NR 29
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U1 0
U2 0
PU IS&T & SPIE
PI BELLINGHAM
PA 1000 20TH ST, BELLINGHAM, WA 98225 USA
SN 1017-9909
EI 1560-229X
J9 J ELECTRON IMAGING
JI J. Electron. Imaging
PD JAN
PY 2017
VL 26
IS 1
AR 013014
DI 10.1117/1.JEI.26.1.013014
PG 13
WC Engineering, Electrical & Electronic; Optics; Imaging Science &
Photographic Technology
SC Engineering; Optics; Imaging Science & Photographic Technology
GA EP0EO
UT WOS:000397059800044
ER
PT J
AU Englander, JA
Conway, BA
AF Englander, Jacob A.
Conway, Bruce A.
TI Automated Solution of the Low-Thrust Interplanetary Trajectory Problem
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article
ID GRAVITY-ASSIST TRAJECTORIES; GLOBAL OPTIMIZATION; GENETIC ALGORITHM;
DESIGN
AB Preliminary design of low-thrust interplanetary missions is a highly complex process. The mission designer must choose discrete parameters, such as the number of flybys, the bodies at which those flybys are performed, and in some cases, the final destination. In addition, a time history of control variables must be chosen that defines the trajectory. There are often many thousands, if not millions, of possible trajectories to be evaluated, which can be a very expensive process in terms of the number of human analyst hours required. An automated approach is therefore very desirable. This work presents such an approach by posing the mission design problem as a hybrid optimal control problem. The method is demonstrated on hypothetical missions to Mercury, the main asteroid belt, and Pluto.
C1 [Englander, Jacob A.] NASA, Goddard Space Flight Ctr, Nav & Mission Design Branch, Greenbelt, MD 20771 USA.
[Conway, Bruce A.] Univ Illinois, Dept Aerosp Engn, 104 South Wright St,Mail Code 236, Urbana, IL 61801 USA.
RP Englander, JA (reprint author), NASA, Goddard Space Flight Ctr, Nav & Mission Design Branch, Greenbelt, MD 20771 USA.
FU NASA Graduate Student Researchers Program; NASA Goddard Space Flight
Center Internal Research and Development Program
FX This research was funded by the NASA Graduate Student Researchers
Program, the NASA Goddard Space Flight Center Internal Research and
Development Program, and several customer-funded studies at NASA Goddard
Space Flight Center. The authors would like to acknowledge Matthew
Vavrina at a.i. solutions; Donald Ellison, Dr. Alexander Ghosh, and Ryne
Beeson at the University of Illinois; and Jeremy Knittel at NASA Goddard
Space Flight Center for their ongoing contributions to evolutionary
mission trajectory generator project. Frank Vaughn, Wayne Yu, and Greg
Marr of NASA Goddard Space Flight Center and Chelsea Welch of Lockheed
Martin assisted with testing.
NR 44
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U2 0
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0731-5090
EI 1533-3884
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD JAN
PY 2017
VL 40
IS 1
BP 15
EP 27
PG 13
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA EP0SV
UT WOS:000397097900002
ER
PT J
AU Hikes, J
Liounis, AJ
Christian, JA
AF Hikes, Jacob
Liounis, Andrew J.
Christian, John A.
TI Parametric Covariance Model for Horizon-Based Optical Navigation
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article
ID IMAGE
C1 [Hikes, Jacob; Liounis, Andrew J.; Christian, John A.] West Virginia Univ, Benjamin M Statler Coll Engn & Mineral Resources, Dept Mech & Aerosp Resources, Morgantown, WV 26506 USA.
[Liounis, Andrew J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Hikes, J (reprint author), West Virginia Univ, Benjamin M Statler Coll Engn & Mineral Resources, Dept Mech & Aerosp Resources, Morgantown, WV 26506 USA.
FU NASA [NNX13AJ25A]
FX This work was made possible by NASA under award NNX13AJ25A. The authors
thank Christopher D'Souza of the NASA Johnson Space Center for
encouragement to investigate this problem. An earlier version of this
manuscript was presented as American Astronomical Soceity Paper AAS
16-441 at the 26th AAS/AIAA Space Flight Mechanics Meeting in Napa,
California, 14-18 February 2016.
NR 8
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U2 0
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0731-5090
EI 1533-3884
J9 J GUID CONTROL DYNAM
JI J. Guid. Control Dyn.
PD JAN
PY 2017
VL 40
IS 1
BP 170
EP U233
PG 9
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA EP0SV
UT WOS:000397097900014
ER
PT J
AU Jesick, M
Demcak, S
Young, B
Jones, D
McCandless, SE
Schadegg, M
AF Jesick, Mark
Demcak, Stuart
Young, Brian
Jones, Drew
McCandless, Sarah Elizabeth
Schadegg, Maximilian
TI Navigation Overview for the Mars Atmosphere and Volatile Evolution
Mission
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
AB The Mars Atmosphere and Volatile Evolution mission is the first mission devoted primarily to the study of the Martian atmosphere. The spacecraft launched on 18 November 2013, entered Mars orbit on 22 September 2014, and continues to acquire measurements of Mars's upper atmosphere in an effort to understand the loss of Martian volatiles to space. The navigation team is responsible for estimating and predicting the spacecraft's position and velocity, and designing and reconstructing propulsive maneuvers. After Mars orbit insertion, the team faced additional challenges unique to the mission's orbit and tracking data schedule, including the determination of the atmospheric density at each periapsis, which is necessary to keep the spacecraft within a predefined density corridor. This paper briefly describes the Mars Atmosphere and Volatile Evolution mission, shows how it fits into previous and ongoing Mars exploration efforts, and overviews the operations of the navigation team from launch through the nominal science phase.
C1 [Jesick, Mark; Demcak, Stuart; Young, Brian; Jones, Drew; McCandless, Sarah Elizabeth; Schadegg, Maximilian] CALTECH, Jet Prop Lab, Mission Design & Nav Sect, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Jesick, M (reprint author), CALTECH, Jet Prop Lab, Mission Design & Nav Sect, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
FU NASA
FX The authors acknowledge the spacecraft team at Lockheed Martin for their
collaboration and contributions that have enabled a successfully
navigated mission. The navigation work described in this paper was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA.
NR 33
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PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD JAN
PY 2017
VL 54
IS 1
BP 29
EP 43
DI 10.2514/1.A33618
PG 15
WC Engineering, Aerospace
SC Engineering
GA EM7UF
UT WOS:000395517100003
ER
PT J
AU Kazemba, CD
Braun, RD
Clark, IG
Schoenenberger, M
AF Kazemba, Cole D.
Braun, Robert D.
Clark, Ian G.
Schoenenberger, Mark
TI Survey of Blunt-Body Supersonic Dynamic Stability
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID EMBEDDED NEWTONIAN FLOW; TRANSONIC SPEEDS; REENTRY CAPSULE; ENTRY
VEHICLES; MOTION; AERODYNAMICS; SIMULATIONS; DRAG
C1 [Kazemba, Cole D.] NASA, STC Inc, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Braun, Robert D.] Georgia Inst Technol, Atlanta, GA 30332 USA.
[Clark, Ian G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Schoenenberger, Mark] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Kazemba, CD (reprint author), NASA, STC Inc, Ames Res Ctr, Moffett Field, CA 94035 USA.
FU NASA Office of the Chief Technologist's Space Technology Research
Fellowship under NASA [NNX11AN20H]
FX This work was supported by a NASA Office of the Chief Technologist's
Space Technology Research Fellowship under NASA grant NNX11AN20H.
NR 83
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U1 0
U2 0
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD JAN
PY 2017
VL 54
IS 1
BP 109
EP 127
DI 10.2514/1.A33552
PG 19
WC Engineering, Aerospace
SC Engineering
GA EM7UF
UT WOS:000395517100010
ER
PT J
AU Karlgaard, CD
Kutty, P
Schoenenberger, M
AF Karlgaard, Christopher D.
Kutty, Prasad
Schoenenberger, Mark
TI Coupled Inertial Navigation and Flush Air Data Sensing Algorithm for
Atmosphere Estimation
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID SCIENCE LABORATORY ENTRY; SYSTEM SENSOR PLACEMENT; WIND ESTIMATION;
MARS; RECONSTRUCTION; OBSERVABILITY; OPTIMIZATION; DESCENT; LOCATION;
VEHICLES
AB This paper describes an algorithm for atmospheric state estimation based on a coupling between inertial navigation and flush air data-sensing pressure measurements. The navigation state is used in the atmospheric estimation algorithm along with the pressure measurements and a model of the surface pressure distribution to estimate the atmosphere using a nonlinear weighted least-squares algorithm. The approach uses a high-fidelity model of atmosphere stored in table-lookup form, along with simplified models propagated along the trajectory within the algorithm to aid the solution. Thus, the method is a reduced-order Kalman filter in which the inertial states are taken from the navigation solution and atmospheric states are estimated in the filter. The algorithm is applied to data from the Mars Science Laboratory entry, descent, and landing from August2012. Reasonable estimates of the atmosphere are produced by the algorithm. The observability of winds along the trajectory are examined using an index based on the observability Gramian and the pressure measurement sensitivity matrix. The results indicate that bank reversals are responsible for adding information content. The algorithm is applied to the design of the pressure measurement system for the Mars 2020 mission. A linear covariance analysis is performed to assess estimator performance. The results indicate that the new estimator produces more precise estimates of atmospheric states than existing algorithms.
C1 [Karlgaard, Christopher D.; Kutty, Prasad] Analyt Mech Associates Inc, Hampton, VA 23666 USA.
[Schoenenberger, Mark] NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Hampton, VA 23666 USA.
[Karlgaard, Christopher D.; Schoenenberger, Mark] AIAA, Reston, VA 20191 USA.
[Kutty, Prasad] Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA.
RP Karlgaard, CD (reprint author), Analyt Mech Associates Inc, Hampton, VA 23666 USA.; Karlgaard, CD (reprint author), AIAA, Reston, VA 20191 USA.
NR 48
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U1 0
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PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD JAN
PY 2017
VL 54
IS 1
BP 128
EP 140
DI 10.2514/1.A33331
PG 13
WC Engineering, Aerospace
SC Engineering
GA EM7UF
UT WOS:000395517100011
ER
PT J
AU Brune, AJ
Hosder, S
Edquist, KT
Tobin, SA
AF Brune, Andrew J.
Hosder, Serhat
Edquist, Karl T.
Tobin, Steven A.
TI Thermal Protection System Response Uncertainty of a Hypersonic
Inflatable Aerodynamic Decelerator
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID POLYNOMIAL CHAOS; SENSITIVITY-ANALYSIS
AB The objective of this paper is to investigate the uncertainty in the bondline temperature response of a flexible thermal protection system subject to uncertain parameters in the hypersonic flowfield and thermal response modeling of a hypersonic inflatable aerodynamic decelerator configuration for ballistic Mars entry. An inflatable decelerator with a 10m major diameter is selected for this study based on the forebody dimensions scaled from the 6m test article that was tested in the NASA Ames Research Center's National Full-Scale Aerodynamics Complex facility. A global nonlinear sensitivity analysis study for the bondline temperature uncertainty shows that the dimension of uncertain parameters can reduce from 22 to 8. An uncertainty analysis of the bondline temperature in the reduced dimensions indicates that the bondline temperature varies by as much as 125% above the nominal prediction and exceeds the temperature limit of 400 degrees C. The largest uncertainty occurred at 70s in the trajectory before separation of the inflatable decelerator for transition to a secondary descent technology. The main contributors to the bondline temperature uncertainty are the insulator and outer fabric conductivities, as well as the freestream density. The thickness and initial density of the insulator layer, closest to the gas barrier layer, are also shown to be significant contributors to the bondline temperature uncertainty, especially earlier in the trajectory.
C1 [Brune, Andrew J.] Missouri Univ Sci & Technol, Dept Aerosp & Mech Engn, Rolla, MO 65409 USA.
[Hosder, Serhat] Missouri Univ Sci & Technol, Aerosp Engn, Dept Aerosp & Mech Engn, Rolla, MO 65409 USA.
[Edquist, Karl T.] NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Engn Directorate, Hampton, VA 23681 USA.
[Tobin, Steven A.] NASA, Langley Res Ctr, Struct & Thermal Syst Branch, Engn Directorate, Hampton, VA 23681 USA.
[Brune, Andrew J.; Hosder, Serhat; Edquist, Karl T.; Tobin, Steven A.] AIAA, Reston, VA 20191 USA.
RP Brune, AJ (reprint author), Missouri Univ Sci & Technol, Dept Aerosp & Mech Engn, Rolla, MO 65409 USA.; Brune, AJ (reprint author), AIAA, Reston, VA 20191 USA.
FU NASA [NNX13AL58H]
FX This work was supported by a NASA Space Technology Research Fellowship
under training project grant no. NNX13AL58H (Serhat Hosder, Principal
Investigator; and Karl Edquist, Research Collaborator). The authors
would like to thank John Dec from NASA Langley Research Center for
providing guidance and technical support for the thermal protection
system thermal response modeling process and providing necessary
information to make this work possible.
NR 39
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PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD JAN
PY 2017
VL 54
IS 1
BP 141
EP 154
DI 10.2514/1.A33732
PG 14
WC Engineering, Aerospace
SC Engineering
GA EM7UF
UT WOS:000395517100012
ER
PT J
AU Rhode, MN
Oberkampf, WL
AF Rhode, Matthew N.
Oberkampf, William L.
TI Estimation of Uncertainties for a Model Validation Experiment in a Wind
Tunnel
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID COMPUTATIONAL FLUID-DYNAMICS; SUPERSONIC RETROPROPULSION; MARS ENTRY;
DESCENT
AB A high-quality model validation experiment was performed in the NASA Langley Research Center Unitary Plan Wind Tunnel to assess the predictive accuracy of computational-fluid-dynamics models for a blunt-body supersonic retropropulsion configuration at freestream Mach numbers from 2.4 to 4.6. Static and fluctuating surface pressure data were acquired on a 5-in.-diam (127-mm-diam) test article with a forebody composed of a spherically blunted, 70deg half-angle cone and a cylindrical aft body. One unpowered configuration with a smooth outer mold line was tested as well as three powered, forward-firing nozzle configurations: a centerline nozzle, three nozzles equally spaced around the forebody, and a combination with all four nozzles. A key objective of the experiment was the determination of experimental uncertainties from a range of sources such as random measurement variation, flowfield nonuniformity, and model/instrumentation uncertainties. This paper discusses 1)the design of the experiment to best capture these uncertainties for the baseline unpowered configuration, 2)the methodology used in quantifying the various sources of uncertainty, and 3)examples of the uncertainties applied to unpowered and powered experimental results. The uncertainty analysis, which concentrates on the unpowered configuration, showed that flowfield nonuniformity was the dominant contributor to the overall uncertainty. This finding is in agreement with other wind-tunnel experiments that have quantified various sources of uncertainty.
C1 [Rhode, Matthew N.] NASA, Langley Res Ctr, Aerothermodynam Branch, Mail Stop 408A, Hampton, VA 23681 USA.
[Oberkampf, William L.] WL Oberkampf Consulting, Austin, TX 78633 USA.
[Rhode, Matthew N.; Oberkampf, William L.] AIAA, Reston, VA 20191 USA.
RP Oberkampf, WL (reprint author), WL Oberkampf Consulting, Austin, TX 78633 USA.; Oberkampf, WL (reprint author), AIAA, Reston, VA 20191 USA.
EM wloconsulting@gmail.com
FU NASA
FX The authors would like to acknowledge the support of the NASA
Exploration Technology Development and Demonstration (ETDD) Program and
Fundamental Aeronautics Program (FAP). The work documented herein was
performed jointly by the ETDD EDL Technology Development Project as well
as FAP's Hypersonics Project, both of which are managed at NASA Langley
Research Center and supported by NASA Ames Research Center, NASA Johnson
Space Center, and the Jet Propulsion Laboratory. Particular recognition
goes to Scott Berry, Karl Edquist, Bil Kleb, Guy Schauerhamer, Kerry
Zarchi, Ashley Korzun, Chris Laws, Courtney Spells, Aaron Fuchs, Bryan
Falman, Ricky Hall, and Steve Jones for their efforts in the design,
planning, and execution of this experiment. A special thank you is
extended to Bruce Graham for his helpful suggestions with the software
scripts that were used in the analysis of these data.
NR 25
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PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD JAN
PY 2017
VL 54
IS 1
BP 155
EP 168
DI 10.2514/1.A33563
PG 14
WC Engineering, Aerospace
SC Engineering
GA EM7UF
UT WOS:000395517100013
ER
PT J
AU Lobbia, MA
AF Lobbia, Marcus A.
TI Multidisciplinary Design Optimization of Waverider-Derived Crew Reentry
Vehicles
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID HL-20; ENVIRONMENT
AB The development of a multidisciplinary design optimization framework for crew reentry vehicles is presented. A waverider design methodology is used as the basis for the parametric design technique, with required modifications (e.g., leading edge blunting and integration of a cylindrical payload volume representing the crew compartment) used to allow the generation of practical reentry configurations. In addition to the shape design code, aerodynamics analysis, mass estimating, and trajectory/aeroheating analyses are linked using a multiobjective genetic algorithm optimization process to maximize vehicle downrange, additional payload mass capability, and lift-to-drag ratio. Pareto fronts were generated for three different launch vehicle capabilities ranging from 12,000 to 26,000kg to orbit, and highlight the relationships between reentry vehicle payload mass, maximum lift-to-drag ratio, and downrange, as well as the fact that a medium-class or larger launch vehicle was required to meet the baseline mission payload mass requirement. Although the modifications necessary for the crew reentry vehicle mission resulted in a substantial reduction in lift-to-drag ratio relative to the idealized waveriders used in the design process, comparisons of several designs to the NASA HL-20 concept indicated that the waverider-derived design process can produce vehicles with an almost 30% improvement in maximum lift-to-drag ratio and the ability to carry additional payload mass on longer downrange trajectories.
C1 [Lobbia, Marcus A.] Aerosp Corp, Launch Strike & Range Dept, 2310 E El Segundo Blvd,Mail Stop M1-557, El Segundo, CA 90245 USA.
[Lobbia, Marcus A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Lobbia, MA (reprint author), Aerosp Corp, Launch Strike & Range Dept, 2310 E El Segundo Blvd,Mail Stop M1-557, El Segundo, CA 90245 USA.; Lobbia, MA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 26
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U1 0
U2 0
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD JAN
PY 2017
VL 54
IS 1
BP 233
EP 245
DI 10.2514/1.A33253
PG 13
WC Engineering, Aerospace
SC Engineering
GA EM7UF
UT WOS:000395517100019
ER
PT J
AU Lobbia, MA
AF Lobbia, Marcus A.
TI Rapid Supersonic/Hypersonic Aerodynamics Analysis Model for Arbitrary
Geometries
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
C1 [Lobbia, Marcus A.] Aerosp Corp, Launch Strike & Range Dept, 2310 E El Segundo Blvd,Mail Stop M1-557, El Segundo, CA 90245 USA.
[Lobbia, Marcus A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Lobbia, MA (reprint author), Aerosp Corp, Launch Strike & Range Dept, 2310 E El Segundo Blvd,Mail Stop M1-557, El Segundo, CA 90245 USA.; Lobbia, MA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 17
TC 0
Z9 0
U1 0
U2 0
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD JAN
PY 2017
VL 54
IS 1
BP 315
EP +
DI 10.2514/1.A33514
PG 8
WC Engineering, Aerospace
SC Engineering
GA EM7UF
UT WOS:000395517100027
ER
PT J
AU Harvey, N
Dunn, CE
Kruizinga, GL
Young, LE
AF Harvey, Nate
Dunn, Charles E.
Kruizinga, Gerhard L.
Young, Lawrence E.
TI Triggering Conditions for GRACE Ranging Measurement Signal-to-Noise
Ratio Dips
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
C1 [Harvey, Nate; Dunn, Charles E.; Kruizinga, Gerhard L.; Young, Lawrence E.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Harvey, N (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
FU NASA
FX This research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with NASA. Our
thanks to Srinivas Bettadpur, Ab Davis, and Sumita Nandi for useful
conversations about the GRACE spacecraft and instruments.
NR 4
TC 0
Z9 0
U1 0
U2 0
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0022-4650
EI 1533-6794
J9 J SPACECRAFT ROCKETS
JI J. Spacecr. Rockets
PD JAN
PY 2017
VL 54
IS 1
BP 326
EP 329
DI 10.2514/1.A33578
PG 4
WC Engineering, Aerospace
SC Engineering
GA EM7UF
UT WOS:000395517100029
ER
PT J
AU Bennett, GJ
Stephens, DB
Verdugo, FR
AF Bennett, Gareth J.
Stephens, David B.
Verdugo, Francisco Rodriguez
TI Resonant mode characterisation of a cylindrical Helmholtz cavity excited
by a shear layer
SO JOURNAL OF THE ACOUSTICAL SOCIETY OF AMERICA
LA English
DT Article
ID NOISE-SOURCE-IDENTIFICATION; FLOW; OSCILLATIONS; SCALE; SOUND; DUCTS
AB This paper investigates the interaction between the shear-layer over a circular cavity with a relatively small opening and the flow-excited acoustic response of the volume within to shear-layer instability modes. Within the fluid-resonant category of cavity oscillation, most research has been conducted on rectangular geometries: generally restricted to longitudinal standing waves, or when cylindrical: to Helmholtz resonance. In practical situations, however, where the cavity is subject to a range of flow speeds, many different resonant mode types may be excited. The current work presents a cylindrical cavity design where Helmholtz oscillation, longitudinal resonance, and azimuthal acoustic modes may all be excited upon varying the flow speed. Experiments performed show how lock-on between each of the three fluid-resonances and shear-layer instability modes can be generated. A circumferential array of microphones flush-mounted with the internal surface of the cavity wall was used to decompose the acoustic pressure field into acoustic modes and has verified the excitation of higher order azimuthal modes by the shear-layer. For azimuthal modes especially, the location of the cavity opening affects the pressure response. A numerical solution is validated and provides additional insight and will be applied to more complex aeronautical and automotive geometries in the future. (C) 2017 Acoustical Society of America.
C1 [Bennett, Gareth J.; Stephens, David B.] Univ Dublin, Sch Engn, Dept Mech & Mfg Engn, Trinity Coll Dublin, Dublin D02 PN40, Ireland.
[Verdugo, Francisco Rodriguez] Univ Rome Tre, Dipartimento Ingn Meccan Ind, Rome, Italy.
[Stephens, David B.] NASA, Glenn Res Ctr, Cleveland, OH 44070 USA.
[Verdugo, Francisco Rodriguez] Loccioni, Via Fiume 16, Angeli Di Rosora, Italy.
RP Bennett, GJ (reprint author), Univ Dublin, Sch Engn, Dept Mech & Mfg Engn, Trinity Coll Dublin, Dublin D02 PN40, Ireland.
EM gareth.bennett@tcd.ie
FU Marie Curie Early Stage Research Training grant; European Union
[FP7/2007-2013, 620188]
FX D.B.S. was supported as a visiting scholar to Trinity College Dublin by
the Erasmus Mundus Master of Mechanical Engineering programme before
taking up his position in NASA. F.R.V. spent this research period in
Trinity College Dublin as a graduate student and was supported by a
Marie Curie Early Stage Research Training grant. The research leading to
these results has received funding from the European Union's Seventh
Framework Programme (Grant No. FP7/2007-2013) for the Clean Sky Joint
Technology Initiative under grant agreement No. 620188.
NR 46
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PU ACOUSTICAL SOC AMER AMER INST PHYSICS
PI MELVILLE
PA STE 1 NO 1, 2 HUNTINGTON QUADRANGLE, MELVILLE, NY 11747-4502 USA
SN 0001-4966
EI 1520-8524
J9 J ACOUST SOC AM
JI J. Acoust. Soc. Am.
PD JAN
PY 2017
VL 141
IS 1
BP 7
EP 18
DI 10.1121/1.4973212
PG 12
WC Acoustics; Audiology & Speech-Language Pathology
SC Acoustics; Audiology & Speech-Language Pathology
GA EM4UP
UT WOS:000395308700016
PM 28147611
ER
PT J
AU Park, O
Burns, RA
Buxton, ORH
Clemens, N
AF Park, Okjoo
Burns, Ross A.
Buxton, Oliver R. H.
Clemens, Noelt.
TI Mixture fraction, soot volume fraction, and velocity imaging in the
soot-inception region of a turbulent non-premixed jet flame
SO PROCEEDINGS OF THE COMBUSTION INSTITUTE
LA English
DT Article
DE Soot; Turbulent jet flame; LII; PIV; PLIF
ID LAMINAR DIFFUSION FLAMES; NONPREMIXED FLAMES; TEMPERATURE-MEASUREMENTS;
TRANSPORT; KRYPTON; EVOLUTION; GROWTH; XENON
AB An experimental study is performed to investigate the feasibility of conducting simultaneous mixture fraction, soot volume fraction and velocity imaging in sooting jet flames. The measurements are performed in the soot-inception region of ethylene jet flames, where the yellow luminous region first appears in the flame. Three-component velocity and soot volume fraction are measured by stereoscopic particle image velocimetry and laser-induced incandescence, respectively. The mixture fraction is inferred from laser-induced fluorescence of krypton gas seeded into the fuel stream. To obtain mixture fraction from the fluorescence signal, the signal must be corrected for density and fluorescence quenching effects. This correction is accomplished by invoking an assumed state relationship that is derived from a laminar strained-flame calculation. Once properly calibrated, the krypton planar laser-induced fluorescence data give the mixture fraction, temperature and major species near the regions of soot formation. The krypton is seeded into the fuel jet at a mole fraction of approximately 4%. The fluorescence of krypton is achieved by two-photon absorption at 214.7 nm and the resulting fluorescence is collected at 760.2 nm. The krypton fluorescence signal is rather weak, particularly near the reaction zones where density is lowest, and so adequate signal-to-noise ratios could be achieved in a region only about 1 mm in height, which effectively limited this study to a line measurement of mixture fraction. The temperature field derived from the mixture fraction field was compared to temperatures obtained from thermocouple measurements. The mean radial temperature profiles using the different techniques show excellent agreement and this serves to validate the methodology used to map from fluorescence signal to mixture fraction and temperature. The resulting data are of high enough quality as to allow the investigation of the kinematics, thermo-chemical state and even the dissipation fields near regions of soot formation. (C) 2016 by The Combustion Institute. Published by Elsevier Inc.
C1 [Park, Okjoo; Clemens, Noelt.] Univ Texas Austin, Dept Aerosp Engn & Engn Mech, Austin, TX 78712 USA.
[Burns, Ross A.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Buxton, Oliver R. H.] Imperial Coll, Dept Aeronaut, London, England.
RP Clemens, N (reprint author), Univ Texas Austin, Dept Aerosp Engn & Engn Mech, Austin, TX 78712 USA.
EM clemens@mail.utexas.edu
FU US National Science Foundation [CBET-1134020]; Strategic Environmental
Research Development Program [W912HQ-11-C-0035]
FX This work was sponsored by the US National Science Foundation
(CBET-1134020) and the Strategic Environmental Research Development
Program (W912HQ-11-C-0035).
NR 38
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PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 1540-7489
EI 1873-2704
J9 P COMBUST INST
JI Proc. Combust. Inst.
PY 2017
VL 36
IS 1
BP 899
EP 907
DI 10.1016/j.proci.2016.08.048
PG 9
WC Thermodynamics; Energy & Fuels; Engineering, Chemical; Engineering,
Mechanical
SC Thermodynamics; Energy & Fuels; Engineering
GA EP6BY
UT WOS:000397464200089
ER
PT J
AU Reddy, SN
Nanda, S
Hegde, UG
Hicks, MC
Kozinski, JA
AF Reddy, Sivamohan N.
Nanda, Sonil
Hegde, Uday G.
Hicks, Michael C.
Kozinski, Janusz A.
TI Ignition of n-propanol-air hydrothermal flames during supercritical
water oxidation
SO PROCEEDINGS OF THE COMBUSTION INSTITUTE
LA English
DT Article
DE Hydrothermal flames; Near-critical water; Supercritical water;
n-propanol; Ignition delay
ID DIFFUSION FLAMES; HIGH-PRESSURES; COMBUSTION
AB A novel concept was applied for the in situ study of the ignition of n-propanol-air hydrothermal flames during supercritical water oxidation. An innovative experimental arrangement including NASA's supercritical water oxidation facility was used to study the effect of reactor and oxidant (air) temperature on the spontaneous ignition of hydrothermal flames. New data were obtained concerning time-and temperature-resolved profiles of n-propanol in hydrothermal flames. Transient temperature profiles were recorded and the sudden increase in the temperature was used to determine the onset of flame ignition. The optimal reactor temperatures for flame ignition (ignition delay similar to 1 s) were determined as 380 degrees C (at oxidant temperature of 450 degrees C) and 420 degrees C (at oxidant temperature of 400 degrees C) with 20.7 MPa pressure and 1.5 mL/s oxidant (air) flow rate. The influence of buoyancy on ignition is also discussed in terms of Froude number. Time delays associated with the flame ignition at near-critical and supercritical environments as well as possible routes towards their diminution are elaborated. The ignition mechanism of n -propanol-air hydrothermal flames together with the ignition maps have been proposed for the first time. (C) 2016 by The Combustion Institute. Published by Elsevier Inc.
C1 [Reddy, Sivamohan N.; Nanda, Sonil; Kozinski, Janusz A.] York Univ, Lassonde Sch Engn, Dept Earth & Space Sci & Engn, Toronto, ON, Canada.
[Reddy, Sivamohan N.] Indian Inst Technol Roorkee, Dept Chem Engn, Roorkee, Uttar Pradesh, India.
[Hegde, Uday G.] Case Western Reserve Univ, Dept Mech & Aerosp Engn, Cleveland, OH USA.
[Hicks, Michael C.] NASA, Glenn Res Ctr, Cleveland, OH USA.
RP Kozinski, JA (reprint author), York Univ, Lassonde Sch Engn, Dept Earth & Space Sci & Engn, Toronto, ON, Canada.
EM janusz.kozinski@lassonde.yorku.ca
FU Natural Sciences and Engineering Research Council of Canada (NSERC);
Lassonde School of Engineering
FX The authors would like to thank Natural Sciences and Engineering
Research Council of Canada (NSERC) for proving funding to conduct this
emerging area of research. The technical assistance from NASA and
support from the Lassonde School of Engineering are greatly appreciated.
NR 23
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PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 1540-7489
EI 1873-2704
J9 P COMBUST INST
JI Proc. Combust. Inst.
PY 2017
VL 36
IS 2
BP 2503
EP 2511
DI 10.1016/j.proci.2016.05.042
PG 9
WC Thermodynamics; Energy & Fuels; Engineering, Chemical; Engineering,
Mechanical
SC Thermodynamics; Energy & Fuels; Engineering
GA EP5ZY
UT WOS:000397458900097
ER
PT J
AU Farouk, TI
Dietrich, D
Alam, FE
Dryer, FL
AF Farouk, T. I.
Dietrich, D.
Alam, F. E.
Dryer, F. L.
TI Isolated n-decane droplet combustion - Dual stage and single stage
transition to "Cool Flame" droplet burning
SO PROCEEDINGS OF THE COMBUSTION INSTITUTE
LA English
DT Article
DE Cool flame; Droplet combustion; Alkanes; Dual-stage; Ignition energy
ID MICROGRAVITY EXPERIMENTS
AB Observations of "Cool Flame" burning for large diameter isolated droplets on board the International Space Station have stimulated interest in combustion initiation/generation of non-premixed combustion modes. For a number of n-alkane fuels at large initial droplet diameters, the initiation process was observed to first establish a hot flame condition that radiatively extinguished, followed by a quasi-steady, "Cool Flame" droplet burning mode. However, recent large diameter n-decane experiments show that depending on the ig-nition energy supplied, the first stage hot flame condition was absent, with an apparent, direct establishment of a "Cool Flame" burning mode that continued to diffusive extinction. Here we report these experimental observations and elucidate the underlying parameters resulting in dual and single stage "Cool Flame" burning. Detailed, transient sphero-symmetric droplet combustion modeling is applied to interpret the experiments. The simulations indicate that the balance and duration of the ignition energy applied, the energy release associated with reaction of partially premixed fuel vapor surrounding the droplet, heat flux to the drop surface, and far field diffusive heat loss all play key roles as to whether a dual stage, radiatively extinguished hot-flame-to-Cool-Flame-transition for only large droplets or direct establishment of "Cool Flame" burning for all droplet sizes occurs. The rate at which the reactive partially premixed vapor layer surrounding the droplet is formed, its volume, and its subsequent reaction significantly influence the observed transition to "Cool Flame" burning. The initial droplet temperature relative to saturation and flash point temperatures of the fuel and the liquid phase heat capacity contribute to the thermal transport requirement at the droplet surface for establishing the partially premixed reactive layer surrounding the droplet, which through its reaction history defines whether a transition to "Cool Flame" burning can be initiated without a requirement for radiative extinction of a hot flame burning mode. (C) 2016 by The Combustion Institute. Published by Elsevier Inc.
C1 [Farouk, T. I.; Alam, F. E.] Univ South Carolina, Dept Mech Engn, Columbia, SC 29208 USA.
[Dietrich, D.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Dryer, F. L.] Princeton Univ, Dept Mech & Aerosp Engn, Princeton, NJ 08544 USA.
RP Farouk, TI (reprint author), Univ South Carolina, Dept Mech Engn, Columbia, SC 29208 USA.
EM tfarouk@sc.edu
FU National Aeronautics and Space Administration (NASA) [NNX14AG461A,
NNX09AW 19A]
FX This study was supported by the National Aeronautics and Space
Administration (NASA) through grant numbers NNX14AG461A (TF and FEA) and
NNX09AW 19A (FLD)
NR 21
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PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 1540-7489
EI 1873-2704
J9 P COMBUST INST
JI Proc. Combust. Inst.
PY 2017
VL 36
IS 2
BP 2523
EP 2530
DI 10.1016/j.proci.2016.07.015
PG 8
WC Thermodynamics; Energy & Fuels; Engineering, Chemical; Engineering,
Mechanical
SC Thermodynamics; Energy & Fuels; Engineering
GA EP5ZY
UT WOS:000397458900099
ER
PT J
AU Cuoci, A
Saufi, AE
Frassoldati, A
Dietrich, DL
Williams, FA
Faravelli, T
AF Cuoci, Alberto
Saufi, Abd E.
Frassoldati, Alessio
Dietrich, Daniel L.
Williams, Forman A.
Faravelli, Tiziano
TI Flame extinction and low-temperature combustion of isolated fuel
droplets of n-alkanes
SO PROCEEDINGS OF THE COMBUSTION INSTITUTE
LA English
DT Article
DE Low-temperature chemistry; Cool flame; Extinction; Microgravity; Droplet
ID INITIAL DIAMETER; COOL-FLAMES; MICROGRAVITY; HEPTANE; MODEL
AB A recent set of experiments carried out onboard the International Space Station (ISS) have shown that large n-alkane droplets, after the radiative extinction of the visible flame, can burn quasi-steadily in a low-temperature regime, up to a diffusive extinction accompanied by the formation of a vapor cloud. The experiments have also demonstrated that small droplets are unable to exhibit radiative extinction, but instead burn to completion or disruptively extinguish.
In this work, we applied a mathematical model able to reproduce the experimental data in terms of vaporization rates, standoff ratios, extinction diameters. A detailed kinetic mechanism (with similar to 450 species and similar to 17,000 reactions) was taken into account, in order to correctly reproduce the low-temperature combustion regime. The role of several parameters (initial diameter of the droplet, composition of the gaseous environment, and pressure) on the extinction of the hot-temperature flames was numerically investigated. Predictions are found in good agreement with experimental measurements, showing that only droplets with an initial diameter larger than a critical diameter undergo radiative extinction. A linear relationship between the squared critical diameter and the molar fraction of oxygen in the atmosphere was found and demonstrated on the basis of scaling arguments. (C) 2016 by The Combustion Institute. Published by Elsevier Inc.
C1 [Cuoci, Alberto; Saufi, Abd E.; Frassoldati, Alessio; Faravelli, Tiziano] G Natta Politecn Milano, Dept Chem Mat & Chem Engn, Piazza Leonardo Vinci 32, I-20133 Milan, Italy.
[Dietrich, Daniel L.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Williams, Forman A.] Univ Calif San Diego, Dept Mech & Aerosp Engn, San Diego, CA 92093 USA.
RP Cuoci, A (reprint author), G Natta Politecn Milano, Dept Chem Mat & Chem Engn, Piazza Leonardo Vinci 32, I-20133 Milan, Italy.
EM alberto.cuoci@polimi.it
FU NASA Space Life and Physical Sciences Research and Applications Program;
International Space Station Program
FX The authors would like to acknowledge Prof. Eliseo Ranzi of Politecnico
di Milano for the useful and inspiring discussions. This work was
supported by the NASA Space Life and Physical Sciences Research and
Applications Program and the International Space Station Program. Mr. J.
Mark Hickman served as the project manager.
NR 22
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PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 1540-7489
EI 1873-2704
J9 P COMBUST INST
JI Proc. Combust. Inst.
PY 2017
VL 36
IS 2
BP 2531
EP 2539
DI 10.1016/j.proci.2016.08.019
PG 9
WC Thermodynamics; Energy & Fuels; Engineering, Chemical; Engineering,
Mechanical
SC Thermodynamics; Energy & Fuels; Engineering
GA EP5ZY
UT WOS:000397458900100
ER
PT J
AU Xu, YH
Hicks, MC
Avedisian, CT
AF Xu, Yuhao
Hicks, Michael C.
Avedisian, C. Thomas
TI The combustion of iso-octane droplets with initial diameters from 0.5 to
5 mm: Effects on burning rate and flame extinction
SO PROCEEDINGS OF THE COMBUSTION INSTITUTE
LA English
DT Article
DE Droplet combustion; Spherical symmetry; Microgravity; iso-Octane;
Surrogate fuel
ID N-HEPTANE; COOL-FLAMES; CONVECTION; MICROGRAVITY; IGNITION; SOOT;
OXIDATION; MIXTURES; KINETICS; GASOLINE
AB The burning characteristics of iso-octane droplets in the standard atmosphere are reported over a large range of initial droplet diameters (0.5 mm < D-o < 5 mm) for near one-dimensional droplet flames as promoted by low gravity. A ground-based drop tower and a space-based platform (International Space Station) were used to provide an environment to examine the influence of D-o that encompasses regimes where radiation does not have an effect on burning to where it does. For D-o < 2.7 mm, the droplets burned to completion without extinction. Larger droplets evidenced extinction due to radiative emissions from the flames to the ambience that produced a two stage burning process. The burning rate (K) was nearly constant in the first stage and then gradually decreased. Concurrently, radiation emissions dropped by two orders of magnitude and 'flickering' flames were noted during the transition. After extinction, burning entered a regime where K gradually decreased with time and approached values commensurate with evaporation in a heated environment (i. e., no combustion). Energy balances based on scale analyses related K and flame temperature (T-f) to D-o : a balance at the flame including radiation losses led to the scaling K similar to D-o(-n) in reasonable agreement with the data for D-o > 2 mm; an energy balance at the droplet surface showed that T-f quickly dropped from similar to 1600 K to similar to 700 K after flame extinction, followed by a gradual reduction of T-f to near ambient temperature. The trends in the data are also discussed for potentially revealing a possible low temperature combustion regime. (C) 2016 by The Combustion Institute. Published by Elsevier Inc.
C1 [Xu, Yuhao; Avedisian, C. Thomas] Cornell Univ, Sibley Sch Mech & Aerosp Engn, Ithaca, NY 14853 USA.
[Hicks, Michael C.] Combust & Reacting Syst Branch, NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Avedisian, CT (reprint author), Cornell Univ, Sibley Sch Mech & Aerosp Engn, Ithaca, NY 14853 USA.
EM cta2@cornell.edu
FU National Aeronautics and Space Administration [NNX08AI51G]
FX This research was funded by the National Aeronautics and Space
Administration under Grants NNX08AI51G. The authors thank D.L. Dietrich
(NASA) and V. Nayagam (Case Western Reserve University) for some
assistance with the ISS experiments. The help of Hee Dae Tak, Meilin
Dong, Do Hyun Chung, Nan Wei, and Yiren Shen with some of the
experiments and video image analysis is appreciated. We also appreciate
the interest of F.A. Williams (UCSD), F.L. Dryer (Princeton), and T.
Farouk (U South Carolina) in this study.
NR 47
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PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 1540-7489
EI 1873-2704
J9 P COMBUST INST
JI Proc. Combust. Inst.
PY 2017
VL 36
IS 2
BP 2541
EP 2548
DI 10.1016/j.proci.2016.07.096
PG 8
WC Thermodynamics; Energy & Fuels; Engineering, Chemical; Engineering,
Mechanical
SC Thermodynamics; Energy & Fuels; Engineering
GA EP5ZY
UT WOS:000397458900101
ER
PT J
AU Bhattacharjee, S
Simsek, A
Miller, F
Olson, S
Ferkul, P
AF Bhattacharjee, Subrata
Simsek, Aslihan
Miller, Fletcher
Olson, Sandra
Ferkul, Paul
TI Radiative, thermal, and kinetic regimes of opposed-flow flame spread: A
comparison between experiment and theory
SO PROCEEDINGS OF THE COMBUSTION INSTITUTE
LA English
DT Article
DE Flame spread; Microgravity; Extinction velocity; Radiative extinction;
Space station
ID THIN FUELS; MICROGRAVITY
AB The three regimes of opposed-flow flame spread - radiative, thermal, and kinetic regimes - are well known. For thermally thin fuels, the spread rate is independent of opposing flow velocity in the thermal regime. It decreases with an increase in the flow velocity in the kinetic regime, leading to blow off extinction. In the radiative regime which occurs mostly in a buoyancy-free environment of microgravity, the spread rate decreases with a decrease in flow velocity leading to radiative extinction unless the oxygen level is very high. In a recent experiment aboard the International Space Station, thin sheets of PMMA were ignited in a flow tunnel with the opposing flow varying over a wide range. All three regimes of flame spread were captured in a single set of experiments for the first time. Instantaneous spread rates were obtained from digital video processing and compared with a computational model in all three regimes along with the evolution of flame shapes. Spread rates in the radiative and thermal regimes are also compared with existing theories of flame spread in the thermal and the radiative regime producing remarkable qualitative agreement. (C) 2016 by The Combustion Institute. Published by Elsevier Inc.
C1 [Bhattacharjee, Subrata; Simsek, Aslihan; Miller, Fletcher] San Diego State Univ, Mech Engn, San Diego, CA 92182 USA.
[Olson, Sandra; Ferkul, Paul] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Bhattacharjee, S (reprint author), San Diego State Univ, Mech Engn, San Diego, CA 92182 USA.
EM prof.bhattacharjee@gmail.com
FU NASA ISS Research Project Office [G00010752]
FX This work was funded by the NASA ISS Research Project Office (Grant No.
G00010752) with David Urban serving as the contract monitor. We want to
acknowledge the invaluable assistance of astronauts Reid Wiseman and
Alex Gerst, who ran these BASS-II experiments. We also acknowledge the
contribution of summer interns Laura Lima, Daniel Santos, and Neil
Bhattacharjee for processing the BASS data.
NR 20
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PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 1540-7489
EI 1873-2704
J9 P COMBUST INST
JI Proc. Combust. Inst.
PY 2017
VL 36
IS 2
BP 2963
EP 2969
DI 10.1016/j.proci.2016.06.025
PG 7
WC Thermodynamics; Energy & Fuels; Engineering, Chemical; Engineering,
Mechanical
SC Thermodynamics; Energy & Fuels; Engineering
GA EP5ZY
UT WOS:000397458900149
ER
PT J
AU Zhao, X
Liao, YTT
Johnston, MC
T'ien, JS
Ferkul, PV
Olson, SL
AF Zhao, Xiaoyang
Liao, Ya-Ting T.
Johnston, Michael C.
T'ien, James S.
Ferkul, Paul V.
Olson, Sandra L.
TI Concurrent flame growth, spread, and quenching over composite fabric
samples in low speed purely forced flow in microgravity
SO PROCEEDINGS OF THE COMBUSTION INSTITUTE
LA English
DT Article
DE Concurrent flame spread in forced flow; Microgravity combustion;
Quenching extinction; Solid flammability boundary; Material flammability
ID MODEL; FUEL
AB Flame growth, spread, and quenching extinction over a thin composite cotton-fiberglass fabric blend (referred to as the SIBAL fabric) were studied in low-speed concurrent purely forced flows aboard the International Space Station. The tests were conducted in a small flow duct within the Microgravity Science Glovebox. The fuel samples measured 1.2 and 2.2 cm wide and 10 cm long. Ambient oxygen was varied from 21% down to 16% molar concentration and flow speed from 55 cm/s down to 1 cm/s. A slow purely forced flow resulted in a small flame, enabling us to observe the entire history of flame development including ignition, flame growth, steady spread (in some cases), and decay at the end of the sample. In addition, by decreasing flow velocity during some of the tests, low-speed flame quenching extinction limits were determined as a function of oxygen percentage. The quenching speeds were found to be between 1 and 5 cm/s with higher extinction speeds in lower oxygen atmospheres. The shape of the quenching boundary supports the prediction by earlier theoretical models. These long duration microgravity experiments provide a rare opportunity for solid fuel combustion since microgravity time in ground-based facilities is generally not sufficient. This is the first time that a low-speed quenching boundary in concurrent spread is mapped in a clean and unambiguous manner. A previously developed three-dimensional transient model is modified to compare with the experiment. The modification includes the use of two-step SIBAL fabric pyrolysis kinetics where the rate constants are determined using Thermo-Gravimetric Analysis data. The model yields good quantitative comparison on the quenching boundary, the flame transient development, and the steady flame spread rates. (C) 2016 by The Combustion Institute. Published by Elsevier Inc.
C1 [Zhao, Xiaoyang; Liao, Ya-Ting T.; Johnston, Michael C.; T'ien, James S.] Case Western Reserve Univ, Dept Mech & Aerosp Engn, Cleveland, OH 44106 USA.
[Ferkul, Paul V.] Univ Space Res Assoc, Cleveland, OH 44135 USA.
[Olson, Sandra L.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP T'ien, JS (reprint author), Case Western Reserve Univ, Dept Mech & Aerosp Engn, Cleveland, OH 44106 USA.
EM jst2@case.edu
FU NASA; Underwriters Laboratories
FX This research was funded by NASA. YTL would like to acknowledge the
support from Underwriters Laboratories. We would like to thank Jay
Owens, Tibor Lorik, and Chuck Bunnell for engineering support and ISS
crew members Don Pettit, Sunita Williams, Chris Cassidy, Alexander
Gerst, and Reid Wiseman for conducting this experiment. This paper is
dedicated to the memory of Xiaoyang Zhao, our lead author, who left us
prematurely.
NR 16
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 1540-7489
EI 1873-2704
J9 P COMBUST INST
JI Proc. Combust. Inst.
PY 2017
VL 36
IS 2
BP 2971
EP 2978
DI 10.1016/j.proci.2016.06.028
PG 8
WC Thermodynamics; Energy & Fuels; Engineering, Chemical; Engineering,
Mechanical
SC Thermodynamics; Energy & Fuels; Engineering
GA EP5ZY
UT WOS:000397458900150
ER
PT J
AU McKinnell, S
Seki, MP
Ichii, T
AF McKinnell, Skip
Seki, Michael P.
Ichii, Taro
TI Special issue on the advances in understanding of the North Pacific
subtropical front ecosystem Preface
SO PROGRESS IN OCEANOGRAPHY
LA English
DT Editorial Material
ID LONGLINE FISHING GROUNDS; OCEANOGRAPHIC REGIME; OCEAN; ZONE
C1 [McKinnell, Skip] Salmoforsk Int Environm Consulting, 2280 Brighton Ave, Victoria, BC V8S 2G2, Canada.
[Seki, Michael P.] NOAA, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, 1845 Wasp Blvd,Bldg 176, Honolulu, HI 96818 USA.
[Ichii, Taro] Japan Fisheries Res & Educ Agcy, Natl Res Inst Far Seas Fisheries, Kanazawa Ku, 2-12-4 Fukuura, Yokohama, Kanagawa 2368648, Japan.
RP McKinnell, S (reprint author), Salmoforsk Int Environm Consulting, 2280 Brighton Ave, Victoria, BC V8S 2G2, Canada.
EM mckinnell@shaw.ca; Michael.Seki@noaa.gov; ichii@affrc.go.jp
NR 21
TC 0
Z9 0
U1 0
U2 0
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0079-6611
J9 PROG OCEANOGR
JI Prog. Oceanogr.
PD JAN
PY 2017
VL 150
SI SI
BP 1
EP 2
DI 10.1016/j.pocean.2017.01.007
PG 2
WC Oceanography
SC Oceanography
GA EM3PQ
UT WOS:000395227500001
ER
PT J
AU McKinnell, S
Seki, MP
AF McKinnell, Skip
Seki, Michael P.
TI Arcane epipelagic fishes of the subtropical North Pacific and factors
associated with their distribution
SO PROGRESS IN OCEANOGRAPHY
LA English
DT Article
ID ZONE CHLOROPHYLL FRONT; NEON FLYING SQUID; INTERANNUAL VARIABILITY;
OMMASTREPHES-BARTRAMII; OCEAN
AB In 1992, a moratorium was declared by the United Nations. General Assembly to end the practice of large-scale pelagic driftnet fishing. During two years leading up to the moratorium, three scientific research and fishery observer programs involving Canada, Japan, Korea, China-Taipei and the United States had collected significant amounts of information about the distribution and abundance of the epipelagic fauna in the subtropical North Pacific Ocean. The pan-regional distributions of the fishes in 1990 and 1991, most of which were taken as bycatch in 9910 fishing operations (357,150 km of driftnet) are described. More species were observed per fishing operation in 1991 than in 1990. Principal coordinate analysis of the incidence of the commonly caught fish species was used to show that, except for an anomaly in the region of the Shatsky Rise (165 degrees E), the composition of the catch changed from the coast of Japan across more than 6000 km to the eastern boundary of the fishery (145 degrees W). The analysis suggested that the fish species composition changed rather little with increasing latitude within the southern part of the domain (25-35 degrees N), before changing more rapidly north of the Kuroshio Extension region to a more subarctic, transition zone fauna. (C) 2016 Published by Elsevier Ltd.
C1 [McKinnell, Skip] North Pacific Marine Sci Org, Inst Ocean Sci, 9860 West Saanich Rd, Patricia Bay, BC, Canada.
[Seki, Michael P.] NOAA, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, IRC, 1845 Wasp Blvd,Bldg 176, Honolulu, HI 96818 USA.
[McKinnell, Skip] Salmoforsk Int, Victoria, BC, Canada.
RP McKinnell, S (reprint author), North Pacific Marine Sci Org, Inst Ocean Sci, 9860 West Saanich Rd, Patricia Bay, BC, Canada.
NR 31
TC 0
Z9 0
U1 0
U2 0
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0079-6611
J9 PROG OCEANOGR
JI Prog. Oceanogr.
PD JAN
PY 2017
VL 150
SI SI
BP 48
EP 61
DI 10.1016/j.pocean.2016.07.008
PG 14
WC Oceanography
SC Oceanography
GA EM3PQ
UT WOS:000395227500006
ER
PT J
AU Durgonics, T
Komjathy, A
Verkhoglyadova, O
Shume, EB
Benzon, HH
Mannucci, AJ
Butala, MD
Hoeg, P
Langley, RB
AF Durgonics, Tibor
Komjathy, Attila
Verkhoglyadova, Olga
Shume, Esayas B.
Benzon, Hans-Henrik
Mannucci, Anthony J.
Butala, Mark D.
Hoeg, Per
Langley, Richard B.
TI Multiinstrument observations of a geomagnetic storm and its effects on
the Arctic ionosphere: A case study of the 19 February 2014 storm
SO RADIO SCIENCE
LA English
DT Article
ID TOTAL ELECTRON-CONTENT; E-POP MISSION; POLAR-CAP; SPACE WEATHER;
NOVEMBER 2003; RING CURRENT; GPS; PHASE; SCINTILLATIONS; TIMED/GUVI
AB We present a multiinstrumented approach for the analysis of the Arctic ionosphere during the 19 February 2014 highly complex, multiphase geomagnetic storm, which had the largest impact on the disturbance storm-time index that year. The geomagnetic storm was the result of two powerful Earth-directed coronal mass ejections (CMEs). It produced a strong long lasting negative storm phase over Greenland with a dominant energy input in the polar cap. We employed global navigation satellite system (GNSS) networks, geomagnetic observatories, and a specific ionosonde station in Greenland. We complemented the approach with spaceborne measurements in order to map the state and variability of the Arctic ionosphere. In situ observations from the Canadian CASSIOPE (CAScade, Smallsat and IOnospheric Polar Explorer) satellite's ion mass spectrometer were used to derive ion flow data from the polar cap topside ionosphere during the event. Our research specifically found that (1) thermospheric O/N-2 measurements demonstrated significantly lower values over the Greenland sector than prior to the storm time. (2) An increased ion flow in the topside ionosphere was observed during the negative storm phase. (3) Negative storm phase was a direct consequence of energy input into the polar cap. (4) Polar patch formation was significantly decreased during the negative storm phase. This paper addresses the physical processes that can be responsible for this ionospheric storm development in the northern high latitudes. We conclude that ionospheric heating due to the CME's energy input caused changes in the polar atmosphere resulting in Ne upwelling, which was the major factor in high-latitude ionosphere dynamics for this storm.
C1 [Durgonics, Tibor; Benzon, Hans-Henrik; Hoeg, Per] Tech Univ Denmark, Natl Space Inst, Lyngby, Denmark.
[Durgonics, Tibor; Komjathy, Attila; Verkhoglyadova, Olga; Shume, Esayas B.; Mannucci, Anthony J.] NASA, Jet Prop Lab, Pasadena, CA USA.
[Komjathy, Attila; Langley, Richard B.] Univ New Brunswick, Dept Geodesy & Geomat Engn, Fredericton, NB, Canada.
[Shume, Esayas B.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Butala, Mark D.] Univ Illinois, Dept Elect & Comp Engn, Champaign, IL USA.
RP Durgonics, T (reprint author), Tech Univ Denmark, Natl Space Inst, Lyngby, Denmark.; Durgonics, T (reprint author), NASA, Jet Prop Lab, Pasadena, CA USA.
EM tibdu@space.dtu.dk
OI Durgonics, Tibor/0000-0002-9499-9585; Hoeg, Per/0000-0002-3172-5587
FU NRA ROSES 2014/A.26 GNSS Remote Sensing Science Team Award; NASA Mission
Operations and Data Analysis program; ESA [4000105775/2012/NL/WE,
4000112279/2014/D/MRP]; Natural Sciences and Engineering Research
Council of Canada; Canadian Space Agency
FX The authors wish to thank Lowell Digisonde International for providing
access to Thule Digisonde data used in this work; the Greenland GPS
Network (GNET) operated by the Technical University of Denmark, National
Space Institute (DTU Space) in cooperation with the American National
Science Foundation, Ohio State University, and the nonprofit university
governed consortium UNAVCO for GPS data; the Technical University of
Denmark, National Space Institute's Geomagnetism Section for
magnetometer observations; and NASA Jet Propulsion Laboratory for GIM
data processing. Portions of this work were done at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
NASA. NRA ROSES 2014/A.26 GNSS Remote Sensing Science Team Award is
gratefully acknowledged. The GUVI data used here were provided through
support from the NASA Mission Operations and Data Analysis program. The
GUVI instrument was designed and built by The Aerospace Corporation and
The Johns Hopkins University. The principal investigator is Andrew B.
Christensen and the chief scientist and co-PI is Larry J. Paxton. The
authors also acknowledge the use of SuperDARN convection data and
CASSIOPE IRM sensor data from e-POP. Tibor Durgonics gratefully
acknowledges partial funding support for his Ph.D. program provided by
activities in ESA contracts (4000105775/2012/NL/WE and
4000112279/2014/D/MRP). Richard B. Langley acknowledges funding support
from the Natural Sciences and Engineering Research Council of Canada and
the Canadian Space Agency. Data used in this paper can be obtained from
the authors.
NR 59
TC 0
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U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0048-6604
EI 1944-799X
J9 RADIO SCI
JI Radio Sci.
PD JAN
PY 2017
VL 52
IS 1
BP 146
EP 165
DI 10.1002/2016RS006106
PG 20
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
GA EO1TT
UT WOS:000396481500011
ER
PT B
AU Morgan, MA
AF Morgan, Matthew A.
BA Morgan, MA
BF Morgan, MA
TI Classical Absorptive Filters
SO REFLECTIONLESS FILTERS
SE Artech House Microwave Library
LA English
DT Article; Book Chapter
C1 [Morgan, Matthew A.] Lockheed Martin Fed Syst, Manassas, VA 20110 USA.
[Morgan, Matthew A.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Morgan, Matthew A.] Natl Radio Astron Observ, Cent Dev Lab, Charlottesville, VA 22903 USA.
[Morgan, Matthew A.] Green Bank Telescope, K Band Focal Plane Array Dev Project, Green Bank, WV 24944 USA.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band GHz Cryogen IF Amplifier Prod 6 211 275, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band Receiver Cartridge Testing 6, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band GHz 3 84 116, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band Orthomode Transducer OMT Prod 6, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] CDL, Integrated Receiver Dev Program, Charlottesville, VA 22903 USA.
RP Morgan, MA (reprint author), Lockheed Martin Fed Syst, Manassas, VA 20110 USA.; Morgan, MA (reprint author), NASA, Jet Prop Lab, Pasadena, CA 91109 USA.; Morgan, MA (reprint author), Natl Radio Astron Observ, Cent Dev Lab, Charlottesville, VA 22903 USA.; Morgan, MA (reprint author), Green Bank Telescope, K Band Focal Plane Array Dev Project, Green Bank, WV 24944 USA.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band GHz Cryogen IF Amplifier Prod 6 211 275, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band Receiver Cartridge Testing 6, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band GHz 3 84 116, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band Orthomode Transducer OMT Prod 6, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), CDL, Integrated Receiver Dev Program, Charlottesville, VA 22903 USA.
NR 12
TC 0
Z9 0
U1 0
U2 0
PU ARTECH HOUSE
PI NORWOOD
PA 685 CANTON ST, NORWOOD, MA 02062 USA
BN 978-1-63081-327-7
J9 ARTECH HSE MICROW LI
PY 2017
BP 35
EP 54
PG 20
WC Engineering, Electrical & Electronic; Physics, Applied;
Telecommunications
SC Engineering; Physics; Telecommunications
GA BH0XR
UT WOS:000396947600002
ER
PT B
AU Morgan, MA
AF Morgan, Matthew A.
BA Morgan, MA
BF Morgan, MA
TI Foundations of Reflectionless Filters
SO REFLECTIONLESS FILTERS
SE Artech House Microwave Library
LA English
DT Article; Book Chapter
C1 [Morgan, Matthew A.] Lockheed Martin Fed Syst, Manassas, VA 20110 USA.
[Morgan, Matthew A.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Morgan, Matthew A.] Natl Radio Astron Observ, Cent Dev Lab, Charlottesville, VA 22903 USA.
[Morgan, Matthew A.] Green Bank Telescope, K Band Focal Plane Array Dev Project, Green Bank, WV 24944 USA.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band GHz Cryogen IF Amplifier Prod 6 211 275, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band Receiver Cartridge Testing 6, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band GHz 3 84 116, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band Orthomode Transducer OMT Prod 6, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] CDL, Integrated Receiver Dev Program, Charlottesville, VA 22903 USA.
RP Morgan, MA (reprint author), Lockheed Martin Fed Syst, Manassas, VA 20110 USA.; Morgan, MA (reprint author), NASA, Jet Prop Lab, Pasadena, CA 91109 USA.; Morgan, MA (reprint author), Natl Radio Astron Observ, Cent Dev Lab, Charlottesville, VA 22903 USA.; Morgan, MA (reprint author), Green Bank Telescope, K Band Focal Plane Array Dev Project, Green Bank, WV 24944 USA.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band GHz Cryogen IF Amplifier Prod 6 211 275, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band Receiver Cartridge Testing 6, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band GHz 3 84 116, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band Orthomode Transducer OMT Prod 6, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), CDL, Integrated Receiver Dev Program, Charlottesville, VA 22903 USA.
NR 10
TC 0
Z9 0
U1 0
U2 0
PU ARTECH HOUSE
PI NORWOOD
PA 685 CANTON ST, NORWOOD, MA 02062 USA
BN 978-1-63081-327-7
J9 ARTECH HSE MICROW LI
PY 2017
BP 55
EP 80
PG 26
WC Engineering, Electrical & Electronic; Physics, Applied;
Telecommunications
SC Engineering; Physics; Telecommunications
GA BH0XR
UT WOS:000396947600003
ER
PT B
AU Morgan, MA
AF Morgan, Matthew A.
BA Morgan, MA
BF Morgan, MA
TI Subnetwork Expansion
SO REFLECTIONLESS FILTERS
SE Artech House Microwave Library
LA English
DT Article; Book Chapter
ID ABSORPTIVE BANDSTOP FILTER
C1 [Morgan, Matthew A.] Lockheed Martin Fed Syst, Manassas, VA 20110 USA.
[Morgan, Matthew A.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Morgan, Matthew A.] Natl Radio Astron Observ, Cent Dev Lab, Charlottesville, VA 22903 USA.
[Morgan, Matthew A.] Green Bank Telescope, K Band Focal Plane Array Dev Project, Green Bank, WV 24944 USA.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band GHz Cryogen IF Amplifier Prod 6 211 275, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band Receiver Cartridge Testing 6, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band GHz 3 84 116, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band Orthomode Transducer OMT Prod 6, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] CDL, Integrated Receiver Dev Program, Charlottesville, VA 22903 USA.
RP Morgan, MA (reprint author), Lockheed Martin Fed Syst, Manassas, VA 20110 USA.; Morgan, MA (reprint author), NASA, Jet Prop Lab, Pasadena, CA 91109 USA.; Morgan, MA (reprint author), Natl Radio Astron Observ, Cent Dev Lab, Charlottesville, VA 22903 USA.; Morgan, MA (reprint author), Green Bank Telescope, K Band Focal Plane Array Dev Project, Green Bank, WV 24944 USA.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band GHz Cryogen IF Amplifier Prod 6 211 275, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band Receiver Cartridge Testing 6, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band GHz 3 84 116, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band Orthomode Transducer OMT Prod 6, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), CDL, Integrated Receiver Dev Program, Charlottesville, VA 22903 USA.
NR 9
TC 0
Z9 0
U1 0
U2 0
PU ARTECH HOUSE
PI NORWOOD
PA 685 CANTON ST, NORWOOD, MA 02062 USA
BN 978-1-63081-327-7
J9 ARTECH HSE MICROW LI
PY 2017
BP 81
EP 105
PG 25
WC Engineering, Electrical & Electronic; Physics, Applied;
Telecommunications
SC Engineering; Physics; Telecommunications
GA BH0XR
UT WOS:000396947600004
ER
PT B
AU Morgan, MA
AF Morgan, Matthew A.
BA Morgan, MA
BF Morgan, MA
TI Duality Reduction
SO REFLECTIONLESS FILTERS
SE Artech House Microwave Library
LA English
DT Article; Book Chapter
C1 [Morgan, Matthew A.] Lockheed Martin Fed Syst, Manassas, VA 20110 USA.
[Morgan, Matthew A.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Morgan, Matthew A.] Natl Radio Astron Observ, Cent Dev Lab, Charlottesville, VA 22903 USA.
[Morgan, Matthew A.] Green Bank Telescope, K Band Focal Plane Array Dev Project, Green Bank, WV 24944 USA.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band GHz Cryogen IF Amplifier Prod 6 211 275, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band Receiver Cartridge Testing 6, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band GHz 3 84 116, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band Orthomode Transducer OMT Prod 6, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] CDL, Integrated Receiver Dev Program, Charlottesville, VA 22903 USA.
RP Morgan, MA (reprint author), Lockheed Martin Fed Syst, Manassas, VA 20110 USA.; Morgan, MA (reprint author), NASA, Jet Prop Lab, Pasadena, CA 91109 USA.; Morgan, MA (reprint author), Natl Radio Astron Observ, Cent Dev Lab, Charlottesville, VA 22903 USA.; Morgan, MA (reprint author), Green Bank Telescope, K Band Focal Plane Array Dev Project, Green Bank, WV 24944 USA.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band GHz Cryogen IF Amplifier Prod 6 211 275, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band Receiver Cartridge Testing 6, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band GHz 3 84 116, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band Orthomode Transducer OMT Prod 6, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), CDL, Integrated Receiver Dev Program, Charlottesville, VA 22903 USA.
NR 5
TC 0
Z9 0
U1 0
U2 0
PU ARTECH HOUSE
PI NORWOOD
PA 685 CANTON ST, NORWOOD, MA 02062 USA
BN 978-1-63081-327-7
J9 ARTECH HSE MICROW LI
PY 2017
BP 107
EP 120
PG 14
WC Engineering, Electrical & Electronic; Physics, Applied;
Telecommunications
SC Engineering; Physics; Telecommunications
GA BH0XR
UT WOS:000396947600005
ER
PT B
AU Morgan, MA
AF Morgan, Matthew A.
BA Morgan, MA
BF Morgan, MA
TI Generalized Reflectionless Filters
SO REFLECTIONLESS FILTERS
SE Artech House Microwave Library
LA English
DT Article; Book Chapter
C1 [Morgan, Matthew A.] Lockheed Martin Fed Syst, Manassas, VA 20110 USA.
[Morgan, Matthew A.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Morgan, Matthew A.] Natl Radio Astron Observ, Cent Dev Lab, Charlottesville, VA 22903 USA.
[Morgan, Matthew A.] Green Bank Telescope, K Band Focal Plane Array Dev Project, Green Bank, WV 24944 USA.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band GHz Cryogen IF Amplifier Prod 6 211 275, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band Receiver Cartridge Testing 6, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band GHz 3 84 116, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band Orthomode Transducer OMT Prod 6, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] CDL, Integrated Receiver Dev Program, Charlottesville, VA 22903 USA.
RP Morgan, MA (reprint author), Lockheed Martin Fed Syst, Manassas, VA 20110 USA.; Morgan, MA (reprint author), NASA, Jet Prop Lab, Pasadena, CA 91109 USA.; Morgan, MA (reprint author), Natl Radio Astron Observ, Cent Dev Lab, Charlottesville, VA 22903 USA.; Morgan, MA (reprint author), Green Bank Telescope, K Band Focal Plane Array Dev Project, Green Bank, WV 24944 USA.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band GHz Cryogen IF Amplifier Prod 6 211 275, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band Receiver Cartridge Testing 6, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band GHz 3 84 116, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band Orthomode Transducer OMT Prod 6, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), CDL, Integrated Receiver Dev Program, Charlottesville, VA 22903 USA.
NR 9
TC 0
Z9 0
U1 0
U2 0
PU ARTECH HOUSE
PI NORWOOD
PA 685 CANTON ST, NORWOOD, MA 02062 USA
BN 978-1-63081-327-7
J9 ARTECH HSE MICROW LI
PY 2017
BP 121
EP 152
PG 32
WC Engineering, Electrical & Electronic; Physics, Applied;
Telecommunications
SC Engineering; Physics; Telecommunications
GA BH0XR
UT WOS:000396947600006
ER
PT B
AU Morgan, MA
AF Morgan, Matthew A.
BA Morgan, MA
BF Morgan, MA
TI Transmission-Line Reflectionless Filters
SO REFLECTIONLESS FILTERS
SE Artech House Microwave Library
LA English
DT Article; Book Chapter
C1 [Morgan, Matthew A.] Lockheed Martin Fed Syst, Manassas, VA 20110 USA.
[Morgan, Matthew A.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Morgan, Matthew A.] Natl Radio Astron Observ, Cent Dev Lab, Charlottesville, VA 22903 USA.
[Morgan, Matthew A.] Green Bank Telescope, K Band Focal Plane Array Dev Project, Green Bank, WV 24944 USA.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band GHz Cryogen IF Amplifier Prod 6 211 275, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band Receiver Cartridge Testing 6, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band GHz 3 84 116, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band Orthomode Transducer OMT Prod 6, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] CDL, Integrated Receiver Dev Program, Charlottesville, VA 22903 USA.
RP Morgan, MA (reprint author), Lockheed Martin Fed Syst, Manassas, VA 20110 USA.; Morgan, MA (reprint author), NASA, Jet Prop Lab, Pasadena, CA 91109 USA.; Morgan, MA (reprint author), Natl Radio Astron Observ, Cent Dev Lab, Charlottesville, VA 22903 USA.; Morgan, MA (reprint author), Green Bank Telescope, K Band Focal Plane Array Dev Project, Green Bank, WV 24944 USA.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band GHz Cryogen IF Amplifier Prod 6 211 275, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band Receiver Cartridge Testing 6, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band GHz 3 84 116, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band Orthomode Transducer OMT Prod 6, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), CDL, Integrated Receiver Dev Program, Charlottesville, VA 22903 USA.
NR 10
TC 0
Z9 0
U1 0
U2 0
PU ARTECH HOUSE
PI NORWOOD
PA 685 CANTON ST, NORWOOD, MA 02062 USA
BN 978-1-63081-327-7
J9 ARTECH HSE MICROW LI
PY 2017
BP 153
EP 175
PG 23
WC Engineering, Electrical & Electronic; Physics, Applied;
Telecommunications
SC Engineering; Physics; Telecommunications
GA BH0XR
UT WOS:000396947600007
ER
PT B
AU Morgan, MA
AF Morgan, Matthew A.
BA Morgan, MA
BF Morgan, MA
TI Reflectionless Multiplexers
SO REFLECTIONLESS FILTERS
SE Artech House Microwave Library
LA English
DT Article; Book Chapter
C1 [Morgan, Matthew A.] Lockheed Martin Fed Syst, Manassas, VA 20110 USA.
[Morgan, Matthew A.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Morgan, Matthew A.] Natl Radio Astron Observ, Cent Dev Lab, Charlottesville, VA 22903 USA.
[Morgan, Matthew A.] Green Bank Telescope, K Band Focal Plane Array Dev Project, Green Bank, WV 24944 USA.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band GHz Cryogen IF Amplifier Prod 6 211 275, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band Receiver Cartridge Testing 6, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band GHz 3 84 116, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band Orthomode Transducer OMT Prod 6, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] CDL, Integrated Receiver Dev Program, Charlottesville, VA 22903 USA.
RP Morgan, MA (reprint author), Lockheed Martin Fed Syst, Manassas, VA 20110 USA.; Morgan, MA (reprint author), NASA, Jet Prop Lab, Pasadena, CA 91109 USA.; Morgan, MA (reprint author), Natl Radio Astron Observ, Cent Dev Lab, Charlottesville, VA 22903 USA.; Morgan, MA (reprint author), Green Bank Telescope, K Band Focal Plane Array Dev Project, Green Bank, WV 24944 USA.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band GHz Cryogen IF Amplifier Prod 6 211 275, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band Receiver Cartridge Testing 6, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band GHz 3 84 116, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band Orthomode Transducer OMT Prod 6, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), CDL, Integrated Receiver Dev Program, Charlottesville, VA 22903 USA.
NR 6
TC 0
Z9 0
U1 0
U2 0
PU ARTECH HOUSE
PI NORWOOD
PA 685 CANTON ST, NORWOOD, MA 02062 USA
BN 978-1-63081-327-7
J9 ARTECH HSE MICROW LI
PY 2017
BP 177
EP 189
PG 13
WC Engineering, Electrical & Electronic; Physics, Applied;
Telecommunications
SC Engineering; Physics; Telecommunications
GA BH0XR
UT WOS:000396947600008
ER
PT B
AU Morgan, MA
AF Morgan, Matthew A.
BA Morgan, MA
BF Morgan, MA
TI Applications of Reflectionless Filters
SO REFLECTIONLESS FILTERS
SE Artech House Microwave Library
LA English
DT Article; Book Chapter
C1 [Morgan, Matthew A.] Lockheed Martin Fed Syst, Manassas, VA 20110 USA.
[Morgan, Matthew A.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Morgan, Matthew A.] Natl Radio Astron Observ, Cent Dev Lab, Charlottesville, VA 22903 USA.
[Morgan, Matthew A.] Green Bank Telescope, K Band Focal Plane Array Dev Project, Green Bank, WV 24944 USA.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band GHz Cryogen IF Amplifier Prod 6 211 275, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band Receiver Cartridge Testing 6, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band GHz 3 84 116, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band Orthomode Transducer OMT Prod 6, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] CDL, Integrated Receiver Dev Program, Charlottesville, VA 22903 USA.
RP Morgan, MA (reprint author), Lockheed Martin Fed Syst, Manassas, VA 20110 USA.; Morgan, MA (reprint author), NASA, Jet Prop Lab, Pasadena, CA 91109 USA.; Morgan, MA (reprint author), Natl Radio Astron Observ, Cent Dev Lab, Charlottesville, VA 22903 USA.; Morgan, MA (reprint author), Green Bank Telescope, K Band Focal Plane Array Dev Project, Green Bank, WV 24944 USA.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band GHz Cryogen IF Amplifier Prod 6 211 275, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band Receiver Cartridge Testing 6, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band GHz 3 84 116, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band Orthomode Transducer OMT Prod 6, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), CDL, Integrated Receiver Dev Program, Charlottesville, VA 22903 USA.
NR 17
TC 0
Z9 0
U1 0
U2 0
PU ARTECH HOUSE
PI NORWOOD
PA 685 CANTON ST, NORWOOD, MA 02062 USA
BN 978-1-63081-327-7
J9 ARTECH HSE MICROW LI
PY 2017
BP 191
EP 211
PG 21
WC Engineering, Electrical & Electronic; Physics, Applied;
Telecommunications
SC Engineering; Physics; Telecommunications
GA BH0XR
UT WOS:000396947600009
ER
PT B
AU Morgan, MA
AF Morgan, Matthew A.
BA Morgan, MA
BF Morgan, MA
TI Tools for Advanced Topology Creation
SO REFLECTIONLESS FILTERS
SE Artech House Microwave Library
LA English
DT Article; Book Chapter
C1 [Morgan, Matthew A.] Lockheed Martin Fed Syst, Manassas, VA 20110 USA.
[Morgan, Matthew A.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Morgan, Matthew A.] Natl Radio Astron Observ, Cent Dev Lab, Charlottesville, VA 22903 USA.
[Morgan, Matthew A.] Green Bank Telescope, K Band Focal Plane Array Dev Project, Green Bank, WV 24944 USA.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band GHz Cryogen IF Amplifier Prod 6 211 275, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band Receiver Cartridge Testing 6, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band GHz 3 84 116, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] Atacama Large Millimeter Array ALMA, Band Orthomode Transducer OMT Prod 6, San Pedro De Atacama, Chile.
[Morgan, Matthew A.] CDL, Integrated Receiver Dev Program, Charlottesville, VA 22903 USA.
RP Morgan, MA (reprint author), Lockheed Martin Fed Syst, Manassas, VA 20110 USA.; Morgan, MA (reprint author), NASA, Jet Prop Lab, Pasadena, CA 91109 USA.; Morgan, MA (reprint author), Natl Radio Astron Observ, Cent Dev Lab, Charlottesville, VA 22903 USA.; Morgan, MA (reprint author), Green Bank Telescope, K Band Focal Plane Array Dev Project, Green Bank, WV 24944 USA.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band GHz Cryogen IF Amplifier Prod 6 211 275, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band Receiver Cartridge Testing 6, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band GHz 3 84 116, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), Atacama Large Millimeter Array ALMA, Band Orthomode Transducer OMT Prod 6, San Pedro De Atacama, Chile.; Morgan, MA (reprint author), CDL, Integrated Receiver Dev Program, Charlottesville, VA 22903 USA.
NR 7
TC 0
Z9 0
U1 0
U2 0
PU ARTECH HOUSE
PI NORWOOD
PA 685 CANTON ST, NORWOOD, MA 02062 USA
BN 978-1-63081-327-7
J9 ARTECH HSE MICROW LI
PY 2017
BP 213
EP 230
PG 18
WC Engineering, Electrical & Electronic; Physics, Applied;
Telecommunications
SC Engineering; Physics; Telecommunications
GA BH0XR
UT WOS:000396947600010
ER
PT J
AU Croll, A
Markert, J
Volz, M
Ostrogorsky, A
AF Croll, Arne
Markert, Jochen
Volz, Martin
Ostrogorsky, Aleksandar
TI Wetting angles of monovalent indium iodide on different substrates
SO CRYSTAL RESEARCH AND TECHNOLOGY
LA English
DT Article
DE Indium iodide; wetting; radiation detector
ID GERMANIUM-CRYSTALS; GROWTH
AB Wetting angles of molten Indium monoiodide (InI) on two different substrates, fused silica and pyrolytic boron nitride (pBN), were measured and compared to literature values for carbon and ceramic aluminum oxide. pBN showed the highest value of 128.5 degrees, versus 105 degrees for fused silica. The latter also showed a strong decrease with temperature, similar to aluminium oxide. From the wetting angles and the known surface tension, the work of adhesion for both substrates was determined. A reaction of the pBN with InI precludes its use as a crucible, however, leaving fused silica as the best crucible choice.
C1 [Croll, Arne] Univ Alabama, RSESC, VBRH M65,301 Sparkman Dr, Huntsville, AL 35899 USA.
[Croll, Arne; Markert, Jochen] Univ Freiburg, Kristallog, Hermann Herder Str 5, D-79104 Freiburg, Germany.
[Volz, Martin] NASA, Marshall Space Flight Ctr, EM 31, Huntsville, AL 35812 USA.
[Ostrogorsky, Aleksandar] IIT, MMAE, Chicago, IL 60616 USA.
RP Croll, A (reprint author), Univ Alabama, RSESC, VBRH M65,301 Sparkman Dr, Huntsville, AL 35899 USA.; Croll, A (reprint author), Univ Freiburg, Kristallog, Hermann Herder Str 5, D-79104 Freiburg, Germany.
EM arne.croell@uah.edu
NR 22
TC 0
Z9 0
U1 0
U2 0
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA POSTFACH 101161, 69451 WEINHEIM, GERMANY
SN 0232-1300
EI 1521-4079
J9 CRYST RES TECHNOL
JI Cryst. Res. Technol.
PD JAN
PY 2017
VL 52
IS 1
SI SI
AR UNSP 1600179
DI 10.1002/crat.201600179
PG 5
WC Crystallography
SC Crystallography
GA EN9ZX
UT WOS:000396359200007
ER
PT J
AU Khazanov, GV
Boardsen, S
Krivorutsky, EN
Engebretson, MJ
Sibeck, D
Chen, S
Breneman, A
AF Khazanov, G. V.
Boardsen, S.
Krivorutsky, E. N.
Engebretson, M. J.
Sibeck, D.
Chen, S.
Breneman, A.
TI Lower hybrid frequency range waves generated by ion polarization drift
due to electromagnetic ion cyclotron waves: Analysis of an event
observed by the Van Allen Probe B
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE wave; wave interactions; nonlinear phenomena; parametric processes
ID PLASMA; INSTABILITY; EXCITATION; TURBULENCE; REGION; ACCELERATION;
OSCILLATIONS
AB We analyze a wave event that occurred near noon between 07:03 and 07:08 UT on 23 February 2014 detected by the Van Allen Probes B spacecraft, where waves in the lower hybrid frequency range (LHFR) and electromagnetic ion cyclotron (EMIC) waves are observed to be highly correlated, with Pearson correlation coefficient of similar to 0.86. We assume that the correlation is the result of LHFR wave generation by the ions' polarization drift in the electric field of the EMIC waves. To check this assumption the drift velocities of electrons and H+, He+, and O+ ions in the measured EMIC wave electric field were modeled. Then the LHFR wave linear instantaneous growth rates for plasma with these changing drift velocities and different plasma compositions were calculated. The time distribution of these growth rates, their frequency distribution, and the frequency dependence of the ratio of the LHFR wave power spectral density (PSD) parallel and perpendicular to the ambient magnetic field to the total PSD were found. These characteristics of the growth rates were compared with the corresponding characteristics of the observed LHFR activity. Reasonable agreement between these features and the strong correlation between EMIC and LHFR energy densities support the assumption that the LHFR wave generation can be caused by the ions' polarization drift in the electric field of an EMIC wave.
C1 [Khazanov, G. V.; Sibeck, D.; Chen, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Boardsen, S.] Univ Maryland, Goddard Planetary Heliophys Inst, Baltimore, MD 21201 USA.
[Krivorutsky, E. N.] Prime Circuits Inc, NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Engebretson, M. J.] Augsburg Coll, Dept Phys, Minneapolis, MN USA.
[Breneman, A.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN USA.
RP Krivorutsky, EN (reprint author), Prime Circuits Inc, NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
EM george.v.khazanov@nasa.gov; krivorutskye@hotmail.com
FU NASA the Van Allen Probes Project; NASA [NAS5-01072]; NASA LWS Program
FX Funding support for this study was provided by NASA the Van Allen Probes
(formerly known as the Radiation Belt Storm Probes (RBSP)) Project,
including NASA prime contract NAS5-01072, and NASA LWS Program. The data
for this paper are available from George V. Khazanov at george.
v.khazanov@ nasa. gov.The EMFISIS data from the Van Allen Probes are
available at http:// emfisis. physics.uiowa.edu/. The Van Allen Probes
EFW data are available at http://www.space.umn.edu/missions/
rbspefw-home-university-of-minnesota/. OMNI data are available at the
NASA/GSFC's Space Physics Data Facility's CDAWeb, at http://cdaweb.
gsfc.nasa.gov/istp_public/. We acknowledge use of these data.
NR 33
TC 0
Z9 0
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PY 2017
VL 122
IS 1
BP 449
EP 463
DI 10.1002/2016JA022814
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EM9UE
UT WOS:000395655800033
ER
PT J
AU Graham, DB
Khotyaintsev, YV
Norgren, C
Vaivads, A
Andre, M
Toledo-Redondo, S
Lindqvist, PA
Marklund, GT
Ergun, RE
Paterson, WR
Gershman, DJ
Giles, BL
Pollock, CJ
Dorelli, JC
Avanov, LA
Lavraud, B
Saito, Y
Magnes, W
Russell, CT
Strangeway, RJ
Torbert, RB
Burch, JL
AF Graham, D. B.
Khotyaintsev, Yu. V.
Norgren, C.
Vaivads, A.
Andre, M.
Toledo-Redondo, S.
Lindqvist, P. -A.
Marklund, G. T.
Ergun, R. E.
Paterson, W. R.
Gershman, D. J.
Giles, B. L.
Pollock, C. J.
Dorelli, J. C.
Avanov, L. A.
Lavraud, B.
Saito, Y.
Magnes, W.
Russell, C. T.
Strangeway, R. J.
Torbert, R. B.
Burch, J. L.
TI Lower hybrid waves in the ion diffusion and magnetospheric inflow
regions
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE Magnetic reconnection; Ion diffusion region; Lower hybrid waves
ID MAGNETIC RECONNECTION; EARTHS MAGNETOPAUSE; DRIFT INSTABILITY;
ASYMMETRIC RECONNECTION; PLASMA ACCELERATION; ELECTRIC-FIELD; FREQUENCY;
MMS
AB The role and properties of lower hybrid waves in the ion diffusion region and magnetospheric inflow region of asymmetric reconnection are investigated using the Magnetospheric Multiscale (MMS) mission. Two distinct groups of lower hybrid waves are observed in the ion diffusion region and magnetospheric inflow region, which have distinct properties and propagate in opposite directions along the magnetopause. One group develops near the ion edge in the magnetospheric inflow, where magnetosheath ions enter the magnetosphere through the finite gyroradius effect and are driven by the ion-ion cross-field instability due to the interaction between the magnetosheath ions and cold magnetospheric ions. This leads to heating of the cold magnetospheric ions. The second group develops at the sharpest density gradient, where the Hall electric field is observed and is driven by the lower hybrid drift instability. These drift waves produce cross-field particle diffusion, enabling magnetosheath electrons to enter the magnetospheric inflow region thereby broadening the density gradient in the ion diffusion region.
C1 [Graham, D. B.; Khotyaintsev, Yu. V.; Norgren, C.; Vaivads, A.; Andre, M.] Swedish Inst Space Phys, Uppsala, Sweden.
[Norgren, C.] Uppsala Univ, Dept Phys & Astron, Uppsala, Sweden.
[Toledo-Redondo, S.] European Space Agcy ESAC, Madrid, Spain.
[Lindqvist, P. -A.; Marklund, G. T.] KTH Royal Inst Technol, Sch Elect Engn, Space & Plasma Phys, Stockholm, Sweden.
[Ergun, R. E.] Univ Colorado Boulder, Lab Atmospher & Space Phys, Boulder, CO USA.
[Paterson, W. R.; Gershman, D. J.; Giles, B. L.; Pollock, C. J.; Dorelli, J. C.; Avanov, L. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Gershman, D. J.; Avanov, L. A.] Univ Maryland, Dept Astron, College Pk, MD USA.
[Lavraud, B.] Univ Toulouse UPS, Inst Rech Astrophys & Plantol, Toulouse, France.
[Lavraud, B.] Ctr Natl Rech Sci, Toulouse, France.
[Saito, Y.] JAXA, Inst Space & Aeronaut Sci, Sagamihara, Kanagawa, Japan.
[Magnes, W.] Austrian Acad Sci, Space Res Inst, Graz, Austria.
[Russell, C. T.; Strangeway, R. J.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA USA.
[Torbert, R. B.] Univ New Hampshire, Ctr Space Sci, Durham, NH USA.
[Burch, J. L.] Southwest Res Inst, San Antonio, TX USA.
RP Graham, DB (reprint author), Swedish Inst Space Phys, Uppsala, Sweden.
EM dgraham@irfu.se
FU Swedish National Space Board [175/15]
FX We thank the entire MMS team and instrument PIs for data access and
support. We thank the SCM team for the high-quality magnetic field data.
This work was supported by the Swedish National Space Board, grant
175/15. MMS data are available at
https://lasp.colorado.edu/mms/sdc/public.
NR 51
TC 1
Z9 1
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PY 2017
VL 122
IS 1
BP 517
EP 533
DI 10.1002/2016JA023572
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EM9UE
UT WOS:000395655800038
ER
PT J
AU Halekas, JS
Ruhunusiri, S
Harada, Y
Collinson, G
Mitchell, DL
Mazelle, C
McFadden, JP
Connerney, JEP
Espley, JR
Eparvier, F
Luhmann, JG
Jakosky, BM
AF Halekas, J. S.
Ruhunusiri, S.
Harada, Y.
Collinson, G.
Mitchell, D. L.
Mazelle, C.
McFadden, J. P.
Connerney, J. E. P.
Espley, J. R.
Eparvier, F.
Luhmann, J. G.
Jakosky, B. M.
TI Structure, dynamics, and seasonal variability of the Mars-solar wind
interaction: MAVEN Solar Wind Ion Analyzer in-flight performance and
science results
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE Mars; solar wind
ID MARTIAN BOW SHOCK; QUASI-PARALLEL SHOCKS; HOT FLOW ANOMALIES;
DIAMAGNETIC CAVITIES UPSTREAM; AMPLITUDE MAGNETIC-STRUCTURES; PILE-UP
BOUNDARY; GLOBAL-SURVEYOR; PHOBOS OBSERVATIONS; CROSS-HELICITY; ALFVEN
WAVES
AB We report on the in-flight performance of the Solar Wind Ion Analyzer (SWIA) and observations of the Mars-solar wind interaction made during the Mars Atmosphere and Volatile EvolutioN (MAVEN) prime mission and a portion of its extended mission, covering 0.85 Martian years. We describe the data products returned by SWIA and discuss the proper handling of measurements made with different mechanical attenuator states and telemetry modes, and the effects of penetrating and scattered backgrounds, limited phase space coverage, and multi-ion populations on SWIA observations. SWIA directly measures solar wind protons and alpha particles upstream from Mars. SWIA also provides proxy measurements of solar wind and neutral densities based on products of charge exchange between the solar wind and the hydrogen corona. Together, upstream and proxy observations provide a complete record of the solar wind experienced by Mars, enabling organization of the structure, dynamics, and ion escape from the magnetosphere. We observe an interaction that varies with season and solar wind conditions. Solar wind dynamic pressure, Mach number, and extreme ultraviolet flux all affect the bow shock location. We confirm the occurrence of order-of-magnitude seasonal variations of the hydrogen corona. We find that solar wind Alfven waves, which provide an additional energy input to Mars, vary over the mission. At most times, only weak mass loading occurs upstream from the bow shock. However, during periods with near-radial interplanetary magnetic fields, structures consistent with Short Large Amplitude Magnetic Structures and their wakes form upstream, dramatically reconfiguring the Martian bow shock and magnetosphere.
C1 [Halekas, J. S.; Ruhunusiri, S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA USA.
[Harada, Y.; Mitchell, D. L.; McFadden, J. P.; Luhmann, J. G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA USA.
[Collinson, G.; Connerney, J. E. P.; Espley, J. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Mazelle, C.] Inst Rech Astrophys & Planetol, Toulouse, France.
[Eparvier, F.; Jakosky, B. M.] Univ Colorado Boulder, Lab Atmospher & Space Phys, Boulder, CO USA.
RP Halekas, JS (reprint author), Univ Iowa, Dept Phys & Astron, Iowa City, IA USA.
EM jasper-halekas@uiowa.edu
OI Halekas, Jasper/0000-0001-5258-6128
FU CNES
FX Analysis of SWEA data was partially supported by CNES. All MAVEN data
are publicly available through the Planetary Data System
(http://ppi.pds.nasa.gov). We thank two reviewers for carefully reading
this long paper and providing constructive feedback that improved the
manuscript.
NR 130
TC 7
Z9 7
U1 1
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PY 2017
VL 122
IS 1
BP 547
EP 578
DI 10.1002/2016JA023167
PG 32
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EM9UE
UT WOS:000395655800040
ER
PT J
AU Ruhunusiri, S
Halekas, JS
Espley, JR
Mazelle, C
Brain, D
Harada, Y
DiBraccio, GA
Livi, R
Larson, DE
Mitchell, DL
Jakosky, BM
Howes, GG
AF Ruhunusiri, Suranga
Halekas, J. S.
Espley, J. R.
Mazelle, C.
Brain, D.
Harada, Y.
DiBraccio, G. A.
Livi, R.
Larson, D. E.
Mitchell, D. L.
Jakosky, B. M.
Howes, G. G.
TI Characterization of turbulence in the Mars plasma environment with MAVEN
observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID MAGNETIC-FIELD FLUCTUATIONS; LOW-FREQUENCY WAVES; SOLAR-WIND;
MAGNETOHYDRODYNAMIC TURBULENCE; MARTIAN MAGNETOSPHERE; BOW SHOCK;
INTERSTELLAR TURBULENCE; ALFVENIC TURBULENCE; MAG/ER OBSERVATIONS;
CYCLOTRON WAVES
AB We characterize turbulence in the Mars plasma environment in a global scale for the first time by computing spectral indices for magnetic field fluctuations (slopes in the magnetic field power spectra) and determining how they vary with frequency and in different regions. In the magnetosheath, unlike in the solar wind, we find an absence of the inertial range which has a spectral index value equal to the Kolmogorov scaling value of -5/3. Instead, as observed in the magnetosheaths of other planets, we find that the spectral indices transition from low negative values close to -0.5 at low frequencies (< proton gyrofrequency) to values much lower than -5/3 at high frequencies (> proton gyrofrequency). This indicates that the pristine solar wind is modified at the Martian bow shock and that the fluctuations are dominated by locally generated fluctuations in the magnetosheath. The absence of spectral indices with the Kolmogorov scaling value indicates that the fluctuations in the magnetosheath do not have sufficient time to interact with one another leading to a fully developed energy cascade. Spectral index values near the Kolmogorov scaling value are observed for the low-frequency range near the magnetic pileup boundary, and this indicates the presence of fully developed energy cascade. In the wake, we find that the spectral indices have approximately the same values, typically near -2, for both the low-and high-frequency ranges. We observe seasonal variations of the spectral indices, mainly in the upstream region, which indicate the seasonal variations of the proton cyclotron waves.
C1 [Ruhunusiri, Suranga; Halekas, J. S.; Howes, G. G.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Espley, J. R.; DiBraccio, G. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Mazelle, C.] CNRS, IRAP, Toulouse, France.
[Mazelle, C.] Paul Sabatier Univ, Dept Phys, Toulouse, France.
[Brain, D.; Jakosky, B. M.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[Harada, Y.; Livi, R.; Larson, D. E.; Mitchell, D. L.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
RP Ruhunusiri, S (reprint author), Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
EM suranga-ruhunusiri@uiowa.edu
OI Halekas, Jasper/0000-0001-5258-6128
FU NASA; CNES; NASA Postdoctoral Program appointment at the NASA Goddard
Space Flight Center; NSF CAREER award [AGS-054061]
FX This work was supported by NASA. C. Mazelle was supported by CNES, and
G. A. DiBraccio was supported by a NASA Postdoctoral Program appointment
at the NASA Goddard Space Flight Center, administered by Universities
Space Research Association through a contract with NASA. G. Howes was
supported by NSF CAREER award AGS-054061. We thank J. E. P. Connerney
for the MAG data. MAVEN data are publicly available through the
Planetary Data System.
NR 83
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J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PY 2017
VL 122
IS 1
BP 656
EP 674
DI 10.1002/2016JA023456
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EM9UE
UT WOS:000395655800046
ER
PT J
AU Turner, DL
O'Brien, TP
Fennell, JF
Claudepierre, SG
Blake, JB
Jaynes, AN
Baker, DN
Kanekal, S
Gkioulidou, M
Henderson, MG
Reeves, GD
AF Turner, D. L.
O'Brien, T. P.
Fennell, J. F.
Claudepierre, S. G.
Blake, J. B.
Jaynes, A. N.
Baker, D. N.
Kanekal, S.
Gkioulidou, M.
Henderson, M. G.
Reeves, G. D.
TI Investigating the source of near-relativistic and relativistic electrons
in Earth's inner radiation belt
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID PHASE-SPACE DENSITY; GEOMAGNETIC STORMS; IMPENETRABLE BARRIER; ZEBRA
STRIPES; OUTER ZONE; ACCELERATION; ENERGY; DYNAMICS; PARTICLE;
MAGNETOSPHERE
AB Using observations from NASA's Van Allen Probes, we study the role of sudden particle enhancements at low L shells (SPELLS) as a source of inner radiation belt electrons. SPELLS events are characterized by electron intensity enhancements of approximately an order of magnitude or more in less than 1day at L<3. During quiet and average geomagnetic conditions, the phase space density radial distributions for fixed first and second adiabatic invariants are peaked at 2. This work was
primarily supported by funding from NASA (Van Allen Probes contract
NAS5-01072) and research supported by the International Space Science
Institute's International Teams program.
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J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PY 2017
VL 122
IS 1
BP 695
EP 710
DI 10.1002/2016JA023600
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EM9UE
UT WOS:000395655800048
ER
PT J
AU Remya, B
Reddy, RV
Tsurutani, BT
Lakhina, GS
AF Remya, B.
Reddy, R. V.
Tsurutani, B. T.
Lakhina, G. S.
TI Comment on "Effects of electron temperature anisotropy on proton mirror
instability evolution" by Ahmadi et al. (2016)
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID EARTHS BOW SHOCK; MAGNETIC-FIELD; LION ROARS; WAVES DOWNSTREAM;
SOLAR-WIND; MAGNETOSHEATH; SIMULATIONS; FLUCTUATIONS; DEPLETION; PLASMA
AB In a recent paper, Ahmadi et al. (2016) analyze the effect of electron temperature anisotropy on proton mirror instability. They find that the electron whistler instability grows faster and consumes all the available electron free energy so that no anisotropy is left to fuel the proton mirror mode growth. In this comment we present both observational and theoretical arguments about why we think this is incorrect.
C1 [Remya, B.] Acad Sinica, Inst Earth Sci, Taipei, Taiwan.
[Reddy, R. V.; Lakhina, G. S.] Indian Inst Geomagnetism, New Bombay, India.
[Tsurutani, B. T.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Remya, B (reprint author), Acad Sinica, Inst Earth Sci, Taipei, Taiwan.
EM remyaphysics@gmail.com
FU Academia Sinica in Taiwan; National Academy of Sciences, India under the
NASI-Senior Scientist Platinum Jubilee Fellowship Scheme
FX This work was supported by the Academia Sinica in Taiwan. G.S.L. thanks
the National Academy of Sciences, India for the support under the
NASI-Senior Scientist Platinum Jubilee Fellowship Scheme. Portions of
this research were performed at the Jet Propulsion Laboratory,
California Institute of Technology under contract with NASA.
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J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PY 2017
VL 122
IS 1
BP 745
EP 747
DI 10.1002/2016JA023148
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EM9UE
UT WOS:000395655800051
ER
PT J
AU Barrie, AC
Smith, SE
Dorelli, JC
Gershman, DJ
Yeh, P
Schiff, C
Avanov, LA
AF Barrie, A. C.
Smith, S. E.
Dorelli, J. C.
Gershman, D. J.
Yeh, P.
Schiff, C.
Avanov, L. A.
TI Performance of a space-based wavelet compressor for plasma count data on
the MMS Fast Plasma Investigation
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID IMAGES; JPEG
AB Data compression has been a staple of imaging instruments for years. Recently, plasma measurements have utilized compression with relatively low compression ratios. The Fast Plasma Investigation (FPI) on board the Magnetospheric Multiscale (MMS) mission generates data roughly 100 times faster than previous plasma instruments, requiring a higher compression ratio to fit within the telemetry allocation. This study investigates the performance of a space-based compression standard employing a Discrete Wavelet Transform and a Bit Plane Encoder (DWT/BPE) in compressing FPI plasma count data. Data from the first 6months of FPI operation are analyzed to explore the error modes evident in the data and how to adapt to them. While approximately half of the Dual Electron Spectrometer (DES) maps had some level of loss, it was found that there is little effect on the plasma moments and that errors present in individual sky maps are typically minor. The majority of Dual Ion Spectrometer burst sky maps compressed in a lossless fashion, with no error introduced during compression. Because of induced compression error, the size limit for DES burst images has been increased for Phase1B. Additionally, it was found that the floating point compression mode yielded better results when images have significant compression error, leading to floating point mode being used for the fast survey mode of operation for Phase1B. Despite the suggested tweaks, it was found that wavelet-based compression, and a DWT/BPE algorithm in particular, is highly suitable to data compression for plasma measurement instruments and can be recommended for future missions.
C1 [Barrie, A. C.; Smith, S. E.; Dorelli, J. C.; Gershman, D. J.; Yeh, P.; Schiff, C.; Avanov, L. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Barrie, A. C.] Aurora Engn, Towson, MD USA.
[Barrie, A. C.] Univ Colorado, Aerosp Engn Sci, Boulder, CO 80309 USA.
[Smith, S. E.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Gershman, D. J.; Avanov, L. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
RP Barrie, AC (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Barrie, AC (reprint author), Aurora Engn, Towson, MD USA.; Barrie, AC (reprint author), Univ Colorado, Aerosp Engn Sci, Boulder, CO 80309 USA.
EM alexander.c.barrie@nasa.gov
NR 13
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SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PY 2017
VL 122
IS 1
BP 765
EP 779
DI 10.1002/2016JA022645
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EM9UE
UT WOS:000395655800054
ER
PT J
AU Smith, AW
Slavin, JA
Jackman, CM
Fear, RC
Poh, GK
DiBraccio, GA
Jasinski, JM
Trenchi, L
AF Smith, A. W.
Slavin, J. A.
Jackman, C. M.
Fear, R. C.
Poh, G. -K.
DiBraccio, G. A.
Jasinski, J. M.
Trenchi, L.
TI Automated force-free flux rope identification
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID TRAVELING COMPRESSION REGIONS; COMPREHENSIVE MAGNETIC-FIELD;
MINIMUM-VARIANCE ANALYSIS; MESSENGER OBSERVATIONS; GEOTAIL OBSERVATIONS;
EARTHS MAGNETOTAIL; GEOMAGNETIC TAIL; CONSTANT-ALPHA; PLASMA SHEET;
MERCURYS
AB We describe a method developed to automatically identify quasi force-free magnetotail flux ropes from in situ spacecraft magnetometer data. The method locates significant (greater than 1 sigma) deflections of the north-south component of the magnetic field coincident with enhancements in other field components. The magnetic field data around the deflections are then processed using Minimum Variance Analysis (MVA) to narrow the selection down to those that exhibit the characteristics of flux ropes. The subset of candidates that fulfills the requirements are then compared to a cylindrical, linear (constant-) force-free model. Those that can be well approximated as force free are then accepted. The model fit also provides a measure of the physical parameters that describe the flux rope (i.e., core field and radius). This process allows for the creation of a repeatable, consistent catalog of flux ropes. Automation allows a greater volume of data to be covered, saving time and allowing the exploration of potential selection biases. The technique is applied to MESSENGER (MErcury Surface, Space ENvironment, GEochemistry, and Ranging) magnetometer data in the Hermean magnetotail and successfully locates flux ropes, some of which match previously known encounters. Assumptions of the method and potential future applications are discussed.
C1 [Smith, A. W.; Jackman, C. M.; Fear, R. C.; Trenchi, L.] Univ Southampton, Dept Phys & Astron, Southampton, Hants, England.
[Slavin, J. A.; Poh, G. -K.; Jasinski, J. M.] Univ Michigan, Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
[DiBraccio, G. A.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD USA.
RP Smith, AW (reprint author), Univ Southampton, Dept Phys & Astron, Southampton, Hants, England.
EM AW.Smith@soton.ac.uk
FU STFC Ernest Rutherford Fellowship [ST/L004399/1, ST/K004298/2,
ST/L002809/1]; NASA Postdoctoral Program appointment at the NASA Goddard
Space Flight Center
FX The data used in this study were available from the Planetary Data
System (PDS): http://pds.jpl.nasa.gov. A.W.S. is funded by a SEPnet PhD
studentship. C.M.J. is supported by STFC Ernest Rutherford Fellowship
ST/L004399/1. R.C.F. is supported by STFC Ernest Rutherford Fellowship
ST/K004298/2. G.A.D. is supported by a NASA Postdoctoral Program
appointment at the NASA Goddard Space Flight Center, administered by
Universities Space Research Association through a contract with NASA.
L.T. is supported by STFC Ernest Rutherford grant ST/L002809/1. Cluster
data used in this paper were downloaded from the European Space Agency's
Cluster and Double Star Science Archive
(http://www.cosmos.esa.int/web/csa/access). Geotail magnetic field
(electric field and/or plasma) data were provided by T. Nagai (H.
Hayakawa and/or Y. Saito) through DARTS at Institute of Space and
Astronautical Science, JAXA in Japan.
NR 65
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J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PY 2017
VL 122
IS 1
BP 780
EP 791
DI 10.1002/2016JA022994
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EM9UE
UT WOS:000395655800055
ER
PT J
AU Hara, T
Brain, DA
Mitchell, DL
Luhmann, JG
Seki, K
Hasegawa, H
Mcfadden, JP
Halekas, JS
Espley, JR
Harada, Y
Livi, R
DiBraccio, GA
Connerney, JEP
Mazelle, C
Andersson, L
Jakosky, BM
AF Hara, Takuya
Brain, David A.
Mitchell, David L.
Luhmann, Janet G.
Seki, Kanako
Hasegawa, Hiroshi
Mcfadden, James P.
Halekas, Jasper S.
Espley, Jared R.
Harada, Yuki
Livi, Roberto
DiBraccio, Gina A.
Connerney, John E. P.
Mazelle, Christian
Andersson, Laila
Jakosky, Bruce M.
TI MAVEN observations of a giant ionospheric flux rope near Mars resulting
from interaction between the crustal and interplanetary draped magnetic
fields
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE Mars; MAVEN; flux rope; Grad-Shafranov equation; ionosphere; ICME
ID SOLAR-WIND CONDITIONS; MESSENGER OBSERVATIONS; TRANSFER EVENTS; SPATIAL
STRUCTURE; VENUS IONOSPHERE; MAGNETOPAUSE; PLASMA; DAYSIDE;
RECONNECTION; MAGNETOSPHERE
AB We present Mars Atmosphere and Volatile EvolutioN (MAVEN) observations of a giant magnetic flux rope in the Martian dayside ionosphere. The flux rope was observed at an altitude of <300km, downstream from strong subsolar crustal magnetic fields. The peak field amplitude was approximate to 200nT, resulting in the largest difference between the observed magnetic field strength and a model for crustal magnetic fields of the entire MAVEN primary science phase. MAVEN detected planetary ions, including H+, O+, and O2+, across the structure. The axial orientation estimated for the flux rope indicates that it likely formed as a result of interactions between the local crustal and overlaid draped interplanetary magnetic fields. Pitch angle distributions of ionospheric photoelectrons imply that this structure is connected to the Martian upper atmosphere. However, the flux rope is not present in observations at the next commensurable orbit crossing (approximately two Martian days later), implying that it eventually detaches from the atmosphere and is carried downstream. The flux rope observations occurred during an interplanetary coronal mass ejection event at Mars, suggesting that the disturbed upstream state played a role in allowing the interplanetary magnetic field to penetrate deeper into the Martian ionosphere than is typical, allowing the formation of the flux rope.
C1 [Hara, Takuya; Mitchell, David L.; Luhmann, Janet G.; Mcfadden, James P.; Harada, Yuki; Livi, Roberto] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Brain, David A.; Andersson, Laila; Jakosky, Bruce M.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[Seki, Kanako] Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Tokyo, Japan.
[Hasegawa, Hiroshi] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa, Japan.
[Halekas, Jasper S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Espley, Jared R.; DiBraccio, Gina A.; Connerney, John E. P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Mazelle, Christian] CNRS, Inst Rech Astrophys & Planetol, Toulouse, France.
[Mazelle, Christian] Univ Paul Sabatier, Toulouse, France.
RP Hara, T (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM hara@ssl.berkeley.edu
OI Halekas, Jasper/0000-0001-5258-6128
FU CNES; NASA Postdoctoral Program
FX The MAVEN data used in this paper are publicly available in NASA's
Planetary Data System (http://ppi.pds.nasa.gov/mission/MAVEN). Analysis
of SWEA data was partially supported by CNES. T. Hara thanks C.O. Lee
for helpful discussions with respect to the space weather events
observed by MAVEN. G.A. DiBraccio was supported by a NASA Postdoctoral
Program appointment at the NASA Goddard Space Flight Center,
administered by Universities Space Research Association through a
contract with NASA. Simulation results have been provided by the
Community Coordinated Modeling Center at Goddard Space Flight Center
through their real-time runs system (http://ccmc.gsfc.nasa.gov). The WSA
model was developed by N. Arge at AFRL, and the ENLIL Model was
developed by D. Odstrcil at GMU.
NR 59
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SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PY 2017
VL 122
IS 1
BP 828
EP 842
DI 10.1002/2016JA023347
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EM9UE
UT WOS:000395655800059
ER
PT J
AU Steckiewicz, M
Garnier, P
Andre, N
Mitchell, DL
Andersson, L
Penou, E
Beth, A
Fedorov, A
Sauvaud, JA
Mazelle, C
Brain, DA
Espley, JR
McFadden, J
Halekas, JS
Larson, DE
Lillis, RJ
Luhmann, JG
Soobiah, Y
Jakosky, BM
AF Steckiewicz, M.
Garnier, P.
Andre, N.
Mitchell, D. L.
Andersson, L.
Penou, E.
Beth, A.
Fedorov, A.
Sauvaud, J. -A.
Mazelle, C.
Brain, D. A.
Espley, J. R.
McFadden, J.
Halekas, J. S.
Larson, D. E.
Lillis, R. J.
Luhmann, J. G.
Soobiah, Y.
Jakosky, B. M.
TI Comparative study of the Martian suprathermal electron depletions based
on Mars Global Surveyor, Mars Express, and Mars Atmosphere and Volatile
EvolutioN mission observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE Mars; MAVEN mission; MGS mission; MEX mission; nightside suprathermal
electron depletions
ID SOLAR-WIND; MAGNETIC-FIELD; ENVIRONMENT; IONOSPHERE; DEPENDENCE
AB Nightside suprathermal electron depletions have been observed at Mars by three spacecraft to date: Mars Global Surveyor, Mars Express, and the Mars Atmosphere and Volatile EvolutioN (MAVEN) mission. This spatial and temporal diversity of measurements allows us to propose here a comprehensive view of the Martian electron depletions through the first multispacecraft study of the phenomenon. We have analyzed data recorded by the three spacecraft from 1999 to 2015 in order to better understand the distribution of the electron depletions and their creation mechanisms. Three simple criteria adapted to each mission have been implemented to identify more than 134,500 electron depletions observed between 125 and 900km altitude. The geographical distribution maps of the electron depletions detected by the three spacecraft confirm the strong link existing between electron depletions and crustal magnetic field at altitudes greater than similar to 170km. At these altitudes, the distribution of electron depletions is strongly different in the two hemispheres, with a far greater chance to observe an electron depletion in the Southern Hemisphere, where the strongest crustal magnetic sources are located. However, the unique MAVEN observations reveal that below a transition region near 160-170km altitude the distribution of electron depletions is the same in both hemispheres, with no particular dependence on crustal magnetic fields. This result supports the suggestion made by previous studies that these low-altitudes events are produced through electron absorption by atmospheric CO2.
C1 [Steckiewicz, M.; Garnier, P.; Andre, N.; Penou, E.; Fedorov, A.; Sauvaud, J. -A.; Mazelle, C.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Steckiewicz, M.; Garnier, P.; Andre, N.; Penou, E.; Fedorov, A.; Sauvaud, J. -A.; Mazelle, C.] CNRS, IRAP, Toulouse, France.
[Mitchell, D. L.; McFadden, J.; Lillis, R. J.; Luhmann, J. G.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA USA.
[Andersson, L.; Brain, D. A.; Jakosky, B. M.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO USA.
[Beth, A.] Imperial Coll London, Dept Phys, London, England.
[Espley, J. R.; Soobiah, Y.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Halekas, J. S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA USA.
RP Steckiewicz, M (reprint author), Univ Toulouse, UPS OMP, IRAP, Toulouse, France.; Steckiewicz, M (reprint author), CNRS, IRAP, Toulouse, France.
EM morgane.steckiewicz@irap.omp.eu
OI Andersson, Laila/0000-0002-6384-7036
FU French Space Agency CNES; NASA through Mars Exploration Program; MAVEN
project; CNRS; CNES; Observatoire de Paris; Universite Paul Sabatier,
Toulouse, France
FX This work has been supported by the French Space Agency CNES for the
part based on observations obtained with the SWEA instrument on MAVEN.
The MAVEN project is supported by NASA through the Mars Exploration
Program. The authors acknowledge the support of the MAVEN project and
particularly of the instrument and science teams. Data analysis was
performed with the AMDA science analysis system (http://amda.cdpp.eu)
provided by the Centre de Donnees de la Physique des Plasmas CDPP
supported by CNRS; CNES; Observatoire de Paris; and Universite Paul
Sabatier, Toulouse, France. The MGS, MEX, and MAVEN data used in this
paper are publicly available through the Planetary Data System
(http://ppi.pds.nasa.gov/). The authors sincerely thank the two
anonymous reviewers for their constructive comments.
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J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PY 2017
VL 122
IS 1
BP 857
EP 873
DI 10.1002/2016JA023205
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EM9UE
UT WOS:000395655800061
ER
PT J
AU Vogt, MF
Withers, P
Fallows, K
Andersson, L
Girazian, Z
Mahaffy, PR
Benna, M
Elrod, MK
Connerney, JEP
Espley, JR
Eparvier, FG
Jakosky, BM
AF Vogt, Marissa F.
Withers, Paul
Fallows, Kathryn
Andersson, Laila
Girazian, Zachary
Mahaffy, Paul R.
Benna, Mehdi
Elrod, Meredith K.
Connerney, John E. P.
Espley, Jared R.
Eparvier, Frank G.
Jakosky, Bruce M.
TI MAVEN observations of dayside peak electron densities in the ionosphere
of Mars
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE Mars; ionosphere; planetary ionospheres; electron densities; electron
temperatures
ID PILE-UP BOUNDARY; MARTIAN IONOSPHERE; GLOBAL-SURVEYOR; MONOCHROMATIC
RADIATION; PROFILES ANALYSIS; GRAZING-INCIDENCE; MAGNETIC-FIELD;
ROTATING EARTH; ATMOSPHERE; TEMPERATURES
AB The peak electron density in the dayside Martian ionosphere is a valuable diagnostic of the state of the ionosphere. Its dependence on factors like the solar zenith angle, ionizing solar irradiance, neutral scale height, and electron temperature has been well studied. The Mars Atmosphere and Volatile EvolutioN spacecraft's September 2015 deep dip orbits, in which the orbital periapsis was lowered to similar to 125km, provided the first opportunity since Viking to sample in situ a complete dayside electron density profile including the main peak. Here we present peak electron density measurements from 37 deep dip orbits and describe conditions at the altitude of the main peak, including the electron temperature and composition of the ionosphere and neutral atmosphere. We find that the dependence of the peak electron density and the altitude of the main peak on solar zenith angle are well described by analytical photochemical theory. Additionally, we find that the electron temperatures at the main peak display a dependence on solar zenith angle that is consistent with the observed variability in the peak electron density. Several peak density measurements were made in regions of large crustal magnetic field, but there is no clear evidence that the crustal magnetic field strength influences the peak electron density, peak altitude, or electron temperature. Finally, we find that the fractional abundance of O-2(+) and CO2+ at the peak altitude is variable but that the two species together consistently represent similar to 95% of the total ion density.
C1 [Vogt, Marissa F.; Withers, Paul; Fallows, Kathryn] Boston Univ, Ctr Space Phys, Boston, MA USA.
[Withers, Paul] Boston Univ, Dept Astron, Boston, MA USA.
[Andersson, Laila; Eparvier, Frank G.; Jakosky, Bruce M.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO USA.
[Girazian, Zachary; Mahaffy, Paul R.; Benna, Mehdi; Elrod, Meredith K.; Connerney, John E. P.; Espley, Jared R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Benna, Mehdi] Univ Maryland, CRESST, Baltimore, MD USA.
[Elrod, Meredith K.] Univ Maryland, CRESST, College Pk, MD USA.
RP Vogt, MF (reprint author), Boston Univ, Ctr Space Phys, Boston, MA USA.
EM mvogt@bu.edu
OI Andersson, Laila/0000-0002-6384-7036
FU NASA [NNX13AO35G]
FX M.V. and P.W. were supported by NASA grant NNX13AO35G. Solar wind
proxies from MAVEN's SWIA instrument were kindly provided by Jasper
Halekas. We thank two anonymous reviewers for their helpful suggestions.
MAVEN data are available via the Planetary Plasma Interactions node of
NASA's Planetary Data System at http://ppi.pds.nasa.gov/.
NR 42
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J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PY 2017
VL 122
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BP 891
EP 906
DI 10.1002/2016JA023473
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EM9UE
UT WOS:000395655800063
ER
PT J
AU Hara, T
Luhmann, JG
Leblanc, F
Curry, SM
Seki, K
Brain, DA
Halekas, JS
Harada, Y
McFadden, JP
Livi, R
DiBraccio, GA
Connerney, JEP
Jakosky, BM
AF Hara, Takuya
Luhmann, Janet G.
Leblanc, Francois
Curry, Shannon M.
Seki, Kanako
Brain, David A.
Halekas, Jasper S.
Harada, Yuki
McFadden, James P.
Livi, Roberto
DiBraccio, Gina A.
Connerney, John E. P.
Jakosky, Bruce M.
TI MAVEN observations on a hemispheric asymmetry of precipitating ions
toward the Martian upper atmosphere according to the upstream solar wind
electric field
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE Mars; MAVEN; ion precipitation; hemispheric asymmetry; solar wind
dependence; sputtering
ID MARS EXPRESS; PROTON PRECIPITATION; MAGNETIC-FIELD; IMF DIRECTION;
ESCAPE; DISTRIBUTIONS; VENUS; DEPOSITION; MISSION; CONSEQUENCES
AB The Mars Atmosphere and Volatile Evolution (MAVEN) observations show that the global spatial distribution of ions precipitating toward the Martian upper atmosphere has a highly asymmetric pattern relative to the upstream solar wind electric field. MAVEN observations indicate that precipitating planetary heavy ion fluxes measured in the downward solar wind electric field (-E) hemisphere are generally larger than those measured in the upward electric field (+E) hemisphere, as expected from modeling. The -E (+E) hemispheres are defined by the direction of solar wind electric field pointing toward (or away from) the planet. On the other hand, such an asymmetric precipitating pattern relative to the solar wind electric field is less clear around the terminator. Strong precipitating fluxes are sometimes found even in the +E field hemisphere under either strong upstream solar wind dynamic pressure or strong interplanetary magnetic field periods. The results imply that those intense precipitating ion fluxes are observed when the gyroradii of pickup ions are estimated to be relatively small compared with the planetary scale. Therefore, the upstream solar wind parameters are important factors in controlling the global spatial pattern and flux of ions precipitating into the Martian upper atmosphere.
C1 [Hara, Takuya; Luhmann, Janet G.; Curry, Shannon M.; Harada, Yuki; McFadden, James P.; Livi, Roberto] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Leblanc, Francois] Univ Paris 06, CNRS, LATMOS IPSL, Paris, France.
[Seki, Kanako] Univ Tokyo, Grad Sch Sci, Dept Earth & Planetary Sci, Tokyo 1138654, Japan.
[Brain, David A.; Jakosky, Bruce M.] Univ Colorado Boulder, Lab Atmospher & Space Phys, Boulder, CO USA.
[Halekas, Jasper S.] Univ Iowa, Dept Phys & Astron, Iowa City, IA USA.
[DiBraccio, Gina A.; Connerney, John E. P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Hara, T (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM hara@ssl.berkeley.edu
OI Halekas, Jasper/0000-0001-5258-6128
FU NASA Postdoctoral Program appointment at the NASA Goddard Space Flight
Center
FX The MAVEN data used in this paper are publicly available in NASA's
Planetary Data System (http://ppi.pds.nasa.gov/mission/MAVEN). G. A.
DiBraccio was supported by a NASA Postdoctoral Program appointment at
the NASA Goddard Space Flight Center, administered by Universities Space
Research Association through a contract with NASA.
NR 49
TC 0
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U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PY 2017
VL 122
IS 1
BP 1083
EP 1101
DI 10.1002/2016JA023348
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EM9UE
UT WOS:000395655800076
ER
PT J
AU Liu, GP
England, S
Lillis, RJ
Mahaffy, PR
Elrod, M
Benna, M
Jakosky, B
AF Liu, Guiping
England, Scott
Lillis, Robert J.
Mahaffy, Paul R.
Elrod, Meredith
Benna, Mehdi
Jakosky, Bruce
TI Longitudinal structures in Mars' upper atmosphere as observed by
MAVEN/NGIMS
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE atmospheric tides; longitudinal tidal structure; thermosphere variation;
planetary-scale waves; upper atmosphere; non-migrating tides
ID ELECTRON-DENSITY PROFILES; GLOBAL SURVEYOR; NONMIGRATING TIDES; NEUTRAL
ATMOSPHERE; ACCELEROMETER DATA; MGS ACCELEROMETER; THERMAL TIDES;
IN-SITU; TEMPERATURE; OCCULTATION
AB Here we report the first comprehensive study of longitudinal structures in Mars' neutral upper atmosphere associated with atmospheric tides in composition, density and temperature using the Mars Atmosphere and Volatile Evolution Mission/Neutral Gas Ion Mass Spectrometer observations during 2015. These are in situ measurements of number densities of atmospheric species (including CO2, Ar, N-2, and CO) in the altitude range from 120 to 200 km above the areoid (corresponding to a total density range from similar to 10(8)-10(11)cm(-3)), providing a data set that is larger than all previous measurements of these waves combined. These observations span from 70 degrees latitude and cover a wide range of local times and solar longitudes (Ls), allowing for the study of longitudinal structures under various conditions. Furthermore, the data in May and November 2015 are at similar latitudes and local times but different Ls (similar to 340 degrees in May, close to northern spring equinox, and 70 degrees in November, close to northern summer solstice and aphelion), ideal for studying the seasonal effects of tides. Our analysis shows that in each month the Ar density varies with longitude having a large wave structure. It is dominated by wave 2 and 3, accounting for 8-16% of the change of the mean density. Comparison shows that the longitudinal structures at a constant CO2 density level have different amplitudes at different seasons, although their patterns are similar. The temperature structure has a phase difference from the density variation, indicating the dissipation of tides in this altitude region. The longitudinal structure is seen in all species, including major and minor species, consistent with the tidal signatures.
C1 [Liu, Guiping; England, Scott; Lillis, Robert J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[England, Scott] Virginia Polytech Inst & State Univ, Aerosp & Ocean Engn, Blacksburg, VA 24061 USA.
[Mahaffy, Paul R.; Elrod, Meredith; Benna, Mehdi] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Jakosky, Bruce] Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
RP Liu, GP (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM guiping@ssl.berkeley.edu
FU NASA Mars Data Analysis Program [NNX16AJ42G]; NASA Mars Exploration
Program
FX The NGIMS Level 2 data are publicly available on the Planetary Data
System (PDS) at http://pds.nasa.gov. G.L., S.L.E., and R.J. Lillis were
supported by the NASA Mars Data Analysis Program through grant
NNX16AJ42G. The MAVEN mission has been funded through the NASA Mars
Exploration Program.
NR 33
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U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PY 2017
VL 122
IS 1
BP 1258
EP 1268
DI 10.1002/2016JA023455
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EM9UE
UT WOS:000395655800089
ER
PT J
AU Loop, MS
Howard, G
de los Campos, G
Al-Hamdan, MZ
Safford, MM
Levitan, EB
McClure, LA
AF Loop, Matthew Shane
Howard, George
de los Campos, Gustavo
Al-Hamdan, Mohammad Z.
Safford, Monika M.
Levitan, Emily B.
McClure, Leslie A.
TI Heat Maps of Hypertension, Diabetes Mellitus, and Smoking in the
Continental United States
SO CIRCULATION-CARDIOVASCULAR QUALITY AND OUTCOMES
LA English
DT Article
DE cardiovascular diseases; diabetes mellitus; epidemiology; hypertension;
risk factors
ID GEOGRAPHIC-DISTRIBUTION; STROKE; US; PREVALENCE; VALIDITY; OBESITY;
HEALTH; BELT; RISK
AB Background Geographic variations in cardiovascular mortality are substantial, but descriptions of geographic variations in major cardiovascular risk factors have relied on data aggregated to counties. Herein, we provide the first description of geographic variation in the prevalence of hypertension, diabetes mellitus, and smoking within and across US counties.
Methods and Results We conducted a cross-sectional analysis of baseline risk factor measurements and latitude/longitude of participant residence collected from 2003 to 2007 in the REGARDS study (Reasons for Geographic and Racial Differences in Stroke). Of the 30239 participants, all risk factor measurements and location data were available for 28887 (96%). The mean (SD) age of these participants was 64.8(+/- 9.4) years; 41% were black; 55% were female; 59% were hypertensive; 22% were diabetic; and 15% were current smokers. In logistic regression models stratified by race, the median(range) predicted prevalence of the risk factors were as follows: for hypertension, 49% (45%-58%) among whites and 72% (68%-78%) among blacks; for diabetes mellitus, 14% (10%-20%) among whites and 31% (28%-41%) among blacks; and for current smoking, 12% (7%-16%) among whites and 18% (11%-22%) among blacks. Hypertension was most prevalent in the central Southeast among whites, but in the west Southeast among blacks. Diabetes mellitus was most prevalent in the west and central Southeast among whites but in south Florida among blacks. Current smoking was most prevalent in the west Southeast and Midwest among whites and in the north among blacks.
Conclusions Geographic disparities in prevalent hypertension, diabetes mellitus, and smoking exist within states and within counties in the continental United States, and the patterns differ by race.
C1 [Loop, Matthew Shane; Levitan, Emily B.] Univ Alabama Birmingham, Sch Publ Hlth, Dept Epidemiol, 137 E Franklin St,Suite 203, Chapel Hill, NC 27599 USA.
[Howard, George] Univ Alabama Birmingham, Sch Publ Hlth, Dept Biostat, 137 E Franklin St,Suite 203, Chapel Hill, NC 27599 USA.
[de los Campos, Gustavo] Michigan State Univ, Dept Epidemiol & Biostat, E Lansing, MI 48824 USA.
[de los Campos, Gustavo] Michigan State Univ, Dept Stat & Probabil, E Lansing, MI 48824 USA.
[Al-Hamdan, Mohammad Z.] NASA, Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL USA.
[Safford, Monika M.] Weill Cornell Med Coll, Weill Dept Med, Div Gen Internal Med, New York, NY USA.
[McClure, Leslie A.] Drexel Univ, Dept Epidemiol & Biostat, Philadelphia, PA 19104 USA.
RP Loop, MS (reprint author), Univ Alabama Birmingham, Sch Publ Hlth, Dept Epidemiol, 137 E Franklin St,Suite 203, Chapel Hill, NC 27599 USA.
EM loop2@uab.edu
FU National Institute of Neurological Disorders and Stroke, National
Institutes of Health, Department of Health and Human Service [U01
NS041588]; American Heart Association [14PRE18830073]; National Heart,
Lung, and Blood Institute, National Institutes of Health, Department of
Health and Human Services [5T32HL00745734]
FX This research project is supported by a cooperative agreement U01
NS041588 from the National Institute of Neurological Disorders and
Stroke, National Institutes of Health, Department of Health and Human
Service. The content is solely the responsibility of the authors and
does not necessarily represent the official views of the National
Institute of Neurological Disorders and Stroke or the National
Institutes of Health. Representatives of the funding agency have been
involved in the review of the article but not directly involved in the
collection, management, analysis, or interpretation of the data. A full
list of participating REGARDS investigators and institutions can be
found at http://www.regardsstudy.org. This research project was also
partially funded by an American Heart Association 2014 Predoctoral
Fellowship (14PRE18830073) and 5T32HL00745734 from the National Heart,
Lung, and Blood Institute, National Institutes of Health, Department of
Health and Human Services.
NR 23
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Z9 0
U1 0
U2 0
PU LIPPINCOTT WILLIAMS & WILKINS
PI PHILADELPHIA
PA TWO COMMERCE SQ, 2001 MARKET ST, PHILADELPHIA, PA 19103 USA
SN 1941-7705
EI 1941-7713
J9 CIRC-CARDIOVASC QUAL
JI Circ.-Cardiovasc. Qual. Outcomes
PD JAN
PY 2017
VL 10
IS 1
AR UNSP e003350
DI 10.1161/CIRCOUTCOMES.116.003350
PG 6
WC Cardiac & Cardiovascular Systems
SC Cardiovascular System & Cardiology
GA EL1OB
UT WOS:000394388600013
ER
PT J
AU Dietrich, DL
Calabria, R
Massoli, P
Nayagam, V
Williams, FA
AF Dietrich, D. L.
Calabria, R.
Massoli, P.
Nayagam, V.
Williams, F. A.
TI Experimental Observations of the Low-Temperature Burning of
Decane/Hexanol Droplets in Microgravity
SO COMBUSTION SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Droplet combustion; Low-temperature combustion; Microgravity
ID HEPTANE ISOLATED DROPLETS; N-HEPTANE; COOL-FLAMES; COMBUSTION
EXPERIMENTS; CONVECTION; EXTINCTION; IGNITION; RATES; MIXTURES; PRESSURE
AB This article presents the results of experiments conducted aboard the International Space Station involving the combustion of large bi-component droplets of decane and hexanol (50/50 by volume) in air ambients with ambient pressures between 0.05 and 0.30 MPa. The experiments showed the presence of sustained low-temperature or cool-flame burning following radiative extinction of large droplets at ambient pressures greater than or equal to 0.10 MPa. The droplet diameters at cool-flame extinction were larger for the decane/hexanol droplets than for pure decane droplets at atmospheric pressure, suggesting that hexanol inhibits the cool-flame burning. At 0.20 MPa large fiber-supported droplets radiatively extinguished then burned with a cool flame for a period of time before the hot flame spontaneously re-ignited. At the highest ambient pressure of approximately 0.30 MPa the droplets again radiatively extinguished and burned with a cool flame. Contrary to the 0.20 MPa tests, however, the hot flame did not spontaneously re-ignite, but the droplet burned to completion with a cool flame. Further, more detailed analyses of all camera and radiometer data suggest that the cool-flame burning at 0.30 MPa is fundamentally different than the cool-flame burning at atmospheric pressure. This result does not appear to be consistent with expectations based on currently available cool-flame chemical kinetics and may suggest the need for a different chemical-kinetic mechanism.
C1 [Dietrich, D. L.] NASA, John H Glenn Res Ctr, Combust Phys & Reacting Proc Branch, Cleveland, OH USA.
[Calabria, R.; Massoli, P.] CNR, Ist Motori, Dept Energy & Transportat, Naples, Italy.
[Nayagam, V.] Case Western Reserve Univ, Dept Mech & Aerosp Engn, Cleveland, OH 44106 USA.
[Williams, F. A.] Univ Calif San Diego, Dept Mech & Aerosp Engn, La Jolla, CA 92093 USA.
RP Dietrich, DL (reprint author), NASA, John H Glenn Res Ctr, Mail Stop 110-3,21000 Brookpark Rd, Cleveland, OH 44135 USA.
EM Daniel.l.dietrich@nasa.gov
NR 48
TC 0
Z9 0
U1 1
U2 1
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA
SN 0010-2202
EI 1563-521X
J9 COMBUST SCI TECHNOL
JI Combust. Sci. Technol.
PY 2017
VL 189
IS 3
BP 520
EP 554
DI 10.1080/00102202.2016.1225730
PG 35
WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary;
Engineering, Chemical
SC Thermodynamics; Energy & Fuels; Engineering
GA EL2HS
UT WOS:000394441300006
ER
PT J
AU Erickson, TM
Pearce, MA
Reddy, SM
Timms, NE
Cavosie, AJ
Bourdet, J
Rickard, WDA
Nemchin, AA
AF Erickson, Timmons M.
Pearce, Mark A.
Reddy, Steven M.
Timms, Nicholas E.
Cavosie, Aaron J.
Bourdet, Julien
Rickard, William D. A.
Nemchin, Alexander A.
TI Microstructural constraints on the mechanisms of the transformation to
reidite in naturally shocked zircon
SO CONTRIBUTIONS TO MINERALOGY AND PETROLOGY
LA English
DT Article
DE Shock metamorphism; EBSD; zircon; Reidite; Ries impact crater
ID PLANAR DEFORMATION FEATURES; HIGH-PRESSURE; PHASE-TRANSITION; RIES
CRATER; U-PB; CRYSTALLINE ROCKS; IMPACT STRUCTURES; VREDEFORT DOME;
ZRSIO4; METAMORPHISM
AB Zircon (ZrSiO4) is used to study impact structures because it responds to shock loading and unloading in unique, crystallographically controlled manners. One such phenomenon is the transformation of zircon to the high-pressure polymorph, reidite. This study quantifies the geometric and crystallographic orientation relationships between these two phases using naturally shocked zircon grains. Reidite has been characterized in 32 shocked zircon grains (shocked to stages II and III) using a combination of electron backscatter diffraction (EBSD) and focused ion beam cross-sectional imaging techniques. The zircon-bearing clasts were obtained from within suevite breccia from the Nordlingen 1973 borehole, close to the center of the 14.4 Ma Ries impact crater, in Bavaria, Germany. We have determined that multiple sets (up to 4) of reidite lamellae can form in a variety of non-rational habit planes within the parent zircon. However, EBSD mapping demonstrates that all occurrences of lamellar reidite have a consistent interphase misorientation relationship with the host zircon that is characterized by an approximate alignment of a {100}(zircon) with a {112} (reidite) and alignment of a {112}(zircon) with a conjugate {112}(reidite). Given the tetragonal symmetry of zircon and reidite, we predict that there are eight possible variants of this interphase relationship for reidite transformation within a single zircon grain. Furthermore, laser Raman mapping of one reidite-bearing grain shows that moderate metamictization can inhibit reidite formation, thereby highlighting that the transformation is controlled by zircon crystallinity. In addition to lamellar reidite, submicrometer-scale granules of reidite were observed in one zircon. The majority of reidite granules have a topotaxial alignment that is similar to the lamellar reidite, with some additional orientation dispersion. We confirm that lamellar reidite likely forms via a deviatoric transformation mechanism in highly crystalline zircon, whereas granular reidite forms via a reconstructive transformation from low-crystallinity ZrSiO4 within the reidite stability field. The results of this study further refine the formation mechanisms and conditions of reidite transformation in naturally shocked zircon.
C1 [Erickson, Timmons M.; Reddy, Steven M.; Timms, Nicholas E.; Cavosie, Aaron J.; Nemchin, Alexander A.] Curtin Univ, Dept Appl Geol, GPO Box U1984, Perth, WA 6845, Australia.
[Pearce, Mark A.] CSIRO Mineral Resources, Australian Resources Res Ctr, 26 Dick Perry Ave, Kensington, WA 6151, Australia.
[Cavosie, Aaron J.] Univ Wisconsin Madison, Dept Geosci, NASA, Astrobiol Inst, Madison, WI 53706 USA.
[Cavosie, Aaron J.] Univ Puerto Rico Mayaguez, Dept Geol, Mayaguez, PR 00681 USA.
[Bourdet, Julien] CSIRO Energy, Australian Resources Res Ctr, 26 Dick Perry Ave, Kensington, WA 6151, Australia.
[Rickard, William D. A.] Curtin Univ, Dept Imaging & Appl Phys, GPO Box 1984, Perth, WA 6845, Australia.
[Nemchin, Alexander A.] Swedish Museum Nat Hist, Dept Geosci, S-10405 Stockholm, Sweden.
RP Erickson, TM (reprint author), Curtin Univ, Dept Appl Geol, GPO Box U1984, Perth, WA 6845, Australia.
EM Timmons.Erickson@gmail.com
FU Curtin International Postgraduate Research Scholarship from Curtin
University Office of Research and Development; US National Science
Foundation [EAR-1145118]; NASA Astrobiology program; CSIRO Office of the
Chief Executive Postdoctoral Fellowship; ARC Core to Crust Fluid System
Centre of Excellence; ARC [LE130100053]; Curtin University, University
of Western Australia; CSIRO; Australian Resource Characterisation
Facility (ARCF); National Resource Sciences Precinct (NRSP)-CSIRO,
Curtin University; University of Western Australia-Science and Industry
Endowment Fund
FX We would like to thank Gisele Posges, Deputy Director of the Ries Crater
Museum, for supplying the samples. TME acknowledges financial support
from a Curtin International Postgraduate Research Scholarship from
Curtin University Office of Research and Development. AJC acknowledges
support from the US National Science Foundation (EAR-1145118) and the
NASA Astrobiology program. MAP was supported by a CSIRO Office of the
Chief Executive Postdoctoral Fellowship. Analytical costs were supported
by the ARC Core to Crust Fluid System Centre of Excellence. The ARC
(LE130100053), Curtin University, University of Western Australia, and
CSIRO are acknowledged for funding the Tescan Mira3 FEG-SEM housed in
the John de Laeter Centre's Microscopy & Microanalysis Facility at
Curtin University. The Tescan Lyra3 FIB-SEM is part of the Australian
Resource Characterisation Facility (ARCF), under the auspices of the
National Resource Sciences Precinct (NRSP)-a collaboration between
CSIRO, Curtin University and The University of Western Australia-and is
supported by the Science and Industry Endowment Fund. We would like to
thank Gordon Moore for thorough editorial handling and two anonymous
reviewers for their significant improvements to the manuscript.
NR 71
TC 1
Z9 1
U1 1
U2 1
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0010-7999
EI 1432-0967
J9 CONTRIB MINERAL PETR
JI Contrib. Mineral. Petrol.
PD JAN
PY 2017
VL 172
IS 1
AR 6
DI 10.1007/s00410-016-1322-0
PG 26
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA EO0LQ
UT WOS:000396389700006
ER
PT J
AU Nghiem, SV
Zuffada, C
Shah, R
Chew, C
Lowe, ST
Mannucci, AJ
Cardellach, E
Brakenridge, GR
Geller, G
Rosenqvist, A
AF Nghiem, Son V.
Zuffada, Cinzia
Shah, Rashmi
Chew, Clara
Lowe, Stephen T.
Mannucci, Anthony J.
Cardellach, Estel
Brakenridge, G. Robert
Geller, Gary
Rosenqvist, Ake
TI Wetland monitoring with Global Navigation Satellite System reflectometry
SO EARTH AND SPACE SCIENCE
LA English
DT Review
DE wetland; methane; water cycle; energy cycle; GNSS-R; GPS
ID SEA-LEVEL RISE; L-BAND SAR; OCEAN ALTIMETRY; SOIL-MOISTURE; GPS SIGNALS;
AMAZON FLOODPLAIN; DATA SETS; WATER; RADAR; IMAGERY
AB Information about wetland dynamics remains a major missing gap in characterizing, understanding, and projecting changes in atmospheric methane and terrestrial water storage. A review of current satellite methods to delineate and monitor wetland change shows some recent advances, but much improved sensing technologies are still needed for wetland mapping, not only to provide more accurate global inventories but also to examine changes spanning multiple decades. Global Navigation Satellite Systems Reflectometry (GNSS-R) signatures from aircraft over the Ebro River Delta in Spain and satellite measurements over the Mississippi River and adjacent watersheds demonstrate that inundated wetlands can be identified under different vegetation conditions including a dense rice canopy and a thick forest with tall trees, where optical sensors and monostatic radars provide limited capabilities. Advantages as well as constraints of GNSS-R are presented, and the synergy with various satellite observations are considered to achieve a breakthrough capability for multidecadal wetland dynamics monitoring with frequent global coverage at multiple spatial and temporal scales.
C1 [Nghiem, Son V.; Zuffada, Cinzia; Shah, Rashmi; Chew, Clara; Lowe, Stephen T.; Mannucci, Anthony J.; Geller, Gary] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Cardellach, Estel] CSIC, Inst Ciencies Espai, IEEC, Barcelona, Spain.
[Brakenridge, G. Robert] Univ Colorado, Inst Arctic & Alpine Res, Community Surface Dynam Modeling Syst, Boulder, CO 80309 USA.
[Geller, Gary] Group Earth Observat, Geneva, Switzerland.
[Rosenqvist, Ake] Solo Earth Observat sOloEO, Tokyo, Japan.
RP Nghiem, SV (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM Son.V.Nghiem@jpl.nasa.gov
FU National Aeronautics and Space Administration (NASA); NASA LCLUC
Program; Advanced Concepts Program at JPL; Spanish Grant
[ESP2015-70014-C2-2-R]; European FP7 grant [FP7-SPACE-2013-1 607126]
FX The research carried out at the Jet Propulsion Laboratory (JPL),
California Institute of Technology, was supported under a contract with
the National Aeronautics and Space Administration (NASA). The work
related to land cover and land use change (LCLUC) research by Nghiem is
supported by the NASA LCLUC Program. Nghiem and Shah are also partially
supported by the Advanced Concepts Program at JPL. Cardellach is
partially supported by Spanish Grant ESP2015-70014-C2-2-R and European
FP7 grant FP7-SPACE-2013-1 607126. TechDemoSat-1 GNSS Reflectometry data
set courtesy of Surrey Satellite Technology Ltd via www.merrbys.org
website under Creative Commons License CC-BY-NC. We thank Adrian Strauch
of the University of Bonn and Lammert Hilarides from Wetlands
International for providing feedback on our wetland discussion. We
appreciate the agreement from Steven Rimer, the Manager of the Big Lake
National Wildlife Refuge, for the use of his wetland photograph in this
paper. Availability of data used in this paper: GOLD-RTR test airborne
data from Institut de Ciencies de l'Espai/CSIC-IEEC, TDS-1 satellite
data from Surrey Satellites Technology Ltd via www.merrbys.org website
under Creative Commons License CC-BY-NC, QuikSCAT satellite data from
the NASA Jet Propulsion Laboratory PO.DAAC, MODIS satellite data form
MODIS Web http://modis.gsfc.nasa.gov/data/, river gauge data from U.S.
Geological Survey http://waterdata.usgs.gov/nwis, digital elevation
model data from http://www2.jpl.nasa.gov/srtm/, and land cover and land
use data from Institut Cartografic i Geologic de Catalunya
http://www.icc.cat/vissir3/.
NR 101
TC 1
Z9 1
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2333-5084
J9 EARTH SPACE SCI
JI Earth Space Sci.
PD JAN
PY 2017
VL 4
IS 1
BP 16
EP 39
DI 10.1002/2016EA000194
PG 24
WC Geosciences, Multidisciplinary
SC Geology
GA EL4GU
UT WOS:000394580500002
PM 28331894
ER
PT J
AU Carlson, JK
Pollack, AG
Driggers, WB
Castro, JI
Brame, AB
Lee, JL
AF Carlson, John K.
Pollack, Adam G.
Driggers, William B., III
Castro, Jose I.
Brame, Adam B.
Lee, Jennifer L.
TI Revised analyses suggest that the lesser electric ray Narcine bancroftii
is not at risk of extinction
SO ENDANGERED SPECIES RESEARCH
LA English
DT Article
DE Generalized linear model; Trawl; IUCN Red List; Endangered Species Act
ID ABUNDANCE; MODELS; CATCH; FISH
AB Among rays inhabiting US coastal waters in the western North Atlantic Ocean, a species of potential concern is the lesser electric ray Narcine bancroftii. The most recent International Union for the Conservation of Nature (IUCN) Red List Assessment indicates the species is Critically Endangered, which represents the highest risk of extinction based on IUCN criteria. The basis of this alarming designation was a reported 98% decline in abundance based on analyses of a long-term, fisheries-independent trawl survey conducted in the northern Gulf of Mexico since 1972. The status of this species generated considerable concern within the conservation community, prompting a petition for its inclusion under the US Endangered Species Act. We critically examined all available sources of data relative to the abundance of lesser electric ray, including those utilized in the original analysis, and found lesser electric rays do not appear to be at risk of extinction. Contrary to the earlier analysis, we found no evidence of decline in the relative abundance of lesser electric rays, with trends in abundance being relatively flat with high variability. Our investigation determined that analyses of previous trawl surveys did not address major changes over time in survey design and disregarded the strong habitat preference of lesser electric rays. It is critical that the best possible information be used when considering the conservation status of a given species to minimize undue burdens and ensure that increasingly limited resources are applied to the recovery of those species that are truly in peril.
C1 [Carlson, John K.] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Panama City Lab, 3500 Delwood Beach Rd, Panama City, FL 32408 USA.
[Pollack, Adam G.] Riverside Technol Inc, Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Mississippi Lab, Drawer 1207, Pascagoula, MS 39567 USA.
[Driggers, William B., III] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Mississippi Lab, PO Drawer 1207, Pascagoula, MS 39567 USA.
[Castro, Jose I.] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, 75 Virginia Beach Dr, Miami, FL 33149 USA.
[Brame, Adam B.; Lee, Jennifer L.] Natl Marine Fisheries Serv, Southeast Reg Off, 263 13th Ave S, St Petersburg, FL 33701 USA.
RP Carlson, JK (reprint author), Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Panama City Lab, 3500 Delwood Beach Rd, Panama City, FL 32408 USA.
EM john.carlson@noaa.gov
NR 23
TC 0
Z9 0
U1 0
U2 0
PU INTER-RESEARCH
PI OLDENDORF LUHE
PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY
SN 1863-5407
EI 1613-4796
J9 ENDANGER SPECIES RES
JI Endanger. Species Res.
PY 2017
VL 32
BP 177
EP 186
DI 10.3354/esr00799
PG 10
WC Biodiversity Conservation
SC Biodiversity & Conservation
GA EO9SB
UT WOS:000397027300003
ER
PT J
AU Nguyen, HN
Castro-Wallace, SL
Rodrigues, DF
AF Nguyen, Hang N.
Castro-Wallace, Sarah L.
Rodrigues, Debora F.
TI Acute toxicity of graphene nanoplatelets on biological wastewater
treatment process
SO ENVIRONMENTAL SCIENCE-NANO
LA English
DT Article
ID WALLED CARBON NANOTUBES; ACTIVATED-SLUDGE PROCESS; SEWAGE-TREATMENT
PLANTS; 16S RIBOSOMAL-RNA; REAL-TIME PCR; MICROBIAL COMMUNITY;
PHOSPHORUS REMOVAL; BACTERIAL COMMUNITY; POTENTIAL RELEASE; BATCH
REACTORS
AB This study investigates the acute toxicity of graphene to sludge microbial communities. The acute toxicity was investigated with concentrations varying from low to relatively high concentrations of graphene (between 0 and 300 mg L-1) to understand the impact of different concentrations of graphene on the biological wastewater treatment process. The experiments were performed with a 10 h continuous aeration using batch reactors to simulate the wastewater biological treatment process. Results showed that increasing concentrations of graphene in the reactors led to decreasing COD, BOD5, ammonia and phosphate removals. In addition, abundances of ammonia oxidizing bacteria, ammonia monooxygenase and phosphate accumulating bacteria decreased along with the overall sludge microbial metabolic activity. The 16S rRNA deep sequencing of the sludge microbial community exposed to different concentrations of graphene showed that the abundances of the two most abundant phyla, i.e. Proteobacteria and Bacteriodetes, changed with increasing concentrations of graphene. The results also showed that releases of graphene concentrations at 10 mg L-1 and higher seem to present a short term impact in the wastewater treatment process.
C1 [Nguyen, Hang N.; Rodrigues, Debora F.] Univ Houston, Dept Civil & Environm Engn, Houston, TX 77204 USA.
[Castro-Wallace, Sarah L.] NASA, Johnson Space Ctr, Microbiol Lab, Houston, TX 77058 USA.
RP Rodrigues, DF (reprint author), Univ Houston, Dept Civil & Environm Engn, Houston, TX 77204 USA.
EM dfrigirodrigues@uh.edu
FU NSF [104093]
FX This project was supported by the NSF Career Award Nano-health #104093.
The authors would like to acknowledge Douglas J. Botkin for training
Hang to use the Miseq. Hang also would like to thank Kelly Hainline, an
undergraduate student participating in the UH Research experience of
undergraduates.
NR 55
TC 0
Z9 0
U1 0
U2 0
PU ROYAL SOC CHEMISTRY
PI CAMBRIDGE
PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS,
ENGLAND
SN 2051-8153
EI 2051-8161
J9 ENVIRON SCI-NANO
JI Environ.-Sci. Nano
PY 2017
VL 4
IS 1
BP 160
EP 169
DI 10.1039/c6en00442c
PG 10
WC Chemistry, Multidisciplinary; Environmental Sciences; Nanoscience &
Nanotechnology
SC Chemistry; Environmental Sciences & Ecology; Science & Technology -
Other Topics
GA EL7BV
UT WOS:000394777000015
ER
PT J
AU van Marle, MJE
Field, RD
van der Werf, GR
de Wagt, IAE
Houghton, RA
Rizzo, LV
Artaxo, P
Tsigaridis, K
AF van Marle, Margreet J. E.
Field, Robert D.
van der Werf, Guido R.
de Wagt, Ivan A. Estrada
Houghton, Richard A.
Rizzo, Luciana V.
Artaxo, Paulo
Tsigaridis, Kostas
TI Fire and deforestation dynamics in Amazonia (1973-2014)
SO GLOBAL BIOGEOCHEMICAL CYCLES
LA English
DT Article
DE horizontal visibility; South America; historic fire emissions; proxy
data; deforestation; Amazonia
ID LAND-COVER CHANGE; BRAZILIAN AMAZON; SOUTHEAST-ASIA; SATELLITE DATA;
BURNED AREA; EL-NINO; BIOMASS; EMISSIONS; TRENDS; FOREST
AB Consistent long-term estimates of fire emissions are important to understand the changing role of fire in the global carbon cycle and to assess the relative importance of humans and climate in shaping fire regimes. However, there is limited information on fire emissions from before the satellite era. We show that in the Amazon region, including the Arc of Deforestation and Bolivia, visibility observations derived from weather stations could explain 61% of the variability in satellite-based estimates of bottom-up fire emissions since 1997 and 42% of the variability in satellite-based estimates of total column carbon monoxide concentrations since 2001. This enabled us to reconstruct the fire history of this region since 1973 when visibility information became available. Our estimates indicate that until 1987 relatively few fires occurred in this region and that fire emissions increased rapidly over the 1990s. We found that this pattern agreed reasonably well with forest loss data sets, indicating that although natural fires may occur here, deforestation and degradation were the main cause of fires. Compared to fire emissions estimates based on Food and Agricultural Organization's Global Forest and Resources Assessment data, our estimates were substantially lower up to the 1990s, after which they were more in line. These visibility-based fire emissions data set can help constrain dynamic global vegetation models and atmospheric models with a better representation of the complex fire regime in this region.
C1 [van Marle, Margreet J. E.; van der Werf, Guido R.; de Wagt, Ivan A. Estrada] Vrije Univ Amsterdam, Fac Earth & Life Sci, Amsterdam, Netherlands.
[Field, Robert D.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA.
[Field, Robert D.; Tsigaridis, Kostas] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Houghton, Richard A.] Woods Hole Res Ctr, Falmouth, MA USA.
[Rizzo, Luciana V.] Univ Fed Sao Paulo, Dept Exact & Earth Sci, Sao Paulo, Brazil.
[Artaxo, Paulo] Univ Sao Paulo, Inst Phys, Sao Paulo, Brazil.
[Tsigaridis, Kostas] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
RP van Marle, MJE (reprint author), Vrije Univ Amsterdam, Fac Earth & Life Sci, Amsterdam, Netherlands.
EM m.j.e.van.marle@vu.nl
OI Marle, van, Margreet/0000-0001-7473-5550
FU European Research Council (ERC) [280061]; NASA Atmospheric Chemistry
Modeling and Analysis Program; NASA Carbon Monitoring System; FAPESP
[2003/05014-0]; CNPq
FX We would like to thank Enrico Dammers, Benjamin Aouizerats, and Douglas
Morton for useful discussions. Furthermore, we acknowledge INPE for
making the PRODES publicly available
(http://www.obt.inpe.br/prodes/index.php). GFED4s data is publicly
available at http://www.globalfiredata.org/data.html. Visibility
observations were obtained from the NOAA National Climatic Data Center
Integrated Surface Database
(https://catalog.data.gov/dataset/integrated-surface-global-hourly-data)
. FAO-based carbon emissions related to deforestation, the VOD-based net
forest loss, and the visibility-based time series developed during this
research can be requested via the corresponding author. This research
was funded by the European Research Council (ERC) grant 280061 (M.v.M.
G.v. d.W.), NASA Atmospheric Chemistry Modeling and Analysis Program
(R.F.), NASA Carbon Monitoring System (R.H.), FAPESP grant 2003/05014-0
(P.A.), and CNPq (P.A.). We thank two reviewers for their constructive
comments and helpful suggestions on an earlier version of this
manuscript.
NR 59
TC 0
Z9 0
U1 1
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0886-6236
EI 1944-9224
J9 GLOBAL BIOGEOCHEM CY
JI Glob. Biogeochem. Cycle
PD JAN
PY 2017
VL 31
IS 1
BP 24
EP 38
DI 10.1002/2016GB005445
PG 15
WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric
Sciences
GA EM1PD
UT WOS:000395088600002
PM 28286373
ER
PT J
AU Holzmann, GJ
AF Holzmann, Gerard J.
TI The Value of Doubt
SO IEEE SOFTWARE
LA English
DT Article
C1 [Holzmann, Gerard J.] Jet Prop Lab, Pasadena, CA 91109 USA.
RP Holzmann, GJ (reprint author), Jet Prop Lab, Pasadena, CA 91109 USA.
EM gholzmann@acm.org
NR 3
TC 0
Z9 0
U1 0
U2 0
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 0740-7459
EI 1937-4194
J9 IEEE SOFTWARE
JI IEEE Softw.
PD JAN-FEB
PY 2017
VL 34
IS 1
BP 106
EP 109
PG 4
WC Computer Science, Software Engineering
SC Computer Science
GA EP1CC
UT WOS:000397122000020
ER
PT J
AU Sorgenfrei, T
Jauss, T
Croll, A
Reimann, C
Friedrich, J
Volz, M
AF Sorgenfrei, Tina
Jauss, Thomas
Croll, Arne
Reimann, Christian
Friedrich, Jochen
Volz, Marint
TI The Critical Growth Rate for Particle Incorporation during the
Directional Solidification of Solar Silicon under Microgravity
SO INTERNATIONAL JOURNAL OF MICROGRAVITY SCIENCE AND APPLICATION
LA English
DT Article
DE Foreign phase particle; Particle engulfment; Particle pushing; Melt
growth; Silicon; VGF; Directional solidification
ID FLOATING-ZONE GROWTH; INTERFACE; BEHAVIOR
AB Foreign phase particles, which are engulfed by a growth front and then incorporated into a growing crystal, can cause a variety of problems. These problems can influence the crystal growth process and the preparation of the crystal or reduce the performance of resulting devices. In photovoltaics, the incorporation of SiC particles in VGF silicon leads to a relatively high material loss due to wire saw damages and shunts in the resulting solar cells. Due to the setup of the directional solidification the formation of SiC particles can hardly be avoided. Therefore, it is important to control the incorporation of the particles. It is known that the incorporation is dependent on the size of the particles and on the velocity of the moving solid-liquid interface. Existing theoretical models describe the transition between pushing and engulfment, but growth experiments show that the experimental values for the transition between these two states deviate significantly from the theoretical ones. In this work, several experiments under 1 G conditions and an experiment under mu g conditions were done to investigate this question. The ttg setup is necessary to get as close as possible to diffusive conditions which are the basic parameters for the theoretical calculations.
C1 [Sorgenfrei, Tina; Jauss, Thomas; Croll, Arne] Univ Freiburg, Crystallog, Hermann Herder Str 5, D-79104 Freiburg, Germany.
[Reimann, Christian; Friedrich, Jochen] Fraunhofer Inst Integrated Circuits & Devices, Schottkystr 10, D-91058 Erlangen, Germany.
[Volz, Marint] NASA, Marshall Space Flight Ctr, Huntsville, AL USA.
RP Sorgenfrei, T (reprint author), Univ Freiburg, Crystallog, Hermann Herder Str 5, D-79104 Freiburg, Germany.
EM tina.sorgenfrei@fmf.uni-freiburg.de
FU DIR/BMWi [FKZ 50WM1147]
FX This work was funded by the DIR/BMWi under FKZ 50WM1147. The authors
thank M. Azizi, L. Rees-Isele, C. Lehmann, and M. Kranz-Probst for
sample preparation and evaluation, and J. Quick for the assistance with
the magnetic field experiments at NASA MSFC. The assistance of the
Airbus DS, OHB, Moraba, and SSC teams during the TEXUS 51 campaign is
greatly appreciated.
NR 18
TC 0
Z9 0
U1 0
U2 0
PU JAPAN SOC MICROGRAVITY APPLICATION
PI TOKYP
PA JAPAN SOC MICROGRAVITY APPLICATION, TOKYP, 00000, JAPAN
SN 0915-3616
EI 2188-9783
J9 INT J MICROGRAVITY S
JI Int. J. Microgravity Sci. Appl.
PY 2017
VL 34
IS 1
AR 340115
DI 10.15011//jasma.34.340115
PG 8
WC Physics, Applied
SC Physics
GA EO4ZZ
UT WOS:000396704100015
ER
PT J
AU Zhang, MW
Hu, CM
Kowalewski, MG
Janz, SJ
Lee, ZP
Wei, JW
AF Zhang, Minwei
Hu, Chuanmin
Kowalewski, Matthew G.
Janz, Scott J.
Lee, Zhongping
Wei, Jianwei
TI Atmospheric correction of hyperspectral airborne GCAS measurements over
the Louisiana Shelf using a cloud shadow approach
SO INTERNATIONAL JOURNAL OF REMOTE SENSING
LA English
DT Article
ID WATER-LEAVING RADIANCE; OCEAN COLOR; ALGORITHM; COASTAL; REFLECTANCE;
SEDIMENT; SURFACE
AB As an image-driven method to correct for atmospheric effects, the cloud shadow (CS) approach does not require accurate radiometric calibration of the sensor, making it feasible to process remotely sensed data when radiometric calibration may contain non-negligible uncertainties. Using measurements from the Geostationary Coastal and Air Pollution Events Airborne Simulator and from the Moderate Resolution Imaging Spectroradiometer over the Louisiana Shelf, we evaluate the CS approach to airplane measurements in turbid-water environments. The original CS approach somehow produced remote-sensing reflectance (R-rs, sr(-1)) with an abnormal spectral shape, likely a result of the assumption of identical path radiance for the pair of pixels in and out of the shadow, which is not exactly valid for measurements made from a low-altitude airplane. To overcome this limitation, an empirical scheme using an effective wavelength-dependent radiance reflectance for the cloud (gamma, sr(-1)) was developed and reasonable GCAS R-rs retrievals are then generated, which were further validated against in situ R-rs. Issues and challenges in applying CS to measurements of low-altitude airplanes are discussed.
C1 [Zhang, Minwei; Hu, Chuanmin] Univ S Florida, Coll Marine Sci, St Petersburg, FL 33701 USA.
[Kowalewski, Matthew G.; Janz, Scott J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Lee, Zhongping; Wei, Jianwei] Univ Massachusetts, Sch Environm, Boston, MA 02125 USA.
RP Zhang, MW (reprint author), Univ S Florida, St Petersburg, FL 33701 USA.
EM minweizhang@mail.usf.edu
FU NASA
FX This work was supported by the NASA through the programme of North
Atlantic Aerosols and Marine Ecosystems Study (NAAMES) and also through
a grant to support NASA's GEO-CAPE mission design.
NR 27
TC 0
Z9 0
U1 0
U2 0
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND
SN 0143-1161
EI 1366-5901
J9 INT J REMOTE SENS
JI Int. J. Remote Sens.
PY 2017
VL 38
IS 4
BP 1162
EP 1179
DI 10.1080/01431161.2017.1280633
PG 18
WC Remote Sensing; Imaging Science & Photographic Technology
SC Remote Sensing; Imaging Science & Photographic Technology
GA EL4WW
UT WOS:000394622600011
ER
PT J
AU Fayne, JV
Bolten, JD
Doyle, CS
Fuhrmann, S
Rice, MT
Houser, PR
Lakshmi, V
AF Fayne, Jessica V.
Bolten, John D.
Doyle, Colin S.
Fuhrmann, Sven
Rice, Matthew T.
Houser, Paul R.
Lakshmi, Venkat
TI Flood mapping in the lower Mekong River Basin using daily MODIS
observations
SO INTERNATIONAL JOURNAL OF REMOTE SENSING
LA English
DT Article
ID NOAA/AVHRR DATA; INDEX; PRODUCTS; DROUGHT
AB In flat homogenous terrain such as in Cambodia and Vietnam, the monsoon season brings significant and consistent flooding between May and November. To monitor flooding in the Lower Mekong region, the near real-time NASA Flood Extent Product (NASA-FEP) was developed using seasonal normalized difference vegetation index (NDVI) differences from the 250 m resolution Moderate Resolution Imaging Spectroradiometer (MODIS) sensor compared to daily observations. The use of a percentage change interval classification relating to various stages of flooding reduces might be confusing to viewers or potential users, and therefore reducing the product usage. To increase the product usability through simplification, the classification intervals were compared with other commonly used change detection schemes to identify the change classification scheme that best delineates flooded areas. The percentage change method used in the NASA-FEP proved to be helpful in delineating flood boundaries compared to other change detection methods. The results of the accuracy assessments indicate that the -75% NDVI change interval can be reclassified to a descriptive 'flood' classification. A binary system was used to simplify the interpretation of the NASA-FEP by removing extraneous information from lower interval change classes.
C1 [Fayne, Jessica V.; Lakshmi, Venkat] Univ South Carolina, Sch Earth Ocean & Environm, Columbia, SC 29208 USA.
[Bolten, John D.] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Code 617, Greenbelt, MD USA.
[Doyle, Colin S.] Univ Texas Austin, Dept Geog & Environm, Austin, TX USA.
[Fuhrmann, Sven; Rice, Matthew T.; Houser, Paul R.] George Mason Univ, Dept Geog & Geoinformat Sci, Fairfax, VA USA.
RP Fayne, JV (reprint author), Univ South Carolina, Sch Earth Ocean & Environm, Columbia, SC 29208 USA.
EM jfayne2@gmu.edu
FU NASA Applied Sciences Program - Water Resources Applications Program;
NASA [NNX15AN39G]
FX The funding from the NASA Applied Sciences Program - Water Resources
Applications, Program Manager Bradley D. Doorn, NASA Grant Number
NNX15AN39G is gratefully acknowledged.
NR 44
TC 0
Z9 0
U1 0
U2 0
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND
SN 0143-1161
EI 1366-5901
J9 INT J REMOTE SENS
JI Int. J. Remote Sens.
PY 2017
VL 38
IS 6
BP 1737
EP 1757
DI 10.1080/01431161.2017.1285503
PG 21
WC Remote Sensing; Imaging Science & Photographic Technology
SC Remote Sensing; Imaging Science & Photographic Technology
GA EL5HF
UT WOS:000394651500014
ER
PT J
AU Johnson, DL
Vaughan, WW
AF Johnson, Dale L.
Vaughan, William W.
TI Natural Terrestrial Environment from Selected Field Data Measurements:
Results and Applications for Launch Vehicle Development
SO JOURNAL OF AEROSPACE TECHNOLOGY AND MANAGEMENT
LA English
DT Review
DE Aerospace meteorology; Launch/space vehicle development; Mission
operations; Atmospheric environment; Atmospheric variability;
Meteorological rockets; Sequential detail wind profiles
AB This paper is mainly a review presenting 3 unique NASA natural environment field projects. Included are some important natural environment technical results and applications that are applicable in the design, development and operations of launch vehicles as well as in advancing the atmospheric state-of-the-art. For the design, development, testing, launch and flight of various launch vehicles all natural terrestrial environments are considered, with normally wind being the main contributor or driver to the design of a launch vehicle.
C1 [Johnson, Dale L.] NASA, Huntsville, AL USA.
[Vaughan, William W.] NASA Emeritus, NASA Marshall Space Flight Ctr, Earth Sci Branch, Huntsville, AL USA.
[Vaughan, William W.] NASA Marshall Space Flight Ctr, Earth Sci Branch, Huntsville, AL 35812 USA.
RP Vaughan, WW (reprint author), NASA Marshall Space Flight Ctr, Earth Sci Branch, Huntsville, AL 35812 USA.
EM williamwvaughan@aol.com
NR 10
TC 0
Z9 0
U1 0
U2 0
PU INST AERONAUTICA & ESPACO-IAE
PI SAO PAULO
PA PRACA MAL EDUARDO GOMES 50, VILA ACACIAS, SAO JOSE DOS CAMPOS, SAO
PAULO, 122228-901, BRAZIL
SN 1984-9648
EI 2175-9146
J9 J AEROSP TECHNOL MAN
JI J. Aerosp. Technol. Manag.
PD JAN-MAR
PY 2017
VL 9
IS 1
BP 5
EP 17
DI 10.5028/jatm.v9i1.636
PG 13
WC Engineering, Aerospace
SC Engineering
GA EM9LD
UT WOS:000395632200001
ER
PT J
AU West, TK
Reuter, BW
Walker, EL
Kleb, B
Park, MA
AF West, Thomas K.
Reuter, Bryan W.
Walker, Eric L.
Kleb, Bil
Park, Michael A.
TI Uncertainty Quantification and Certification Prediction of Low-Boom
Supersonic Aircraft Configurations
SO JOURNAL OF AIRCRAFT
LA English
DT Article
ID POLYNOMIAL CHAOS; SENSITIVITY-ANALYSIS; REENTRY FLOWS; WORKSHOP
AB The primary objective of this work was to develop and demonstrate a process for accurate and efficient uncertainty quantification and certification prediction of low-boom, supersonic, transport aircraft. High-fidelity computational-fluid-dynamics models of multiple low-boom configurations were investigated, including the Lockheed Martin SEEB-ALR body of revolution, the NASA 69 deg delta wing, and the Lockheed Martin 1021-01 configuration. Anonintrusive polynomial chaos surrogate approach was used for reduced computational cost of propagating mixed inherent (aleatory) and epistemic uncertainty through both the computational-fluid-dynamics model and the near-field to ground-level boom propagation model. Amethodology has also been introduced to quantify the plausibility of a design to pass a certification under uncertainty. Results of this study include the analysis of each of the three configurations of interest under inviscid and fully turbulent flow assumptions. A comparison of the uncertainty outputs and sensitivity analyses between the configurations is also given. The results of this study illustrate the flexibility and robustness of the developed framework as a tool for uncertainty quantification and certification prediction of low-boom, supersonic aircraft.
C1 [West, Thomas K.] NASA, Langley Res Ctr, Vehicle Anal Branch, Syst Anal & Concepts Directorate, Hampton, VA 23681 USA.
[Reuter, Bryan W.] Univ Texas Austin, Inst Computat Engn & Sci, Austin, TX 78712 USA.
[Walker, Eric L.] NASA, Langley Res Ctr, Test Operat Excellence, Res Directorate, Hampton, VA 23681 USA.
[Kleb, Bil; Park, Michael A.] NASA, Langley Res Ctr, Computat Aerosci Branch, Res Directorate, Hampton, VA 23681 USA.
RP West, TK (reprint author), NASA, Langley Res Ctr, Vehicle Anal Branch, Syst Anal & Concepts Directorate, Hampton, VA 23681 USA.
NR 44
TC 0
Z9 0
U1 0
U2 0
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
EI 1533-3868
J9 J AIRCRAFT
JI J. Aircr.
PD JAN
PY 2017
VL 54
IS 1
BP 40
EP 53
DI 10.2514/1.C033907
PG 14
WC Engineering, Aerospace
SC Engineering
GA EM8HY
UT WOS:000395553300004
ER
PT J
AU Castner, R
Zaman, K
Fagan, A
Heath, C
AF Castner, Raymond
Zaman, Khairul
Fagan, Amy
Heath, Christopher
TI Wedge Shock and Nozzle Exhaust Plume Interaction in a Supersonic Jet
Flow
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT 52nd AIAA Aerospace Sciences Meeting
CY JAN 12-18, 2014
CL National Harbor, MD
SP AIAA
ID UNSTRUCTURED GRIDS; TURBULENT FLOWS; IMPLICIT
AB Fundamental research for sonic boom reduction is needed to quantify the interaction of shock waves generated from the aircraft wing or tail surfaces with a nozzle exhaust plume. Aftbody shock waves that interact with the exhaust plume contribute to the near-field pressure signature of a vehicle. The plume and shock interaction is studied using computational fluid dynamics and compared with experimental data from a coaxial convergent-divergent nozzle flow in an open jet facility. A simple diamond-shaped wedge is used to generate the shock in the outer flow to study its impact on the inner jet flow. Results show that the compression from the wedge deflects both the nozzle plume and the shocks on the opposite side of the plume. The sonic boom pressure signature of the nozzle exhaust plume is modified by the presence of the wedge. Both the experimental results and computational predictions show changes in plume deflection and location of the shock from the wedge.
C1 [Castner, Raymond; Zaman, Khairul] NASA, John H Glenn Res Ctr, Inlet & Nozzle Branch, 21000 Brookpk Road, Cleveland, OH 44135 USA.
[Fagan, Amy] NASA, John H Glenn Res Ctr, Opt Instrumentat Branch, 21000 Brookpk Road, Cleveland, OH 44135 USA.
[Heath, Christopher] NASA, John H Glenn Res Ctr, Multidisciplinary Design Anal Optimizat, 21000 Brookpk Road, Cleveland, OH 44135 USA.
RP Castner, R (reprint author), NASA, John H Glenn Res Ctr, Inlet & Nozzle Branch, 21000 Brookpk Road, Cleveland, OH 44135 USA.
NR 30
TC 0
Z9 0
U1 0
U2 0
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
EI 1533-3868
J9 J AIRCRAFT
JI J. Aircr.
PD JAN
PY 2017
VL 54
IS 1
BP 125
EP 134
DI 10.2514/1.C033623
PG 10
WC Engineering, Aerospace
SC Engineering
GA EM8HY
UT WOS:000395553300012
ER
PT J
AU Orr, JS
Dennehy, CJ
AF Orr, Jeb S.
Dennehy, Cornelius J.
TI Analysis of the X-15 Flight 3-65-97 Divergent Limit-Cycle Oscillation
SO JOURNAL OF AIRCRAFT
LA English
DT Article
AB A brief history of the X-15-3 adaptive control system and an analysis of the destructive limit-cycle oscillation that occurred during its final November 1967 flight are presented. The X-15 was a piloted single-seat rocket-propelled hypersonic research aircraft operated by the NASA Flight Research Center from 1959 until 1968. Due to the limited information previously available in the public domain and the 1968 decision by the accident investigation board to forego detailed analysis of the adaptive control system's role in the accident, it was widely assumed in the adaptive controls community that an anomalous behavior of the adaptive component caused the loss of control. Notwithstanding the complex human factors and subsystem failures that contributed to the accident, it is shown that the adaptation dynamics were not a causal factor. The limit cycle observed in the flight data is reproduced in a nonlinear time-domain simulation. Describing function analysis reveals that the instability was caused by a latent design error in the inner-loop structural filters that did not account for the nonlinear behavior of the X-15 servoactuator under rate saturation when coupled with the lightly damped aircraft longitudinal mode at high Mach numbers.
C1 [Orr, Jeb S.] Charles Stark Draper Lab Inc, Dynam & Control, Huntsville, AL 35812 USA.
[Dennehy, Cornelius J.] NASA, Engn & Safety Ctr, Guidance Nav & Control Tech Discipline Team, Greenbelt, MD 20771 USA.
RP Orr, JS (reprint author), Charles Stark Draper Lab Inc, Dynam & Control, Huntsville, AL 35812 USA.
EM jorr@draper.com
FU NASA Engineering and Safety Center [TI-14-00957]
FX This work was prepared by The Charles Stark Draper Laboratory, Inc., in
support of NASA Engineering and Safety Center's assessment TI-14-00957.
The contributions of Immanuel Barshi and Irving Statler (NASA Ames
Research Center) were instrumental in understanding the human factors of
the accident. The authors would also like to thank Mike Ruth (Orbital
ATK) and Miguel De Virgilio (The Aerospace Corporation) for the many
insightful discussions regarding this analysis.
NR 27
TC 0
Z9 0
U1 0
U2 0
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0021-8669
EI 1533-3868
J9 J AIRCRAFT
JI J. Aircr.
PD JAN
PY 2017
VL 54
IS 1
BP 135
EP 148
DI 10.2514/1.C033703
PG 14
WC Engineering, Aerospace
SC Engineering
GA EM8HY
UT WOS:000395553300013
ER
PT J
AU Minchew, BM
Simons, M
Riel, B
Milillo, P
AF Minchew, B. M.
Simons, M.
Riel, B.
Milillo, P.
TI Tidally induced variations in vertical and horizontal motion on Rutford
Ice Stream, West Antarctica, inferred from remotely sensed observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-EARTH SURFACE
LA English
DT Article
DE synthetic aperture radar; glacier mechanics; ice-ocean interactions; ice
shelf buttressing; ice-bed mechanics; ice rheology
ID RADAR INTERFEROMETRY; BASAL MECHANICS; PINE ISLAND; OCEAN TIDES; INSAR
DATA; SHEET; VELOCITY; FLOW; MARGINS; SHELF
AB To better understand the influence of stress changes over floating ice shelves on grounded ice streams, we develop a Bayesian method for inferring time-dependent 3-D surface velocity fields from synthetic aperture radar (SAR) and optical remote sensing data. Our specific goal is to observe ocean tide-induced variability in vertical ice shelf position and horizontal ice stream flow. Thus, we consider the special case where observed surface displacement at a given location can be defined by a 3-D secular velocity vector, a family of 3-D sinusoidal functions, and a correction to the digital elevation model used to process the SAR data. Using nearly 9months of SAR data collected from multiple satellite viewing geometries with the COSMO-SkyMed 4-satellite constellation, we infer the spatiotemporal response of Rutford Ice Stream, West Antarctica, to ocean tidal forcing. Consistent with expected tidal uplift, inferred vertical motion over the ice shelf is dominated by semidiurnal and diurnal tidal constituents. Horizontal ice flow variability, on the other hand, occurs primarily at the fortnightly spring-neap tidal period (M-sf). We propose that periodic grounding of the ice shelf is the primary mechanism for translating vertical tidal motion into horizontal flow variability, causing ice flow to accelerate first and most strongly over the ice shelf. Flow variations then propagate through the grounded ice stream at a mean rate of approximate to 29km/d and decay quasi-linearly with distance over approximate to 85km upstream of the grounding zone.
C1 [Minchew, B. M.; Simons, M.; Riel, B.] CALTECH, Div Geol & Planetary Sci, Seismol Lab, Pasadena, CA 91125 USA.
[Minchew, B. M.] British Antarctic Survey, Cambridge, England.
[Milillo, P.] Univ Basilicata, Sch Engn, Potenza, Italy.
[Milillo, P.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Minchew, BM (reprint author), CALTECH, Div Geol & Planetary Sci, Seismol Lab, Pasadena, CA 91125 USA.; Minchew, BM (reprint author), British Antarctic Survey, Cambridge, England.
EM bremin15@bas.ac.uk
OI Milillo, Pietro/0000-0002-1171-3976; Simons, Mark/0000-0003-1412-6395
FU NASA [NNX14AH80G]; NSF Earth Sciences Postdoctoral Fellowship award
[1452587]; NASA Earth and Space Sciences fellowship; NASA postdoctoral
fellowship
FX We thank E. Smith and A. Smith for providing the seismic data, and we
benefitted from conversations with H. Gudmundsson, H. Martens, V. Tsai,
J. Thompson, and P. Agram. B.M. was partially funded by NASA Cyospheric
Sciences award NNX14AH80G, NSF Earth Sciences Postdoctoral Fellowship
award 1452587, and donations from the Albert Parvin and ARCS LA Chapter
foundations. B.R. was partially funded by a NASA Earth and Space
Sciences fellowship. P.M. was partially funded by a NASA postdoctoral
fellowship, and much of this work was completed while he was a visiting
student at the California Institute of Technology. Original COSMO-SkyMed
products (copyright ASI-Agenzia Spaziale Italiana, 2013-2016) are
archived at JPL and were processed under license from ASI as part of a
collaborative project between CIDOT and JPL/Caltech. Displacement fields
and other processed SAR data are available from the authors upon
request, and the velocity field components will be archived at the
National Snow and Ice Data Center (NSIDC; see nsidc.org). Software used
to infer time-dependent, 3-D velocity fields is freely available at
https://github.com/bminchew/fourDvel.
NR 94
TC 1
Z9 1
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9003
EI 2169-9011
J9 J GEOPHYS RES-EARTH
JI J. Geophys. Res.-Earth Surf.
PD JAN
PY 2017
VL 122
IS 1
BP 167
EP 190
DI 10.1002/2016JF003971
PG 24
WC Geosciences, Multidisciplinary
SC Geology
GA EL8XY
UT WOS:000394904900009
ER
PT J
AU Lee, CC
Kibblewhite, RE
Paavola, CD
Orts, WJ
Wagschal, K
AF Lee, Charles C.
Kibblewhite, Rena E.
Paavola, Chad D.
Orts, William J.
Wagschal, Kurt
TI Production of D-Xylonic Acid from Hemicellulose Using Artificial Enzyme
Complexes
SO JOURNAL OF MICROBIOLOGY AND BIOTECHNOLOGY
LA English
DT Article
DE Lignocellulose; multienzyme assembly; bioconversion; glucuronoxylan;
xylonic acid
ID PAENIBACILLUS SP DG-22; D-XYLOSE; SACCHAROMYCES-CEREVISIAE; NANOPARTICLE
ARRAYS; CHAPERONIN PROTEIN; XYLANASE; BIOMASS; CELLULOSOMES; CLONING;
1,2,4-BUTANETRIOL
AB Lignocellulosic biomass represents a potentially large resource to supply the world's fuel and chemical feedstocks. Enzymatic bioconversion of this substrate offers a reliable strategy for accessing this material under mild reaction conditions. Owing to the complex nature of lignocellulose, many different enzymatic activities are required to function in concert to perform efficient transformation. In nature, large multienzyme complexes are known to effectively hydrolyze lignocellulose into constituent monomeric sugars. We created artificial complexes of enzymes, called rosettazymes, in order to hydrolyze glucuronoxylan, a common lignocellulose component, into its cognate sugar D-xylose and then further convert the D-xylose into D-xylonic acid, a Department of Energy top-30 platform chemical. Four different types of enzymes (endoxylanase, alpha-glucuronidase, beta-xylosidase, and xylose dehydrogenase) were incorporated into the artificial complexes. We demonstrated that tethering our enzymes in a complex resulted in significantly more activity (up to 71%) than the same amount of enzymes free in solution. We also determined that varying the enzyme composition affected the level of complex-related activity enhancement as well as overall yield.
C1 [Lee, Charles C.; Kibblewhite, Rena E.; Orts, William J.; Wagschal, Kurt] USDA ARS WRRC, Bioprod Res Unit, Albany, CA 94710 USA.
[Paavola, Chad D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Lee, CC (reprint author), USDA ARS WRRC, Bioprod Res Unit, Albany, CA 94710 USA.
EM Charles.Lee@ars.usda.gov
FU United States Department of Agriculture [CRIS 2030-41000-054-00];
National Institute of Food and Agriculture [2012-03998]
FX We thank Bruce Mackey and Linda Whitehand for consultations on the
statistical design of the experiments. This work was supported by the
United States Department of Agriculture (CRIS 2030-41000-054-00) and
National Institute of Food and Agriculture (grant 2012-03998). The
mention of firm names or trade products does not imply that they are
endorsed or recommended by the US Department of Agriculture (USDA) over
other firms or similar products not mentioned. The USDA is an equal
opportunity provider and employer.
NR 49
TC 0
Z9 0
U1 1
U2 1
PU KOREAN SOC MICROBIOLOGY & BIOTECHNOLOGY
PI SEOUL
PA KOREA SCI TECHNOL CENTER #507, 635-4 YEOGSAM-DONG, KANGNAM-GU, SEOUL
135-703, SOUTH KOREA
SN 1017-7825
EI 1738-8872
J9 J MICROBIOL BIOTECHN
JI J. Microbiol. Biotechnol.
PD JAN
PY 2017
VL 27
IS 1
BP 77
EP 83
DI 10.4014/jmb.1606.06041
PG 7
WC Biotechnology & Applied Microbiology; Microbiology
SC Biotechnology & Applied Microbiology; Microbiology
GA EO2PG
UT WOS:000396537800011
ER
PT J
AU Terborg, A
Stano, GT
AF Terborg, Amanda
Stano, Geoffrey T.
TI Impacts to Aviation Weather Center Operations Using Total Lightning
Observations from the Pseudo-GLM
SO JOURNAL OF OPERATIONAL METEOROLOGY
LA English
DT Article
ID VHF RADIO PICTURES; MAPPING ARRAY; SYSTEM; SATELLITE
AB The Aviation Weather Center (AWC) is responsible for delivering accurate, consistent, and timely weather information for safe and efficient flight across the United States airspace system along with international obligations. One of the key concerns for forecasters is the prediction and monitoring of convection which directly affects air routes as well as ground operations. Lightning observations are a vital component of available observations helping to confirm the presence of convection and verify forecasts. Up to this time the AWC has relied solely on ground-based cloud-to-ground only detection networks. With the upcoming launch of the Geostationary Lightning Mapper (GLM) aboard GOES-R, the AWC has the opportunity to expand the use of lightning observations by observing total lightning (i.e., the combination of both cloud-to-ground and intra-cloud observations). AWC and NASA's Short-term Prediction Research and Transition Center (SPoRT) have collaborated to assess a demonstration GLM product, the pseudo-GLM, derived from ground-based lightning mapping arrays. This collaboration has focused on the utility of using total lightning in aviation weather forecasting in preparation for the GLM instrument. This paper presents several small cases identified by forecasters using the pseudo-GLM data in operations and discusses the role of GLM data in the future.
C1 [Terborg, Amanda] Univ Wisconsin, NWS NCEP Aviat Weather Ctr, CIMSS, SSEC, Kansas City, MO USA.
[Stano, Geoffrey T.] ENSCO Inc, NASA, Short Term Predict Res & Transit Ctr SPoRT, Huntsville, AL USA.
RP Terborg, A (reprint author), 7220 NW 101st Terr,Rm 101, Kansas City, MO 64153 USA.
EM amanda.terborg@noaa.gov
FU GOES-R
FX The authors would like to thank the GOES-R Proving Ground for funding
these total lightning efforts. Additionally, the authors wish to thank
the Aviation Weather Center forecasters, particularly Ed Holicky, for
their invaluable feedback and case examples used in the evaluation and
with this paper.
NR 34
TC 0
Z9 0
U1 0
U2 0
PU NATL WEATHER ASSOC
PI NORMAN
PA 350 DAVID L BOREN BLVD, STE 2750, NORMAN, OK USA
SN 2325-6184
J9 J OPER METEOROL
JI J. Oper. Meteorol.
PY 2017
VL 5
IS 1
DI 10.15191/nwajom.2017.0501
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EM4GJ
UT WOS:000395271200001
ER
PT J
AU Hambric, SA
Shepherd, MR
Schiller, NH
Snider, R
May, C
AF Hambric, Stephen A.
Shepherd, Micah R.
Schiller, Noah H.
Snider, Royce
May, Carl
TI Quieting a Rib-Framed Honeycomb Core Sandwich Panel for a Rotorcraft
Roof
SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY
LA English
DT Article
ID SOUND-TRANSMISSION LOSS
AB A rotorcraft roof composite sandwich panel has been redesigned to optimize sound power transmission loss (TL) and minimize structure-borne sound for frequencies between 1 and 4 kHz where gear-meshing noise from the transmission has the most impact on speech intelligibility. The roof section, framed by a grid of ribs, was originally constructed of a single honeycomb core/composite face sheet sandwich panel. The original panel has acoustic coincidence frequencies near 600 Hz, leading to poor TL across the frequency range of 1-4 kHz. To quiet the panel, the cross section was split into two thinner sandwich subpanels separated by an air gap. The air gap was sized to target the fundamental mass-spring-mass resonance of the panel system to less than 500 Hz, well below the frequency range of interest. The panels were designed to withstand structural loading from normal rotorcraft operation, as well as "man-on-the-roof" static loads experienced during maintenance operations. Thin layers of viscoelastomer were included in the face sheet ply layups, increasing panel damping loss factors from about 0.01 to 0.05. TL measurements show the optimized panel provides 6-11 dB of acoustic TL improvement and 6-15 dB of structure-borne sound reduction at critical rotorcraft transmission tonal frequencies. Analytic panel TL theory simulates the measured performance within 3 dB over most frequencies. Detailed finite element/boundary element modeling simulates TL slightly more accurately, within 2 dB for frequencies up to 4 kHz, and also simulates structure-borne sound well, generally within 3 dB.
C1 [Hambric, Stephen A.; Shepherd, Micah R.] Penn State Univ, ARL, State Coll, PA 16801 USA.
[Schiller, Noah H.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Snider, Royce; May, Carl] Bell Helicopter Textron, Ft Worth, TX USA.
RP Hambric, SA (reprint author), Penn State Univ, ARL, State Coll, PA 16801 USA.
EM sah19@arl.psu.edu
FU NASA [NNL11AA02C, NRA NNH09ZEA001N]
FX The authors thank NASA for their support under NASA Contract #
NNL11AA02C, under NRA NNH09ZEA001N, Subtopic A. 3.3.1: Fundamental
Vibro-Acoustic Modeling and Validation. We also thank David Gries of the
3M corporation for suggesting the use of VHB 9469 viscoelastic material.
NR 15
TC 0
Z9 0
U1 1
U2 1
PU AMER HELICOPTER SOC INC
PI ALEXANDRIA
PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA
SN 0002-8711
EI 2161-6027
J9 J AM HELICOPTER SOC
JI J. Am. Helicopter Soc.
PD JAN
PY 2017
VL 62
IS 1
AR 012009
DI 10.4050/JAHS.62.012009
PG 10
WC Engineering, Aerospace
SC Engineering
GA EK7TQ
UT WOS:000394128500009
ER
PT J
AU Lakshminarayan, VK
Sitaraman, J
Wissink, AM
AF Lakshminarayan, Vinod K.
Sitaraman, Jayanarayanan
Wissink, Andrew M.
TI Application of Strand Grid Framework to Complex Rotorcraft Simulations
SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY
LA English
DT Article
ID FLOW COMPUTATIONS; ALGORITHM
AB The strand grid approach is a flow solution method where a prismatic-like grid using "strands" is grown to a short distance from the body surface to capture the viscous boundary layer, and the rest of the domain is covered using an adaptive Cartesian grid. The approach offers several advantages in terms of nearly automatic grid generation and adaptation, ability to implement fast and efficient flow solvers that use structured data in both the strand and Cartesian grids, and the development of an efficient and highly scalable domain connectivity algorithm. An earlier work by the authors introduced a strand grid solver called mStrand, which will appear in future versions of the HPCMP CREATETM-AV Helios framework. This paper presents application of the mStrand/Helios strand grid framework for complex rotorcraft problems. The test cases presented are the UH-60A high-speed forward flight and high-altitude stall problems as well as the HART II blade-vortex interaction problem. The results show that the solution obtained using the strand grid framework is as good as that obtained using well-established structured and unstructured solution methodologies.
C1 [Lakshminarayan, Vinod K.] NASA, Ames Res Ctr, Sci & Tech Corp, Moffett Field, CA 94035 USA.
[Sitaraman, Jayanarayanan] Parallel Geometr Algorithms LLC, Sunnyvale, CA USA.
[Wissink, Andrew M.] US Army, Aviat Dev Directorate ADD AMRDEC, Moffett Field, CA USA.
RP Lakshminarayan, VK (reprint author), NASA, Ames Res Ctr, Sci & Tech Corp, Moffett Field, CA 94035 USA.
EM vinod.k.lakshminarayan.ctr@mail.mil
FU U.S. Department of Defense HPC Modernization Program Office
FX Material presented in this paper is a product of the CREATE-AV Element
of the Computational Research and Engineering for Acquisition Tools and
Environments (CREATE) Program sponsored by the U.S. Department of
Defense HPC Modernization Program Office. This work was conducted at the
High Performance Computing Institute for Advanced Rotorcraft Modeling
and Simulation (HIARMS). The authors would like to acknowledge Buvana
Jayaraman and Beatrice Roget for providing help while setting up various
cases.
NR 43
TC 0
Z9 0
U1 0
U2 0
PU AMER HELICOPTER SOC INC
PI ALEXANDRIA
PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA
SN 0002-8711
EI 2161-6027
J9 J AM HELICOPTER SOC
JI J. Am. Helicopter Soc.
PD JAN
PY 2017
VL 62
IS 1
AR 012008
DI 10.4050/JAHS.62.012008
PG 16
WC Engineering, Aerospace
SC Engineering
GA EK7TQ
UT WOS:000394128500008
ER
PT J
AU Ramasamy, M
Yamauchi, GK
AF Ramasamy, Manikandan
Yamauchi, Gloria K.
TI Using Model-Scale Tandem-Rotor Measurements in Ground Effect to
Understand Full-Scale CH-47D Outwash
SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY
LA English
DT Article
ID JET
AB Downwash and outwash characteristics of a model-scale tandem-rotor system in the presence of the ground were analyzed by identifying and understanding the physical mechanisms contributing to the observed flow field behavior. A building block approach was followed in simplifying the problem, separating the effects of the fuselage, effects of one rotor on the other, etc. Flow field velocities were acquired in a vertical plane at four aircraft azimuths of a small-scale tandem rotor system using the particle image velocimetry technique for radial distances up to four times the rotor diameter. Results were compared against full-scale CH-47D measurements. Excellent correlation was found between the small-and full-scale mean flow fields (after appropriate normalization using rotor and wall jet parameters). Following the scalability analysis, the effect of rotor height on the outwash was also studied. Close to the aircraft, an increase in rotor height above ground decreased the outwash velocity at all aircraft azimuths. However, farther away, the longitudinal and lateral axes of the aircraft showed increasing and decreasing outwash velocities, respectively, with increasing rotor height. Baseline rotor measurements were made out-of-ground effect to understand the nature of inflow distribution for realistic rotor configurations and their modified characteristics in the presence of the ground.
C1 [Ramasamy, Manikandan] US Army, Aviat Dev Directorate AFDD, Aviat & Missile Res Dev & Engn Ctr, Res Dev & Engn Command,Ames Res Ctr, Moffett Field, CA 94035 USA.
[Yamauchi, Gloria K.] NASA, Ames Res Ctr, Aeromech Off, Moffett Field, CA 94035 USA.
RP Ramasamy, M (reprint author), US Army, Aviat Dev Directorate AFDD, Aviat & Missile Res Dev & Engn Ctr, Res Dev & Engn Command,Ames Res Ctr, Moffett Field, CA 94035 USA.
EM manikandan.ramasamy.civ@mail.mil
NR 30
TC 0
Z9 0
U1 0
U2 0
PU AMER HELICOPTER SOC INC
PI ALEXANDRIA
PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA
SN 0002-8711
EI 2161-6027
J9 J AM HELICOPTER SOC
JI J. Am. Helicopter Soc.
PD JAN
PY 2017
VL 62
IS 1
AR 012004
DI 10.4050/JAHS.62.012004
PG 14
WC Engineering, Aerospace
SC Engineering
GA EK7TQ
UT WOS:000394128500004
ER
PT J
AU Brandis, AM
Johnston, CO
Cruden, BA
Prabhu, DK
AF Brandis, A. M.
Johnston, C. O.
Cruden, B. A.
Prabhu, D. K.
TI Equilibrium Radiative Heating from 9.5 to 15.5km/s for Earth Atmospheric
Entry
SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER
LA English
DT Article
ID LUNAR-RETURN CONDITIONS; SHOCK-LAYER RADIATION; II FLIGHT EXPERIMENT
AB This paper presents an overview of the analysis and measurements of equilibrium radiation obtained in NASA Ames Research Center's Electric Arc Shock Tube facility as a part of recent testing aimed at reaching shock velocities up to 15.5km/s. The goal of these experiments was to measure the level of radiation encountered during high-speed Earth entry conditions, such as would be relevant for an asteroid, interplanetary, or lunar return mission. These experiments provided the first spectrally and spatially resolved data for high-speed Earth entry and cover conditions ranging from 9.5 to 15.5km/s at 13.3 and 26.6Pa (0.1 and 0.2torr). The present analysis endeavors to provide a detailed comparison of shock tube radiation measurements and simulations at high-speed conditions. A comprehensive comparison between the spectrally resolved absolute equilibrium radiance measured in the Electric Arc Shock Tube facility and NASA's predictive tools is presented. To provide a more accurate representation of the agreement between the experimental and simulation results, the integrated value of radiance is compared across four spectral regions (vacuum ultraviolet, ultraviolet/ visible, visible/ near infrared, and infrared) as a function of velocity. Results have generally shown excellent agreement between the two codes and the shock tube data for the ultraviolet through infrared spectral regions; however, discrepancies have been identified in the vacuum ultraviolet. As a result of the analysis presented in this paper, an updated parametric uncertainty for high-speed radiation in air is evaluated to be [9.0%, -6.3%]. Furthermore, due to the nature of the radiating environment at these high shock speeds, initial calculations aimed at modeling phenomena that become more significant with increasing shock speed are performed. These phenomena include analyzing the radiating species emitting ahead of the shock and the increased significance of radiative cooling mechanisms.
C1 [Brandis, A. M.; Cruden, B. A.; Prabhu, D. K.] ERC Inc, NASA, Ames Res Ctr, Aerothermodynam Branch, Moffett Field, CA 94035 USA.
[Johnston, C. O.] NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23669 USA.
RP Brandis, AM (reprint author), ERC Inc, NASA, Ames Res Ctr, Aerothermodynam Branch, Moffett Field, CA 94035 USA.
EM aaron.m.brandis@nasa.gov
FU NASA's Entry Systems Modeling project; NASA Ames Research Center
[NNA10DE12C, NNA15BB15C, NAS2-03144]; ERC Inc. [NNA10DE12C]; AMA Inc.
[NNA15BB15C]; University Affiliated Research Center
FX The authors would like to thank NASA's Entry Systems Modeling project
for their funding of this work. At the time of this work, Aaron Brandis,
Brett Cruden and Dinesh Prabhu were supported through the NNA10DE12C
contract between NASA Ames Research Center and ERC Inc. Aaron Brandis,
Brett Cruden and Dinesh Prabhu are now currently employed through the
NNA15BB15C contract between NASA Ames Research Center and AMA Inc. For a
portion of this work, Aaron Brandis was also supported through the
NAS2-03144 contract between NASA Ames Research Center and the University
Affiliated Research Center.
NR 34
TC 0
Z9 0
U1 0
U2 0
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0887-8722
EI 1533-6808
J9 J THERMOPHYS HEAT TR
JI J. Thermophys. Heat Transf.
PD JAN
PY 2017
VL 31
IS 1
BP 178
EP 192
DI 10.2514/1.T4878
PG 15
WC Thermodynamics; Engineering, Mechanical
SC Thermodynamics; Engineering
GA EM1UK
UT WOS:000395102400018
ER
PT J
AU Bae, SY
Korniski, RJ
Shearn, M
Manohara, HM
Shahinian, H
AF Bae, Sam Y.
Korniski, Ronald J.
Shearn, Michael
Manohara, Harish M.
Shahinian, Hrayr
TI 4-mm-diameter three-dimensional imaging endoscope with steerable camera
for minimally invasive surgery (3-D-MARVEL)
SO NEUROPHOTONICS
LA English
DT Article
DE endoscopy; stereo imaging; minimally invasive surgery; three-dimensional
imaging; three-dimensional camera
ID STEREOPSIS; BLUR
AB High-resolution three-dimensional (3-D) imaging (stereo imaging) by endoscopes in minimally invasive surgery, especially in space-constrained applications such as brain surgery, is one of the most desired capabilities. Such capability exists at larger than 4-mm overall diameters. We report the development of a stereo imaging endoscope of 4-mm maximum diameter, called Multiangle, Rear-Viewing Endoscopic Tool (MARVEL) that uses a single-lens system with complementary multibandpass filter (CMBF) technology to achieve 3-D imaging. In addition, the system is endowed with the capability to pan from side-to-side over an angle of +/- 25 deg, which is another unique aspect of MARVEL for such a class of endoscopes. The design and construction of a single-lens, CMBF aperture camera with integrated illumination to generate 3-D images, and the actuation mechanism built into it is summarized. (C) 2017 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Bae, Sam Y.; Korniski, Ronald J.; Shearn, Michael; Manohara, Harish M.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Shahinian, Hrayr] Skull Base Inst, 8635 West Third St,Suite 1170-W, Los Angeles, CA 90048 USA.
[Bae, Sam Y.] NuVasive Inc, 101 Enterprise,Suite 100, Aliso Viejo, CA 92656 USA.
[Shearn, Michael] Terra Bella Google, 1600 Amphitheatre Pkwy, Mountain View, CA 94043 USA.
RP Manohara, HM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Harish.Manohara@jpl.nasa.gov
FU Skull Base Institute of Los Angeles, California; National Aeronautics
and Space Administration
FX We thank Dr. Pantazis Mouroulis for all the advice on optics design, Dr.
John Choi [ex-Jet Propulsion Laboratory (JPL)], and summer students
Allen Ream, Eric Fritz, and Andrew Strongrich for their valuable
contributions to this development. This work was carried out with
funding from the Skull Base Institute of Los Angeles, California. This
research was carried out at the JPL, California Institute of Technology,
under a contract with the National Aeronautics and Space Administration.
Government sponsorship is acknowledged.
NR 27
TC 0
Z9 0
U1 5
U2 5
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 2329-423X
EI 2329-4248
J9 NEUROPHOTONICS
JI Neurophotonics
PD JAN
PY 2017
VL 4
IS 1
AR 011008
DI 10.1117/1.NPh.4.1.011008
PG 7
WC Neurosciences; Optics
SC Neurosciences & Neurology; Optics
GA EO0DM
UT WOS:000396368500008
PM 27752521
ER
PT J
AU Vasefi, F
MacKinnon, N
Farkas, DL
Katebb, B
AF Vasefi, Fartash
MacKinnon, Nicholas
Farkas, Daniel L.
Katebb, Babak
TI Review of the potential of optical technologies for cancer diagnosis in
neurosurgery: a step toward intraoperative neurophotonics
SO NEUROPHOTONICS
LA English
DT Review
DE neurophotonics; optical imaging; brain tumor; image-guided therapy;
intraoperative brain mapping
ID RESOLVED FLUORESCENCE SPECTROSCOPY; MAGNETIC-RESONANCE; COHERENCE
TOMOGRAPHY; TUMOR RESECTION; BRAIN-TUMORS; GUIDED NEUROSURGERY; INITIAL
EXPERIENCE; GLIOMA SURGERY; WHITE-MATTER; ULTRASOUND
AB Advances in image-guided therapy enable physicians to obtain real-time information on neurological disorders such as brain tumors to improve resection accuracy. Image guidance data include the location, size, shape, type, and extent of tumors. Recent technological advances in neurophotonic engineering have enabled the development of techniques for minimally invasive neurosurgery. Incorporation of these methods in intraoperative imaging decreases surgical procedure time and allows neurosurgeons to find remaining or hidden tumor or epileptic lesions. This facilitates more complete resection and improved topology information for postsurgical therapy (i.e., radiation). We review the clinical application of recent advances in neurophotonic technologies including Raman spectroscopy, thermal imaging, optical coherence tomography, and fluorescence spectroscopy, highlighting the importance of these technologies in live intraoperative tissue mapping during neurosurgery. While these technologies need further validation in larger clinical trials, they show remarkable promise in their ability to help surgeons to better visualize the areas of abnormality and enable safe and successful removal of malignancies. (C) The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI.
C1 [Vasefi, Fartash; MacKinnon, Nicholas; Farkas, Daniel L.] Spectral Mol Imaging Inc, 13412 Ventura Blvd,Suite 250, Sherman Oaks, CA 91423 USA.
[Vasefi, Fartash; Katebb, Babak] Brain Mapping Fdn, 8159 Santa Monica Blvd,Suite 200, West Hollywood, CA 90046 USA.
[Vasefi, Fartash; Katebb, Babak] SBMT, 8159 Santa Monica Blvd,Suite 200, West Hollywood, CA 90046 USA.
[Farkas, Daniel L.] Univ Southern Calif, Dept Biomed Engn, 1042 Downey Way, Los Angeles, CA 90089 USA.
[Katebb, Babak] Calif Neurosurg Inst, 25751 McBean Pkwy 305, Santa Clarita, CA 91355 USA.
[Katebb, Babak] NASA, NCNBE, Res Pk,POB 23, Moffett Field, CA 94035 USA.
RP Vasefi, F (reprint author), Spectral Mol Imaging Inc, 13412 Ventura Blvd,Suite 250, Sherman Oaks, CA 91423 USA.; Vasefi, F; Katebb, B (reprint author), Brain Mapping Fdn, 8159 Santa Monica Blvd,Suite 200, West Hollywood, CA 90046 USA.; Vasefi, F; Katebb, B (reprint author), SBMT, 8159 Santa Monica Blvd,Suite 200, West Hollywood, CA 90046 USA.; Katebb, B (reprint author), Calif Neurosurg Inst, 25751 McBean Pkwy 305, Santa Clarita, CA 91355 USA.; Katebb, B (reprint author), NASA, NCNBE, Res Pk,POB 23, Moffett Field, CA 94035 USA.
EM fvasefi@opmol.com; Babak.Kateb@WorldBrainMapping.Org
FU US Department of Health and Human Services; National Institutes of
Health (under NCI SBIR Grant) [1R44CA183169-01A1]
FX Spectral Molecular Imaging, Inc. (D. L. Farkas, PI) acknowledges support
from the US Department of Health and Human Services (under the
Qualifying Therapeutic Discovery Program of the Patent Protection and
Affordable Care Act of 2010), and by the National Institutes of Health
(under NCI SBIR Grant No. 1R44CA183169-01A1). This collaborative project
is also made possible by Society for Brain Mapping & Therapeutics, Brain
Mapping Foundation, and National Center for NanoBioElectronics and
California Neurosurgical Institute.
NR 75
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U2 0
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 2329-423X
EI 2329-4248
J9 NEUROPHOTONICS
JI Neurophotonics
PD JAN
PY 2017
VL 4
IS 1
AR 011010
DI 10.1117/1.NPh.4.1.011010
PG 10
WC Neurosciences; Optics
SC Neurosciences & Neurology; Optics
GA EO0DM
UT WOS:000396368500010
PM 28042588
ER
PT J
AU Liston, DB
Wong, LR
Stone, LS
AF Liston, Dorion B.
Wong, Lily R.
Stone, Leland S.
TI Oculometric Assessment of Sensorimotor Impairment Associated with TBI
SO OPTOMETRY AND VISION SCIENCE
LA English
DT Article
DE sensorimotor; traumatic brain injury; diagnostic tool; pursuit eye
movement; neurological impairment
ID TRAUMATIC BRAIN-INJURY; CLOSED-HEAD INJURY; PURSUIT EYE-MOVEMENTS;
SMOOTH-PURSUIT; VISUAL TRACKING; NERVE PALSIES; DEFICITS; CONCUSSION;
PERCEPTION; VELOCITY
AB Purpose. Diffuse tissue damage from impact or blast traumatic brain injury (TBI) degrades information processing throughout the brain, often resulting in impairments in sensorimotor function. We have developed an eye-movement assessment test, consisting of a simple, appropriately randomized, radial tracking task together with a broad set of oculometric measures that can be combined to yield a sensitive overall indicator of sensorimotor functional status. We show here that this multidimensional method can be used to detect and characterize sensorimotor deficits associated with TBI.
Methods. To compare dynamic visuomotor processing of TBI subjects (n = 34) with a separate control population (n = 41), we used the Comprehensive Oculometric Behavioral Response Assessment (COBRA) method (Liston & Stone, J Vision. 14: 12, 2014) to quantify 10 performance metrics for each subject. Each TBI subject's set of oculometrics was then combined to compute a single TBI impairment vector whose magnitude we refer to as the impairment index.
Results. In our TBI population, several individual oculometrics were significantly degraded, including pursuit latency, initial pursuit acceleration, pursuit gain, catch-up saccade amplitude, proportion smooth tracking, and speed responsiveness. Furthermore, the TBI impairment index discriminated TBI subjects from controls with an 81% probability that increased with self-reported TBI severity; although the 9 subjects self-reporting "little-to-no'' residual impairment were statistically indistinguishable from controls (58% probability), the remaining 25 subjects were easily detectable (91% probability). Given the demonstrated link between higher-order visual perception/cognition and eye movements, we interpret the observed TBI-related impairments as degradations in the speed, accuracy, and precision of information processing within cortical circuits supporting higher-order visual processing and sensorimotor control, not just low-level brainstem motor deficits.
Conclusions. We conclude that multidimensional oculometric testing could be used as a sensitive screen for subtle neurological signs of subclinical neurological insults, to quantify functional impairment, to monitor deterioration or recovery, and to evaluate treatment efficacy.
C1 [Liston, Dorion B.; Wong, Lily R.; Stone, Leland S.] NASA, Ames Res Ctr, Mountain View, CA USA.
[Liston, Dorion B.; Wong, Lily R.] San Jose State Univ, San Jose, CA 95192 USA.
RP Liston, DB (reprint author), San Jose State Univ, Bldg 262,Room 222,POB 1,MS 262-2, Moffett Field, CA 94035 USA.
EM dorion.liston@gmail.com
FU Office of Naval Research Force Health Protection program
[N0001415IP00028/30]
FX This work has been supported by the Office of Naval Research Force
Health Protection program (N0001415IP00028/30). The authors thank Laura
Jamison from Santa Clara Valley Medical Center for invaluable assistance
in recruiting subjects. DL and LS share a non-provisional patent
application (application #61994673), which is a subject of this
publication, not yet licensed or otherwise commercialized.
NR 40
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U1 0
U2 0
PU LIPPINCOTT WILLIAMS & WILKINS
PI PHILADELPHIA
PA TWO COMMERCE SQ, 2001 MARKET ST, PHILADELPHIA, PA 19103 USA
SN 1040-5488
EI 1538-9235
J9 OPTOMETRY VISION SCI
JI Optom. Vis. Sci.
PD JAN
PY 2017
VL 94
IS 1
BP 51
EP 59
PG 9
WC Ophthalmology
SC Ophthalmology
GA EM5ZZ
UT WOS:000395393900008
PM 27391532
ER
PT J
AU Wilhelm, MB
Davila, AF
Eigenbrode, JL
Parenteau, MN
Jahnke, LL
Liu, XL
Summons, RE
Wray, JJ
Stamos, BN
O'Reilly, SS
Williams, A
AF Wilhelm, Mary Beth
Davila, Alfonso F.
Eigenbrode, Jennifer L.
Parenteau, Mary N.
Jahnke, Linda L.
Liu, Xiao-Lei
Summons, Roger E.
Wray, James J.
Stamos, Brian N.
O'Reilly, Shane S.
Williams, Amy
TI Xeropreservation of functionalized lipid biomarkers in hyperarid soils
in the Atacama Desert
SO ORGANIC GEOCHEMISTRY
LA English
DT Article
DE Preservation; Lipid; Biomarker; Desert; Atacama; Mars; Hyperarid; FAME
ID ORGANIC-MATTER; FATTY-ACIDS; EL-NINO; CHILE; LIFE; MARS; MICROORGANISMS;
BIOSYNTHESIS; PRESERVATION; SEDIMENTS
AB Our understanding of long-term organic matter preservation comes mostly from studies in aquatic systems. In contrast, taphonomic processes in extremely dry environments are relatively understudied and are poorly understood. We investigated the accumulation and preservation of lipid biomarkers in hyperarid soils in the Yungay region of the Atacama Desert. Lipids from seven soil horizons in a 2.5 m vertical profile were extracted and analyzed using GC-MS and LC-MS. Diagnostic functionalized lipids and geolipids were detected and increased in abundance and diversity with depth. Deeper clay units contain fossil organic matter (radiocarbon dead) that has been protected from rainwater since the onset of hyperaridity. We show that these clay units contain lipids in an excellent state of structural preservation with functional groups and unsaturated bonds in carbon chains. This indicates that minimal degradation of lipids has occurred in these soils since the time of their deposition between > 40,000 and 2 million years ago. The exceptional structural preservation of biomarkers is likely due to the long-term hyperaridity that has minimized microbial and enzymatic activity, a taphonomic process we term xeropreservation (i.e., preservation by drying). The degree of biomarker preservation allowed us to reconstruct major changes in ecology in the Yungay region that reflect a shift in hydrological regime from wet to dry since the early Quaternary. Our results suggest that hyperarid environments, which comprise 7.5% of the continental landmass, could represent a rich and relatively unexplored source of paleobiological information on Earth. Published by Elsevier Ltd.
C1 [Wilhelm, Mary Beth; Wray, James J.] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
[Wilhelm, Mary Beth; Davila, Alfonso F.; Parenteau, Mary N.; Jahnke, Linda L.] NASA, Space Sci & Astrobiol Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Davila, Alfonso F.] SETI Inst, 189 N Bernardo Ave, Mountain View, CA 94043 USA.
[Eigenbrode, Jennifer L.] NASA, Planetary Environm Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Liu, Xiao-Lei; Summons, Roger E.; O'Reilly, Shane S.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02141 USA.
[Stamos, Brian N.] Univ Texas Arlington, Dept Chem & Biochem, Arlington, TX 76019 USA.
[Williams, Amy] Towson Univ, Dept Phys Astron & Geosci, 8000 York Rd, Towson, MD 21252 USA.
RP Wilhelm, MB (reprint author), NASA, Space Sci & Astrobiol Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM marybeth.wilhelm@nasa.gov; mary.n.parenteau@nasa.gov;
linda.l.jahnke@nasa.gov; jwray@eas.gatech.edu
RI Wray, James/B-8457-2008
OI Wray, James/0000-0001-5559-2179
FU National Science Foundation [DGE-1148903]; NASA Astrobiology Institute
Early Career Collaboration Award; NASA Astrobiology Institute (NAI
Grant) [NNX15BB01A]; NASA Exobiology grant [NNX15AM17G]; NASA
Astrobiology Institute Foundations of Complex Life, Evolution,
Preservation, and Detection on Earth and Beyond [NNA13AA90A]; Simons
Foundation Collaboration on the Origins of Life (SCOL); EU; Irish
Research Council
FX This work was supported primarily by the National Science Foundation
Graduate Research Fellowship Program under Grant No. DGE-1148903 to
M.B.W. Additional support was provided by a NASA Astrobiology Institute
Early Career Collaboration Award to M.B.W. A.F.D. acknowledges funding
from the NASA Astrobiology Institute (NAI Grant NNX15BB01A to the SETI
Institute). M.N.P. was supported by NASA Exobiology grant NNX15AM17G.
R.E.S. acknowledges support from the NASA Astrobiology Institute
(NNA13AA90A) Foundations of Complex Life, Evolution, Preservation, and
Detection on Earth and Beyond. X.-L.L. and RES were further supported by
the Simons Foundation Collaboration on the Origins of Life (SCOL).
S.S.O. was supported by the EU Marie Curie Actions Program and the Irish
Research Council (ELEVATE Career-Development Fellowship). We thank
Carolyn Colonero and Kate French of MIT for technical assistance and
Terry Jordan, Lujendra Ojha, Max Bernstein, and Raechel Harnoto for
helpful discussions. Finally, we thank Dr. Phil Meyers and one anonymous
reviewer for helpful and constructive comments.
NR 66
TC 0
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U2 0
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0146-6380
J9 ORG GEOCHEM
JI Org. Geochem.
PD JAN
PY 2017
VL 103
BP 97
EP 104
DI 10.1016/j.orggeochem.2016.10.015
PG 8
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EO2JA
UT WOS:000396521400009
ER
PT J
AU Sugg, JW
Fuhrmann, CM
Perry, LB
Hall, DK
Konradll, CE
AF Sugg, Johnathan W.
Fuhrmann, Christopher M.
Perry, L. Baker
Hall, Dorothy K.
Konradll, Charles E.
TI Sub-regional snow cover distribution across the southern Appalachian
Mountains
SO PHYSICAL GEOGRAPHY
LA English
DT Article
DE Fractional snow cover; snow sub-regions; synoptic scale circulation;
Southern Appalachian Mountains
ID FLOW SNOWFALL; MODIS; PATTERNS; USA; CLIMATOLOGY; ACCURACY; PRODUCTS;
FORESTS; MODEL
AB Snowfall in the Southern Appalachian Mountain region of the eastern US is characterized by much spatiotemporal variability. Annual snowfall totals vary by up to 75 cm, and variations in snowfall intensity can lead to large differences in the local snowfall distribution. Research has shown that the synoptic pattern associated with the snowfall strongly influences the regional-scale distribution of snow cover. However, topographic variability results in locally complex snow cover patterns that are not well understood or documented. In this study, we characterize the snow covered area (SCA) and fractional snow cover associated with different synoptic patterns in 14 individual sub-regions. We analyze 63 snow events using Moderate-resolution Imaging Spectroradiometer standard snow cover products to ascertain both qualitative and quantitative differences in snow cover across sub-regions. Among sub-regions, there is significant variation in the snow cover pattern from individual synoptic classes. Furthermore, the percent SCA follows the regional snowfall climatology, and sub-regions with the highest elevations and northerly latitudes exhibit the greatest variability. Results of the sub-regional analysis provide valuable guidance to forecasters by contributing a deeper understanding of local snow cover patterns and their relationship to synoptic-scale circulation features.
C1 [Sugg, Johnathan W.; Konradll, Charles E.] Univ North Carolina Chapel Hill, Dept Geog, Chapel Hill, NC USA.
[Fuhrmann, Christopher M.] Mississippi State Univ, Dept Geosci, Mississippi State, MS 39762 USA.
[Perry, L. Baker] Appalachian State Univ, Dept Geog & Planning, Boone, NC 28608 USA.
[Hall, Dorothy K.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD USA.
RP Sugg, JW (reprint author), Univ North Carolina Chapel Hill, Dept Geog, Chapel Hill, NC USA.
EM jwsugg@live.unc.edu
FU Earth Observing System Program (MODIS Science Team)
FX The research conducted at Goddard Space Flight Center was supported by
the Earth Observing System Program (MODIS Science Team).
NR 43
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U2 0
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND
SN 0272-3646
EI 1930-0557
J9 PHYS GEOGR
JI Phys. Geogr.
PY 2017
VL 38
IS 2
BP 105
EP 123
DI 10.1080/02723646.2016.1162020
PG 19
WC Environmental Sciences; Geography, Physical; Geosciences,
Multidisciplinary; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Physical Geography; Geology;
Meteorology & Atmospheric Sciences
GA EO5TQ
UT WOS:000396756200002
ER
PT J
AU Darr, SR
Camarotti, CF
Hartwig, JW
Chung, JN
AF Darr, S. R.
Camarotti, C. F.
Hartwig, J. W.
Chung, J. N.
TI Hydrodynamic model of screen channel liquid acquisition devices for
in-space cryogenic propellant management
SO PHYSICS OF FLUIDS
LA English
DT Article
ID SUPERFLUID-HELIUM; SYSTEM; FLOW; SELECTION; DESIGN
AB Technologies that enable the storage and transfer of cryogenic propellants in space will be needed for the next generation vehicles that will carry humans to Mars. One of the candidate technologies is the screen channel liquid acquisition device (LAD), which uses a metal woven wire mesh to separate the liquid and vapor phases so that single-phase liquid propellant can be transferred in microgravity. In this work, an experiment is carried out that provides measurements of the velocity and pressure fields in a screen channel LAD. These data are used to validate a new analytical solution of the liquid flow through a screen channel LAD. This hydrodynamic model, which accounts for non-uniform injection through the screen, is compared with the traditional pressure term summation model which assumes a constant, uniform injection velocity. Results show that the new model performs best against the new data and historical data. The velocity measurements inside the screen channel LAD are used to provide a more accurate velocity profile which further improves the new model. The result of this work is a predictive tool that will instill confidence in the design of screen channel LADs for future in-space propulsion systems. Published by AIP Publishing.
C1 [Darr, S. R.; Camarotti, C. F.; Chung, J. N.] Univ Florida, Dept Mech & Aerosp Engn, Gainesville, FL 32611 USA.
[Hartwig, J. W.] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Darr, SR (reprint author), Univ Florida, Dept Mech & Aerosp Engn, Gainesville, FL 32611 USA.
EM gatorsamd@ufl.edu; jnchung@ufl.edu
OI Darr, Samuel/0000-0002-1891-405X
FU NASA Glenn Research Center; Department of Mechanical and Aerospace
Engineering at the University of Florida
FX This work was funded partially by the E-Cryo program of the NASA Glenn
Research Center and partially by the Department of Mechanical and
Aerospace Engineering at the University of Florida.
NR 38
TC 0
Z9 0
U1 1
U2 1
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 1070-6631
EI 1089-7666
J9 PHYS FLUIDS
JI Phys. Fluids
PD JAN
PY 2017
VL 29
IS 1
AR 017101
DI 10.1063/1.4973671
PG 18
WC Mechanics; Physics, Fluids & Plasmas
SC Mechanics; Physics
GA EM5YY
UT WOS:000395391200034
ER
PT J
AU Khazanov, GV
Sibeck, DG
Tel'nikhin, AA
Kronberg, TK
AF Khazanov, G. V.
Sibeck, D. G.
Tel'nikhin, A. A.
Kronberg, T. K.
TI Spectra of keV protons related to ion-cyclotron wave packets
SO PHYSICS OF PLASMAS
LA English
DT Article
ID IN-SITU OBSERVATIONS; VAN ALLEN PROBES; PC1 PULSATIONS; PRECIPITATION;
DISTRIBUTIONS; ACCELERATION; STORMS
AB We use the Fokker-Planck-Kolmogorov equation to study the statistical aspects of stochastic dynamics of the radiation belt (RB) protons driven by nonlinear electromagnetic ion-cyclotron (EMIC) wave packets. We obtain the spectra of keV protons scattered by these waves that show steeping near the gyroresonance, the signature of resonant wave-particle interaction that cannot be described by a simple power law. The most likely mechanism for proton precipitation events in RBs is shown to be nonlinear wave-particle interaction, namely, the scattering of RB protons into the loss cone by EMIC waves.
C1 [Khazanov, G. V.; Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Tel'nikhin, A. A.; Kronberg, T. K.] Altai State Univ, Dept Phys & Technol, Barnaul, Russia.
RP Khazanov, GV (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM george.v.khazanov@nasa.gov
FU National Aeronautics and Space Administration SMD/Heliophysics
Supporting Research; Living With a Star programs for Geospace SRT; NASA
Van Allen Probes
FX This material is based upon work supported by the National Aeronautics
and Space Administration SMD/Heliophysics Supporting Research, Living
With a Star programs for Geospace SR&T, and NASA Van Allen Probes
(formerly known as the Radiation Belt Storm Probes (RBSP)).
NR 23
TC 0
Z9 0
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 1070-664X
EI 1089-7674
J9 PHYS PLASMAS
JI Phys. Plasmas
PD JAN
PY 2017
VL 24
IS 1
AR 012902
DI 10.1063/1.4973323
PG 7
WC Physics, Fluids & Plasmas
SC Physics
GA EM6AL
UT WOS:000395395100043
ER
PT J
AU Wilson, SR
Swieringa, KA
Leonard, RD
Freitag, E
Edwards, DJ
AF Wilson, Sara R.
Swieringa, Kurt A.
Leonard, Robert D.
Freitag, Evan
Edwards, David J.
TI Statistical engineering approach to improve the realism of
computer-simulated experiments with aircraft trajectory clustering
SO QUALITY ENGINEERING
LA English
DT Article
DE dynamic time warping; gap statistic; k-means; statistical engineering;
trajectory clustering
AB This article presents a statistical engineering approach for clustering aircraft trajectories. The clustering methodology was developed to address the need to incorporate more realistic trajectories in fast-time computer simulations used to evaluate an aircraft spacing algorithm. The methodology is a combination of Dynamic Time Warping and k-Means clustering, and can be viewed as one of many possible solutions to the immediate problem. The implementation of this statistical engineering approach is also repeatable, scalable, and extendable to the investigation of other air traffic management technologies. Development of the clustering methodology is presented in addition to an application and description of results.
C1 [Wilson, Sara R.; Swieringa, Kurt A.] NASA, Langley Res Ctr, 4 Langley Blvd,Bldg 1230,Mail Stop 238, Hampton, VA 23681 USA.
[Leonard, Robert D.; Freitag, Evan; Edwards, David J.] Virginia Commonwealth Univ, Dept Stat Sci & Operat Res, Richmond, VA USA.
RP Wilson, SR (reprint author), NASA, Langley Res Ctr, 4 Langley Blvd,Bldg 1230,Mail Stop 238, Hampton, VA 23681 USA.
EM sara.r.wilson@nasa.gov
FU NASA Airspace Operations and Safety Program Airspace Technology
Demonstration Project
FX The authors appreciate the support of the NASA Airspace Operations and
Safety Program Airspace Technology Demonstration Project for funding
this research effort.
NR 22
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Z9 0
U1 0
U2 0
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA
SN 0898-2112
EI 1532-4222
J9 QUAL ENG
JI Qual. Eng.
PY 2017
VL 29
IS 2
BP 167
EP 180
DI 10.1080/08982112.2016.1147050
PG 14
WC Engineering, Industrial; Statistics & Probability
SC Engineering; Mathematics
GA EM6FI
UT WOS:000395407800001
ER
PT J
AU Akella, S
Todling, R
Suarez, M
AF Akella, Santha
Todling, Ricardo
Suarez, Max
TI Assimilation for skin SST in the NASA GEOS atmospheric data assimilation
system
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE SST; diurnal warming; AVHRR; coupled data sssimilation; NWP
ID SEA-SURFACE TEMPERATURE; COOL-SKIN; SAHARAN DUST; IN-SITU; OCEAN;
CLIMATE; RADIATION; PACIFIC; OFFICE; IMPACT
AB The present article describes the sea surface temperature (SST) developments implemented in the Goddard EarthObserving System, Version 5 (GEOS) Atmospheric Data Assimilation System (ADAS). These are enhancements that contribute to the development of an atmosphere-ocean coupled data assimilation system using GEOS. In the current quasioperational GEOS-ADAS, the SST is a boundary condition prescribed based on the OSTIA product, therefore SST and skin SST (T-s) are identical.
This work modifies the GEOS-ADAS T-s by modelling and assimilating near sea surface sensitive satellite infrared (IR) observations. The atmosphere-ocean interface layer of the GEOS atmospheric general circulation model (AGCM) is updated to include near-surface diurnal warming and cool-skin effects. The GEOS analysis system is also updated to directly assimilate SST-relevant Advanced Very High Resolution Radiometer (AVHRR) radiance observations.
Data assimilation experiments designed to evaluate the T-s modification in GEOS-ADAS show improvements in the assimilation of radiance observations that extend beyond the thermal infrared bands of AVHRR. In particular, many channels of hyperspectral sensors, such as those of the Atmospheric Infrared Sounder (AIRS), and Infrared Atmospheric Sounding Interferometer (IASI) are also better assimilated. We also obtained improved fit to withheld in situ buoy measurement of near-surface SST. Evaluation of forecast skill scores show neutral to marginal benefit from the modified T-s.
C1 [Akella, Santha; Todling, Ricardo; Suarez, Max] NASA, Global Modeling & Assimilat Off, GSFC, Greenbelt, MD USA.
[Akella, Santha] Sci Syst & Applicat Inc, Lanham, MD USA.
[Suarez, Max] Univ Space Res Assoc, GESTAR, Columbia, MD USA.
RP Akella, S (reprint author), NASA, Goddard Space Flight Ctr, Code 610-1, Greenbelt, MD 20771 USA.
EM santha.akella@nasa.gov
FU NASA ROSES [NNH10ZDA001N-MAP]
FX This work was partially funded by NASA ROSES 2010, NNH10ZDA001N-MAP. We
thank Michele Rienecker for her initial guidance. Xu Li and John Derber
are thanked for sharing their initial development within the GSI. We
thank Chelle Gentemann for helpful suggestions and diagnostics performed
on our diurnal warming model, and Xubin Zeng and Anton Beljaars for
sharing their diurnal model and helping with evaluation of results. We
thank F. Xu and Alex Ignatov for making the iQuam dataset publicly
available. Thanks are also due to Will McCarty and Meta Sienkiewicz for
their help with satellite bias correction and radiative transfer,
Lawrence Takacs for help with the forecast verification, and Chris
Fairall for suggestions on the bulk to skin temperature modelling.
Computations were performed at NASA NCCS.
NR 63
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Z9 0
U1 0
U2 0
PU WILEY
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-9009
EI 1477-870X
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD JAN
PY 2017
VL 143
IS 703
BP 1032
EP 1046
DI 10.1002/qj.2988
PN B
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EO2XY
UT WOS:000396560600036
ER
PT J
AU Hanu, AR
Barberiz, J
Bonneville, D
Byun, SH
Chen, L
Ciambella, C
Dao, E
Deshpande, V
Garnett, R
Hunter, SD
Jhirad, A
Johnston, EM
Kordic, M
Kurnell, M
Lopera, L
McFadden, M
Melnichuk, A
Nguyen, J
Otto, A
Scott, R
Wagner, DL
Wiendels, M
AF Hanu, A. R.
Barberiz, J.
Bonneville, D.
Byun, S. H.
Chen, L.
Ciambella, C.
Dao, E.
Deshpande, V.
Garnett, R.
Hunter, S. D.
Jhirad, A.
Johnston, E. M.
Kordic, M.
Kurnell, M.
Lopera, L.
McFadden, M.
Melnichuk, A.
Nguyen, J.
Otto, A.
Scott, R.
Wagner, D. L.
Wiendels, M.
TI NEUDOSE: A CubeSat Mission for Dosimetry of Charged Particles and
Neutrons in Low-Earth Orbit
SO RADIATION RESEARCH
LA English
DT Article
ID INTERNATIONAL-SPACE-STATION; GALACTIC COSMIC-RAYS; RADIATION
ENVIRONMENT; CHROMOSOME-ABERRATIONS; ENERGY-SPECTRUM; MARS; EXPLORATION;
RISKS; MICRODOSIMETRY; IRRADIATION
AB During space missions, astronauts are exposed to a stream of energetic and highly ionizing radiation particles that can suppress immune system function, increase cancer risks and even induce acute radiation syndrome if the exposure is large enough. As human exploration goals shift from missions in low-Earth orbit (LEO) to long-duration interplanetary missions, radiation protection remains one of the key technological issues that must be resolved. In this work, we introduce the NEUtron DOSimetry & Exploration (NEU-DOSE) CubeSat mission, which will provide new measurements of dose and space radiation quality factors to improve the accuracy of cancer risk projections for current and future space missions. The primary objective of the NEU-DOSE CubeSat is to map the in situ lineal energy spectra produced by charged particles and neutrons in LEO where most of the preparatory activities for future interplanetary missions are currently taking place. To perform these measurements, the NEUDOSE CubeSat is equipped with the Charged & Neutral Particle Tissue Equivalent Proportional Counter (CNP-TEPC), an advanced radiation monitoring instrument that uses active coincidence techniques to separate the interactions of charged particles and neutrons in real time. The NEUDOSE CubeSat, currently under development at McMaster University, provides a modern approach to test the CNP-TEPC instrument directly in the unique environment of outer space while simultaneously collecting new georeferenced lineal energy spectra of the radiation environment in LEO. (C) 2017 by Radiation Research Society
C1 [Hanu, A. R.; Hunter, S. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Barberiz, J.; Jhirad, A.; Kordic, M.; Melnichuk, A.; Nguyen, J.; Wiendels, M.] McMaster Univ, Dept Elect & Comp Engn, Hamilton, ON L8S 4K1, Canada.
[Bonneville, D.; Chen, L.; Kurnell, M.; Wagner, D. L.] McMaster Univ, Dept Engn Phys, Hamilton, ON L8S 4K1, Canada.
[Byun, S. H.; Dao, E.; Garnett, R.; Johnston, E. M.; McFadden, M.] McMaster Univ, Dept Med Phys & Appl Radiat Sci, Hamilton, ON L8S 4K1, Canada.
[Deshpande, V.] McMaster Univ, Dept Mech Engn, Hamilton, ON L8S 4K1, Canada.
[Otto, A.; Scott, R.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4K1, Canada.
[Ciambella, C.; Lopera, L.] McMaster Univ, Sch Engn Practice & Technol, Hamilton, ON L8S 4K1, Canada.
RP Hanu, AR (reprint author), NASA, Goddard Space Flight Ctr, Astroparticle Phys, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM andrei.hanu@nasa.gov
FU NASA Postdoctoral Program at Goddard Space Flight Center
FX ARH was supported by an appointment to the NASA Postdoctoral Program at
Goddard Space Flight Center (administered by Oak Ridge Associated
Universities through a contract with NASA).
NR 45
TC 0
Z9 0
U1 0
U2 0
PU RADIATION RESEARCH SOC
PI LAWRENCE
PA 810 E TENTH STREET, LAWRENCE, KS 66044 USA
SN 0033-7587
EI 1938-5404
J9 RADIAT RES
JI Radiat. Res.
PD JAN
PY 2017
VL 187
IS 1
BP 42
EP 49
DI 10.1667/RR14491.1
PG 8
WC Biology; Biophysics; Radiology, Nuclear Medicine & Medical Imaging
SC Life Sciences & Biomedicine - Other Topics; Biophysics; Radiology,
Nuclear Medicine & Medical Imaging
GA EM1XR
UT WOS:000395111100005
PM 28001909
ER
PT J
AU Horne, RA
Sackett, CA
AF Horne, R. A.
Sackett, C. A.
TI A cylindrically symmetric magnetic trap for compact Bose-Einstein
condensate atom interferometer gyroscopes
SO REVIEW OF SCIENTIFIC INSTRUMENTS
LA English
DT Review
AB We present a variant of the time-orbiting potential trap suitable for Bose-Einstein condensate atom interferometers, which provides weak, cylindrically symmetric confinement as well as support for the atoms against gravity. This trapping configuration is well-suited for the implementation of a compact atom interferometer based gyroscope. The trap is made up of six coils, which were produced using photolithographic techniques and take up a modest volume of approximately 1 cubic inch inside a vacuum chamber. The trapping frequencies and thermal characteristics of the trap are presented, showing cylindrical symmetry and scalability of the trapping frequencies from 1 Hz to 8 Hz in the symmetry plane.
C1 [Horne, R. A.] NASA, Langley Res Ctr, Revolutionary Aviat Technol Branch, Mail Stop 207, Hampton, VA 23681 USA.
[Sackett, C. A.] Univ Virginia, Dept Phys, 382 McCormick Rd, Charlottesville, VA 22904 USA.
RP Horne, RA (reprint author), NASA, Langley Res Ctr, Revolutionary Aviat Technol Branch, Mail Stop 207, Hampton, VA 23681 USA.
FU NASA [1502012]
FX This work was supported by NASA Grant No. 1502012.
NR 20
TC 0
Z9 0
U1 1
U2 1
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0034-6748
EI 1089-7623
J9 REV SCI INSTRUM
JI Rev. Sci. Instrum.
PD JAN
PY 2017
VL 88
IS 1
AR 013102
DI 10.1063/1.4973123
PG 6
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA EM6BD
UT WOS:000395396900003
PM 28147663
ER
PT J
AU Guhathakurta, M
AF Guhathakurta, M.
TI Too Big to Solve? Heliophysics Pioneers a New Approach to Intractable
Problems
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Editorial Material
C1 [Guhathakurta, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Guhathakurta, M (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM madhulika.guhathakurta@nasa.gov
NR 6
TC 1
Z9 1
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD JAN
PY 2017
VL 15
IS 1
BP 12
EP 13
DI 10.1002/2016SW001502
PG 2
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA EL4GT
UT WOS:000394580400002
ER
PT J
AU Petrinec, SM
Redmon, RJ
Rastaetter, L
AF Petrinec, S. M.
Redmon, R. J.
Rastaetter, L.
TI Nowcasting and forecasting of the magnetopause and bow shock-A status
update
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Review
ID MAGNETIC-FIELD ORIENTATION; HIGH-LATITUDE MAGNETOPAUSE; 6.6 RE; EARTHS
MAGNETOPAUSE; MODEL PREDICTIONS; MHD SIMULATIONS; CLOCK ANGLE; MACH
NUMBER; SHAPE; CROSSINGS
AB There has long been interest in knowing the shape and location of the Earth's magnetopause and of the standing fast-mode bow shock upstream of the Earth's magnetosphere. This quest for knowledge spans both the research and operations arenas. Pertinent to the latter, nowcasting and near-term forecasting are important for determining the extent to which the magnetosphere is compressed or expanded due to the influence of the solar wind bulk plasma and fields and the coupling to other magnetosphere-ionosphere processes with possible effects on assets. This article provides an update to a previous article on the same topic published 15 years earlier, with focus on studies that have been conducted, the current status of nowcasting and forecasting of geophysical boundaries, and future endeavors.
C1 [Petrinec, S. M.] Lockheed Martin Adv Technol Ctr, Palo Alto, CA 94304 USA.
[Redmon, R. J.] NOAA, Space Weather Predict Ctr, Boulder, CO USA.
[Rastaetter, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Petrinec, SM (reprint author), Lockheed Martin Adv Technol Ctr, Palo Alto, CA 94304 USA.
EM petrinec@lmsal.com
FU NSF [1303186]
FX This manuscript describes recent modeling efforts and web site tool
development; no observations are explicitly used in this paper.
Real-time web sites rely upon observations from solar wind monitors
(http://www.swpc.noaa.gov/products/ace-real-time-solarwind; and
http://www.swpc.noaa.gov/products/real-time-solar-wind), while empirical
models in the literature are based upon observations from a variety of
spacecraft, which are available to the public and stored at CDAWeb. This
effort was supported at Lockheed Martin by NSF grant 1303186.
NR 72
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U1 2
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD JAN
PY 2017
VL 15
IS 1
BP 36
EP 43
DI 10.1002/2016SW001565
PG 8
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA EL4GT
UT WOS:000394580400005
ER
PT J
AU Jones, AD
Kanekal, SG
Baker, DN
Klecker, B
Looper, MD
Mazur, JE
Schiller, Q
AF Jones, A. D.
Kanekal, S. G.
Baker, D. N.
Klecker, B.
Looper, M. D.
Mazur, J. E.
Schiller, Q.
TI SAMPEX observations of the South Atlantic anomaly secular drift during
solar cycles 22-24
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID VAN-ALLEN BELT; RADIATION BELT; TELESCOPE; INSTRUMENT; PARTICLES;
MOTION; SPACE
AB It is observed that charged particle intensities are very high near the South Atlantic anomaly (SAA) and are a potential hazard to spacecraft passing through the region. In this study, we examine the secular drift of the SAA location at similar to 400-600 km altitude over nearly two solar cycles, using particle count rates to trace the geomagnetic field lines in the region near the SAA. We use data from the Low-Energy Ion Composition Analyzer sensor on board the SAMPEX (Solar, Anomalous, and Magnetospheric Particle Explorer) spacecraft to measure both the longitudinal and latitudinal drifts of the SAA. We find that the longitudinal drift rate is 0.20 +/- 0.04 degrees west per year and that the latitudinal drift rate is 0.11 +/- 0.01 degrees south per year. These measurements are compared with the IGRF12 (International Geomagnetic Reference Field) model calculations based on an analysis of magnetic field minima in the region of the SAA. Our results, which are in good agreement with model results and prior measurements when declining spacecraft altitude is taken into account, have important space weather implications.
C1 [Jones, A. D.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Jones, A. D.; Kanekal, S. G.; Schiller, Q.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Baker, D. N.] Univ Colorado, Lab Atmospher & Space Sci, Boulder, CO 80309 USA.
[Klecker, B.] Max Planck Inst Extraterr Phys, Munich, Germany.
[Looper, M. D.] Aerosp Corp, El Segundo, CA 90245 USA.
[Mazur, J. E.] Aerosp Corp, Chantilly, VA USA.
RP Jones, AD (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.; Jones, AD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM ashley.jones@nasa.gov
NR 40
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U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD JAN
PY 2017
VL 15
IS 1
BP 44
EP 52
DI 10.1002/2016SW001525
PG 9
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA EL4GT
UT WOS:000394580400006
ER
PT J
AU Gordeev, E
Sergeev, V
Tsyganenko, N
Kuznetsova, M
Rastaetter, L
Raeder, J
Toth, G
Lyon, J
Merkin, V
Wiltberger, M
AF Gordeev, E.
Sergeev, V.
Tsyganenko, N.
Kuznetsova, M.
Rastaeetter, L.
Raeder, J.
Toth, G.
Lyon, J.
Merkin, V.
Wiltberger, M.
TI The substorm cycle as reproduced by global MHD models
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID OPEN MAGNETIC-FLUX; SOLAR-WIND; MAGNETOSPHERIC SUBSTORM; PHASE DURATION;
PLASMA SHEET; FIELD; MAGNETOTAIL; IONOSPHERE; SIMULATION; INTENSITY
AB Recently, Gordeev et al. (2015) suggested a method to test global MHD models against statistical empirical data. They showed that four community-available global MHD models supported by the Community Coordinated Modeling Center (CCMC) produce a reasonable agreement with reality for those key parameters (the magnetospheric size, magnetic field, and pressure) that are directly related to the large-scale equilibria in the outer magnetosphere. Based on the same set of simulation runs, here we investigate how the models reproduce the global loading-unloading cycle. We found that in terms of global magnetic flux transport, three examined CCMC models display systematically different response to idealized 2h north then 2h south interplanetary magnetic field (IMF) B-z variation. The LFM model shows a depressed return convection and high loading rate during the growth phase as well as enhanced return convection and high unloading rate during the expansion phase, with the amount of loaded/unloaded magnetotail flux and the growth phase duration being the closest to their observed empirical values during isolated substorms. Two other models exhibit drastically different behavior. In the BATS-R-US model the plasma sheet convection shows a smooth transition to the steady convection regime after the IMF southward turning. In the Open GGCM a weak plasma sheet convection has comparable intensities during both the growth phase and the following slow unloading phase. We also demonstrate potential technical problem in the publicly available simulations which is related to postprocessing interpolation and could affect the accuracy of magnetic field tracing and of other related procedures.
C1 [Gordeev, E.; Sergeev, V.; Tsyganenko, N.] St Petersburg State Univ, Earth Phys Dept, St Petersburg, Russia.
[Kuznetsova, M.; Rastaeetter, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Raeder, J.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
[Toth, G.] Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA.
[Lyon, J.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA.
[Merkin, V.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Wiltberger, M.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
RP Gordeev, E (reprint author), St Petersburg State Univ, Earth Phys Dept, St Petersburg, Russia.
EM evgeny.i.gordeev@spbu.ru
FU Russian Science Foundation [14-17-00072]; National Science Foundation;
CCMC
FX This study was supported by Russian Science Foundation grant
14-17-00072. The National Center for Atmospheric Research is supported
by the National Science Foundation. Model computations were performed at
the Community Coordinated Modeling Center, NASA GSFC, and all simulation
results can be found in the CCMC database (https://ccmc.gsfc.nasa.gov/)
under the names shown in Table S2 in the supporting information. The
authors would like to acknowledge the CCMC staff for their generous
support throughout the work described in this paper. The solar wind and
activity indices were provided by the NASA CDAWeb and OMNIWeb sites. For
the substorm onset list we gratefully acknowledge the SuperMAG
initiative and the SuperMAG collaborators. We thank M. Kholeva for her
help in the manuscript preparation.
NR 61
TC 1
Z9 1
U1 1
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD JAN
PY 2017
VL 15
IS 1
BP 131
EP 149
DI 10.1002/2016SW001495
PG 19
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA EL4GT
UT WOS:000394580400012
ER
PT J
AU Welling, DT
Anderson, BJ
Crowley, G
Pulkkinen, AA
Rastatter, L
AF Welling, D. T.
Anderson, B. J.
Crowley, G.
Pulkkinen, A. A.
Rastaetter, L.
TI Exploring predictive performance: A reanalysis of the geospace model
transition challenge
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID IONOSPHERE-THERMOSPHERE MODEL; SOLAR-WIND; GLOBAL SIMULATIONS;
GEOMAGNETIC-FIELD; INDUCED CURRENTS; EMPIRICAL-MODEL; MHD SIMULATIONS;
OCTOBER 2003; RING CURRENT; MAGNETOSPHERE
AB The Pulkkinen et al. (2013) study evaluated the ability of five different geospace models to predict surface dB/dt as a function of upstream solar drivers. This was an important step in the assessment of research models for predicting and ultimately preventing the damaging effects of geomagnetically induced currents. Many questions remain concerning the capabilities of these models. This study presents a reanalysis of the Pulkkinen et al. (2013) results in an attempt to better understand the models' performance. The range of validity of the models is determined by examining the conditions corresponding to the empirical input data. It is found that the empirical conductance models on which global magnetohydrodynamic models rely are frequently used outside the limits of their input data. The prediction error for the models is sorted as a function of solar driving and geomagnetic activity. It is found that all models show a bias toward underprediction, especially during active times. These results have implications for future research aimed at improving operational forecast models.
C1 [Welling, D. T.] Univ Michigan, Dept Climate & Space, Ann Arbor, MI 48109 USA.
[Anderson, B. J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Crowley, G.] Atmospher & Space Technol Res Associates, Boulder, CO USA.
[Pulkkinen, A. A.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD USA.
[Rastaetter, L.] NASA, Goddard Space Flight Ctr, Community Coordinated Modeling Ctr, Greenbelt, MD USA.
RP Welling, DT (reprint author), Univ Michigan, Dept Climate & Space, Ann Arbor, MI 48109 USA.
EM dwelling@umich.edu
OI Welling, Daniel/0000-0002-0590-1022
NR 61
TC 2
Z9 2
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD JAN
PY 2017
VL 15
IS 1
BP 192
EP 203
DI 10.1002/2016SW001505
PG 12
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA EL4GT
UT WOS:000394580400016
ER
PT J
AU Cyr, OCS
Posner, A
Burkepile, JT
AF Cyr, O. C. St.
Posner, A.
Burkepile, J. T.
TI Solar energetic particle warnings from a coronagraph
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID II RADIO-BURSTS; GROUND-LEVEL EVENTS; MASS EJECTIONS; PROTON EVENTS;
CYCLE 23; AUTOMATIC DETECTION; FORECASTING METHODS; PREDICTION MODEL;
STEREO MISSION; COSMIC RAYS
AB We report here the concept of using near-real time observations from a coronagraph to provide early warning of a fast coronal mass ejection (CME) and the possible onset of a solar energetic particle (SEP) event. The 1 January 2016, fast CME, and its associated SEP event are cited as an example. The CME was detected by the ground-based K-Cor coronagraph at Mauna Loa Solar Observatory and by the SOHO Large Angle and Spectrometric Coronagraph. The near-real-time availability of the high-cadence K-Cor observations in the low corona leads to an obvious question: Why has no one attempted to use a coronagraph as an early warning device for SEP events? The answer is that the low image cadence and the long latency of existing spaceborne coronagraphs make them valid for archival studies but typically unsuitable for near-real-time forecasting. The January 2016 event provided favorable CME viewing geometry and demonstrated that the primary component of a prototype ground-based system for SEP warnings is available several hours on most days. We discuss how a conceptual CME-based warning system relates to other techniques, including an estimate of the relative SEP warning times, and how such a system might be realized.
C1 [Cyr, O. C. St.] NASA, GSFC, Greenbelt, MD 20771 USA.
[Posner, A.] NASA, HQ, Washington, DC 20546 USA.
[Burkepile, J. T.] NCAR, HAO, Boulder, CO USA.
RP Cyr, OCS (reprint author), NASA, GSFC, Greenbelt, MD 20771 USA.
EM Chris.StCyr@nasa.gov
FU National Science Foundation
FX The initial idea to investigate a coronagraph-based SEP warning
technique came from a discussion with N. Zapp and D. Fry, both of
NASA-JSC. Several individuals have contributed through discussions or
assistance in data analysis: T. Alberti, C. Balch, D. Falconer, B.
Heber, L. Jian, S. Kahler, J. Labrenz, M. Laurenza, G. Michalek, M.
Nunez, I. Richardson, S. St. Cyr, K. Schenk, B. J. Thompson, R.
Wimmer-Schweingruber, H. Xie, and S. Yashiro. MLSO data are freely
available online courtesy of the Mauna Loa Solar Observatory
(www2.hao.ucar.edu/mlso), operated by the High Altitude Observatory, as
part of the National Center for Atmospheric Research (NCAR). NCAR is
supported by the National Science Foundation. SOHO is a project of
international cooperation between ESA and NASA. SOHO LASCO data are
freely available online, and CME data were taken from the CDAW LASCO
catalog. This CME catalog is generated and maintained at the CDAW Data
Center by NASA and the Catholic University of America in cooperation
with the Naval Research Laboratory. SDO data are courtesy of the
NASA/SDO and the AIA, EVE, and HMI science teams. The authors thank the
reviewers for their constructive comments. The authors are not aware of
any conflicts of interest relating to the content of this manuscript.
NR 150
TC 0
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U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD JAN
PY 2017
VL 15
IS 1
BP 240
EP 257
DI 10.1002/2016SW001545
PG 18
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA EL4GT
UT WOS:000394580400019
ER
PT J
AU Wada, Y
Reager, JT
Chao, BF
Wang, J
Lo, MH
Song, CQ
Li, YW
Gardner, AS
AF Wada, Yoshihide
Reager, John T.
Chao, Benjamin F.
Wang, Jida
Lo, Min-Hui
Song, Chunqiao
Li, Yuwen
Gardner, Alex S.
TI Recent Changes in Land Water Storage and its Contribution to Sea Level
Variations
SO SURVEYS IN GEOPHYSICS
LA English
DT Review
DE Land water storage; Sea level rise (SLR); Groundwater depletion (GWD);
Reservoir impoundment; Climate variability
ID FOREST RESOURCES ASSESSMENT; MULTIMISSION SATELLITE ALTIMETRY; GLOBAL
WETLAND AREA; US HIGH-PLAINS; COVER DATA SET; GROUNDWATER DEPLETION;
TIBETAN PLATEAU; CLIMATE-CHANGE; ARAL SEA; AMAZON DEFORESTATION
AB Sea level rise is generally attributed to increased ocean heat content and increased rates glacier and ice melt. However, human transformations of Earth's surface have impacted water exchange between land, atmosphere, and ocean, ultimately affecting global sea level variations. Impoundment of water in reservoirs and artificial lakes has reduced the outflow of water to the sea, while river runoff has increased due to ground-water mining, wetland and endorheic lake storage losses, and deforestation. In addition, climate-driven changes in land water stores can have a large impact on global sea level variations over decadal timescales. Here, we review each component of negative and positive land water contribution separately in order to highlight and understand recent changes in land water contribution to sea level variations.
C1 [Wada, Yoshihide] NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
[Wada, Yoshihide] Columbia Univ, Ctr Climate Syst Res, 2880 Broadway, New York, NY 10025 USA.
[Wada, Yoshihide] Univ Utrecht, Fac Geosci, Dept Phys Geog, Heidelberglaan 2, NL-3584 CS Utrecht, Netherlands.
[Wada, Yoshihide] Int Inst Appl Syst Anal, A-2361 Laxenburg, Austria.
[Reager, John T.; Gardner, Alex S.] CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Chao, Benjamin F.; Li, Yuwen] Acad Sinica, Inst Earth Sci, Taipei 11529, Taiwan.
[Wang, Jida] Kansas State Univ, Dept Geog, 118 Seaton Hall, Manhattan, KS 66506 USA.
[Lo, Min-Hui] Natl Taiwan Univ, Dept Atmospher Sci, Taipei 10673, Taiwan.
[Song, Chunqiao] Univ Calif Los Angeles, Dept Geog, 1255 Bunche Hall, Los Angeles, CA 90095 USA.
RP Wada, Y (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.; Wada, Y (reprint author), Columbia Univ, Ctr Climate Syst Res, 2880 Broadway, New York, NY 10025 USA.; Wada, Y (reprint author), Univ Utrecht, Fac Geosci, Dept Phys Geog, Heidelberglaan 2, NL-3584 CS Utrecht, Netherlands.; Wada, Y (reprint author), Int Inst Appl Syst Anal, A-2361 Laxenburg, Austria.
EM y.wada@uu.nl
FU Japan Society for the Promotion of Science (JSPS) [JSPS-2014-878]; NASA
FX The International Space Science Institute (ISSI) in Bern, Switzerland,
and specifically Anny Cazenave and Nicolas Champollion, are acknowledged
for hosting the ISSI Workshop on Integrative study of the mean sea level
and its components. Y. Wada is supported by Japan Society for the
Promotion of Science (JSPS) Oversea Research Fellowship (grant no.
JSPS-2014-878). A portion of this research was conducted at the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with NASA. We acknowledge for the ICOLD Register Committee
chairman Patrick Ledelliou, and Dam Surveillance past chairman Bernard
Goguel, who removed duplicates from the ICOLD Register database. We wish
to thank one anonymous referee and Anny Cazenave for the constructive
comments and suggestions, which substantially improved the quality of
the manuscript.
NR 119
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U1 0
U2 0
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0169-3298
EI 1573-0956
J9 SURV GEOPHYS
JI Surv. Geophys.
PD JAN
PY 2017
VL 38
IS 1
SI SI
BP 131
EP 152
DI 10.1007/s10712-016-9399-6
PG 22
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EM1JE
UT WOS:000395073100007
ER
PT J
AU Slangen, ABA
Adloff, F
Jevrejeva, S
Leclercq, PW
Marzeion, B
Wada, Y
Winkelmann, R
AF Slangen, A. B. A.
Adloff, F.
Jevrejeva, S.
Leclercq, P. W.
Marzeion, B.
Wada, Y.
Winkelmann, R.
TI A Review of Recent Updates of Sea-Level Projections at Global and
Regional Scales
SO SURVEYS IN GEOPHYSICS
LA English
DT Review
DE Sea-level change; Regional sea-level change; Sea-level projections; Ice
sheets; Glaciers; Terrestrial water storage; Mediterranean
ID GREENLAND ICE-SHEET; SURFACE MASS-BALANCE; CLIMATE MODELS; GROUNDWATER
DEPLETION; GLACIER CONTRIBUTIONS; RECONCILED ESTIMATE; WEST ANTARCTICA;
PINE ISLAND; RISE; WATER
AB Sea-level change (SLC) is a much-studied topic in the area of climate research, integrating a range of climate science disciplines, and is expected to impact coastal communities around the world. As a result, this field is rapidly moving, and the knowledge and understanding of processes contributing to SLC is increasing. Here, we discuss noteworthy recent developments in the projection of SLC contributions and in the global mean and regional sea-level projections. For the Greenland Ice Sheet contribution to SLC, earlier estimates have been confirmed in recent research, but part of the source of this contribution has shifted from dynamics to surface melting. New insights into dynamic discharge processes and the onset of marine ice sheet instability increase the projected range for the Antarctic contribution by the end of the century. The contribution from both ice sheets is projected to increase further in the coming centuries to millennia. Recent updates of the global glacier outline database and new global glacier models have led to slightly lower projections for the glacier contribution to SLC (7-17 cm by 2100), but still project the glaciers to be an important contribution. For global mean sea-level projections, the focus has shifted to better estimating the uncertainty distributions of the projection time series, which may not necessarily follow a normal distribution. Instead, recent studies use skewed distributions with longer tails to higher uncertainties. Regional projections have been used to study regional uncertainty distributions, and regional projections are increasingly being applied to specific regions, countries, and coastal areas.
C1 [Slangen, A. B. A.] Univ Utrecht, Inst Marine & Atmospher Res Utrecht IMAU, Utrecht, Netherlands.
[Slangen, A. B. A.] CSIRO, CSIRO Oceans & Atmosphere, Hobart, Tas, Australia.
[Adloff, F.] Meteo France, CNRS, GAME, CNRM, Toulouse, France.
[Jevrejeva, S.] Natl Oceanog Ctr, Liverpool, Merseyside, England.
[Leclercq, P. W.] Univ Oslo, Dept Geosci, Oslo, Norway.
[Marzeion, B.] Univ Bremen, Inst Geog, Bremen, Germany.
[Wada, Y.] Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY USA.
[Wada, Y.] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
[Wada, Y.] Univ Utrecht, Dept Phys Geog, Utrecht, Netherlands.
[Wada, Y.] Int Inst Appl Syst Anal, Laxenburg, Austria.
[Winkelmann, R.] Univ Potsdam, Potsdam Inst Climate Impact Res, Potsdam, Germany.
RP Slangen, ABA (reprint author), Univ Utrecht, Inst Marine & Atmospher Res Utrecht IMAU, Utrecht, Netherlands.; Slangen, ABA (reprint author), CSIRO, CSIRO Oceans & Atmosphere, Hobart, Tas, Australia.
EM aimee.slangen@gmail.com
FU CSIRO Australia Office of the Chief Executive Fellowship;
NWO-Netherlands Polar Programme; European Research Council under the
European Union [320816]; Japan Society for the Promotion of Science
(JSPS) [JSPS-2014-878]; AXA postdoctoral fellowship
FX This paper is a result of the ISSI Workshop on Integrative Study of Sea
Level, held in Bern, Switzerland, 2-6 February 2015. A.S. was supported
by a CSIRO Australia Office of the Chief Executive Fellowship and the
NWO-Netherlands Polar Programme. P.L. was funded by the European
Research Council under the European Union's Seventh Framework Programme
(FP/2007-2013)/ERC Grant Agreement No. 320816. Y.W. was supported by a
Japan Society for the Promotion of Science (JSPS) Overseas Research
Fellowship (Grant No. JSPS-2014-878). F.A. was supported by an AXA
postdoctoral fellowship.
NR 98
TC 2
Z9 2
U1 1
U2 1
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0169-3298
EI 1573-0956
J9 SURV GEOPHYS
JI Surv. Geophys.
PD JAN
PY 2017
VL 38
IS 1
SI SI
BP 385
EP 406
DI 10.1007/s10712-016-9374-2
PG 22
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EM1JE
UT WOS:000395073100017
ER
PT J
AU Zaretsky, EV
Branzai, EV
AF Zaretsky, Erwin V.
Branzai, Emanuel V.
TI Rolling Bearing Service Life Based on Probable Cause for Removal-A
Tutorial
SO TRIBOLOGY TRANSACTIONS
LA English
DT Article
DE Bearing life prediction; rolling-element fatigue; rolling bearing
service life
AB In 1947 and 1952 G. Lundberg and A. Palmgren developed what is now referred to as the Lundberg-Palmgren model for rolling bearing life prediction based on classical rolling-element fatigue. Today, bearing fatigue probably accounts for less than 5% of bearings removed from service for cause. A bearing service life prediction methodology and tutorial indexed to eight probable causes for bearing removal, including fatigue, are presented that incorporate strict series reliability; Weibull statistical analysis; available published field data from the Naval Air Rework Facility; and similar to 224,000 rolling-element bearings removed for rework from commercial aircraft engines. Bearing service life L-serv can be benchmarked and calculated to the bearing L-10 fatigue life as follows: L-serv = X-1/m L-10, where X is the number of bearings removed from service because of fatigue divided by the total of all bearings removed from service regardless of cause and m is the Weibull modulus of the bearings removed from service. The most conservative bearing L-10 service life calculation is obtained assuming an exponential distribution where m = 1.1. Of the similar to 224,000 commercial engine bearings removed from service for rework, 1,977 or 0.88% were rejected because of fatigue. From the Naval Air Rework Facility bearing data, eliminating rolling-element fatigue as a cause for removal, the L-10 service life of these bearings would increase by approximately 3%.
C1 [Zaretsky, Erwin V.] NASA Glenn Res Ctr, Cleveland, OH USA.
[Branzai, Emanuel V.] IRB Associates Inc, Brea, CA USA.
RP Zaretsky, EV (reprint author), NASA Glenn Res Ctr, Cleveland, OH USA.
EM evzaretsky@gmail.com
NR 23
TC 0
Z9 0
U1 0
U2 0
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA
SN 1040-2004
EI 1547-397X
J9 TRIBOL T
JI Tribol. Trans.
PY 2017
VL 60
IS 2
BP 300
EP 312
DI 10.1080/10402004.2016.1163761
PG 13
WC Engineering, Mechanical
SC Engineering
GA EO6CR
UT WOS:000396779900011
ER
PT J
AU Abbott, BP
Abbott, R
Abbott, TD
Abernathy, MR
Acernese, F
Ackley, K
Adams, C
Adams, T
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Agatsuma, K
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Ain, A
Ajith, P
Allen, B
Allocca, A
Altin, PA
Anderson, SB
Anderson, WG
Arai, K
Araya, MC
Arceneaux, CC
Areeda, JS
Arnaud, N
Arun, KG
Ascenzi, S
Ashton, G
Ast, M
Aston, SM
Astone, P
Aufmuth, P
Aulbert, C
Babak, S
Bacon, P
Bader, MKM
Baldaccini, F
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Zweizig, J.
CA LIGO Sci Collaboration
LIGO Sci Collaboration
VIRGO Collaboration
TI The basic physics of the binary black hole merger GW150914
SO ANNALEN DER PHYSIK
LA English
DT Article
ID GRAVITATIONAL-RADIATION; NEUTRON-STAR; GENERAL-RELATIVITY; STELLAR
ORBITS; MAXIMUM MASS; WAVES; PULSAR
AB The first direct gravitational-wave detection was made by the Advanced Laser Interferometer Gravitational Wave Observatory on September 14, 2015. The GW150914 signal was strong enough to be apparent, without using any waveform model, in the filtered detector strain data. Here, features of the signal visible in the data are analyzed using concepts from Newtonian physics and general relativity, accessible to anyone with a general physics background. The simple analysis presented here is consistent with the fully general-relativistic analyses published elsewhere, in showing that the signal was produced by the inspiral and subsequent merger of two black holes. The black holes were each of approximately 35M(circle dot), still orbited each other as close as similar to 350 km apart and subsequently merged to form a single black hole. Similar reasoning, directly from the data, is used to roughly estimate how far these black holes were from the Earth, and the energy that they radiated in gravitational waves.
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[Gaur, G.; Sengupta, A. S.] Indian Inst Technol, Ahmadabad 382424, Gujarat, India.
[Gergely, L.; Tapai, M.] Univ Szeged, Dom Ter 9, H-6720 Szeged, Hungary.
[Gill, K.; Hughey, B.; Pratt, J.; Szczepanczyk, M. J.; Zanolin, M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA.
[Haney, M.; Unnikrishnan, C. S.] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India.
[Grado, A.] Univ Naples Federico II, INAF, Osservatorio Astron Capodimonte, I-80131 Naples, Italy.
[Gustafson, R.; Neunzert, A.; Riles, K.; Sauter, O. E. S.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Henry, J.; Lange, J.; O'Shaughnessy, R.; Rizzo, M.; Whelan, J. T.; Zhang, Y.] Rochester Inst Technol, Rochester, NY 14623 USA.
[Huerta, E. A.] Univ Illinois, NCSA, Urbana, IL 61801 USA.
[Husa, S.; Jimenez-Forteza, F.; Keitel, D.; Oliver, M.; Sintes, A. M.] Univ Illes Balears, IAC3 IEEC, E-07122 Palma De Mallorca, Spain.
[Jaranowski, P.] Univ Bialystok, PL-15424 Bialystok, Poland.
[Jawahar, S.; Lockerbie, N. A.; Tokmakov, K. V.] Univ Strathclyde, SUPA, Glasgow G1 1XQ, Lanark, Scotland.
[Haris, K.; Pai, A.; Saleem, M.] IISER TVM, CET Campus, Trivandrum 695016, Kerala, India.
[Kehl, M. S.; Kumar, P.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Khazanov, E. A.; Palashov, O.; Sergeev, A.] Inst Appl Phys, Nizhnii Novgorod 603950, Russia.
[Kim, J.; Kim, Y. -M.; Lee, C. H.] Pusan Natl Univ, Busan 609735, South Korea.
[Kim, K.; Lee, H. K.] Hanyang Univ, Seoul 133791, South Korea.
[Kim, W.; King, E. J.; Munch, J.; Ottaway, D. J.; Veitch, P. J.] Univ Adelaide, Adelaide, SA 5005, Australia.
[Krolak, A.; Kutynia, A.; Zadrozny, A.] NCBJ, PL-05400 Otwock, Poland.
[Krolak, A.] IM PAN, PL-00956 Warsaw, Poland.
[Lasky, P. D.; Levin, Y.; Qiu, S.; Sammut, L.; Thrane, E.] Monash Univ, Clayton, Vic 3800, Australia.
[Lee, H. M.] Seoul Natl Univ, Seoul 151742, South Korea.
[Li, T. G. F.] Chinese Univ Hong Kong, Shatin, Hong Kong, Peoples R China.
[Littenberg, T. B.] Univ Alabama, Huntsville, AL 35899 USA.
[Lombardi, A. L.; Nedkova, K.; Zuraw, S. E.] Univ Massachusetts, Amherst, MA 01003 USA.
[Loriette, V.; Maksimovic, I.] CNRS, ESPCI, F-75005 Paris, France.
[Marchesoni, F.] Univ Camerino, Dipartimento Fis, I-62032 Camerino, Italy.
[McGuire, S. C.] Southern Univ & A&M Coll, Baton Rouge, LA 70813 USA.
[Mikhailov, E. E.; Rew, H.; Romanov, G.; Zhang, M.] Coll William & Mary, Williamsburg, VA 23187 USA.
[Millhouse, M.] Montana State Univ, Bozeman, MT 59717 USA.
[Mirshekari, S.; Sturani, R.] Univ Estadual Paulista, ICTP South Amer Inst Fundamental Res, Inst Fis Teor, BR-01140070 Sao Paulo, SP, Brazil.
[Moore, C. J.] Univ Cambridge, Cambridge CB2 1TN, England.
[Nayak, R. K.; Samajdar, A.] IISER Kolkata, Mohanpur 741252, W Bengal, India.
[O'Dell, J.] Rutherford Appleton Lab, HSIC, Didcot OX11 0QX, Oxon, England.
[Ogin, G. H.] Whitman Coll, 345 Boyer Ave, Walla Walla, WA 99362 USA.
[Oh, J. J.; Oh, S. H.; Son, E. J.] Natl Inst Math Sci, Daejeon 305390, South Korea.
[Pedurand, R.] Univ Lyon, F-69361 Lyon, France.
[Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA.
[Rosinska, D.] Univ Zielona Gora, Janusz Gil Inst Astron, PL-65265 Zielona, Gora, Poland.
[Sakellariadou, M.] Univ London, Kings Coll London, London WC2R 2LS, England.
[Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA.
[Trozzo, L.] Univ Siena, I-53100 Siena, Italy.
[Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA.
[Venkateswara, K.] Univ Washington, Seattle, WA 98195 USA.
[Wade, L. E.; Wade, M.] Kenyon Coll, Gambier, OH 43022 USA.
[Willis, J. L.] Abilene Christian Univ, Abilene, TX 79699 USA.
RP Abbott, BP (reprint author), CALTECH, LIGO, Pasadena, CA 91125 USA.
RI Gemme, Gianluca/C-7233-2008; Di Virgilio, Angela Dora
Vittoria/E-9078-2015; Sergeev, Alexander/F-3027-2017; Harms,
Jan/J-4359-2012; Leonardi, Matteo/G-9694-2015; Rocchi,
Alessio/O-9499-2015;
OI Davies, Gareth/0000-0002-4289-3439; Principe, Maria/0000-0002-6327-0628;
Gemme, Gianluca/0000-0002-1127-7406; Pitkin,
Matthew/0000-0003-4548-526X; Di Virgilio, Angela Dora
Vittoria/0000-0002-2237-7533; Rocchi, Alessio/0000-0002-1382-9016; Nitz,
Alexander/0000-0002-1850-4587; Murphy, David/0000-0002-8538-815X; Berry,
Christopher/0000-0003-3870-7215; Piccinni, Ornella
Juliana/0000-0001-5478-3950; Haney, Maria/0000-0001-7554-3665; Cesarini,
Elisabetta/0000-0001-9127-3167; Wang, Gang/0000-0002-9668-8772
FU United States National Science Foundation (NSF); Science and Technology
Facilities Council (STFC) of the United Kingdom; Max-Planck-Society
(MPS); State of Niedersachsen/Germany [GEO600]; Australian Research
Council; Netherlands Organisation for Scientific Research; Council of
Scientific and Industrial Research of India; Department of Science and
Technology, India; Science & Engineering Research Board (SERB), India;
Ministry of Human Resource Development, India; Spanish Ministerio de
Economia y Competitividad; Conselleria d'Economia i Competitivitat;
Conselleria d'Educacio, Cultura i Universitats of the Govern de les
Illes Balears; National Science Centre of Poland; European Commission;
Royal Society; Scottish Funding Council; Scottish Universities Physics
Alliance; Hungarian Scientific Research Fund (OTKA); Lyon Institute of
Origins (LIO); National Research Foundation of Korea; Industry Canada;
Province of Ontario through Ministry of Economic Development and
Innovation; Natural Science and Engineering Research Council Canada;
Canadian Institute for Advanced Research; Brazilian Ministry of Science,
Technology, and Innovation; Fundacao de Amparo a Pesquisa do Estado de
Sao Paulo (FAPESP); Russian Foundation for Basic Research; Leverhulme
Trust; Research Corporation; Ministry of Science and Technology (MOST),
Taiwan; Kavli Foundation
FX The authors gratefully acknowledge the support of the United States
National Science Foundation (NSF) for the construction and operation of
the LIGO Laboratory and Advanced LIGO as well as the Science and
Technology Facilities Council (STFC) of the United Kingdom, the
Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for
support of the construction of Advanced LIGO and construction and
operation of the GEO600 detector. Additional support for Advanced LIGO
was provided by the Australian Research Council. The authors gratefully
acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN),
the French Centre National de la Recherche Scientifique (CNRS) and the
Foundation for Fundamental Research on Matter supported by the
Netherlands Organisation for Scientific Research, for the construction
and operation of the Virgo detector and the creation and support of the
EGO consortium. The authors also gratefully acknowledge research support
from these agencies as well as by the Council of Scientific and
Industrial Research of India, Department of Science and Technology,
India, Science & Engineering Research Board (SERB), India, Ministry of
Human Resource Development, India, the Spanish Ministerio de Economia y
Competitividad, the Conselleria d'Economia i Competitivitat and
Conselleria d'Educacio, Cultura i Universitats of the Govern de les
Illes Balears, the National Science Centre of Poland, the European
Commission, the Royal Society, the Scottish Funding Council, the
Scottish Universities Physics Alliance, the Hungarian Scientific
Research Fund (OTKA), the Lyon Institute of Origins (LIO), the National
Research Foundation of Korea, Industry Canada and the Province of
Ontario through the Ministry of Economic Development and Innovation, the
Natural Science and Engineering Research Council Canada, Canadian
Institute for Advanced Research, the Brazilian Ministry of Science,
Technology, and Innovation, Fundacao de Amparo a Pesquisa do Estado de
Sao Paulo (FAPESP), Russian Foundation for Basic Research, the
Leverhulme Trust, the Research Corporation, Ministry of Science and
Technology (MOST), Taiwan and the Kavli Foundation. The authors
gratefully acknowledge the support of the NSF, STFC, MPS, INFN, CNRS and
the State of Niedersachsen/Germany for provision of computational
resources.
NR 53
TC 1
Z9 1
U1 3
U2 3
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA POSTFACH 101161, 69451 WEINHEIM, GERMANY
SN 0003-3804
EI 1521-3889
J9 ANN PHYS-BERLIN
JI Ann. Phys.-Berlin
PD JAN
PY 2017
VL 529
IS 1-2
AR UNSP 1600209
DI 10.1002/andp.201600209
PG 17
WC Physics, Multidisciplinary
SC Physics
GA EL2GI
UT WOS:000394437700003
ER
PT J
AU Dias, LA
Litz, J
Garrison, L
Martinez, A
Barry, K
Speakman, T
AF Dias, Laura Aichinger
Litz, Jenny
Garrison, Lance
Martinez, Anthony
Barry, Kevin
Speakman, Todd
TI Exposure of cetaceans to petroleum products following the Deepwater
Horizon oil spill in the Gulf of Mexico
SO ENDANGERED SPECIES RESEARCH
LA English
DT Article
DE Cetacean; Oil exposure; Deepwater Horizon; Oil spill; Petroleum
ID BOTTLE-NOSED DOLPHINS; TURSIOPS-TRUNCATUS
AB The Deepwater Horizon (DWH) oil spill was by far the largest offshore oil spill in the history of the USA. For 87 d, the well spilled millions of barrels of oil into the Gulf of Mexico, extensively affecting the habitat of numerous species of cetaceans. Previous studies have suggested that cetaceans would be able to detect and avoid oiled waters and, when in contact, oil would not adhere to their slick skin. However, photographic evidence and field observations gathered following the DWH oil spill documented at least 11 cetacean species swimming through oil and sheen, with oil adhered to their skin. This study not only documented direct exposure of cetaceans to petroleum products but also the persistence of the oil on their skin. In addition, given the extent of the DWH oil spill, the number of affected species and individuals was likely far greater than the documented occurrences captured during this study. Based on this evidence, we suggest that during oil spills in cetacean habitat, direct exposure of whales and dolphins to petroleum products will likely occur and should therefore be taken into account during response activities and damage assessments.
C1 [Dias, Laura Aichinger] Univ Miami, CIMAS, 4600 Rickenbacker Causeway, Miami, FL 33149 USA.
[Dias, Laura Aichinger; Litz, Jenny; Garrison, Lance; Martinez, Anthony] Natl Ocean & Atmospher Adm, Southeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, 75 Virginia Beach Dr, Miami, FL 33149 USA.
[Barry, Kevin] Natl Ocean & Atmospher Adm, Southeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, 3209 Frederic St, Pascagoula, MS 39567 USA.
[Speakman, Todd] JHT Inc, 2710 Discovery Dr,Suite 600, Orlando, FL 32826 USA.
[Speakman, Todd] Natl Ocean & Atmospher Adm, Natl Ctr Coastal Ocean Sci, Hollings Marine Lab, 331 Ft Johnson Rd, Charleston, SC 29412 USA.
RP Dias, LA (reprint author), Univ Miami, CIMAS, 4600 Rickenbacker Causeway, Miami, FL 33149 USA.; Dias, LA (reprint author), Natl Ocean & Atmospher Adm, Southeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, 75 Virginia Beach Dr, Miami, FL 33149 USA.
EM laura.dias@noaa.gov
FU Cooperative Institute for Marine and Atmospheric Studies (CIMAS), a
Cooperative Institute of the University of Miami; National Oceanic and
Atmospheric Administration, cooperative [NA15OAR4320064]
FX We greatly recognize the efforts of the many researchers, staff and
institutions that provided support for field work and data collection
during and after the DWH oil spill. Photographs used in this study were
collected by the NOAA (Brenda Rone, Adam U, Ronald Wooten, Brian Stacey
and other scientific crew), LDWF (Mandy Tumlin), and USCG. The LDWF and
the Emerald Coast Wildlife Refuge, authorized through Letters of
Authority from the National Marine Fisheries Service re gional office,
responded to the stranded ce taceans included in this study. We thank
the scientific party and crew members of the NOAA ship `Gordon Gunter'
and aircrafts. Thanks to Jill Bodnar (ORR) and Liz Stratton (SEFSC) for
providing access to additional data. We also appreciate the valuable
input provided ments. NOAA and NCCOS activities were conducted under
Marine Mammal Protection Act Permit number 779-1633. This research was
carried out (in part) under the auspices of the Cooperative Institute
for Marine and Atmospheric Studies (CIMAS), a Cooperative Institute of
the University of Miami and the National Oceanic and Atmospheric
Administration, cooperative agreement # NA15OAR4320064. This work was
part of the DWH NRDA, being conducted cooperatively among NOAA, other
federal and state Trustees, and BP PLC. The findings and conclusions in
this paper are those of the authors and do not necessarily represent the
view of NOAA or of any other natural resource Trustee for the
BP/Deepwater Horizon NRDA.
NR 17
TC 3
Z9 3
U1 0
U2 0
PU INTER-RESEARCH
PI OLDENDORF LUHE
PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY
SN 1863-5407
EI 1613-4796
J9 ENDANGER SPECIES RES
JI Endanger. Species Res.
PY 2017
VL 33
BP 119
EP 125
DI 10.3354/esr00770
PG 7
WC Biodiversity Conservation
SC Biodiversity & Conservation
GA EN0EN
UT WOS:000395683200010
ER
PT J
AU Smith, CR
Rowles, TK
Hart, LB
Townsend, FI
Wells, RS
Zolman, ES
Balmer, BC
Quigley, B
Ivancic, M
McKercher, W
Tumlin, MC
Mullin, KD
Adams, JD
Wu, QZ
Mcfee, W
Collier, TK
Schwacke, LH
AF Smith, Cynthia R.
Rowles, Teresa K.
Hart, Leslie B.
Townsend, Forrest I.
Wells, Randall S.
Zolman, Eric S.
Balmer, Brian C.
Quigley, Brian
Ivancic, Marina
McKercher, Willie
Tumlin, Mandy C.
Mullin, Keith D.
Adams, Jeffrey D.
Wu, Qingzhong
Mcfee, Wayne
Collier, Tracy K.
Schwacke, Lori H.
TI Slow recovery of Barataria Bay dolphin health following the Deepwater
Horizon oil spill (2013-2014), with evidence of persistent lung disease
and impaired stress response
SO ENDANGERED SPECIES RESEARCH
LA English
DT Article
DE Dolphin; Health; Oil; Toxicology; Pulmonary; Stress; Cortisol; Prognosis
ID BOTTLE-NOSED DOLPHINS; TURSIOPS-TRUNCATUS; RIVER OTTERS; RESPIRATORY
SYMPTOMS; CANTABRIA SPAIN; CLEANUP WORKERS; USA; HAPTOGLOBIN;
POLLUTANTS; ASTURIAS
AB The 2010 Deepwater Horizon (DWH) disaster resulted in large-scale oil contamination of the northern Gulf of Mexico. As part of the Natural Resource Damage Assessment designed to investigate the potential impacts of the DWH oil spill, comprehensive health assessments were conducted on bottlenose dolphins Tursiops truncatus living in oiled bays (Barataria Bay [BB], Louisiana, and Mississippi Sound [MS], Mississippi/Alabama) and a reference bay with no evidence of DWH oil contamination (Sarasota Bay [SB], Florida). As previously reported, multiple health issues were detected in BB dolphins during 2011. In the present study, follow-on capture-release health assessments of BB dolphins were performed (2013, 2014) and indicated an overall improvement in population health, but demonstrated that pulmonary abnormalities and impaired stress response persisted for at least 4 yr after the DWH disaster. Specifically, moderate to severe lung disease remained elevated, and BB dolphins continued to release low levels of cortisol in the face of capture stress. The proportion of guarded or worse prognoses in BB improved over time, but 4 yr post-spill, they were still above the proportion seen in SB. Health assessments performed in MS in 2013 showed similar findings to BB, characterized by an elevated prevalence of low serum cortisol and moderate to severe lung disease. Prognosis scores for dolphins examined in MS in 2013 were similar to BB in 2013. Data from these follow-on studies confirmed that dolphins living in areas affected by the DWH spill were more likely to be ill; however, some improvement in population health has occurred over time.
C1 [Smith, Cynthia R.; Ivancic, Marina] Natl Marine Mammal Fdn, 2240 Shelter Isl Dr,Suite 200, San Diego, CA 92106 USA.
[Rowles, Teresa K.; Adams, Jeffrey D.] NOAA, Natl Marine Fisheries Serv, Off Protected Resources, 1315 East West Highway, Silver Spring, MD 20910 USA.
[Hart, Leslie B.; Zolman, Eric S.; Balmer, Brian C.; Quigley, Brian; Mcfee, Wayne; Schwacke, Lori H.] NOAA, Natl Ctr Coastal Ocean Sci, 331 Ft Johnson Rd, Charleston, SC 29412 USA.
[Hart, Leslie B.] Coll Charleston, Dept Hlth & Human Performance, 66 George St, Charleston, SC 29424 USA.
[Townsend, Forrest I.] Bayside Hosp Anim, 251 Racetrack Rd NE,Ft Walton Beach, Fort Walton Beach, FL 32547 USA.
[Wells, Randall S.; Balmer, Brian C.] Mote Marine Lab, Chicago Zool Soc, 1600 Ken Thompson Pkwy, Sarasota, FL 34236 USA.
[McKercher, Willie] Mississippi Dept Environm Qual, POB 2261, Jackson, MS 39225 USA.
[Tumlin, Mandy C.] Louisiana Dept Wildlife & Fisheries, 2000 Quail Dr, Baton Rouge, LA 70898 USA.
[Mullin, Keith D.] NOAA, Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, 3209 Frederic St, Pascagoula, MS 39567 USA.
[Wu, Qingzhong; Collier, Tracy K.] Univ Corp Atmospher Res, Joint Off Sci Support, 3300 Mitchell Lane, Boulder, CO 80301 USA.
RP Smith, CR (reprint author), Natl Marine Mammal Fdn, 2240 Shelter Isl Dr,Suite 200, San Diego, CA 92106 USA.
EM cynthia.smith@nmmf.org
FU National Marine Mammal Health & Stranding Response Program; Dolphin
Quest, Inc.; Morris Animal Foundation's Betty White Wildlife Rapid
Response Fund; Disney's Animal Program and Environmental Initiatives;
Georgia Aquarium; Office of Naval Research [N000141110203]
FX We appreciate the efforts of numerous organizations and their
researchers, veterinarians, and technicians who provided support for the
health assessment projects, which include our home institutions as well
as the National Institute of Standards and Technology, SeaWorld and
Busch Gardens, Texas Marine Mammal Stranding Network, Audubon Nature
Institute, International Fund for Animal Welfare, National Park Service,
Alabama Department of Conservation and Natural Resources, Dolphin Quest,
and Georgia Aquarium. We especially thank for their efforts: Eric
Anderson, Mark Baird, Veronica Cendejas, Elsburgh Clarke, James
Daugomah, Sylvain DeGuise, Deborah Fau quier, Denise Greig, Larry
Fulford, Larry Hansen, Jeremy Hartley, Jean Herrman, Nick Kellar, Trip
Kolkmeyer, Suzanne Lane, Lauren McGeorge, Amanda Moors, Lauren Noble,
Todd Speakman, Jay Sweeney, Lydia Staggs, John Venturella, Blaine West,
and Rob Yordi. Amy Rosenstein performed thorough background literature
searches that contributed to data interpretation. We thank Dr. Ailsa
Hall for her insight, recommendations, and review of this work. This
work was part of the Deepwater Horizon NRDA being conducted
cooperatively among NOAA, other Federal and State Trustees, and BP.
Activities were conducted under National Marine Fisheries Service
Scientific Research Permit 932-1905/MA-009526, approved by a NOAA Animal
Care and Use Committee, and some funding was contributed by the National
Marine Mammal Health & Stranding Response Program. Sarasota Bay health
assessments were funded in part by Dolphin Quest, Inc., Morris Animal
Foundation's Betty White Wildlife Rapid Response Fund, Disney's Animal
Program and Environmental Initiatives, Georgia Aquarium, and the Office
of Naval Research (including ONR Award N000141110203), and were
performed under National Marine Fisheries Service Scientific Research
Permit No. 15543 and approved by Mote Marine Laboratory's Institutional
Animal Care and Use Committee.
NR 46
TC 6
Z9 6
U1 0
U2 0
PU INTER-RESEARCH
PI OLDENDORF LUHE
PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY
SN 1863-5407
EI 1613-4796
J9 ENDANGER SPECIES RES
JI Endanger. Species Res.
PY 2017
VL 33
BP 127
EP 142
DI 10.3354/esr00778
PG 16
WC Biodiversity Conservation
SC Biodiversity & Conservation
GA EN0EN
UT WOS:000395683200011
ER
PT J
AU Hornsby, FE
McDonald, TL
Balmer, BC
Speakman, TR
Mullin, KD
Rosel, PE
Wells, RS
Telander, AC
Marcy, PW
Klaphake, KC
Schwacke, LH
AF Hornsby, Fawn E.
McDonald, Trent L.
Balmer, Brian C.
Speakman, Todd R.
Mullin, Keith D.
Rosel, Patricia E.
Wells, Randall S.
Telander, Andrew C.
Marcy, Peter W.
Klaphake, Kristen C.
Schwacke, Lori H.
TI Using salinity to identify common bottlenose dolphin habitat in
Barataria Bay, Louisiana, USA
SO ENDANGERED SPECIES RESEARCH
LA English
DT Article
DE Tursiops truncatus; Habitat; Deepwater Horizon; Barataria Bay;
Telemetry; Salinity; Photo-ID
ID TURSIOPS-TRUNCATUS; SEASONAL-VARIATION; SARASOTA; IMPACTS; FLORIDA;
GENES
AB Following the Deepwater Horizon (DWH) oil spill, numerous studies were conducted to determine impacts on common bottlenose dolphins Tursiops truncatus. Common bottlenose dolphins are found in estuarine environments of the northern Gulf of Mexico which vary in salinity, depending on location (e.g. distance to freshwater source), season, and ocean tides. Although common bottlenose dolphins can be found in low-salinity waters (<15 ppt), they cannot tolerate very low salinity for long periods of time. We matched dolphin telemetry data in Barataria Bay, Louisiana (USA), with contemporaneous estimates of salinity to establish a salinity threshold and identify preferred dolphin habitat. Dolphins frequently used areas where salinity was higher than similar to 11 ppt, sometimes used areas for short periods of time with predicted salinity of similar to 8 ppt, and avoided waters with salinities below similar to 5 ppt. While not a hard boundary, the similar to 8 ppt threshold can be used to delineate reasonable polygons of preferred dolphin habitat. We temporally averaged the location of the similar to 8 ppt isohaline from 2005 through 2012 to establish areas of preferred dolphin habitat. In Barataria Bay, the polygon of dolphin habitat encompasses 1167 km(2), and extends from the bay's barrier islands to approximately half-way through marshes in northern parts of the bay. This polygon of suitable common bottlenose dolphin habitat was then ultimately used to quantify cetacean injury due to DWH oil.
C1 [Hornsby, Fawn E.; McDonald, Trent L.; Telander, Andrew C.; Marcy, Peter W.; Klaphake, Kristen C.] Western EcoSyst Technol Inc, Laramie, WY 82072 USA.
[Balmer, Brian C.; Speakman, Todd R.; Schwacke, Lori H.] NOAA, Natl Ctr Coastal Ocean Sci, Hollings Marine Lab, Charleston, SC 29412 USA.
[Mullin, Keith D.] NOAA, Southeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Pascagoula, MS 39568 USA.
[Rosel, Patricia E.] NOAA, Southeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Lafayette, LA 70506 USA.
[Wells, Randall S.] Mote Marine Lab, Chicago Zool Soc, Sarasota Dolphin Res Program, Chicago, FL 34236 USA.
RP Hornsby, FE (reprint author), Western EcoSyst Technol Inc, Laramie, WY 82072 USA.
EM fhornsby@west-inc.com
NR 39
TC 4
Z9 4
U1 0
U2 0
PU INTER-RESEARCH
PI OLDENDORF LUHE
PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY
SN 1863-5407
EI 1613-4796
J9 ENDANGER SPECIES RES
JI Endanger. Species Res.
PY 2017
VL 33
BP 181
EP 192
DI 10.3354/esr00807
PG 12
WC Biodiversity Conservation
SC Biodiversity & Conservation
GA EN0EN
UT WOS:000395683200014
ER
PT J
AU McDonald, TL
Hornsby, FE
Speakman, TR
Zolman, ES
Mullin, KD
Sinclair, C
Rosel, PE
Thomas, L
Schwacke, LH
AF McDonald, Trent L.
Hornsby, Fawn E.
Speakman, Todd R.
Zolman, Eric S.
Mullin, Keith D.
Sinclair, Carrie
Rosel, Patricia E.
Thomas, Len
Schwacke, Lori H.
TI Survival, density, and abundance of common bottlenose dolphins in
Barataria Bay (USA) following the Deepwater Horizon oil spill
SO ENDANGERED SPECIES RESEARCH
LA English
DT Article
DE Robust design; Photo-identification; Tursiops truncatus;
Capture-recapture; Spatial-capture model
ID GULF-OF-MEXICO; CAPTURE-RECAPTURE DATA; TURSIOPS-TRUNCATUS; SEASONAL
ABUNDANCE; COASTAL WATERS; ROBUST DESIGN; FLORIDA; RESPONSES; PATTERNS;
CAROLINA
AB To assess potential impacts of the Deepwater Horizon oil spill in April 2010, we conducted boat-based photo-identification surveys for common bottlenose dolphins Tursiops truncatus in Barataria Bay, Louisiana, USA (similar to 230 km(2), located 167 km WNW of the spill center). Crews logged 838 h of survey effort along pre-defined routes on 10 occasions between late June 2010 and early May 2014. We applied a previously unpublished spatial version of the robust design capture-recapture model to estimate survival and density. This model used photo locations to estimate density in the absence of study area boundaries and to separate mortality from permanent emigration. To estimate abundance, we applied density estimates to saltwater (salinity > similar to 8 ppt) areas of the bay where telemetry data suggested that dolphins reside. Annual dolphin survival varied between 0.80 and 0.85 (95% CIs varied from 0.77 to 0.90) over 3 yr following the Deepwater Horizon spill. In 2 non-oiled bays (in Florida and North Carolina), historic survival averages approximately 0.95. From June to November 2010, abundance increased from 1300 (95% CI +/- similar to 130) to 3100 (95% CI +/- similar to 400), then declined and remained between similar to 1600 and similar to 2400 individuals until spring 2013. In fall 2013 and spring 2014, abundance increased again to approximately 3100 individuals. Dolphin abundance prior to the spill was unknown, but we hypothesize that some dolphins moved out of the sampled area, probably northward into marshes, prior to initiation of our surveys in late June 2010, and later immigrated back into the sampled area.
C1 [McDonald, Trent L.; Hornsby, Fawn E.] Western EcoSystems Technol Inc, Laramie, WY 82070 USA.
[Speakman, Todd R.; Zolman, Eric S.; Schwacke, Lori H.] NOAA, Natl Ctr Coastal Ocean Sci, Hollings Marine Lab, Charleston, SC 29412 USA.
[Mullin, Keith D.; Sinclair, Carrie] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Pascagoula, MS 39568 USA.
[Rosel, Patricia E.] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Lafayette, LA 70506 USA.
[Thomas, Len] Univ St Andrews, Ctr Res Ecol & Environm Modelling, St Andrews KY16 9LZ, Fife, Scotland.
RP McDonald, TL (reprint author), Western EcoSystems Technol Inc, Laramie, WY 82070 USA.
EM tmcdonald@west-inc.com
NR 70
TC 6
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U1 0
U2 0
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PI OLDENDORF LUHE
PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY
SN 1863-5407
EI 1613-4796
J9 ENDANGER SPECIES RES
JI Endanger. Species Res.
PY 2017
VL 33
BP 193
EP 209
DI 10.3354/esr00806
PG 17
WC Biodiversity Conservation
SC Biodiversity & Conservation
GA EN0EN
UT WOS:000395683200015
ER
PT J
AU Rosel, PE
Wilcox, LA
Sinclair, C
Speakman, TR
Tumlin, MC
Litz, JA
Zolman, ES
AF Rosel, P. E.
Wilcox, L. A.
Sinclair, C.
Speakman, T. R.
Tumlin, M. C.
Litz, J. A.
Zolman, E. S.
TI Genetic assignment to stock of stranded common bottlenose dolphins in
south eastern Louisiana after the Deepwater Horizon oil spill
SO ENDANGERED SPECIES RESEARCH
LA English
DT Article
DE Assignment test; Mixed stock analysis; Genetic stock identification;
Microsatellite
ID GULF-OF-MEXICO; MAIN HAWAIIAN-ISLANDS; TURSIOPS-TRUNCATUS;
POPULATION-STRUCTURE; MICROSATELLITE MARKERS; MULTILOCUS GENOTYPES;
CETACEAN POPULATIONS; SEASONAL ABUNDANCE; CHINOOK SALMON; FISH STOCKS
AB Degradation of marine ecosystems is an increasing problem and extends beyond nearshore coastal waters with significant human development. However, measuring ecosystem damage and decreased ecosystem function can be difficult. Marine mammals have often been recommended as indicators for evaluating ecosystem health. Between March 2010 and July 2014, a significant cetacean unusual mortality event occurred across the northern Gulf of Mexico, where multiple demographically independent populations of common bottlenose dolphins Tursiops truncatus occur adjacent to one another. Some populations are fairly small and restricted to small habitat areas, while other populations have higher abundances and cover broader geographic ranges. An integral component to determining the impact of this event on these populations is identifying what percentage of each population the stranded animals comprise. We applied genetic assignment test methods to stranded dolphins from southeastern Louisiana to determine the proportion of dead dolphins that came from the local estuarine population versus the population found in adjacent coastal waters. Forty-one microsatellite loci were genotyped in 156 live dolphins sampled to represent the 2 potential stocks of origin and in 131 dead stranded dolphins of unknown origin. Both classical assignment tests and genetic stock identification methods indicated that approximately 6 to 7% of the sampled stranded dolphins originated from the Western Coastal Stock and the remainder from the smaller, estuarine stock in Barataria Bay, Louisiana.
C1 [Rosel, P. E.; Wilcox, L. A.] Southeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Lafayette, LA 70506 USA.
[Sinclair, C.] Southeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Pascagoula, MS 39568 USA.
[Speakman, T. R.] NOAA, Natl Ctr Coastal Ocean Sci, Hollings Marine Lab, Charleston, SC 29412 USA.
[Tumlin, M. C.] Louisiana Dept Wildlife & Fisheries, Baton Rouge, LA 70808 USA.
[Litz, J. A.] Southeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Miami, FL 33149 USA.
RP Rosel, PE (reprint author), Southeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Lafayette, LA 70506 USA.
EM patricia.rosel@noaa.gov
NR 80
TC 4
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U1 0
U2 0
PU INTER-RESEARCH
PI OLDENDORF LUHE
PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY
SN 1863-5407
EI 1613-4796
J9 ENDANGER SPECIES RES
JI Endanger. Species Res.
PY 2017
VL 33
BP 221
EP 234
DI 10.3354/esr00780
PG 14
WC Biodiversity Conservation
SC Biodiversity & Conservation
GA EN0EN
UT WOS:000395683200017
ER
PT J
AU Hohn, AA
Thomas, L
Carmichael, RH
Litz, J
Clemons-Chevis, C
Shippee, SF
Sinclair, C
Smith, S
Speakman, TR
Tumlin, MC
Zolman, ES
AF Hohn, A. A.
Thomas, L.
Carmichael, R. H.
Litz, J.
Clemons-Chevis, C.
Shippee, S. F.
Sinclair, C.
Smith, S.
Speakman, T. R.
Tumlin, M. C.
Zolman, E. S.
TI Assigning stranded bottlenose dolphins to source stocks using stable
isotope ratios following the Deepwater Horizon oil spill
SO ENDANGERED SPECIES RESEARCH
LA English
DT Article
DE Carbon; Nitrogen; Sulfur; Tursiops truncatus; Stock structure; Gulf of
Mexico
ID GULF-OF-MEXICO; TROUT CYNOSCION-NEBULOSUS; UNUSUAL MORTALITY EVENT;
EASTERN NORTH-ATLANTIC; MAIN HAWAIIAN-ISLANDS; ESTUARINE FOOD WEBS;
TURSIOPS-TRUNCATUS; POPULATION-STRUCTURE; COASTAL WATERS; SEASONAL
ABUNDANCE
AB The potential for stranded dolphins to serve as a tool for monitoring free-ranging populations would be enhanced if their stocks of origin were known. We used stable isotopes of carbon, nitrogen, and sulfur from skin to assign stranded bottlenose dolphins Tursiops truncatus to different habitats, as a proxy for stocks (demographically independent populations), following the Deepwater Horizon oil spill. Model results from biopsy samples collected from dolphins from known habitats (n = 205) resulted in an 80.5% probability of correct assignment. These results were applied to data from stranded dolphins (n = 217), resulting in predicted assignment probabilities of 0.473, 0.172, and 0.355 to Estuarine, Barrier Island (BI), and Coastal stocks, respectively. Differences were found west and east of the Mississippi River, with more Coastal dolphins stranding in western Louisiana and more Estuarine dolphins stranding in Mississippi. Within the Estuarine East Stock, 2 groups were identified, one predominantly associated with Mississippi and Alabama estuaries and another with western Florida. delta N-15 values were higher in stranded samples for both Estuarine and BI stocks, potentially indicating nutritional stress. High probabilities of correct assignment of the biopsy samples indicate predictable variation in stable isotopes and fidelity to habitat. The power of delta S-34 to discriminate habitats relative to salinity was essential. Stable isotopes may provide guidance regarding where additional testing is warranted to confirm demographic independence and aid in determining the source habitat of stranded dolphins, thus increasing the value of biological data collected from stranded individuals.
C1 [Hohn, A. A.] Southeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Natl Ocean & Atmospher Adm, 101 Pivers Isl Rd, Beaufort, NC 28516 USA.
[Thomas, L.] Univ St Andrews, CREEM, Observ Buchanan Gardens, St Andrews KY16 9LZ, Fife, Scotland.
[Carmichael, R. H.] Dauphin Isl Sea Lab, Dauphin Isl, AL 36528 USA.
[Carmichael, R. H.] Univ S Alabama, Mobile, AL 36688 USA.
[Litz, J.] Southeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Natl Ocean & Atmospher Adm, 75 Virginia Key Dr, Miami, FL 33149 USA.
[Clemons-Chevis, C.] Inst Marine Mammal Studies, POB 207, Gulfport, MS 39502 USA.
[Shippee, S. F.] Marine Wildlife Response, 1557 Highway 98 W, Mary Esther, FL 32569 USA.
[Sinclair, C.] Southeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Natl Ocean & Atmospher Adm, 3209 Frederic St, Pascagoula, MS 39567 USA.
[Smith, S.] Audubon Aquarium Amer, 1 Canal St, New Orleans, LA 70124 USA.
[Speakman, T. R.] Natl Centers Coastal Ocean Sci, Natl Ocean Serv, Natl Ocean & Atmospher Adm, Hollings Marine Lab, 331 Ft Johnson, Charleston, SC 29412 USA.
[Tumlin, M. C.] Louisiana Dept Wildlife & Fisheries, 2000 Quail Dr, Baton Rouge, LA USA.
[Smith, S.] Amazon River Dolphin Conservat Fdn, 805 Hidalgo St, New Orleans, LA 70124 USA.
RP Hohn, AA (reprint author), Southeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Natl Ocean & Atmospher Adm, 101 Pivers Isl Rd, Beaufort, NC 28516 USA.
EM aleta.hohn@noaa.gov
FU Deepwater Horizon NRDA investigation
FX This study was conducted as part of, and was funded by, the Deepwater
Horizon NRDA investigation, which was cooperatively conducted by NOAA,
other Federal and State Trustees, and BP. The scientific results and
conclusions of this publication, as well as any views or opinions
expressed herein, are those of the authors and do not necessarily
represent the view of NOAA or any other natural resource Trustee for the
BP/Deepwater Horizon NRDA. We thank the members of the Marine Mammal
Stranding Network (MMSN) in the northern GoM for their tireless efforts
during a large and long UME. We appreciate the willingness of Gulf World
to provide samples although ultimately their area of coverage was
outside the range of this study. Staff from the Southeast Fisheries
Science Center laboratories and National Center for Coastal Ocean
Science Hollings Marine Laboratory were instrumental in obtaining
stranding data and biopsy samples during health assessments or vessel
surveys. We appreciate the input of other members of the Population
Quantification Team, Brian Balmer, Cormac Booth, Lance Garrison, Fawn
Hornsby, Nick Kellar, Trent McDonald, Keith Mullin, Patricia Rosel, Teri
Rowles, and Randall Wells, and the statistics review team, Phil Dixon,
Jay Ver Hoef, Tomo Eguchi, Trent McDonald, Robin Waples, and Ailsa Hall.
The manuscript was reviewed by Colleen Bryan, Alex Chester, Steven
Christopher, Jessica Reiner, all from NOAA, and 2 anonymous reviewers.
Barbie Byrd, NOAA Beaufort Lab, assisted with preparation of the
figures. Remote biopsy samples were collected under Marine Mammal
Protection Act (MMPA) Permit No. 14450 and those collected during health
assessments were collected under MMPA Permit No. 932-1905/MA-009526,
both issued by NMFS. Protocols were reviewed and approved by the NOAA
Institutional Animal Care and Use Committee. Response to cetacean
stranding events is conducted by MMSN authorized under Section 112c
(Stranding Agreements from the NMFS regional offices) or Section 109h
(Federal, State, or local government officials) of the MMPA. This
publication does not constitute an endorsement of any commercial product
or intend to be an opinion beyond scientific or other results obtained
by NOAA.
NR 127
TC 3
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U1 0
U2 0
PU INTER-RESEARCH
PI OLDENDORF LUHE
PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY
SN 1863-5407
EI 1613-4796
J9 ENDANGER SPECIES RES
JI Endanger. Species Res.
PY 2017
VL 33
BP 235
EP 252
DI 10.3354/esr00783
PG 18
WC Biodiversity Conservation
SC Biodiversity & Conservation
GA EN0EN
UT WOS:000395683200018
ER
PT J
AU Schwacke, LH
Thomas, L
Wells, RS
Mcfee, WE
Hohn, AA
Mullin, KD
Zolman, ES
Quigley, BM
Rowles, TK
Schwacke, JH
AF Schwacke, Lori H.
Thomas, Len
Wells, Randall S.
Mcfee, Wayne E.
Hohn, Aleta A.
Mullin, Keith D.
Zolman, Eric S.
Quigley, Brian M.
Rowles, Teri K.
Schwacke, John H.
TI Quantifying injury to common bottlenose dolphins from the Deepwater
Horizon oil spill using an age-, sex- and class-structured population
model
SO ENDANGERED SPECIES RESEARCH
LA English
DT Article
DE Population model; Monte Carlo analysis; Survival; Density dependence;
Bayesian model; Deepwater Horizon; Impact assessment; Cetacean
ID EASTERN TROPICAL PACIFIC; WHALES ORCINUS-ORCA; PRINCE-WILLIAM-SOUND;
TURSIOPS-TRUNCATUS; MORTALITY; REPRODUCTION; DEMOGRAPHY; ABUNDANCE;
RECOVERY; BIOLOGY
AB Field studies documented increased mortality, adverse health effects, and reproductive failure in common bottlenose dolphins Tursiops truncatus following the Deepwater Horizon (DWH) oil spill. In order to determine the appropriate type and amount of restoration needed to compensate for losses, the overall extent of injuries to dolphins had to be quantified. Simply counting dead individuals does not consider long-term impacts to populations, such as the loss of future reproductive potential from mortality of females, or the chronic health effects that continue to compromise survival long after acute effects subside. Therefore, we constructed a sex-and age-structured model of population growth and included additional class structure to represent dolphins exposed and unexposed to DWH oil. The model was applied for multiple stocks to predict injured population trajectories using estimates of post-spill survival and reproductive rates. Injured trajectories were compared to baseline trajectories that were expected had the DWH incident not occurred. Two principal measures of injury were computed: (1) lost cetacean years (LCY); the difference between baseline and injured population size, summed over the modeled time period, and (2) time to recovery; the number of years for the stock to recover to within 95% of baseline. For the dolphin stock in Barataria Bay, Louisiana, the estimated LCY was substantial: 30 347 LCY (95% CI: 11 511 to 89 746). Estimated time to recovery was 39 yr (95% CI: 24 to 80). Similar recovery timelines were predicted for stocks in the Mississippi River Delta, Mississippi Sound, Mobile Bay and the Northern Coastal Stock.
C1 [Schwacke, Lori H.; Mcfee, Wayne E.; Zolman, Eric S.; Quigley, Brian M.] Natl Centers Coastal Ocean Sci, Natl Ocean Serv, Natl Ocean & Atmospher Adm, Charleston, SC 29412 USA.
[Thomas, Len] Univ St Andrews, CREEM, Observ Buchanan Gardens, St Andrews KY16 9LZ, Fife, Scotland.
[Wells, Randall S.] Chicago Zool Soc, Mote Marine Lab, Sarasota, FL 34236 USA.
[Hohn, Aleta A.] Southeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Natl Ocean & Atmospher Adm, Beaufort, NC 28516 USA.
[Mullin, Keith D.] Southeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Natl Ocean & Atmospher Adm, Pascagoula, MS 39568 USA.
[Rowles, Teri K.] Off Protected Resources, Natl Marine Fisheries Serv, Natl Ocean & Atmospher Adm, Silver Spring, MD 20910 USA.
[Schwacke, John H.] Sci Res Corp, Charleston, SC 29406 USA.
[Schwacke, Lori H.] Natl Marine Mammal Fdn, San Diego, CA 92106 USA.
RP Schwacke, LH (reprint author), Natl Centers Coastal Ocean Sci, Natl Ocean Serv, Natl Ocean & Atmospher Adm, Charleston, SC 29412 USA.; Schwacke, LH (reprint author), Natl Marine Mammal Fdn, San Diego, CA 92106 USA.
EM lori.schwacke@nmmpfoundation.org
NR 58
TC 5
Z9 5
U1 1
U2 1
PU INTER-RESEARCH
PI OLDENDORF LUHE
PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY
SN 1863-5407
EI 1613-4796
J9 ENDANGER SPECIES RES
JI Endanger. Species Res.
PY 2017
VL 33
BP 265
EP 279
DI 10.3354/esr00777
PG 15
WC Biodiversity Conservation
SC Biodiversity & Conservation
GA EN0EN
UT WOS:000395683200020
ER
PT J
AU Glotter, M
Elliott, J
AF Glotter, Michael
Elliott, Joshua
TI Simulating US agriculture in a modern Dust Bowl drought
SO NATURE PLANTS
LA English
DT Article
ID GLOBAL CROP PRODUCTION; CLIMATE-CHANGE; GREAT-PLAINS; UNITED-STATES;
1930S; TRENDS; TEMPERATURE; RESPONSES; IMPACTS; SYSTEM
AB Drought-induced agricultural loss is one of the most costly impacts of extreme weather(1-3), and without mitigation, climate change is likely to increase the severity and frequency of future droughts(4,5). The Dust Bowl of the 1930s was the driest and hottest for agriculture in modern US history. Improvements in farming practices have increased productivity, but yields today are still tightly linked to climate variation(6) and the impacts of a 1930s-type drought on current and future agricultural systems remain unclear. Simulations of biophysical process and empirical models suggest that Dust-Bowl-type droughts today would have unprecedented consequences, with yield losses similar to 50% larger than the severe drought of 2012. Damages at these extremes are highly sensitive to temperature, worsening by similar to 25% with each degree centigrade of warming. We find that high temperatures can be more damaging than rainfall deficit, and, without adaptation, warmer mid-century temperatures with even average precipitation could lead to maize losses equivalent to the Dust Bowl drought. Warmer temperatures alongside consecutive droughts could make up to 85% of rain-fed maize at risk of changes that may persist for decades. Understanding the interactions of weather extremes and a changing agricultural system is therefore critical to effectively respond to, and minimize, the impacts of the next extreme drought event.
C1 [Glotter, Michael] Univ Chicago, Dept Geophys Sci, 5734 S Ellis Ave, Chicago, IL 60637 USA.
[Elliott, Joshua] NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
[Elliott, Joshua] Univ Chicago, Computat Inst, 5735 S Ellis Ave, Chicago, IL 60637 USA.
RP Glotter, M (reprint author), Univ Chicago, Dept Geophys Sci, 5734 S Ellis Ave, Chicago, IL 60637 USA.; Elliott, J (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.; Elliott, J (reprint author), Univ Chicago, Computat Inst, 5735 S Ellis Ave, Chicago, IL 60637 USA.
EM glotter@uchicago.edu; jelliott@ci.uchicago.edu
FU NSF through Decision Making Under Uncertainty program [SES-0951576]; NSF
Graduate Fellowship [DGE-1144082]; NSF [OCI-1148443]
FX This research was performed as part of the Center for Robust
Decision-making on Climate and Energy Policy (RDCEP) at the University
of Chicago. RDCEP is funded by a grant from NSF (no. SES-0951576)
through the Decision Making Under Uncertainty program. M.G. acknowledges
support of an NSF Graduate Fellowship (no. DGE-1144082). We thank C.
Muller, A. Ruane and J. Winter-as well as the AgMIP (Agricultural Model
Intercomparison and Improvement Project) community-for valuable insight
in formulating the ideas for this research. We acknowledge the World
Climate Research Programme'sWorking Group on Coupled Modelling, and we
thank the climate modelling groups for producing and making available
their model output. For CMIP, the US Department of Energy's Program for
Climate Model Diagnosis and Intercomparison provides coordinating
support and software infrastructure development in partnership with the
Global Organization for Earth System Science Portals. Computing for this
project was facilitated using the Swift parallel scripting language (NSF
grant OCI-1148443), and completed in part with resources provided by the
University of Chicago Research Computing Center.
NR 55
TC 0
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U1 0
U2 0
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2055-026X
EI 2055-0278
J9 NAT PLANTS
JI Nat. Plants
PD JAN
PY 2017
VL 3
IS 1
AR 16193
DI 10.1038/nplants.2016.193
PG 6
WC Plant Sciences
SC Plant Sciences
GA EN3HI
UT WOS:000395899200001
ER
PT J
AU Gadallah, KAK
Marchione, D
Koehler, SPK
McCoustra, MRS
AF Gadallah, Kamel A. K.
Marchione, Demian
Koehler, Sven P. K.
McCoustra, Martin R. S.
TI Molecular hydrogen production from amorphous solid water during low
energy electron irradiation
SO PHYSICAL CHEMISTRY CHEMICAL PHYSICS
LA English
DT Article
ID LOW-MASS PROTOSTAR; INTERSTELLAR HEAVY-WATER; SOLAR-TYPE PROTOSTARS;
DEUTERIUM FRACTIONATION; STIMULATED DESORPTION; INNER REGIONS;
DEUTERATED MOLECULES; SPECTROSCOPIC SURVEY; SURFACE-CHEMISTRY; IRAS
16293-2422
AB This work investigates the production of molecular hydrogen isotopologues (H-2, HD, and D-2) during low energy electron irradiation of layered and isotopically labelled thin films of amorphous solid water (ASW) in ultrahigh vacuum. Experimentally, the production of these molecules with both irradiation time and incident electron energy in the range 400 to 500 eV is reported as a function of the depth of a buried D2O layer in an H2O film. H-2 is produced consistently in all measurements, reflecting the H2O component of the film, though it does exhibit a modest reduction in intensity at the time corresponding to product escape from the buried D2O layer. In contrast, HD and D-2 production exhibit peaks at times corresponding to product escape from the buried D2O layer in the composite film. These features broaden the deeper the HD or D-2 is formed due to diffusion. A simple random-walk model is presented that can qualitatively explain the appearance profile of these peaks as a function of the incident electron penetration.
C1 [Gadallah, Kamel A. K.; Marchione, Demian; McCoustra, Martin R. S.] Heriot Watt Univ, Sch Engn & Phys Sci, Edinburgh EH14 4AS, Midlothian, Scotland.
[Gadallah, Kamel A. K.] Al Azhar Univ, Fac Sci, Astron & Meteorol Dept, POB 11884, Cairo, Egypt.
[Marchione, Demian] CALTECH, Div Sci, Jet Prop Lab, Pasadena, CA 91109 USA.
[Koehler, Sven P. K.] Univ Manchester, Sch Chem, Manchester M13 9PL, Lancs, England.
[Koehler, Sven P. K.] Univ Manchester, Dalton Cumbrian Facil, Westlakes Sci & Technol Pk, Moor Row CA24 3HA, England.
RP Gadallah, KAK (reprint author), Heriot Watt Univ, Sch Engn & Phys Sci, Edinburgh EH14 4AS, Midlothian, Scotland.; Gadallah, KAK (reprint author), Al Azhar Univ, Fac Sci, Astron & Meteorol Dept, POB 11884, Cairo, Egypt.
EM Kamel.Gadallah71@Gmail.com
OI Gadallah, Kamel/0000-0001-8496-5763; Koehler, Sven/0000-0002-6303-6524;
McCoustra, Martin/0000-0002-5716-110X
FU Egyptian Science & Technology Development Fund (STDF) [6119]; UK Science
and Technology Facilities Council (STFC) [ST/M001075/1]; Engineering and
Physical Sciences Research Council (EPSRC) [GR/T27044/02]; European
Community FP7-ITN Marie-Curie Programme (LASSIE) [238258]
FX This work was financially supported by the Egyptian Science & Technology
Development Fund (STDF; Project ID: 6119). We thank all the team at the
STDF. MRSM acknowledges the support of the UK Science and Technology
Facilities Council (STFC, ST/M001075/1), Engineering and Physical
Sciences Research Council (EPSRC, GR/T27044/02) and the European
Community FP7-ITN Marie-Curie Programme (LASSIE project, grant agreement
#238258). DM clarifies that his contribution to this work has been done
as a private venture and not in the author's capacity as an affiliate of
the Jet Propulsion Laboratory, California Institute of Technology.
NR 71
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U1 2
U2 2
PU ROYAL SOC CHEMISTRY
PI CAMBRIDGE
PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS,
ENGLAND
SN 1463-9076
EI 1463-9084
J9 PHYS CHEM CHEM PHYS
JI Phys. Chem. Chem. Phys.
PY 2017
VL 19
IS 4
BP 3349
EP 3357
DI 10.1039/c6cp06928b
PG 9
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA EL9KZ
UT WOS:000394940400075
PM 28091646
ER
PT J
AU de Sousa, CHR
Hilker, T
Waring, R
de Moura, YM
Lyapustin, A
AF de Sousa, Celio Helder Resende
Hilker, Thomas
Waring, Richard
de Moura, Yhasmin Mendes
Lyapustin, Alexei
TI Progress in Remote Sensing of Photosynthetic Activity over the Amazon
Basin
SO REMOTE SENSING
LA English
DT Article
DE MAIAC; MODIS; Amazon; tropical forest; drought; photosynthesis; GPP;
light use efficiency; Sun-induced fluorescence; eddy-flux
ID LIGHT-USE EFFICIENCY; PHOTOCHEMICAL REFLECTANCE INDEX; TERRESTRIAL
CHLOROPHYLL FLUORESCENCE; DOUGLAS-FIR FOREST; ATMOSPHERIC CORRECTION;
RADIATIVE-TRANSFER; CARBON EXCHANGE; RAIN-FOREST; DROUGHT; SPACE
AB Although quantifying the massive exchange of carbon that takes place over the Amazon Basin remains a challenge, progress is being made as the remote sensing community moves from using traditional, reflectance-based vegetation indices, such as the Normalized Difference Vegetation Index (NDVI), to the more functional Photochemical Reflectance Index (PRI). This new index, together with satellite-derived estimates of canopy light interception and Sun-Induced Fluorescence (SIF), provide improved estimates of Gross Primary Production (GPP). This paper traces the development of these new approaches, compares the results of their analyses from multiple years of data acquired across the Amazon Basin and suggests further improvements in instrument design, data acquisition and processing. We demonstrated that our estimates of PRI are in generally good agreement with eddy-flux tower measurements of photosynthetic light use efficiency (epsilon) at four sites in the Amazon Basin: r(2) values ranged from 0.37 to 0.51 for northern flux sites and to 0.78 for southern flux sites. This is a significant advance over previous approaches seeking to establish a link between global-scale photosynthetic activity and remotely-sensed data. When combined with measurements of Sun-Induced Fluorescence (SIF), PRI provides realistic estimates of seasonal variation in photosynthesis over the Amazon that relate well to the wet and dry seasons. We anticipate that our findings will steer the development of improved approaches to estimate photosynthetic activity over the tropics.
C1 [de Sousa, Celio Helder Resende; Waring, Richard] Oregon State Univ, Dept Forest Ecosyst & Soc, Corvallis, OR 97331 USA.
[Hilker, Thomas] Oregon State Univ, Dept Forest Engn Resources & Management, Corvallis, OR 97331 USA.
[de Moura, Yhasmin Mendes] INPE, Div Sensoriamento Remoto, BR-12227010 Sao Jose Dos Campos, SP, Brazil.
[Lyapustin, Alexei] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP de Sousa, CHR (reprint author), Oregon State Univ, Dept Forest Ecosyst & Soc, Corvallis, OR 97331 USA.
EM celio.sousa@oregonstate.edu; thomas.hilker@oregonstate.edu;
richard.waring@oregonstate.edu; yhas.mendes@gmail.com;
alexei.i.lyapustin@nasa.gov
FU CAPES Brazil (Coordenacao de Aperfeicoamento de Pessoal de Nivel
Superior) [BEX 1233-13-0]
FX This research was supported in part by a scholarship from CAPES Brazil
(Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior, Grant
Number BEX 1233-13-0) awarded to the author. Many thanks to the
reviewers who provided insightful suggestions on an earlier draft of the
manuscript.
NR 66
TC 0
Z9 0
U1 1
U2 1
PU MDPI AG
PI BASEL
PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD JAN
PY 2017
VL 9
IS 1
AR 48
DI 10.3390/rs9010048
PG 23
WC Remote Sensing
SC Remote Sensing
GA EM7LN
UT WOS:000395492600048
ER
PT J
AU Goncalves, F
Treuhaft, R
Law, B
Almeida, A
Walker, W
Baccini, A
dos Santos, JR
Graca, P
AF Goncalves, Fabio
Treuhaft, Robert
Law, Beverly
Almeida, Andre
Walker, Wayne
Baccini, Alessandro
dos Santos, Joao Roberto
Graca, Paulo
TI Estimating Aboveground Biomass in Tropical Forests: Field Methods and
Error Analysis for the Calibration of Remote Sensing Observations
SO REMOTE SENSING
LA English
DT Article
DE forest inventory; allometry; uncertainty; error propagation; Amazon;
ICESat; GLAS
ID TAPAJOS NATIONAL FOREST; CARBON STOCKS; RAIN-FOREST; AMAZONIAN FORESTS;
SECONDARY FOREST; LIDAR; UNCERTAINTY; BRAZIL; ALLOMETRY; TREES
AB Mapping and monitoring of forest carbon stocks across large areas in the tropics will necessarily rely on remote sensing approaches, which in turn depend on field estimates of biomass for calibration and validation purposes. Here, we used field plot data collected in a tropical moist forest in the central Amazon to gain a better understanding of the uncertainty associated with plot-level biomass estimates obtained specifically for the calibration of remote sensing measurements. In addition to accounting for sources of error that would be normally expected in conventional biomass estimates (e.g., measurement and allometric errors), we examined two sources of uncertainty that are specific to the calibration process and should be taken into account in most remote sensing studies: the error resulting from spatial disagreement between field and remote sensing measurements (i.e., co-location error), and the error introduced when accounting for temporal differences in data acquisition. We found that the overall uncertainty in the field biomass was typically 25% for both secondary and primary forests, but ranged from 16 to 53%. Co-location and temporal errors accounted for a large fraction of the total variance (>65%) and were identified as important targets for reducing uncertainty in studies relating tropical forest biomass to remotely sensed data. Although measurement and allometric errors were relatively unimportant when considered alone, combined they accounted for roughly 30% of the total variance on average and should not be ignored. Our results suggest that a thorough understanding of the sources of error associated with field-measured plot-level biomass estimates in tropical forests is critical to determine confidence in remote sensing estimates of carbon stocks and fluxes, and to develop strategies for reducing the overall uncertainty of remote sensing approaches.
C1 [Goncalves, Fabio] Canopy Remote Sensing Solut, BR-88032 Florianopolis, SC, Brazil.
[Treuhaft, Robert] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Law, Beverly] Oregon State Univ, Dept Forest Ecosyst & Soc, Corvallis, OR 97331 USA.
[Almeida, Andre] Univ Fed Sergipe, Dept Engn Agr, BR-49100 Sao Cristovao, SE, Brazil.
[Walker, Wayne; Baccini, Alessandro] Woods Hole Res Ctr, Falmouth, MA 02540 USA.
[dos Santos, Joao Roberto] Natl Inst Space Res INPE, BR-12227 Sao Jose Dos Campos, SP, Brazil.
[Graca, Paulo] Natl Inst Res Amazonia INPA, Dept Environm Dynam, BR-69067 Manaus, AM, Brazil.
RP Goncalves, F (reprint author), Canopy Remote Sensing Solut, BR-88032 Florianopolis, SC, Brazil.
EM fabio@canopyrss.tech; robert.n.treuhaft@jpl.nasa.gov;
bev.law@oregonstate.edu; andre.almeida@ufs.br; wwalker@whrc.org;
abaccini@whrc.org; joao.roberto@inpe.br; pmlag@inpa.gov.br
FU CAPES Foundation; Brazilian Ministry of Education, through the
CAPES/Fulbright Doctoral Program [BEX-2684/06-3]; Office of Science
(BER), US Department of Energy (DOE) [DE-FG02-07ER64361]; Conselho
Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq/MCTI)
[010301/2009-7]; Instituto Chico Mendes de Conservacao da Biodiversidade
(ICMBio/MMA, SISBIO) [20591-2]
FX The research described in this paper was carried out in part at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration, under
the Terrestrial Ecology program element. F.G. was partially funded by
the CAPES Foundation, Brazilian Ministry of Education, through the
CAPES/Fulbright Doctoral Program (process BEX-2684/06-3). B.L. was
supported by Office of Science (BER), US Department of Energy (DOE grant
no. DE-FG02-07ER64361). The authors would like to thank Brazil's
Conselho Nacional de Desenvolvimento Cientifico e Tecnologico
(CNPq/MCTI, Scientific Expedition process 010301/2009-7) and Instituto
Chico Mendes de Conservacao da Biodiversidade (ICMBio/MMA, SISBIO
process 20591-2) for research authorizations, and the Santarem office of
the Large Scale Biosphere-Atmosphere Experiment in Amazonia (LBA) for
providing logistical support. They would also like to thank Edilson
Oliveira (UFAC) and the local assistants Jony Oliveira, Raimundo dos
Santos, Iracelio Silva, and Emerson Pedroso for the invaluable help with
the field acquisitions.
NR 63
TC 0
Z9 0
U1 2
U2 2
PU MDPI AG
PI BASEL
PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD JAN
PY 2017
VL 9
IS 1
AR 47
DI 10.3390/rs9010047
PG 23
WC Remote Sensing
SC Remote Sensing
GA EM7LN
UT WOS:000395492600047
ER
PT J
AU Ulsig, L
Nichol, CJ
Huemmrich, KF
Landis, DR
Middleton, EM
Lyapustin, AI
Mammarella, I
Levula, J
Porcar-Castell, A
AF Ulsig, Laura
Nichol, Caroline J.
Huemmrich, Karl F.
Landis, David R.
Middleton, Elizabeth M.
Lyapustin, Alexei I.
Mammarella, Ivan
Levula, Janne
Porcar-Castell, Albert
TI Detecting Inter-Annual Variations in the Phenology of Evergreen Conifers
Using Long-Term MODIS Vegetation Index Time Series
SO REMOTE SENSING
LA English
DT Article
DE phenology; MODIS; Photochemical Reflectance Index (PRI); Normalized
Difference Vegetation Index (NDVI); ecosystem productivity; time series
analysis
ID LIGHT-USE EFFICIENCY; PHOTOCHEMICAL REFLECTANCE INDEX; SCOTS PINE
FOREST; RADIATION USE EFFICIENCY; DECIDUOUS FOREST; CARBON-DIOXIDE;
PHOTOSYNTHETIC EFFICIENCY; MONITORING VEGETATION; MEDITERRANEAN FOREST;
OPTICAL INDICATOR
AB Long-term observations of vegetation phenology can be used to monitor the response of terrestrial ecosystems to climate change. Satellite remote sensing provides the most efficient means to observe phenological events through time series analysis of vegetation indices such as the Normalized Difference Vegetation Index (NDVI). This study investigates the potential of a Photochemical Reflectance Index (PRI), which has been linked to vegetation light use efficiency, to improve the accuracy of MODIS-based estimates of phenology in an evergreen conifer forest. Timings of the start and end of the growing season (SGS and EGS) were derived from a 13-year-long time series of PRI and NDVI based on a MAIAC (multi-angle implementation of atmospheric correction) processed MODIS dataset and standard MODIS NDVI product data. The derived dates were validated with phenology estimates from ground-based flux tower measurements of ecosystem productivity. Significant correlations were found between the MAIAC time series and ground-estimated SGS (R-2 = 0.36-0.8), which is remarkable since previous studies have found it difficult to observe inter-annual phenological variations in evergreen vegetation from satellite data. The considerably noisier NDVI product could not accurately predict SGS, and EGS could not be derived successfully from any of the time series. While the strongest relationship overall was found between SGS derived from the ground data and PRI, MAIAC NDVI exhibited high correlations with SGS more consistently (R-2 > 0.6 in all cases). The results suggest that PRI can serve as an effective indicator of spring seasonal transitions, however, additional work is necessary to confirm the relationships observed and to further explore the usefulness of MODIS PRI for detecting phenology.
C1 [Ulsig, Laura; Nichol, Caroline J.] Univ Edinburgh, Sch GeoSci, Alexander Crum Brown Rd, Edinburgh EH9 3FF, Midlothian, Scotland.
[Huemmrich, Karl F.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol JCET, Catonsville, MD 20771 USA.
[Landis, David R.] Global Sci & Technol, Greenbelt, MD 20770 USA.
[Middleton, Elizabeth M.; Lyapustin, Alexei I.] NASA Goddard Space Flight Ctr, Earth Sci, Greenbelt, MD 20771 USA.
[Mammarella, Ivan] Univ Helsinki, Dept Phys, POB 48, Helsinki 00014, Finland.
[Levula, Janne] Univ Helsinki, SMEARII, Hyytiala Forestry Field Stn, Deptartment Phys, Hyytialantie 124, FI-35500 Korkeakoski, Finland.
[Porcar-Castell, Albert] Univ Helsinki, Dept Forest Sci, Viikki Plant Sci Ctr ViPS, POB 27, Helsinki 00014, Finland.
RP Ulsig, L; Nichol, CJ (reprint author), Univ Edinburgh, Sch GeoSci, Alexander Crum Brown Rd, Edinburgh EH9 3FF, Midlothian, Scotland.
EM laura.ulsig@gmail.com; caroline.nichol@ed.ac.uk;
karl.f.huemmrich@nasa.gov; david.r.landis@nasa.gov;
elizabeth.m.middleton@nasa.gov; alexei.i.lyapustin@nasa.gov;
ivan.mammarella@helsinki.fi; janne.levula@helsinki.fi;
joan.porcar@helsinki.fi
OI Mammarella, Ivan/0000-0002-8516-3356
FU Academy of Finland [1288039]
FX We thank the National Centre of Excellence (272041) and ICOS-FINLAND
(281255) funded by Academy of Finland, and the Academy of Finland
(Project # 1288039). We further offer thanks to Pasi Kolari for his
support in preparing the flux dataset used in this analysis.
NR 70
TC 0
Z9 0
U1 0
U2 0
PU MDPI AG
PI BASEL
PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD JAN
PY 2017
VL 9
IS 1
AR 49
DI 10.3390/rs9010049
PG 21
WC Remote Sensing
SC Remote Sensing
GA EM7LN
UT WOS:000395492600049
ER
PT J
AU Vollrath, A
Zucca, F
Bekaert, D
Bonforte, A
Guglielmino, F
Hooper, AJ
Stramondo, S
AF Vollrath, Andreas
Zucca, Francesco
Bekaert, David
Bonforte, Alessandro
Guglielmino, Francesco
Hooper, Andrew J.
Stramondo, Salvatore
TI Decomposing DInSAR Time-Series into 3-D in Combination with GPS in the
Case of Low Strain Rates: An Application to the Hyblean Plateau, Sicily,
Italy
SO REMOTE SENSING
LA English
DT Article
DE DInSAR time-series; StaMPS; TRAIN; SISTEM; tropospheric correction; GPS;
joint inversion; neotectonics
ID SURFACE DEFORMATION; SAR-INTERFEROMETRY; ATMOSPHERIC DELAY; 1693
EARTHQUAKE; C-BAND; INSAR; SUBSIDENCE; EASTERN; FAULT; FIELD
AB Differential Interferometric SAR (DInSAR) time-series techniques can be used to derive surface displacement rates with accuracies of 1 mm/year, by measuring the one-dimensional distance change between a satellite and the surface over time. However, the slanted direction of the measurements complicates interpretation of the signal, especially in regions that are subject to multiple deformation processes. The Simultaneous and Integrated Strain Tensor Estimation from Geodetic and Satellite Deformation Measurements (SISTEM) algorithm enables decomposition into a three-dimensional velocity field through joint inversion with GNSS measurements, but has never been applied to interseismic deformation where strain rates are low. Here, we apply SISTEM for the first time to detect tectonic deformation on the Hyblean Foreland Plateau in South-East Sicily. In order to increase the signal-to-noise ratio of the DInSAR data beforehand, we reduce atmospheric InSAR noise using a weather model and combine it with a multi-directional spatial filtering technique. The resultant three-dimensional velocity field allows identification of anthropogenic, as well as tectonic deformation, with sub-centimeter accuracies in areas of sufficient GPS coverage. Our enhanced method allows for a more detailed view of ongoing deformation processes as compared to the single use of either GNSS or DInSAR only and thus is suited to improve assessments of regional seismic hazard.
C1 [Vollrath, Andreas; Zucca, Francesco] Univ Pavia, Dept Earth & Environm Sci, Via Ferrata 1, I-27100 Pavia, Italy.
[Bekaert, David] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Bekaert, David; Hooper, Andrew J.] Univ Leeds, Sch Earth & Environm, COMET, Leeds LS2 9JT, W Yorkshire, England.
[Bonforte, Alessandro; Guglielmino, Francesco] INGV, Sez Catania, Osservatorio Etneo, Piazza Roma 2, I-95125 Catania, Italy.
[Stramondo, Salvatore] INGV, Via Vigna Murata 605, I-00143 Rome, Italy.
RP Vollrath, A (reprint author), Univ Pavia, Dept Earth & Environm Sci, Via Ferrata 1, I-27100 Pavia, Italy.
EM andreas.vollrath01@universitadipavia.it; francesco.zucca@unipv.it;
david.bekaert@jpl.nasa.gov; alessandro.bonforte@ingv.it;
francesco.guglielmino@ingv.it; a.hooper@leeds.ac.uk;
salvatore.stramondo@ingv.it
OI Bekaert, David/0000-0002-0408-0488
FU Ministry of Education, Universities and Research (MIUR), University of
Pavia, Italy; European Space Agency [13948]
FX This research was funded by the Ministry of Education, Universities and
Research (MIUR), University of Pavia, Italy. The work was conducted at
the INGV in Rome and Catania as well as the COMET School of Environment,
Leeds. Part of this work was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration. COMET is the NERC
Centre for the Observation and Modelling of Earthquakes, Volcanoes and
Tectonics. Fruitful discussions and valuable input was given by
Carlo-Alberto Brunori (INGV Roma), Guido Ventura (INGV Roma), Fabiano
Costantini (Univ. di Tor Vergata/ESA), Christian Bignami (INGV Roma),
Pablo J. Gonzalez (Univ. of Liverpool) and Karsten Spaans (COMET).
Additionally the authors want to acknowledge the European Space Agency
for the kind provision of ENVISAT data under the project ID 13948 and
INGV, who provided the GPS time-series data.
NR 98
TC 0
Z9 0
U1 0
U2 0
PU MDPI AG
PI BASEL
PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD JAN
PY 2017
VL 9
IS 1
AR 33
DI 10.3390/rs9010033
PG 22
WC Remote Sensing
SC Remote Sensing
GA EM7LN
UT WOS:000395492600033
ER
PT J
AU Jin, SY
Xu, HF
AF Jin, Shiyun
Xu, Huifang
TI Solved: The enigma of labradorite feldspar with incommensurately
modulated structure
SO AMERICAN MINERALOGIST
LA English
DT Article
DE Intermediate plagioclase; incommensurate; modulated structure; density
modulation; single-crystal XRD; e-plagioclase; labradorite; aperiodic
crystal; Invited Centennial article
ID INTERMEDIATE PLAGIOCLASE FELDSPAR; INITIO STRUCTURE SOLUTION;
ELECTRON-MICROSCOPY; CALCIC PLAGIOCLASE; LOW-TEMPERATURE;
SOLID-SOLUTION; DIFFRACTION; ANORTHITE; DISORDER; ORDER
AB Intermediate plagioclase feldspars are the most abundant minerals in the Earth's crust. Their incommensurately modulated structure has puzzled geologists and crystallographers for decades since the phenomenon in a labradorite was reported in 1940. Solving the structure is a necessary step toward mapping the complex subsolidus phase relations of plagioclase solid solution. The structure of a homogeneous labradorite (An(51)) single crystal from a metamorphic rock is solved and refined from single-crystal X-ray diffraction. The result structure can be simplified as alternating I1-like lamellae domains related by inversion twins. The inversion boundary shows an anorthite-like structure with I (1) over bar symmetry and is richer in Ca than the neighboring domains with opposite polarity. No albite-like subunits appear in the e-plagioclase structure. The modulated structure displays a unique Al-Si ordering pattern. A density modulation with a variation of 17 mol% in composition is also observed and can be properly described only by applying second-order harmonic waves for the atomic modulation functions. The modulated structure reveals details that cannot be observed from refinement with only main reflections and may be used to assess the ordering state and cooling rate of its host rock. The homogeneity of the crystal indicates the closure of the solvus for Boggild intergrowth at low temperature. The highly ordered modulation supports the thermodynamic stability of e-plagioclase. Both Al-Si ordering and Ca-Na ordering are the driving force for formation of the incommensurately modulated structure.
C1 [Jin, Shiyun; Xu, Huifang] Univ Wisconsin, NASA, Astrobiol Inst, Dept Geosci, Madison, WI 53706 USA.
RP Xu, HF (reprint author), Univ Wisconsin, NASA, Astrobiol Inst, Dept Geosci, Madison, WI 53706 USA.
EM hfxu@geology.wisc.edu
FU NSF [EAR-0810150]; NASA Astrobiology Institute [N07-5489]
FX This study was supported by NSF (EAR-0810150) and the NASA Astrobiology
Institute (N07-5489). The authors thank John Ferry for providing us the
sample, and Franklin Hobbs for reading the manuscript and providing many
helpful suggestions. The authors thank Ross Angel for insightful
discussions.
NR 59
TC 1
Z9 1
U1 0
U2 0
PU MINERALOGICAL SOC AMER
PI CHANTILLY
PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA
SN 0003-004X
EI 1945-3027
J9 AM MINERAL
JI Am. Miner.
PD JAN-FEB
PY 2017
VL 102
IS 1-2
BP 21
EP 32
DI 10.2138/am-2017-5807
PG 12
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA EL1TV
UT WOS:000394405000004
ER
PT J
AU Hadnott, BA
Ehlmann, BL
Jolliff, BL
AF Hadnott, Bryne A.
Ehlmann, Bethany L.
Jolliff, Bradley L.
TI Mineralogy and chemistry of San Carlos high-alkali basalts: Analyses of
alteration with application for Mars explorations
SO AMERICAN MINERALOGIST
LA English
DT Article
DE VSWIR spectroscopy; Mars analogs; XRD; geochemistry; alkali basalts; San
Carlos
ID CHEMCAM INSTRUMENT SUITE; GALE CRATER EVIDENCE; YELLOWKNIFE BAY; ROCKS;
WATER; ROVER; DIVERSITY; HISTORY; ANALOG; CRUST
AB The discovery of Fe, Mg, and Al phyllosilicates on Mars using visible and short-wave infrared (VSWIR) spectroscopy from orbit indicates aqueous alteration of basaltic rocks. Analyses at Gusev Crater by the Spirit rover and Gale Crater by the Curiosity rover have discovered alkaline basaltic rocks. In this work, multiple methods VSWIR spectroscopy, X-ray diffraction (XRD), and chemical analyses were used to study a suite of alkaline basalts from San Carlos, Arizona, which have been altered by water in an oxidative, semi-arid environment. As an analog for the weathering of alkaline basaltic rocks on Mars, a suite of rocks visually identified to have different degrees of alteration were characterized to understand the spectral, mineralogical, and chemical trends in alteration as sensed by multiple techniques. Samples with strong 1.9.mu m H2O-related absorptions in VSWIR commonly exhibited absorption bands at 1.4, 2.2, and/or 2.31 mu m, indicating the presence of clay minerals or silica as well as features at 0.5-0.9 mu m indicative of ferric iron oxides. Primary mineralogy for all samples, as determined by point analyses with the microprobe and XRD, consisted of olivine, plagioclase, nepheline, augite, and titanomagnetite. Compositional imaging and spot analyses with the microprobe revealed distinct alteration textures and phases, suggesting weathering pathways involving the oxidation of iron in olivine and primary Fe2+ oxides to form Fe3+ oxides as well as the formation of aluminum phyllosilicates and magnesium phyllosilicates from feldspars and olivines, respectively, while pyroxene remained relatively unaltered. Bivariate plots of major oxides both from bulk-chemical analysis and microprobe measurements also revealed trends in alkali and silica depletion and calcium enrichment, but there was little chemical fractionation in most of the major oxides. The strength of the 1.9 mu m H2O absorption, loss on ignition, and depletion in silica and sodium, correlated with increasing alteration. The data sets provide an analog for understanding possible weathering pathways in martian alkaline basalts and thresholds for the detection of aqueous alteration in multiple data sets.
C1 [Hadnott, Bryne A.; Jolliff, Bradley L.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63105 USA.
[Hadnott, Bryne A.; Ehlmann, Bethany L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Ehlmann, Bethany L.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Hadnott, Bryne A.] Cornell Univ, Dept Earth & Atmospher Sci, Room 414 Spaces Sci Bldg,122 Garden Ave, Ithaca, NY 14853 USA.
RP Hadnott, BA (reprint author), Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63105 USA.; Hadnott, BA (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.; Hadnott, BA (reprint author), Cornell Univ, Dept Earth & Atmospher Sci, Room 414 Spaces Sci Bldg,122 Garden Ave, Ithaca, NY 14853 USA.
EM bah248@cornell.edu
FU MSL Participating Scientist grant; Caltech Summer Undergraduate Research
Fellowship; National Science Foundation [NSF EAR-1161543]
FX Many thanks to Raymond Arvidson for guidance and Paul Carpenter for
invaluable/help using the electron microprobe and X-ray diffractometer.
This work was partially funded by an MSL Participating Scientist grant
to Bethany Ehlmann and the Caltech Summer Undergraduate Research
Fellowship provided programmatic support to Bryne Hadnott. Use of the
Bruker d8 Advance X-ray diffractometer in Earth and Planetary Sciences
at Washington University in St. Louis was supported by the National
Science Foundation, award no. NSF EAR-1161543.
NR 62
TC 0
Z9 0
U1 1
U2 1
PU MINERALOGICAL SOC AMER
PI CHANTILLY
PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA
SN 0003-004X
EI 1945-3027
J9 AM MINERAL
JI Am. Miner.
PD JAN-FEB
PY 2017
VL 102
IS 1-2
BP 284
EP 301
DI 10.2138/am-2017-5608
PG 18
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA EL1TV
UT WOS:000394405000030
ER
PT J
AU Rubin, DM
Fairen, AG
Martinez-Frias, J
Frydenvang, J
Gasnault, O
Gelfenbaum, G
Goetz, W
Grotzinger, JP
Le Mouelic, S
Mangold, N
Newsom, H
Oehler, DZ
Rapin, W
Schieber, J
Wiens, RC
AF Rubin, David M.
Fairen, A. G.
Martinez-Frias, J.
Frydenvang, J.
Gasnault, O.
Gelfenbaum, G.
Goetz, W.
Grotzinger, J. P.
Le Mouelic, S.
Mangold, N.
Newsom, H.
Oehler, D. Z.
Rapin, W.
Schieber, J.
Wiens, R. C.
TI Fluidized-sediment pipes in Gale crater, Mars, and possible Earth
analogs
SO GEOLOGY
LA English
DT Article
ID CHEMCAM INSTRUMENT SUITE; ARABIA TERRA; DEPOSITS; SYSTEM; CANDOR; WATER;
UNIT
AB Since landing in Gale crater, the Mars Science Laboratory rover Curiosity has traversed fluvial, lacustrine, and eolian sedimentary rocks that were deposited within the crater similar to 3.6 to 3.2 b.y. ago. Here we describe structures interpreted to be pipes formed by vertical movement of fluidized sediment. Like many pipes on Earth, those in Gale crater are more resistant to erosion than the host rock; they form near other pipes, dikes, or deformed sediment; and some contain internal concentric or eccentric layering. These structures provide new evidence of the importance of subsurface aqueous processes in shaping the near-surface geology of Mars.
C1 [Rubin, David M.] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA.
[Fairen, A. G.] CSIC, Inst Nacl Tecn Aeroespacial, Ctr Astrobiol, Torrejon De Ardoz 28850, Spain.
[Fairen, A. G.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Martinez-Frias, J.] Univ Complutense Madrid, CSIC, Inst Geociencias IGEO, E-28040 Madrid, Spain.
[Frydenvang, J.; Rapin, W.; Wiens, R. C.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Gasnault, O.] Inst Rech Astrophys & Planetol, F-31400 Toulouse, France.
[Gelfenbaum, G.] US Geol Survey, Pacific Coastal & Marine Sci Ctr, Santa Cruz, CA 95060 USA.
[Goetz, W.] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany.
[Grotzinger, J. P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Le Mouelic, S.; Mangold, N.] Univ Nantes, CNRS UMR6112, Lab Planetol & Geodynam Nantes, F-44322 Nantes 3, France.
[Newsom, H.] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA.
[Oehler, D. Z.] NASA, LZ Technol, Johnson Space Ctr, Houston, TX 77058 USA.
[Schieber, J.] Indiana Univ, Dept Geol Sci, Bloomington, IN 47408 USA.
RP Rubin, DM (reprint author), Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA.
FU NASA Mars Exploration Program; NASA MSL Participating Scientist Program;
Project icyMARS, European Research Council [307496]
FX This work could not have been completed without the NASA Mars Science
Laboratory (MSL) engineering, management, and operations teams,
supported by the NASA Mars Exploration Program. Support for Rubin,
Goetz, and Oehler was provided by the NASA MSL Participating Scientist
Program. Fairen was supported by the Project icyMARS, European Research
Council Starting grant 307496. We thank Margie Chan, Andrew Hurst, David
Loope, Massimo Moretti, Jeff Peakall, and James Schmitt for constructive
reviews.
NR 36
TC 0
Z9 0
U1 1
U2 1
PU GEOLOGICAL SOC AMER, INC
PI BOULDER
PA PO BOX 9140, BOULDER, CO 80301-9140 USA
SN 0091-7613
EI 1943-2682
J9 GEOLOGY
JI Geology
PD JAN
PY 2017
VL 45
IS 1
BP 7
EP 10
DI 10.1130/G38339.1
PG 4
WC Geology
SC Geology
GA EN6OT
UT WOS:000396124000004
ER
PT J
AU Tang, A
Kim, Y
Xu, YN
Virbila, G
Reck, T
Chang, MCF
AF Tang, Adrian
Kim, Yanghyo
Xu, Yinuo
Virbila, Gabriel
Reck, Theodore
Chang, M-C Frank
TI Evaluation of 28 nm CMOS Receivers at 183 GHz for Space-borne
Atmospheric Remote Sensing
SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS
LA English
DT Article
DE 183 GHz Radiometer Receiver; 28 nm CMOS
ID WATER-VAPOR; STATION
AB This letter discusses the capability of 28 nm CMOS technology to implement receivers at the 183 GHz band enabling the potential of future radiometers for monitoring atmospheric water vapor. To demonstrate the potential of 28 nm for constructing receivers at these frequencies, a prototype LNA and downconverter chip is demonstrated and measurements of both gain and noise performance are presented. The prototype receiver consumes 191 mW of DC power while providing noise temperatures on the order of 2700 K which demonstrates the potential for use in payload restricted cubesats and other small spacecraft platforms.
C1 [Tang, Adrian; Kim, Yanghyo; Xu, Yinuo; Virbila, Gabriel; Chang, M-C Frank] Univ Calif Los Angeles, High Speed Elect Lab, Los Angeles, CA 90095 USA.
[Tang, Adrian; Reck, Theodore] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Tang, A (reprint author), Univ Calif Los Angeles, High Speed Elect Lab, Los Angeles, CA 90095 USA.; Tang, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 9
TC 0
Z9 0
U1 1
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1531-1309
EI 1558-1764
J9 IEEE MICROW WIREL CO
JI IEEE Microw. Wirel. Compon. Lett.
PD JAN
PY 2017
VL 27
IS 1
BP 100
EP 102
DI 10.1109/LMWC.2016.2630002
PG 3
WC Engineering, Electrical & Electronic
SC Engineering
GA EK2ZI
UT WOS:000393795300034
ER
PT J
AU Ladbury, RL
Lauenstein, JM
AF Ladbury, R. L.
Lauenstein, J. -M.
TI Evaluating Constraints on Heavy-Ion SEE Susceptibility Imposed by Proton
SEE Testing and Other Mixed Environments
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article; Proceedings Paper
CT 53rd IEEE Nuclear and Space Radiation Effects Conference (NSREC)
CY JUL 11-15, 2016
CL Portland, OR
SP IEEE, IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm
DE Heavy Ions; probabilistic risk assessment; proton radiation effects;
radiation hardness assurance methodology; single-event effects;
single-event latchup
ID RISK-ASSESSMENT; EVENT; MICROELECTRONICS; SPECTRA; MODEL
AB We develop metrics for assessing effectiveness of proton SEE data for bounding heavy-ion SEE susceptibility. The simplest metric is just the areal coverage for the test, which can be expressed as the area on the test part which is struck on average by a single ion. This simple quantity can yield important insights into the efficacy of a given SEE test. We also develop methods for bounding heavy-ion SEE rates with proton data for both nondestructive and destructive SEE modes and for identifying the SEE response characteristics that render such bounding methods ineffective.
C1 [Ladbury, R. L.; Lauenstein, J. -M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Ladbury, RL (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Raymond.L.Ladbury@nasa.gov; jean.m.lauenstein@nasa.gov
FU NASA program; NASA Engineering and Safety Center
FX This research was supported by the NASA program and the NASA Engineering
and Safety Center.
NR 13
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PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
EI 1558-1578
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD JAN
PY 2017
VL 64
IS 1
BP 301
EP 308
DI 10.1109/TNS.2016.2640948
PN 1
PG 8
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA EO0RB
UT WOS:000396404500044
ER
PT J
AU George, JS
Clymer, DA
Turflinger, TL
Mason, LW
Stone, S
Koga, R
Beach, E
Huntington, K
Lauenstein, JM
Titus, J
Sivertz, M
AF George, J. S.
Clymer, D. A.
Turflinger, T. L.
Mason, L. W.
Stone, S.
Koga, R.
Beach, E.
Huntington, K.
Lauenstein, J. -M.
Titus, J.
Sivertz, M.
TI Response Variability in Commercial MOSFET SEE Qualification
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article; Proceedings Paper
CT 53rd IEEE Nuclear and Space Radiation Effects Conference (NSREC)
CY JUL 11-15, 2016
CL Portland, OR
SP IEEE, IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm
DE Failure distribution; MOSFET; single-event burnout; trench
ID POWER MOSFETS; BURNOUT; IRRADIATION; DEGRADATION; HARDNESS; PROTON;
SPACE
AB Single-event effects (SEE) evaluation of five different part types of next generation, commercial trench MOSFETs indicates large part-to-part variation in determining a safe operating area (SOA) for drain-source voltage (VDS) following a test campaign that exposed >50 samples per part type to heavy ions. These results suggest a determination of a SOA using small sample sizes may fail to capture the full extent of the part-to-part variability. An example method is discussed for establishing a Safe Operating Area using a one-sided statistical tolerance limit based on the number of test samples. Burn-in is shown to be a critical factor in reducing part-to-part variation in part response. Implications for radiation qualification requirements are also explored.
C1 [George, J. S.; Turflinger, T. L.; Koga, R.] Aerosp Corp, El Segundo, CA 90245 USA.
[Clymer, D. A.; Mason, L. W.; Stone, S.; Beach, E.; Huntington, K.] Lockheed Martin Corp, Littleton, CO 80125 USA.
[Lauenstein, J. -M.] NASA GSFC, Greenbelt, MD 20771 USA.
[Titus, J.] NAVSEA Crane, Crane, IN 47522 USA.
[Sivertz, M.] Brookhaven Natl Lab, NASA Space Radiat Lab, Upton, NY 11973 USA.
RP George, JS (reprint author), Aerosp Corp, El Segundo, CA 90245 USA.
EM Jeffrey.S.George@aero.org
NR 22
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PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
EI 1558-1578
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD JAN
PY 2017
VL 64
IS 1
BP 317
EP 324
DI 10.1109/TNS.2016.2633358
PN 1
PG 8
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA EO0RB
UT WOS:000396404500046
ER
PT J
AU Xapsos, MA
Stauffer, C
Phan, A
McClure, SS
Ladbury, RL
Pellish, JA
Campola, MJ
LaBel, KA
AF Xapsos, M. A.
Stauffer, C.
Phan, A.
McClure, S. S.
Ladbury, R. L.
Pellish, J. A.
Campola, M. J.
LaBel, K. A.
TI Inclusion of Radiation Environment Variability in Total Dose Hardness
Assurance Methodology
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article; Proceedings Paper
CT 53rd IEEE Nuclear and Space Radiation Effects Conference (NSREC)
CY JUL 11-15, 2016
CL Portland, OR
SP IEEE, IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm
DE Displacement damage dose; radiation design margin; radiation hardness
assurance; total ionizing dose
ID MODEL
AB Variability of the space radiation environment is investigated with regard to parts categorization for total dose hardness assurance methods. It is shown that it can have a significant impact. A modified approach is developed that uses current environment models more consistently and replaces the radiation design margin concept with one of failure probability during a mission.
C1 [Xapsos, M. A.; Ladbury, R. L.; Pellish, J. A.; Campola, M. J.; LaBel, K. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Stauffer, C.; Phan, A.] AS&D Inc, Greenbelt, MD 20771 USA.
[McClure, S. S.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
RP Xapsos, MA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Michael.A.Xapsos@nasa.gov
FU NASA Living With a Star Space Environment Testbed Program
FX This work was supported by the NASA Living With a Star Space Environment
Testbed Program.
NR 17
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PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
EI 1558-1578
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD JAN
PY 2017
VL 64
IS 1
BP 325
EP 331
DI 10.1109/TNS.2016.2607021
PN 1
PG 7
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA EO0RB
UT WOS:000396404500047
ER
PT J
AU Chen, DK
Wilcox, E
Ladbury, RL
Kim, H
Phan, A
Seidleck, C
Label, K
AF Chen, Dakai
Wilcox, Edward
Ladbury, Raymond L.
Kim, Hak
Phan, Anthony
Seidleck, Christina
Label, Kenneth
TI Heavy Ion Irradiation Fluence Dependence for Single-Event Upsets in a
NAND Flash Memory
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article; Proceedings Paper
CT 53rd IEEE Nuclear and Space Radiation Effects Conference (NSREC)
CY JUL 11-15, 2016
CL Portland, OR
SP IEEE, IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm
DE Flash memories; heavy ion testing; single-event effect; standards;
testing guidelines; testing techniques
ID CROSS-SECTION; CELLS
AB We investigated the single-event effect (SEE) susceptibility of the Micron 16 nm NAND flash, and found that the single-event upset (SEU) cross section varied inversely with cumulative fluence. We attribute the effect to the variable upset sensitivities of the memory cells. Furthermore, the effect impacts only single cell upsets in general. The rate of multiple-bit upsets remained relatively constant with fluence. The current test standards and procedures assume that SEU follow a Poisson process and do not take into account the variability in the error rate with fluence. Therefore, traditional SEE testing techniques may underestimate the on-orbit event rate for a device with variable upset sensitivity.
C1 [Chen, Dakai; Ladbury, Raymond L.; Label, Kenneth] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wilcox, Edward; Kim, Hak; Phan, Anthony; Seidleck, Christina] NASA, Goddard Space Flight Ctr, ASRC Space & Def Inc, Greenbelt, MD 20771 USA.
RP Chen, DK (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM dakai.chen-1@nasa.gov; ted.wilcox@nasa.gov
FU NASA Electronics Parts and Packaging Program (NEPP)
FX This work was supported by the NASA Electronics Parts and Packaging
Program (NEPP).
NR 20
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PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
EI 1558-1578
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD JAN
PY 2017
VL 64
IS 1
BP 332
EP 337
DI 10.1109/TNS.2016.2615719
PN 1
PG 6
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA EO0RB
UT WOS:000396404500048
ER
PT J
AU Javanainen, A
Galloway, KF
Nicklaw, C
Bosser, AL
Ferlet-Cavrois, V
Lauenstein, JM
Pintacuda, F
Reed, RA
Schrimpf, RD
Weller, RA
Virtanen, A
AF Javanainen, Arto
Galloway, Kenneth F.
Nicklaw, Christopher
Bosser, Alexandre L.
Ferlet-Cavrois, Veronique
Lauenstein, Jean-Marie
Pintacuda, Francesco
Reed, Robert A.
Schrimpf, Ronald D.
Weller, Robert A.
Virtanen, A.
TI Heavy Ion Induced Degradation in SiC Schottky Diodes: Bias and Energy
Deposition Dependence
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article; Proceedings Paper
CT 53rd IEEE Nuclear and Space Radiation Effects Conference (NSREC)
CY JUL 11-15, 2016
CL Portland, OR
SP IEEE, IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm
DE Current-voltage characteristics; ion radiation effects; modeling; power
semiconductor devices; Schottky diodes; silicon carbide
ID IMPACT IONIZATION COEFFICIENTS; SINGLE-EVENT BURNOUT; SILICON-CARBIDE;
BARRIER DIODES; THERMAL-DAMAGE; SIMULATION
AB Experimental results on ion-induced leakage current increase in 4H-SiC Schottky power diodes are presented. Monte Carlo and TCAD simulations show that degradation is due to the synergy between applied bias and ion energy deposition. This degradation is possibly related to thermal spot annealing at the metal semiconductor interface. This thermal annealing leads to an inhomogeneity of the Schottky barrier that could be responsible for the increase leakage current as a function of fluence.
C1 [Javanainen, Arto; Bosser, Alexandre L.; Virtanen, A.] Univ Jyvaskyla, Dept Phys, FI-40014 Jyvaskyla, Finland.
[Javanainen, Arto; Galloway, Kenneth F.; Reed, Robert A.; Schrimpf, Ronald D.; Weller, Robert A.] Vanderbilt Univ, Elect Engn & Comp Sci Dept, 221 Kirkland Hall, Nashville, TN 37235 USA.
[Nicklaw, Christopher] Silvaco Inc, Santa Clara, CA 95054 USA.
[Ferlet-Cavrois, Veronique] European Space Agcy, NL-2200 AG Noordwijk, Netherlands.
[Lauenstein, Jean-Marie] NASA, GSFC, Code 561-4, Greenbelt, MD 20771 USA.
[Pintacuda, Francesco] STMicroelectron Srl, I-95121 Catania, Italy.
RP Javanainen, A (reprint author), Univ Jyvaskyla, Dept Phys, FI-40014 Jyvaskyla, Finland.
EM arto.javanainen@jyu.fi; kenneth.f.galloway@vanderbilt.edu;
chris.nicklaw@silvaco.com; alexander.l.bosser@jyu.fi;
veronique.ferlet-cavrois@esa.int; jean.m.lauenstein@nasa.gov;
francesco.pintacuda@st.com; robert.reed@vanderbilt.edu;
ron.schrimpf@vanderbilt.edu; robert.a.weller@vanderbilt.edu;
ari.j.virtanen@jyu.fi
FU Walter Ahlstrom Foundation through the Tutkijat Maailmalle program;
European Space Agency (ESA/ESTEC) [4000111630/14/NL/PA]; Academy of
Finland under the Finnish Centre of Excellence Programme [2513553]
FX This work was supported by the Walter Ahlstrom Foundation through the
Tutkijat Maailmalle program, the European Space Agency (ESA/ESTEC
Contract 4000111630/14/NL/PA), and the Academy of Finland under the
Finnish Centre of Excellence Programme 2012-2017 (Project No 2513553,
Nuclear and Accelerator Based Physics).
NR 23
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PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
EI 1558-1578
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD JAN
PY 2017
VL 64
IS 1
BP 415
EP 420
DI 10.1109/TNS.2016.2616921
PN 1
PG 6
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA EO0RB
UT WOS:000396404500059
ER
PT J
AU Zeinolabedinzadeh, S
Ulusoy, AC
Inanlou, F
Ying, HB
Gong, YY
Fleetwood, ZE
Roche, NJH
Khachatrian, A
McMorrow, D
Buchner, SP
Warner, JH
Paki-Amouzou, P
Cressler, JD
AF Zeinolabedinzadeh, Saeed
Ulusoy, Ahmet C.
Inanlou, Farzad
Ying, Hanbin
Gong, Yunyi
Fleetwood, Zachary E.
Roche, Nicolas J. -H.
Khachatrian, Ani
McMorrow, Dale
Buchner, Stephen P.
Warner, Jeffrey H.
Paki-Amouzou, Pauline
Cressler, John D.
TI Single-Event Effects in a Millimeter-Wave Receiver Front-End Implemented
in 90 nm, 300 GHz SiGe HBT Technology
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article; Proceedings Paper
CT 53rd IEEE Nuclear and Space Radiation Effects Conference (NSREC)
CY JUL 11-15, 2016
CL Portland, OR
SP IEEE, IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm
DE Cubesat; extreme environments; millimeterwave; radar; radiometer;
receiver; SiGe; silicon-germanium; single-event transient; space
missions; two-photon absorption laser; W-band
ID 2-PHOTON ABSORPTION; ION MICROBEAM; LASER-LIGHT; BROAD-BEAM; TRANSIENTS;
RF; CIRCUITS; GENERATION; METHODOLOGY; ELECTRONICS
AB The single-event transient (SET) response of a W-band (75-110 GHz) radar receiver front-end is investigated in this paper. A new technique to facilitate the SET testing of the high frequency transceivers is proposed and demonstrated experimentally. The entire radar receiver front-end, including the high frequency signal sources and modulators, were designed and fully integrated in 90 nm 300 GHz SiGe process technology (Global Foundries SiGe 9HP). Two-photon absorption (TPA) laser pulses were utilized to induce transient currents in different devices in various circuit blocks. The study shows how short transient pulses from the high frequency tuned circuits are propagated throughout the receiver and are broadened while passing through low-pass filters present at supply nodes and the low-pass filter following the down-conversion mixer, thus affecting the digital data at the output of the receiver. The proposed methodology allows the study of the effect of SETs on the recovered digital data at the output of the high frequency receivers, thus allowing bit error rate calculations. Comprehensive device and circuit level simulations were also performed, and a close agreement between the measurement results and simulation data was demonstrated. To the authors' best knowledge, this is the first study of SET on full receiver at millimeter-wave (mmW) frequencies.
C1 [Zeinolabedinzadeh, Saeed; Ying, Hanbin; Gong, Yunyi; Fleetwood, Zachary E.; Cressler, John D.] Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA.
[Ulusoy, Ahmet C.] Michigan State Univ, E Lansing, MI 48824 USA.
[Inanlou, Farzad] JPL, Pasadena, CA 91109 USA.
[Roche, Nicolas J. -H.] George Washington Univ, Washington, DC 20052 USA.
[Roche, Nicolas J. -H.; Khachatrian, Ani; McMorrow, Dale; Buchner, Stephen P.; Warner, Jeffrey H.] Naval Res Lab, Washington, DC 20375 USA.
[Khachatrian, Ani] Sotera Def, Annapolis Jct, MD 20701 USA.
[Paki-Amouzou, Pauline] Def Threat Reduct Agcy, Ft Belvoir, VA 22060 USA.
RP Zeinolabedinzadeh, S (reprint author), Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA.
EM namarvar3@mail.gatech.edu
FU Defense Threat Reduction Agency [HDTRA1-13-C-0058]; Global Foundries
FX This work was supported in part by the Defense Threat Reduction Agency
under contract HDTRA1-13-C-0058, and Global Foundries.
NR 31
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U1 0
U2 0
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
EI 1558-1578
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD JAN
PY 2017
VL 64
IS 1
BP 536
EP 543
DI 10.1109/TNS.2016.2638698
PN 1
PG 8
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA EO0RB
UT WOS:000396404500076
ER
PT J
AU Hands, A
Lei, F
Ryden, K
Dyer, C
Underwood, C
Mertens, C
AF Hands, Alex
Lei, Fan
Ryden, Keith
Dyer, Clive
Underwood, Craig
Mertens, Chris
TI New Data and Modelling for Single Event Effects in the Stratospheric
Radiation Environment
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article; Proceedings Paper
CT 53rd IEEE Nuclear and Space Radiation Effects Conference (NSREC)
CY JUL 11-15, 2016
CL Portland, OR
SP IEEE, IEEE Nucl & Plasma Sci Soc, Radiat Effects Comm
DE High altitude radiation environment; single event effects; stratosphere
ID SEU RATES; ATMOSPHERE; BALLOON; UPSETS; NM
AB The upper atmosphere is a transition region between the neutron-dominated aviation environment and satellite environment where primary protons and ions dominate. We report high altitude balloon measurements and model results characterising this radiation environment for single event effects (SEE) in avionics. Our data, from the RaySure solid-state radiation monitor, reveal markedly different altitude profiles for low linear energy transfer (LET) and high LET energy depositions. We use models to show that the difference is caused by the influence of primary cosmic ray particles, which induce counts in RaySure via both direct and indirect ionization. Using the new Model of Atmospheric Ionizing Radiation Effects (MAIRE), we use particle fluxes and LET spectra to calculate single event upset (SEU) rates as a function of altitude from ground level to the edge of space at 100 km altitude. The results have implications for a variety of applications including high altitude space tourism flights, UAVs and missions to the Martian surface.
C1 [Hands, Alex; Ryden, Keith; Underwood, Craig] Univ Surrey, Surrey Space Ctr, Guildford GU2 7JP, Surrey, England.
[Lei, Fan] RadMod Res, Surrey GU15 2PD, England.
[Dyer, Clive] Surrey Space Ctr, Surrey GU2 7JP, England.
[Dyer, Clive] CSDRadConsultancy, Surrey GU2 7JP, England.
[Mertens, Chris] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Hands, A (reprint author), Univ Surrey, Surrey Space Ctr, Guildford GU2 7JP, Surrey, England.
FU NASA Science Mission Directorate under the Hands-On Project Experience
(HOPE)-4 opportunity
FX This work was supported by the NASA Science Mission Directorate under
the Hands-On Project Experience (HOPE)-4 opportunity.
NR 26
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U1 1
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
EI 1558-1578
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD JAN
PY 2017
VL 64
IS 1
BP 587
EP 595
DI 10.1109/TNS.2016.2612000
PN 1
PG 9
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA EO0RB
UT WOS:000396404500083
ER
PT J
AU Shi, SC
Mehdi, I
AF Shi, Sheng-Cai
Mehdi, Imran
TI Guest Editorial Mini-Special Issue on the 27th International Symposium
on Space Terahertz Technology
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Editorial Material
C1 [Shi, Sheng-Cai] Purple Mt Observ, Millimeter & Submillimeter Wave Lab, Nanjing, Jiangsu, Peoples R China.
[Mehdi, Imran] Jet Prop Lab, Instrument Elect & Sensors Sect, Pasadena, CA 91109 USA.
RP Shi, SC (reprint author), Purple Mt Observ, Millimeter & Submillimeter Wave Lab, Nanjing, Jiangsu, Peoples R China.
NR 0
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U1 1
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD JAN
PY 2017
VL 7
IS 1
BP 1
EP 1
DI 10.1109/TTHZ.2016.2636058
PG 1
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA EO0LH
UT WOS:000396388800001
ER
PT J
AU Rice, MS
Gupta, S
Treiman, AH
Stack, KM
Calef, F
Edgar, LA
Grotzinger, J
Lanza, N
Le Deit, L
Lasue, J
Siebach, KL
Vasavada, A
Wiens, RC
Williams, J
AF Rice, Melissa S.
Gupta, Sanjeev
Treiman, Allan H.
Stack, Kathryn M.
Calef, Fred
Edgar, Lauren A.
Grotzinger, John
Lanza, Nina
Le Deit, Laetitia
Lasue, Jeremie
Siebach, Kirsten L.
Vasavada, Ashwin
Wiens, Roger C.
Williams, Joshua
TI Geologic overview of the Mars Science Laboratory rover mission at the
Kimberley, Gale crater, Mars
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Mars Science Laboratory; Gale crater; sediment provenance; diagenesis;
fluvio-deltaic processes; landscape evolution
ID PEACE VALLIS FAN; IN-SITU; CONSTRAINTS; MINERALOGY; ROCKS; EVOLUTION;
ORIGIN; SPECTROSCOPY; SANDSTONE; DEPOSITS
AB The Mars Science Laboratory (MSL) Curiosity rover completed a detailed investigation at the Kimberley waypoint within Gale crater from sols 571-634 using its full science instrument payload. From orbital images examined early in the Curiosity mission, the Kimberley region had been identified as a high-priority science target based on its clear stratigraphic relationships in a layered sedimentary sequence that had been exposed by differential erosion. Observations of the stratigraphic sequence at the Kimberley made by Curiosity are consistent with deposition in a prograding, fluvio-deltaic system during the late Noachian to early Hesperian, prior to the existence of most of Mount Sharp. Geochemical and mineralogic analyses suggest that sediment deposition likely took place under cold conditions with relatively low water-to-rock ratios. Based on elevated K2O abundances throughout the Kimberley formation, an alkali feldspar protolith is likely one of several igneous sources from which the sediments were derived. After deposition, the rocks underwent multiple episodes of diagenetic alteration with different aqueous chemistries and redox conditions, as evidenced by the presence of Ca-sulfate veins, Mn-oxide fracture fills, and erosion-resistant nodules. More recently, the Kimberley has been subject to significant aeolian abrasion and removal of sediments to create modern topography that slopes away from Mount Sharp, a process that has continued to the present day.
C1 [Rice, Melissa S.; Williams, Joshua] Western Washington Univ, Dept Geol, Bellingham, WA 98225 USA.
[Gupta, Sanjeev] Imperial Coll London, Dept Earth Sci & Engn, London, England.
[Treiman, Allan H.] Lunar & Planetary Inst, 3303 NASA Rd 1, Houston, TX 77058 USA.
[Stack, Kathryn M.; Calef, Fred; Vasavada, Ashwin] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Edgar, Lauren A.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Grotzinger, John] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Lanza, Nina; Wiens, Roger C.] Los Alamos Natl Lab, Space Remote Sensing, Los Alamos, NM USA.
[Le Deit, Laetitia] Univ Nantes, Lab Planetol & Geodynam, Nantes, France.
[Lasue, Jeremie] CNRS, Inst Rech Astrophys & Planetol, Observ Midi Pyrenees, Toulouse, France.
[Siebach, Kirsten L.] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA.
RP Rice, MS (reprint author), Western Washington Univ, Dept Geol, Bellingham, WA 98225 USA.
EM melissa.rice@wwu.edu
FU NASA Astrobiology Institute (NAI) Postdoctoral Program; MSL
Participating Scientist Program; United Kingdom Space Agency (UKSA);
French Space Agency (CNES)
FX We acknowledge the exceptional skills and diligent efforts made by the
MSL project's science, engineering, and management teams in making this
work possible. We are also grateful to the many MSL team members who
participated in tactical and strategic operations during the Kimberley
campaign. We thank Ryan Anderson and two anonymous reviewers, whose
comments have improved the manuscript. Rice was supported by the NASA
Astrobiology Institute (NAI) Postdoctoral Program and the MSL
Participating Scientist Program. Gupta was supported by grants from the
United Kingdom Space Agency (UKSA). Le Deit and Lasue acknowledge the
support of the French Space Agency (CNES). Data presented in this paper
are archived in the Planetary Data System (pds.nasa.gov).
NR 64
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U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD JAN
PY 2017
VL 122
IS 1
BP 2
EP 20
DI 10.1002/2016JE005200
PG 19
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EM1QA
UT WOS:000395090900001
ER
PT J
AU Deming, LD
Seager, S
AF Deming, L. Drake
Seager, Sara
TI Illusion and reality in the atmospheres of exoplanets
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Review
DE exoplanets; atmospheric composition and structure; planetary atmospheres
ID SUPER-EARTH EXOPLANET; EXTRASOLAR GIANT PLANETS; TRANSMISSION SPECTRAL
SURVEY; WEBB-SPACE-TELESCOPE; HOT-JUPITER; HD 189733B; TAU-BOOTIS;
WATER-ABSORPTION; MU-M; TEMPERATURE INVERSION
AB The atmospheres of exoplanets reveal all their properties beyond mass, radius, and orbit. Based on bulk densities, we know that exoplanets larger than 1.5 Earth radii must have gaseous envelopes and, hence, atmospheres. We discuss contemporary techniques for characterization of exoplanetary atmospheres. The measurements are difficult, becauseeven in current favorable casesthe signals can be as small as 0.001% of the host star's flux. Consequently, some early results have been illusory and not confirmed by subsequent investigations. Prominent illusions to date include polarized scattered light, temperature inversions, and the existence of carbon planets. The field moves from the first tentative and often incorrect conclusions, converging to the reality of exoplanetary atmospheres. That reality is revealed using transits for close-in exoplanets and direct imaging for young or massive exoplanets in distant orbits. Several atomic and molecular constituents have now been robustly detected in exoplanets as small as Neptune. In our current observations, the effects of clouds and haze appear ubiquitous. Topics at the current frontier include the measurement of heavy element abundances in giant planets, detection of carbon-based molecules, measurement of atmospheric temperature profiles, definition of heat circulation efficiencies for tidally locked planets, and the push to detect and characterize the atmospheres of super-Earths. Future observatories for this quest include the James Webb Space Telescope and the new generation of extremely large telescopes on the ground. On a more distant horizon, NASA's study concepts for the Habitable Exoplanet Imaging Mission (HabEx) and the Large UV/Optical/Infrared Surveyor (LUVOIR) missions could extend the study of exoplanetary atmospheres to true twins of Earth.
C1 [Deming, L. Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Deming, L. Drake] NASA, Astrobiol Inst, Virtual Planetary Lab, Seattle, WA USA.
[Seager, Sara] MIT, Dept Earth & Planetary Sci, Cambridge, MA USA.
[Seager, Sara] MIT, Dept Phys, Cambridge, MA 02139 USA.
RP Deming, LD (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.; Deming, LD (reprint author), NASA, Astrobiol Inst, Virtual Planetary Lab, Seattle, WA USA.
EM ddeming@astro.umd.edu
NR 173
TC 1
Z9 1
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD JAN
PY 2017
VL 122
IS 1
BP 53
EP 75
DI 10.1002/2016JE005155
PG 23
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EM1QA
UT WOS:000395090900003
ER
PT J
AU Farrell, WM
Hurley, DM
Esposito, VJ
McLain, JL
Zimmerman, MI
AF Farrell, W. M.
Hurley, D. M.
Esposito, V. J.
McLain, J. L.
Zimmerman, M. I.
TI The statistical mechanics of solar wind hydroxylation at the Moon,
within lunar magnetic anomalies, and at Phobos
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Moon; Phobos; hydroxyl
ID TEMPERATURE-PROGRAMMED DESORPTION; WATER; IMPLANTATION; ADSORPTION;
SURFACE; SWIRLS; EJECTA
AB We present a new formalism to describe the outgassing of hydrogen initially implanted by the solar wind protons into exposed soils on airless bodies. The formalism applies a statistical mechanics approach similar to that applied recently to molecular adsorption onto activated surfaces. The key element enabling this formalism is the recognition that the interatomic potential between the implanted H and regolith-residing oxides is not of singular value but possess a distribution of trapped energy values at a given temperature, F(U,T). All subsequent derivations of the outward diffusion and H retention rely on the specific properties of this distribution. We find that solar wind hydrogen can be retained if there are sites in the implantation layer with activation energy values exceeding 0.5eV. We especially examine the dependence of H retention applying characteristic energy values found previously for irradiated silica and mature lunar samples. We also apply the formalism to two cases that differ from the typical solar wind implantation at the Moon. First, we test for a case of implantation in magnetic anomaly regions where significantly lower-energy ions of solar wind origin are expected to be incident with the surface. In magnetic anomalies, H retention is found to be reduced due to the reduced ion flux and shallower depth of implantation. Second, we also apply the model to Phobos where the surface temperature range is not as extreme as the Moon. We find the H atom retention in this second case is higher than the lunar case due to the reduced thermal extremes (that reduces outgassing).
C1 [Farrell, W. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hurley, D. M.; Zimmerman, M. I.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Esposito, V. J.] NASA, Goddard Space Flight Ctr, Goddard Summer Intern Program, Greenbelt, MD USA.
[McLain, J. L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Farrell, WM (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM william.m.farrell@nasa.gov
FU NASA's Solar System Exploration Research Virtual Institute
FX The authors gratefully acknowledge support from NASA's Solar System
Exploration Research Virtual Institute in completion of this work. The
analytical data in Figures 4, 5, 7, 8, 10, 11, and 13 are directly
reproducible via the equations in section 2. The supporting Monte Carlo
simulation results in Figures 9 and 10 are from a code that is available
from the lead author upon request.
NR 44
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U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD JAN
PY 2017
VL 122
IS 1
BP 269
EP 289
DI 10.1002/2016JE005168
PG 21
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EM1QA
UT WOS:000395090900014
ER
PT J
AU Huang, MH
Fielding, EJ
Dickinson, H
Sun, JB
Gonzalez-Ortega, JA
Freed, AM
Burgmann, R
AF Huang, Mong-Han
Fielding, Eric J.
Dickinson, Haylee
Sun, Jianbao
Gonzalez-Ortega, J. Alejandro
Freed, Andrew M.
Burgmann, Roland
TI Fault geometry inversion and slip distribution of the 2010 M-w 7.2 El
Mayor-Cucapah earthquake from geodetic data
SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH
LA English
DT Article
DE El Mayor-Cucapah earthquake; geodetic inversion; static inversion with
layered model; shallow slip deficit
ID NEAR-FIELD; POSTSEISMIC DEFORMATION; SOUTHERN CALIFORNIA; LANDERS
EARTHQUAKE; GPS OBSERVATIONS; SURFACE RUPTURE; COSEISMIC SLIP; HECTOR
MINE; INSAR; DISPLACEMENTS
AB The 4 April 2010 M-w 7.2 El Mayor-Cucapah (EMC) earthquake in Baja, California, and Sonora, Mexico, had primarily right-lateral strike-slip motion and a minor normal-slip component. The surface rupture extended about 120km in a NW-SE direction, west of the Cerro Prieto fault. Here we use geodetic measurements including near- to far-field GPS, interferometric synthetic aperture radar (InSAR), and subpixel offset measurements of radar and optical images to characterize the fault slip during the EMC event. We use dislocation inversion methods and determine an optimal nine-segment fault geometry, as well as a subfault slip distribution from the geodetic measurements. With systematic perturbation of the fault dip angles, randomly removing one geodetic data constraint, or different data combinations, we are able to explore the robustness of the inferred slip distribution along fault strike and depth. The model fitting residuals imply contributions of early postseismic deformation to the InSAR measurements as well as lateral heterogeneity in the crustal elastic structure between the Peninsular Ranges and the Salton Trough. We also find that with incorporation of near-field geodetic data and finer fault patch size, the shallow slip deficit is reduced in the EMC event by reductions in the level of smoothing. These results show that the outcomes of coseismic inversions can vary greatly depending on model parameterization and methodology.
C1 [Huang, Mong-Han; Fielding, Eric J.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Dickinson, Haylee; Freed, Andrew M.] Purdue Univ, Dept Earth Atmospher & Planetary Sci, W Lafayette, IN 47907 USA.
[Sun, Jianbao] China Earthquake Adm, Inst Geol, State Key Lab Earthquake Dynam, Beijing, Peoples R China.
[Gonzalez-Ortega, J. Alejandro] Univ Calif San Diego, Scripps Inst Oceanog, Inst Geophys & Planetary Phys, La Jolla, CA 92093 USA.
[Burgmann, Roland] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
[Burgmann, Roland] Univ Calif Berkeley, Berkeley Seismol Lab, Berkeley, CA 94720 USA.
RP Huang, MH (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Mong-Han.Huang@jpl.nasa.gov
OI Burgmann, Roland/0000-0002-3560-044X; Huang,
Mong-Han/0000-0003-2331-3766
FU ESA [AOE-668]; NASA
FX We highly appreciate the careful review and the comments by Associate
Editor E. Hill, G. Funning, and an anonymous reviewer, which
significantly improved the quality of this manuscript. Original Envisat
SAR data are copyright ESA and were provided under ESA data grant
AOE-668 and data licenses to UNAVCO for the EarthScope and WInSAR
projects. Original ALOS SAR data are copyright JAXA and were provided
through the Alaska Satellite Facility. The PBO GPS data are available at
the UNAVCO website (ftp://data-out.unavco.org/pub/products/sinex/). The
SCEC community velocity model is available at the website
(http://scec.usc.edu/scecpedia/Community_Velocity_Model). The first-year
aftershock catalog is from CICESE (http://resnom.cicese.mx/). The joint
inversion based slip distribution can be found in Table S1. We thank D.
Dreger for providing the codes for computing data weighting, smoothing,
and geodetic inversions. S. Leprince provided the digital versions of
his COSI-Corr analysis of SPOT images. We would like to thank CICESE for
the GPS installation and acquisition and X. Xu for sharing their shallow
slip deficit results. Part of this research was supported by the NASA
Earth Surface and Interior Focus Area and performed at the Jet
Propulsion Laboratory, California Institute of Technology. M.-H. Huang
is supported by an appointment to the NASA Postdoctoral Program at the
Jet Propulsion Laboratory, administered by Oak Ridge Associated
Universities through a contract with NASA.
NR 38
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U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9313
EI 2169-9356
J9 J GEOPHYS RES-SOL EA
JI J. Geophys. Res.-Solid Earth
PD JAN
PY 2017
VL 122
IS 1
BP 607
EP 621
DI 10.1002/2016JB012858
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EM9VH
UT WOS:000395658900035
ER
PT J
AU Yungster, S
Paxson, DE
Perkins, HD
AF Yungster, Shaye
Paxson, Daniel E.
Perkins, Hugh D.
TI Numerical Investigation of Shrouded Ejector-Enhanced Pulse Combustor
Performance at High Pressure
SO JOURNAL OF PROPULSION AND POWER
LA English
DT Article
ID DETONATION ENGINES; NOX FORMATION; AIR MIXTURES
AB A computational fluid dynamics investigation of a pressure-gain combustor system for gas turbine applications is described. The system consists of a valved pulse combustor and an ejector, housed within a shroud. The computational fluid dynamics solver is first validated by comparing its output to experimental measurements done on a pulse combustor operating at sea-level static conditions. Subsequently, the combustor inlet pressure and temperature are increased in the simulations to more closely align with those seen downstream of a compressor. Several parameters that influence combustor performance are then varied in order to demonstrate the potential benefit of optimization efforts. Emissions calculations are also performed. It is found that efficient high-pressure operation is possible and that system pressure gain of nearly 3% (at gas turbine compatible combustor temperature ratios) is achievable, with nearly smooth exit flow, having a competitive emission index. The potential for pulse combustors to achieve ultra-low levels of NOx emissions at high-pressure conditions is also demonstrated.
C1 [Yungster, Shaye] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
[Paxson, Daniel E.; Perkins, Hugh D.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Yungster, S (reprint author), Ohio Aerosp Inst, Cleveland, OH 44142 USA.
FU NASA [NNC13TA84T.04]
FX This study was supported by NASA under contract number NNC13TA84T.04.
The computational resources were provided by the NASA Advanced
Supercomputing (NAS) Division.
NR 44
TC 0
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PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0748-4658
EI 1533-3876
J9 J PROPUL POWER
JI J. Propul. Power
PD JAN
PY 2017
VL 33
IS 1
BP 29
EP 42
DI 10.2514/1.B36082
PG 14
WC Engineering, Aerospace
SC Engineering
GA EK2SX
UT WOS:000393778100003
ER
PT J
AU Kan, BK
Heister, SD
Paxson, DE
AF Kan, Brandon K.
Heister, Stephen D.
Paxson, Daniel E.
TI Experimental Study of Pressure Gain Combustion with Hypergolic Rocket
Propellants
SO JOURNAL OF PROPULSION AND POWER
LA English
DT Article
ID HYDROGEN-PEROXIDE; DETONATION; MECHANISM
AB This paper summarizes experimental observations of pulsed combustion occurring in a 4.5 cm diameter, nozzleless rocket combustor for pressure gain combustion applications. The combustor featured an impinging jet injector and operated on high-concentration hydrogen peroxide with a catalyst-laced hydrocarbon-based fuel. Pressure oscillations in the 200-700 Hz range were found. For a 10 bar manifold pressure, peak-pressure responses exceeding 60 bar were recorded in the feed system. Transient propellant spray destruction and formation were observed through an optically accessible combustor section. The pulse combustion frequency was tightly tied to atomization, mixing, and hydrogen peroxide decomposition processes; furthermore, frequency was well correlated with the injection velocity for a given injector design. While a precise description is still lacking, the combustion of a mixture of decomposed hydrogen peroxide and fuel appears to be best described as a constant-volume combustion event.
C1 [Kan, Brandon K.; Heister, Stephen D.] Purdue Univ, Sch Aeronaut & Astronaut, 315 North Grant Street, W Lafayette, IN 47907 USA.
[Paxson, Daniel E.] NASA, John H Glenn Res Ctr Lewis Field, Div Instrumentat & Controls, MS 77-1, Cleveland, OH 44135 USA.
RP Kan, BK (reprint author), Purdue Univ, Sch Aeronaut & Astronaut, 315 North Grant Street, W Lafayette, IN 47907 USA.
NR 28
TC 0
Z9 0
U1 0
U2 0
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0748-4658
EI 1533-3876
J9 J PROPUL POWER
JI J. Propul. Power
PD JAN
PY 2017
VL 33
IS 1
BP 112
EP 120
DI 10.2514/1.B36195
PG 9
WC Engineering, Aerospace
SC Engineering
GA EK2SX
UT WOS:000393778100011
ER
PT J
AU Kojima, JJ
Fischer, DG
Chen, JY
AF Kojima, Jun J.
Fischer, David G.
Chen, Jyh-Yuan
TI Code-Validation Scalar Measurements in High-Pressure Hydrogen-Added
Methane Combustion
SO JOURNAL OF PROPULSION AND POWER
LA English
DT Article
ID TURBINE MODEL COMBUSTOR; SPONTANEOUS RAMAN-SCATTERING; SOOT FORMATION;
ELEVATED PRESSURE; LIF MEASUREMENTS; SWIRL FLAMES; LASER-LIGHT;
NARROW-BAND; JET FLAMES; LAMINAR
AB The latest combustion model-validation experiments are presented using a time-, space-, and polarization-resolved subframe-burst gating Raman spectroscopy system. A modification to the original subframe-burst gating diagnostics system enables parallel detection of both polarized and depolarized Raman components for the first time in a high-pressure flame tube, which permits signal detection with reduced background noise, and consequently more precise determination of temperature and species in optically harsh flames. This technique is applied to the measurement of mass fractions of the major species and temperature in a swirl-stabilized hydrogen-methane flame at an elevated pressure of 15.5 bar. The single-shot linear Raman spectra are reduced to provide quantitative multiscalar information throughout the primary reaction zone. The experimental dataset is plotted along with the laminar flamelet calculations for different Lewis numbers and strain rates to allow better interpretation. Time-dependent analysis of the recorded samples using cross correlations, probability density functions, and scatter plots reveals the characteristic behavior of the quantities over a range of mixture fractions, including the local flame structure and the influence of turbulence-chemistry interactions.
C1 [Kojima, Jun J.] Ohio Aerosp Inst, 22800 Cedar Point Rd, Cleveland, OH 44142 USA.
[Fischer, David G.] NASA, John H Glenn Res Ctr, 21000 Brookpark Rd, Cleveland, OH 44135 USA.
[Chen, Jyh-Yuan] Univ Calif Berkeley, 6181 Etcheverry Hall, Berkeley, CA 94720 USA.
RP Kojima, JJ (reprint author), Ohio Aerosp Inst, 22800 Cedar Point Rd, Cleveland, OH 44142 USA.
EM Jun.J.Kojima@nasa.gov
FU Fundamental Aeronautics Program's Transformational Tools and
Technologies; former Supersonics Project at NASAJohn H. Glenn Research
Center
FX This work was supported principally by the Fundamental Aeronautics
Program's Transformational Tools and Technologies and former Supersonics
Project at NASAJohn H. Glenn Research Center. The authors acknowledge
Alan Revilock, Kurt Rusmisel, and Julius Mirecki for their assistance in
the construction and operation of the facilities.
NR 37
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U1 1
U2 1
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0748-4658
EI 1533-3876
J9 J PROPUL POWER
JI J. Propul. Power
PD JAN
PY 2017
VL 33
IS 1
BP 285
EP 302
DI 10.2514/1.B36108
PG 18
WC Engineering, Aerospace
SC Engineering
GA EK2SX
UT WOS:000393778100028
ER
PT J
AU Schaefer, AL
Croom, SM
Allen, JT
Brough, S
Medling, AM
Ho, IT
Scott, N
Richards, SN
Pracy, MB
Gunawardhana, MLP
Norberg, P
Alpaslan, M
Bauer, AE
Bekki, K
Bland-Hawthorn, J
Bloom, JV
Bryant, JJ
Couch, WJ
Driver, SP
Fogarty, LMR
Foster, C
Goldstein, G
Green, AW
Hopkins, AM
Konstantopoulos, IS
Lawrence, JS
Lopez-Sanchez, AR
Lorente, NPF
Owers, MS
Sharp, R
Sweet, SM
Taylor, EN
van de Sande, J
Walcher, CJ
Wong, OI
AF Schaefer, A. L.
Croom, S. M.
Allen, J. T.
Brough, S.
Medling, A. M.
Ho, I. -T.
Scott, N.
Richards, S. N.
Pracy, M. B.
Gunawardhana, M. L. P.
Norberg, P.
Alpaslan, M.
Bauer, A. E.
Bekki, K.
Bland-Hawthorn, J.
Bloom, J. V.
Bryant, J. J.
Couch, W. J.
Driver, S. P.
Fogarty, L. M. R.
Foster, C.
Goldstein, G.
Green, A. W.
Hopkins, A. M.
Konstantopoulos, I. S.
Lawrence, J. S.
Lopez-Sanchez, A. R.
Lorente, N. P. F.
Owers, M. S.
Sharp, R.
Sweet, S. M.
Taylor, E. N.
van de Sande, J.
Walcher, C. J.
Wong, O. I.
TI The SAMI Galaxy Survey: spatially resolving the environmental quenching
of star formation in GAMA galaxies
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: evolution; galaxies: general; galaxies: interactions;
galaxies: statistics; galaxies: stellar content; galaxies: structure
ID DIGITAL SKY SURVEY; INTEGRAL-FIELD SPECTROSCOPY; INITIAL MASS FUNCTION;
EARLY DATA RELEASE; FORMING GALAXIES; H-ALPHA; CLUSTER GALAXIES; SPIRAL
GALAXIES; STELLAR MASS; REDSHIFT SURVEY
AB We use data from the Sydney-AAO Multi-Object Integral Field Spectrograph Galaxy Survey and the Galaxy And Mass Assembly (GAMA) survey to investigate the spatially resolved signatures of the environmental quenching of star formation in galaxies. Using dust-corrected measurements of the distribution of H alpha emission, we measure the radial profiles of star formation in a sample of 201 star-forming galaxies covering three orders of magnitude in stellar mass (M-*; 10(8.1)-10(10.95)M(circle dot)) and in fifth nearest neighbour local environment density (Sigma(5); 10(-1.3)-10(2.1) Mpc(-2)). We show that star formation rate gradients in galaxies are steeper in dense (log(10)(Sigma(5)/Mpc(2)) > 0.5) environments by 0.58 +/- 0.29 dex re(-1) in galaxies with stellar masses in the range 10(10) < M-*/M-circle dot < 10(11) and that this steepening is accompanied by a reduction in the integrated star formation rate. However, for any given stellar mass or environment density, the star formation morphology of galaxies shows large scatter. We also measure the degree to which the star formation is centrally concentrated using the unitless scale-radius ratio (r50, Ha/r50, cont), which compares the extent of ongoing star formation to previous star formation. With this metric, we find that the fraction of galaxies with centrally concentrated star formation increases with environment density, from similar to 5 +/- 4 per cent in low-density environments (log10(Sigma 5/Mpc2) < 0.0) to 30 +/- 15 per cent in the highest density environments (log(10)(Sigma(5)/Mpc(2)) > 1.0). These lines of evidence strongly suggest that with increasing local environment density, the star formation in galaxies is suppressed, and that this starts in their outskirts such that quenching occurs in an outside-in fashion in dense environments and is not instantaneous.
C1 [Schaefer, A. L.; Croom, S. M.; Allen, J. T.; Scott, N.; Richards, S. N.; Pracy, M. B.; Bland-Hawthorn, J.; Bloom, J. V.; Bryant, J. J.; Fogarty, L. M. R.; van de Sande, J.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Schaefer, A. L.; Brough, S.; Richards, S. N.; Bauer, A. E.; Bryant, J. J.; Foster, C.; Green, A. W.; Hopkins, A. M.; Konstantopoulos, I. S.; Lawrence, J. S.; Lopez-Sanchez, A. R.; Lorente, N. P. F.; Owers, M. S.] AAO, POB 915, N Ryde, NSW 1670, Australia.
[Schaefer, A. L.; Croom, S. M.; Allen, J. T.; Brough, S.; Scott, N.; Richards, S. N.; Bloom, J. V.; Bryant, J. J.; Wong, O. I.] Univ Sydney, Sch Phys, CAASTRO ARC Ctr Excellence All Sky Astrophys, Bldg A28, Sydney, NSW 2006, Australia.
[Medling, A. M.; Ho, I. -T.; Sharp, R.; Sweet, S. M.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia.
[Ho, I. -T.] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
[Gunawardhana, M. L. P.; Norberg, P.] Univ Durham, Inst Computat Cosmol, Dept Phys, Durham DH1 3LE, England.
[Gunawardhana, M. L. P.; Norberg, P.] Univ Durham, Ctr Extragalact Astron, Durham DH1 3LE, England.
[Alpaslan, M.] NASA, Ames Res Ctr, N232, Mountain View, CA 94035 USA.
[Bekki, K.; Driver, S. P.; Taylor, E. N.] Univ Western Australia, Int Ctr Radio Astron Res, 35 Stirling Highway, Crawley, WA 6009, Australia.
[Couch, W. J.; Wong, O. I.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, POB 218, Hawthorn, Vic 3122, Australia.
[Driver, S. P.] Univ St Andrews, SUPA Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Goldstein, G.; Lopez-Sanchez, A. R.; Owers, M. S.] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia.
[Konstantopoulos, I. S.] Envizi, Natl Innovat Ctr, Suite 213,Australian Technol Pk,4 Cornwallis St, Eveleigh, NSW 2015, Australia.
[Walcher, C. J.] Leibniz Inst Astrophysik Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany.
RP Schaefer, AL (reprint author), Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.; Schaefer, AL (reprint author), AAO, POB 915, N Ryde, NSW 1670, Australia.; Schaefer, AL (reprint author), Univ Sydney, Sch Phys, CAASTRO ARC Ctr Excellence All Sky Astrophys, Bldg A28, Sydney, NSW 2006, Australia.
EM adam.schaefer@uni.sydney.edu.au
OI Bryant, Julia/0000-0003-1627-9301
FU Australian Research Council Centre of Excellence for All-sky
Astrophysics (CAASTRO) [CE110001020]; Australian Research Council (ARC)
Centre of Excellence program; NSW State Government's Science Leveraging
Fund; European Research Council [DEGAS-259586]; Australian Research
Council [FT100100457, FT140101166, FT140100255]; SIEF John Stocker
Fellowship; Science and Technology Facilities Council [ST/L00075X/1];
ARC [FL140100278]; University of Sydney Postdoctoral Research Fellowship
FX The SAMI Galaxy Survey is based on observation made at the
Anglo-Australian Telescope. The SAMI was developed jointly by the
University of Sydney and the Australian Astronomical Observatory. The
SAMI input catalogue is based on data taken from the SDSS, the GAMA
Survey and the VST ATLAS Survey. The SAMI Galaxy Survey is funded by the
Australian Research Council Centre of Excellence for All-sky
Astrophysics (CAASTRO), through project number CE110001020, and other
participating institutions. The SAMI Galaxy Survey website is
http://sami-survey.org/.; The CAASTRO is a collaboration between The
University of Sydney, The Australian National University, The University
of Melbourne, Swinburne University of Technology, The University of
Queensland, The University of Western Australia and Curtin University,
the latter two participating together as the International Centre for
Radio Astronomy Research (ICRAR). CAASTRO is funded under the Australian
Research Council (ARC) Centre of Excellence program, with additional
funding from the seven participating universities and from the NSW State
Government's Science Leveraging Fund.; ALS acknowledges support from a
European Research Council grant (DEGAS-259586). SMC acknowledges the
support of an Australian Research Council Future Fellowship
(FT100100457). SB acknowledges funding support from the Australian
Research Council through a Future Fellowship (FT140101166). JTA
acknowledges the award of an SIEF John Stocker Fellowship. MLPG
acknowledges support from a European Research Council grant
(DEGAS-259586) and the Science and Technology Facilities Council
(ST/L00075X/1). MSO acknowledges the funding support from the Australian
Research Council through a Future Fellowship Fellowship (FT140100255).
MA is funded by an appointment to the NASA Postdoctoral Program at Ames
Research Centre, administered by Universities Space Research Association
through a contract with NASA. JvdS is funded under Bland-Hawthorn's ARC
Laureate Fellowship (FL140100278). NS acknowledges support of a
University of Sydney Postdoctoral Research Fellowship. This research
made use of ASTROPY, a community-developed core PYTHON package for
Astronomy (Astropy Collaboration et al. 2013). We also used the NUMPY
and SCIPY scientific PYTHON libraries.
NR 118
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U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN
PY 2017
VL 464
IS 1
BP 121
EP 142
DI 10.1093/mnras/stw2289
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EK0VX
UT WOS:000393646300010
ER
PT J
AU Rani, B
Krichbaum, TP
Lee, SS
Sokolovsky, K
Kang, S
Byun, DY
Mosunova, D
Zensus, JA
AF Rani, B.
Krichbaum, T. P.
Lee, S. -S.
Sokolovsky, K.
Kang, S.
Byun, D. -Y.
Mosunova, D.
Zensus, J. A.
TI Probing the gamma-ray variability in 3C 279 using broad-band
observations
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies:active; galaxies:jets; quasars:individual:3C 279;
gamma-rays:general; radio continuum:galaxies; X-rays:galaxies
ID LARGE-AREA TELESCOPE; ACTIVE GALACTIC NUCLEI; X-RAY; S5 0716+714;
MULTIWAVELENGTH OBSERVATIONS; ENERGY-DISTRIBUTION; MAGNETIC-FIELDS;
LIGHT CURVES; RADIO; BLAZARS
AB We present the results of a broad-band radio-to-GeV observing campaign organized to get a better understanding of the radiation processes responsible for the gamma-ray flares observed in 3C 279. The total intensity and polarization observations of the source were carried out between 2013 December 28 and 2014 January 03 using the Fermi-Large Area Telescope, Swift-XRT, Swift-UVOT, and Korean VLBI Network telescopes. A prominent flare observed in the optical/near-UV passbands was found to be correlated with a concurrent gamma-ray flare at a confidence level >95 per cent, which suggests a co-spatial origin of the two. Moreover, the flaring activity in the two regimes was accompanied by no significant spectral variations. A peak in the X-ray light curve coincides with the peaks of the fractional polarization curves at 43 and 86 GHz radio bands. No prominent variation was noticed for the total intensity and the electric vector position angle observations at radio bands during this period. We noticed a possible hint of steepening of the radio spectrum with an increase in percentage polarization, which suggests that the radio polarization variations could be simply due to a spectral change. In a simple scenario, the correlated optical/gamma-ray flares could be caused by the same population of emitting particles. The coincidence of the increase in radio polarization with the X-ray flux supports the picture that X-rays are produced via inverse-Compton scattering of radio photons. The observed fractional variability for the gamma-ray flare similar to 0.23 does not exceed that in the optical regime, which is inconsistent with what we usually observe for 3C 279; it could be due to different dependencies of the magnetic field and the external radiation field energy density profiles along the jet.
C1 [Rani, B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Rani, B.; Krichbaum, T. P.; Zensus, J. A.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Lee, S. -S.; Kang, S.; Byun, D. -Y.] Korea Astron & Space Sci Inst, 776 Daedeok Daero, Daejeon 34055, South Korea.
[Lee, S. -S.; Kang, S.; Byun, D. -Y.] Univ Sci & Technol, 217 Gajeong Ro, Daejeon 34055, South Korea.
[Sokolovsky, K.; Mosunova, D.] Lebedev Phys Inst, Astro Space Ctr, Profsoyuznaya 84-32, Moscow 117997, Russia.
[Sokolovsky, K.] Natl Observ Athens, IAASARS, GR-15236 Penteli, Greece.
[Sokolovsky, K.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Univ Pr 13, Moscow 119992, Russia.
RP Rani, B (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Rani, B; Krichbaum, TP (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
EM bindu.rani@nasa.gov; tkrichbaum@mpifr-bonn.mpg.de
FU National Aeronautics and Space Administration in the United States;
Department of Energy in the United States; Commissariat a l'Energie
Atomique in France; Centre National de la Recherche
Scientifique/Institut National de Physique Nucleaire et de Physique des
Particules in France; Agenzia Spaziale Italiana in Italy; Istituto
Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture,
Sports, Science and Technology (MEXT) in Japan; High Energy Accelerator
Research Organization (KEK) in Japan; Japan Aerospace Exploration Agency
(JAXA) in Japan; K. A. Wallenberg Foundation in Sweden; Swedish Research
Council in Sweden; Swedish National Space Board in Sweden; NASA
Postdoctoral Program at the Goddard Space Flight Center; KREONET (Korea
Research Environment Open NETwork); RFBR [14-02-31789]; National
Research Foundation of Korea (NRF) grant - Korea government (MSIP)
[NRF-2016R1C1B2006697]; Istituto Nazionale di Astrofisica in Italy;
Centre National d'Etudes Spatiales in France
FX The Fermi/LAT Collaboration acknowledges the generous support of a
number of agencies and institutes that have supported the Fermi/LAT
Collaboration. These include the National Aeronautics and Space
Administration and the Department of Energy in the United States, the
Commissariat a l'Energie Atomique and the Centre National de la
Recherche Scientifique/Institut National de Physique Nucleaire et de
Physique des Particules in France, the Agenzia Spaziale Italiana and the
Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of
Education, Culture, Sports, Science and Technology (MEXT), High Energy
Accelerator Research Organization (KEK) and Japan Aerospace Exploration
Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish
Research Council and the Swedish National Space Board in Sweden.
Additional support for science analysis during the operations phase is
gratefully acknowledged from the Istituto Nazionale di Astrofisica in
Italy and the Centre National d'Etudes Spatiales in France. This
research was supported by an appointment to the NASA Postdoctoral
Program at the Goddard Space Flight Center, administered by Universities
Space Research Association through a contract with NASA. We would like
to thank the referee for his/her constructive comments. BR acknowledges
the help of M. Bottcher, Vassilis Karamanavis, Greg Madejski, Roopesh
Ojha, Jeremy Perkins, and Dave Thompson for fruitful discussions and
comments that improved the manuscript. BR is thankful to D.
Emmanoulopoulos for the useful discussions on statistical analysis. The
KVN is a facility operated by the Korea Astronomy and Space Science
Institute. The KVN operations are supported by KREONET (Korea Research
Environment Open NETwork) which is managed and operated by KISTI (Korea
Institute of Science and Technology Information). KVS is supported by
the RFBR grant 14-02-31789. SSL and KS are supported by the National
Research Foundation of Korea (NRF) grant funded by the Korea government
(MSIP) (No. NRF-2016R1C1B2006697).
NR 62
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EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN
PY 2017
VL 464
IS 1
BP 418
EP 427
DI 10.1093/mnras/stw2342
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EK0VX
UT WOS:000393646300032
ER
PT J
AU Su, T
Marriage, TA
Asboth, V
Baker, AJ
Bond, JR
Crichton, D
Devlin, MJ
Dunner, R
Farrah, D
Frayer, DT
Gralla, MB
Hall, K
Halpern, M
Harris, AI
Hilton, M
Hincks, AD
Hughes, JP
Niemack, MD
Page, LA
Partridge, B
Rivera, J
Scott, D
Sievers, JL
Thornton, RJ
Viero, MP
Wang, L
Wollack, EJ
Zemcov, M
AF Su, T.
Marriage, T. A.
Asboth, V.
Baker, A. J.
Bond, J. R.
Crichton, D.
Devlin, M. J.
Dunner, R.
Farrah, D.
Frayer, D. T.
Gralla, M. B.
Hall, K.
Halpern, M.
Harris, A. I.
Hilton, M.
Hincks, A. D.
Hughes, J. P.
Niemack, M. D.
Page, L. A.
Partridge, B.
Rivera, J.
Scott, D.
Sievers, J. L.
Thornton, R. J.
Viero, M. P.
Wang, L.
Wollack, E. J.
Zemcov, M.
TI On the redshift distribution and physical properties of ACT-selected
DSFGs
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: evolution; galaxies: high-redshift; galaxies: starburst;
galaxies: star formation; submillimetre: galaxies
ID STAR-FORMING GALAXIES; ATACAMA COSMOLOGY TELESCOPE; SOUTH-POLE
TELESCOPE; DIGITAL SKY SURVEY; GRAVITATIONALLY LENSED GALAXIES; SPECTRAL
ENERGY-DISTRIBUTIONS; RESOLUTION ALMA OBSERVATIONS; FAR-INFRARED
PROPERTIES; GREEN BANK TELESCOPE; MU-M OBSERVATIONS
AB We present multi-wavelength detections of nine candidate gravitationally lensed dusty starforming galaxies (DSFGs) selected at 218 GHz (1.4 mm) from the Atacama Cosmology Telescope (ACT) equatorial survey. Among the brightest ACT sources, these represent the subset of the total ACT sample lying in Herschel SPIRE fields, and all nine of the 218 GHz detections were found to have bright Herschel counterparts. By fitting their spectral energy distributions (SEDs) with a modified blackbody model with power-law temperature distribution, we find the sample has a median redshift of z = 4.1(-1.0)(+1.1) (68 per cent confidence interval), as expected for 218 GHz selection, and an apparent total infrared luminosity of log10(mu LIR/L-circle dot) = 13.86(-0.30)(+0.33), which suggests that they are either strongly lensed sources or unresolved collections of unlensed DSFGs. The effective apparent diameter of the sample is root mu d = 4.2(-1.0)(+1.7) kpc, further evidence of strong lensing or multiplicity, since the typical diameter of DSFGs is 1.0-2.5 kpc. We emphasize that the effective apparent diameter derives from SED modelling without the assumption of optically thin dust (as opposed to image morphology). We find that the sources have substantial optical depth (tau = 4.2(-1.9)(+3.7)) to dust around the peak in the modified blackbody spectrum (lambda(obs) <= 500 mu m), a result that is robust to model choice.
C1 [Su, T.; Marriage, T. A.; Crichton, D.; Gralla, M. B.; Hall, K.] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.
[Asboth, V.; Hincks, A. D.; Scott, D.] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada.
[Baker, A. J.; Hughes, J. P.; Rivera, J.] Rutgers State Univ, Dept Phys & Astron, 136 Frelinghuysen Rd, Piscataway, NJ 08854 USA.
[Bond, J. R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Devlin, M. J.] Univ Penn, Dept Phys & Astron, 209 South 33rd St, Philadelphia, PA 19104 USA.
[Dunner, R.] Pontificia Univ Catolica, Dept Astron & Astrofis, Casilla 306, Santiago 22, Chile.
[Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
[Frayer, D. T.] Natl Radio Astron Observ, POB 2, Green Bank, WV 24944 USA.
[Gralla, M. B.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Gralla, M. B.; Halpern, M.] Univ Arizona, Steward Observ, Dept Astron, 933 North Cherry Ave, Tucson, AZ 85721 USA.
[Harris, A. I.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Hilton, M.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
[Hincks, A. D.] Univ Roma La Sapienza, Dept Phys, Piazzale Aldo Moro 5, I-00185 Rome, Italy.
[Niemack, M. D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA.
[Page, L. A.] Princeton Univ, Joseph Henry Labs Phys, Jadwin Hall, Princeton, NJ 08544 USA.
[Partridge, B.] Haverford Coll, Dept Astron, Haverford, PA 19041 USA.
[Sievers, J. L.] Univ KwaZulu Natal, Sch Chem & Phys, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
[Thornton, R. J.] West Chester Univ, Dept Phys, 700 S High St, W Chester, PA 19382 USA.
[Viero, M. P.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 382 Via Pueblo Mall, Stanford, CA 94305 USA.
[Wang, L.] SRON Netherlands Inst Space Res, Landleven 12, NL-9747 AD Groningen, Netherlands.
[Wollack, E. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Zemcov, M.] Rochester Inst Technol, Sch Phys & Astron, Ctr Detectors, 1 Lomb Mem Dr, Rochester, NY 14623 USA.
[Zemcov, M.] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Su, T; Marriage, TA (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.; Asboth, V (reprint author), Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada.
EM tsu5@jhu.edu; marriage@jhu.edu; vasboth@phas.ubc.ca
RI Wollack, Edward/D-4467-2012
OI Wollack, Edward/0000-0002-7567-4451
FU National Science Foundation [AST-0955810]; U.S. National Science
Foundation [AST-0408698, AST-0965625]; Princeton University; University
of Pennsylvania; Canada Foundation for Innovation (CFI); CFI under
Compute Canada; Government of Ontario; Ontario Research Fund - Research
Excellence; University of Toronto; Moore Foundation; Norris Foundation;
Associates of Caltech; state of California; state of Illinois; state of
Maryland; NSF; NSF under a cooperative agreement; CARMA partner
universities; Alfred P. Sloan Foundation; National Aeronautics and Space
Administration; National Science Foundation; U.S. Department of Energy;
Japanese Monbukagakusho; Max Planck Society; Higher Education Funding
Council for England; U.S. Department of Energy Office of Science;
Comision Nacional de Investigacion Cientifica y Tecnologica de Chile
(CONICYT); Compute Canada; [PHY-0855887]; [PHY-1214379]
FX We thank our LMT collaborators for permission to make use of the
spectroscopic redshift for ACT-S J0107+0001 in advance of publication.
We thank Zhen-Yi Cai for providing model source distributions. AJB
acknowledges support from the National Science Foundation though grant
AST-0955810. ACT was supported by the U.S. National Science Foundation
through awards AST-0408698 and AST-0965625 for the ACT project, as well
as awards PHY-0855887 and PHY-1214379. ACT funding was also provided by
Princeton University, the University of Pennsylvania, and a Canada
Foundation for Innovation (CFI) award to UBC. ACT operates in the Parque
Astronomico Atacama in northern Chile under the auspices of the Comision
Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT).
Computations were performed on the GPC supercomputer at the SciNet HPC
Consortium. SciNet is funded by the CFI under the auspices of Compute
Canada, the Government of Ontario, the Ontario Research Fund - Research
Excellence; and the University of Toronto. Support for CARMA
construction was derived from the Moore and Norris Foundations, the
Associates of Caltech, the states of California, Illinois, and Maryland,
and the NSF. CARMA development and operations were supported by the NSF
under a cooperative agreement, and by the CARMA partner universities.
The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc. We have used optical imaging from SDSS. Funding for
the SDSS and SDSS-II has been provided by the Alfred P. Sloan
Foundation, the Participating Institutions, the National Science
Foundation, the U.S. Department of Energy, the National Aeronautics and
Space Administration, the Japanese Monbukagakusho, the Max Planck
Society, and the Higher Education Funding Council for England. Funding
for SDSS-III has been provided by the Alfred P. Sloan Foundation, the
Participating Institutions, the National Science Foundation, and the
U.S. Department of Energy Office of Science. Part of our NIR imaging is
based on observations obtained as part of the VHS, ESO Progam,
179.A-2010 (PI: McMahon). We also have used data based on observations
obtained with the Apache Point Observatory 3.5-metre telescope, which is
owned and operated by the Astrophysical Research Consortium. This
publication makes use of data products from the WISE, which is a joint
project of the University of California, Los Angeles, and the Jet
Propulsion Laboratory/California Institute of Technology, funded by the
National Aeronautics and Space Administration. Some of the observations
reported in this paper were obtained with the Southern African Large
Telescope (SALT). Finally, we acknowledge the MNRAS reviewer and editor
for comments that improved the paper.
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JI Mon. Not. Roy. Astron. Soc.
PD JAN
PY 2017
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EP 984
DI 10.1093/mnras/stw2334
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EK0VX
UT WOS:000393646300075
ER
PT J
AU Schneider, T
Teixeira, J
Bretherton, CS
Brient, F
Pressel, KG
Schar, C
Siebesma, AP
AF Schneider, Tapio
Teixeira, Joao
Bretherton, Christopher S.
Brient, Florent
Pressel, Kyle G.
Schar, Christoph
Siebesma, A. Pier
TI COMMENTARY: Climate goals and computing the future of clouds
SO NATURE CLIMATE CHANGE
LA English
DT Editorial Material
ID LARGE-EDDY SIMULATION; EMISSIONS
C1 [Schneider, Tapio; Pressel, Kyle G.] CALTECH, Pasadena, CA 91125 USA.
[Teixeira, Joao] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
[Bretherton, Christopher S.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
[Brient, Florent] CNRS, Meteo France, Ctr Natl Rech Meteorol, F-31057 Toulouse, France.
[Schar, Christoph] ETH, Inst Atmospher & Climate Sci, CH-8092 Zurich, Switzerland.
[Siebesma, A. Pier] Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands.
[Siebesma, A. Pier] Delft Univ Technol, NL-2600 AA Delft, Netherlands.
RP Schneider, T (reprint author), CALTECH, Pasadena, CA 91125 USA.
EM tapio@caltech.edu
FU US Department of Energy [DE-SC0012451]
FX We thank Momme Hell (Univ. California) for contributing to preparing
Fig. 3. C.B. acknowledges grant DE-SC0012451 from the US Department of
Energy.
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EI 1758-6798
J9 NAT CLIM CHANGE
JI Nat. Clim. Chang.
PD JAN
PY 2017
VL 7
IS 1
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WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric
Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA EN9VC
UT WOS:000396346700004
ER
PT J
AU Carlson, KM
Gerber, JS
Mueller, ND
Herrero, M
MacDonald, GK
Brauman, KA
Havlik, P
O'Connell, CS
Johnson, JA
Saatchi, S
West, PC
AF Carlson, Kimberly M.
Gerber, James S.
Mueller, Nathaniel D.
Herrero, Mario
MacDonald, Graham K.
Brauman, Kate A.
Havlik, Petr
O'Connell, Christine S.
Johnson, Justin A.
Saatchi, Sassan
West, Paul C.
TI Greenhouse gas emissions intensity of global croplands
SO NATURE CLIMATE CHANGE
LA English
DT Article
ID NITROUS-OXIDE; METHANE EMISSION; FOOD SECURITY; N2O EMISSIONS;
SUSTAINABLE INTENSIFICATION; AGRONOMIC ASSESSMENT; FERTILIZER NITROGEN;
WATER MANAGEMENT; FLOODED RICE; LAND-USE
AB Stabilizing greenhouse gas (GHG) emissions fromcroplands as agricultural demand grows is a critical component of climate change mitigation(1-3). Emissions intensity metrics-including carbon dioxide equivalent emissions per kilocalorie produced ('production intensity')-can highlight regions, management practices, and crops as potential foci for mitigation(4-7). Yet the spatial and crop-wise distribution of emissions intensity has been uncertain. Here, we develop global crop-specific circa 2000 estimates of GHG emissions and GHG intensity in high spatial detail, reporting the effects of rice paddy management, peatland draining, and nitrogen (N) fertilizer on CH4, CO2 and N-2O emissions. Global mean production intensity is 0.16 Mg CO(2)e M kcal(-1), yet certain cropping practices contribute disproportionately to emissions. Peatland drainage (3.7 Mg CO(2)e M kcal(-1))-concentrated in Europe and Indonesia-accounts for 32% of these cropland emissions despite peatlands producing just 1.1% of total crop kilocalories. Methane emissions fromrice (0.58 Mg CO(2)e M kcal(-1)), a crucial food staple supplying 15% of total crop kilocalories, contribute 48% of cropland emissions, with outsized production intensity in Vietnam. In contrast, N2O emissions from N fertilizer application (0.033 Mg CO(2)e M kcal(-1)) generate only 20% of cropland emissions. We find that current total GHG emissions are largely unrelated to production intensity across crops and countries. Climate mitigation policies should therefore be directed to locations where crops have both high emissions and high intensities.
C1 [Carlson, Kimberly M.; Gerber, James S.; MacDonald, Graham K.; Brauman, Kate A.; O'Connell, Christine S.; Johnson, Justin A.; West, Paul C.] Univ Minnesota, Inst Environm, St Paul, MN 55108 USA.
[Carlson, Kimberly M.] Univ Hawaii, Dept Nat Resources & Environm Management, Honolulu, HI 96822 USA.
[Mueller, Nathaniel D.] Harvard Univ, Dept Earth & Planetary Sci, Harvard, MA 02138 USA.
[Mueller, Nathaniel D.] Harvard Univ, Dept Organism & Evolutionary Biol, Harvard, MA 02138 USA.
[Herrero, Mario] CSIRO, St Lucia, Qld, Australia.
[MacDonald, Graham K.] McGill Univ, Dept Geog, Montreal, PQ H3A 0B9, Canada.
[Havlik, Petr] Int Inst Appl Syst Anal, Ecosyst Serv & Management Program, Laxenburg, Austria.
[O'Connell, Christine S.] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA.
[Saatchi, Sassan] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Carlson, KM (reprint author), Univ Minnesota, Inst Environm, St Paul, MN 55108 USA.; Carlson, KM (reprint author), Univ Hawaii, Dept Nat Resources & Environm Management, Honolulu, HI 96822 USA.
EM kimcarlson@gmail.com
OI Carlson, Kimberly/0000-0003-2162-1378
FU Gordon and Betty Moore Foundation; University of Minnesota Institute on
the Environment; USDA National Institute of Food and Agriculture Hatch
project [HAW01136-H]; USDA Agriculture and Food Research Initiative
[2016-67012-25208]; NSF Hydrological Sciences grant [1521210]; Belmont
Forum/FACCE-JPI-funded DEVIL project [NE/M021327/1]
FX We thank J. Foley for conversations conceptualizing this project. P.
Engstrom, H. Rodrigues, D. Makowski, M. Ogg, S. Seibert and J. van de
Steeg assisted with methods and data development. The Gordon and Betty
Moore Foundation provided primary research funding, with additional
support from the University of Minnesota Institute on the Environment,
USDA National Institute of Food and Agriculture Hatch project
HAW01136-H, managed by the College of Tropical Agriculture and Human
Resources (K.M.C.), USDA Agriculture and Food Research Initiative
fellowship 2016-67012-25208 (N.D.M.), NSF Hydrological Sciences grant
1521210 (N.D.M.), and the Belmont Forum/FACCE-JPI-funded DEVIL project
NE/M021327/1 (J.S.G., M.H. and P.C.W.). The funders had no role in study
design, data collection and analysis, decision to publish, or
preparation of the manuscript.
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SN 1758-678X
EI 1758-6798
J9 NAT CLIM CHANGE
JI Nat. Clim. Chang.
PD JAN
PY 2017
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BP 63
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DI 10.1038/NCLIMATE3158
PG 9
WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric
Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA EN9VC
UT WOS:000396346700017
ER
PT J
AU Khan, R
AF Khan, Rubab
TI SPITZER PHOTOMETRY OF similar to 1 MILLION STARS IN M31 AND 15 OTHER
GALAXIES
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; surveys; techniques: photometric
ID HUBBLE-SPACE-TELESCOPE; EXTRAGALACTIC DISTANCE DATABASE; COLOR-MAGNITUDE
DIAGRAMS; ETA CAR ANALOGS; NEARBY GALAXIES; KEY PROJECT; ANDROMEDA
NEBULA; MAGELLANIC-CLOUD; MASSIVE STARS; CENSUS
AB We present Spitzer IRAC 3.6-8 mu m and Multiband Imaging Photometer 24 mu m point-source catalogs for M31 and 15 other mostly large, star-forming galaxies at distances similar to 3.5-14 Mpc, including M51, M83, M101, and NGC 6946. These catalogs contain similar to 1 million sources including similar to 859,000 in M31 and similar to 116,000 in the other galaxies. They were created following the procedures described in Khan et al. through a combination of pointspread function (PSF) fitting and aperture photometry. These data products constitute a resource to improve our understanding of the IR-bright (3.6-24 mu m) point-source populations in crowded extragalactic stellar fields and to plan observations with the James Webb Space Telescope.
C1 [Khan, Rubab] NASA, Goddard Space Flight Ctr, Postdoctoral Program, MC 665 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Khan, Rubab] Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
RP Khan, R (reprint author), NASA, Goddard Space Flight Ctr, Postdoctoral Program, MC 665 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.; Khan, R (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
EM rubab@uw.edu
FU National Aeronautics and Space Administration (NASA); JWST Fellowship
FX We thank the referee for helpful suggestions; Krzysztof Stanek,
Christopher Kochanek, and George Sonneborn for productive discussions;
and Martha Boyer and Karl Gordon for providing the M31 image mosaics.
This work is based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology under a contract with the National
Aeronautics and Space Administration (NASA). We extend our gratitude to
the SINGS Legacy Survey and the LVL Survey for making their data
publicly available. This research has made use of NED, which is operated
by the JPL and Caltech, under contract with NASA and the HEASARC Online
Service, provided by NASA's GSFC. R.K. is supported through a JWST
Fellowship hosted by the Goddard Space Flight Center and awarded as part
of the NASA Postdoctoral Program operated by the Oak Ridge Associated
Universities on behalf of NASA.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
EI 1538-4365
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD JAN
PY 2017
VL 228
IS 1
AR 5
DI 10.3847/1538-4365/228/1/5
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EK2OL
UT WOS:000393766500002
ER
PT J
AU Toigo, AD
Waugh, DW
Guzewich, SD
AF Toigo, A. D.
Waugh, D. W.
Guzewich, S. D.
TI What causes Mars' annular polar vortices?
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE polar vortex
ID STRATOSPHERIC ARCTIC VORTEX; POTENTIAL VORTICITY; DYNAMICS; CIRCULATION;
ATMOSPHERE; DUST; GCM
AB A distinctive feature of the Martian atmosphere is that the winter polar vortices exhibit annuli of high potential vorticity (PV) with a local minimum near the pole. These annuli are seen in observations, reanalyses, and free-running general circulation model simulations of Mars, but are not generally a feature of Earth's polar vortices, where there is a monotonic increase in magnitude of PV with latitude. The creation and maintenance of the annular polar vortices on Mars are not well understood. Here we use simulations with a Martian general circulation model to the show that annular vortices are related to another distinctive, and possibly unique in the solar system, feature of the Martian atmosphere: the condensation of the predominant atmospheric gas species (CO2) in polar winter regions. The latent heat associated with CO2 condensation leads to destruction of PV in the polar lower atmosphere, inducing the formation of an annular PV structure.
C1 [Toigo, A. D.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Waugh, D. W.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[Guzewich, S. D.] Univ Space Res Assoc, NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Waugh, DW (reprint author), Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
EM waugh@jhu.edu
OI Guzewich, Scott/0000-0003-1149-7385
FU NASA Mars Fundamental Research Program [NNX14AG53G]
FX The authors gratefully recognize funding from the NASA Mars Fundamental
Research Program through grant NNX14AG53G. All simulations were
performed on the supercomputers of the NASA Advanced Supercomputing
Division at the NASA Ames Research Center. The MACDA data set is
available at 10.5285/78114093-E2BD-4601-8AE5-3551E62AEF2B, upon free
registration to the Centre for Environmental Data Analysis. All other
data are available from the corresponding author upon direct request.
NR 27
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN
PY 2017
VL 44
IS 1
BP 71
EP 78
DI 10.1002/2016GL071857
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA EK5GM
UT WOS:000393954900009
ER
PT J
AU Collier, MR
Newheart, A
Poppe, AR
Hills, HK
Farrell, WM
AF Collier, Michael R.
Newheart, Anastasia
Poppe, Andrew R.
Hills, H. Kent
Farrell, William M.
TI Stair-step particle flux spectra on the lunar surface: Evidence for
nonmonotonic potentials?
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE SIDE; nonmonotonic potentials; plasma sheet; lunar surface potential
ID PHOTOELECTRON SHEATH; SOLAR-WIND; PLASMA; SPACE; FIELDS; RADIATION;
SHADOW; RATES; MOON; IONS
AB We present examples of unusual stair-step differential flux spectra observed by the Apollo 14 Suprathermal Ion Detector Experiment on the lunar dayside surface in Earth's magnetotail. These spectra exhibit a relatively constant differential flux below some cutoff energy and then drop off precipitously, by about an order of magnitude or more, at higher energies. We propose that these spectra result from photoions accelerated on the lunar dayside by nonmonotonic potentials (i.e.,potentials that do not decay to zero monotonically) and present a model for the expected differential flux. The energy of the cutoff and the magnitude of the differential flux are related to the properties of the local space environment and are consistent with the observed flux spectra. If this interpretation is correct, these surface-based ion observations provide a unique perspective that both complements and enhances the conclusions obtained by remote-sensing orbiter observations on the Moon's exospheric and electrostatic properties.
C1 [Collier, Michael R.; Hills, H. Kent; Farrell, William M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Collier, Michael R.; Poppe, Andrew R.; Farrell, William M.] NASA, Ames Res Ctr, DREAM2, SSERVI, Moffett Field, CA 94035 USA.
[Newheart, Anastasia] St Marys Coll Maryland, Dept Phys, St Marys City, MD 20686 USA.
[Poppe, Andrew R.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Hills, H. Kent] Adnet Syst Inc, Lanham, MD USA.
RP Collier, MR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Collier, MR (reprint author), NASA, Ames Res Ctr, DREAM2, SSERVI, Moffett Field, CA 94035 USA.
EM michael.r.collier@nasa.gov
OI Collier, Michael/0000-0001-9658-6605
FU NASA Solar System Exploration Research Virtual Institute, through the
Dynamic Response of the Environment at Asteroids, the Moon, and moons of
Mars (DREAM2) team; NASA's Lunar Advanced Science and Exploration
Research program [NNX13AJ97G]
FX Special thanks to David G. Sibeck for pointing out and supplying useful
references and to Peter Chi and Dave Williams for help accessing data.
This work was supported by the NASA Solar System Exploration Research
Virtual Institute, through the Dynamic Response of the Environment at
Asteroids, the Moon, and moons of Mars (DREAM2) team. Andrew R. Poppe
acknowledges support from NASA's Lunar Advanced Science and Exploration
Research program, grant NNX13AJ97G. The data used in this paper are
available through the NASA Space Science Data Coordinated Archive
(nssdc.gsfc.nasa.gov).
NR 42
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN
PY 2017
VL 44
IS 1
BP 79
EP 87
DI 10.1002/2016GL071457
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA EK5GM
UT WOS:000393954900010
ER
PT J
AU Royer, EM
Ajello, JM
Holsclaw, GM
West, RA
Esposito, LW
Bradley, ET
AF Royer, E. M.
Ajello, J. M.
Holsclaw, G. M.
West, R. A.
Esposito, L. W.
Bradley, E. T.
TI Cassini UVIS observations of Titan ultraviolet airglow intensity
dependence with solar zenith angle
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Titan; airglow; upper atmosphere; ultraviolet
AB The Cassini Ultraviolet Imaging Spectrometer (UVIS) observed the airglow (dayglow and nightglow) of Titan over a range of solar zenith angles (SZA) from 14 to 150 degrees on five separate observations obtained between 2008 and 2012. The modeling of the solar cycle normalized UVIS observations indicates that a Chapman layer function provides a satisfactory fit to the intensity of the EUV and FUV airglow molecular emissions of the N-2 Lyman-Birge-Hopfield band system (LBH a1gX1 Sigma g+) the Carroll-Yoshino band system (c41 Sigma u+X1 Sigma g+) and of several atomic multiplets of nitrogen (NI, II) as a function of SZA. This result shows that the strongest contribution to the Titan dayglow occurs by processes (photoelectrons and photodissociation) involving the solar EUV flux rather than magnetospheric particle precipitation that dominates emission excitation in the nightglow.
C1 [Royer, E. M.; Ajello, J. M.; Holsclaw, G. M.; Esposito, L. W.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[West, R. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Bradley, E. T.] Univ Cent Florida, Florida Space Inst, Orlando, FL 32816 USA.
RP Royer, EM (reprint author), Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
EM emilie.royer@lasp.colorado.edu
FU Cassini-Huygens Mission; NASA sponsored Cassini Data Analysis Program
FX This work was performed at the Laboratory for Atmospheric and Space
Physics (LASP) at the University of Colorado Boulder. We gratefully
acknowledge financial support through the Cassini-Huygens Mission and
the NASA sponsored Cassini Data Analysis Program. All data supporting
the conclusions of this paper are publicly available in the Planetary
Data System (PDS). We thank the anonymous reviewers for assisting in the
evaluation of this paper.
NR 27
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN
PY 2017
VL 44
IS 1
BP 88
EP 96
DI 10.1002/2016GL071756
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA EK5GM
UT WOS:000393954900011
ER
PT J
AU Zambon, F
Raponi, A
Tosi, F
De Sanctis, MC
McFadden, LA
Carrozzo, FG
Longobardo, A
Ciarniello, M
Krohn, K
Stephan, K
Palomba, E
Pieters, CM
Ammannito, E
Russell, CT
Raymond, CA
AF Zambon, F.
Raponi, A.
Tosi, F.
De Sanctis, M. C.
McFadden, L. A.
Carrozzo, F. G.
Longobardo, A.
Ciarniello, M.
Krohn, K.
Stephan, K.
Palomba, E.
Pieters, C. M.
Ammannito, E.
Russell, C. T.
Raymond, C. A.
TI Spectral analysis of Ahuna Mons from Dawn mission's visible-infrared
spectrometer
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Ahuna Mons; spectroscopy; DAWN; VIR; Ceres; carbonates
ID ASTEROID 1 CERES; REFLECTANCE SPECTROSCOPY; MINERALS; VESTA; WATER
AB Ahuna Mons is the highest mountain on Ceres. A unique complex in terms of size, shape, and morphology, Ahuna is bordered by flanks of the talus around its summit. Recent work by Ruesch et al. () based on Dawn's Framing Camera images shed light on the possible origin of Ahuna Mons. According to Ruesch et al. (2016), Ahuna Mons is formed by a volcanic process involving the ascent of cryomagma and extrusion onto the surface followed by dome development and subsequent spreading. Here we analyzed in detail the composition of Ahuna Mons, using data acquired by the visible and infrared spectrometer aboard Dawn. The spectral analysis reveals a relatively high abundance of carbonates and a nonhomogeneous variation in carbonate composition and abundance along Ahuna's flanks, associated with a lower amount of the Ceres's ubiquitous NH4-phyllosilicates over a large portion of the flanks. The grain size is coarser on the flanks than in the surrounding regions, suggesting the presence of fresher material, also compatible with a larger abundance of carbonates. Thermal variations are seen in Ahuna, supporting the evidence of different compactness of the surface regolith in specific locations. Results of the spectral analysis are consistent with a possible cryovolcanic origin which exposed fresher material that slid down on the flanks.
C1 [Zambon, F.; Raponi, A.; Tosi, F.; De Sanctis, M. C.; Carrozzo, F. G.; Longobardo, A.; Ciarniello, M.; Palomba, E.] INAF, Ist Astrofis & Planetol Spaziali, Rome, Italy.
[McFadden, L. A.] Goddard Space Flight Ctr, Greenbelt, MD USA.
[Krohn, K.; Stephan, K.] German Aerosp Ctr DLR, Inst Planetary Res, Berlin, Germany.
[Pieters, C. M.] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA.
[Ammannito, E.; Russell, C. T.] Univ Calif Los Angeles, Earth Planetary & Space Sci, Los Angeles, CA USA.
[Raymond, C. A.] NASA, Jet Prop Lab, Pasadena, CA USA.
[Raymond, C. A.] CALTECH, Pasadena, CA 91125 USA.
RP Zambon, F (reprint author), INAF, Ist Astrofis & Planetol Spaziali, Rome, Italy.
EM francesca.zambon@iaps.inaf.it
OI Tosi, Federico/0000-0003-4002-2434; Palomba,
Ernesto/0000-0002-9101-6774; Krohn, Katrin/0000-0001-8518-4985; Zambon,
Francesca/0000-0002-4190-6592
FU Italian Space Agency (ASI); Dawn Science, Instrument, and Operations
Teams; ASI; NASA
FX VIR is funded by the Italian Space Agency (ASI) and was developed under
the leadership of INAF-Istituto di Astrofisica e Planetologia Spaziale,
Rome, Italy. The instrument was built by Selex-Galileo, Florence, Italy.
The authors acknowledge the support of the Dawn Science, Instrument, and
Operations Teams. This work was supported by ASI and NASA. The data used
for this analysis are available at
http://sbn.psi.edu/pds/resource/dwncvir.html.
NR 34
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PI WASHINGTON
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SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN
PY 2017
VL 44
IS 1
BP 97
EP 104
DI 10.1002/2016GL071303
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA EK5GM
UT WOS:000393954900012
ER
PT J
AU Schaefer, LN
Wang, T
Escobar-Wolf, R
Oommen, T
Lu, Z
Kim, J
Lundgren, PR
Waite, GP
AF Schaefer, L. N.
Wang, T.
Escobar-Wolf, R.
Oommen, T.
Lu, Z.
Kim, J.
Lundgren, P. R.
Waite, G. P.
TI Three-dimensional displacements of a large volcano flank movement during
the May 2010 eruptions at Pacaya Volcano, Guatemala
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Pacaya Volcano; three-dimensional (3-D) displacements; pixel offsets;
synthetic aperture radar (SAR); volcano instability
ID SURFACE DEFORMATION; DIKE INTRUSION; INTERFEROMETRY; EARTHQUAKE;
KILAUEA; SPACE
AB Although massive flank failure is fairly common in the evolution of volcanoes, measurements of flank movement indicative of instability are rare. Here 3-D displacements from airborne radar amplitude images derived using an amplitude image pixel offset tracking technique show that the west and southwest flanks of Pacaya Volcano in Guatemala experienced large (similar to 4m), discrete landsliding that was ultimately aborted. Pixel offset tracking improved measurement recovery by nearly 50% over classic interferometric synthetic aperture radar techniques, providing unique measurements at the event. The 3-D displacement field shows that the flank moved coherently downslope along a complex failure surface involving both rotational and along-slope movement. Notably, the lack of continuous movement of the slide in the years leading up to the event emphasizes that active movement should not always be expected at volcanoes for which triggering factors (e.g., magmatic intrusions and eruptions) could precipitate sudden major flank instability.
C1 [Schaefer, L. N.; Escobar-Wolf, R.; Oommen, T.; Waite, G. P.] Michigan Technol Univ, Dept Geol & Min Engn & Sci, Houghton, MI 49931 USA.
[Wang, T.; Lu, Z.; Kim, J.] Southern Methodist Univ, Roy M Huffington Dept Earth Sci, Dallas, TX USA.
[Lundgren, P. R.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Schaefer, LN (reprint author), Michigan Technol Univ, Dept Geol & Min Engn & Sci, Houghton, MI 49931 USA.
EM lnschaef@mtu.edu
OI Kim, Jin-Woo/0000-0002-9097-2465; Wang, Teng/0000-0003-3729-0139;
Schaefer, Lauren/0000-0003-3216-7983
FU NASA Earth and Space Science Fellowships Program [NNX13AO50H]; NASA
Earth Surface and Interior Program [NNX14AQ95G]; Shuler-Foscue Endowment
at Southern Methodist University
FX L.S. acknowledges support provided by the NASA Earth and Space Science
Fellowships Program (NNX13AO50H). T.W., J.W.K., and Z.L. acknowledge
support from the NASA Earth Surface and Interior Program (NNX14AQ95G)
and the Shuler-Foscue Endowment at Southern Methodist University. Raw
UAVSAR (Uninhibited Aerial Vehicle Synthetic Aperture Radar) data were
provided by the NASA Jet Propulsion Laboratory-California Institute of
Technology. We thank Yang Zhang for her assistance in providing SLC
images. PALSAR data from the ALOS-1 satellite mission operated by the
Japanese Aerospace Exploration Agency (JAXA) were used under the terms
and conditions of the Western North America Interferometric Synthetic
Aperture Radar Consortium (WInSAR). DInSAR was processed using Gamma.
PSI was processed using StaMPS. MATLAB functions to detect point-like
targets in SAR images are available upon request. We thank Francisco
Delgado and an anonymous reviewer for their help in improving this
manuscript.
NR 38
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PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN
PY 2017
VL 44
IS 1
BP 135
EP 142
DI 10.1002/2016GL071402
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA EK5GM
UT WOS:000393954900017
ER
PT J
AU Behrangi, A
Gardner, AS
Reager, JT
Fisher, JB
AF Behrangi, Ali
Gardner, Alex S.
Reager, John T.
Fisher, Joshua B.
TI Using GRACE to constrain precipitation amount over cold mountainous
basins
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE precipitation; satellite; mountain; GRACE; GPCP; cold region
ID GLOBAL PRECIPITATION; EVAPOTRANSPIRATION; PROJECT; SYSTEM; ALGORITHM;
PRODUCTS
AB Despite the importance for hydrology and climate-change studies, current quantitative knowledge on the amount and distribution of precipitation in mountainous and high-elevation regions is limited due to instrumental and retrieval shortcomings. Here by focusing on two large endorheic basins in High Mountain Asia, we show that satellite gravimetry (Gravity Recovery and Climate Experiment (GRACE)) can be used to provide an independent estimate of monthly accumulated precipitation using mass balance equation. Results showed that the GRACE-based precipitation estimate has the highest agreement with most of the commonly used precipitation products in summer, but it deviates from them in cold months, when the other products are expected to have larger errors. It was found that most of the products capture about or less than 50% of the total precipitation estimated using GRACE in winter. Overall, Global Precipitation Climatology Project (GPCP) showed better agreement with GRACE estimate than other products. Yet on average GRACE showed similar to 30% more annual precipitation than GPCP in the study basins. In basins of appropriate size with an absence of dense ground measurements, as is a typical case in cold mountainous regions, we find GRACE can be a viable alternative to constrain monthly and seasonal precipitation estimates from other remotely sensed precipitation products that show large bias.
C1 [Behrangi, Ali; Gardner, Alex S.; Reager, John T.; Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Behrangi, A (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Ali.Behrangi@jpl.nasa.gov
OI Gardner, Alex/0000-0002-8394-8889
FU National Aeronautics and Space Administration; NASA GRACE; NASA GRACE-FO
[NNH15ZDA001N-GRACE]; NASA Energy and Water Cycle Study
[NNH13ZDA001N-NEWS]
FX We thank Terry Kubar of UCLA for discussion about meteorology of the
study area. Data sets used in this study were collected from various
sources: The latest version of daily GPCP (V2.1) from Goddard Earth
Sciences Data and Information Services Center (GES DISC), GPCC Full Data
Reanalysis version 7.0 at 1 degrees x1 degrees resolution from
ftp://ftp.dwd.de/pub/data/gpcc/html/download_gate.html, GRACE total
water storage from http://grace.jpl.nasa.gov, TRMM products from GES
DISC, APHRODITE from the APHRODITE project
http://www.chikyu.ac.jp/precip/, and CloudSat products are obtained from
CloudSat data processing center:
http://www.cloudsat.cira.colostate.edu/data-products. The research
described in this paper was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration. Financial support was
also made available from NASA GRACE and GRACE-FO (NNH15ZDA001N-GRACE)
and NASA Energy and Water Cycle Study (NNH13ZDA001N-NEWS) awards.
Government sponsorship is acknowledged.
NR 60
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PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN
PY 2017
VL 44
IS 1
BP 219
EP 227
DI 10.1002/2016GL071832
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA EK5GM
UT WOS:000393954900026
ER
PT J
AU Ohlmann, JC
Molemaker, MJ
Baschek, B
Holt, B
Marmorino, G
Smith, G
AF Ohlmann, J. C.
Molemaker, M. J.
Baschek, B.
Holt, B.
Marmorino, G.
Smith, G.
TI Drifter observations of submesoscale flow kinematics in the coastal
ocean
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE submesoscale; Lagrangian; kinematics
ID SOUTHERN CALIFORNIA BIGHT; GULF-OF-MEXICO; LAGRANGIAN OBSERVATIONS;
CURRENT SYSTEM; PART I; MESOSCALE; SURFACE; TRANSITION; VORTICITY;
MOTION
AB Fronts and eddies identified with aerial guidance are seeded with drifters to quantify submesoscale flow kinematics. The Lagrangian observations show mean divergence and vorticity values that can exceed 5 times the Coriolis frequency. Values are the largest observed in the field to date and represent an extreme departure from geostrophic dynamics. The study also quantifies errors and biases associated with Lagrangian observations of the underlying velocity strain tensor. The greatest error results from undersampling, even with a large number of drifters. A significant bias comes from inhomogeneous sampling of convergent regions that accumulate drifters within a few hours of deployment. The study demonstrates a Lagrangian sampling paradigm for targeted submesoscale structures over a broad range of scales and presents flow kinematic values associated with vertical velocities O(10)mh(-1) that can have profound implications on ocean biogeochemistry.
C1 [Ohlmann, J. C.] Univ Calif Santa Barbara, Earth Res Inst, Santa Barbara, CA 93106 USA.
[Molemaker, M. J.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
[Baschek, B.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
[Baschek, B.] Helmholtz Zentrum Geesthacht, Inst Coastal Res, Geesthacht, Germany.
[Holt, B.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Marmorino, G.; Smith, G.] Naval Res Lab, Washington, DC 20375 USA.
RP Ohlmann, JC (reprint author), Univ Calif Santa Barbara, Earth Res Inst, Santa Barbara, CA 93106 USA.
EM carter@eri.ucsb.edu
FU National Aeronautics and Space Administration [NASA: SB110079]; National
Oceanic and Atmospheric Administration (NOAA) [NA10OAR4320156]; Office
of Naval Research (ONR) [N000141210105, N00014141062, 72-9201, 72-1C02]
FX The authors wish to acknowledge the Southern California Marine Institute
for use of their marine facilities. Discussions with Denny Kirwan and
Baylor Fox-Kemper helped shape the study. The LAPCOD 2015 meeting
facilitated these conversations. Support for this work comes from the
National Aeronautics and Space Administration (NASA: SB110079), the
National Oceanic and Atmospheric Administration (NOAA; NA10OAR4320156),
and the Office of Naval Research (ONR; N000141210105, N00014141062,
72-9201 and 72-1C02). Data used in the study are available from the
authors.
NR 38
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U1 0
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN
PY 2017
VL 44
IS 1
BP 330
EP 337
DI 10.1002/2016GL071537
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA EK5GM
UT WOS:000393954900039
ER
PT J
AU Garfinkel, CI
Son, SW
Song, K
Aquila, V
Oman, LD
AF Garfinkel, Chaim I.
Son, Seok-Woo
Song, Kanghyun
Aquila, Valentina
Oman, Luke D.
TI Stratospheric variability contributed to and sustained the recent hiatus
in Eurasian winter warming
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE hiatus; stratosphere-troposphere coupling; Eurasian temperature
ID POLAR VORTEX; NORTHERN-HEMISPHERE; TEMPERATURE TRENDS; CMIP5 MODELS;
IN-SITU; WEATHER; CLIMATE; TROPOSPHERE; FORECASTS; PACIFIC
AB The recent hiatus in global-mean surface temperature warming was characterized by a Eurasian winter cooling trend, and the cause(s) for this cooling is unclear. Here we show that the observed hiatus in Eurasian warming was associated with a recent trend toward weakened stratospheric polar vortices. Specifically, by calculating the change in Eurasian surface air temperature associated with a given vortex weakening, we demonstrate that the recent trend toward weakened polar vortices reduced the anticipated Eurasian warming due to increasing greenhouse gas concentrations. Those model integrations whose stratospheric vortex evolution most closely matches that in reanalysis data also simulate a hiatus. While it is unclear whether the recent weakening of the midwinter stratospheric polar vortex was forced, a properly configured model can simulate substantial deviations of the polar vortex on decadal timescales and hence such hiatus events, implying that similar hiatus events may recur even as greenhouse gas concentrations rise.
C1 [Garfinkel, Chaim I.] Hebrew Univ Jerusalem, Fredy & Nadine Herrmann Inst Earth Sci, Jerusalem, Israel.
[Son, Seok-Woo; Song, Kanghyun] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul, South Korea.
[Aquila, Valentina] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[Oman, Luke D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Garfinkel, CI (reprint author), Hebrew Univ Jerusalem, Fredy & Nadine Herrmann Inst Earth Sci, Jerusalem, Israel.
EM chaim.garfinkel@mail.huji.ac.il
OI garfinkel, chaim/0000-0001-7258-666X
FU Israel Science Foundation [1558/14]; European Research Council under the
European Union [677756]; Korea Meteorological Administration Research
and Development Program [KMIPA 2015-2094, KMIPA 2015-2100]; NASA MAP
program
FX C.I.G. was supported by the Israel Science Foundation (grant 1558/14)
and by a European Research Council starting grant under the European
Unions Horizon 2020 research and innovation programme (grant agreement
677756). S.W.S. and K.H.S. are funded by the Korea Meteorological
Administration Research and Development Program under grant KMIPA
2015-2094 and KMIPA 2015-2100. We thank the two anonymous reviewers for
their helpful comments, those involved in model development at
GSFC-GMAO, and support by the NASA MAP program. High-performance
computing resources were provided by the NASA Center for Climate
Simulation (NCCS). Correspondence and requests for data should be
addressed to C.I.G. (email: chaim.garfinkel@mail.huji.ac.il).
NR 49
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PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN
PY 2017
VL 44
IS 1
BP 374
EP 382
DI 10.1002/2016GL072035
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA EK5GM
UT WOS:000393954900044
PM 28356606
ER
PT J
AU Yang, YM
Verkhoglyadova, O
Mlynczak, MG
Mannucci, AJ
Meng, X
Langley, RB
Hunt, LA
AF Yang, Yu-Ming
Verkhoglyadova, Olga
Mlynczak, Martin G.
Mannucci, Anthony J.
Meng, Xing
Langley, Richard B.
Hunt, Linda A.
TI Satellite-based observations of tsunami-induced mesosphere airglow
perturbations
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE airglow; tsunami; SABER; space-based; mesosphere
ID ATMOSPHERIC GRAVITY-WAVES; IONOSPHERIC DISTURBANCES; LOWER THERMOSPHERE;
SABER EXPERIMENT; TOHOKU; OXYGEN; INTENSITIES; RESPONSES; MIDDLE; O-2
AB Tsunami-induced airglow emission perturbations were retrieved by using space-based measurements made by the Sounding of the Atmosphere using Broad-band Emission Radiometry (SABER) instrument on board the Thermosphere-Ionosphere-Mesosphere Energetics Dynamics spacecraft. At and after the time of the Tohoku-Oki earthquake on 11 March 2011, and the Chile earthquake on 16 September 2015, the spacecraft was performing scans over the Pacific Ocean. Significant (similar to 10% relative to the ambient emission profiles) and coherent nighttime airglow perturbations were observed in the mesosphere following Sounding of the Atmosphere using Broad-band Emission Radiometry limb scans intercepting tsunami-induced atmospheric gravity waves. Simulations of emission variations are consistent with the physical characteristics of the disturbances at the locations of the corresponding SABER scans. Airglow observations and model simulations suggest that atmospheric neutral density and temperature perturbations can lead to the observed amplitude variations and multipeak structures in the emission profiles. This is the first time that airglow emission rate perturbations associated with tsunamis have been detected with space-based measurements.
C1 [Yang, Yu-Ming; Verkhoglyadova, Olga; Mannucci, Anthony J.; Meng, Xing] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Mlynczak, Martin G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Langley, Richard B.] Univ New Brunswick, Dept Geodesy & Geomat Engn, Fredericton, NB, Canada.
[Hunt, Linda A.] Sci Syst & Applicat Inc, Hampton, VA USA.
RP Yang, YM (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Oscar.Yang@jpl.nasa.gov
OI Hunt, Linda/0000-0002-5330-541X
NR 42
TC 1
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U1 1
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN
PY 2017
VL 44
IS 1
BP 522
EP 532
DI 10.1002/2016GL070764
PG 11
WC Geosciences, Multidisciplinary
SC Geology
GA EK5GM
UT WOS:000393954900060
ER
PT J
AU Wood, JD
Griffis, TJ
Baker, JM
Frankenberg, C
Verma, M
Yuen, K
AF Wood, Jeffrey D.
Griffis, Timothy J.
Baker, John M.
Frankenberg, Christian
Verma, Manish
Yuen, Karen
TI Multiscale analyses of solar-induced florescence and gross primary
production
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE OCO-2; tall tower fluxes; SIF; GPP; eddy covariance
ID INDUCED CHLOROPHYLL FLUORESCENCE; TERRESTRIAL GROSS; ECOSYSTEM
RESPIRATION; ATMOSPHERE EXCHANGE; EDDY COVARIANCE; TALL TOWER;
PHOTOSYNTHESIS; SPACE; MODELS; FLUXES
AB Solar-induced fluorescence (SIF) has shown great promise for probing spatiotemporal variations in terrestrial gross primary production (GPP), the largest component flux of the global carbon cycle. However, scale mismatches between SIF and ground-based GPP have posed challenges toward fully exploiting these data. We used SIF obtained at high spatial sampling rates and resolution by NASA's Orbiting Carbon Observatory-2 satellite to elucidate GPP-SIF relationships across space and time in the U.S. Corn Belt. Strong linear scaling functions (R(2)0.79) that were consistent across instantaneous to monthly time scales were obtained for corn ecosystems and for a heterogeneous landscape based on tall tower observations. Although the slope of the corn function was similar to 56% higher than for the landscape, SIF was similar for corn (C-4) and soybean (C-3). Taken together, there is strong observational evidence showing robust linear GPP-SIF scaling that is sensitive to plant physiology but insensitive to the spatial or temporal scale.
C1 [Wood, Jeffrey D.; Griffis, Timothy J.; Baker, John M.] Univ Minnesota, Dept Soil Water & Climate, St Paul, MN 55108 USA.
[Wood, Jeffrey D.] Univ Missouri, Sch Nat Resources, Columbia, MO 65211 USA.
[Baker, John M.] ARS, Soil & Water Res Unit, USDA, St Paul, MN USA.
[Frankenberg, Christian] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Frankenberg, Christian; Yuen, Karen] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Verma, Manish] Univ Michigan, Consulting Stat Comp & Analyt Res, Ann Arbor, MI 48109 USA.
RP Wood, JD (reprint author), Univ Minnesota, Dept Soil Water & Climate, St Paul, MN 55108 USA.; Wood, JD (reprint author), Univ Missouri, Sch Nat Resources, Columbia, MO 65211 USA.
EM woodjd@missouri.edu
OI Wood, Jeffrey/0000-0001-6422-2882; Verma, Manish/0000-0002-0722-8732
FU United States Department of Agriculture [USDA-NIFA2013-67019-21364];
Minnesota Corn Research and Promotion Council [4101-15SP]; U.S.
Department of Energy's Office of Science; University of Minnesota
Supercomputing Institute; U.S. Department of Energy [4000150689]
FX The authors would like to acknowledge funding support provided by the
United States Department of Agriculture (USDA-NIFA2013-67019-21364) and
the Minnesota Corn Research and Promotion Council (4101-15SP). Funding
for this AmeriFlux core site was provided by the U.S. Department of
Energy's Office of Science. We are grateful to the University of
Minnesota Supercomputing Institute for partial support of this work.
J.D.W. acknowledges U.S. Department of Energy support for the University
of Missouri (subcontract 4000150689). Corn GPP data are available from
AmeriFlux (http://ameriflux.lbl.gov/), and tall tower data are archived
at http://www.biometeorology.umn.edu/. The solar-induced fluorescence
data (v. B7101r) were produced by the OCO-2 project at the Jet
Propulsion Laboratory, California Institute of Technology, and obtained
from the OCO-2 data archive maintained at the NASA Goddard Earth Science
Data and Information Services Center. The MODIS FPAR/LAI (MCD15A2 v5),
GPP (MYD17A2H v6), and EVI/NDVI (MYD13Q1 v5) were obtained from the Land
Processes DAAC. The authors declare no conflict of interest.
NR 40
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U1 3
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN
PY 2017
VL 44
IS 1
BP 533
EP 541
DI 10.1002/2016GL070775
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA EK5GM
UT WOS:000393954900061
ER
PT J
AU Hockman, BJ
Frick, A
Reid, RG
Nesnas, IAD
Pavone, M
AF Hockman, Benjamin J.
Frick, Andreas
Reid, Robert G.
Nesnas, Issa A. D.
Pavone, Marco
TI Design, Control, and Experimentation of Internally-Actuated Rovers for
the Exploration of Low-gravity Planetary Bodies
SO JOURNAL OF FIELD ROBOTICS
LA English
DT Article
ID MISSION
AB This paper discusses the design, control, and experimentation of internally-actuated rovers for the exploration of low-gravity (micro-g to milli-g) planetary bodies, such as asteroids, comets, or small moons. The rover is actuated by spinning three internal flywheels, which allows all subsystems to be packaged in one sealed enclosure and enables the platform to be minimalistic, thereby reducing its cost. By controlling the spin rate of the flywheels, the rover can achieve large surface coverage by attitude-controlled hops, fine mobility by tumbling, and coarse instrument pointing by changing the orientation relative to the ground. We first discuss the dynamics of such rovers, their control, and key design features (e.g., flywheel shape and orientation, geometry of external spikes, and system engineering aspects). We then discuss the design and control of a first-of-a-kind test bed that enables the accurate emulation of a microgravity environment for mobility experiments, which consists of a three-degree-of-freedom gimbal attached to an actively controlled gantry crane. Finally, we present experimental results on the test bed that provide key insights for rover control and validate our theoretical analysis. (C) 2016 Wiley Periodicals, Inc.
C1 [Hockman, Benjamin J.] Stanford Univ, Dept Mech Engn, Stanford, CA 94305 USA.
[Frick, Andreas; Reid, Robert G.; Nesnas, Issa A. D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Pavone, Marco] Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA.
RP Pavone, M (reprint author), Stanford Univ, Dept Aeronaut & Astronaut, Stanford, CA 94305 USA.
EM bhockman@stanford.edu; andreas.frick@jpl.nasa.gov;
robert.g.reid@jpl.nasa.gov; issa.a.nesnas@jpl.nasa.gov;
pavone@stanford.edu
FU NASA under Innovative Advanced Concepts program [NNX14AT49G]
FX The research described in this paper is supported by NASA under the
Innovative Advanced Concepts program (Grant No. NNX14AT49G). The authors
wish to acknowledge insightful discussions with Dr. J. C. Castillo
(JPL), Dr. C. Zuffada (JPL), Dr. T. Cwik (JPL), Dr. J. Zmuidzinas (JPL),
and B. Wilcox (JPL). Government sponsorship acknowledged.
NR 26
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1556-4959
EI 1556-4967
J9 J FIELD ROBOT
JI J. Field Robot.
PD JAN
PY 2017
VL 34
IS 1
SI SI
BP 5
EP 24
DI 10.1002/rob.21656
PG 20
WC Robotics
SC Robotics
GA EK1FR
UT WOS:000393671700002
ER
PT J
AU Landt, H
Ward, MJ
Balokovic, M
Kynoch, D
Storchi-Bergmann, T
Boisson, C
Done, C
Schimoia, J
Stern, D
AF Landt, H.
Ward, M. J.
Balokovic, M.
Kynoch, D.
Storchi-Bergmann, T.
Boisson, C.
Done, C.
Schimoia, J.
Stern, D.
TI On the black hole mass of the gamma-ray emitting narrow-line Seyfert 1
galaxy 1H 0323+342
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE quasars: emission lines; quasars: individual: 1H 0323+342; galaxies:
Seyfert-infrared: galaxies; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; RADIUS-LUMINOSITY RELATIONSHIP; X-RAY;
EMISSION-LINE; HOST-GALAXY; REGION; VARIABILITY; TELESCOPE; SPECTRUM;
SAMPLE
AB Narrow-line Seyfert 1 galaxies have been identified by the Fermi Gamma-Ray Space Telescope as a rare class of gamma-ray emitting active galactic nuclei. The lowest redshift candidate among them is the source 1H 0323+342. Here we present quasi-simultaneous Gemini near-infrared and Keck optical spectroscopy for it, from which we derive a black hole mass based on both the broad Balmer and Paschen emission lines. We supplement these observations with a Nuclear Spectroscopic Telescope Array X-ray spectrum taken about two years earlier, from which we constrain the black hole mass based on the short time-scale spectral variability. Our multiwavelength observations suggest a black hole mass of similar to 2 x 10(7) M-circle dot, which agrees well with previous estimates. We build the spectral energy distribution and show that it is dominated by the thermal and reprocessed emission from the accretion disc rather than the non-thermal jet component. A detailed spectral fitting with the energy-conserving accretion disc model of Done et al. constrains the Eddington ratio to L/L-Edd similar to 0.5 for a (non-rotating) Schwarzschild black hole and to L/L-Edd similar to 1 for a Kerr black hole with dimensionless spin of a* = 0.8. Higher spin values and so higher Eddington ratios are excluded, since they would strongly overpredict the observed soft X-ray flux.
C1 [Landt, H.; Ward, M. J.; Kynoch, D.; Done, C.] Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England.
[Balokovic, M.] CALTECH, Cahill Ctr Astron & Astrophys, 1216 E Calif Blvd, Pasadena, CA 91125 USA.
[Storchi-Bergmann, T.; Schimoia, J.] Univ Fed Rio Grande do Sul, Dept Astron, IF, CP 15051, BR-91501970 Porto Alegre, RS, Brazil.
[Boisson, C.] PSL Res Univ Paris, Univ Paris Diderot, CNRS, LUTH,Observ Paris, 5 Pl Jules Janssen, F-92195 Meudon, France.
[Done, C.] Japan Aerosp Explorat Agcy, ISAS, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan.
[Stern, D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Landt, H (reprint author), Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England.
EM hermine.landt@durham.ac.uk
FU Observatoire de Paris; European Union [267209]; National Aeronautics and
Space Administration (NASA) Headquarters under the NASA Earth and Space
Science Fellowship Program [NNX14AQ07H]; STFC studentship; W.M. Keck
Foundation; NASA
FX MJW and DK would like to thank the Observatoire de Paris for its
hospitality and support during some months of this work in the framework
of the Laboratoire Europeen Associe (LEA) ELGA (European Laboratory for
Gamma-ray Astronomy). We thank Maria Marcha for kindly making their
optical spectrum available to us in electronic format. HL is supported
by a European Union CO-FUND/Durham Junior Research Fellowship (under EU
grant agreement number 267209). MB acknowledges support from the
National Aeronautics and Space Administration (NASA) Headquarters under
the NASA Earth and Space Science Fellowship Program grant no.
NNX14AQ07H. DK acknowledges the receipt of an STFC studentship. This
work is partly based on observations obtained at the Gemini Observatory,
which is operated by the Association of Universities for Research in
Astronomy, Inc., under a cooperative agreement with the NSF on behalf of
the Gemini partnership: the National Science Foundation (United States),
the National Research Council (Canada), CONICYT (Chile), the Australian
Research Council (Australia), Ministerio da Ciencia, Tecnologia e
Inovacao (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion
Productiva (Argentina). Some of the data presented herein were obtained
at the W.M. Keck Observatory, which is operated as a scientific
partnership among the California Institute of Technology, the University
of California and NASA. The Observatory was made possible by the
generous financial support of the W.M. Keck Foundation. This work made
use of data from the NuSTAR mission, a project led by the California
Institute of Technology, managed by the Jet Propulsion Laboratory and
funded by NASA.
NR 64
TC 0
Z9 0
U1 2
U2 2
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN
PY 2017
VL 464
IS 3
BP 2565
EP 2576
DI 10.1093/mnras/stw2447
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EK0WK
UT WOS:000393647600004
ER
PT J
AU Bottom, M
Wallace, JK
Bartos, RD
Shelton, JC
Serabyn, E
AF Bottom, M.
Wallace, J. K.
Bartos, R. D.
Shelton, J. C.
Serabyn, E.
TI Speckle suppression and companion detection using coherent differential
imaging
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE instrumentation: high angular resolution; techniques: image processing;
techniques: interferometric; brown dwarfs; planetary systems
ID CORONAGRAPHIC PHASE-DIVERSITY; ADAPTIVE OPTICS; VORTEX CORONAGRAPH;
BROWN DWARF; CONTRAST; SUBTRACTION; TELESCOPE; STARS
AB Residual speckles due to aberrations arising from optical errors after the split between the wavefront sensor and the science camera path are the most significant barriers to imaging extrasolar planets. While speckles can be suppressed using the science camera in conjunction with the deformable mirror, this requires knowledge of the phase of the electric field in the focal plane. We describe a method which combines a coronagraph with a simple phase-shifting interferometer to measure and correct speckles in the full focal plane. We demonstrate its initial use on the Stellar Double Coronagraph at the Palomar Observatory. We also describe how the same hardware can be used to distinguish speckles from true companions by measuring the coherence of the optical field in the focal plane. We present results observing the brown dwarf HD49197b with this technique, demonstrating the ability to detect the presence of a companion even when it is buried in the speckle noise, without the use of any standard `calibration' techniques. We believe this is the first detection of a substellar companion using the coherence properties of light.
C1 [Bottom, M.] CALTECH, MC 249-17,1200 E Calif Blvd, Pasadena, CA 91125 USA.
[Wallace, J. K.; Bartos, R. D.; Shelton, J. C.; Serabyn, E.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Bottom, M (reprint author), CALTECH, MC 249-17,1200 E Calif Blvd, Pasadena, CA 91125 USA.
EM mbottom@caltech.edu
FU NASA Space Technology Research Fellowship [NNX13AN42H]
FX We are very pleased to acknowledge the Palomar Observatory staff for
their support. During the course of this work, MB was supported by a
NASA Space Technology Research Fellowship, grant NNX13AN42H. Part of
this work was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with the National Aeronautics
and Space Administration (NASA).
NR 26
TC 0
Z9 0
U1 1
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN
PY 2017
VL 464
IS 3
BP 2937
EP 2951
DI 10.1093/mnras/stw2544
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EK0WK
UT WOS:000393647600034
ER
PT J
AU Doyle, TF
Howell, SB
Petit, V
Lepine, S
AF Doyle, T. F.
Howell, S. B.
Petit, V.
Lepine, S.
TI DA white dwarfs in the Kepler field
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE techniques: photometric; techniques: spectroscopic; white dwarfs
ID ZZ-CETI STARS; OPTICAL SPECTROSCOPY; INSTABILITY STRIP; COMPACT
PULSATORS; DISCOVERY; CATALOG; LINES
AB We present 16 new, and confirm 7 previously identified, DA white dwarfs in the Kepler field through ground-based spectroscopy with the Hale 200 '', Kitt Peak 4-m, and Bok 2.3-m telescopes. Using atmospheric models, we determine their effective temperatures and surface gravities to constrain their position with respect to the ZZ Ceti (DA pulsator) instability strip, and look for the presence or absence of pulsation with Kepler's unprecedented photometry. Our results are as follows. (i) From our measurements of temperature and surface gravity, 12 of the 23 DA white dwarfs from this work fall well outside of the instability strip. The Kepler photometry available for 11 of these WDs allows us to confirm that none are pulsating. One of these 11 happens to be a presumed binary, KIC 11604781, with a period of similar to 5 d. (ii) The remaining 11 DA white dwarfs are instability strip candidates, potentially falling within the current, empirical instability strip, after accounting for uncertainties. These WDs will help constrain the strip's location further, as eight are near the blue edge and three are near the red edge of the instability strip. Four of these WDs do not have Kepler photometry, so ground-based photometry is needed to determine the pulsation nature of these white dwarfs. The remaining seven have Kepler photometry available, but do not show any periodicity on typical WD pulsation time-scales.
C1 [Doyle, T. F.; Petit, V.] Florida Inst Technol, 150 W Univ Blvd, Melbourne, FL 32907 USA.
[Howell, S. B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Lepine, S.] Georgia State Univ, 33 Gilmer St SE, Atlanta, GA 30302 USA.
RP Doyle, TF (reprint author), Florida Inst Technol, 150 W Univ Blvd, Melbourne, FL 32907 USA.; Howell, SB (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM trisha.mizusawa@gmail.com; steve.b.howell@nasa.gov
FU NASA [NAS5-26555]; NASA Office of Space Science [NNX13AC07G]; NASA
Science Mission directorate
FX White dwarf models were provided by Dr. Detlev Koester at the University
of Kiel in Germany. Balmer/Lyman lines in the models were calculated
with the modified Stark broadening profiles of Tremblay & Bergeron
(2009), kindly made available by the authors. Some of the data presented
in this paper were obtained from the Mikulski Archive for Space
Telescopes (MAST). STScI is operated by the Association of Universities
for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support
for MAST for non-HST data is provided by the NASA Office of Space
Science via grant NNX13AC07G and by other grants and contracts. This
paper includes data collected by the Kepler mission. Funding for the
Kepler mission is provided by the NASA Science Mission directorate. This
research has made use of the NASA Exoplanet Archive, which is operated
by the California Institute of Technology, under contract with the
National Aeronautics and Space Administration under the Exoplanet
Exploration Program. This research is based on observations at Kitt Peak
National Observatory, National Optical Astronomy Observatory, which is
operated by the Association of Universities for Research in Astronomy
(AURA) under cooperative agreement with the National Science Foundation.
This paper made use of the facilities at the Kitt Peak National
Observatory and the Palomar Observatory. The authors would like to thank
the telescope operators and staff at both of these institutions. We
thank Mark Everett for help with the Mayall observations and Jay Holberg
and David Sing for help with the Bok observations.
NR 28
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U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN
PY 2017
VL 464
IS 3
BP 3464
EP 3485
DI 10.1093/mnras/stw2490
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EK0WK
UT WOS:000393647600071
ER
PT J
AU Acero, F
Katsuda, S
Ballet, J
Petre, R
AF Acero, Fabio
Katsuda, Satoru
Ballet, Jean
Petre, Robert
TI Measurement of the X-ray proper motion in the south-east rim of
RXJ1713.7-3946
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: supernova remnants; ISM: individual objects: RXJ1713.7-3946;
X-rays: ISM
ID REMNANT RX J1713.7-3946; CORE-COLLAPSE SUPERNOVAE; GAMMA-RAY;
ACCELERATION; EMISSION; GAS
AB We report on the first proper motion measurement in the supernova remnant RXJ1713.7-3946 using the XMM-Newton X-ray telescope on a 13 yr time interval. This expansion measurement is carried out in the south-east region of the remnant, where two sharp filament structures are observed. For the outermost filament, the proper motion is 0.75(-0.06)(+0.05) +/- 0.069(syst) arcsec yr(-1) which is equivalent to a shock speed of similar to 3500 km s(-1) at a distance of 1 kpc. In contrast with the bright north-west region, where the shock is interacting with the border of the cavity, the shock in the south-east region is probably expanding in the original ambient medium carved by the progenitor and can be used to derive the current density at the shock and the age of the remnant. In the case where the shock is evolving in a wind profile (rho proportional to r(-s), s = 2) or in a uniform medium (s = 0), we estimate an age of similar to 2300 yr and similar to 1800 yr respectively for an ejecta power-law index of n = 9. The specific case of an ejecta power-law index of n = 7, and s = 0, yields an age of similar to 1500 yr, which would reconcile RXJ1713.7-3946 with the historical records of SN 393. In all scenarios, we derive similar upstream densities of the order of 0.01 cm(-3), compatible with the lack of thermal X-rays from the shocked ambient medium.
C1 [Acero, Fabio; Ballet, Jean] Univ Paris Diderot, CEA Saclay, Lab AIM, IRFU SAp,CEA DRF,CNRS, Bat 709, Gif Sur Yvette, France.
[Katsuda, Satoru] Chuo Univ, Fac Sci & Engn, Dept Phys, Bunkyo Ku, 1-13-27 Kasuga, Tokyo 1128551, Japan.
[Petre, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Acero, F (reprint author), Univ Paris Diderot, CEA Saclay, Lab AIM, IRFU SAp,CEA DRF,CNRS, Bat 709, Gif Sur Yvette, France.
EM fabio.acero@cea.fr
NR 19
TC 0
Z9 0
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JAN
PY 2017
VL 597
AR A106
DI 10.1051/0004-6361/201629618
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EI3LS
UT WOS:000392392900130
ER
PT J
AU Giannini, E
Schmidt, RW
Wambsganss, J
Alsubai, K
Andersen, JM
Anguita, T
Bozza, V
Bramich, DM
Browne, P
Novati, SC
Damerdji, Y
Diehl, C
Dodds, P
Dominik, M
Elyiv, A
Fang, X
Jaimes, RF
Finet, F
Gerner, T
Gu, S
Hardis, S
Harpsoe, K
Hinse, TC
Hornstrup, A
Hundertmark, M
Jessen-Hansen, J
Jorgensen, UG
Juncher, D
Kains, N
Kerins, E
Korhonen, H
Liebig, C
Lund, MN
Lundkvist, MS
Maier, G
Mancini, L
Masi, G
Mathiasen, M
Penny, M
Proft, S
Rabus, M
Rahvar, S
Ricci, D
Scarpetta, G
Sahu, K
Schafer, S
Schonebeck, F
Skottfelt, J
Snodgrass, C
Southworth, J
Surdej, J
Tregloan-Reed, J
Vilela, C
Wertz, O
Zimmer, F
AF Giannini, E.
Schmidt, R. W.
Wambsganss, J.
Alsubai, K.
Andersen, J. M.
Anguita, T.
Bozza, V.
Bramich, D. M.
Browne, P.
Novati, S. Calchi
Damerdji, Y.
Diehl, C.
Dodds, P.
Dominik, M.
Elyiv, A.
Fang, X.
Jaimes, R. Figuera
Finet, F.
Gerner, T.
Gu, S.
Hardis, S.
Harpsoe, K.
Hinse, T. C.
Hornstrup, A.
Hundertmark, M.
Jessen-Hansen, J.
Jorgensen, U. G.
Juncher, D.
Kains, N.
Kerins, E.
Korhonen, H.
Liebig, C.
Lund, M. N.
Lundkvist, M. S.
Maier, G.
Mancini, L.
Masi, G.
Mathiasen, M.
Penny, M.
Proft, S.
Rabus, M.
Rahvar, S.
Ricci, D.
Scarpetta, G.
Sahu, K.
Schaefer, S.
Schoenebeck, F.
Skottfelt, J.
Snodgrass, C.
Southworth, J.
Surdej, J.
Tregloan-Reed, J.
Vilela, C.
Wertz, O.
Zimmer, F.
TI MiNDSTEp differential photometry of the gravitationally lensed quasars
WFI 2033-4723 and HE0047-1756: microlensing and a new time delay
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE gravitational lensing: micro; techniques: photometric; quasars: general
ID HAMBURG ESO SURVEY; BRIGHT QSOS; LENSING EXPERIMENT; IMAGE SUBTRACTION;
COLOR VARIATIONS; HE 0435-1223; COSMOGRAIL; REDSHIFT; GALAXY; FLUX
AB Aims. We present V and R photometry of the gravitationally lensed quasars WFI 2033-4723 and HE 0047-1756. The data were taken by the MiNDSTEp collaboration with the 1.54 m Danish telescope at the ESO La Silla observatory from 2008 to 2012.
Methods. Differential photometry has been carried out using the image subtraction method as implemented in the HOTPAnTS package, additionally using GALFIT for quasar photometry.
Results. The quasar WFI 2033-4723 showed brightness variations of order 0.5 mag in V and R during the campaign. The two lensed components of quasar HE 0047-1756 varied by 0.2-0.3 mag within five years. We provide, for the first time, an estimate of the time delay of component B with respect to A of Delta t = (7.6 +/- 1.8) days for this object. We also find evidence for a secular evolution of the magnitude difference between components A and B in both filters, which we explain as due to a long-duration microlensing event. Finally we find that both quasars WFI 2033-4723 and HE 0047-1756 become bluer when brighter, which is consistent with previous studies.
C1 [Giannini, E.; Finet, F.; Harpsoe, K.; Hornstrup, A.; Liebig, C.] Heidelberg Univ, Astronom Rechen Inst, Zentrum Astron, Monchhofstr 12-14, D-69120 Heidelberg, Germany.
[Mancini, L.; Rabus, M.] Qatar Environm & Energy Res Inst QEERI, Doha, Qatar.
[Kains, N.; Schaefer, S.] Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA.
[Liebig, C.; Masi, G.] Univ Copenhagen, Niels Bohr Inst, Oster Voldgade 5, DK-1350 Copenhagen, Denmark.
[Korhonen, H.; Proft, S.] Univ Copenhagen, Ctr Star & Planet Format, Oster Voldgade 5, DK-1350 Copenhagen, Denmark.
[Vilela, C.; Wertz, O.] Univ Andres Bello, Dept Ciencias Fis, Ave Republ 220, Santiago, Chile.
[Schaefer, S.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Juncher, D.; Maier, G.; Penny, M.] Univ Salerno, Dipartimento Fis ER Caianiello, Via Giovanni Paolo II 132, I-84084 Fisciano, SA, Italy.
[Surdej, J.] Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy.
[Masi, G.] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Penny, M.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Penny, M.; Scarpetta, G.] Open Univ, Dept Phys Sci, Ctr Elect Imaging, Milton Keynes MK7 6AA, Bucks, England.
[Bramich, D. M.; Harpsoe, K.; Proft, S.; Rabus, M.; Tregloan-Reed, J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rabus, M.] IIASS, Vietri Sul Mare, SA, Italy.
[Kains, N.] Univ Liege, Inst Astrophys & Geophys, Allee 6 Aout,Bat B5c, B-4000 Liege, Belgium.
[Mathiasen, M.] Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany.
[Alsubai, K.; Southworth, J.] Georg August Univ Gottingen, Inst Astrophys, Friedrich Hund Pl 1, D-37077 Gottingen, Germany.
[Giannini, E.; Anguita, T.; Damerdji, Y.; Dominik, M.] Subaru Telescope, Natl Astron Observ Japan, 650 North Aohoku Pl, Hilo, HI 96720 USA.
[Jorgensen, U. G.; Maier, G.; Mathiasen, M.] Ukrainian Acad Sci, Main Astron Observ, Friedrich Hund Pl 1, UA-03680 Kiev, Ukraine.
[Giannini, E.; Novati, S. Calchi; Kains, N.; Ricci, D.; Schaefer, S.; Southworth, J.] Aarhus Univ, Dept Phys Astron, Stellar Astrophys Ctr, Ny Munkegade 120, DK-8000 Aarhus C, Denmark.
[Anguita, T.; Diehl, C.; Harpsoe, K.; Lundkvist, M. S.; Rahvar, S.; Schaefer, S.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark.
[Jorgensen, U. G.] Ohio State Univ, Dept Astron, 140W 18th Ave, Columbus, OH 43210 USA.
[Bozza, V.; Hundertmark, M.; Surdej, J.] KASI, Daejeon 305348, South Korea.
[Wambsganss, J.; Jaimes, R. Figuera; Kerins, E.; Masi, G.] Tech Univ Denmark, Natl Space Inst, DK-2800 Lyngby, Denmark.
[Anguita, T.; Hornstrup, A.; Tregloan-Reed, J.; Vilela, C.] Univ Manchester, Jodrell Bank Ctr Astrophy, Manchester, Lancs, England.
[Kains, N.; Liebig, C.; Lund, M. N.] Ctr Backyard Astrophys, Bellatrix Astron Observ, Ceccano, FR, Italy.
[Kains, N.] Pontificia Univ Caolic Chile, Inst Astrofis, Fac Fis, Ctr Astro Ingn, Vicun Mackenna 4860, Santiago, Chile.
[Maier, G.] Sharif Univ Technol, Dept Phys, Tehran, Iran.
[Bramich, D. M.; Hardis, S.] Perimeter Inst Theoret Phys, 31 Caroline St N, Waterloo, ON N2L 2Y5, Canada.
[Fang, X.] Univ Nacl Autonoma Mexico, Observ Astron Nacl, Ensenada, BC 22860, Mexico.
[Kains, N.; Lundkvist, M. S.; Mathiasen, M.] Inst Astrofis Canarias, San Cristobal la Laguna 38205, Spain.
[Alsubai, K.; Lund, M. N.; Masi, G.] Space Telescope Sci Inst STScI, Pacific Grove, CA USA.
[Browne, P.; Harpsoe, K.; Korhonen, H.; Rahvar, S.] Open Univ, Dept Phys Sci, Planetary & Space Sci, Milton Keynes MK7 6AA, Bucks, England.
[Anguita, T.; Rabus, M.] Max Planck Inst Sonnensyst Forsch, Justus von Liebig Weg 3, D-37077 Gottingen, Germany.
[Fang, X.; Juncher, D.] Keele Univ, Astrophys Grp, Newcastle Lyme, Keele ST5 5BG, Staffs, England.
[Dominik, M.; Elyiv, A.; Harpsoe, K.; Juncher, D.; Rabus, M.] Chinese Acad Sci, Lab Struct & Evolut Celestial Objects, Kunming 650011, Peoples R China.
[Bozza, V.; Finet, F.; Hardis, S.; Juncher, D.; Ricci, D.; Schaefer, S.] NASA, Exoplanet Sci Inst, CALTECH, MS 100-22, Pasadena, MS 10022 USA.
[Hinse, T. C.; Juncher, D.; Masi, G.] Univ Bologna, Dipartimento Fis Astron, Viale Berti Pichat 6-2, I-40127 Bologna, Italy.
[Andersen, J. M.; Novati, S. Calchi; Hinse, T. C.; Scarpetta, G.] Millennium Inst Astrophys, Tenerife, Chile.
[Browne, P.; Dominik, M.; Hardis, S.; Hornstrup, A.; Southworth, J.; Vilela, C.] Univ Laguna, Dept Astrofis, San Cristobal la Laguna 38206, Spain.
[Alsubai, K.; Dodds, P.; Masi, G.; Ricci, D.] Armagh Observ, Coll Hill, BT61 9DG Armagh, North Ireland.
[Kains, N.; Maier, G.; Rahvar, S.; Schaefer, S.] Chinese Acad Sci, Yunnan Observ, Kunming 650216, Yunnan, Peoples R China.
RP Giannini, E (reprint author), Heidelberg Univ, Astronom Rechen Inst, Zentrum Astron, Monchhofstr 12-14, D-69120 Heidelberg, Germany.
EM emanuela@ari.uni-heidelberg.de
FU FONDECYT proyecto [11130630]; Ministry of Economy, Development, and
Tourism's Millennium Science Initiative [IC120009]; NPRP from the Qatar
National Research Fund (a member of Qatar Foundation) [NPRP-09-476-1-78,
X-019-1-006]; Villum foundation; European Union [268421]; KASI travel
grant [2012-1-410-02]; Korea Research Council for Fundamental Science
and Technology (KRCF); Spanish Ministry of Economy and Competitiveness
(MINECO) [MINECO SEV-2011-0187]; Danish National Research Foundation
[DNRF106]; ASTERISK project - European Research Council [267864];
Communaute francaise de Belgique - Actions de recherche concertees -
Academie Wallonie-Europe; International Max Planck Research School for
Astrophysics (IMPRS-HD); HGSFP
FX We would like to thank the anonymous referee for having significantly
contributed to improving the quality of this manuscript. We would like
to thank Armin Rest for introducing us to the HoTPANnTS software. We
also thank Ekaterina Koptelova for having provided the light curves of
quasar UM673. E.G. gratefully acknowledges the support of the
International Max Planck Research School for Astrophysics (IMPRS-HD) and
the HGSFP. E.G. also thanks Katie Ramire for helpful suggestions. T.A.
acknowledges support from FONDECYT proyecto 11130630 and the Ministry of
Economy, Development, and Tourism's Millennium Science Initiative
through grant IC120009, awarded to The Millennium Institute of
Astrophysics, MAS. M.D. and M.H. are supported by NPRP grant
NPRP-09-476-1-78 from the Qatar National Research Fund (a member of
Qatar Foundation). M.H. acknowledges support from the Villum foundation.
This publication was made possible by NPRP grant # X-019-1-006 from the
Qatar National Research Fund (a member of Qatar Foundation). The
research leading to these results has received funding from the European
Union Seventh Framework Programme (FP7/2007- 2013) under grant agreement
No. 268421. T.C.H. would like to acknowledge financial support from KASI
travel grant 2012-1-410-02 and Korea Research Council for Fundamental
Science and Technology (KRCF). D.R. acknowledges financial support from
the Spanish Ministry of Economy and Competitiveness (MINECO) under the
2011 Severo Ochoa Program MINECO SEV-2011-0187. Funding for the Stellar
Astrophysics Centre is provided by The Danish National Research
Foundation (grant agreement No.: DNRF106). The research is supported by
the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler)
funded by the European Research Council (grant agreement No.: 267864).
Y.D., A.E., F.F., D.R., O.W., and J. Surdej acknowledge support from the
Communaute francaise de Belgique - Actions de recherche concertees -
Academie Wallonie-Europe.
NR 40
TC 0
Z9 0
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JAN
PY 2017
VL 597
AR A49
DI 10.1051/0004-6361/201527422
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EI3LS
UT WOS:000392392900016
ER
PT J
AU Kooistra, R
Kamp, I
Fukagawa, M
Menard, F
Momose, M
Tsukagoshi, T
Kudo, T
Kusakabe, N
Hashimoto, J
Abe, L
Brandner, W
Brandt, TD
Carson, JC
Egner, SE
Feldt, M
Goto, M
Grady, CA
Guyon, O
Hayano, Y
Hayashi, M
Hayashi, SS
Henning, T
Hodapp, KW
Ishii, M
Iye, M
Janson, M
Kandori, R
Knapp, GR
Kuzuhara, M
Kwon, J
Matsuo, T
McElwain, MW
Miyama, S
Morino, JI
Moro-Martin, A
Nishimura, T
Pyo, TS
Serabyn, E
Suenaga, T
Suto, H
Suzuki, R
Takahashi, YH
Takami, M
Takato, N
Terada, H
Thalmann, C
Tomono, D
Turner, EL
Watanabe, M
Wisniewski, J
Yamada, T
Takami, H
Usuda, T
Tamura, M
Currie, T
Akiyama, E
Mayama, S
Follette, KB
Nakagawa, T
AF Kooistra, Robin
Kamp, Inga
Fukagawa, Misato
Menard, Franois
Momose, Munetake
Tsukagoshi, Takashi
Kudo, Tomoyuki
Kusakabe, Nobuhiko
Hashimoto, Jun
Abe, Lyu
Brandner, Wolfgang
Brandt, Timothy D.
Carson, Joseph C.
Egner, Sebastian E.
Feldt, Markus
Goto, Miwa
Grady, Carol A.
Guyon, Olivier
Hayano, Yutaka
Hayashi, Masahiko
Hayashi, Saeko S.
Henning, Thomas
Hodapp, Klaus W.
Ishii, Miki
Iye, Masanori
Janson, Markus
Kandori, Ryo
Knapp, Gillian R.
Kuzuhara, Masayuki
Kwon, Jungmi
Matsuo, Taro
McElwain, Michael W.
Miyama, Shoken
Morino, Jun-Ichi
Moro-Martin, Amaya
Nishimura, Tetsuo
Pyo, Tae-Soo
Serabyn, Eugene
Suenaga, Takuya
Suto, Hiroshi
Suzuki, Ryuji
Takahashi, Yasuhiro H.
Takami, Michihiro
Takato, Naruhisa
Terada, Hiroshi
Thalmann, Christian
Tomono, Daigo
Turner, Edwin L.
Watanabe, Makoto
Wisniewski, John
Yamada, Toru
Takami, Hideki
Usuda, Tomonori
Tamura, Motohide
Currie, Thayne
Akiyama, Eiji
Mayama, Satoshi
Follette, Katherine B.
Nakagawa, Takao
TI Radial decoupling of small and large dust grains in the transitional
disk RX J1615.3-3255
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE circumstellar matter; planet-disk interactions; planets and satellites:
formation; protoplanetary disks
ID MAIN-SEQUENCE STARS; SPITZER C2D SURVEY; T-TAURI STARS; PROTOPLANETARY
DISKS; CIRCUMSTELLAR DISK; PLANET FORMATION; HD 100546; LKCA 15; YOUNG;
SYSTEM
AB We present H-band (1.6 mu m) scattered light observations of the transitional disk RX J1615.3-3255, located in the similar to 1 Myr old Lupus association. From a polarized intensity image, taken with the HiCIAO instrument of the Subaru Telescope, we deduce the position angle and the inclination angle of the disk. The disk is found to extend out to 68 +/- 12 AU in scattered light and no clear structure is observed. Our inner working angle of 24 AU does not allow us to detect a central decrease in intensity similar to that seen at 30 AU in the 880 mu m continuum observations. We compare the observations with multiple disk models based on the spectral energy distribution (SED) and submm interferometry and find that an inner rim of the outer disk at 30 AU containing small silicate grains produces a polarized intensity signal which is an order of magnitude larger than observed. We show that a model in which the small dust grains extend smoothly into the cavity found for large grains is closer to the actual H-band observations. A comparison of models with di ff erent dust size distributions suggests that the dust in the disk might have undergone significant processing compared to the interstellar medium.
C1 [Kooistra, Robin; Kamp, Inga] Univ Groningen, Kapteyn Astron Inst, Postbus 800, NL-9700 AV Groningen, Netherlands.
[Fukagawa, Misato] Nagoya Univ, Grad Sch Sci, Div Particle & Astrophys Sci, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648602, Japan.
[Menard, Franois] Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France.
[Momose, Munetake; Tsukagoshi, Takashi] Ibaraki Univ, Coll Sci, 2-1-1 Bunkyo, Mito, Ibaraki 3108512, Japan.
[Kudo, Tomoyuki; Egner, Sebastian E.; Guyon, Olivier; Hayano, Yutaka; Hayashi, Saeko S.; Currie, Thayne] Subaru Telescope, 650 North Aohoku Pl, Hilo, HI 96720 USA.
[Kusakabe, Nobuhiko; Hashimoto, Jun; Suto, Hiroshi] Astrobiol Ctr NINS, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Abe, Lyu] Univ Nice Sophia Antipolis, Lab Lagrange UMR 7293, Observ Cote Azur, CNRS, 28 Ave Valrose, F-06108 Nice 2, France.
[Brandner, Wolfgang] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Brandt, Timothy D.] Inst Adv Study, Dept Astrophys, Olden Lane, Princeton, NJ 08540 USA.
[Carson, Joseph C.] Coll Charleston, Dept Phys & Astron, 58 Coming St, Charleston, SC 29424 USA.
[Goto, Miwa] Ludwig Maximilians Univ Munchen, Univ Sternwarte Munchen, Scheinerstr 1, D-81679 Munich, Germany.
[Grady, Carol A.] Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 20771 USA.
[Grady, Carol A.] Eureka Sci, 2452 Delmer,Suite 100, Oakland, CA 96002 USA.
[Grady, Carol A.] Goddard Ctr Astrobiol, Greenbelt, MD USA.
[Hayashi, Masahiko; Ishii, Miki; Iye, Masanori; Kandori, Ryo; Morino, Jun-Ichi; Suenaga, Takuya; Suto, Hiroshi; Suzuki, Ryuji; Takahashi, Yasuhiro H.; Takami, Hideki; Usuda, Tomonori; Akiyama, Eiji] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Hodapp, Klaus W.] Univ Hawaii, Inst Astron, 640 N Aohoku Pl, Hilo, HI 96720 USA.
[Janson, Markus] Stockholm Univ, Dept Astron, AlbaNova Univ Ctr, S-10691 Stockholm, Sweden.
[Knapp, Gillian R.] Princeton Univ, Dept Astrophys Sci, Peyton Hall,Ivy Lane, Princeton, NJ 08544 USA.
[Kuzuhara, Masayuki] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, 2-12-1 Ookayama, Tokyo 1528551, Japan.
[Kwon, Jungmi] Univ Tokyo, Dept Astron, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan.
[Matsuo, Taro] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, 1-1 Machikaneyamacho, Toyonaka, Osaka 5600043, Japan.
[Miyama, Shoken] Hiroshima Univ, 1-3-2 Kagamiyama, Higashihiroshima, Hiroshima 7398511, Japan.
[Moro-Martin, Amaya] CAB CSIC INTA, Dept Astrophys, Madrid 28850, Spain.
[Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Suenaga, Takuya] Grad Univ Adv Studies, Dept Astron Sci, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Takami, Michihiro] Acad Sin, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan.
[Thalmann, Christian] ETH, Inst Astron, Swiss Fed Inst Technol, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.
[Turner, Edwin L.] Univ Tokyo, Kavli Inst Phys & Math Universe, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778568, Japan.
[Watanabe, Makoto] Hokkaido Univ, Dept Cosmosci, Kita Ku, Sapporo, Hokkaido 0600810, Japan.
[Wisniewski, John] Univ Oklahoma, HL Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA.
[Yamada, Toru] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan.
[Mayama, Satoshi] Grad Univ Adv Studies SOKENDAI, Ctr Promot Integrated Sci, Hayama, Kanagawa 2400193, Japan.
[Mayama, Satoshi] Grad Univ Adv Studies SOKENDAI, Dept Astron Sci, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Nakagawa, Takao] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan.
RP Kooistra, R (reprint author), Univ Groningen, Kapteyn Astron Inst, Postbus 800, NL-9700 AV Groningen, Netherlands.
EM kooistra@astro.rug.nl
RI MIYAMA, Shoken/A-3598-2015
FU Netherlands Foundation for Scientific Research through the VICI
[639.043.006]; ANR of France [ANR-16-CE31-0013]
FX We thank The Netherlands Foundation for Scientific Research support
through the VICI grant 639.043.006. F.Me. acknowledges funding from ANR
of France under contract number ANR-16-CE31-0013.
NR 42
TC 0
Z9 0
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JAN
PY 2017
VL 597
AR A132
DI 10.1051/0004-6361/201628696
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EI3LS
UT WOS:000392392900044
ER
PT J
AU Masini, A
Comastri, A
Puccetti, S
Balokovic, M
Gandhi, P
Guainazzi, M
Bauer, FE
Boggs, SE
Boorman, PG
Brightman, M
Christensen, FE
Craig, WW
Farrah, D
Hailey, CJ
Harrison, FA
Koss, MJ
LaMassa, SM
Ricci, C
Stern, D
Walton, DJ
Zhang, WW
AF Masini, A.
Comastri, A.
Puccetti, S.
Balokovic, M.
Gandhi, P.
Guainazzi, M.
Bauer, F. E.
Boggs, S. E.
Boorman, P. G.
Brightman, M.
Christensen, F. E.
Craig, W. W.
Farrah, D.
Hailey, C. J.
Harrison, F. A.
Koss, M. J.
LaMassa, S. M.
Ricci, C.
Stern, D.
Walton, D. J.
Zhang, W. W.
TI The Phoenix galaxy as seen by NuSTAR
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; galaxies: Seyfert; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; X-RAY-EMISSION; SEYFERT 2 GALAXIES; XMM-NEWTON;
AGN; REFLECTION; VARIABILITY; ABSORPTION; MRK-1210; MISSION
AB Aims. We study the long-term variability of the well-known Seyfert 2 galaxy Mrk 1210 (also known as UGC4203, or the Phoenix galaxy).
Methods. The source was observed by many X-ray facilities in the last 20 yr. Here we present a NuSTAR observation and put the results in the context of previously published observations.
Results. NuSTAR observed Mrk 1210 in 2012 for 15.4 ks. The source showed Compton-thin obscuration similar to that observed by Chandra, Suzaku, BeppoSAX and XMM-Newton over the past two decades, but different from the first observation by ASCA in 1995, in which the active nucleus was caught in a low flux state or was obscured by Compton-thick matter with a reflection-dominated spectrum. Thanks to the high-quality hard X-ray spectrum obtained with NuSTAR and exploiting the long-term spectral coverage spanning 16.9 yr, we can precisely disentangle the transmission and reflection components and put constraints on both the intrinsic long-term variability and hidden nucleus scenarios. In the former case, the distance between the reflector and the source must be at least similar to 2 pc, while in the latter the eclipsing cloud may be identified with a water maser-emitting clump.
C1 [Masini, A.; Comastri, A.] INAF, Osservatorio Astron Bologna, Via Ranzani 1, I-40127 Bologna, Italy.
[Masini, A.] Univ Bologna, Dipartimento Fis & Astron DIFA, Viale Berti Pichat 6-2, I-40127 Bologna, Italy.
[Puccetti, S.] ASDC ASI, Via Politecn, I-00133 Rome, Italy.
[Puccetti, S.] INAF, Osservatorio Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, Italy.
[Balokovic, M.; Brightman, M.; Harrison, F. A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Gandhi, P.] Univ Durham, Dept Phys, Ctr Extragalact Astron, Durham DH1 3LE, England.
[Gandhi, P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Guainazzi, M.] Inst Space & Astronaut Sci JAXA, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525252, Japan.
[Guainazzi, M.] European Space Astron Ctr ESA, POB 78, Madrid 28691, Spain.
[Bauer, F. E.; Ricci, C.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Casilla 306, Santiago 22, Chile.
[Bauer, F. E.] Pontificia Univ Catolica Chile, Fac Fis, Ctr Astroingn, Casilla 306, Santiago 22, Chile.
[Bauer, F. E.] Millennium Inst Astrophys MAS, Nuncio Monsenor Sotero Sanz 100, Santiago, Chile.
[Bauer, F. E.; Ricci, C.] Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA.
[Boggs, S. E.; Craig, W. W.] EMBIGGEN Anillo, Concepcion, Chile.
[Christensen, F. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Craig, W. W.] Tech Univ Denmark, DTU Space Natl Space Inst, Elektrovej 327, DK-2800 Lyngby, Denmark.
[Farrah, D.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Hailey, C. J.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
[Koss, M. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[LaMassa, S. M.] ETH, Dept Phys, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.
[Stern, D.; Walton, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Walton, D. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, W. W.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA.
RP Masini, A (reprint author), INAF, Osservatorio Astron Bologna, Via Ranzani 1, I-40127 Bologna, Italy.; Masini, A (reprint author), Univ Bologna, Dipartimento Fis & Astron DIFA, Viale Berti Pichat 6-2, I-40127 Bologna, Italy.
EM alberto.masini4@unibo.it
FU NASA [NNG08FD60C]; National Aeronautics and Space Administration;
ASI/INAF [I/037/12/0-011/13]; NASA Headquarters under the NASA Earth and
Space Science Fellowship Program [NNX14AQ07H]; STFC [ST/J003697/2]; NASA
NuSTAR A01 Award [NNX15AV27G]; CONICYT-Chile [Basal-CATA PFB-06/2007];
FONDECYT [1141218]; "EMBIGGEN" Anillo [ACT1101]; China-CONICYT fund;
Ministry of Economy, Development; Tourism's Millennium Science
Initiative [IC120009]
FX We thank the anonymous referee for useful suggestions that helped to
improve the paper. This work was supported under NASA Contract
NNG08FD60C, and it made use of data from the NuSTAR mission, a project
led by the California Institute of Technology, managed by the Jet
Propulsion Laboratory, and funded by the National Aeronautics and Space
Administration. We thank the NuSTAR Operations, Software, and
Calibration teams for support with the execution and analysis of these
observations. This research made use of the NuSTAR Data Analysis
Software (NuSTARDAS) jointly developed by the ASI Science Data Center
(ASDC, Italy) and the California Institute of Technology (USA). This
research has also made use of data obtained from the Chandra Data
Archive and the Chandra Source Catalog, and software provided by the
Chandra X-ray Center (CXC). A.M., A.C., and S.P. acknowledge support
from the ASI/INAF grant I/037/12/0-011/13. M.B. acknowledges support
from NASA Headquarters under the NASA Earth and Space Science Fellowship
Program, grant NNX14AQ07H. P.G. and P.B. thank STFC for support (grant
ST/J003697/2). S.L.M. is supported by an appointment to the NASA
Postdoctoral Program at the NASA Goddard Space Flight Center,
administered by Universities Space Research Association under contract
with NASA. We acknowledge support from NASA NuSTAR A01 Award NNX15AV27G
(F.E.B.), CONICYT-Chile grants Basal-CATA PFB-06/2007 (F.E.B., C.R.),
FONDECYT Regular 1141218 (F.E.B., C.R.), "EMBIGGEN" Anillo ACT1101
(F.E.B., C.R.), the China-CONICYT fund (C.R.), and the Ministry of
Economy, Development, and Tourism's Millennium Science Initiative
through grant IC120009, awarded to The Millennium Institute of
Astrophysics, MAS (F.E.B.).
NR 40
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PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JAN
PY 2017
VL 597
AR A100
DI 10.1051/0004-6361/201629444
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EI3LS
UT WOS:000392392900116
ER
PT J
AU Milli, J
Hibon, P
Christiaens, V
Choquet, E
Bonnefoy, M
Kennedy, GM
Wyatt, MC
Absil, O
Gonzalez, CAG
del Burgo, C
Matra, L
Augereau, JC
Boccaletti, A
Delacroix, C
Ertel, S
Dent, WRF
Forsberg, P
Fusco, T
Girard, JH
Habraken, S
Huby, E
Karlsson, M
Lagrange, AM
Mawet, D
Mouillet, D
Perrin, M
Pinte, C
Pueyo, L
Reyes, C
Soummer, R
Surdej, J
Tarricq, Y
Wahhaj, Z
AF Milli, J.
Hibon, P.
Christiaens, V.
Choquet, E.
Bonnefoy, M.
Kennedy, G. M.
Wyatt, M. C.
Absil, O.
Gonzalez, C. A. Gomez
del Burgo, C.
Matra, L.
Augereau, J. -C.
Boccaletti, A.
Delacroix, C.
Ertel, S.
Dent, W. R. F.
Forsberg, P.
Fusco, T.
Girard, J. H.
Habraken, S.
Huby, E.
Karlsson, M.
Lagrange, A. -M.
Mawet, D.
Mouillet, D.
Perrin, M.
Pinte, C.
Pueyo, L.
Reyes, C.
Soummer, R.
Surdej, J.
Tarricq, Y.
Wahhaj, Z.
TI Discovery of a low-mass companion inside the debris ring surrounding the
F5V star HD 206893
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE brown dwarfs; circumstellar matter; planet-disk interactions; planetary
systems
ID GEMINI PLANET IMAGER; BROWN DWARFS; EVOLUTIONARY MODELS; BETA-PICTORIS;
GIANT PLANETS; DISK; EXOPLANETS; CORONAGRAPH; PHOTOMETRY; REDUCTION
AB Aims. Uncovering the ingredients and the architecture of planetary systems is a very active field of research that has fuelled many new theories on giant planet formation, migration, composition, and interaction with the circumstellar environment. We aim at discovering and studying new such systems, to further expand our knowledge of how low-mass companions form and evolve.
Methods. We obtained high-contrast H-band images of the circumstellar environment of the F5V star HD 206893, known to host a debris disc never detected in scattered light. These observations are part of the SPHERE High Angular Resolution Debris Disc Survey (SHARDDS) using the InfraRed Dual-band Imager and Spectrograph (IRDIS) installed on VLT/SPHERE.
Results. We report the detection of a source with a contrast of 3 : 6 x 10(-5) in the H-band, orbiting at a projected separation of 270 milliarcsec or 10 au, corresponding to a mass in the range 24 to 73 M-Jup for an age of the system in the range 0.2 to 2 Gyr. The detection was confirmed ten months later with VLT /NaCo, ruling out a background object with no proper motion. A faint extended emission compatible with the disc scattered light signal is also observed.
Conclusions. The detection of a low-mass companion inside a massive debris disc makes this system an analog of other young planetary systems such as beta Pictoris, HR 8799 or HD 95086 and requires now further characterisation of both components to understand their interactions.
C1 [Milli, J.; Absil, O.; Ertel, S.; Girard, J. H.] ESO, Alonso Cordova 3107, Santiago, Chile.
[Bonnefoy, M.; Matra, L.; Ertel, S.; Habraken, S.; Huby, E.] Univ Chile, Dept Astron, Casilla 36-D, Santiago, Chile.
[Christiaens, V.; Augereau, J. -C.; Girard, J. H.] Millenium Nucleus Protoplanetary Disks ALMA Early, Santiago, Chile.
[Girard, J. H.; Pueyo, L.] Univ Liege, Space Sci Technol & Astrophys Res STAR Inst, 19c Allee 6 Aout, B-4000 Liege, Belgium.
[Bonnefoy, M.; Augereau, J. -C.; Lagrange, A. -M.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Matra, L.; Pueyo, L.] Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France.
[Girard, J. H.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge, England.
[Milli, J.; Ertel, S.] Inst Nacl Astrofis, Opt Elect, Luis Enrique Erro 1, Puebla, Mexico.
[Dent, W. R. F.; Karlsson, M.] PSL Res Univ, Sorbonne Univ, UPMC Univ Paris 06, Univ Paris Diderot, 5 Pl Jules Janssen, F-92195 Meudon, France.
[Wyatt, M. C.] Cornell Univ, Sibley Sch Mech & Aerosp Engn, Ithaca, NY USA.
[del Burgo, C.; Pinte, C.] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85719 USA.
[Kennedy, G. M.; Habraken, S.] Atacama Large Millimeter Submillimeter Array ALMA, Santiago Cent Off, Alonso Cordova 3107,Casilla 763, Santiago, Chile.
[Fusco, T.; Mawet, D.] Uppsala Univ, Dept Engn Sci, Angstrom Lab, POB 534, S-75121 Uppsala, Sweden.
[Fusco, T.; Pueyo, L.] French Aerosp Lab, ONERA, BP72,29 Ave Div Leclerc, F-92322 Chatillon, France.
[Wyatt, M. C.; Lagrange, A. -M.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Ertel, S.; Lagrange, A. -M.] CALTECH, Dept Astron, 1200 Calif Blvd, Pasadena, CA 91125 USA.
RP Milli, J (reprint author), ESO, Alonso Cordova 3107, Santiago, Chile.
EM jmilli@eso.org
OI Kennedy, Grant/0000-0001-6831-7547; Delacroix,
Christian/0000-0003-0150-4430
FU ESO fellowship programme; NASA through Hubble Fellowship by STScI
[HST-HF2-51355, HST-AR-12652]; NASA [NAS5-26555]; European Research
Council under the European Union's Seventh Framework Programme (ERC
Grant) [337569]; French Community of Belgium through an ARC grant for
Concerted Research Action; Royal Society; European Union through ERC
grant [279973]; Millennium Science Initiative (Chilean Ministry of
Economy) [RC130007]; Mexican CONACyT [CB-2012-183007]
FX J.M. is supported by the ESO fellowship programme. He thanks R. Galicher
for his re-reduction of the NIRI data, and O. Wertz for his help with
VIP and NEGFC. E.C. is supported by NASA through Hubble Fellowship grant
HST-HF2-51355 and HST-AR-12652 awarded by STScI, operated by the AURA,
Inc., for NASA under contract NAS5-26555. O.A. is a F.R.S.-FNRS Research
Associate. The research leading to these results was partly funded by
the European Research Council under the European Union's Seventh
Framework Programme (ERC Grant Agreement No. 337569), and by the French
Community of Belgium through an ARC grant for Concerted Research Action.
G.M.K. is supported by the Royal Society as a Royal Society University
Research Fellow. M.C.W. and L.M. are supported by the European Union
through ERC grant 279973. V.C. acknowledges J. Smoker and M. Espinoza
for their help with NaCo. V.C. is supported by the Millennium Science
Initiative (Chilean Ministry of Economy) through grant RC130007. C.d.B.
acknowledges support from the Mexican CONACyT research grant
CB-2012-183007.
NR 41
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SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JAN
PY 2017
VL 597
AR L2
DI 10.1051/0004-6361/201629908
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EI3LS
UT WOS:000392392900143
ER
PT J
AU Schmieder, B
Mein, P
Mein, N
Levens, PJ
Labrosse, N
Ofman, L
AF Schmieder, B.
Mein, P.
Mein, N.
Levens, P. J.
Labrosse, N.
Ofman, L.
TI H alpha Doppler shifts in a tornado in the solar corona
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Sun: filaments, prominences
ID QUIESCENT PROMINENCE; MAGNETIC-FIELD; TRANSVERSE OSCILLATIONS; RESONANT
ABSORPTION; DYNAMICS; PLASMA; FILAMENT; WAVES; THREADS; MODEL
AB Contex t. High resolution movies in 193 from from the Atmospheric Imaging Assembly (AIA) on the Solar Dynamic Observatory (SDO) show apparent rotation in the leg of a prominence observed during a coordinated campaign. Such structures are commonly referred to as tornadoes. Time-distance intensity diagrams of the AIA data show the existence of oscillations suggesting that the structure is rotating.
Aims. The aim of this paper is to understand if the cool plasma at chromospheric temperatures inside the tornado is rotating around its central axis.
Methods. The tornado was also observed in H alpha with a cadence of 30 s by the MSDP spectrograph, operating at the Solar Tower in Meudon. The MSDP provides sequences of simultaneous spectra in a 2D field of view from which a cube of Doppler velocity maps is retrieved.
Results. The H alpha Doppler maps show a pattern with alternatively blueshifted and redshifted areas of 5 to 10 0 0 wide. Over time the blueshifted areas become redshifted and vice versa, with a quasi-periodicity of 40 to 60 min. Weaker amplitude oscillations with periods of 4 to 6 min are superimposed onto these large period oscillations.
Conclusions. The Doppler pattern observed in H alpha cannot be interpreted as rotation of the cool plasma inside the tornado. The H alpha velocity observations give strong constraints on the possible interpretations of the AIA tornado.
C1 [Schmieder, B.; Mein, P.] Univ Paris Diderot, UPMC Univ Paris 06, Sorbonne Univ, LESIA,Observ Paris,PSL Res Univ,CNRS,Sorbon Paris, 5 Pl Jules Janssen, F-92195 Meudon, France.
[Mein, N.] Observatoire Paris, 61 Ave Observ, F-75014 Paris, France.
[Levens, P. J.; Labrosse, N.] Univ Glasgow, SUPA Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland.
[Ofman, L.] CUA, Code 671, Greenbelt, MD 20771 USA.
[Ofman, L.] NASA, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA.
RP Schmieder, B (reprint author), Univ Paris Diderot, UPMC Univ Paris 06, Sorbonne Univ, LESIA,Observ Paris,PSL Res Univ,CNRS,Sorbon Paris, 5 Pl Jules Janssen, F-92195 Meudon, France.
EM brigitte.schmieder@obspm.fr
FU STFC Research Studentship [ST/K502005/1]; STFC [ST/L000741/1]; NASA
[NNG11PL10A]
FX The authors would like to thank the anonymous referee for his/her
fruitful comments, R. Lecocguen, D. Crussaire and the team at the MSDP
for acquiring the H alpha observations. We thank G. Aulanier for
fruitful discussions and the sketch of a "tornado", which has been drawn
by Sylvain Cnudde. We deeply thank L. Fletcher for giving many comments
on the manuscript to improve its clarity. P.J.L. acknowledges support
from an STFC Research Studentship ST/K502005/1. N.L. acknowledges
support from STFC grant ST/L000741/1. L.O. would like to acknowledge
support by NASA Cooperative Agreement grant NNG11PL10A to CUA. The AIA
data are provided courtesy of NASA/SDO and the AIA science team.
NR 44
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SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JAN
PY 2017
VL 597
AR A109
DI 10.1051/0004-6361/201628771
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EI3LS
UT WOS:000392392900052
ER
PT J
AU Schwarm, FW
Schonherr, G
Falkner, S
Pottschmidt, K
Wolff, MT
Becker, PA
Sokolova-Lapa, E
Klochkov, D
Ferrigno, C
Furst, F
Hemphill, PB
Marcu-Cheatham, DM
Dauser, T
Wilms, J
AF Schwarm, F. -W.
Schoenherr, G.
Falkner, S.
Pottschmidt, K.
Wolff, M. T.
Becker, P. A.
Sokolova-Lapa, E.
Klochkov, D.
Ferrigno, C.
Furst, F.
Hemphill, P. B.
Marcu-Cheatham, D. M.
Dauser, T.
Wilms, J.
TI Cyclotron resonant scattering feature simulations I. Thermally averaged
cyclotron scattering cross sections, mean free photon-path tables, and
electron momentum sampling
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE X-rays: binaries; stars: neutron; methods: numerical
ID STRONG MAGNETIC-FIELDS; LINE FORMATION; COMPTONIZATION; ABSORPTION;
RADIATION; EMISSION; GEOMETRY
AB Context. Electron cyclotron resonant scattering features (CRSFs) are observed as absorption-like lines in the spectra of X-ray pulsars. A significant fraction of the computing time for Monte Carlo simulations of these quantum mechanical features is spent on the calculation of the mean free path for each individual photon before scattering, since it involves a complex numerical integration over the scattering cross section and the (thermal) velocity distribution of the scattering electrons.
Aims. We aim to numerically calculate interpolation tables which can be used in CRSF simulations to sample the mean free path of the scattering photon and the momentum of the scattering electron. The tables also contain all the information required for sampling the scattering electron's final spin.
Methods. The tables were calculated using an adaptive Simpson integration scheme. The energy and angle grids were refined until a prescribed accuracy is reached. The tables are used by our simulation code to produce artificial CRSF spectra. The electron momenta sampled during these simulations were analyzed and justified using theoretically determined boundaries.
Results. We present a complete set of tables suited for mean free path calculations of Monte Carlo simulations of the cyclotron scattering process for conditions expected in typical X-ray pulsar accretion columns (0.01 <= B/B-crit <= 0.12, where B-crit = 4.413 x 10(13) G, and 3 keV <= k(B)T <= 15 keV). The sampling of the tables is chosen such that the results have an estimated relative error of at most 1 = 15 for all points in the grid. The tables are available online (see link in footnote, page 1).
C1 [Schwarm, F. -W.; Falkner, S.; Dauser, T.; Wilms, J.] Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, Sternwartstr 7, D-96049 Bamberg, Germany.
[Schoenherr, G.] Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany.
[Pottschmidt, K.] CRESST, Dept Phys, Baltimore, MD 21250 USA.
[Pottschmidt, K.] UMBC, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Pottschmidt, K.; Marcu-Cheatham, D. M.] NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA.
[Wolff, M. T.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Becker, P. A.] George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA.
[Sokolova-Lapa, E.] AM Lomonosov Moscow State Univ, Fac Phys, Moscow 119991, Russia.
[Sokolova-Lapa, E.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Univ Pr 13, Moscow 119992, Russia.
[Klochkov, D.] Univ Tubingen IAAT, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany.
[Ferrigno, C.] Univ Geneva, ISDC Data Ctr Astrophys, Chemin Ecologia 16, CH-1290 Versoix, Switzerland.
[Furst, F.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Hemphill, P. B.] Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr, San Diego, CA 92093 USA.
RP Schwarm, FW (reprint author), Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, Sternwartstr 7, D-96049 Bamberg, Germany.
EM fritz.schwarm@sternwarte.uni-erlangen.de
FU Deutsche Forschungsgemeinschaft under DFG grant [WI 1860/11-1];
Deutsches Zentrum fur Luft- und Raumfahrt under DLR grant [50 OR 1113,
50 OR 1207, 50 OR 1411]; Chief of Naval Research; National Aeronautics
and Space Administration Astrophysical Data Analysis Program
FX This work has been partially funded by the Deutsche
Forschungsgemeinschaft under DFG grant number WI 1860/11-1 and by the
Deutsches Zentrum fur Luft- und Raumfahrt under DLR grant numbers 50 OR
1113, 50 OR 1207, and 50 OR 1411. M.T.W. is supported by the Chief of
Naval Research and by the National Aeronautics and Space Administration
Astrophysical Data Analysis Program. We thank the International Space
Science Institute in Bern for inspiring team meetings. The fruitful
discussions within the MAGNET collaboration also had a very positive
impact on this work.
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J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JAN
PY 2017
VL 597
AR A3
DI 10.1051/0004-6361/201629352
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EI3LS
UT WOS:000392392900109
ER
PT J
AU Wehus, IK
Fuskeland, U
Eriksen, HK
Banday, AJ
Dickinson, C
Ghosh, T
Gorski, KM
Lawrence, CR
Leahy, JP
Maino, D
Reich, P
Reich, W
AF Wehus, I. K.
Fuskeland, U.
Eriksen, H. K.
Banday, A. J.
Dickinson, C.
Ghosh, T.
Gorski, K. M.
Lawrence, C. R.
Leahy, J. P.
Maino, D.
Reich, P.
Reich, W.
TI Monopole and dipole estimation for multi-frequency sky maps by linear
regression
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Correction
DE methods: statistical; cosmology: observations; Galaxy: general; radio
continuum: general
ID RADIO-CONTINUUM EMISSION; PROBE WMAP OBSERVATIONS; SPECTRAL INDEXES;
1420 MHZ; POWER; GHZ
AB We describe a simple but efficient method for deriving a consistent set of monopole and dipole corrections for multi-frequency sky map data sets, allowing robust parametric component separation with the same data set. The computational core of this method is linear regression between pairs of frequency maps, often called T-T plots. Individual contributions from monopole and dipole terms are determined by performing the regression locally in patches on the sky, while the degeneracy between different frequencies is lifted whenever the dominant foreground component exhibits a significant spatial spectral index variation. Based on this method, we present two different, but each internally consistent, sets of monopole and dipole coefficients for the nine-year WMAP, Planck 2013, SFD 100 mu m, Haslam 408 MHz and Reich & Reich 1420 MHz maps. The two sets have been derived with different analysis assumptions and data selection, and provide an estimate of residual systematic uncertainties. In general, our values are in good agreement with previously published results. Among the most notable results are a relative dipole between the WMAP and Planck experiments of 10-15 mu K (depending on frequency), an estimate of the 408MHz map monopole of 8.9 +/- 1.3 K, and a non-zero dipole in the 1420 MHz map of 0.15 +/- 0.03 K pointing towards Galactic coordinates (l, b) = (308 degrees, -36 degrees) +/- 14 degrees. These values represent the sum of any instrumental and data processing offsets, as well as any Galactic or extra-Galactic component that is spectrally uniform over the full sky.
C1 [Wehus, I. K.; Lawrence, C. R.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA USA.
[Wehus, I. K.; Fuskeland, U.; Eriksen, H. K.] Univ Oslo, Inst Theoret Astrophys, N-0371 Oslo, Norway.
[Banday, A. J.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France.
[Banday, A. J.] CNRS, IRAP, 9 Av Colonel Roche,BP 44346, F-31028 Toulouse 4, France.
[Dickinson, C.; Leahy, J. P.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England.
[Ghosh, T.] Univ Paris Sud 11, Inst Astrophys Spatiale, CNRS UMR 8617, Batiment 121, F-91898 Orsay, France.
[Gorski, K. M.] Univ Warsaw Observ, Aleje Ujazdowskie 4, PL-00478 Warsaw, Poland.
[Maino, D.] Univ Milan, Dipartimento Fis, Via Celoria 16, I-20133 Milan, Italy.
[Maino, D.] INAF IASF Milano, Via E Bassini 15, I-20135 Milan, Italy.
[Reich, P.; Reich, W.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
RP Wehus, IK (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA USA.; Wehus, IK (reprint author), Univ Oslo, Inst Theoret Astrophys, N-0371 Oslo, Norway.
EM i.k.wehus@astro.uio.no
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SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JAN
PY 2017
VL 597
AR A131
DI 10.1051/0004-6361/201525659
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EI3LS
UT WOS:000392392900006
ER
PT J
AU Ho, JC
Yeo, H
AF Ho, Jimmy C.
Yeo, Hyeonsoo
TI Assessment of comprehensive analysis predictions of helicopter rotor
blade loads in forward flight
SO JOURNAL OF FLUIDS AND STRUCTURES
LA English
DT Article
DE RCAS; Rotor aeromechanics; Rotor aeroelasticity; Blade structural loads;
Pitch link force; Blade airloads
ID AIRLOADS; VORTEX; WAKES
AB Comparisons of helicopter rotor blade loads, between rotorcraft comprehensive analysis predictions using a free vortex wake model and measured data, are provided for the UH-60A, SA 330 (research Puma), SA 349/2, and H-34 rotors in forward flight. The rotors are modeled as being isolated from the rest of the vehicle. The comparisons encompass a total of 24 test points featuring wide variations in advance ratio for a thorough assessment of the predictions. With the exception of chord bending moment for the case of UH-60A, the analysis correctly predicts trends in half peak-to-peak values of blade structural loads and pitch link force. Most of the predictions in half peak-to-peak blade structural loads and pitch link force deviate from the measured data by no more than 40% and most of the deviations are underpredictions. The predictions typically resemble the measured data in shapes of the waveforms for both flap bending moment and normal force, but this is less often the case for chord bending and torsion moments. While the analysis may capture the 1/rev harmonic contents in pitching moment waveforms, it consistently underpredicts any higher harmonics.
C1 [Ho, Jimmy C.] Sci & Technol Corp, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Yeo, Hyeonsoo] US Army Aviat Dev Directorate, Aviat & Missile Res, Dev & Engn Ctr, Res Dev & Engn Command RDECOM,Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Ho, JC (reprint author), Sci & Technol Corp, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM jimmy.c.ho2.ctr@mail.mil
NR 31
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U1 5
U2 5
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0889-9746
J9 J FLUID STRUCT
JI J. Fluids Struct.
PD JAN
PY 2017
VL 68
BP 194
EP 223
DI 10.1016/j.jfluidstructs.2016.09.007
PG 30
WC Engineering, Mechanical; Mechanics
SC Engineering; Mechanics
GA EJ5OP
UT WOS:000393267900013
ER
PT J
AU Achuthavarier, D
Wang, H
Schubert, SD
Sienkiewicz, M
AF Achuthavarier, D.
Wang, H.
Schubert, S. D.
Sienkiewicz, M.
TI Impact of DYNAMO observations on NASA GEOS-5 reanalyses and the
representation of MJO initiation
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE MJO; DYNAMO; GEOS-5; reanalysis
ID MADDEN-JULIAN OSCILLATION; STATIC ENERGY BUDGET; TRIMODAL
CHARACTERISTICS; FORECAST SKILL; CLIMATE MODELS; CONVECTION;
VARIABILITY; PATTERNS; PACIFIC; SYSTEM
AB This study examines the impact of the Dynamics of the Madden-Julian Oscillation (DYNAMO) campaign in situ observations on NASA Goddard Earth Observing System version 5 (GEOS-5) reanalyses and the improvements gained thereby in the representation of the Madden-Julian Oscillation (MJO) initiation processes. To this end, we produced a global, high-resolution (1/4 degrees spatially) reanalysis that assimilates the level-4, quality-controlled DYNAMO upper air soundings from about 87 stations in the equatorial Indian Ocean region along with a companion data-denied control reanalysis. The DYNAMO reanalysis produces a more realistic vertical structure of the temperature and moisture in the central tropical Indian Ocean by correcting the model biases, namely, the cold and dry biases in the lower troposphere and warm bias in the upper troposphere. The reanalysis horizontal winds are substantially improved, in that, the westerly acceleration and vertical shear of the zonal wind are enhanced. The DYNAMO reanalysis shows enhanced low-level diabatic heating, moisture anomalies and vertical velocity during the MJO initiation. Due to the warmer lower troposphere, the deep convection is invigorated, which is evident in convective cloud fraction. The GEOS-5 atmospheric general circulation model (AGCM) employed in the reanalysis is overall successful in assimilating the additional DYNAMO observations, except for an erroneous model response for medium rain rates, between 700 and 600hPa, reminiscent of a bias in earlier versions of the AGCM. The moist heating profile shows a sharp decrease there due to the excessive convective rain re-evaporation, which is partly offset by the temperature increment produced by the analysis.
C1 [Achuthavarier, D.; Wang, H.; Schubert, S. D.; Sienkiewicz, M.] NASA GSFC, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Achuthavarier, D.] Univ Space Res Assoc, Columbia, MD 21046 USA.
[Wang, H.; Sienkiewicz, M.] Sci Syst & Applicat Inc, Lanham, MD USA.
RP Achuthavarier, D (reprint author), NASA GSFC, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.; Achuthavarier, D (reprint author), Univ Space Res Assoc, Columbia, MD 21046 USA.
EM deepthi.achuthavarier@nasa.gov
OI Wang, Hailan/0000-0001-7320-247X; Sienkiewicz, Meta/0000-0002-9267-4568
FU NOAA Earth System Science (ESS) program
FX This study has been supported by the NOAA Earth System Science (ESS)
program. The authors thank the data assimilation and modeling groups at
the Global Modeling and Assimilation Office (GMAO) at the Goddard Space
Flight Center (GSFC) for guidance in conducting the assimilation
experiments. The assimilation runs are produced using the High-End
Computing (HEC) platforms of the NASA Center for Climate Simulation
(NCCS) at the GSFC. The DYNAMO and other data used in this study are
listed in the references. The reanalyses data produced in this study are
archived at the NCCS at the GSFC and are available from the authors upon
request.
NR 53
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U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN
PY 2017
VL 122
IS 1
BP 179
EP 201
DI 10.1002/2016JD025363
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EK4DR
UT WOS:000393877800011
ER
PT J
AU Fauchez, T
Davis, AB
Cornet, C
Szczap, F
Platnick, S
Dubuisson, P
Thieuleux, F
AF Fauchez, Thomas
Davis, Anthony B.
Cornet, Celine
Szczap, Frederic
Platnick, Steven
Dubuisson, Philippe
Thieuleux, Francois
TI A fast hybrid (3-D/1-D) model for thermal radiative transfer in cirrus
via successive orders of scattering
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE cirrus; 3-D radiative transfer; thermal infrared; scattering by ice
crystals
ID OPTIMAL ESTIMATION ALGORITHM; MULTIPLE-SCATTERING; ICE CLOUDS; MARINE
STRATOCUMULUS; EFFECTIVE EMISSIVITY; INFORMATION-CONTENT;
OPTICAL-THICKNESS; SPECTRAL REGION; AVHRR CHANNELS; PART I
AB We investigate the impact of cirrus cloud heterogeneity on the direct emission by cloud or surface and on the scattering by ice particles in the thermal infrared (TIR). Realistic 3-D cirri are modeled with the 3DCLOUD code, and top-of-atmosphere radiances are simulated by the 3-D Monte Carlo radiative transfer (RT) algorithm 3DMCPOL for two (8.65 m and 12.05 m) channels of the Imaging Infrared Radiometer on CALIPSO. At nadir, comparisons of 1-D and 3-D RT show that 3-D radiances are larger than their 1-D counterparts for direct emission but smaller for scattered radiation. For our cirrus cases, 99% of the 3-D total radiance is computed by the third scattering order, which corresponds to 90% of the total computational effort, but larger optical thicknesses need more scattering orders. To radically accelerate the 3-D RT computations (using only few percent of 3-D RT time with a Monte Carlo code), even in the presence of large optical depths, we develop a hybrid model based on exact 3-D direct emission, the first scattering order from 1-D in each homogenized column, and an empirical adjustment linearly dependent on the optical thickness to account for higher scattering orders. Good agreement is found between the hybrid model and the exact 3-D radiances for two very different cirrus models without changing the empirical parameters. We anticipate that a future deterministic implementation of the hybrid model will be fast enough to process multiangle thermal imagery in a practical tomographic reconstruction of 3-D cirrus fields.
C1 [Fauchez, Thomas] Univ Space Res Assoc, Greenbelt, MD 20771 USA.
[Fauchez, Thomas; Platnick, Steven] NASA, Goddard Space Flight Ctr, Climate & Radiat Lab, Greenbelt, MD 20771 USA.
[Davis, Anthony B.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Cornet, Celine; Dubuisson, Philippe; Thieuleux, Francois] Univ Lille 1, UMR 8518, Lab Opt Atmospher, Villeneuve Dascq, France.
[Szczap, Frederic] Univ Blaise Pascal, UMR 6016, Lab Meteorol Phys, Clermont Ferrand, France.
RP Fauchez, T (reprint author), Univ Space Res Assoc, Greenbelt, MD 20771 USA.
EM thomas.j.fauchez@nasa.gov
OI Davis, Anthony/0000-0003-1279-1420
FU Remote Sensing Theory program
FX This work was partially conducted at the Laboratoire d'Optique
Atmospherique (LOA, UMR 8518, Lille 1 University France) and at the
Climate and Radiation Laboratory (NASA/GSFC, code 613) under the NASA
Post doctoral Program (NPP) and the Universities Space Research
Association (USRA). This research was also carried out partially at the
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
Furthermore, A.D. acknowledges funding from the Remote Sensing Theory
program managed at NASA/HQs by Lucia Tsaoussi. We also thank our
anonymous reviewers for their many pertinent comments, leading to much
improved quality of the present paper.
NR 72
TC 1
Z9 1
U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN
PY 2017
VL 122
IS 1
BP 344
EP 366
DI 10.1002/2016JD025607
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EK4DR
UT WOS:000393877800020
ER
PT J
AU Suhir, E
Ghaffarian, R
Yi, S
AF Suhir, E.
Ghaffarian, R.
Yi, S.
TI Reliability physics behind the QFN state of stress
SO JOURNAL OF MATERIALS SCIENCE-MATERIALS IN ELECTRONICS
LA English
DT Article
ID PREDICTED STRESSES; THERMAL-STRESSES; ENDS
AB A physically meaningful analytical stress model is developed for the explanation of the reliability physics underlying the relief in the thermally induced interfacial shearing stresses in a typical Quad Flat No-lead (QFN) assembly. The stress relief in a QFN design is, in effect, an implementation of the general concept developed and quantified by the first author about a decade ago of using inhomogeneous bonds for lower thermal stresses in adhesively bonded or soldered assemblies. It is shown also that the maximum stress in the QFN design can be minimized, if the lengths of the peripheral zones are established based on the requirement that the stresses at the ends of the assembly are made equal to the stresses at the ends of its mid-portion. In the carried out numerical example the gain in the relief in the maximum interfacial shearing stress owing to the application of a bond with an elevated compliance is 9.94 %. When the optimized inhomogeneous bond is applied, the gain is 16.87 %. The gain in the stress relief owing to the optimized inhomogeneous bond (with respect to the homogeneous compliant bond) is 10.66 %. The computed interfacial stresses are below the yield stress of the solder material.
C1 [Suhir, E.; Yi, S.] Portland State Univ, Portland, OR 97207 USA.
[Suhir, E.] ERS Co, 727 Alvina Ct, Los Altos, CA 94024 USA.
[Ghaffarian, R.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Suhir, E (reprint author), Portland State Univ, Portland, OR 97207 USA.; Suhir, E (reprint author), ERS Co, 727 Alvina Ct, Los Altos, CA 94024 USA.
EM suhire@aol.com
NR 40
TC 0
Z9 0
U1 1
U2 1
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0957-4522
EI 1573-482X
J9 J MATER SCI-MATER EL
JI J. Mater. Sci.-Mater. Electron.
PD JAN
PY 2017
VL 28
IS 2
BP 2160
EP 2171
DI 10.1007/s10854-016-5781-x
PG 12
WC Engineering, Electrical & Electronic; Materials Science,
Multidisciplinary; Physics, Applied; Physics, Condensed Matter
SC Engineering; Materials Science; Physics
GA EK9GR
UT WOS:000394232600133
ER
PT J
AU Lim, LF
Starr, RD
Evans, LG
Parsons, AM
Zolensky, ME
Boynton, WV
AF Lim, Lucy F.
Starr, Richard D.
Evans, Larry G.
Parsons, Ann M.
Zolensky, Michael E.
Boynton, William V.
TI Modeling orbital gamma-ray spectroscopy experiments at carbonaceous
asteroids
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID SPECTROMETER; METEORITES; ABUNDANCES; CHONDRITES; UREILITES; TRANSPORT;
SURFACE; STONY; MOON; MARS
AB To evaluate the feasibility of measuring differences in bulk composition among carbonaceous meteorite parent bodies from an asteroid or comet orbiter, we present the results of a performance simulation of an orbital gamma-ray spectroscopy (GRS) experiment in a Dawn-like orbit around spherical model asteroids with a range of carbonaceous compositions. The orbital altitude was held equal to the asteroid radius for 4.5months. Both the asteroid gamma-ray spectrum and the spacecraft background flux were calculated using the MCNPX Monte-Carlo code. GRS is sensitive to depths below the optical surface (to approximate to 20-50cm depth depending on material density). This technique can therefore measure underlying compositions beneath a sulfur-depleted (e.g., Nittler etal. ) or desiccated surface layer. We find that 3 sigma uncertainties of under 1 wt% are achievable for H, C, O, Si, S, Fe, and Cl for five carbonaceous meteorite compositions using the heritage Mars Odyssey GRS design in a spacecraft-deck-mounted configuration at the Odyssey end-of-mission energy resolution, FWHM=5.7keV at 1332keV. The calculated compositional uncertainties are smaller than the compositional differences between carbonaceous chondrite subclasses.
C1 [Lim, Lucy F.; Starr, Richard D.; Evans, Larry G.; Parsons, Ann M.] NASA, Goddard Space Flight Ctr, Code 691, Greenbelt, MD 20771 USA.
[Starr, Richard D.] Catholic Univ Amer, Washington, DC 20064 USA.
[Evans, Larry G.] Comp Sci Corp, Lanham, MD 20706 USA.
[Zolensky, Michael E.] NASA, ARES, Johnson Space Ctr, Houston, TX 77058 USA.
[Boynton, William V.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
RP Lim, LF (reprint author), NASA, Goddard Space Flight Ctr, Code 691, Greenbelt, MD 20771 USA.
EM lucy.f.lim@nasa.gov
NR 30
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
EI 1945-5100
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JAN
PY 2017
VL 52
IS 1
BP 174
EP 190
DI 10.1111/maps.12786
PG 17
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EK1KB
UT WOS:000393683100010
ER
PT J
AU Seol, ML
Jeon, SB
Han, JW
Choi, YK
AF Seol, Myeong-Lok
Jeon, Seung-Bae
Han, Jin-Woo
Choi, Yang-Kyu
TI Ferrofluid-based triboelectric-electromagnetic hybrid generator for
sensitive and sustainable vibration energy harvesting
SO NANO ENERGY
LA English
DT Article
DE Energy harvesting; Ferrofluid; Magnetic fluid; Triboelectric
nanogenerator; Electromagnetic generator
ID MECHANICAL ENERGY; WAVE ENERGY; CONTACT ELECTRIFICATION; FLOATING
OSCILLATOR; NANOGENERATOR; WATER; SENSORS; PERFORMANCE; PACKAGE; SYSTEM
AB A vibration energy harvester that utilizes a liquid medium has been the subject of active research recently given its advantages of shape adaptability, scalability, and durability. In this work, a ferrofluid-based vibration energy harvester with a hybrid triboelectric-electromagnetic operating mechanism is proposed for the first time. The ferrofluid suspension solution is made with water and magnetic nanoparticles. Electrostatic induction between the polymer sidewall and the solvent water activates a triboelectric generator component, while electromagnetic induction between the suspended magnetic nanoparticles and an outer coil activates the electromagnetic generator component. Experimental results for the ferrofluid-embedded hybrid energy harvester showed an extremely low threshold amplitude and a wide operating frequency range, both of which can be particularly advantageous for harvesting subtle and irregular vibrations.
C1 [Seol, Myeong-Lok; Jeon, Seung-Bae; Choi, Yang-Kyu] Korea Adv Inst Sci & Technol, Sch Elect Engn, 291 Daehak Ro, Daejeon 34141, South Korea.
[Seol, Myeong-Lok; Han, Jin-Woo] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
RP Choi, YK (reprint author), Korea Adv Inst Sci & Technol, Sch Elect Engn, 291 Daehak Ro, Daejeon 34141, South Korea.
EM ykchoi@ee.kaist.ac.kr
OI Seol, Myeong-Lok/0000-0001-5724-2244
FU Center for Integrated Smart Sensors Project - Ministry of Science, ICT &
Future Planning as Global Frontier Project [CISS-2011-0031848]; Open
Innovation Lab Project from the National Nanofab Center (NNFC); EndRun
Project
FX M.L.S. and S.B.J. equally contributed to this work. This work was
supported by the Center for Integrated Smart Sensors Project funded by
the Ministry of Science, ICT & Future Planning as Global Frontier
Project (CISS-2011-0031848). This work is also supported by the Open
Innovation Lab Project from the National Nanofab Center (NNFC) and the
EndRun Project.
NR 49
TC 1
Z9 1
U1 7
U2 7
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 2211-2855
EI 2211-3282
J9 NANO ENERGY
JI Nano Energy
PD JAN
PY 2017
VL 31
BP 233
EP 238
DI 10.1016/j.nanoen.2016.11.038
PG 6
WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science,
Multidisciplinary; Physics, Applied
SC Chemistry; Science & Technology - Other Topics; Materials Science;
Physics
GA EJ8BE
UT WOS:000393446500026
ER
PT J
AU Lacey, SD
Walsh, ED
Hitz, E
Dai, JQ
Connell, JW
Hu, LB
Lin, Y
AF Lacey, Steven D.
Walsh, Evan D.
Hitz, Emily
Dai, Jiaqi
Connell, John W.
Hu, Liangbing
Lin, Yi
TI Highly compressible, binderless and ultrathick holey graphene-based
electrode architectures
SO NANO ENERGY
LA English
DT Article
DE Holey graphene; Mesoporous carbon; Compressible graphene; Scalable
fabrication; Ultrathick electrode architecture; Lithium-oxygen battery
ID LITHIUM-AIR BATTERIES; RECHARGEABLE LI-O-2 BATTERIES; POROUS GRAPHENE;
CARBON NANOTUBE; BULK PREPARATION; OXYGEN BATTERY; HIGH-CAPACITY;
CATALYST; CATHODE; OXIDE
AB Graphene is a renowned material due to its unique structural characteristics and chemical properties. By heating graphene powder in an open-ended tube furnace, a highly compressible carbon material, holey graphene (hG), can be created with controlled porosity and be further decorated with nanosized catalysts using a solvent-free procedure to impart functionality and electrocatalytic activity. For the first time, we demonstrate an additive-free, dry press method to compression mold hG-based materials into ultrathick, binderless and high mass loading architectures using a hydraulic press at room temperature. The compressibility and structure of the hG allows for fabrication of unique ultrathick electrode architectures (mixed, sandwich, and double-decker) using both hG and catalyst/hG nanohybrid materials. These high mass loading, mixed and stacked hG electrode architectures are the first of their kind and are successfully demonstrated as lithium-oxygen (Li-O-2) cathodes. The scalable, binderless, and solventless dry press method and novel additive-free electrode architectures presented here greatly advance both electrode fabrication options, and open up new electrode designs for potential energy storage advancements.
C1 [Lacey, Steven D.; Hitz, Emily; Dai, Jiaqi; Hu, Liangbing] Univ Maryland, Dept Mat Sci & Engn, College Pk, MD 20742 USA.
[Lacey, Steven D.; Walsh, Evan D.; Hitz, Emily] NASA, Langley Res Ctr, NASA Internships Fellowships Scholarships NIFS Pr, Hampton, VA 23681 USA.
[Connell, John W.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Mail Stop 226, Hampton, VA 23681 USA.
[Lin, Yi] Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA.
RP Hu, LB (reprint author), Univ Maryland, Dept Mat Sci & Engn, College Pk, MD 20742 USA.; Lin, Y (reprint author), Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA.
EM binghu@umd.edu; yilin-1@nasa.gov
FU NASA Langley Internal Research and Development (IRAD) Program; IRAD
through the NASA Interns, Fellows, and Scholars (NIFS) Program
FX This work was supported by the NASA Langley Internal Research and
Development (IRAD) Program. S.D.L., E.D.W. and E.H. were supported by
IRAD through the NASA Interns, Fellows, and Scholars (NIFS) Program and
conducted their laboratory experiments as interns at the NASA Langley
Research Center. We would like to thank J. Baughman and J. Alexa
(Analytical Mechanics Associates, Inc.) for assistance in EDS and XRD
measurements, respectively.
NR 41
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Z9 1
U1 19
U2 19
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 2211-2855
EI 2211-3282
J9 NANO ENERGY
JI Nano Energy
PD JAN
PY 2017
VL 31
BP 386
EP 392
DI 10.1016/j.nanoen.2016.11.005
PG 7
WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science,
Multidisciplinary; Physics, Applied
SC Chemistry; Science & Technology - Other Topics; Materials Science;
Physics
GA EJ8BE
UT WOS:000393446500043
ER
PT J
AU Bose, M
Clinton, JF
Ceylan, S
Euchner, F
van Driel, M
Khan, A
Giardini, D
Lognonne, P
Banerdt, WB
AF Bose, M.
Clinton, J. F.
Ceylan, S.
Euchner, F.
van Driel, M.
Khan, A.
Giardini, D.
Lognonne, P.
Banerdt, W. B.
TI A probabilistic framework for single-station location of seismicity on
Earth and Mars
SO PHYSICS OF THE EARTH AND PLANETARY INTERIORS
LA English
DT Article
DE Mars; Earth; Waveforms; Marsquakes; Earthquakes; Location; Surface
waves; Body-waves; Travel times
ID TRAVEL-TIMES; BROAD-BAND; INTERIOR STRUCTURE; WAVE; MODEL; MANTLE;
CONSTRAINTS; PARAMETERS; INVERSION; IMPACTS
AB Locating the source of seismic energy from a single three-component seismic station is associated with large uncertainties, originating from challenges in identifying seismic phases, as well as inevitable pick and model uncertainties. The challenge is even higher for planets such as Mars, where interior structure is a priori largely unknown. In this study, we address the single-station location problem by developing a probabilistic framework that combines location estimates from multiple algorithms to estimate the probability density function (PDF) for epicentral distance, back azimuth, and origin time. Each algorithm uses independent and complementary information in the seismic signals. Together, the algorithms allow locating seismicity ranging from local to teleseismic quakes. Distances and origin times of large regional and teleseismic events (M > 5.5) are estimated from observed and theoretical body- and multi-orbit surface-wave travel times. The latter are picked from the maxima in the waveform envelopes in various frequency bands. For smaller events at local and regional distances, only first arrival picks of body waves are used, possibly in combination with fundamental Rayleigh RI waveform maxima where detectable; depth phases, such as pP or PmP, help constrain source depth and improve distance estimates. Back azimuth is determined from the polarization of the Rayleigh- and/or P-wave phases. When seismic signals are good enough for multiple approaches to be used, estimates from the various methods are combined through the product of their PDFs, resulting in an improved event location and reduced uncertainty range estimate compared to the results obtained from each algorithm independently. To verify our approach, we use both earthquake recordings from existing Earth stations and synthetic Martian seismograms. The Mars synthetics are generated with a full-waveform scheme (AxiSEM) using spherically symmetric seismic velocity, density and attenuation models of Mars that incorporate existing knowledge of Mars internal structure, and include expected ambient and instrumental noise. While our probabilistic framework is developed mainly for application to Mars in the context of the upcoming InSight mission, it is also relevant for locating seismic events on Earth in regions with sparse instrumentation. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Bose, M.; Ceylan, S.; Euchner, F.; van Driel, M.; Khan, A.; Giardini, D.] Swiss Fed Inst Technol, Inst Geophys, Zurich, Switzerland.
[Bose, M.; Clinton, J. F.] Swiss Fed Inst Technol, Swiss Seismol Serv, Zurich, Switzerland.
[Lognonne, P.] Inst Phys Globe Paris, Paris, France.
[Banerdt, W. B.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Bose, M (reprint author), ETH, Sonneggstr 5, CH-8092 Zurich, Switzerland.
EM mboese@sed.ethz.ch
FU SNF-ANR [157133]; SEFRI; Swiss National Supercomputing Centre (CSCS)
[s528, s682]
FX We would like to thank Jan Becker from Gempa GmbH for integration of our
proposed probabilistic framework for single-station location in the
marslocgui tool. We would also like to thank Naomi Murdoch and David
Mimoun for making their Martian noise model available prior to
publication. This work was funded by joint SNF-ANR project 157133
'Seismology on Mars' and the SEFRI project 'MarsQuake Service -
Preparatory Phase'. Additional support came from a grant from the Swiss
National Supercomputing Centre (CSCS) under project IDs s528 and s682.
We would like to thank an anonymous reviewer and editor Mark Jellinek
for their comments. This is InSight contribution #12.
NR 65
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0031-9201
EI 1872-7395
J9 PHYS EARTH PLANET IN
JI Phys. Earth Planet. Inter.
PD JAN
PY 2017
VL 262
BP 48
EP 65
DI 10.1016/j.pepi.2016.11.003
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EJ5HM
UT WOS:000393248400005
ER
PT J
AU Alexiadis, A
Alberini, F
Meyer, ME
AF Alexiadis, Alessio
Alberini, Federico
Meyer, Marit E.
TI Geopolymers from lunar and Martian soil simulants
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE JSC LUNAR-1A; JSC MARS-1A; Mars; Moon; Geopolymer
AB This work discusses the geopolymerization of lunar dust simulant JSC LUNAR-1A and Martian dust simulant JSC MARS-1A. The geopolymerization of JSC LUNAR-1A occurs easily and produces a hard, rock-like, material. The geopolymerization of JSC MARS-1A requires milling to reduce the particle size. Tests were carried out to measure, for both JSC LUNAR-1A and JSC MARS-1A geopolymers, the maximum compressive and flexural strengths. In the case of the lunar simulant, these are higher than those of conventional cements. In the case of the Martian simulant, they are close to those of common building bricks. (C) 2016 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Alexiadis, Alessio; Alberini, Federico] Univ Birmingham, Sch Chem Engn, Birmingham B15 2TT, W Midlands, England.
[Meyer, Marit E.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Alexiadis, A (reprint author), Univ Birmingham, Sch Chem Engn, Birmingham B15 2TT, W Midlands, England.
EM a.alexiadis@bham.ac.uk
NR 16
TC 0
Z9 0
U1 5
U2 5
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD JAN 1
PY 2017
VL 59
IS 1
BP 490
EP 495
DI 10.1016/j.asr.2016.10.003
PG 6
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA EI8PJ
UT WOS:000392769500041
ER
PT J
AU Hays, L
Beaty, D
AF Hays, Lindsay
Beaty, David
TI Conference Report: Biosignature Preservation and Detection in Mars
Analog Environments
SO ASTROBIOLOGY
LA English
DT Editorial Material
DE Biosignature preservation; Biosignature detection; Mars analog
environments; Conference report; Astrobiological exploration
AB The Conference on Biosignature Preservation and Detection in Mars Analog Environments held in May 2016 brought together scientists to discuss microbial biosignatures in Mars analog habitable environments. Five analog environments were discussed: (1) hydrothermal spring systems, (2) subaqueous environments, (3) subaerial environments, (4) subsurface environments, and (5) iron-rich systems. This paper details the major messages that resulted from the discussions and will be followed by a review paper that adds significant detail from the published literature and interpretations from the writing committee of the workshop for future research and application to astrobiological exploration missions.
C1 [Hays, Lindsay; Beaty, David] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 321-690, Pasadena, CA 91109 USA.
RP Hays, L (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 321-690, Pasadena, CA 91109 USA.
EM lindsay.e.hays@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX The research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration.
NR 1
TC 0
Z9 0
U1 1
U2 1
PU MARY ANN LIEBERT, INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
EI 1557-8070
J9 ASTROBIOLOGY
JI Astrobiology
PD JAN
PY 2017
VL 17
IS 1
BP 1
EP 2
DI 10.1089/ast.2016.1608
PG 2
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA EI9KC
UT WOS:000392825800001
PM 28072548
ER
PT J
AU Hallar, AG
Molotch, NP
Hand, JL
Livneh, B
McCubbin, IB
Petersen, R
Michalsky, J
Lowenthal, D
Kunkel, KE
AF Hallar, A. Gannet
Molotch, Noah P.
Hand, Jenny L.
Livneh, Ben
McCubbin, Ian B.
Petersen, Ross
Michalsky, Joseph
Lowenthal, Douglas
Kunkel, Kenneth E.
TI Impacts of increasing aridity and wildfires on aerosol loading in the
intermountain Western US
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE aridity; wildfires; aerosol; aerosol optical depth; IMPROVE
ID UNITED-STATES; CLIMATE-CHANGE; NORTH-AMERICA; AIR-QUALITY; MODELS;
TRENDS; PROJECTIONS; POLLUTION; DROUGHT; SYSTEM
AB Feedbacks between climate warming, land surface aridity, and wildfire-derived aerosols represent a large source of uncertainty in future climate predictions. Here, long-term observations of aerosol optical depth, surface level aerosol loading, fire-area burned, and hydrologic simulations are used to show that regional-scale increases in aridity and resulting wildfires have significantly increased summertime aerosol loading in remote high elevation regions of the Intermountain West of the United States. Surface summertime organic aerosol loading and total aerosol optical depth were both strongly correlated (p < 0.05) with aridity and fire area burned at high elevation sites across major western US mountain ranges. These results demonstrate that surface-level organic aerosol loading is dominated by summertime wildfires at many high elevation sites. This analysis provides new constraints for climate projections on the influence of drought and resulting wildfires on aerosol loading. These empirical observations will help better constrain projected increases in organic aerosol loading with increased fire activity under climate change.
C1 [Hallar, A. Gannet; Petersen, Ross; Lowenthal, Douglas] Univ Utah, Dept Atmospher Sci, Salt Lake City, UT 84112 USA.
[Hallar, A. Gannet; Lowenthal, Douglas] Desert Res Inst, Div Atmospher Sci, Reno, NV USA.
[Hallar, A. Gannet; McCubbin, Ian B.; Petersen, Ross] Desert Res Inst, Storm Peak Lab, Steamboat Springs, CO USA.
[Molotch, Noah P.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA.
[Molotch, Noah P.] Inst Arctic & Alpine Res, Boulder, CO USA.
[Molotch, Noah P.; McCubbin, Ian B.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Hand, Jenny L.] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA.
[Livneh, Ben; Michalsky, Joseph] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Livneh, Ben] Univ Colorado, Dept Civil Environm & Architectural Engn, Boulder, CO 80309 USA.
[Michalsky, Joseph] NOAA, Earth Syst Res Lab, Boulder, CO USA.
[Kunkel, Kenneth E.] North Carolina State Univ, Cooperat Inst Climate & Satellites, Asheville, NC USA.
[Kunkel, Kenneth E.] Natl Ctr Environm Informat, Asheville, NC USA.
RP Hallar, AG (reprint author), Univ Utah, Dept Atmospher Sci, Salt Lake City, UT 84112 USA.; Hallar, AG (reprint author), Desert Res Inst, Div Atmospher Sci, Reno, NV USA.; Hallar, AG (reprint author), Desert Res Inst, Storm Peak Lab, Steamboat Springs, CO USA.
EM gannet.hallar@utah.edu
FU National Science Foundation [DEB 0832652]; US Environmental Protection
Agency; National Park Service; US Department of Agriculture Forest
Service (USDA-FS); US Geological Survey (USGS); USDA [2012-67003-19802];
NOAA through the Cooperative Institute for Climate and Satellites-North
Carolina [NA14NES432003]
FX We appreciate the capabilities of the USDA UV-B Monitoring and Research
Program for data storage and advice. The Steamboat Ski Resort provided
logistical support and in-kind donations for Storm Peak Laboratory. The
Desert Research Institute is a permittee of the Medicine-Bow Routt
National Forests and an equal opportunity service provider and employer.
The authors appreciate the effort of Douglas Moore at the Sevilleta Long
Term Ecological Research for maintaining the Aeronet site. The research
at Sevilleta Long Term Ecological Research is funded by the National
Science Foundation (Grant DEB 0832652) and administered by the US Fish
and Wildlife Service within the National Wildlife Refuge. IMPROVE is a
collaborative association of state, tribal, and federal agencies, and
international partners and is funded by the US Environmental Protection
Agency, with contracting and research support from the National Park
Service. The Air Quality Group at the University of California, Davis,
is the central analytical laboratory, with ion analysis provided by the
Research Triangle Institute and carbon analysis provided by the Desert
Research Institute. The US Department of Agriculture Forest Service
(USDA-FS) and the US Geological Survey (USGS) supports the MTBS program.
A G H was supported by a sabbatical from DRI to conduct this analysis. N
M was supported by USDA grant 2012-67003-19802. KK was supported by NOAA
through the Cooperative Institute for Climate and Satellites-North
Carolina under Cooperative Agreement NA14NES432003.'
NR 43
TC 0
Z9 0
U1 6
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-9326
J9 ENVIRON RES LETT
JI Environ. Res. Lett.
PD JAN
PY 2017
VL 12
IS 1
AR 014006
DI 10.1088/1748-9326/aa510a
PG 8
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA EK1DN
UT WOS:000393666100001
ER
PT J
AU Rosenzweig, C
Arnell, NW
Ebi, KL
Lotze-Campen, H
Raes, F
Rapley, C
Smith, MS
Cramer, W
Frieler, K
Reyer, CPO
Schewe, J
van Vuuren, D
Warszawski, L
AF Rosenzweig, Cynthia
Arnell, Nigel W.
Ebi, Kristie L.
Lotze-Campen, Hermann
Raes, Frank
Rapley, Chris
Smith, Mark Stafford
Cramer, Wolfgang
Frieler, Katja
Reyer, Christopher P. O.
Schewe, Jacob
van Vuuren, Detlef
Warszawski, Lila
TI Assessing inter-sectoral climate change risks: the role of ISIMIP
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Editorial Material
ID MODEL INTERCOMPARISON PROJECT; NINO SOUTHERN-OSCILLATION; 2 DEGREES-C;
MULTIMODEL ENSEMBLE; WATER-RESOURCES; CHANGE IMPACTS; FLOOD RISK;
ADAPTATION; FRAMEWORK; UNCERTAINTIES
AB The aims of the Inter-Sectoral Impact Model Intercomparison Project (ISIMIP) are to provide a framework for the intercomparison of global and regional-scale risk models within and across multiple sectors and to enable coordinated multi-sectoral assessments of different risks and their aggregated effects. The overarching goal is to use the knowledge gained to support adaptation and mitigation decisions that require regional or global perspectives within the context of facilitating transformations to enable sustainable development, despite inevitable climate shifts and disruptions. ISIMIP uses community-agreed sets of scenarios with standardized climate variables and socioeconomic projections as inputs for projecting future risks and associated uncertainties, within and across sectors. The results are consistent multi-model assessments of sectoral risks and opportunities that enable studies that integrate across sectors, providing support for implementation of the Paris Agreement under the United Nations Framework Convention on Climate Change.
C1 [Rosenzweig, Cynthia] NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
[Rosenzweig, Cynthia] Columbia Univ, Ctr Climate Syst Res, 2880 Broadway, New York, NY 10025 USA.
[Arnell, Nigel W.] Univ Reading, Dept Meteorol, Reading RG6 6AR, Berks, England.
[Arnell, Nigel W.] Univ Reading, Walker Inst, Reading RG6 6AR, Berks, England.
[Ebi, Kristie L.] Univ Washington, Dept Global Hlth, 4225 Roosevelt Way 100, Seattle, WA 98105 USA.
[Lotze-Campen, Hermann; Frieler, Katja; Reyer, Christopher P. O.; Schewe, Jacob; Warszawski, Lila] Potsdam Inst Climate Impact Res, Telegraphenberg A 31, D-14473 Potsdam, Germany.
[Lotze-Campen, Hermann] Humboldt Univ, Dept Agr Econ, Philippstr 13, D-10099 Berlin, Germany.
[Raes, Frank] European Commiss, Joint Res Ctr, IES, Via Enrico Fermi,TP 263, I-21020 Ispra, Italy.
[Raes, Frank] Univ Bocconi, Dept Policy Anal & Publ Management, Via Sarfatti, I-25 Milan, Italy.
[Rapley, Chris] UCL, Dept Earth Sci, Gower St, London WC1E 6BT, England.
[Smith, Mark Stafford] CSIRO Land & Water, GPO Box 1700, Canberra, ACT 2601, Australia.
[Cramer, Wolfgang] Aix Marseille Univ, Avignon Univ, Inst Mediterraneen Biodivers & Ecol Marine & Cont, CNRS,IRD, Technopole Arbois Mediterranee,Bat Villemin BP 80, F-13545 Aix En Provence 04, France.
[van Vuuren, Detlef] PBL Netherlands Environm Assessment Agcy, Postbus 30314, NL-2500 GH The Hague, Netherlands.
[van Vuuren, Detlef] Univ Utrecht, Copernicus Inst Sustainable Dev, Fac Geosci, Postbus 80-115, NL-3508 TC Utrecht, Netherlands.
RP Rosenzweig, C (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.; Rosenzweig, C (reprint author), Columbia Univ, Ctr Climate Syst Res, 2880 Broadway, New York, NY 10025 USA.
RI Cramer, Wolfgang/B-8221-2008; Stafford Smith, Mark/G-1680-2010
OI Cramer, Wolfgang/0000-0002-9205-5812; Stafford Smith,
Mark/0000-0002-1333-3651
NR 114
TC 0
Z9 0
U1 4
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-9326
J9 ENVIRON RES LETT
JI Environ. Res. Lett.
PD JAN
PY 2017
VL 12
IS 1
AR 010301
DI 10.1088/1748-9326/12/1/010301
PG 16
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA EK1DK
UT WOS:000393665800001
ER
PT J
AU Bhanja, SN
Rodell, M
Li, BL
Saha, D
Mukherjee, A
AF Bhanja, Soumendra N.
Rodell, Matthew
Li, Bailing
Saha, Dipankar
Mukherjee, Abhijit
TI Spatio-temporal variability of groundwater storage in India
SO JOURNAL OF HYDROLOGY
LA English
DT Article
DE Groundwater; India; Groundwater spatial variability; Groundwater
monitoring network design
ID SOIL-MOISTURE; SCALES; GRACE
AB Groundwater level measurements from 3907 monitoring wells, distributed within 22 major river basins of India, are assessed to characterize their spatial and temporal variability. Groundwater storage (GWS) anomalies (relative to the long-term mean) exhibit strong seasonality, with annual maxima observed during the monsoon season and minima during pre-monsoon season. Spatial variability of GWS anomalies increases with the extent of measurements, following the power law relationship, i.e., log-(spatial variability) is linearly dependent on log-(spatial extent). In addition, the impact of well spacing on spatial variability and the power law relationship is investigated. We found that the mean GWS anomaly sampled at a 0.25 degree grid scale closes to unweighted average over all wells. The absolute error corresponding to each basin grows with increasing scale, i.e., from 0.25 degree to 1 degree. It was observed that small changes in extent could create very large changes in spatial variability at large grid scales. Spatial variability of GWS anomaly has been found to vary with climatic conditions. To our knowledge, this is the first study of the effects of well spacing on groundwater spatial variability. The results may be useful for interpreting large scale groundwater variations from unevenly spaced or sparse groundwater well observations or for siting and prioritizing wells in a network for groundwater management. The output of this study could be used to maintain a cost effective groundwater monitoring network in the study region and the approach can also be used in other parts of the globe. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Bhanja, Soumendra N.; Mukherjee, Abhijit] Indian Inst Technol, Dept Geol & Geophys, Kharagpur 721302, W Bengal, India.
[Bhanja, Soumendra N.; Rodell, Matthew; Li, Bailing] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20771 USA.
[Saha, Dipankar] Govt India, Minist Water Resources River Dev & Ganga Rejuvena, Cent Ground Water Board, Faridabad, Haryana, India.
[Mukherjee, Abhijit] Indian Inst Technol, Sch Environm Sci & Engn, Kharagpur 721302, W Bengal, India.
RP Bhanja, SN; Mukherjee, A (reprint author), Indian Inst Technol, Dept Geol & Geophys, Kharagpur 721302, W Bengal, India.
EM soumendrabhanja@gmail.com; amukh2@gmail.com
OI Rodell, Matthew/0000-0003-0106-7437; Bhanja,
Soumendra/0000-0002-9434-8483
FU CSIR (Government of India); U.S. Department of State
FX SNB acknowledges CSIR (Government of India) for their support through
SPM fellowship. SNB also acknowledges U.S. Department of State for the
Fulbright fellowship. This manuscript uses open source data of the
Central Ground Water Board (CGWB), Ministry of Water Resources, River
Development and Ganga Rejuvenation, Government of India. Dr. Saha
acknowledge the support provided by the Chairman, CGWB, during the
study. The opinion expressed in the paper is of author's own and not of
the affiliated Department. We acknowledge P. Malakar and C. Nirmale, for
their help with groundwater level data retrievals. Tropical Rainfall
Measuring Mission (TRMM) (2011), TRMM (TMPA/3B43) Rainfall Estimate L3 1
month 0.25 degree x 0.25 degree V7, version, Greenbelt, MD, Goddard
Earth Sciences Data and Information Services Center (GES DISC), Accessed
on 20th November, 2015. SNB thanks Dr. S. Verma for her advice.
NR 21
TC 1
Z9 1
U1 4
U2 4
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-1694
EI 1879-2707
J9 J HYDROL
JI J. Hydrol.
PD JAN
PY 2017
VL 544
BP 428
EP 437
DI 10.1016/j.jhydrol.2016.11.052
PG 10
WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources
SC Engineering; Geology; Water Resources
GA EI8OR
UT WOS:000392767000036
ER
PT J
AU Matra, L
Dent, WRF
Wyatt, MC
Kral, Q
Wilner, DJ
Panic, O
Hughes, AM
de Gregorio-Monsalvo, I
Hales, A
Augereau, JC
Greaves, J
Roberge, A
AF Matra, L.
Dent, W. R. F.
Wyatt, M. C.
Kral, Q.
Wilner, D. J.
Panic, O.
Hughes, A. M.
de Gregorio-Monsalvo, I.
Hales, A.
Augereau, J. -C.
Greaves, J.
Roberge, A.
TI Exocometary gas structure, origin and physical properties around beta
Pictoris through ALMA CO multitransition observations
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE molecular processes; comets: general; circumstellar matter; stars:
individual: beta Pictoris; planetary systems; submillimetre: planetary
systems
ID CIRCUMSTELLAR DISK; DEBRIS DISK; MOLECULAR GAS; PLANETARY SYSTEM; NEARBY
STARS; CA-II; DUST; EVOLUTION; CARBON; COLLISIONS
AB Recent ALMA observations unveiled the structure of CO gas in the 23 Myr old beta Pictoris planetary system, a component that has been discovered in many similarly young debris discs. We here present ALMA CO J = 2-1 observations, at an improved spectro-spatial resolution and sensitivity compared to previous CO J = 3-2 observations. We find that (1) the CO clump is radially broad, favouring the resonant migration over the giant impact scenario for its dynamical origin, (2) the CO disc is vertically tilted compared to the main dust disc, at an angle consistent with the scattered light warp. We then use position-velocity diagrams to trace Keplerian radii in the orbital plane of the disc. Assuming a perfectly edge-on geometry, this shows a CO scaleheight increasing with radius as R-0.75, and an electron density [derived from CO line ratios through non-local thermodynamic equilibrium (NLTE) analysis] in agreement with thermodynamical models. Furthermore, we show how observations of optically thin line ratios can solve the primordial versus secondary origin dichotomy in gas-bearing debris discs. As shown for beta Pictoris, subthermal (NLTE) CO excitation is symptomatic of H-2 densities that are insufficient to shield CO from photodissociation over the system's lifetime. This means that replenishment from exocometary volatiles must be taking place, proving the secondary origin of the disc. In this scenario, assuming steady state production/destruction of CO gas, we derive the CO+CO2 ice abundance by mass in beta Pic's exocomets to be at most similar to 6 per cent, consistent with comets in our own Solar system and in the coeval HD181327 system.
C1 [Matra, L.; Wyatt, M. C.; Kral, Q.; Panic, O.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Matra, L.] European Southern Observ, Alonso de Cordova 3107, Santiago, Chile.
[Dent, W. R. F.; de Gregorio-Monsalvo, I.; Hales, A.] ALMA SCO, Alonso de Cordova 3107, Santiago, Chile.
[Wilner, D. J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Hughes, A. M.] Wesleyan Univ, Van Vleck Observ, Dept Astron, 96 Foss Hill Dr, Middletown, CT 06459 USA.
[Augereau, J. -C.] Univ Grenoble Alpes, IPAG, UMR 5274, F-38000 Grenoble, France.
[Augereau, J. -C.] CNRS, IPAG, UMR 5274, F-38000 Grenoble, France.
[Greaves, J.] Cardiff Univ, Sch Phys & Astron, 4 Parade, Cardiff CF24 3AA, Wales.
[Roberge, A.] NASA, Exoplanets & Stellar Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Matra, L (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.; Matra, L (reprint author), European Southern Observ, Alonso de Cordova 3107, Santiago, Chile.
EM l.matra@ast.cam.ac.uk
FU STFC; ESO; European Union through ERC [279973]; Royal Society Dorothy
Hodgkin Fellowship; NSF [AST-1412647]
FX The authors would like to acknowledge Daniel Apai for providing the disc
spine from HST observations, and Grant Kennedy for providing the SED
fitting parameters. LM acknowledges support by STFC and ESO through
graduate studentships and, together with MCW and QK, by the European
Union through ERC grant number 279973. Work of OP is funded by the Royal
Society Dorothy Hodgkin Fellowship, and AMH gratefully acknowledges
support from NSF grant AST-1412647. This paper makes use of the
following ALMA data: ADS/JAO. ALMA#2012.1.00142.S and ADS/JAO.
ALMA#2011.0.00087.S. ALMA is a partnership of ESO (representing its
member states), NSF (USA) and NINS (Japan), together with NRC (Canada),
NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation
with the Republic of Chile. The Joint ALMA Observatory is operated by
ESO, AUI/NRAO and NAOJ.
NR 74
TC 2
Z9 2
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN
PY 2017
VL 464
IS 2
BP 1415
EP 1433
DI 10.1093/mnras/stw2415
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EK0WF
UT WOS:000393647100011
ER
PT J
AU Oh, K
Schawinski, K
Koss, M
Trakhtenbrot, B
Lamperti, I
Ricci, C
Mushotzky, R
Veilleux, S
Berney, S
Crenshaw, DM
Gehrels, N
Harrison, F
Masetti, N
Soto, KT
Stern, D
Treister, E
Ueda, Y
AF Oh, Kyuseok
Schawinski, Kevin
Koss, Michael
Trakhtenbrot, Benny
Lamperti, Isabella
Ricci, Claudio
Mushotzky, Richard
Veilleux, Sylvain
Berney, Simon
Crenshaw, D. Michael
Gehrels, Neil
Harrison, Fiona
Masetti, Nicola
Soto, Kurt T.
Stern, Daniel
Treister, Ezequiel
Ueda, Yoshihiro
TI BAT AGN Spectroscopic Survey - III. An observed link between AGN
Eddington ratio and narrow-emission-line ratios
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE black hole physics; galaxies: active; galaxies: nuclei; quasars: general
ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; MASS-METALLICITY RELATION;
BLACK-HOLE GROWTH; SHELL ABSORPTION-LINES; QUASI-STELLAR OBJECTS;
ULTRA-FAST OUTFLOWS; STAR-FORMATION RATE; HOST GALAXIES; OPTICALLY DULL
AB We investigate the observed relationship between black hole mass (M-BH), bolometric luminosity (L-bol) and Eddington ratio (lambda(Edd)) with optical emission-line ratios ([N II] lambda 6583/H alpha, [S II] lambda lambda 6716, 6731/H alpha, [O I] lambda 6300/H alpha, [O III] lambda 5007/H beta, [Ne III] lambda 3869/H beta and He II lambda 4686/H beta) of hard X-ray-selected active galactic nuclei (AGN) from the BAT AGN Spectroscopic Survey. We show that the [N II] lambda 6583/H alpha ratio exhibits a significant correlation with lambda(Edd) (R-Pear = -0.44, p-value = 3 x 10(-13), sigma = 0.28 dex), and the correlation is not solely driven by M-BH or L-bol. The observed correlation between [N II] lambda 6583/H alpha ratio and M-BH is stronger than the correlation with L-bol, but both are weaker than the lambda(Edd) correlation. This implies that the large-scale narrow lines of AGN host galaxies carry information about the accretion state of the AGN central engine. We propose that [N II] lambda 6583/H alpha is a useful indicator of Eddington ratio with 0.6 dex of rms scatter, and that it can be used to measure lambda(Edd) and thus M-BH from the measured L-bol, even for high-redshift obscured AGN. We briefly discuss possible physical mechanisms behind this correlation, such as the mass-metallicity relation, X-ray heating, and radiatively driven outflows.
C1 [Oh, Kyuseok; Schawinski, Kevin; Koss, Michael; Trakhtenbrot, Benny; Lamperti, Isabella; Berney, Simon; Soto, Kurt T.] Swiss Fed Inst Technol, Dept Phys, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.
[Ricci, Claudio] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Casilla 306, Santiago 22, Chile.
[Mushotzky, Richard; Veilleux, Sylvain; Treister, Ezequiel] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Mushotzky, Richard; Veilleux, Sylvain] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Crenshaw, D. Michael] Georgia State Univ, Dept Phys & Astron, Astron Off, One Pk Pl South SE,Suite 700, Atlanta, GA 30303 USA.
[Gehrels, Neil] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Harrison, Fiona] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Masetti, Nicola] INAF Ist Astrofis Spaziale & Fis Cosm Bologna, Via Gobetti 101, I-40129 Bologna, Italy.
[Masetti, Nicola] Univ Andres Bello, Dept Ciencias Fis, Fernandez Concha 700, Santiago 7591583, Chile.
[Stern, Daniel] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 169-224, Pasadena, CA 91109 USA.
[Ueda, Yoshihiro] Kyoto Univ, Dept Astron, Kyoto 6068502, Japan.
RP Oh, K; Schawinski, K; Koss, M (reprint author), Swiss Fed Inst Technol, Dept Phys, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.
EM ohk@phys.ethz.ch; kevin.schawinski@phys.ethz.ch; mike.koss@phys.ethz.ch
OI Trakhtenbrot, Benny/0000-0002-3683-7297
FU Swiss National Science Foundation (SNSF) [200021_157021, PP00P2_138979,
PP00P2_166159]; SNSF through the Ambizione fellowship [PZ00P2_154799/1];
SNFS through the Ambizione fellowship [PP00P2 138979/1]; CONICYT-Chile
'EMBIGGEN' Anillo [ACT1101]; FONDECYT [1141218, 1160999]; Basal-CATA
[PFB-06/2007]; China-CONICYT; NASA
FX KO and KS acknowledge support from the Swiss National Science Foundation
(SNSF) through Project grants 200021_157021, PP00P2_138979, and
PP00P2_166159. MK acknowledges support from the SNSF through the
Ambizione fellowship grant PZ00P2_154799/1. MK and KS acknowledge
support from the SNFS through the Ambizione fellowship grant PP00P2
138979/1. CR acknowledges financial support from the CONICYT-Chile
'EMBIGGEN' Anillo (grant ACT1101), FONDECYT 1141218, Basal-CATA
PFB-06/2007 and China-CONICYT fund. ET acknowledges support from the
CONICYT-Chile 'EMBIGGEN' Anillo (grant ACT1101), FONDECYT 1160999, and
Basal-CATA PFB-06/2007. The work of DS was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with NASA. This research has made use of NASA's ADS Service.
NR 78
TC 0
Z9 0
U1 3
U2 3
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN
PY 2017
VL 464
IS 2
BP 1466
EP 1473
DI 10.1093/mnras/stw2467
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EK0WF
UT WOS:000393647100015
ER
PT J
AU Ward, JL
Oliveira, JM
van Loon, JT
Sewilo, M
AF Ward, J. L.
Oliveira, J. M.
van Loon, J. Th.
Sewilo, M.
TI K-band integral field spectroscopy and optical spectroscopy of massive
young stellar objects in the Small Magellanic Cloud
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE circumstellar matter; stars: formation; stars: protostars; H II regions;
Magellanic Clouds; infrared: stars
ID STAR-FORMING REGION; LOW-METALLICITY ENVIRONMENTS; BLANKETED MODEL
ATMOSPHERES; DATA CUBES APPLICATION; 20-CM RADIO-CONTINUUM; H-II REGION;
ACCRETION RATES; PHYSICAL-PROPERTIES; INFRARED-EMISSION; GALAXY
EVOLUTION
AB We present K-band integral field spectroscopic observations towards 17 massive young stellar objects (YSOs) in the low-metallicity Small Magellanic Cloud (SMC) and two YSO candidates in the compact H II regions N81 and N88 A (also in the SMC). These sources, originally identified using Spitzer photometry and/or spectroscopy, have been resolved into 29 K-band continuum sources. By comparing Br gamma emission luminosities with those presented for a Galactic sample of massive YSOs, we find tentative evidence for increased accretion rates in the SMC. Around half of our targets exhibit emission-line (Br gamma, He I and H-2) morphologies that extend significantly beyond the continuum source and we have mapped both the emission morphologies and the radial velocity fields. This analysis also reveals evidence for the existence of ionized low-density regions in the centre outflows from massive YSOs. Additionally, we present an analysis of optical spectra towards a similar sample of massive YSOs in the SMC, revealing that the optical emission is photoexcited and originates near the outer edges of molecular clouds, and is therefore consistent with a high mean-free path of UV photons in the interstellar medium (ISM) of the SMC. Finally, we discuss the sample of YSOs in an evolutionary context incorporating the results of previous infrared and radio observations, as well as the near-infrared and optical observations presented in this work. Our spectroscopic analysis in both the K band and the optical regimes, combined with previously obtained infrared and radio data, exposes differences between properties of massive YSOs in our own Galaxy and the SMC, including tracers of accretion, discs and YSO-ISM interactions.
C1 [Ward, J. L.; Oliveira, J. M.; van Loon, J. Th.] Keele Univ, Lennard Jones Labs, Phys & Astrophys, Keele ST5 5BG, Staffs, England.
[Sewilo, M.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
RP Ward, JL (reprint author), Keele Univ, Lennard Jones Labs, Phys & Astrophys, Keele ST5 5BG, Staffs, England.
EM j.l.ward@keele.ac.uk
FU Science and Technology Facilities Council of the UK (STFC); STFC;
SINFONI at the ESO's VLT [092.C-0723(A)]
FX The authors thank the anonymous referee for his/her useful comments. JLW
acknowledges financial support from the Science and Technology
Facilities Council of the UK (STFC) via the PhD studentship programme.
We would like to thank the staff at ESO's Paranal observatory for their
support during the observations. Some of the observations reported in
this paper were obtained with the SALT. This paper made use of
information from the RMS survey data base at
http://rms.leeds.ac.uk/cgi-bin/public/RMS_DATABASE.cgi, which was
constructed with support from STFC. This research has made use of the
SIMBAD data base, operated at CDS, Strasbourg, France. The paper is
based on data obtained with SINFONI at the ESO's VLT under programme
092.C-0723(A).
NR 87
TC 0
Z9 0
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JAN
PY 2017
VL 464
IS 2
BP 1512
EP 1552
DI 10.1093/mnras/stw2386
PG 41
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EK0WF
UT WOS:000393647100021
ER
PT J
AU Fukumori, I
AF Fukumori, Ichiro
TI Kamifusen, the self-inflating Japanese paper balloon
SO PHYSICS TODAY
LA English
DT Editorial Material
C1 [Fukumori, Ichiro] CALTECH, Jet Prop Lab, Earth Sci Sect, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
RP Fukumori, I (reprint author), CALTECH, Jet Prop Lab, Earth Sci Sect, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
NR 2
TC 0
Z9 0
U1 2
U2 2
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0031-9228
EI 1945-0699
J9 PHYS TODAY
JI Phys. Today
PD JAN
PY 2017
VL 70
IS 1
BP 78
EP 79
DI 10.1063/PT.3.3437
PG 2
WC Physics, Multidisciplinary
SC Physics
GA EI9QW
UT WOS:000392844800022
ER
PT J
AU Hausfather, Z
Cowtan, K
Clarke, DC
Jacobs, P
Richardson, M
Rohde, R
AF Hausfather, Zeke
Cowtan, Kevin
Clarke, David C.
Jacobs, Peter
Richardson, Mark
Rohde, Robert
TI Assessing recent warming using instrumentally homogeneous sea surface
temperature records
SO SCIENCE ADVANCES
LA English
DT Article
ID IN-SITU; UNCERTAINTY; FLOATS
AB Sea surface temperature (SST) records are subject to potential biases due to changing instrumentation and measurement practices. Significant differences exist between commonly used composite SST reconstructions from the National Oceanic and Atmospheric Administration's Extended Reconstruction Sea Surface Temperature (ERSST), the Hadley Centre SST data set (HadSST3), and the Japanese Meteorological Agency's Centennial Observation-Based Estimates of SSTs (COBE-SST) from 2003 to the present. The update from ERSST version 3b to version 4 resulted in an increase in the operational SST trend estimate during the last 19 years from 0.07 degrees to 0.12 degrees C per decade, indicating a higher rate of warming in recent years. We show that ERSST version 4 trends generally agree with largely independent, near-global, and instrumentally homogeneous SST measurements from floating buoys, Argo floats, and radiometer-based satellite measurements that have been developed and deployed during the past two decades. We find a large cooling bias in ERSST version 3b and smaller but significant cooling biases in HadSST3 and COBE-SST from 2003 to the present, with respect to most series examined. These results suggest that reported rates of SST warming in recent years have been underestimated in these three data sets.
C1 [Hausfather, Zeke] Univ Calif Berkeley, Energy & Resources Grp, Berkeley, CA 94720 USA.
[Hausfather, Zeke; Rohde, Robert] Berkeley Earth, Berkeley, CA 94705 USA.
[Cowtan, Kevin] Univ York, Dept Chem, York, N Yorkshire, England.
[Jacobs, Peter] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA.
[Richardson, Mark] CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Hausfather, Z (reprint author), Univ Calif Berkeley, Energy & Resources Grp, Berkeley, CA 94720 USA.; Hausfather, Z (reprint author), Berkeley Earth, Berkeley, CA 94705 USA.
EM hausfath@berkeley.edu
OI Richardson, Mark/0000-0001-7063-631X; Jacobs, Peter/0000-0002-6951-7126
FU Berkeley Earth; NASA; George Mason University
FX Z.H. and R.R. were funded by Berkeley Earth. M.R.'s research was carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA. P.J. was funded by George Mason
University. No specific grants were allocated to support this project.
NR 38
TC 0
Z9 0
U1 2
U2 2
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 2375-2548
J9 SCI ADV
JI Sci. Adv.
PD JAN
PY 2017
VL 3
IS 1
AR e1601207
DI 10.1126/sciadv.1601207
PG 13
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EK2XI
UT WOS:000393789900011
PM 28070556
ER
PT J
AU Ye, HC
Fetzer, EJ
Wong, S
Lambrigtsen, BH
AF Ye, Hengchun
Fetzer, Eric J.
Wong, Sun
Lambrigtsen, Bjorn H.
TI Rapid decadal convective precipitation increase over Eurasia during the
last three decades of the 20th century
SO SCIENCE ADVANCES
LA English
DT Article
ID NORTHERN EURASIA; CLIMATE-CHANGE; UNITED-STATES; WATER-VAPOR;
TEMPERATURE; FREQUENCY; INTENSITY; EXTREMES; MODELS; RAINFALL
AB Convective precipitation-localized, short-lived, intense, and sometimes violent-is at the root of challenges associated with observation, simulation, and prediction of precipitation. The understanding of long-term changes in convective precipitation characteristics and their role in precipitation extremes and intensity over extratropical regions are imperative to future water resource management; however, they have been studied very little. We show that annual convective precipitation total has been increasing astonishingly fast, at a rate of 18.4%/degrees C, of which 16% is attributable to an increase in convective precipitation occurrence, and 2.4% is attributable to increased daily intensity based on the 35 years of two (combined) historical data sets of 3-hourly synoptic observations and daily precipitation. We also reveal that annual daily precipitation extreme has been increasing at a rate of about 7.4%/degrees C in convective events only. Concurrently, the overall increase in mean daily precipitation intensity is mostly due to increased convective precipitation, possibly at the expanse of nonconvective precipitation. As a result, transitional seasons are becoming more summer-like as convective becomes the dominant precipitation type that has accompanied higher daily extremes and intensity since the late 1980s. The data also demonstrate that increasing convective precipitation and daily extremes appear to be directly linearly associated with higher atmospheric water vapor accompanying a warming climate over northern Eurasia.
C1 [Ye, Hengchun] Calif State Univ Los Angeles, Dept Geosci & Environm, Los Angeles, CA 90032 USA.
[Ye, Hengchun; Fetzer, Eric J.; Wong, Sun; Lambrigtsen, Bjorn H.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Ye, HC (reprint author), Calif State Univ Los Angeles, Dept Geosci & Environm, Los Angeles, CA 90032 USA.; Ye, HC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM hye2@calstatela.edu
FU NASA [NNX15AQ06A]
FX This research was supported by NASA Minority University Research and
Education Project (MUREP) Institutional Research Opportunity grant
NNX15AQ06A.
NR 34
TC 0
Z9 0
U1 0
U2 0
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 2375-2548
J9 SCI ADV
JI Sci. Adv.
PD JAN
PY 2017
VL 3
IS 1
AR e1600944
DI 10.1126/sciadv.1600944
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EK2XI
UT WOS:000393789900008
PM 28138545
ER
PT J
AU Gu, Y
Wang, CL
Ma, J
Nemiroff, RJ
Kao, DL
Parra, D
AF Gu, Yi
Wang, Chaoli
Ma, Jun
Nemiroff, Robert J.
Kao, David L.
Parra, Denis
TI Visualization and recommendation of large image collections toward
effective sensemaking
SO INFORMATION VISUALIZATION
LA English
DT Article
DE Large image collection; graph layout; progressive drawing; node
comparison; visual recommendation
ID GRAPH VISUALIZATION; INFORMATION VISUALIZATION; DYNAMIC NETWORKS; SOCIAL
NETWORKS; LAYOUT; NAVIGATION; ANALYTICS; DIAGRAMS; WORDLE
AB In our daily lives, images are among the most commonly found data which we need to handle. We present iGraph, a graph-based approach for visual analytics of large image collections and their associated text information. Given such a collection, we compute the similarity between images, the distance between texts, and the connection between image and text to construct iGraph, a compound graph representation which encodes the underlying relationships among these images and texts. To enable effective visual navigation and comprehension of iGraph with tens of thousands of nodes and hundreds of millions of edges, we present a progressive solution that offers collection overview, node comparison, and visual recommendation. Our solution not only allows users to explore the entire collection with representative images and keywords but also supports detailed comparison for understanding and intuitive guidance for navigation. The visual exploration of iGraph is further enhanced with the implementation of bubble sets to highlight group memberships of nodes, suggestion of abnormal keywords or time periods based on text outlier detection, and comparison of four different recommendation solutions. For performance speedup, multiple graphics processing units and central processing units are utilized for processing and visualization in parallel. We experiment with two image collections and leverage a cluster driving a display wall of nearly 50million pixels. We show the effectiveness of our approach by demonstrating experimental results and conducting a user study.
C1 [Gu, Yi; Wang, Chaoli] Univ Notre Dame, Dept Comp Sci & Engn, 384 Fitzpatrick Hall, Notre Dame, IN 46556 USA.
[Ma, Jun] Michigan Technol Univ, Dept Comp Sci, Houghton, MI 49931 USA.
[Nemiroff, Robert J.] Michigan Technol Univ, Dept Phys, Houghton, MI 49931 USA.
[Kao, David L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Parra, Denis] Pontificia Univ Catolica Chile, Dept Ciencia Comp, Santiago, Chile.
EM chaoli.wang@nd.edu
FU U.S. National Science Foundation [IIS-1017935, IIS-1456763,
IIS-1455886]; FONDECYT [11150783]
FX The author(s) disclosed receipt of the following financial support for
the research, authorship, and/or publication of this article: This
research was supported, in part, by the U.S. National Science Foundation
through grants IIS-1017935, IIS-1456763, IIS-1455886, and the Notre Dame
Andronico Luksic Grants Program. Denis Parra was supported by FONDECYT
Grant 11150783.
NR 75
TC 0
Z9 0
U1 7
U2 7
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 1473-8716
EI 1473-8724
J9 INFORM VISUAL
JI Inf. Vis.
PD JAN
PY 2017
VL 16
IS 1
BP 21
EP 47
DI 10.1177/1473871616630778
PG 27
WC Computer Science, Software Engineering
SC Computer Science
GA EI6MB
UT WOS:000392608700002
ER
PT J
AU Sorek-Hamer, M
Broday, DM
Chatfield, R
Esswein, R
Stafoggia, M
Lepeule, J
Lyapustin, A
Kloog, I
AF Sorek-Hamer, Meytar
Broday, David M.
Chatfield, Robert
Esswein, Robert
Stafoggia, Massimo
Lepeule, Johanna
Lyapustin, Alexei
Kloog, Itai
TI Monthly analysis of PM ratio characteristics and its relation to AOD
SO JOURNAL OF THE AIR & WASTE MANAGEMENT ASSOCIATION
LA English
DT Article
ID AEROSOL OPTICAL DEPTH; FINE PARTICULATE MATTER; COMPONENT
CONCENTRATIONS; PM2.5 CONCENTRATIONS; SATELLITE DATA; MODIS; RETRIEVALS;
PREDICTIONS; PRODUCTS; NETWORK
AB Airborne particulate matter (PM) is derived from diverse sources-natural and anthropogenic. Climate change processes and remote sensing measurements are affected by the PM properties, which are often lumped into homogeneous size fractions that show spatiotemporal variation. Since different sources are attributed to different geographic locations and show specific spatial and temporal PM patterns, we explored the spatiotemporal characteristics of the PM2.5/PM10 ratio in different areas. Furthermore, we examined the statistical relationships between AERONET aerosol optical depth (AOD) products, satellite-based AOD, and the PM ratio, as well as the specific PM size fractions. PM data from the northeastern United States, from San Joaquin Valley, CA, and from Italy, Israel, and France were analyzed, as well as the spatial and temporal co-measured AOD products obtained from the MultiAngle Implementation of Atmospheric Correction (MAIAC) algorithm. Our results suggest that when both the AERONET AOD and the AERONET fine-mode AOD are available, the AERONET AOD ratio can be a fair proxy for the ground PM ratio. Therefore, we recommend incorporating the fine-mode AERONET AOD in the calibration of MAIAC. Along with a relatively large variation in the observed PM ratio (especially in the northeastern United States), this shows the need to revisit MAIAC assumptions on aerosol microphysical properties, and perhaps their seasonal variability, which are used to generate the look-up tables and conduct aerosol retrievals. Our results call for further scrutiny of satellite-borne AOD, in particular its errors, limitations, and relation to the vertical aerosol profile and the particle size, shape, and composition distribution. This work is one step of the required analyses to gain better understanding of what the satellite-based AOD represents.
Implications: The analysis results recommend incorporating the fine-mode AERONET AOD in MAIAC calibration. Specifically, they indicate the need to revisit MAIAC regional aerosol microphysical model assumptions used to generate look-up tables (LUTs) and conduct retrievals. Furthermore, relatively large variations in measured PM ratio shows that adding seasonality in aerosol microphysics used in LUTs, which is currently static, could also help improve accuracy of MAIAC retrievals. These results call for further scrutiny of satellite-borne AOD for better understanding of its limitations and relation to the vertical aerosol profile and particle size, shape, and composition.
C1 [Sorek-Hamer, Meytar; Broday, David M.] Technion Israel Inst, Fac Civil & Environm Engn, IL-32000 Haifa, Israel.
[Sorek-Hamer, Meytar; Kloog, Itai] Ben Gurion Univ Negev, Dept Geog & Environm Dev, Beer Sheva, Israel.
[Chatfield, Robert; Esswein, Robert] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Stafoggia, Massimo] Lazio Reg Hlth Serv Rome, Dept Epidemiol, Rome, Italy.
[Lepeule, Johanna] INSERM, Grenoble, France.
[Lepeule, Johanna] Univ Grenoble Alpes, IAB U1209, Team Environm Epidemiol, Grenoble, France.
[Lyapustin, Alexei] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
EM meytar@tx.technion.ac.il
OI Broday, David/0000-0002-6525-3979
NR 41
TC 0
Z9 0
U1 6
U2 6
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA
SN 1096-2247
EI 2162-2906
J9 J AIR WASTE MANAGE
JI J. Air Waste Manage. Assoc.
PY 2017
VL 67
IS 1
BP 27
EP 38
DI 10.1080/10962247.2016.1208121
PG 12
WC Engineering, Environmental; Environmental Sciences; Meteorology &
Atmospheric Sciences
SC Engineering; Environmental Sciences & Ecology; Meteorology & Atmospheric
Sciences
GA EI7ED
UT WOS:000392659700004
PM 27589199
ER
PT J
AU Tang, CH
Coull, BA
Schwartz, J
Lyapustin, AI
Di, Q
Koutrakis, P
AF Tang, Chia-Hsi
Coull, Brent A.
Schwartz, Joel
Lyapustin, Alexei I.
Di, Qian
Koutrakis, Petros
TI Developing particle emission inventories using remote sensing (PEIRS)
SO JOURNAL OF THE AIR & WASTE MANAGEMENT ASSOCIATION
LA English
DT Article
ID AEROSOL OPTICAL DEPTH; AIR-POLLUTION; PM2.5 CONCENTRATIONS; DAILY
DEATHS; LUNG-CANCER; MORTALITY; ASSOCIATION; RETRIEVALS; REANALYSIS;
ADMISSIONS
AB Information regarding the magnitude and distribution of PM2.5 emissions is crucial in establishing effective PM regulations and assessing the associated risk to human health and the ecosystem. At present, emission data is obtained from measured or estimated emission factors of various source types. Collecting such information for every known source is costly and time-consuming. For this reason, emission inventories are reported periodically and unknown or smaller sources are often omitted or aggregated at large spatial scale. To address these limitations, we have developed and evaluated a novel method that uses remote sensing data to construct spatially resolved emission inventories for PM2.5. This approach enables us to account for all sources within a fixed area, which renders source classification unnecessary. We applied this method to predict emissions in the northeastern United States during the period 2002-2013 using high-resolution 1 km x 1 km aerosol optical depth (AOD). Emission estimates moderately agreed with the EPA National Emission Inventory (R-2 = 0.66-0.71, CV = 17.7-20%). Predicted emissions are found to correlate with land use parameters, suggesting that our method can capture emissions from land-use-related sources. In addition, we distinguished small-scale intra-urban variation in emissions reflecting distribution of metropolitan sources. In essence, this study demonstrates the great potential of remote sensing data to predict particle source emissions cost-effectively.
Implications: We present a novel method, particle emission inventories using remote sensing (PEIRS), using remote sensing data to construct spatially resolved PM2.5 emission inventories. Both primary emissions and secondary formations are captured and predicted at a high spatial resolution of 1 km x 1 km. Using PEIRS, large and comprehensive data sets can be generated cost-effectively and can inform development of air quality regulations.
C1 [Tang, Chia-Hsi; Schwartz, Joel; Di, Qian; Koutrakis, Petros] Harvard TH Chan Sch Publ Hlth, Dept Environm Hlth, 401 Pk Dr, Boston, MA 02215 USA.
[Coull, Brent A.] Harvard TH Chan Sch Publ Hlth, Dept Biostat, Boston, MA USA.
[Lyapustin, Alexei I.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
EM cht710@mail.harvard.edu
FU U.S. EPA [RD83479801]
FX This publication was made possible by U.S. EPA grant RD83479801. Its
contents are solely the responsibility of the grantee and do not
necessarily represent the official views of the U.S. EPA. Further, the
U.S. EPA does not endorse the purchase of any commercial products or
services mentioned in the publication.
NR 31
TC 1
Z9 1
U1 5
U2 5
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA
SN 1096-2247
EI 2162-2906
J9 J AIR WASTE MANAGE
JI J. Air Waste Manage. Assoc.
PY 2017
VL 67
IS 1
BP 53
EP 63
DI 10.1080/10962247.2016.1214630
PG 11
WC Engineering, Environmental; Environmental Sciences; Meteorology &
Atmospheric Sciences
SC Engineering; Environmental Sciences & Ecology; Meteorology & Atmospheric
Sciences
GA EI7ED
UT WOS:000392659700007
PM 27653469
ER
PT J
AU Choker, M
Baghdadi, N
Zribi, M
El Hajj, M
Paloscia, S
Verhoest, NEC
Lievens, H
Mattia, F
AF Choker, Mohammad
Baghdadi, Nicolas
Zribi, Mehrez
El Hajj, Mohammad
Paloscia, Simonetta
Verhoest, Niko E. C.
Lievens, Hans
Mattia, Francesco
TI Evaluation of the Oh, Dubois and IEM Backscatter Models Using a Large
Dataset of SAR Data and Experimental Soil Measurements
SO Water
LA English
DT Article
DE Oh; Dubois; IEM; AIEM; SAR images; soil moisture; surface roughness
ID INTEGRAL-EQUATION MODEL; BARE AGRICULTURAL FIELDS; SYNTHETIC-APERTURE
RADAR; TERRASAR-X DATA; L-BAND SAR; SIR-C/X-SAR; SURFACE-ROUGHNESS;
SEMIEMPIRICAL CALIBRATION; MOISTURE ESTIMATION; CORRELATION LENGTH
AB The aim of this paper is to evaluate the most used radar backscattering models (Integral Equation Model "IEM", Oh, Dubois, and Advanced Integral Equation Model "AIEM") using a wide dataset of SAR (Synthetic Aperture Radar) data and experimental soil measurements. These forward models reproduce the radar backscattering coefficients (sigma(0)) from soil surface characteristics (dielectric constant, roughness) and SAR sensor parameters (radar wavelength, incidence angle, polarization). The analysis dataset is composed of AIRSAR, SIR-C, JERS-1, PALSAR-1, ESAR, ERS, RADARSAT, ASAR and TerraSAR-X data and in situ measurements (soil moisture and surface roughness). Results show that Oh model version developed in 1992 gives the best fitting of the backscattering coefficients in HH and VV polarizations with RMSE values of 2.6 dB and 2.4 dB, respectively. Simulations performed with the Dubois model show a poor correlation between real data and model simulations in HH polarization (RMSE = 4.0 dB) and better correlation with real data in VV polarization (RMSE = 2.9 dB). The IEM and the AIEM simulate the backscattering coefficient with high RMSE when using a Gaussian correlation function. However, better simulations are performed with IEM and AIEM by using an exponential correlation function (slightly better fitting with AIEM than IEM). Good agreement was found between the radar data and the simulations using the calibrated version of the IEM modified by Baghdadi (IEM_B) with bias less than 1.0 dB and RMSE less than 2.0 dB. These results confirm that, up to date, the IEM modified by Baghdadi (IEM_B) is the most adequate to estimate soil moisture and roughness from SAR data.
C1 [Choker, Mohammad; Baghdadi, Nicolas; El Hajj, Mohammad] Irstea Inst Natl Rech Sci & Technol Environm & Ag, UMR TETIS, 500 Rue Francois Breton, F-34093 Montpellier 5, France.
[Zribi, Mehrez] CESBIO, 18 Ave Edouard Belin,Bpi 2801, F-31401 Toulouse 9, France.
[Paloscia, Simonetta] CNR IFAC Natl Res Council, Inst Appl Phys, Via Madonna del Piano 10, I-50019 Florence, Italy.
[Verhoest, Niko E. C.; Lievens, Hans] Univ Ghent, Lab Hydrol & Water Management, B-9000 Ghent, Belgium.
[Lievens, Hans] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mattia, Francesco] CNR, ISSIA, Via Amendola 122-D, I-70126 Bari, Italy.
RP Choker, M (reprint author), Irstea Inst Natl Rech Sci & Technol Environm & Ag, UMR TETIS, 500 Rue Francois Breton, F-34093 Montpellier 5, France.
EM mohammad.choker@teledetection.fr; nicolas.baghdadi@teledetection.fr;
mehrez.zribi@ird.fr; mohammad.el-hajj@teledetection.fr;
s.paloscia@ifac.cnr.it; niko.verhoest@UGent.be; hans.lievens@UGent.be;
mattia@ba.issia.cnr.it
RI Verhoest, Niko/C-9726-2010;
OI Verhoest, Niko/0000-0003-4116-8881; baghdadi,
nicolas/0000-0002-9461-4120
FU IRSTEA (National Research Institute of Science and Technology for
Environment and Agriculture); French Space Study Center (CNES, TOSCA);
French ANR (ANR AMETHYST project); Belgian Science Policy Office
[SR/00/302]
FX Authors are grateful to the space agencies for kindly providing the
AIRSAR, SIR-C, JERS-1, ERS-1/2, RADARSAT-1/2, ASAR, PALSAR-1,
TerraSAR-X, COSMO-SkyMed, and ESAR data. This research is supported by
IRSTEA (National Research Institute of Science and Technology for
Environment and Agriculture), the French Space Study Center (CNES, TOSCA
2016), the French ANR (ANR AMETHYST project) and the Belgian Science
Policy Office (Contract SR/00/302). Hans Lievens is a postdoctoral
research of the Research Foundation Flanders (FWO).
NR 60
TC 0
Z9 0
U1 7
U2 7
PU MDPI AG
PI BASEL
PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND
SN 2073-4441
J9 WATER-SUI
JI Water
PD JAN
PY 2017
VL 9
IS 1
AR 38
DI 10.3390/w9010038
PG 27
WC Water Resources
SC Water Resources
GA EJ0ZN
UT WOS:000392939900038
ER
PT J
AU Provencal, S
Buchard, V
da Silva, AM
Leduc, R
Barrette, N
Elhacham, E
Wang, SH
AF Provencal, Simon
Buchard, Virginie
da Silva, Arlindo M.
Leduc, Richard
Barrette, Nathalie
Elhacham, Emily
Wang, Sheng-Hsiang
TI Evaluation of PM2.5 Surface Concentrations Simulated by Version 1 of
NASA's MERRA Aerosol Reanalysis over Israel and Taiwan
SO AEROSOL AND AIR QUALITY RESEARCH
LA English
DT Article
DE MERRAero; Evaluation; Fine particulate matter; Israel; Taiwan
ID SULFUR-DIOXIDE; UNITED-STATES; AIR-QUALITY; ATMOSPHERIC AEROSOLS;
CHEMICAL-COMPOSITION; PARTICULATE MATTER; MODEL PERFORMANCE; DAILY
MORTALITY; COASTAL AREA; EMISSIONS
AB Version 1 of the NASA MERRA Aerosol Reanalysis (MERRAero) assimilates bias-corrected aerosol optical depth (AOD) data from MODIS-Terra and MODIS-Aqua, and simulates particulate matter (PM) concentration data to reproduce a consistent database of AOD and PM concentration around the world from 2002 to the end of 2015. The purpose of this paper is to evaluate MERRAero's simulation of fine PM concentration against surface measurements in two regions of the world with relatively high levels of PM concentration but with profoundly different PM composition, those of Israel and Taiwan. Being surrounded by major deserts, Israel's PM load is characterized by a significant contribution of mineral dust, and secondary contributions of sea salt particles, given its proximity to the Mediterranean Sea, and sulfate particles originating from Israel's own urban activities and transported from Europe. Taiwan's PM load is composed primarily of anthropogenic particles (sulfate, nitrate and carbonaceous particles) locally produced or transported from China, with an additional contribution of springtime transport of mineral dust originating from Chinese and Mongolian deserts. The evaluation in Israel produced favorable results with MERRAero slightly overestimating measurements by 6% on average and reproducing an excellent year-to-year and seasonal fluctuation. The evaluation in Taiwan was less favorable with MERRAero underestimating measurements by 42% on average. Two likely reasons explain this discrepancy: emissions of anthropogenic PM and their precursors are largely uncertain in China, and MERRAero doesn't include nitrate particles in its simulation, a pollutant of predominately anthropogenic sources. MERRAero nevertheless simulates well the concentration of fine PM during the summer, when Taiwan is least affected by the advection of pollution from China.
C1 [Provencal, Simon; Leduc, Richard; Barrette, Nathalie] Univ Laval, Dept Geog, Quebec City, PQ, Canada.
[Buchard, Virginie; da Silva, Arlindo M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Buchard, Virginie] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA.
[Elhacham, Emily] Tel Aviv Univ, Dept Geophys Atmospher & Planetary Sci, Tel Aviv, Israel.
[Wang, Sheng-Hsiang] Natl Cent Univ, Dept Atmospher Sci, Taoyuan, Taiwan.
RP Provencal, S (reprint author), Univ Laval, Dept Geog, Quebec City, PQ, Canada.
EM simon.provencal.1@ulaval.ca
NR 43
TC 0
Z9 0
U1 5
U2 5
PU TAIWAN ASSOC AEROSOL RES-TAAR
PI TAICHUNG COUNTY
PA CHAOYANG UNIV TECH, DEPT ENV ENG & MGMT, PROD CTR AAQR, NO 168, JIFONG E
RD, WUFONG TOWNSHIP, TAICHUNG COUNTY, 41349, TAIWAN
SN 1680-8584
EI 2071-1409
J9 AEROSOL AIR QUAL RES
JI Aerosol Air Qual. Res.
PD JAN
PY 2017
VL 17
IS 1
BP 253
EP 261
DI 10.4209/aaqr.2016.04.0145
PG 9
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA EI2IX
UT WOS:000392311500023
ER
PT J
AU Gupta, KK
Choi, SB
Lung, SF
Ibrahim, A
AF Gupta, K. K.
Choi, S. B.
Lung, S. F.
Ibrahim, A.
TI Aerothermoelastic-Acoustics Simulation of Flight Vehicles
SO AIAA JOURNAL
LA English
DT Article
ID EULER; MESH
AB This paper describes a novel computational-fluid-dynamics-based numerical solution procedure for effective simulation of aerothermoacoustics problems with application to aerospace vehicles. A finite element idealization is employed for both fluid and structure domains, which fully accounts for thermal effects. The accuracies of both the fluid and structure capabilities are verified with flight-and ground-test data. A time integration of the structural equations of motion, with the governing flow equations, is conducted for the computation of the unsteady aerodynamic forces, which uses a transpiration boundary condition at the surface nodal points in lieu of the updating of the fluid mesh. Two example problems are presented herein to that effect. The first one relates to a cantilever wing with a NACA 0012 airfoil. The solution results demonstrate the effect of temperature loading that causes a significant increase in acoustic response. Asecond example, the hypersonic X-43 vehicle, is also analyzed; and relevant results are presented. The common finite element-based aerothermoelastic-acoustics simulation process, its applicability to the efficient and routine solution of complex practical problems, the employment of the effective transpiration boundary condition in the computational fluid dynamics solution, and the development and public domain distribution of an associated code are unique features of this paper.
C1 [Gupta, K. K.] NASA, Armstrong Flight Res Ctr, Res Engn Directorate, Edwardsville, IL 93523 USA.
[Choi, S. B.] Calif State Univ Los Angeles, Dept Mech Engn, Los Angeles, CA 90032 USA.
[Lung, S. F.] Jacobs Technol Inc, Struct Engn, Edwardsville, IL 93523 USA.
[Ibrahim, A.] Norfolk State Univ, Dept Engn, Norfolk, VA 23504 USA.
RP Gupta, KK (reprint author), NASA, Armstrong Flight Res Ctr, Res Engn Directorate, Edwardsville, IL 93523 USA.
NR 19
TC 0
Z9 0
U1 0
U2 0
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD JAN
PY 2017
VL 55
IS 1
BP 49
EP 56
DI 10.2514/1.J055088
PG 8
WC Engineering, Aerospace
SC Engineering
GA EI5CI
UT WOS:000392511000005
ER
PT J
AU Schaefer, J
Hosder, S
West, T
Rumsey, C
Carlson, JR
Kleb, W
AF Schaefer, John
Hosder, Serhat
West, Thomas
Rumsey, Christopher
Carlson, Jan-Renee
Kleb, William
TI Uncertainty Quantification of Turbulence Model Closure Coefficients for
Transonic Wall-Bounded Flows
SO AIAA JOURNAL
LA English
DT Article; Proceedings Paper
CT 22nd AIAA Computational Fluid Dynamics Conference
CY JUN 22-26, 2015
CL Dallas, TX
SP AIAA
ID COMPUTATIONAL FLUID-DYNAMICS; POLYNOMIAL CHAOS; SENSITIVITY-ANALYSIS;
SIMULATIONS; EXPANSIONS
AB The goal of this work is to quantify the uncertainty and sensitivity of commonly used turbulence models in Reynolds-averaged Navier-Stokes codes due to uncertainty in the values of closure coefficients for transonic wall-bounded flows and to rank the contribution of each coefficient to uncertainty in various output flow quantities of interest. Specifically, uncertainty quantification of turbulence model closure coefficients is performed for transonic flow over an axisymmetric bump and the RAE 2822 transonic airfoil. Three turbulence models are considered: the Spalart-Allmaras model, Wilcox (2006) k-omega model, and Menter shear-stress transport model. The FUN3D code developed by NASA Langley Research Center is used as the flow solver. The uncertainty quantification analysis employs stochastic expansions based on non-intrusive polynomial chaos for efficient uncertainty propagation. Several integrated and point quantities are considered as uncertain outputs for both computational fluid dynamics problems. Closure coefficients are treated as epistemic uncertain variables represented with intervals. Sobol indices are used to rank the relative contributions of each closure coefficient to the total uncertainty in the output quantities of interest. This study identifies a number of closure coefficients for each turbulence model for which more information will reduce the amount of uncertainty in the output significantly for transonic wall-bounded flows.
C1 [Schaefer, John] Missouri Univ Sci & Technol, Dept Aerosp & Mech Engn, Rolla, MO 65409 USA.
[Hosder, Serhat] Missouri Univ Sci & Technol, Aerosp Engn, Dept Aerosp & Mech Engn, Rolla, MO 65409 USA.
[West, Thomas] NASA Langley Res Ctr, Vehicle Anal Branch, Syst Anal & Concepts Directorate, Hampton, VA 23681 USA.
[Rumsey, Christopher; Carlson, Jan-Renee; Kleb, William] NASA Langley Res Ctr, Computat Aerosci Branch, Res Directorate, Hampton, VA 23681 USA.
FU NASA [NNX14AN17A]; NASA Langley Research Center; Langley Aerospace
Research Student Scholars program
FX The support for the first and the second authors for this research is
provided under NASA Grant NNX14AN17A (Mujeeb Malik, program monitor).
The first author would also like to thank the NASA Langley Research
Center and the 2014 Langley Aerospace Research Student Scholars program
for additional support. The authors would like to give special thanks to
Philippe Spalart, David Wilcox, Florian Menter, and Gary Coleman for
their contributions to this research. Thanks to Aaron Erb for his help
preparing certain figures.
NR 41
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PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
EI 1533-385X
J9 AIAA J
JI AIAA J.
PD JAN
PY 2017
VL 55
IS 1
BP 195
EP 213
DI 10.2514/1.J054902
PG 19
WC Engineering, Aerospace
SC Engineering
GA EI5CI
UT WOS:000392511000018
ER
PT J
AU Amblard, A
Temi, P
Gaspari, M
Brighenti, F
AF Amblard, A.
Temi, P.
Gaspari, M.
Brighenti, F.
TI SPECTRAL ENERGY DISTRIBUTION MAPPING OF TWO ELLIPTICAL GALAXIES ON
SUB-kpc SCALES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: elliptical and lenticular,cD; galaxies: ISM; infrared:
galaxies; infrared: ISM
ID STELLAR POPULATION GRADIENTS; LARGE GALACTOCENTRIC RADII; STAR-FORMATION
HISTORIES; MOLECULAR CLOUD CONTENT; LINE-STRENGTH INDEXES; IONIZED-GAS;
ATLAS(3D) PROJECT; METALLICITY GRADIENTS; BLACK-HOLES; HOT GAS
AB We use high-resolution Herschel-PACS data of two nearby elliptical galaxies, IC 1459 and NGC 2768, to characterize their dust and stellar content. IC 1459 and NGC 2768 have an unusually large amount of dust for elliptical galaxies ((1-3) x 10(5) M-circle dot); this dust is also not distributed along the stellar content. Using data from GALEX (ultra-violet) to PACS (far-infrared, FIR), we analyze the spectral energy distribution (SED) of these galaxies with CIGALEMC as a function of the projected position, binning images in 7 ''.2 pixels. From this analysis, we derive maps of SED parameters, such as the metallicity, the stellar mass, the fraction of young stars, and the dust mass. The larger amount of dust in FIR maps seems related in our model to a larger fraction of young stars which can reach up to 4% in the dustier area. The young stellar population is fitted as a recent (similar to 0.5 Gyr) short burst of star formation for both galaxies. The metallicities, which are fairly large at the center of both galaxies, decrease with the radial distance with a fairly steep gradient for elliptical galaxies.
C1 [Amblard, A.; Temi, P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Amblard, A.] BAER Inst, Sonoma, CA USA.
[Gaspari, M.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Brighenti, F.] Univ Bologna, Dept Astron, Via Ranzani 1, I-40127 Bologna, Italy.
RP Amblard, A (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
FU National Aeronautics and Space Administration; National Science
Foundation; Alfred P. Sloan Foundation; U.S. Department of Energy Office
of Science; University of Arizona; Brazilian Participation Group;
Brookhaven National Laboratory; University of Cambridge; Carnegie Mellon
University; University of Florida; French Participation Group; German
Participation Group; Harvard University; Instituto de Astrofisica de
Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns
Hopkins University; Lawrence Berkeley National Laboratory; Max Planck
Institute for Astrophysics; Max Planck Institute for Extraterrestrial
Physics; New Mexico State University; New York University; Ohio State
University; Pennsylvania State University; University of Portsmouth;
Princeton University; Spanish Participation Group; University of Tokyo;
University of Utah; Vanderbilt University; University of Virginia;
University of Washington; Yale University; NASA through Einstein
Postdoctoral Fellowship [PF-160137]; NASA [NAS8-03060]
FX This publication makes use of data products from the Two Micron All Sky
Survey, which is a joint project of the University of Massachusetts and
the Infrared Processing and Analysis Center/California Institute of
Technology, funded by the National Aeronautics and Space Administration
and the National Science Foundation. This publication makes use of data
from SDSS-III. Funding for SDSS-III has been provided by the Alfred P.
Sloan Foundation, the Participating Institutions, the National Science
Foundation, and the U.S. Department of Energy Office of Science. The
SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the
Astrophysical Research Consortium for the Participating Institutions of
the SDSS-III Collaboration including the University of Arizona, the
Brazilian Participation Group, Brookhaven National Laboratory,
University of Cambridge, Carnegie Mellon University, University of
Florida, the French Participation Group, the German Participation Group,
Harvard University, the Instituto de Astrofisica de Canarias, the
Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins
University, Lawrence Berkeley National Laboratory, Max Planck Institute
for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New
Mexico State University, New York University, Ohio State University,
Pennsylvania State University, University of Portsmouth, Princeton
University, the Spanish Participation Group, University of Tokyo,
University of Utah, Vanderbilt University, University of Virginia,
University of Washington, and Yale University. This work is based in
part on observations made with the Spitzer Space Telescope, which is
operated by the Jet Propulsion Laboratory, California Institute of
Technology under a contract with NASA. This work is based in part on
observations made with the NASA Galaxy Evolution Explorer. GALEX is
operated for NASA by the California Institute of Technology under NASA
contract. This research has made use of the NASA/IPAC Extragalactic
Database (NED) which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration. MG is supported by NASA through
Einstein Postdoctoral Fellowship Award Number PF-160137 issued by the
Chandra X-ray Observatory Center, which is operated by the SAO for and
on behalf of NASA under contract NAS8-03060.
NR 124
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 1
PY 2017
VL 834
IS 1
AR 20
DI 10.3847/1538-4357/834/1/20
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EH6GR
UT WOS:000391871500008
ER
PT J
AU Ciardi, DR
Beichman, CA
Horch, EP
Howell, SB
AF Ciardi, David R.
Beichman, Charles A.
Horch, Elliott P.
Howell, Steve B.
TI UNDERSTANDING THE EFFECTS OF STELLAR MULTIPLICITY ON THE DERIVED PLANET
RADII FROM TRANSIT SURVEYS: IMPLICATIONS FOR KEPLER, K2, AND TESS (vol
805, 16, 2015)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
AB There was an error in the published version of Equation (6); the equation should read as
X-R equivalent to R-p(true)/R-p(observed) = (R-t star/R-1 star)root F-total/F-t. (6)
The calculations and results presented in the paper utilized the correct form of the equation and are unaffected by the error in the equation. The authors sincerely regret the error.
C1 [Ciardi, David R.; Beichman, Charles A.] Caltech Pasadena, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Horch, Elliott P.] Southern Connecticut State Univ, Dept Phys, New Haven, CT USA.
[Howell, Steve B.] NASA, Ames Res Ctr, Mountain View, CA USA.
RP Ciardi, DR (reprint author), Caltech Pasadena, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
EM ciardi@ipac.caltech.edu
NR 1
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U1 0
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 1
PY 2017
VL 834
IS 1
AR 96
DI 10.3847/1538-4357/834/1/96
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EI0HB
UT WOS:000392152700025
ER
PT J
AU Fischer, TC
Machuca, C
Diniz, MR
Crenshaw, DM
Kraemer, SB
Riffel, RA
Schmitt, HR
Baron, F
Storchi-Bergmann, T
Straughn, AN
Revalski, M
Pope, CL
AF Fischer, Travis C.
Machuca, C.
Diniz, M. R.
Crenshaw, D. M.
Kraemer, S. B.
Riffel, R. A.
Schmitt, H. R.
Baron, F.
Storchi-Bergmann, T.
Straughn, A. N.
Revalski, M.
Pope, C. L.
TI GEMINI NEAR INFRARED FIELD SPECTROGRAPH OBSERVATIONS OF THE SEYFERT 2
GALAXY MRK 573: IN SITU ACCELERATION OF IONIZED AND MOLECULAR GAS OFF
FUELING FLOWS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (Mrk 573); galaxies: kinematics
and dynamics; galaxies: Seyfert
ID NARROW-LINE REGION; ACTIVE GALACTIC NUCLEI; SPACE-TELESCOPE
OBSERVATIONS; MASS OUTFLOWS; IFU OBSERVATIONS; HOST GALAXIES;
KINEMATICS; FEEDBACK; II.; STELLAR
AB We present near-infrared and optical emission-line and stellar kinematics of the Seyfert 2 galaxy Mrk 573 using the Near-Infrared Field Spectrograph (NIFS) at Gemini North and Dual Imaging Spectrograph at Apache Point Observatory, respectively. By obtaining full kinematic maps of the infrared ionized and molecular gas and stellar kinematics in a similar to 700. x. 2100. pc(2) circumnuclear region of Mrk. 573, we find that kinematics within the NarrowLine Region are largely due to a combination of both rotation and in situ acceleration of material originating in the host disk. Combining these observations with large-scale, optical long-slit spectroscopy that traces ionized gas emission out to several kpcs, we find that rotation kinematics dominate the majority of the gas. We find that outflowing gas extends to distances less than 1 kpc, suggesting that outflows in Seyfert galaxies may not be powerful enough to evacuate their entire bulges.
C1 [Fischer, Travis C.; Straughn, A. N.] Goddard Space Flight Ctr, Astrophys Sci Div, Code 665, Greenbelt, MD 20771 USA.
[Machuca, C.; Crenshaw, D. M.; Baron, F.; Revalski, M.; Pope, C. L.] Georgia State Univ, Astron Off, Dept Phys & Astron, 25 Pk Pl,Suite 605, Atlanta, GA 30303 USA.
[Diniz, M. R.; Riffel, R. A.] Univ Fed Santa Maria, Ctr Ciencias Nat Exatas, Dept Fis, BR-97105900 Santa Maria, RS, Brazil.
[Kraemer, S. B.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Dept Phys, Washington, DC 20064 USA.
[Schmitt, H. R.] Naval Res Lab, Washington, DC 20375 USA.
[Storchi-Bergmann, T.] Univ Fed Rio Grande do Sul, Dept Astron, IF, CP 15051, BR-91501970 Porto Alegre, RS, Brazil.
RP Fischer, TC (reprint author), Goddard Space Flight Ctr, Astrophys Sci Div, Code 665, Greenbelt, MD 20771 USA.
EM travis.c.fischer@nasa.gov
FU NASA Postdoctoral Program at the NASA Goddard Space Flight Center;
National Science Foundation [1211651]
FX The authors would like to thank the anonymous referee for their helpful
comments. T.C.F. was supported by an appointment to the NASA
Postdoctoral Program at the NASA Goddard Space Flight Center,
administered by Universities Space Research Association under contract
with NASA. This material is also based on work supported by the National
Science Foundation under grant No. 1211651. This study was based on
observations obtained at the Gemini Observatory (processed using the
Gemini IRAF package), which is operated by the Association of
Universities for Research in Astronomy, Inc., under a cooperative
agreement with the NSF on behalf of the Gemini partnership: the National
Science Foundation (United States), the National Research Council
(Canada), CONICYT (Chile), the Australian Research Council (Australia),
Ministerio da Ciencia, Tecnologia e Inovacao (Brazil) and Ministerio de
Ciencia, Tecnologia e Innovacion Productiva (Argentina).
NR 63
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 1
PY 2017
VL 834
IS 1
AR 30
DI 10.3847/1538-4357/834/1/30
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EH7ZM
UT WOS:000391991200002
ER
PT J
AU Furst, F
Walton, DJ
Stern, D
Bachetti, M
Barret, D
Brightman, M
Harrison, FA
Rana, V
AF Furst, F.
Walton, D. J.
Stern, D.
Bachetti, M.
Barret, D.
Brightman, M.
Harrison, F. A.
Rana, V.
TI SPECTRAL CHANGES IN THE HYPERLUMINOUS PULSAR IN NGC 5907 AS A FUNCTION
OF SUPER-ORBITAL PHASE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; pulsars: individual (NGC 5907 ULX1); X-rays:
binaries
ID X-RAY SOURCE; XMM-NEWTON OBSERVATIONS; PHOTON IMAGING CAMERA;
BLACK-HOLES; BROAD-BAND; ULTRALUMINOUS STATE; ACCRETION DISKS;
NEUTRON-STARS; GX 339-4; 1313 X-1
AB We present broadband, multi-epoch X-ray spectroscopy of the pulsating ultra-luminous X-ray source (ULX) in NGC 5907. Simultaneous XMM-Newton and NuSTAR data from 2014 are best described by a multicolor blackbody model with a temperature gradient as a function of accretion disk radius significantly flatter than expected for a standard thin accretion disk (T(r) proportional to r(-p), with p = 0.608(-0.012)(+0.014)). Additionally, we detect a hard power-law tail at energies above 10 keV, which we interpret as being due to Comptonization. We compare this observation to archival XMM-Newton, Chandra, and NuSTAR data from 2003, 2012, and 2013, and investigate possible spectral changes as a function of phase over the 78-day. super-orbital period of this source. We find that observations taken around phases 0.3-0.4 show very similar temperature profiles, even though the observed flux varies significantly, while one observation taken around phase 0 has a significantly steeper profile. We discuss these findings in light of the recent discovery that the compact object is a neutron star and show that precession of the accretion disk or the neutron star can self-consistently explain most observed phenomena.
C1 [Furst, F.; Walton, D. J.; Brightman, M.; Harrison, F. A.; Rana, V.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Furst, F.] European Space Astron Ctr ESA ESAC, Sci Operat Dept, Villanueva De La Canada, Madrid, Spain.
[Walton, D. J.; Stern, D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Walton, D. J.] Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Bachetti, M.] Osservatorio Astron Cagliari, INAF, Via Sci 5, I-09047 Selargius, CA, Italy.
[Barret, D.] CNRS, IRAP, 9 Ave Colonel Roche,BP 44346, F-31028 Toulouse 4, France.
RP Furst, F (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.; Furst, F (reprint author), European Space Astron Ctr ESA ESAC, Sci Operat Dept, Villanueva De La Canada, Madrid, Spain.
EM fuerst@caltech.edu
OI Bachetti, Matteo/0000-0002-4576-9337; Rana, Vikram/0000-0003-1703-8796;
Walton, Dominic/0000-0001-5819-3552
FU ESA Member States; NASA [NNG08FD60C]; National Aeronautics and Space
Administration
FX We thank the referee for useful comments that helped to improve the
manuscript. Based on observations obtained with XMM-Newton, an ESA
science mission with instruments and contributions directly funded by
ESA Member States and NASA. This work was supported under NASA Contract
No. NNG08FD60C. and made use of data from the NuSTAR mission, a project
led by the California Institute of Technology, managed by the Jet
Propulsion Laboratory, and funded by the National Aeronautics and Space
Administration. We thank the NuSTAR Operations, Software and Calibration
teams for support with the execution and analysis of these observations.
This research has made use of the NuSTAR Data Analysis Software
(NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC,
Italy) and the California Institute of Technology (USA). This work made
use of data supplied by the UK Swift Science Data Centre at the
University of Leicester. This research has made use of a collection of
ISIS functions (ISISscripts) provided by ECAP/Remeis observatory and MIT
(http://www.sternwarte.uni-erlangen.de/isis/). We would like to thank
John E. Davis for the slxfig module, which was used to produce all
figures in this work. The. Swift/BAT transient monitor results were
provided by the Swift/BAT team.
NR 60
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 1
PY 2017
VL 834
IS 1
AR 77
DI 10.3847/1538-4357/834/1/77
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EI0HB
UT WOS:000392152700006
ER
PT J
AU Grefenstette, BW
Fryer, CL
Harrison, FA
Boggs, SE
DeLaney, T
Laming, JM
Reynolds, SP
Alexander, DM
Barret, D
Christensen, FE
Craig, WW
Forster, K
Giommi, P
Hailey, CJ
Hornstrup, A
Kitaguchi, T
Koglin, JE
Lopez, L
Mao, PH
Madsen, KK
Miyasaka, H
Mori, K
Perri, M
Pivovaroff, MJ
Puccetti, S
Rana, V
Stern, D
Westergaard, NJ
Wik, DR
Zhang, WW
Zoglauer, A
AF Grefenstette, Brian W.
Fryer, Chris L.
Harrison, Fiona A.
Boggs, Steven E.
DeLaney, Tracey
Laming, J. Martin
Reynolds, Stephen P.
Alexander, David M.
Barret, Didier
Christensen, Finn E.
Craig, William W.
Forster, Karl
Giommi, Paolo
Hailey, Charles J.
Hornstrup, Alan
Kitaguchi, Takao
Koglin, J. E.
Lopez, Laura
Mao, Peter H.
Madsen, Kristin K.
Miyasaka, Hiromasa
Mori, Kaya
Perri, Matteo
Pivovaroff, Michael J.
Puccetti, Simonetta
Rana, Vikram
Stern, Daniel
Westergaard, Niels J.
Wik, Daniel R.
Zhang, William W.
Zoglauer, Andreas
TI THE DISTRIBUTION OF RADIOACTIVE Ti-44 IN CASSIOPEIA A
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma rays: general; ISM: supernova remnants; nuclear reactions,
nucleosynthesis, abundances; X-rays: individual (Cassiopeia A)
ID CORE-COLLAPSE SUPERNOVAE; RAY EMISSION-LINES; 3-DIMENSIONAL STRUCTURE;
REMNANT CASSIOPEIA; NEUTRON-STAR; CAS-A; EJECTA; EXPLOSION; CONSTRAINTS;
ENERGY
AB The distribution of elements produced in the innermost layers of a supernova explosion is a key diagnostic for studying the collapse of massive stars. Here we present the results of a 2.4 Ms NuSTAR observing campaign aimed at studying the supernova remnant Cassiopeia A (Cas A). We perform spatially resolved spectroscopic analyses of the Ti-44 ejecta, which we use to determine the Doppler shift and thus the three-dimensional (3D) velocities of the 44Ti ejecta. We find an initial Ti-44 mass of (1.54 +/- 0.21) x 10(-4) M-circle dot, which has a present-day average momentum direction of 340 degrees +/- 15 degrees projected onto the plane of the sky (measured clockwise from celestial north) and is tilted by 58 degrees +/- 20 degrees into the plane of the sky away from the observer, roughly opposite to the inferred direction of motion of the central compact object. We find some Ti-44 ejecta that are clearly interior to the reverse shock and some that are clearly exterior to it. Where we observe Ti-44 ejecta exterior to the reverse shock we also see shock-heated iron; however, there are regions where we see iron but do not observe Ti-44. This suggests that the local conditions of the supernova shock during explosive nucleosynthesis varied enough to suppress the production of Ti-44 by at least a factor of two in some regions, even in regions that are assumed to be the result of processes like alpha-rich freezeout that should produce both iron and titanium.
C1 [Grefenstette, Brian W.; Harrison, Fiona A.; Forster, Karl; Mao, Peter H.; Madsen, Kristin K.; Miyasaka, Hiromasa; Rana, Vikram] CALTECH, Cahill Ctr Astrophys, 1216 E Calif Blvd, Pasadena, CA 91125 USA.
[Fryer, Chris L.] Los Alamos Natl Lab, CCS 2, Los Alamos, NM 87545 USA.
[Boggs, Steven E.; Craig, William W.; Zoglauer, Andreas] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[DeLaney, Tracey] West Virginia Wesleyan Coll, Phys & Engn Dept, Buckhannon, WV 26201 USA.
[Laming, J. Martin] Naval Res Lab, Div Space Sci, Code 7684, Washington, DC 20375 USA.
[Reynolds, Stephen P.] NC State Univ, Dept Phys, Raleigh, NC 27695 USA.
[Alexander, David M.] Univ Durham, Dept Phys, Ctr Extragalact Astron, Durham DH1 3LE, England.
[Barret, Didier] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Barret, Didier] CNRS, Inst Rech Astrophys & Planetol, 9 Ave Colonel Roche,BP 44346, F-31028 Toulouse 4, France.
[Christensen, Finn E.; Hornstrup, Alan; Westergaard, Niels J.] Tech Univ Denmark, DTU Space Natl Space Inst, Elektrovej 327, DK-2800 Lyngby, Denmark.
[Craig, William W.; Pivovaroff, Michael J.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Giommi, Paolo; Perri, Matteo; Puccetti, Simonetta] ASI Sci Data Ctr ASDC, Via Politecn, I-00133 Rome, Italy.
[Hailey, Charles J.; Mori, Kaya] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Kitaguchi, Takao] Hiroshima Univ, Dept Phys Sci, 1-3-1 Kagamiyama, Higashihiroshima, Hiroshima 7398526, Japan.
[Koglin, J. E.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA.
[Lopez, Laura] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Lopez, Laura] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Perri, Matteo; Puccetti, Simonetta] INAF Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, Italy.
[Stern, Daniel] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Wik, Daniel R.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Wik, Daniel R.; Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Grefenstette, BW (reprint author), CALTECH, Cahill Ctr Astrophys, 1216 E Calif Blvd, Pasadena, CA 91125 USA.
EM bwgref@srl.caltech.edu
FU NASA [NNG08FD60C, NNH16AC24I]
FX We would like thank Dan Milisavljevic for providing the [S III] data
files, as well as Thomas Janka, Raph Hix, and Adam Burrows for their
helpful comments. This work was supported under NASA contract NNG08FD60C
and made use of data from the NuSTAR mission, a project led by the
California Institute of Technology, managed by the Jet Propulsion
Laboratory, and funded by NASA. J.M.L. was supported by the NASA ADAP
grant NNH16AC24I.
NR 52
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U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 1
PY 2017
VL 834
IS 1
AR 19
DI 10.3847/1538-4357/834/1/19
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EH6GR
UT WOS:000391871500007
ER
PT J
AU Han, C
Udalski, A
Gould, A
Zhu, W
Szymanski, MK
Soszynski, I
Skowron, J
Mroz, P
Poleski, R
Pietrukowicz, P
Kozlowski, S
Ulaczyk, K
Pawlak, M
Yee, JC
Beichman, C
Novati, SC
Carey, S
Bryden, C
Fausnaugh, M
Gaudi, BS
Henderson, CB
Shvartzvald, Y
Wibking, B
AF Han, C.
Udalski, A.
Gould, A.
Zhu, Wei
Szymanski, M. K.
Soszynski, I.
Skowron, J.
Mroz, P.
Poleski, R.
Pietrukowicz, P.
Kozlowski, S.
Ulaczyk, K.
Pawlak, M.
Yee, J. C.
Beichman, C.
Novati, S. Calchi
Carey, S.
Bryden, C.
Fausnaugh, M.
Gaudi, B. S.
Henderson, Calen B.
Shvartzvald, Y.
Wibking, B.
CA OGLE Collaboration
Spitzer Microlensing Team
TI OGLE-2015-BLG-0196: GROUND-BASED GRAVITATIONAL MICROLENS PARALLAX
CONFIRMED BY SPACE-BASED OBSERVATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; gravitational lensing: micro
ID SPITZER OBSERVATIONS; BINARY-LENS; GALACTIC BULGE; SATELLITE MASS;
OGLE-III; PHOTOMETRY; DISTANCES; SYSTEMS; EVENTS; PLANET
AB In this paper, we present an analysis of the binary gravitational microlensing event OGLE-2015-BLG-0196. The event lasted for almost a year, and the light curve exhibited significant deviations from the lensing model based on the rectilinear lens-source relative motion, enabling us to measure the microlens parallax. The ground-based microlens parallax is confirmed by the data obtained from space-based microlens observations using the Spitzer telescope. By additionally measuring the angular Einstein radius from the analysis of the resolved caustic crossing, the physical parameters of the lens are determined up to the twofold degeneracy, u(0) < 0 and u(0) > 0, solutions caused by the well-known "ecliptic" degeneracy. It is found that the binary lens is composed of two M dwarf stars with similar masses, M-1 = 0.38 +/- 0.04M(circle plus) (0.50 +/- 0.05M(circle plus)) and M-2 = 0.38 +/- 0.04M(circle plus) (0.55 +/- 0.06M(circle plus)), and the distance to the lens is D-L = 2.77. +/- 0.23 kpc (3.30 +/- 0.29 kpc). Here the physical parameters outside and inside the parentheses are for the u(0) < 0 and u(0) > 0 solutions, respectively.
C1 [Han, C.] Chungbuk Natl Univ, Dept Phys, Cheongju 361763, South Korea.
[Udalski, A.; Szymanski, M. K.; Soszynski, I.; Skowron, J.; Mroz, P.; Poleski, R.; Pietrukowicz, P.; Kozlowski, S.; Ulaczyk, K.; Pawlak, M.] Univ Warsaw Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland.
[Gould, A.; Zhu, Wei; Poleski, R.; Fausnaugh, M.; Gaudi, B. S.; Wibking, B.] Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA.
[Gould, A.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Yee, J. C.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Beichman, C.] CALTECH, NASA Exoplanet Sci Inst, MS 100-22, Pasadena, CA 91125 USA.
[Novati, S. Calchi] Univ Salerno, Dipartimento Fis ER Caianiello, Via Giovanni Paolo 2, I-84084 Fisciano, SA, Italy.
[Novati, S. Calchi] CALTECH, Ctr Infrared Proc & Anal, Mail Code 100-23,1200 E Calif Blvd, Pasadena, CA 91125 USA.
[Carey, S.] CALTECH, Spitzer Sci Ctr, MS 220-6, Pasadena, CA 91125 USA.
[Bryden, C.; Henderson, Calen B.; Shvartzvald, Y.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Han, C (reprint author), Chungbuk Natl Univ, Dept Phys, Cheongju 361763, South Korea.
FU Creative Research Initiative Program of National Research Foundation of
Korea [2009-0081561]; National Science Centre, Poland [MAESTRO
2014/14/A/ST9/00121]; JPL [1500811]; NSF [AST1516842]; NASA through
Sagan Fellowship Program; NASA
FX Work by C. Han was supported by the Creative Research Initiative Program
(2009-0081561) of National Research Foundation of Korea. The OGLE
project has received funding from the National Science Centre, Poland,
grant MAESTRO 2014/14/A/ST9/00121 to A.U. The OGLE Team thanks Profs. M.
Kubiak, G. Pietrzynski, and L. Wyrzykowski2, former members
of the OGLE Team, for their contribution to the collection of the OGLE
photometric data over the past years. Work by A.G. was supported by JPL
grant 1500811. W.Z. acknowledges the support from NSF grant AST1516842.
Work by J.C.Y. was performed under contract with the California
Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL),
funded by NASA through the Sagan Fellowship Program executed by the NASA
Exoplanet Science Institute. Work by C.B.H. and Y.S. was supported by an
appointment to the NASA Postdoctoral Program at the Jet Propulsion
Laboratory, administered by the Universities Space Research Association
through a contract with NASA. We acknowledge the high-speed internet
service (KREONET) provided by the Korea Institute of Science and
Technology Information (KISTI).
NR 35
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U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 1
PY 2017
VL 834
IS 1
AR 82
DI 10.3847/1538-4357/834/1/82
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EI0HB
UT WOS:000392152700011
ER
PT J
AU Huppenkothen, D
Younes, G
Ingram, A
Kouveliotou, C
Gogus, E
Bachetti, M
Sanchez-Fernandez, C
Chenevez, J
Motta, S
van der Klis, M
Granot, J
Gehrels, N
Kuulkers, E
Tomsick, JA
Walton, DJ
AF Huppenkothen, D.
Younes, G.
Ingram, A.
Kouveliotou, C.
Gogus, E.
Bachetti, M.
Sanchez-Fernandez, C.
Chenevez, J.
Motta, S.
van der Klis, M.
Granot, J.
Gehrels, N.
Kuulkers, E.
Tomsick, J. A.
Walton, D. J.
TI DETECTION OF VERY LOW-FREQUENCY, QUASI-PERIODIC OSCILLATIONS IN THE 2015
OUTBURST OF V404 CYGNI
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: statistical; relativistic processes; stars: black holes;
X-rays: binaries
ID X-RAY BINARIES; ADVECTION-DOMINATED ACCRETION; LENS-THIRRING PRECESSION;
LONG-TERM VARIABILITY; POWER SPECTRAL COMPONENTS; MICROQUASAR GRO
J1655-40; BLACK-HOLE TRANSIENTS; NOVA XTE J1550-564; TIMING BEHAVIOR; GS
2023+338
AB In 2015 June, the black hole X-ray binary (BHXRB) V404 Cygni went into outburst for the first time since 1989. Here, we present a comprehensive search for quasi-periodic oscillations (QPOs) of V404 Cygni during its recent outburst, utilizing data from six instruments on board five different X-ray missions: Swift/XRT, Fermi/GBM, Chandra/ACIS, INTEGRAL's IBIS/ISGRI and JEM-X, and NuSTAR. We report the detection of a QPO at 18 mHz simultaneously with both Fermi/GBM and Swift/XRT, another example of a rare but slowly growing new class of mHz-QPOs in BHXRBs linked to sources with a high orbital inclination. Additionally, we find a duo of QPOs in a Chandra/ACIS observation at 73 mHz and 1.03 Hz, as well as a QPO at 136 mHz in a single Swift/XRT observation that can be interpreted as standard Type-C QPOs. Aside from the detected QPOs, there is significant structure in the broadband power, with a strong feature observable in the Chandra observations between 0.1 and 1 Hz. We discuss our results in the context of current models for QPO formation.
C1 [Huppenkothen, D.] NYU, Ctr Data Sci, 726 Broadway,7th Floor, New York, NY 10003 USA.
[Huppenkothen, D.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA.
[Younes, G.; Kouveliotou, C.] George Washington Univ, Dept Phys, Washington, DC 20052 USA.
[Ingram, A.; van der Klis, M.] Univ Amsterdam, Anton Pannekoek Inst, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.
[Gogus, E.] Sabanci Univ, TR-34956 Istanbul, Turkey.
[Bachetti, M.] Osservatorio Astron Cagliari, INAF, Via Sci 5, I-09047 Selargius, CA, Italy.
[Sanchez-Fernandez, C.; Kuulkers, E.] European Space Astron Ctr ESA ESAC, Sci Operat Dept, E-28691 Madrid, Spain.
[Chenevez, J.] Tech Univ Denmark, DTU Space Natl Space Inst, Elektrovej 327-328, DK-2800 Lyngby, Denmark.
[Motta, S.] Univ Oxford, Dept Phys, Astrophys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England.
[Granot, J.] Open Univ Israel, Dept Nat Sci, 1 Univ Rd,POB 808, IL-43537 Raanana, Israel.
[Gehrels, N.] NASA Goddard Space Flight Ctr, Astrophys Sci Div, Mail Code 661, Greenbelt, MD 20771 USA.
[Tomsick, J. A.] Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
[Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Walton, D. J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Huppenkothen, D (reprint author), NYU, Ctr Data Sci, 726 Broadway,7th Floor, New York, NY 10003 USA.; Huppenkothen, D (reprint author), NYU, Dept Phys, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA.
EM daniela.huppenkothen@nyu.edu
OI Bachetti, Matteo/0000-0002-4576-9337; Walton,
Dominic/0000-0001-5819-3552; Younes, George/0000-0002-7991-028X;
Huppenkothen, Daniela/0000-0002-1169-7486
FU Moore-Sloan Data Science Environment at NYU; ESA member states;
Netherlands Organization for Scientific Research (NWO) Veni Fellowship
[639.041.437]; Sardinian Region [L.R. 7/2007]; ESA/PRODEX [90057]
FX We thank the anonymous referee for very helpful comments and
suggestions. We thank Victoria Grinberg for very informative and useful
discussions on INTEGRAL calibration and timing with IBIS/ISGRI. D.H.
acknowledges support by the Moore-Sloan Data Science Environment at NYU.
Partly based on observations with INTEGRAL, an ESA project with
instruments and science data centre funded by ESA member states
(especially the PI countries: Denmark, France, Germany, Italy,
Switzerland, Spain) and with the participation of Russia and the USA. AI
acknowledges support from the Netherlands Organization for Scientific
Research (NWO) Veni Fellowship, grant number 639.041.437. M.B. was
supported in part by the Sardinian Region, in the framework of the
Regional Fundamental Research funds (L.R. 7/2007). J.C. thanks financial
support from ESA/PRODEX Nr. 90057.
NR 142
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U1 0
U2 0
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 1
PY 2017
VL 834
IS 1
AR 90
DI 10.3847/1538-4357/834/1/90
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EI0HB
UT WOS:000392152700019
ER
PT J
AU Jung, I
Finkelstein, SL
Song, M
Dickinson, M
Dekel, A
Ferguson, HC
Fontana, A
Koekemoer, AM
Lu, Y
Mobasher, B
Papovich, C
Ryan, RE
Salmon, B
Straughn, AN
AF Jung, Intae
Finkelstein, Steven L.
Song, Mimi
Dickinson, Mark
Dekel, Avishai
Ferguson, Henry C.
Fontana, Adriano
Koekemoer, Anton M.
Lu, Yu
Mobasher, Bahram
Papovich, Casey
Ryan, Russell E., Jr.
Salmon, Brett
Straughn, Amber N.
TI EVIDENCE FOR REDUCED SPECIFIC STAR FORMATION RATES IN THE CENTERS OF
MASSIVE GALAXIES AT z=4
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE early universe; galaxies: bulges; galaxies: evolution; galaxies:
high-redshift; galaxies: star formation
ID ULTRA-DEEP-FIELD; LYMAN BREAK GALAXIES; GOODS-SOUTH FIELD; SIMILAR-TO 2;
SPECTRAL ENERGY-DISTRIBUTION; HIGH-REDSHIFT GALAXIES; INSIDE-OUT GROWTH;
EXTRAGALACTIC LEGACY SURVEY; COMPACT QUIESCENT GALAXIES; PHASE-3 BILLION
YEARS
AB We perform the first spatially resolved stellar population study of galaxies in the early universe (z = 3.5-6.5), utilizing the Hubble Space Telescope Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey imaging data set over the GOODS-S field. We select a sample of 418 bright and extended galaxies at z. =. 3.5-6.5 from a parent sample of similar to 8000 photometric-redshift-selected galaxies from Finkelstein et al. We first examine galaxies at 3.5 less than or similar to z less than or similar to 4.0 using additional deep K-band survey data from the HAWK-I UDS and GOODS Survey which covers the 4000 angstrom break at these redshifts. We measure the stellar mass, star formation rate, and dust extinction for galaxy inner and outer regions via spatially resolved spectral energy distribution fitting based on a Markov Chain Monte Carlo algorithm. By comparing specific star formation rates (sSFRs) between inner and outer parts of the galaxies we find that the majority of galaxies with high central mass densities show evidence for a preferentially lower sSFR in their centers than in their outer regions, indicative of reduced sSFRs in their central regions. We also study galaxies at z similar to 5 and 6 (here limited to high spatial resolution in the rest-frame ultraviolet only), finding that they show sSFRs which are generally independent of radial distance from the center of the galaxies. This indicates that stars are formed uniformly at all radii in massive galaxies at z similar to 5-6, contrary to massive galaxies at z less than or similar to 4.
C1 [Jung, Intae; Finkelstein, Steven L.] Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA.
[Dickinson, Mark] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Dekel, Avishai] Hebrew Univ Jerusalem, Racah Inst Phys, Ctr Astrophys & Planetary Sci, IL-91904 Jerusalem, Israel.
[Ferguson, Henry C.; Koekemoer, Anton M.; Ryan, Russell E., Jr.; Salmon, Brett] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Fontana, Adriano] Osserv Astron Roma, INAF, Via Frascati 33, I-00040 Monte Porzio Catone, Italy.
[Lu, Yu] Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA.
[Mobasher, Bahram] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[Papovich, Casey] Texas A&M Univ, Dept Phys & Astron, George P & Cynthia W Mitchell Inst Fundamental Ph, College Stn, TX 77843 USA.
[Song, Mimi; Straughn, Amber N.] Goddard Space Flight Ctr, Astrophys Sci Div, Code 665, Greenbelt, MD 20771 USA.
RP Jung, I (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA.
EM itjung@astro.as.utexas.edu
OI Ferguson, Henry/0000-0001-7113-2738; Koekemoer,
Anton/0000-0002-6610-2048
FU NASA [NAS 5-26555]; NASA Astrophysics and Data Analysis Program
[NNX13AI50G, NNX15AM02G]
FX We thank the anonymous referee for helpful comments and suggestions that
improved the paper. I.J. and S.L.F. acknowledge support from the
University of Texas at Austin. This work is based in part on
observations made with the NASA/ESA Hubble Space Telescope, obtained at
the Space Telescope Science Institute, which is operated by the
Association of Universities for Research in Astronomy, Inc., under NASA
contract NAS 5-26555, and also with the Spitzer Space Telescope, which
is operated by the Jet Propulsion Laboratory, California Institute of
Technology under a contract with NASA. I.J. was also supported by the
NASA Astrophysics and Data Analysis Program through grants NNX13AI50G
and NNX15AM02G.
NR 108
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U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 1
PY 2017
VL 834
IS 1
AR 81
DI 10.3847/1538-4357/834/1/81
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EI0HB
UT WOS:000392152700010
ER
PT J
AU Lam, MT
Cordes, JM
Chatterjee, S
Arzoumanian, Z
Crowter, K
Demorest, PB
Dolch, T
Ellis, JA
Ferdman, RD
Fonseca, E
Gonzalez, ME
Jones, G
Jones, ML
Levin, L
Madison, DR
McLaughlin, MA
Nice, DJ
Pennucci, TT
Ransom, SM
Shannon, RM
Siemens, X
Stairs, IH
Stovall, K
Swiggum, JK
Zhu, WW
AF Lam, M. T.
Cordes, J. M.
Chatterjee, S.
Arzoumanian, Z.
Crowter, K.
Demorest, P. B.
Dolch, T.
Ellis, J. A.
Ferdman, R. D.
Fonseca, E.
Gonzalez, M. E.
Jones, G.
Jones, M. L.
Levin, L.
Madison, D. R.
McLaughlin, M. A.
Nice, D. J.
Pennucci, T. T.
Ransom, S. M.
Shannon, R. M.
Siemens, X.
Stairs, I. H.
Stovall, K.
Swiggum, J. K.
Zhu, W. W.
TI THE NANOGRAV NINE-YEAR DATA SET: EXCESS NOISE IN MILLISECOND PULSAR
ARRIVAL TIMES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gravitational waves; pulsars: general
ID TIMING ARRAY DATA; GRAVITATIONAL-WAVES; INTERSTELLAR SCINTILLATION;
DISPERSION MEASURES; BINARY-SYSTEM; DATA RELEASE; SPIN NOISE; PRECISION;
LIMITS; PROPAGATION
AB Gravitational wave (GW) astronomy using a pulsar timing array requires high-quality millisecond pulsars (MSPs), correctable interstellar propagation delays, and high-precision measurements of pulse times of arrival. Here we identify noise in timing residuals that exceeds that predicted for arrival time estimation for MSPs observed by the North American Nanohertz Observatory for Gravitational Waves. We characterize the excess noise using variance and structure function analyses. We find that 26 out of 37 pulsars show inconsistencies with a white-noise-only model based on the short timescale analysis of each pulsar, and we demonstrate that the excess noise has a red power spectrum for 15 pulsars. We also decompose the excess noise into chromatic (radio-frequency-dependent) and achromatic components. Associating the achromatic red-noise component with spin noise and including additional power-spectrum-based estimates from the literature, we estimate a scaling law in terms of spin parameters (frequency and frequency derivative) and data-span length and compare it to the scaling law of Shannon & Cordes. We briefly discuss our results in terms of detection of GWs at nanohertz frequencies.
C1 [Lam, M. T.; Jones, M. L.; McLaughlin, M. A.] West Virginia Univ, Dept Phys, White Hall, Morgantown, WV 26506 USA.
[Lam, M. T.; Jones, M. L.; McLaughlin, M. A.; Pennucci, T. T.] West Virginia Univ, Ctr Gravitat Waves & Cosmol, White Hall, Morgantown, WV 26506 USA.
[Lam, M. T.; Cordes, J. M.; Chatterjee, S.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Lam, M. T.; Cordes, J. M.; Chatterjee, S.] Cornell Univ, Cornell Ctr Astrophys & Planetary Sci, Ithaca, NY 14853 USA.
[Arzoumanian, Z.] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Code 662, Greenbelt, MD 20771 USA.
[Arzoumanian, Z.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Code 662, Greenbelt, MD 20771 USA.
[Crowter, K.; Fonseca, E.; Gonzalez, M. E.; Stairs, I. H.] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada.
[Demorest, P. B.; Stovall, K.] Natl Radio Astron Observ, POB 0, Socorro, NM 87801 USA.
[Dolch, T.] Hillsdale Coll, Dept Phys, 33 E Coll St, Hillsdale, MI 49242 USA.
[Ellis, J. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Ferdman, R. D.] McGill Univ, Dept Phys, 3600 Rue Univ, Montreal, PQ H3A 2T8, Canada.
[Ferdman, R. D.] Univ East Anglia, Dept Phys, Norwich NR4 7TJ, Norfolk, England.
[Gonzalez, M. E.] Vancouver Coastal Hlth Author, Dept Nucl Med, Vancouver, BC V5Z 1M9, Canada.
[Jones, G.; Pennucci, T. T.] Columbia Univ, Dept Phys, 550 W 120th St, New York, NY 10027 USA.
[Levin, L.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Madison, D. R.; Ransom, S. M.] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA.
[Nice, D. J.] Lafayette Coll, Dept Phys, Easton, PA 18042 USA.
[Shannon, R. M.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Box 76, Epping, NSW 1710, Australia.
[Shannon, R. M.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia.
[Siemens, X.; Swiggum, J. K.] Univ Wisconsin, Dept Phys, Ctr Gravitat Cosmol & Astrophys, POB 413, Milwaukee, WI 53201 USA.
[Stovall, K.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA.
[Zhu, W. W.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
RP Lam, MT (reprint author), West Virginia Univ, Dept Phys, White Hall, Morgantown, WV 26506 USA.; Lam, MT (reprint author), West Virginia Univ, Ctr Gravitat Waves & Cosmol, White Hall, Morgantown, WV 26506 USA.; Lam, MT (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.; Lam, MT (reprint author), Cornell Univ, Cornell Ctr Astrophys & Planetary Sci, Ithaca, NY 14853 USA.
EM michael.lam@mail.wvu.edu
OI Chatterjee, Shami/0000-0002-2878-1502
FU NSF PIRE program [0968296]; NSF Physics Frontier Center [1430284]; NSERC
Discovery Grant; NSERC Discovery Accelerator Supplement; Canadian
Institute for Advanced Research; NASA New York Space [NNX15AK07H]; NASA
through Einstein Fellowship [PF3-140116]; NSF [AST-1100968]
FX We thank Paul Baker for the. useful discussion regarding the methods.
The NANOGrav Project receives support from NSF PIRE program award number
0968296 and NSF Physics Frontier Center award number 1430284. NANOGrav
research at UBC is supported by an NSERC Discovery Grant and Discovery
Accelerator Supplement and the Canadian Institute for Advanced Research.
M.T.L. acknowledges partial support by NASA New York Space Grant award
number NNX15AK07H. J.A.E. acknowledges support by NASA through Einstein
Fellowship grant PF3-140116. Portions of this research were carried out
at the Jet Propulsion Laboratory, California Institute of Technology,
under a contract with the National Aeronautics and Space Administration.
T.T.P. was a student at the National Radio Astronomy Observatory (NRAO)
while this project was undertaken. Data for the project were collected
using the facilities of the NRAO and the Arecibo Observatory. The NRAO
is a facility of the NSF operated under cooperative agreement by
Associated Universities, Inc. The Arecibo Observatory is operated by SRI
International under a cooperative agreement with the NSF (AST-1100968),
and in alliance with the Ana G. Mendez-Universidad Metropolitana, and
the Universities Space Research Association.
NR 62
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 1
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EH7ZM
UT WOS:000391991200007
ER
PT J
AU Liu, W
Chiao, M
Collier, MR
Cravens, T
Galeazzi, M
Koutroumpa, D
Kuntz, KD
Lallement, R
Lepri, ST
McCammon, D
Morgan, K
Porter, FS
Snowden, SL
Thomas, NE
Uprety, Y
Ursino, E
Walsh, BM
AF Liu, W.
Chiao, M.
Collier, M. R.
Cravens, T.
Galeazzi, M.
Koutroumpa, D.
Kuntz, K. D.
Lallement, R.
Lepri, S. T.
McCammon, D.
Morgan, K.
Porter, F. S.
Snowden, S. L.
Thomas, N. E.
Uprety, Y.
Ursino, E.
Walsh, B. M.
TI THE STRUCTURE OF THE LOCAL HOT BUBBLE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: bubbles; ISM: structure; X-rays: diffuse background; X-rays: ISM
ID X-RAY-EMISSION; WIND CHARGE-EXCHANGE; XMM-NEWTON OBSERVATIONS;
SOLAR-WIND; INTERSTELLAR-MEDIUM; GALACTIC HALO; ROSAT SURVEY;
ABSORPTION; HYDROGEN; SUZAKU
AB Diffuse X-rays from the Local Galaxy (DXL) is a sounding rocket mission designed to quantify and characterize the contribution of Solar Wind Charge eXchange (SWCX) to the Diffuse X-ray Background and study the properties of the Local Hot Bubble (LHB). Based on the results from the DXL mission, we quantified and removed the contribution of SWCX to the diffuse X-ray background measured by the ROSAT All Sky Survey. The "cleaned" maps were used to investigate the physical properties of the LHB. Assuming thermal ionization equilibrium, we measured a highly uniform temperature distributed around kT = 0.097 keV +/- 0.013 keV (FWHM) +/- 0.006 keV (systematic). We also generated a thermal emission measure map and used it to characterize the three-dimensional (3D) structure of the LHB, which we found to be in good agreement with the structure of the local cavity measured from dust and gas.
C1 [Liu, W.; Galeazzi, M.; Uprety, Y.; Ursino, E.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA.
[Chiao, M.; Collier, M. R.; Porter, F. S.; Snowden, S. L.; Thomas, N. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cravens, T.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Koutroumpa, D.] Univ Versailles St Quentin, F-78280 Guyancourt, France.
[Koutroumpa, D.] UPMC Univ Paris 06, Sorbonne Univ, F-78280 Guyancourt, France.
[Koutroumpa, D.] CNRS INSU, LATMOS IPSL, F-78280 Guyancourt, France.
[Kuntz, K. D.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA.
[Lallement, R.] Univ Paris Diderot, CNRS, GEPI Observ Paris, F-92190 Meudon, France.
[Lepri, S. T.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[McCammon, D.; Morgan, K.] Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA.
[Walsh, B. M.] Boston Univ, Dept Mech Engn, Boston, MA 02215 USA.
[Uprety, Y.] Middle Tennessee State Univ, Dept Phys & Astron, Murfreesboro, TN 37132 USA.
[Ursino, E.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA.
RP Galeazzi, M (reprint author), Univ Miami, Dept Phys, Coral Gables, FL 33124 USA.
EM galeazzi@physics.miami.edu
RI Porter, Frederick/D-3501-2012;
OI Porter, Frederick/0000-0002-6374-1119; McCammon, Dan/0000-0001-5170-4567
FU NASA [NNX11AF04G, NNX09AF09G]
FX This work was supported by NASA award numbers NNX11AF04G and NNX09AF09G.
NR 51
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SN 0004-637X
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J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 1
PY 2017
VL 834
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DI 10.3847/1538-4357/834/1/33
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EH7ZM
UT WOS:000391991200005
ER
PT J
AU McQuinn, KBW
Boyer, ML
Mitchell, MB
Skillman, ED
Gehrz, RD
Groenewegen, MAT
McDonald, I
Sloan, GC
van Loon, JT
Whitelock, PA
Zijlstra, AA
AF McQuinn, Kristen B. W.
Boyer, Martha L.
Mitchell, Mallory B.
Skillman, Evan D.
Gehrz, R. D.
Groenewegen, Martin A. T.
McDonald, Iain
Sloan, G. C.
van Loon, Jacco Th.
Whitelock, Patricia A.
Zijlstra, Albert A.
TI DUSTiNGS. III. DISTRIBUTION OF INTERMEDIATE-AGE AND OLD STELLAR
POPULATIONS IN DISKS AND OUTER EXTREMITIES OF DWARF GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: dwarf; galaxies: evolution; galaxies: fundamental parameters;
galaxies: photometry; galaxies: stellar content; Local Group
ID ASYMPTOTIC GIANT BRANCH; LARGE-MAGELLANIC-CLOUD; STAR-FORMATION HISTORY;
LOCAL GROUP GALAXIES; PLANETARY CAMERA 2; CENTRAL SQUARE KILOPARSEC;
SPITZER-SPACE-TELESCOPE; M33 MONITORING PROJECT; MU-M RANGE; IRREGULAR
GALAXY
AB We have traced the spatial distributions of intermediate-age and old stars in nine dwarf galaxies in the distant parts of the Local Group, using multi-epoch 3.6 and 4.5 mu m data from the DUST in Nearby Galaxies with Spitzer (DUSTiNGS) survey. Using complementary optical imaging from the Hubble Space Telescope, we identify the tip of the red giant branch (TRGB) in the 3.6 mu m photometry, separating thermally pulsating asymptotic giant branch stars from the larger red giant branch populations. Unlike the constant TRGB in the I band, at 3.6 mu m,. the TRGB magnitude varies by similar to 0.7 mag, making it unreliable as a distance indicator. The intermediate-age and old stars are well mixed in two-thirds of the sample, with no evidence of a gradient in the ratio of the intermediate-age to old stellar populations outside the central similar to 1'-2'. Variable AGB stars are detected in the outer extremities of the galaxies, indicating that chemical enrichment from these dust-producing stars may occur in the outer regions of galaxies with some frequency. Theories of structure formation in dwarf galaxies must account for the lack of radial gradients in intermediate-age populations and the presence of these stars in the outer extremities of dwarfs. Finally, we identify unique features in individual galaxies, such as extended tidal features in Sex. A and Sag. DIG and a central concentration of AGB stars in the inner regions of NGC 185 and NGC 147.
C1 [McQuinn, Kristen B. W.] Univ Texas Austin, McDonald Observ, 2515 Speedway,Stop C1402, Austin, TX 78712 USA.
[McQuinn, Kristen B. W.; Mitchell, Mallory B.; Skillman, Evan D.; Gehrz, R. D.] Univ Minnesota, Minnesota Inst Astrophys, Sch Phys & Astron, 116 Church St SE, Minneapolis, MN 55455 USA.
[Boyer, Martha L.] NASA Goddard Space Flight Ctr, Observat Cosmol Lab, Code 664, Greenbelt, MD 20771 USA.
[Boyer, Martha L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Groenewegen, Martin A. T.] Koninklijke Sterrenwacht Belgie, Ringlaan 3, B-1180 Brussels, Belgium.
[McDonald, Iain; Zijlstra, Albert A.] Univ Manchester, Sch Phys & Astron, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Sloan, G. C.] Cornell Univ, Cornell Ctr Astrophys & Planetary Sci, Ithaca, NY 14853 USA.
[Sloan, G. C.] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA.
[Sloan, G. C.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[van Loon, Jacco Th.] Keele Univ, Lennard Jones Labs, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Whitelock, Patricia A.] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa.
[Whitelock, Patricia A.] South African Astron Observ, POB 9, ZA-7935 Observatory, South Africa.
RP McQuinn, KBW (reprint author), Univ Texas Austin, McDonald Observ, 2515 Speedway,Stop C1402, Austin, TX 78712 USA.; McQuinn, KBW (reprint author), Univ Minnesota, Minnesota Inst Astrophys, Sch Phys & Astron, 116 Church St SE, Minneapolis, MN 55455 USA.
EM kmcquinn@astro.as.utexas.edu; martha.boyer@nasa.gov; mitch925@umn.edu;
skillman@astro.umn.edu; gerhz@astro.umn.edu; martin.groenewegen@oma.be;
Iain.Mcdonald-2@manchester.ac.uk; sloan@isc.astro.cornell.edu;
j.t.van.loon@keele.ac.uk
OI Mcquinn, Kristen/0000-0001-5538-2614
FU Spitzer [GO80063]; NASA Astrophysics Data Analysis Program
[N3-ADAP13-0058]; United States Air Force; UK Science and Technology
Facility Council [ST/L000768/1]; South African National Research
Foundation; National Aeronautics and Space Administration
FX This work is supported by Spitzer via grant GO80063 and by the NASA
Astrophysics Data Analysis Program grant number N3-ADAP13-0058. R.D.G.
was supported, in part, by the United States Air Force. A.Z. and I.M.
acknowledge support from the UK Science and Technology Facility Council
under grant ST/L000768/1. P.A.W. thanks the South African National
Research Foundation for a research grant. Many thanks to Andy Dolphin
for assistance with HST/WFPC2 photometry. This research made use of
NASA's Astrophysical Data System, the NASA/IPAC Extragalactic Database
which is operated by the Jet Propulsion Laboratory, California Institute
of Technology, under contract with the National Aeronautics and Space
Administration. We acknowledge the use of the HyperLeda database
(http://leda.univ-lyon1.fr).
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 1
PY 2017
VL 834
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PG 25
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SC Astronomy & Astrophysics
GA EI0HB
UT WOS:000392152700007
ER
PT J
AU Stephens, IW
Gouliermis, D
Looney, LW
Gruendl, RA
Chu, YH
Weisz, DR
Seale, JP
Chen, CHR
Wong, T
Hughes, A
Pineda, JL
Ott, J
Muller, E
AF Stephens, Ian W.
Gouliermis, Dimitrios
Looney, Leslie W.
Gruendl, Robert A.
Chu, You-Hua
Weisz, Daniel R.
Seale, Jonathan P.
Chen, C. -H. Rosie
Wong, Tony
Hughes, Annie
Pineda, Jorge L.
Ott, Jurgen
Muller, Erik
TI STELLAR CLUSTERINGS AROUND "ISOLATED" MASSIVE YSOs IN THE LMC
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: clouds; Magellanic Clouds; stars: formation; stars: massive
ID LARGE-MAGELLANIC-CLOUD; FIELD O-STARS; MOLECULAR CLOUDS; GALAXY
EVOLUTION; KEY PROGRAM; 2ND SURVEY; CATALOG; OBJECTS; IDENTIFICATION;
POPULATIONS
AB Observations suggest that there is a significant fraction of O stars in the field of the Milky Way that appear to have formed in isolation or in low-mass clusters (< 100 M-circle dot). The existence of these high-mass stars that apparently formed in the field challenges the generally accepted paradigm, which requires star formation to occur in clustered environments. In order to understand the physical conditions for the formation of these stars, it is necessary to observe isolated high-mass stars while they are still forming. With the Hubble. Space. Telescope, we observe the seven most isolated massive (> 8 M-circle dot) young stellar objects (MYSOs) in the Large. Magellanic. Cloud. The observations show that while these MYSOs are remote from other MYSOs, OB associations, and even known giant molecular clouds, they are actually not isolated at all. Imaging reveals similar to 100 to several hundred pre-mainsequence (PMS) stars in the vicinity of each MYSO. These previously undetected PMS stars form prominent compact clusters around the MYSOs, and in most cases they are also distributed sparsely across the observed regions. Contrary to what previous high-mass field star studies show, these observations suggest that high-mass stars may not be able to form in clusters with masses less than 100 M-circle dot. If these MYSOs are indeed the best candidates for isolated high-mass star formation, then the lack of isolation is at odds with random sampling of the initial mass function. Moreover, while isolated MYSOs may not exist, we find evidence that isolated clusters containing O stars can exist, which in itself is rare.
C1 [Stephens, Ian W.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA.
[Stephens, Ian W.; Looney, Leslie W.; Gruendl, Robert A.; Chu, You-Hua; Wong, Tony] Univ Illinois, Dept Astron, 1002 West Green St, Urbana, IL 61801 USA.
[Gouliermis, Dimitrios] Heidelberg Univ, Zentrum Astron, Inst Theoret Astrophys, Albert Ueberle Str 2, D-69120 Heidelberg, Germany.
[Gouliermis, Dimitrios] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Chu, You-Hua] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan.
[Weisz, Daniel R.] Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
[Seale, Jonathan P.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Chen, C. -H. Rosie] Max Planck Inst Radio Astron, D-53121 Bonn, Germany.
[Hughes, Annie] IRAP, CNRS, 9 Ave Colonel Roche,BP 44346, F-31028 Toulouse 4, France.
[Hughes, Annie] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France.
[Pineda, Jorge L.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Ott, Jurgen] Natl Radio Astron Observ, POB O,1003 Lopezville Rd, Socorro, NM 87801 USA.
[Muller, Erik] Natl Astron Observ Japan, Chile Observ, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Stephens, Ian W.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RP Stephens, IW (reprint author), Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA.; Stephens, IW (reprint author), Univ Illinois, Dept Astron, 1002 West Green St, Urbana, IL 61801 USA.; Stephens, IW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ian.stephens@cfa.harvard.edu; gouliermis@uni-heidelberg.de
OI Weisz, Daniel/0000-0002-6442-6030
FU NASA [HST-GO-12941 06-A, NAS 5-26555]; German Research Foundation
(Deutsche Forschungsgemeinschaft, DFG) [GO 1659/3-2]; NASA through
Hubble Fellowship - Space Telescope Science Institute [HST-HF-51331.01];
Centre National d'Etudes Spatiales (CNES); Commonwealth of Australia;
Australian Research Council
FX I.W.S. and L.W.L. acknowledge NASA grant HST-GO-12941 06-A. D.A.G.
acknowledges the German Research Foundation (Deutsche
Forschungsgemeinschaft, DFG) grant GO 1659/3-2. D.R.W. is supported by
NASA through Hubble Fellowship grant HST-HF-51331.01 awarded by the
Space Telescope Science Institute. A.H. acknowledges support from the
Centre National d'Etudes Spatiales (CNES). Based on observations made
with the NASA/ESA Hubble Space Telescope, obtained from the data archive
at the Space Telescope Science Institute (STScI). STScI is operated by
the Association of Universities for Research in Astronomy, Inc., under
NASA contract NAS 5-26555. The Mopra Radio Telescope is part of the
Australia Telescope National Facility, which is funded by the
Commonwealth of Australia for operation as a National Facility managed
by CSIRO. The University of New South Wales Digital Filter Bank used for
the observations with the Mopra Telescope was provided with support from
the Australian Research Council. The National Radio Astronomy
Observatory is a facility of the National Science Foundation operated
under cooperative agreement by Associated Universities, Inc. This
research has made use of the SIMBAD database, operated at CDS,
Strasbourg, France, and APLpy, an open-source plotting package for
Python hosted at http://aplpy.github.com.
NR 70
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 1
PY 2017
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PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EI0HB
UT WOS:000392152700023
ER
PT J
AU De Robertis, A
Taylor, K
Wilson, CD
Farley, EV
AF De Robertis, Alex
Taylor, Kevin
Wilson, Christopher D.
Farley, Edward V.
TI Abundance and distribution of Arctic cod (Boreogadus saida) and other
pelagic fishes over the US Continental Shelf of the Northern Bering and
Chukchi Seas
SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY
LA English
DT Article
DE Acoustic surveys; Trawl selectivity; Midwater trawl; Chukchi Sea; Echo
surveys; Arctic zone; Northern Bering Sea; Pelagic fish; Boreogadus
saida
ID POLLOCK THERAGRA-CHALCOGRAMMA; TARGET-STRENGTH MEASUREMENTS;
PRINCE-WILLIAM-SOUND; WALLEYE POLLOCK; BEAUFORT SEAS; SPECIES
ASSEMBLAGES; CLIMATE-CHANGE; WATER MASS; ICE COVER; PACIFIC
AB We conducted acoustic-trawl (AT) surveys of the northern Bering and Chukchi Seas during ice-free periods in 2012 and 2013. The mixed species assemblages in the study area required refinement of standard AT survey methods, and adjustment of trawl catches for the effects of trawl selectivity. Sensitivity analyses indicate that the AT abundance estimates are relatively robust to the assumptions of the analysis. These surveys indicate that midwater fishes are dominated by age-0 Arctic cod (Boreogadus saida), age-0 saffron cod (Eleginus gracilis), capelin (Mallotus villosus), and Pacific herring (Clupea pallasii). In both years, age-0 Arctic cod were distributed principally >= 69.5 degrees N, age-0 saffron cod were abundant in coastal areas between 66.5 and 69.5 degrees N, and Pacific herring were distributed south of 67 degrees N. These three fishes exhibited consistent associations with temperature, salinity and bottom depth: e.g., age-0 Arctic cod were abundant at lower mean water column temperatures than saffron cod. In contrast, capelin were distributed throughout the study area, and were not consistently associated with environmental measures. There was a geographic trend in body length, with smaller Arctic cod, saffron cod and capelin in northern areas, but smaller herring in the south. Arctic cod, saffron cod, herring and capelin were all > 2 times more abundant in 2013 than 2012. Sizeable populations of age-0 Arctic cod were observed in the northern Chukchi Sea, which suggests that this area is an important nursery ground. However, relatively few older Arctic cod were observed in this and other surveys of the area, which suggests that either overwinter mortality of age-0 Arctic cod is high, and/or these fish are not retained on the Chukchi shelf. Published by Elsevier Ltd.
C1 [De Robertis, Alex; Taylor, Kevin; Wilson, Christopher D.] NOAA, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 7600 Sand Point Way NE, Seattle, WA 98115 USA.
[Farley, Edward V.] NOAA, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 17109 Point Lena Loop Rd, Juneau, AK 99801 USA.
[Taylor, Kevin] Johns Hopkins Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA.
RP De Robertis, A (reprint author), NOAA, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 7600 Sand Point Way NE, Seattle, WA 98115 USA.
EM alex.derobertis@noaa.gov
FU Coastal Impact Assistance Program, Fish and Wildlife Service U.S.
Department of the Interior [10-CIAP-010, F12AF00188]; Alaska Fisheries
Science Center, NOAA
FX We are indebted to the captain and crew of F/V Bristol Explorer, Jared
Weems, Jim Murphy, Franz Mueter, and the participants in Arctic Eis
cruises for their assistance at sea. Patrick Ressler, Robert Levine,
Mike Sigler and two anonymous reviewers provided helpful comments on
manuscript drafts. We thank Seth Danielson and Lisa Eisner for providing
the CTD data. This work was funded in part with qualified outer
continental shelf oil and gas revenues by the Coastal Impact Assistance
Program, Fish and Wildlife Service U.S. Department of the Interior
(grants10-CIAP-010 and F12AF00188) and by the Alaska Fisheries Science
Center, NOAA. The findings and conclusions in this paper are those of
the authors and do not necessarily represent the views of the National
Marine Fisheries Service. Reference to trade names does not imply
endorsement by the National Marine Fisheries Service, NOAA.
NR 72
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0967-0645
EI 1879-0100
J9 DEEP-SEA RES PT II
JI Deep-Sea Res. Part II-Top. Stud. Oceanogr.
PD JAN
PY 2017
VL 135
BP 51
EP 65
DI 10.1016/j.dsr2.2016.03.002
PG 15
WC Oceanography
SC Oceanography
GA EI5TK
UT WOS:000392557500005
ER
PT J
AU Vega, SL
Sutton, TM
Murphy, JM
AF Vega, Stacy L.
Sutton, Trent M.
Murphy, James M.
TI Marine-entry timing and growth rates of juvenile Chum Salmon in Alaskan
waters of the Chukchi and northern Bering seas
SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY
LA English
DT Article
DE Chum salmon (Oncorhynchus keta); Otoliths Bering Sea; Chukchi Sea;
Growth rate
ID SIZE-SELECTIVE MORTALITY; PACIFIC SALMON; CLIMATE-CHANGE;
ONCORHYNCHUS-KETA; ATLANTIC SALMON; SURVIVAL RATES; CHINOOK SALMON;
LIFE-HISTORY; COHO SALMON; PINK SALMON
AB Climate change in the Arctic has implications for influences on juvenile Chum Salmon Oncorhynchus keta early life-history patterns, such as altered timing of marine entry and/or early marine growth. Sagittal otoliths were used to estimate marine entry dates and daily growth rates of juvenile Chum Salmon collected during surface trawl surveys in summers 2007, 2012, and 2013 in the Chukchi and northern Bering seas. Inductively coupled plasma-mass spectrometry (ICP-MS) was used to discriminate between freshwater and marine sagittal growth on the otoliths, and daily growth increments were counted to determine marine-entry dates and growth rates to make temporal and regional comparisons of juvenile Chum Salmon characteristics. Marine-entry dates ranged from mid-June to mid-July, with all region and year combinations exhibiting similar characteristics in entry timing (i.e. larger individuals at the time of capture entered the marine environment earlier in the growing season than smaller individuals in the same region/year), as well as similar mean marine-entry dates. Juvenile Chum Salmon growth rates were on average 4.9% body weight per day in both regions in summers 2007 and 2012, and significantly higher (6.8% body weight per day) in the Chukchi Sea in 2013. These results suggest that juvenile Chum Salmon in the northern Bering and Chukchi seas currently exhibit consistent marine-entry timing and early marine growth rates, despite some differences in environmental conditions between regions and among years. This study also provides a baseline of early marine life-history characteristics of Chum Salmon for comparisons with future climate change studies in these regions. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Vega, Stacy L.; Sutton, Trent M.] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, 905 N Koyukuk Dr,2450 Neill Bldg, Fairbanks, AK 99775 USA.
[Murphy, James M.] NOAA, Auke Bay Labs, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 17109 Point Lena Loop Rd, Juneau, AK 99801 USA.
RP Vega, SL (reprint author), Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, 905 N Koyukuk Dr,2450 Neill Bldg, Fairbanks, AK 99775 USA.
EM stacylvega@gmail.com; tmsutton@alaska.edu; jim.murphy@noaa.gov
FU Coastal Impact Assistance Program, Fish and Wildlife Service, U.S.
Department of the Interior
FX We would like to thank all crewmembers aboard the NOAA ship Oscar Dyson,
the F/V Sea Storm, and the F/V Bristol Explorer, as well as technicians
from NOAA/Auke Bay Labs who helped collect and extract otolith samples
for analysis. A special thanks to K. Spaleta for assistance with the
ICP-MS. Thanks to M. Adkison for help in the early stages of this study
and N. Smith for assisting with laboratory analyses for this project.
Portions of this work were performed at the AIL, University of Alaska
Fairbanks. This study was funded with qualified outer continental shelf
oil and gas revenues by the Coastal Impact Assistance Program, Fish and
Wildlife Service, U.S. Department of the Interior. The findings and
conclusions in the paper are those of the authors and do not necessarily
represent the views of the National Marine Fisheries Service, NOM.
Reference to trade names does not imply endorsement by the National
Marine Fisheries Service, NOAA.
NR 50
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0967-0645
EI 1879-0100
J9 DEEP-SEA RES PT II
JI Deep-Sea Res. Part II-Top. Stud. Oceanogr.
PD JAN
PY 2017
VL 135
BP 137
EP 144
DI 10.1016/j.dsr2.2016.02.002
PG 8
WC Oceanography
SC Oceanography
GA EI5TK
UT WOS:000392557500011
ER
PT J
AU Murphy, JM
Howard, KG
Gann, JC
Cieciel, KC
Templin, WD
Guthrie, CM
AF Murphy, James M.
Howard, Kathrine G.
Gann, Jeanette C.
Cieciel, Kristin C.
Templin, William D.
Guthrie, Charles M., III
TI Juvenile Chinook Salmon abundance in the northern Bering Sea:
Implications for future returns and fisheries in the Yukon River
SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY
LA English
DT Article
DE Chinook Salmon; Northern Bering Sea; Yukon River
ID POLLOCK THERAGRA-CHALCOGRAMMA; WALLEYE POLLOCK; SOCKEYE-SALMON; PINK
SALMON; CLIMATE; ALASKA; AGE-0; RECRUITMENT; DRAINAGE; SURVIVAL
AB Juvenile Chinook Salmon (Oncorhynchus tshawytscha) abundance in the northern Bering Sea is used to provide insight into future returns and fisheries in the Yukon River. The status of Yukon River Chinook Salmon is of concern due to recent production declines and subsequent closures of commercial, sport, and personal use fisheries, and severe restrictions on subsistence fisheries in the Yukon River. Surface trawl catch data, mixed layer depth adjustments, and genetic stock mixtures are used to estimate juvenile abundance for the Canadian-origin stock group from the Yukon River. Abundance ranged from a low of 0.62 million in 2012 to a high of 2.58 million in 2013 with an overall average of '1.5 million from 2003 to 2015. Although abundance estimates indicate that average survival is relatively low (average of 5.2%), juvenile abundance was significantly correlated (r=0.87, p= 0.005) with adult returns, indicating that much of the variability in survival occurs "during early life-history stages (freshwater and initial marine). Juvenile abundance in the northern Bering Sea has increased since 2013 due to an increase in early life-history survival (average juveniles-per-spawner increased from 29 to 59). The increase in juvenile abundance is projected to produce larger runs and increased subsistence fishing opportunities for Chinook Salmon in the Yukon River as early as 2016. (C) 2016 Published by Elsevier Ltd.
C1 [Murphy, James M.; Gann, Jeanette C.; Cieciel, Kristin C.; Guthrie, Charles M., III] Natl Marine Fisheries Serv, Auke Bay Labs, 17109 Point Lena Loop Rd, Juneau, AK 99801 USA.
[Howard, Kathrine G.; Templin, William D.] Alaska Dept Fish & Game, 333 Raspberry Rd, Anchorage, AK 99518 USA.
RP Murphy, JM (reprint author), Natl Marine Fisheries Serv, Auke Bay Labs, 17109 Point Lena Loop Rd, Juneau, AK 99801 USA.
EM Jim.Murphy@noaa.gov; Kathrine.Howard@alaska.gov; Jeanette.Gann@noaa.gov;
Kristin.Cieciel@noaa.gov; Bill.Templin@alaska.gov;
Chuck.Guthrie@noaa.gov
FU National Marine Fisheries Service; Alaska Sustainable Salmon Fund
[44606]; Arctic Yukon Kuskokwim Sustainable Salmon Initiative [1003];
State of Alaska's Coastal Impact Assessment Program [F12AF00188]; Bureau
of Ocean Energy Management [M12PG00018]; Arctic Yukon Kuskokwim
Sustainable Salmon Initiative, University of Alaska, Fairbanks Arctic
EIS research program; Alaska Department of Fish and Game's Chinook
Salmon Research Initiative
FX Multiple funding sources have provided support for surface trawl surveys
in the northern Bering Sea. The National Marine Fisheries Service
provided the primary funding support for the surveys from 2003 to 2010.
The Alaska Sustainable Salmon Fund (project 44606) and the Arctic Yukon
Kuskokwim Sustainable Salmon Initiative (project 1003) provided funding
support for the survey in 2011). The State of Alaska's Coastal Impact
Assessment Program (project F12AF00188), the Bureau of Ocean Energy
Management (project M12PG00018), and the Arctic Yukon Kuskokwim
Sustainable Salmon Initiative provided funding support as part of the
University of Alaska, Fairbanks Arctic EIS research program in 2012 and
2013. The Alaska Department of Fish and Game's Chinook Salmon Research
Initiative provided funding support for the 2014 and 2015 surveys.
Vessels supporting the northern Bering Sea surveys include the F/V Sea
Storm (2003-2007), F/V Epic Explorer (2009-2010), F/V Bristol Explorer
(2011-2013), and the F/V Alaskan Endeavor (2014 and 2015). We wish to
thank the many scientists, as well as the captains and crews of the
chartered fishing vessels that have made the northern Bering Sea surveys
possible.
NR 57
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0967-0645
EI 1879-0100
J9 DEEP-SEA RES PT II
JI Deep-Sea Res. Part II-Top. Stud. Oceanogr.
PD JAN
PY 2017
VL 135
BP 156
EP 167
DI 10.1016/j.dsr2.2016.06.002
PG 12
WC Oceanography
SC Oceanography
GA EI5TK
UT WOS:000392557500013
ER
PT J
AU Sigler, MF
Mueter, FJ
Bluhm, BA
Busby, MS
Cokelet, ED
Danielson, SL
De Robertis, A
Eisner, LB
Farley, EV
Iken, K
Kuletz, KJ
Lauth, RR
Logerwell, EA
Pinchuk, AI
AF Sigler, Michael F.
Mueter, Franz J.
Bluhm, Bodil A.
Busby, Morgan S.
Cokelet, Edward D.
Danielson, Seth L.
De Robertis, Alex
Eisner, Lisa B.
Farley, Edward V.
Iken, Katrin
Kuletz, Kathy J.
Lauth, Robert R.
Logerwell, Elizabeth A.
Pinchuk, Alexei I.
TI Late summer zoogeography of the northern Bering and Chukchi seas
SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY
LA English
DT Article
DE Bering Sea; Chukchi Sea; Zoogeography; Zooplankton; Fishes;
Invertebrates; Seabirds
ID COMMUNITY STRUCTURE; ARCTIC-OCEAN; ENVIRONMENTAL CHARACTERISTICS;
CLIMATE-CHANGE; CONTINENTAL-SHELF; FISH ASSEMBLAGES; BENTHIC ECOLOGY;
LEAST AUKLETS; MARINE BIRDS; ZOOPLANKTON
AB Ocean currents, water masses, and seasonal sea ice formation contribute to determining relationships among the biota of the Bering and Chukchi seas. The Bering Sea communicates with the Chukchi Sea via northward advection of water, nutrients, organic matter, and plankton through Bering Strait. We used data from concurrent surveys of zooplankton, pelagic fishes and jellyfish, epibenthic fishes and invertebrates, and seabirds to identify faunal distribution patterns and environmental factors that are related to these faunal distributions within the US portions of the Chukchi Sea shelf and Bering Sea shelf north of Nunivak Island. Regional differences in late summer (August-September) distributions of biota largely reflected the underlying hydrography. Depth, temperature, salinity, stratification, and chlorophyll a, but less so sediment-related or nutrient-related factors, were related to the distributions of the assemblages (zooplanlcton: depth, salinity, stratification; pelagic fishes and jellyfish: depth, stratification, chlorophyll a; epibenthic fishes and invertebrates: depth, temperature, salinity; seabirds: temperature, salinity, stratification). These six environmental factors that most influenced distributions of zooplankton, pelagic fishes/jellyfish, epibenthic fishes and invertebrate, and seabird assemblages likely can be simplified to three factors reflecting bottom depth, water mass, and their stratification and productivity (which are tightly linked in the study region). The assemblages were principally structured from nearshore to offshore and from south to north. The nearshore to offshore contrast usually was stronger in the south, where the enormous discharge of the Yukon River is more apparent and extends farther offshore, influencing zooplankton, pelagic fish/jellyfish, and seabird assemblages. Some assemblages overlapped spatially (e.g., seabird and zooplankton), indicating shared influential environmental factors or trophic linkages among assemblages. The gradients in assemblage composition were gradual for epibenthic taxa, abrupt for zooplankton taxa, and intermediate for pelagic fish/jellyfish and seabird taxa, implying that zooplankton assemblage structure is most strongly tied to water mass, epibenthic least, with the other two taxa intermediates. Three communities (i.e., cross-assemblage groupings) emerged based on maps of ordination axes and core use areas by taxa; one associated with Alaska Coastal Water (warmer, fresher, nutrient depauperate), second associated with Chirikov Basin and the southern Chukchi Sea (colder, saltier, nutrient rich), and third associated with the northern Chukchi shelf (colder and saltier but not as nutrient rich). Gradients in species composition occurred both within and between these communities. The Chirikov Basin/southern Chukchi Sea community was characterized by distinct zooplankton and seabird taxa, but was not strongly associated with distinct pelagic or epibenthic fish and invertebrate taxa. Although comprehensive data were only available for a single year and annual variation may affect the generality of our results, our comprehensive ecosystem survey approach yielded new insights into the ecological relationships (specifically, gradients in assemblage composition and identification of communities) of this Arctic region. Published by Elsevier Ltd.
C1 [Sigler, Michael F.; Farley, Edward V.] NOAA, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 17109 Point Lena Loop Rd, Juneau, AK 99801 USA.
[Mueter, Franz J.; Bluhm, Bodil A.; Pinchuk, Alexei I.] Univ Alaska, Sch Fisheries & Ocean Sci, 17103 Point Lena Loop Rd, Juneau, AK 99801 USA.
[Bluhm, Bodil A.] Univ Tromso, POB 6050 Langnes, N-9037 Tromso, Norway.
[Busby, Morgan S.; De Robertis, Alex; Eisner, Lisa B.; Lauth, Robert R.; Logerwell, Elizabeth A.] NOAA, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 7600 Sand Point Way NE, Seattle, WA USA.
[Cokelet, Edward D.] NOAA, Pacific Marine Environm Lab, Oceans & Atmospher Res, 7600 Sand Point Way NE, Seattle, WA 98115 USA.
[Danielson, Seth L.] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, POB 757220, Fairbanks, AK 99775 USA.
[Kuletz, Kathy J.] US Fish & Wildlife Serv, 1011 East Tudor Rd, Anchorage, AK 99503 USA.
RP Sigler, MF (reprint author), NOAA, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 17109 Point Lena Loop Rd, Juneau, AK 99801 USA.
EM mike.sigler@noaa.gov
FU Coastal Impact Assistance Program (U.S. Fish and Wildlife Service);
University of Alaska Fairbanks [10-CIAP-010 F12AF00188, M12AC00009];
Bureau of Ocean Energy Management; Alaska Fisheries Science Center;
National Oceanic and Atmospheric Administration [M12PG00018]; Division
of Migratory Bird Management, U.S. Fish and Wildlife Service
[M10PG00050]
FX This project was funded through the Coastal Impact Assistance Program
(U.S. Fish and Wildlife Service) and the University of Alaska Fairbanks
(10-CIAP-010 F12AF00188), the Bureau of Ocean Energy Management and the
University of Alaska Fairbanks (Agreement number M12AC00009), the Bureau
of Ocean Energy Management and the Alaska Fisheries Science Center,
National Oceanic and Atmospheric Administration (Agreement number
M12PG00018), and the Bureau of Ocean Energy Management and the Division
of Migratory Bird Management, U.S. Fish and Wildlife Service (Agreement
Number M10PG00050). The seabird density estimates are archived in the
North Pacific Pelagic Seabird Database
(http://alaska.usgs.gov/science/biology/nppsd/index.php).
NR 114
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0967-0645
EI 1879-0100
J9 DEEP-SEA RES PT II
JI Deep-Sea Res. Part II-Top. Stud. Oceanogr.
PD JAN
PY 2017
VL 135
BP 168
EP 189
DI 10.1016/j.dsr2.2016.03.005
PG 22
WC Oceanography
SC Oceanography
GA EI5TK
UT WOS:000392557500014
ER
PT J
AU Hill, MA
Haering, EA
AF Hill, Michael A.
Haering, Edward A., Jr.
TI Ground-to-air flow visualization using Solar Calcium-K line
Background-Oriented Schlieren
SO EXPERIMENTS IN FLUIDS
LA English
DT Article
AB The Calcium-K Eclipse Background-Oriented Schlieren experiment was performed as a proof of concept test to evaluate the effectiveness of using the solar disk as a background to perform the Background-Oriented Schlieren (BOS) method of flow visualization. A ground-based imaging system was equipped with a Calcium-K line optical etalon filter to enable the use of the chromosphere of the sun as the irregular background to be used for BOS. A US Air Force T-38 aircraft performed three supersonic runs which eclipsed the sun as viewed from the imaging system. The images were successfully post-processed using optical flow methods to qualitatively reveal the density gradients in the flow around the aircraft.
C1 [Hill, Michael A.] NASA, Armstrong Flight Res Ctr, POB 273 MS4840A, Edwards AFB, CA 93523 USA.
[Haering, Edward A., Jr.] NASA, Armstrong Flight Res Ctr, POB 273 MS4800, Edwards AFB, CA 93523 USA.
RP Hill, MA (reprint author), NASA, Armstrong Flight Res Ctr, POB 273 MS4840A, Edwards AFB, CA 93523 USA.
EM Michael.a.hill-1@nasa.gov; Edward.a.haering@nasa.gov
FU National Aeronautics and Space Administration Commercial Supersonics
Technology Project; National Aeronautics and Space Administration
Armstrong Flight Research Center
FX The authors thank the National Aeronautics and Space Administration
Commercial Supersonics Technology Project for funding and support,
National Aeronautics and Space Administration Armstrong Flight Research
Center support personnel for enabling these flights, and Major Jonathan
Orso and Colonel Glenn Graham of the US Air Force Test Pilot School for
their skillful flying.
NR 20
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U1 1
U2 1
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0723-4864
EI 1432-1114
J9 EXP FLUIDS
JI Exp. Fluids
PD JAN
PY 2017
VL 58
IS 1
AR 4
DI 10.1007/s00348-016-2285-7
PG 12
WC Engineering, Mechanical; Mechanics
SC Engineering; Mechanics
GA EI6SV
UT WOS:000392628000004
ER
PT J
AU Helvey, M
Pomeroy, C
Pradhan, NC
Squires, D
Stohs, S
AF Helvey, Mark
Pomeroy, Caroline
Pradhan, Naresh C.
Squires, Dale
Stohs, Stephen
TI Can the United States have its fish and eat it too?
SO MARINE POLICY
LA English
DT Article
DE Imported seafood; International trade; Leakage; Marine conservation
policy; Seafood security
ID ENVIRONMENTAL KUZNETS CURVES; LAND-USE; FOOD SECURITY; BIODIVERSITY
CONSERVATION; FISHERIES MANAGEMENT; ECOLOGICAL FOOTPRINT; GLOBAL
DISPLACEMENT; LONGLINE FISHERY; DYNAMIC OCEAN; CONSUMPTION
AB As domestic affluence increases, nations advocate for conservation policies to protect domestic biodiversity that often curtail natural resource production activities such as fishing. If concomitant consumption patterns remain unchanged, environmentally conscious nations with high consumption rates such as the U.S. may only be distancing themselves from the negative environmental impacts associated with consuming resources and commodities produced elsewhere. This unintended displacement of ecosystem impacts, or leakage, associated with conservation policies has not been studied extensively in marine fisheries. This paper examines this topic, drawing on case studies to illustrate the ways in which unilateral marine conservation actions can shift ecosystem impacts elsewhere, as has been documented in land use interventions. The authors argue that the U.S. should recognize these distant ecological consequences and move toward greater self-sufficiency to protect its seafood security and minimize leakage as well as undertake efforts to reduce ecosystem impacts of foreign fisheries on which it relies. Six solutions are suggested for broadening the marine conservation and seafood consumption discussion to address leakage induced by U.S. policy.
C1 [Helvey, Mark] NOAA, Natl Marine Fisheries Serv, Long Beach, CA USA.
[Helvey, Mark] Sustainable Seafood Consultants, 16 Saucito, Foothill Ranch, CA 92610 USA.
[Pomeroy, Caroline] Univ Calif Santa Cruz, Calif Sea Grant Extens Program, Long Marine Lab, 100 Shaffer Rd, Santa Cruz, CA 95060 USA.
[Pradhan, Naresh C.] New England Fishery Management Council, 50 Water St,Mill 2, Newburyport, MA 01950 USA.
[Squires, Dale; Stohs, Stephen] NOAA, Natl Marine Fisheries Serv, Southwest Fisheries Sci Ctr, 8901 La Jolla Shores Dr, La Jolla, CA 92037 USA.
RP Helvey, M (reprint author), Sustainable Seafood Consultants, 16 Saucito, Foothill Ranch, CA 92610 USA.
EM markhelvey2@gmail.com; cpomeroy@ucsd.edu; npradhan@nefmc.org;
dale.squires@noaa.gov; stephen.stohs@noaa.gov
NR 62
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U1 6
U2 6
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0308-597X
EI 1872-9460
J9 MAR POLICY
JI Mar. Pol.
PD JAN
PY 2017
VL 75
BP 62
EP 67
DI 10.1016/j.marpol.2016.10.013
PG 6
WC Environmental Studies; International Relations
SC Environmental Sciences & Ecology; International Relations
GA EH6SP
UT WOS:000391904500008
ER
PT J
AU Noble, E
Druyan, LM
Fulakeza, M
AF Noble, Erik
Druyan, Leonard M.
Fulakeza, Matthew
TI The Sensitivity of WRF Daily Summertime Simulations over West Africa to
Alternative Parameterizations. Part II: Precipitation
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID EASTERLY WAVES; CLIMATE-CHANGE; SQUALL LINES; MODEL; CONVECTION;
DISTURBANCES; VARIABILITY; ATLANTIC; PREDICTION; RAINFALL
AB This paper evaluates the performance of the Weather Research and Forecasting (WRF) Model as a regional atmospheric model over West Africa. It tests WRF's sensitivity to 64 configurations of alternative parameterizations in a series of 104 twelve-day September simulations during 11 consecutive years, 2000-10. The 64 configurations combine WRF parameterizations of cumulus convection, radiation, surface hydrology, and the PBL. Simulated daily and total precipitation results are validated against Global Precipitation Climatology Project (GPCP) and Tropical Rainfall Measuring Mission (TRMM) data. Particular attention is given to westward-propagating precipitation maxima associated with African easterly waves (AEWs). A wide range of daily precipitation validation scores demonstrates the influence of alternative parameterizations. The best WRF performers achieve time-longitude correlations (against GPCP) of between 0.35 and 0.42 and spatiotemporal variability amplitudes only slightly higher than observed estimates. A parallel simulation by the benchmark Regional Model version 3 achieves a higher correlation (0.52) and realistic spatiotemporal variability amplitudes. The largest favorable impact on WRF precipitation validation is achieved by selecting the Grell-Devenyi convection scheme, resulting in higher correlations against observations than using the Kain-Fritch convection scheme. Other parameterizations have less obvious impacts. Validation statistics for optimized WRF configurations simulating the parallel period during 2000-10 are more favorable for 2005, 2006, and 2008 than for other years. The selection of some of the same WRF configurations as high scorers in both circulation and precipitation validations supports the notion that simulations of West African daily precipitation benefit from skillful simulations of associated AEW vorticity centers and that simulations of AEWs would benefit from skillful simulations of convective precipitation.
C1 [Noble, Erik; Druyan, Leonard M.; Fulakeza, Matthew] NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
[Druyan, Leonard M.; Fulakeza, Matthew] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
RP Noble, E (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM erik.noble@nasa.gov
FU NASA [NNX11AR61G, NNX11AR63A]; National Science Foundation [AGS-1000874]
FX The authors gratefully acknowledge the inspiration and encouragement for
this project of the late Professor Thomas Warner. EUN was supported by
NASA Cooperative Agreement NNX11AR61G. LMD and MF were supported by
National Science Foundation Grant AGS-1000874 and NASA Cooperative
Agreement NNX11AR63A. MERRA data were obtained from NASA's GMAO web site
(http://gmao.gsfc.nasa.gov/merra), NCEP Reanalysis-2 data were provided
by the NOAA-ESRL Physical Sciences Division, Boulder, Colorado, from
their website (http://www.esrl.noaa.gov/psd).
NR 68
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U1 5
U2 5
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0027-0644
EI 1520-0493
J9 MON WEATHER REV
JI Mon. Weather Rev.
PD JAN
PY 2017
VL 145
IS 1
BP 215
EP 233
DI 10.1175/MWR-D-15-0294.1
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EI3SP
UT WOS:000392411900012
ER
PT S
AU Tselioudis, G
Konsta, D
AF Tselioudis, G.
Konsta, D.
BE Karacostas, TS
Bais, AF
Nastos, PT
TI The 'Storm Curtain' Effect: Poleward Shift of Clouds, Their Radiative
Effects, and the Role of Midlatitude Storms
SO PERSPECTIVES ON ATMOSPHERIC SCIENCES
SE Springer Atmospheric Sciences
LA English
DT Proceedings Paper
CT 13th International Conference on Meteorology, Climatology and
Atmospheric Physics (COMECAP)
CY SEP 19-21, 2016
CL Aristotle Univ Res Disseminat Ctr, Thessaloniki, GREECE
SP Aristotle Univ Thessaloniki, Sch Phys, Lab Atmospher Phys, Aristotle Univ Thessaloniki, Sch Geol, Dept Meteorol & Climatol, Hellen Meteorol Soc, Mariolopoulos Kanaginis Fdn Environm Sci
HO Aristotle Univ Res Disseminat Ctr
AB Midlatitude storm track density shifts are correlated with satellite-derived cloud properties and radiation effects. We find that high-cloud amount constitutes the primary tracer of storm track shifts, and that high clouds have been shifting poleward in the 1984-2009 time period by 0.30-0.46 degrees per decade in all four major oceanic storm track regions. Driven by the poleward shift of high clouds, the total cloud field and the cloud radiative effect have also been shifting poleward at a rate of 0.12-0.23 degrees per decade, similar to the rate of the poleward shift of the storms in three out of the four major oceanic storm tracks. This poleward total cloud amount shift produces a change in the radiative effect of storm clouds as they move to a region of lower solar insolation.
C1 [Tselioudis, G.] Columbia Univ, NASA, GISS, New York, NY USA.
[Konsta, D.] Natl Observ Athens, IAASARS, Athens, Greece.
RP Konsta, D (reprint author), Natl Observ Athens, IAASARS, Athens, Greece.
EM dkonsta@noa.gr
FU EU FP7 EUCLIPSE program
FX The authors of this work would like to acknowledge support by the EU FP7
EUCLIPSE program.
NR 5
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U1 0
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PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
SN 2194-5217
BN 978-3-319-35095-0; 978-3-319-35094-3
J9 SPRINGER ATMOS SCI
PY 2017
BP 725
EP 731
DI 10.1007/978-3-319-35095-0_104
PG 7
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA BG8KN
UT WOS:000392385800104
ER
PT S
AU Katragkou, E
Gkotovou, I
Kartsios, S
Pavlidis, V
Tsigaridis, K
Trail, M
Nazarenko, L
Karacostas, TS
AF Katragkou, E.
Gkotovou, I.
Kartsios, S.
Pavlidis, V.
Tsigaridis, K.
Trail, M.
Nazarenko, L.
Karacostas, Theodore S.
BE Karacostas, TS
Bais, AF
Nastos, PT
TI AUTH Regional Climate Model Contributions to EURO-CORDEX
SO PERSPECTIVES ON ATMOSPHERIC SCIENCES
SE Springer Atmospheric Sciences
LA English
DT Proceedings Paper
CT 13th International Conference on Meteorology, Climatology and
Atmospheric Physics (COMECAP)
CY SEP 19-21, 2016
CL Aristotle Univ Res Disseminat Ctr, Thessaloniki, GREECE
SP Aristotle Univ Thessaloniki, Sch Phys, Lab Atmospher Phys, Aristotle Univ Thessaloniki, Sch Geol, Dept Meteorol & Climatol, Hellen Meteorol Soc, Mariolopoulos Kanaginis Fdn Environm Sci
HO Aristotle Univ Res Disseminat Ctr
ID CONFIGURATION; ENSEMBLE
AB Regional climate downscaling techniques are being increasingly used to provide higher-resolution climate information than is available directly from contemporary global climate models. The Coordinated Regional Climate Downscaling Experiment (CORDEX) initiative was build to foster communication and knowledge exchange between regional climate modelers. The Department of Meteorology and Climatology of the Aristotle University of Thessaloniki has been contributing to the CORDEX initiative since 2010, with regional climate model simulations over the European domain (EURO-CORDEX). Results of this work are presented here, including two hindcasts and a historical simulation with the Weather Research Forecasting model (WRF), driven by ERA-interim reanalysis and the NASA Earth System Goddard Institute for Space Studies (GISS) ModelE2, respectively. Model simulations are evaluated with the EOBS climatology and the model performance is assessed.
C1 [Katragkou, E.; Gkotovou, I.; Kartsios, S.; Pavlidis, V.; Karacostas, Theodore S.] Aristotle Univ Thessaloniki, Sch Geol, Dept Meteorol & Climatol, Thessaloniki 54124, Greece.
[Tsigaridis, K.; Nazarenko, L.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
[Tsigaridis, K.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Trail, M.] Georgia Inst Technol, Atlanta, GA 30332 USA.
RP Katragkou, E (reprint author), Aristotle Univ Thessaloniki, Sch Geol, Dept Meteorol & Climatol, Thessaloniki 54124, Greece.
EM katragou@auth.gr
FU Greek Research & Technology Network (GRNET) in the National HPC facility
ARIS [001036]; AUTH-Research Committee program "Reinforcing research
activity within AUTH: AUTH-Lecturers"
FX This work was supported by computational time granted from the Greek
Research & Technology Network (GRNET) in the National HPC facility ARIS
under project 001036. This study was financial supported by the
AUTH-Research Committee program "Reinforcing research activity within
AUTH-2014: AUTH-Lecturers". We acknowledge the E-OBS data set and the
data providers in the ECA&D project (http://www.ecad.eu). The model
coupling NASA_GISS/WRF was performed in the framework of the project
REQUA (FP7, People, International Research Staff Exchange Scheme).
NR 8
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U1 1
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PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
SN 2194-5217
BN 978-3-319-35095-0; 978-3-319-35094-3
J9 SPRINGER ATMOS SCI
PY 2017
BP 741
EP 746
DI 10.1007/978-3-319-35095-0_106
PG 6
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA BG8KN
UT WOS:000392385800106
ER
PT S
AU Georgakaki, P
Papadimas, CD
Hatzianastassiou, N
Fotiadi, A
Matsoukas, C
Stackhouse, P
Kanakidou, M
Vardavas, I
AF Georgakaki, P.
Papadimas, C. D.
Hatzianastassiou, N.
Fotiadi, A.
Matsoukas, C.
Stackhouse, P.
Kanakidou, M.
Vardavas, I.
BE Karacostas, TS
Bais, AF
Nastos, PT
TI Direct Effect of Aerosols on Solar Radiation Over the Eastern
Mediterranean Basin on a Daily 1 degrees by 1 degrees Resolution
SO PERSPECTIVES ON ATMOSPHERIC SCIENCES
SE Springer Atmospheric Sciences
LA English
DT Proceedings Paper
CT 13th International Conference on Meteorology, Climatology and
Atmospheric Physics (COMECAP)
CY SEP 19-21, 2016
CL Aristotle Univ Res Disseminat Ctr, Thessaloniki, GREECE
SP Aristotle Univ Thessaloniki, Sch Phys, Lab Atmospher Phys, Aristotle Univ Thessaloniki, Sch Geol, Dept Meteorol & Climatol, Hellen Meteorol Soc, Mariolopoulos Kanaginis Fdn Environm Sci
HO Aristotle Univ Res Disseminat Ctr
AB The climatically sensitive Mediterranean basin, which is characterized by high solar radiation amounts and aerosol loadings, is the focus of this study that aims to determine the direct effect of aerosols on solar radiation (DRE) over the eastern basin. The objective is to reveal detailed patterns of aerosol DRE that are smoothed when obtained at coarse resolution. Therefore, computations of DRE are performed at a concurrent spatial and temporal resolution that has not been achieved to date. The DREs are computed for 1 x 1 degrees latitude-longitude grids with the FORTH detailed spectral radiative transfer model (RTM) using daily input data for various atmospheric and surface parameters, such as clouds, water vapor, ozone and surface albedo, taken from the NASA-Langley Global Earth Observing System database. Key aerosol optical properties, namely aerosol optical depth, single scattering albedo and asymmetry parameter, necessary for the RTM runs, are taken from combined climatologies, like the Global Aerosol Data Set, and the satellite-derived datasets of Total Ozone Mapping Spectrometer and Advanced Very High resolution Radiometer that satisfy daily availability at the RTM required spectral and 1 x 1 degrees resolution. The aerosol DREs are computed at the surface, the top-of-atmosphere and within the atmosphere, over the period 1985-1995.
C1 [Georgakaki, P.; Papadimas, C. D.; Hatzianastassiou, N.] Univ Ioannina, Dept Phys, Lab Meteorol, GR-45110 Ioannina, Greece.
[Fotiadi, A.] Univ Patras, Dept Environm & Nat Resources Management, Patras, Greece.
[Matsoukas, C.] Univ Aegean, Dept Environm, Mitilini, Greece.
[Stackhouse, P.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Stackhouse, P.; Kanakidou, M.] Univ Crete, Dept Chem, Iraklion, Greece.
[Stackhouse, P.; Vardavas, I.] Univ Crete, Dept Phys, Iraklion, Greece.
RP Hatzianastassiou, N (reprint author), Univ Ioannina, Dept Phys, Lab Meteorol, GR-45110 Ioannina, Greece.
EM nhatzian@cc.uoi.gr
NR 7
TC 0
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U1 0
U2 0
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
SN 2194-5217
BN 978-3-319-35095-0; 978-3-319-35094-3
J9 SPRINGER ATMOS SCI
PY 2017
BP 1215
EP 1221
DI 10.1007/978-3-319-35095-0_175
PG 7
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA BG8KN
UT WOS:000392385800175
ER
PT S
AU Voulgarakis, A
Field, R
Fromm, M
AF Voulgarakis, A.
Field, R.
Fromm, M.
BE Karacostas, TS
Bais, AF
Nastos, PT
TI Fire Impacts on High-Altitude Atmospheric Com-Position
SO PERSPECTIVES ON ATMOSPHERIC SCIENCES
SE Springer Atmospheric Sciences
LA English
DT Proceedings Paper
CT 13th International Conference on Meteorology, Climatology and
Atmospheric Physics (COMECAP)
CY SEP 19-21, 2016
CL Aristotle Univ Res Disseminat Ctr, Thessaloniki, GREECE
SP Aristotle Univ Thessaloniki, Sch Phys, Lab Atmospher Phys, Aristotle Univ Thessaloniki, Sch Geol, Dept Meteorol & Climatol, Hellen Meteorol Soc, Mariolopoulos Kanaginis Fdn Environm Sci
HO Aristotle Univ Res Disseminat Ctr
ID INTERANNUAL VARIABILITY; EMISSIONS
AB Fire emissions can strongly impact atmospheric abundances of trace gases and aerosols, in ways that vary strongly in time and space. There is emerging understanding that fires do not only influence areas in the lower troposphere, where the land-surface is in contact with the atmosphere, but can also have significant effects on the upper troposphere and even the stratosphere. Here, I will present example results from our ongoing global modelling studies investigating such effects. First, an overview of recent results will be presented, i.e. from (a) a case study on how high-altitude injections can influence stratospheric composition, and (b) a study that demonstrated how satellite observations can be used to understand the transport of fire pollution into the upper troposphere/lower stratosphere (UTLS), and how such measurements can be used to evaluate convective processes in composition-climate models. Subsequently, the role of typical low-injection fires in driving the interannual variability of UTLS composition will be discussed based on results from recent global model experiments, with a focus on impacts on CO and ozone. The findings show a major role of fire emissions in driving UTLS CO and a minor role in driving UTLS ozone interannual variability.
C1 [Voulgarakis, A.] Imperial Coll, London, England.
[Field, R.] NASA GISS, New York, NY USA.
[Field, R.] Columbia Univ, New York, NY 10027 USA.
[Fromm, M.] Naval Res Lab, Washington, DC 20375 USA.
RP Voulgarakis, A (reprint author), Imperial Coll, London, England.
EM a.voulgarakis@imperial.ac.uk
FU NASA ACMAP; NASA High-End Computing (HEC); Goddard Space Flight Center;
European Commission's Marie Curie International Research Staff Exchange
Scheme (IRSES); Regional climate- air quality interactions (REQUA)
FX The authors wish to thank NASA ACMAP for funding and the NASA High-End
Computing (HEC) Program for computation resources through the NASA
Center for Climate Simulation (NCCS) at Goddard Space Flight Center.
Also, the authors thank the European Commission's Marie Curie
International Research Staff Exchange Scheme (IRSES) for funding under
the project titled " Regional climate- air quality interactions
(REQUA)".
NR 9
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U1 2
U2 2
PU SPRINGER
PI DORDRECHT
PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS
SN 2194-5217
BN 978-3-319-35095-0; 978-3-319-35094-3
J9 SPRINGER ATMOS SCI
PY 2017
BP 1231
EP 1237
DI 10.1007/978-3-319-35095-0_177
PG 7
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA BG8KN
UT WOS:000392385800177
ER
PT J
AU Liu, Y
Diner, DJ
AF Liu, Yang
Diner, David J.
TI Multi-Angle Imager for Aerosols: A Satellite Investigation to Benefit
Public Health
SO PUBLIC HEALTH REPORTS
LA English
DT Editorial Material
DE air pollution; environmental health; remote sensing
ID FINE PARTICULATE MATTER; OPTICAL DEPTH; LAND; RETRIEVAL; POLLUTION;
STATES; MODEL
C1 [Liu, Yang] Emory Univ, Rollins Sch Publ Hlth, 1518 Clifton Rd NE, Atlanta, GA 30322 USA.
[Diner, David J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Liu, Y (reprint author), Emory Univ, Rollins Sch Publ Hlth, 1518 Clifton Rd NE, Atlanta, GA 30322 USA.
EM yang.liu@emory.edu
FU California Institute of Technology, Jet Propulsion Laboratory; NASA
FX The author(s) disclosed receipt of the following financial support for
the research, authorship, and/or publication of this article: Part of
this work was carried out at the California Institute of Technology, Jet
Propulsion Laboratory, under contract with NASA.
NR 10
TC 0
Z9 0
U1 0
U2 0
PU SAGE PUBLICATIONS INC
PI THOUSAND OAKS
PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA
SN 0033-3549
EI 1468-2877
J9 PUBLIC HEALTH REP
JI Public Health Rep.
PD JAN-FEB
PY 2017
VL 132
IS 1
BP 14
EP 17
DI 10.1177/0033354916679983
PG 4
WC Public, Environmental & Occupational Health
SC Public, Environmental & Occupational Health
GA EI3AW
UT WOS:000392363100004
PM 28005476
ER
PT S
AU Zalameda, JN
Burke, ER
Horne, MR
Madaras, EI
AF Zalameda, Joseph N.
Burke, Eric R.
Horne, Michael R.
Madaras, Eric I.
BE Quinn, S
Balandraud, X
TI Large Area Nondestructive Evaluation of a Fatigue Loaded Composite
Structure
SO RESIDUAL STRESS, THERMOMECHANICS & INFRARED IMAGING, HYBRID TECHNIQUES
AND INVERSE PROBLEMS, VOL 9
SE Conference Proceedings of the Society for Experimental Mechanics Series
LA English
DT Proceedings Paper
CT SEM Annual Conference and Exposition on Experimental and Applied
Mechanics
CY JUN 06-09, 2016
CL Orlando, FL
SP Soc Expt Mech
DE Large area composite inspection; Thermography; Acoustic emission; Fiber
break; Delamination
AB Large area nondestructive evaluation (NDE) inspections are required for fatigue testing of composite structures to track damage initiation and growth. Of particular interest is the progression of damage leading to ultimate failure to validate damage progression models. In this work, passive thermography and acoustic emission NDE were used to track damage growth up to failure of a composite three-stringer panel. Fourteen acoustic emission sensors were placed on the composite panel. The signals from the array were acquired simultaneously and allowed for acoustic emission location. In addition, real time thermal data of the composite structure were acquired during loading. Details are presented on the mapping of the acoustic emission locations directly onto the thermal imagery to confirm areas of damage growth leading to ultimate failure. This required synchronizing the acoustic emission and thermal data with the applied loading. In addition, processing of the thermal imagery which included contrast enhancement, removal of optical barrel distortion and correction of angular rotation before mapping the acoustic event locations are discussed.
C1 [Zalameda, Joseph N.; Burke, Eric R.; Madaras, Eric I.] NASA, Langley Res Ctr, MS231, Hampton, VA 23681 USA.
[Horne, Michael R.] NASA, Langley Res Ctr, Natl Inst Aerosp, MS231, Hampton, VA 23681 USA.
RP Zalameda, JN (reprint author), NASA, Langley Res Ctr, MS231, Hampton, VA 23681 USA.
EM joseph.n.zalameda@nasa.gov
FU NASA
FX The authors would like to acknowledge Mr. Wade Jackson of NASA Langley
for ultrasonic inspections, sample preparation, and mounting. Also the
authors would like to acknowledge Mr. William Johnston of Lockheed
Martin for testing support and Mr. Kenneth McLarney, NASA Internship,
Fellowship, and Scholarships (NIFS) student for data processing.
NR 14
TC 0
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U1 0
U2 0
PU SPRINGER
PI NEW YORK
PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES
SN 2191-5644
BN 978-3-319-42255-8; 978-3-319-42254-1
J9 C PROC SOC EXP MECH
PY 2017
BP 21
EP 28
DI 10.1007/978-3-319-42255-8_4
PG 8
WC Thermodynamics; Engineering, Mechanical; Mechanics
SC Thermodynamics; Engineering; Mechanics
GA BG8EL
UT WOS:000392264100004
ER
PT J
AU Bayliss, D
Hojjatpanah, S
Santerne, A
Dragomir, D
Zhou, G
Shporer, A
Colon, KD
Almenara, J
Armstrong, DJ
Barrado, D
Barros, SCC
Bento, J
Boisse, I
Bouchy, F
Brown, DJA
Brown, T
Cameron, A
Cochran, WD
Demangeon, O
Deleuil, M
Diaz, RF
Fulton, B
Horne, K
Hebrard, G
Lillo-Box, J
Lovis, C
Mawet, D
Ngo, H
Osborn, H
Palle, E
Petigura, E
Pollacco, D
Santos, N
Sefako, R
Siverd, R
Sousa, SG
Tsantaki, M
AF Bayliss, D.
Hojjatpanah, S.
Santerne, A.
Dragomir, D.
Zhou, G.
Shporer, A.
Colon, K. D.
Almenara, J.
Armstrong, D. J.
Barrado, D.
Barros, S. C. C.
Bento, J.
Boisse, I.
Bouchy, F.
Brown, D. J. A.
Brown, T.
Cameron, A.
Cochran, W. D.
Demangeon, O.
Deleuil, M.
Diaz, R. F.
Fulton, B.
Horne, K.
Hebrard, G.
Lillo-Box, J.
Lovis, C.
Mawet, D.
Ngo, H.
Osborn, H.
Palle, E.
Petigura, E.
Pollacco, D.
Santos, N.
Sefako, R.
Siverd, R.
Sousa, S. G.
Tsantaki, M.
TI EPIC 201702477b: A TRANSITING BROWN DWARF FROM K2 IN A 41DAY ORBIT
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE planetary systems; techniques: photometric; techniques: spectroscopic
ID RADIAL-VELOCITY MEASUREMENTS; EXTRASOLAR PLANET VALIDATION; JUPITER-MASS
COMPANION; LHS 6343 C; SOPHIE VELOCIMETRY; PHYSICAL-PROPERTIES; GIANT
EXOPLANETS; KEPLER MISSION; CANDIDATES; STELLAR
AB We report the discovery of EPIC 201702477b, a transiting brown dwarf in a long period (40.73691 +/- 0.00037 day) and eccentric (e = 0.2281 +/- 0.0026) orbit. This system was initially reported as a planetary candidate based on two transit events seen in K2 Campaign 1 photometry and later validated as an exoplanet candidate. We confirm the transit and refine the ephemeris with two subsequent ground-based detections of the transit using the Las Cumbres Observatory Global Telescope 1 m telescope network. We rule out any transit timing variations above the level of similar to 30 s. Using high precision radial velocity measurements from HARPS and SOPHIE we identify the transiting companion as a brown dwarf with a mass, radius, and bulk density of 66.9 +/- 1.7 M-J, 0.757 +/- 0.065 R-J, and 191 +/- 51 g cm(-3) respectively. EPIC 201702477b is the smallest radius brown dwarf yet discovered, with a mass just below the H-burning limit. It has the highest density of any planet, substellar mass object, or main-sequence star discovered so far. We find evidence in the set of known transiting brown dwarfs for two populations of objects-high mass brown dwarfs and low mass brown dwarfs. The higher-mass population have radii in very close agreement to theoretical models, and show a lower-mass limit around 60 M-J. This may be the signature of mass-dependent ejection of systems during the formation process.
C1 [Bayliss, D.; Bouchy, F.; Diaz, R. F.; Lovis, C.] Univ Geneva, Astron Observ, 51 Ch Maillettes, CH-1290 Versoix, Switzerland.
[Bayliss, D.; Bento, J.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia.
[Hojjatpanah, S.; Santerne, A.; Barros, S. C. C.; Santos, N.; Sousa, S. G.; Tsantaki, M.] Univ Porto, Inst Astrofis & Ciencias Espaco, CAUP, Rua Estrelas, P-4150762 Oporto, Portugal.
[Hojjatpanah, S.] Univ Zanjan, Dept Phys, Univ Blvd, Zanjan 4537138791, Iran.
[Santerne, A.; Boisse, I.; Demangeon, O.; Deleuil, M.] Aix Marseille Univ, CNRS, Lab Astrophys Marseille, UMR 7326, F-13388 Marseille, France.
[Dragomir, D.] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
[Dragomir, D.] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Zhou, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Shporer, A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Colon, K. D.] NASA, Ames Res Ctr, M-S 244-30, Moffett Field, CA 94035 USA.
[Colon, K. D.] Bay Area Environm Res Inst, 625 2nd St Ste 209, Petaluma, CA 94952 USA.
[Almenara, J.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.
[Armstrong, D. J.; Brown, D. J. A.; Osborn, H.; Pollacco, D.] Univ Warwick, Dept Phys, Gibbet Hill Rd, Coventry CV4 7AL, W Midlands, England.
[Armstrong, D. J.] Queens Univ Belfast, Sch Math & Phys, ARC, Belfast BT7 1NN, Antrim, North Ireland.
[Barrado, D.] Ctr Astrobiol CSIC INTA, Dept Astrofis, ESAC Campus, E-28691 Villanueva De La Canada, Spain.
[Brown, T.; Siverd, R.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Brown, T.] Univ Colorado, Dept Astrophys & Planetary Sci, CASA, 389 UCB, Boulder, CO 80309 USA.
[Cameron, A.; Horne, K.] Univ St Andrews, SUPA Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Cochran, W. D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Cochran, W. D.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Fulton, B.] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
[Hebrard, G.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR7095, 98bis Blvd Arago, F-75014 Paris, France.
[Hebrard, G.] Univ Aix Marseille, Observ Haute Provence, F-04870 St Michel lObservatoire, France.
[Hebrard, G.] CNRS, F-04870 St Michel lObservatoire, France.
[Lillo-Box, J.] European Southern Observ, Alonso de Cordova 3107,Casilla 19001, Santiago, Chile.
[Mawet, D.; Ngo, H.; Petigura, E.] CALTECH, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
[Palle, E.] Inst Astrofis Canarias, E-38205 Tenerife, Spain.
[Santos, N.] Univ Porto, Dept Fis & Astron, Fac Ciencias, Rua Campo Alegre, P-4169007 Oporto, Portugal.
[Sefako, R.] South African Astron Observ, POB 9, ZA-7935 Observatory, South Africa.
[Tsantaki, M.] UNAM, Inst Radioastron & Astrofis, IRyA, Campus Morelia,AP 3-72, Michoacan 58089, Mexico.
RP Bayliss, D (reprint author), Univ Geneva, Astron Observ, 51 Ch Maillettes, CH-1290 Versoix, Switzerland.; Bayliss, D (reprint author), Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia.
EM daniel.bayliss@unige.ch
OI Ngo, Henry/0000-0001-5172-4859; Shporer, Avi/0000-0002-1836-3120;
Armstrong, David/0000-0002-5080-4117; Barrado,
David/0000-0002-5971-9242; Diaz, Rodrigo/0000-0001-9289-5160
FU Swiss National Science Foundation (SNSF); NASA Science Mission
directorate; National Aeronautics and Space Administration under the
Exoplanet Exploration Program; Fundacao para a Ciencia e Tecnologia, FCT
(Portugal) [UID/FIS/04434/2013 (POCI-01-0145-FEDER-007672),
PTDC/FIS-AST/1526/2014 (POCI-01-0145-FEDER-016886), IF/00169/2012,
IF/00028/2014, IF/01312/2014]; POPH/FSE (EC) by FEDER funding through
Programa Operacional de Factores de Competitividade-COMPETE; ESO
Telescopes at La Silla Paranal Observatory [096.C-0657]; W.M. Keck
Foundation; European Union under a Marie Curie Intra-European Fellowship
for Career Development [627202]; Marie Curie Actions of the European
Commission (FP7-COFUND); Spanish grant [AYA2012-38897-C02-01]; European
Research Council under ERC Grant [337591-ExTrA]; European Union Seventh
Framework programme [313014]; CNES [567133]; Fundacao para a Ciencia e
Tecnologia, (FCT) through Investigador FCT [IF/01312/2014, PTDC/FIS-
AST/1526/2014]; UK Science and Technology Facilities Council (STFC)
grant [ST/M001296/1]; NASA through Hubble Fellowship grant - Space
Telescope Science Institute, [HST-HF2-51372.001-A]; NASA [NAS5-26555,
NNX15AV58G, NNX16AE70G]; UKSA; University of Warwick; National Science
Foundation Graduate Research Fellowship [2014184874, DGE-1144469]; NASA
through Sagan Fellowship Program
FX This work has been carried out within the framework of the National
Centre for Competence in Research "PlanetS" supported by the Swiss
National Science Foundation (SNSF). This paper includes data collected
by the K2 mission. Funding for the K2 mission is provided by the NASA
Science Mission directorate. This paper makes use of data and services
from NASA Exoplanet Archive (Akeson et al. 2013), which is operated by
the California Institute of Technology, under contract with the National
Aeronautics and Space Administration under the Exoplanet Exploration
Program. We are grateful to our colleagues who have performed some of
the observations presented here with the HARPS spectrograph: F.
Motalebi, A. Wyttenbach, and B. Lavie. The Porto group acknowledges the
support from the Fundacao para a Ciencia e Tecnologia, FCT (Portugal) in
the form of the grants, projects, and contracts UID/FIS/04434/2013
(POCI-01-0145-FEDER-007672), PTDC/FIS-AST/1526/2014
(POCI-01-0145-FEDER-016886), IF/00169/2012, IF/00028/2014, IF/01312/2014
and POPH/FSE (EC) by FEDER funding through the Programa Operacional de
Factores de Competitividade-COMPETE.; Partly based on observations made
at Observatoire de Haute Provence (CNRS), France and with ESO Telescopes
at the La Silla Paranal Observatory under programme ID 096.C-0657. Some
of the data presented herein were obtained at the W. M. Keck
Observatory, which is operated as a scientific partnership among the
California Institute of Technology, the University of California and the
National Aeronautics and Space Administration. The Observatory was made
possible by the generous financial support of the W.M. Keck Foundation.
The authors wish to recognize and acknowledge the very significant
cultural role and reverence that the summit of Mauna Kea has always had
within the indigenous Hawaiian community.; A.S. is supported by the
European Union under a Marie Curie Intra-European Fellowship for Career
Development with reference FP7-PEOPLE-2013-IEF, number 627202. J.L.-B.
acknowledges financial support from the Marie Curie Actions of the
European Commission (FP7-COFUND) and the Spanish grant
AYA2012-38897-C02-01. J.M.A. acknowledges funding from the European
Research Council under the ERC Grant Agreement n. 337591-ExTrA. D.J.A.
and D.P. acknowledge funding from the European Union Seventh Framework
programme (FP7/2007-2013) under grant agreement No. 313014 (ETAEARTH).
O.D. acknowledges support by CNES through contract 567133. S.C.C.B.
acknowledges support by the Fundacao para a Ciencia e Tecnologia, (FCT)
through the Investigador FCT Contract No. IF/01312/2014 and the grant
reference PTDC/FIS- AST/1526/2014.; K.H. and A.C.C. acknowledge support
from UK Science and Technology Facilities Council (STFC) grant
ST/M001296/1. D. Dragomir acknowledges support provided by NASA through
Hubble Fellowship grant HST-HF2-51372.001-A awarded by the Space
Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., for NASA, under contract
NAS5-26555. D.J.A.B. acknowledges support from the UKSA and the
University of Warwick. B.J.F. notes that this material is based upon
work supported by the National Science Foundation Graduate Research
Fellowship under grant No. 2014184874. Any opinion, findings, and
conclusions or recommendations expressed in this material are those of
the authors(s) and do not necessarily reflect the views of the National
Science Foundation. W.D.C. acknowledges support from NASA Grants
NNX15AV58G and NNX16AE70G. This material is based upon work supported by
the National Science Foundation Graduate Research Fellowship under Grant
No.. DGE-1144469 This work was performed in part under contract with the
Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan
Fellowship Program executed by the NASA Exoplanet Science Institute.
NR 76
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U1 2
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD JAN
PY 2017
VL 153
IS 1
AR 15
DI 10.3847/1538-3881/153/1/15
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EH3PA
UT WOS:000391682800004
ER
PT J
AU Fischer, PD
Brown, ME
Trumbo, SK
Hand, KP
AF Fischer, P. D.
Brown, M. E.
Trumbo, S. K.
Hand, K. P.
TI SPATIALLY RESOLVED SPECTROSCOPY OF EUROPA'S LARGE-SCALE COMPOSITIONAL
UNITS AT 3-4 mu m WITH KECK NIRSPEC
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE planets and satellites: composition; planets and satellites: individual
(Europa); planets and satellites: surfaces
ID GALILEAN SATELLITES; CASSINI VIMS; SURFACE; ICE; SPECTRA; ENCELADUS;
PYTHON; OCEAN
AB We present spatially resolved spectroscopic observations of Europa's surface at 3-4 mu m obtained with the near-infrared spectrograph and adaptive optics system on the Keck II telescope. These are the highest quality spatially resolved reflectance spectra of Europa's surface at 3-4 mu m. The observations spatially resolve Europa's large-scale compositional units at a resolution of several hundred kilometers. The spectra show distinct features and geographic variations associated with known compositional units; in particular, large-scale leading hemisphere chaos shows a characteristic longward shift in peak reflectance near 3.7 mu m compared to icy regions. These observations complement previous spectra of large-scale chaos, and can aid efforts to identify the endogenous non-ice species.
C1 [Fischer, P. D.; Brown, M. E.; Trumbo, S. K.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Hand, K. P.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Fischer, PD (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
EM pfischer@caltech.edu
FU National Science Foundation [1313461]; NASA Earth and Space Science
Fellowship; Jet Propulsion Laboratory, California Institute of
Technology; National Aeronautics and Space Administration; W. M. Keck
Foundation
FX This research was supported by Grant 1313461 from the National Science
Foundation and by the NASA Earth and Space Science Fellowship. K.P.H.
acknowledges support from the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration. The data presented herein were obtained at the
W. M. Keck Observatory, which is operated as a scientific partnership
among the California Institute of Technology, the University of
California, and the National Aeronautics and Space Administration. The
Observatory was made possible by the generous financial support of the
W. M. Keck Foundation. The authors wish to recognize and acknowledge the
very significant cultural role and reverence that the summit of Maunakea
has always had within the indigenous Hawaiian community. We are most
fortunate to have the opportunity to conduct observations from this
mountain.
NR 32
TC 0
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U1 2
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD JAN
PY 2017
VL 153
IS 1
AR 13
DI 10.3847/1538-3881/153/1/13
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EH3PA
UT WOS:000391682800002
ER
PT J
AU Hong, J
Allen, B
Grindlay, J
Barthelmy, S
AF Hong, Jaesub
Allen, Branden
Grindlay, Jonathan
Barthelmy, Scott
TI IMAGING ANALYSIS OF THE HARD X-RAY TELESCOPE ProtoEXIST2 AND NEW
TECHNIQUES FOR HIGH-RESOLUTION CODED-APERTURE TELESCOPES
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE balloons; instrumentation: detectors; techniques: image processing;
X-rays: binaries
ID MISSION; ARRAY
AB Wide-field (greater than or similar to 100 deg(2)) hard X-ray coded-aperture telescopes with high angular resolution (less than or similar to 2') will enable a wide range of time domain astrophysics. For instance, transient sources such as gamma-ray bursts can be precisely localized without the assistance of secondary focusing X-ray telescopes to enable rapid followup studies. On the other hand, high angular resolution in coded-aperture imaging introduces a new challenge in handling the systematic uncertainty: the average photon count per pixel is often too small to establish a proper background pattern or model the systematic uncertainty in a timescale where the model remains invariant. We introduce two new techniques to improve detection sensitivity, which are designed for, but not limited to, a high-resolution coded-aperture system: a self-background modeling scheme which utilizes continuous scan or dithering operations, and a Poisson-statistics based probabilistic approach to evaluate the significance of source detection without subtraction in handling the background. We illustrate these new imaging analysis techniques in high resolution coded-aperture telescope using the data acquired by the wide-field hard X-ray telescope ProtoEXIST2 during a high-altitude balloon flight in fall 2012. We review the imaging sensitivity of ProtoEXIST2 during the flight, and demonstrate the performance of the new techniques using our balloon flight data in comparison with a simulated ideal Poisson background.
C1 [Hong, Jaesub; Allen, Branden; Grindlay, Jonathan] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Barthelmy, Scott] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Hong, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU NASA/APRA grant [NNX14AD59G]
FX This work was supported by NASA/APRA grant NNX14AD59G.
NR 11
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U1 0
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD JAN
PY 2017
VL 153
IS 1
AR 11
DI 10.3847/1538-3881/153/1/11
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EH2ER
UT WOS:000391580800006
ER
PT J
AU Kilpatrick, BM
Lewis, NK
Kataria, T
Deming, D
Ingalls, JG
Krick, JE
Tucker, GS
AF Kilpatrick, Brian M.
Lewis, Nikole K.
Kataria, Tiffany
Deming, Drake
Ingalls, James G.
Krick, Jessica E.
Tucker, Gregory S.
TI SPITZER SECONDARY ECLIPSE DEPTHS WITH MULTIPLE INTRAPIXEL SENSITIVITY
CORRECTION METHODS OBSERVATIONS OF WASP-13b, WASP-15b, WASP-16b,
WASP-62b, AND HAT-P-22b
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE atmospheric effects; methods: numerical; planets and satellites:
atmospheres; planets and satellites: detection; techniques: photometric
ID INFRARED ARRAY CAMERA; M PHASE CURVES; HD 189733B; MU-M; ATMOSPHERIC
CIRCULATION; SPACE-TELESCOPE; GIANT PLANETS; GJ 436; EXOPLANET; EMISSION
AB We measure the 4.5 mu m thermal emission of five transiting hot Jupiters, WASP-13b, WASP-15b, WASP-16b, WASP-62b, and HAT-P-22b using channel 2 of the Infrared Array Camera (IRAC) on the Spitzer Space Telescope. Significant intrapixel sensitivity variations in Spitzer IRAC data require careful correction in order to achieve precision on the order of several hundred parts per million (ppm) for the measurement of exoplanet secondary eclipses. We determine eclipse depths by first correcting the raw data using three independent data reduction methods. The Pixel Gain Map (PMAP), Nearest Neighbors (NNBR), and Pixel Level Decorrelation (PLD) each correct for the intrapixel sensitivity effect in Spitzer photometric time-series observations. The results from each methodology are compared against each other to establish if they reach a statistically equivalent result in every case and to evaluate their ability to minimize uncertainty in the measurement. We find that all three methods produce reliable results. For every planet examined here NNBR and PLD produce results that are in statistical agreement. However, the PMAP method appears to produce results in slight disagreement in cases where the stellar centroid is not kept consistently on the most well characterized area of the detector. We evaluate the ability of each method to reduce the scatter in the residuals as well as in the correlated noise in the corrected data. The NNBR and PLD methods consistently minimize both white and red noise levels and should be considered reliable and consistent. The planets in this study span equilibrium temperatures from 1100 to 2000. K and have brightness temperatures that require either high albedo or efficient recirculation. However, it is possible that other processes such as clouds or disequilibrium chemistry may also be responsible for producing these brightness temperatures.
C1 [Kilpatrick, Brian M.; Tucker, Gregory S.] Brown Univ, Dept Phys, Box 1843, Providence, RI 02904 USA.
[Lewis, Nikole K.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Kataria, Tiffany] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Ingalls, James G.; Krick, Jessica E.] CALTECH, Infrared Proc & Anal Ctr, Spitzer Sci Ctr, Mail Code 220-6, Pasadena, CA 91125 USA.
RP Kilpatrick, BM (reprint author), Brown Univ, Dept Phys, Box 1843, Providence, RI 02904 USA.
EM brian_kilpatrick@brown.edu; nlewis@stsci.org;
tiffany.kataria@jpl.nasa.gov; ddeming@astro.umd.edu;
krick@ipac.caltech.edu
FU Brown University
FX BMK acknowledges Brown University for its financial support of his
contributions to this work. This work is based on observations made with
the Spitzer Space Telescope, which is operated by the Jet Propulsion
Laboratory, California Institute of Technology under a contract with
NASA. We also acknowledge that part of this work was completed at the
Space Telescope Science Institute (STScI) operated by AURA, Inc. This
research has made use of the Exoplanet Orbit Database and the Exoplanet
Data Explorer at exoplanets.org.
NR 31
TC 0
Z9 0
U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD JAN
PY 2017
VL 153
IS 1
AR 22
DI 10.3847/1538-3881/153/1/22
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EH4DH
UT WOS:000391720800007
ER
PT J
AU Yang, Y
Hashimoto, J
Hayashi, SS
Tamura, M
Mayama, S
Rafikov, R
Akiyama, E
Carson, JC
Janson, M
Kwon, J
De Leon, J
Oh, D
Takami, M
Tang, YW
Kudo, T
Kusakabe, N
Abe, L
Brandner, W
Brandt, TD
Egner, S
Feldt, M
Goto, M
Grady, CA
Guyon, O
Hayano, Y
Hayashi, M
Henning, T
Hodapp, KW
Ishii, M
Iye, M
Kandori, R
Knapp, GR
Kuzuhara, M
Matsuo, T
Mcelwain, MW
Miyama, S
Morino, JI
Moro-Martin, A
Nishimura, T
Pyo, TS
Serabyn, E
Suenaga, T
Suto, H
Suzuki, R
Takahashi, YH
Takato, N
Terada, H
Thalmann, C
Turner, EL
Watanabe, M
Wisniewski, J
Yamada, T
Takami, H
Usuda, T
AF Yang, Yi
Hashimoto, Jun
Hayashi, Saeko S.
Tamura, Motohide
Mayama, Satoshi
Rafikov, Roman
Akiyama, Eiji
Carson, Joseph C.
Janson, Markus
Kwon, Jungmi
De Leon, Jerome
Oh, Daehyeon
Takami, Michihiro
Tang, Ya-Wen
Kudo, Tomoyuki
Kusakabe, Nobuhiko
Abe, Lyu
Brandner, Wolfgang
Brandt, Timothy D.
Egner, Sebastian
Feldt, Markus
Goto, Miwa
Grady, Carol A.
Guyon, Olivier
Hayano, Yutaka
Hayashi, Masahiko
Henning, Thomas
Hodapp, Klaus W.
Ishii, Miki
Iye, Masanori
Kandori, Ryo
Knapp, Gillian R.
Kuzuhara, Masayuki
Matsuo, Taro
Mcelwain, Michael W.
Miyama, Shoken
Morino, Jun-Ichi
Moro-Martin, Amaya
Nishimura, Tetsuo
Pyo, Tae-Soo
Serabyn, Eugene
Suenaga, Takuya
Suto, Hiroshi
Suzuki, Ryuji
Takahashi, Yasuhiro H.
Takato, Naruhisa
Terada, Hiroshi
Thalmann, Christian
Turner, Edwin L.
Watanabe, Makoto
Wisniewski, John
Yamada, Toru
Takami, Hideki
Usuda, Tomonori
TI NEAR-INFRARED IMAGING POLARIMETRY OF INNER REGION OF GG TAU A DISK
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE binaries: close; planets and satellites: formation; protoplanetary
disks; stars: pre-main sequence
ID CIRCUMBINARY DISK; PLANET FORMATION; STELLAR MULTIPLICITY;
BINARY-SYSTEMS; YOUNG; DYNAMICS; RING; EVOLUTION; IMAGES; STAR
AB By performing non-masked polarization imaging with Subaru/HiCIAO, polarized scattered light from the inner region of the disk around the GG Tau A system was successfully detected in the H band, with a spatial resolution of approximately 0 07, revealing the complicated inner disk structures around this young binary. This paper reports the observation of an arc-like structure to the north of GG Tau Ab, and part of a circumstellar structure that is noticeable around GG Tau Aa, extending to a distance of approximately 28 au from the primary star. The speckle noise around GG Tau Ab constrains its disk radius to < 13 au. Based on the size of the circumbinary ring and the circumstellar disk around GG Tau Aa, the semimajor axis of the binary's orbit is likely to be 62 au. A comparison of the present observations with previous Atacama Large Millimeter Array and near-infrared H-2 emission observations suggests that the north arc could be part of a large streamer flowing from the circumbinary ring to sustain the circumstellar disks. According to the previous studies, the circumstellar disk around GG Tau Aa has enough mass and can sustain itself for a duration sufficient for planet formation; thus, our study indicates that planets can form within close (separation. 100 au) young binary systems.
C1 [Yang, Yi; Hayashi, Saeko S.; Mayama, Satoshi; Oh, Daehyeon; Hayano, Yutaka; Hayashi, Masahiko; Pyo, Tae-Soo; Suenaga, Takuya; Takato, Naruhisa; Takami, Hideki; Usuda, Tomonori] SOKENDAI Graudate Univ Adv Studies, Dept Astron Sci, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Yang, Yi; Tamura, Motohide; Mayama, Satoshi; Akiyama, Eiji; Oh, Daehyeon; Abe, Lyu; Hayano, Yutaka; Hayashi, Masahiko; Ishii, Miki; Iye, Masanori; Kandori, Ryo; Suenaga, Takuya; Suto, Hiroshi; Suzuki, Ryuji; Takahashi, Yasuhiro H.; Terada, Hiroshi; Takami, Hideki; Usuda, Tomonori] NINS, NAOJ, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Hashimoto, Jun; Tamura, Motohide; Kusakabe, Nobuhiko; Kuzuhara, Masayuki; Suto, Hiroshi] NINS, Astrobiol Ctr, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Hayashi, Saeko S.; Kudo, Tomoyuki; Guyon, Olivier; Hayano, Yutaka; Nishimura, Tetsuo; Pyo, Tae-Soo; Takato, Naruhisa] NINS, NAOJ, Subaru Telescope, 650 North Aohoku Pl, Hilo, HI 96720 USA.
[Tamura, Motohide; De Leon, Jerome; Takahashi, Yasuhiro H.] Univ Tokyo, Dept Astron, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan.
[Rafikov, Roman; Brandt, Timothy D.] Inst Adv Study, Dept Astrophys, Princeton, NJ 08540 USA.
[Carson, Joseph C.] Coll Charleston, Dept Phys & Astron, 58 Coming St, Charleston, SC 29424 USA.
[Janson, Markus] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, SE-10691 Stockholm, Sweden.
[Kwon, Jungmi] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan.
[Oh, Daehyeon] Natl Meteorol Satellite Ctr, 64-18 Guam Gil, Chungbuk, South Korea.
[Takami, Michihiro; Tang, Ya-Wen] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan.
[Abe, Lyu] Univ Nice Sophia Antipolis, CNRS, Lab Lagrange, Observ Cotedazur,UMR 7293, 28 Ave Valrose, F-061082 Nice 2, France.
[Brandner, Wolfgang; Feldt, Markus; Henning, Thomas] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Egner, Sebastian] European Southern Observ, Karl Schwarzschildstr 2, D-85748 Garching, Germany.
[Goto, Miwa] Univ Sternwarte Munchen, Ludwig Maximilians Univ, Scheinerstr 1, D-81679 Munich, Germany.
[Grady, Carol A.; Mcelwain, Michael W.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 20771 USA.
[Grady, Carol A.] Eureka Sci, 2452 Delmer,Suite 100, Oakland, CA 96002 USA.
[Grady, Carol A.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.
[Hodapp, Klaus W.] Univ Hawaii, Inst Astron, 640 N Aohoku Pl, Hilo, HI 96720 USA.
[Knapp, Gillian R.; Moro-Martin, Amaya; Turner, Edwin L.] Princeton Univ, Dept Astrophys Sci, Peyton Hall,Ivy Lane, Princeton, NJ 08544 USA.
[Matsuo, Taro] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, 1-1 Machikaneyamacho, Toyonaka, Osaka 5600043, Japan.
[Miyama, Shoken] Hiroshima Univ, 1-3-2 Kagamiyama, Higashihiroshima, Hiroshima 7398511, Japan.
[Moro-Martin, Amaya] INTA, CAB CSIC, Dept Astrophys, E-28850 Madrid, Spain.
[Serabyn, Eugene] CALTECH, Jet Prop Lab, M-S 171-113 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Thalmann, Christian] Swiss Fed Inst Technol, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.
[Turner, Edwin L.] Univ Tokyo, Kavli Inst Phys & Math Univ, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778568, Japan.
[Watanabe, Makoto] Hokkaido Univ, Dept Cosmosci, Kita Ku, Sapporo, Hokkaido 0600810, Japan.
[Wisniewski, John] Univ Oklahoma, HL Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA.
[Yamada, Toru] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan.
RP Yang, Y (reprint author), SOKENDAI Graudate Univ Adv Studies, Dept Astron Sci, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.; Yang, Y (reprint author), NINS, NAOJ, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
EM yi.yang@nao.ac.jp
RI MIYAMA, Shoken/A-3598-2015
FU U.S. National Science Foundation [1009203]; [15H02063]
FX We would like to thank an anonymous reviewer, whose comments greatly
helped us improve this paper. This study was based on data collected by
Subaru Telescope, which is operated by the National Astronomical
Observatory of Japan (NAOJ), National Institutes of Natural Sciences
(NINS). We thank the Subaru Telescope staff for their support during the
observations. We would like to acknowledge the use of the SIMBAD
database operated by the Strasbourg Astronomical Data Center (CDS),
Strasbourg, France. This paper makes use of the following ALMA data:
ADS/JAO. ALMA#2011.0.00059.S. ALMA is a partnership of ESO (representing
its member states), NSF (USA) and NINS (Japan), together with NRC
(Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in
cooperation with the Republic of Chile. The Joint ALMA Observatory is
operated by ESO, AUI/NRAO and NAOJ. IRAF is distributed by the National
Optical Astronomy Observatory, which is operated by the Association of
Universities for Research in Astronomy (AURA) under a cooperative
agreement with the National Science Foundation. We also thank Dr.
Ruobing Dong for useful discussions with him. M.T. is supported by a
Grant-in-Aid for Scientific Research (No.15H02063). J.C. is supported by
the U.S. National Science Foundation under Award No. 1009203. The
authors wish to recognize and acknowledge the very significant cultural
role and reverence that the summit of Maunakea has always had within the
indigenous Hawaiian community. We are most fortunate to have the
opportunity to conduct observations from this mountain.
NR 44
TC 0
Z9 0
U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD JAN
PY 2017
VL 153
IS 1
AR 7
DI 10.3847/1538-3881/153/1/7
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EH2ER
UT WOS:000391580800002
ER
PT J
AU Abeysekara, AU
Archambault, S
Archer, A
Benbow, W
Bird, R
Buchovecky, M
Buckley, JH
Bugaev, V
Cardenzana, JV
Cerruti, M
Chen, X
Ciupik, L
Connolly, MP
Cui, W
Eisch, JD
Falcone, A
Feng, Q
Finley, JP
Fleischhack, H
Flinders, A
Fortson, L
Furniss, A
Griffin, S
Hakansson, MH
Hanna, D
Hervet, O
Holder, J
Humensky, TB
Kaaret, P
Kar, P
Kertzman, M
Kieda, D
Krause, M
Kumar, S
Lang, MJ
Maier, G
McArthur, S
McCann, A
Meagher, K
Moriarty, P
Mukherjee, R
Nieto, D
Ong, SOA
Otte, AN
Park, N
Pelassa, V
Pohl, M
Popkow, A
Pueschel, E
Ragan, K
Reynolds, PT
Richards, GT
Roache, E
Sadeh, I
Santander, M
Sembroski, GH
Shahinyan, K
Staszak, D
Telezhinsky, I
Tucci, JV
Tyler, J
Wakely, SP
Weinstein, A
Wilhelm, A
Williams, DA
Ahnen, ML
Ansoldi, S
Antonelli, LA
Antoranz, P
Arcaro, C
Babic, A
Banerjee, B
Bangale, P
de Almeida, UB
Barrio, JA
Gonzalez, JB
Bednarek, W
Bernardini, E
Berti, A
Biasuzzi, B
Biland, A
Blanch, O
Bonnefoy, S
Bonnoli, G
Borracci, F
Bretz, T
Carosi, R
Carosi, A
Chatterjee, A
Colin, P
Colombo, E
Contreras, JL
Cortina, J
Covino, S
Cumani, P
Da Vela, P
Dazzi, F
De Angelis, A
De Lotto, B
Wilhelmi, ED
Di Pierro, F
Doert, M
Dominguez, A
Prester, DD
Dorner, D
Doro, M
Einecke, S
Glawion, DE
Elsaesser, D
Engelkemeier, M
Ramazani, VF
Fernandez-Barral, A
Fidalgo, D
Fonseca, MV
Font, L
Fruck, C
Galindo, D
Lopez, RJG
Garczarczyk, M
Gaug, M
Giammaria, P
Godinovic, N
Gora, D
Guberman, D
Hadasch, D
Hahn, A
Hassan, T
Hayashida, M
Herrera, J
Hose, J
Hrupec, D
Hughes, G
Idec, W
Kodani, K
Konno, Y
Kubo, H
Kushida, J
Lelas, D
Lindfors, E
Lombardi, S
Longo, F
Lopez, M
Lopez-Coto, R
Majumdar, P
Makariev, M
Mallot, K
Maneva, G
Manganaro, M
Mannheim, K
Maraschi, L
Marcote, B
Mariotti, M
Martinez, M
Mazin, D
Menzel, U
Mirzoyan, R
Moralejo, A
Moretti, E
Nakajima, D
Neustroev, V
Niedzwiecki, A
Rosillo, MN
Nilsson, K
Nishijima, K
Noda, K
Nogues, L
Nothe, M
Paiano, S
Palacio, J
Palatiello, M
Paneque, D
Paoletti, R
Paredes, JM
Paredes-Fortuny, X
Pedaletti, G
Peresano, M
Perri, L
Persic, M
Poutanen, J
Moroni, PGP
Prandini, E
Puljak, I
Garcia, JR
Reichardt, I
Rhode, W
Ribo, M
Rico, J
Saito, T
Satalecka, K
Schroeder, S
Schweizer, T
Shore, SN
Sillanpaa, A
Sitarek, J
Snidaric, I
Sobczynska, D
Stamerra, A
Strzys, M
Suric, T
Takalo, L
Tavecchio, F
Temnikov, P
Terzic, T
Tescaro, D
Teshima, M
Torres, DF
Torres-Alba, N
Toyama, T
Treves, A
Vanzo, G
Acosta, MV
Vovk, I
Ward, JE
Will, M
Wu, MH
Zanin, R
Hovatta, T
Perez, ID
Smith, PS
Racero, E
Balokovic, M
AF Abeysekara, A. U.
Archambault, S.
Archer, A.
Benbow, W.
Bird, R.
Buchovecky, M.
Buckley, J. H.
Bugaev, V.
Cardenzana, J. V.
Cerruti, M.
Chen, X.
Ciupik, L.
Connolly, M. P.
Cui, W.
Eisch, J. D.
Falcone, A.
Feng, Q.
Finley, J. P.
Fleischhack, H.
Flinders, A.
Fortson, L.
Furniss, A.
Griffin, S.
Hakansson, M. Hn.
Hanna, D.
Hervet, O.
Holder, J.
Humensky, T. B.
Kaaret, P.
Kar, P.
Kertzman, M.
Kieda, D.
Krause, M.
Kumar, S.
Lang, M. J.
Maier, G.
McArthur, S.
McCann, A.
Meagher, K.
Moriarty, P.
Mukherjee, R.
Nieto, D.
Ong, S. Or. A.
Otte, A. N.
Park, N.
Pelassa, V.
Pohl, M.
Popkow, A.
Pueschel, E.
Ragan, K.
Reynolds, P. T.
Richards, G. T.
Roache, E.
Sadeh, I.
Santander, M.
Sembroski, G. H.
Shahinyan, K.
Staszak, D.
Telezhinsky, I.
Tucci, J. V.
Tyler, J.
Wakely, S. P.
Weinstein, A.
Wilhelm, A.
Williams, D. A.
Ahnen, M. L.
Ansoldi, S.
Antonelli, L. A.
Antoranz, P.
Arcaro, C.
Babic, A.
Banerjee, B.
Bangale, P.
de Almeida, U. Barres
Barrio, J. A.
Becerra Gonzalez, J.
Bednarek, W.
Bernardini, E.
Berti, A.
Biasuzzi, B.
Biland, A.
Blanch, O.
Bonnefoy, S.
Bonnoli, G.
Borracci, F.
Bretz, T.
Carosi, R.
Carosi, A.
Chatterjee, A.
Colin, P.
Colombo, E.
Contreras, J. L.
Cortina, J.
Covino, S.
Cumani, P.
Da Vela, P.
Dazzi, F.
De Angelis, A.
De Lotto, B.
de Ona Wilhelmi, E.
Di Pierro, F.
Doert, M.
Dominguez, A.
Prester, D. Dominis
Dorner, D.
Doro, M.
Einecke, S.
Glawion, D. Eisenacher
Elsaesser, D.
Engelkemeier, M.
Ramazani, V. Fallah
Fernandez-Barral, A.
Fidalgo, D.
Fonseca, M. V.
Font, L.
Fruck, C.
Galindo, D.
Garcia Lopez, R. J.
Garczarczyk, M.
Gaug, M.
Giammaria, P.
Godinovic, N.
Gora, D.
Guberman, D.
Hadasch, D.
Hahn, A.
Hassan, T.
Hayashida, M.
Herrera, J.
Hose, J.
Hrupec, D.
Hughes, G.
Idec, W.
Kodani, K.
Konno, Y.
Kubo, H.
Kushida, J.
Lelas, D.
Lindfors, E.
Lombardi, S.
Longo, F.
Lopez, M.
Lopez-Coto, R.
Majumdar, P.
Makariev, M.
Mallot, K.
Maneva, G.
Manganaro, M.
Mannheim, K.
Maraschi, L.
Marcote, B.
Mariotti, M.
Martinez, M.
Mazin, D.
Menzel, U.
Mirzoyan, R.
Moralejo, A.
Moretti, E.
Nakajima, D.
Neustroev, V.
Niedzwiecki, A.
Nievas Rosillo, M.
Nilsson, K.
Nishijima, K.
Noda, K.
Nogues, L.
Noethe, M.
Paiano, S.
Palacio, J.
Palatiello, M.
Paneque, D.
Paoletti, R.
Paredes, J. M.
Paredes-Fortuny, X.
Pedaletti, G.
Peresano, M.
Perri, L.
Persic, M.
Poutanen, J.
Moroni, P. G. Prada
Prandini, E.
Puljak, I.
Garcia, J. R.
Reichardt, I.
Rhode, W.
Ribo, M.
Rico, J.
Saito, T.
Satalecka, K.
Schroeder, S.
Schweizer, T.
Shore, S. N.
Sillanpaa, A.
Sitarek, J.
Snidaric, I.
Sobczynska, D.
Stamerra, A.
Strzys, M.
Suric, T.
Takalo, L.
Tavecchio, F.
Temnikov, P.
Terzic, T.
Tescaro, D.
Teshima, M.
Torres, D. F.
Torres-Alba, N.
Toyama, T.
Treves, A.
Vanzo, G.
Vazquez Acosta, M.
Vovk, I.
Ward, J. E.
Will, M.
Wu, M. H.
Zanin, R.
Hovatta, T.
de la Calle Perez, I.
Smith, P. S.
Racero, E.
Balokovic, M.
CA VERITAS Collaboration
MAGIC Collaboration
TI A SEARCH FOR SPECTRAL HYSTERESIS AND ENERGY-DEPENDENT TIME LAGS FROM
X-RAY AND TeV GAMMA-RAY OBSERVATIONS OF Mrk 421
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE BL Lacertae objects: individual (Markarian 421); galaxies: active; gamma
rays: general; radiation mechanisms: non-thermal
ID BL-LACERTAE OBJECTS; ACTIVE GALACTIC NUCLEI; XMM-NEWTON; MULTIWAVELENGTH
OBSERVATIONS; CORRELATED VARIABILITY; LAC OBJECTS; BLAZARS;
MARKARIAN-421; TELESCOPE; EMISSION
AB Blazars are variable emitters across all wavelengths over a wide range of timescales, from months down to minutes. It is therefore essential to observe blazars simultaneously at different wavelengths, especially in the X-ray and gamma-ray bands, where the broadband spectral energy distributions usually peak. In this work, we report on three " target-of-opportunity" observations of Mrk 421, one of the brightest TeV blazars, triggered by a strong flaring event at TeV energies in 2014. These observations feature long, continuous, and simultaneous exposures with XMM-Newton (covering the X-ray and optical/ultraviolet bands) and VERITAS (covering the TeV gamma-ray band), along with contemporaneous observations from other gamma-ray facilities (MAGIC and Fermi-Large Area Telescope) and a number of radio and optical facilities. Although neither rapid flares nor significant X-ray/TeV correlation are detected, these observations reveal subtle changes in the X-ray spectrum of the source over the course of a few days. We search the simultaneous X-ray and TeV data for spectral hysteresis patterns and time delays, which could provide insight into the emission mechanisms and the source properties (e. g., the radius of the emitting region, the strength of the magnetic field, and related timescales). The observed broadband spectra are consistent with a one-zone synchrotron self-Compton model. We find that the power spectral density distribution at greater than or similar to 4 x 10(-4) Hz from the X-ray data can be described by a power-law model with an index value between 1.2 and 1.8, and do not find evidence for a steepening of the power spectral index (often associated with a characteristic length scale) compared to the previously reported values at lower frequencies.
C1 [Abeysekara, A. U.; Flinders, A.; Kar, P.; Kieda, D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Archambault, S.; Feng, Q.; Griffin, S.; Hanna, D.; McCann, A.; Ragan, K.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Archer, A.; Buckley, J. H.; Bugaev, V.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Benbow, W.; Cerruti, M.; Pelassa, V.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Bird, R.; Buchovecky, M.; Ong, S. Or. A.; Popkow, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Cardenzana, J. V.; Eisch, J. D.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Chen, X.; Hakansson, M. Hn.; Pohl, M.; Telezhinsky, I.; Wilhelm, A.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Chen, X.; Fleischhack, H.; Krause, M.; Maier, G.; Pohl, M.; Sadeh, I.; Telezhinsky, I.; Wilhelm, A.] DESY, Platanenallee 6, D-15738 Zeuthen, Germany.
[Ciupik, L.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Connolly, M. P.; Lang, M. J.; Moriarty, P.] Natl Univ Ireland Galway, Sch Phys, Univ Rd, Galway, Ireland.
[Cui, W.; Finley, J. P.; McArthur, S.; Sembroski, G. H.; Tucci, J. V.] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA.
[Cui, W.] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China.
[Cui, W.] Tsinghua Univ, Ctr Astrophys, Beijing 100084, Peoples R China.
[Falcone, A.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
[Fortson, L.; Shahinyan, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Furniss, A.] Calif State Univ East Bay, Dept Phys, Hayward, CA 94542 USA.
[Hervet, O.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Hervet, O.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Holder, J.; Kumar, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Holder, J.; Kumar, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Humensky, T. B.; Nieto, D.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Kaaret, P.] Univ Iowa, Dept Phys & Astron, Van Allen Hall, Iowa City, IA 52242 USA.
[Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, 837 State St NW, Atlanta, GA 30332 USA.
[Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, 837 State St NW, Atlanta, GA 30332 USA.
[Mukherjee, R.; Santander, M.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Park, N.; Staszak, D.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Pueschel, E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Reynolds, P. T.] Cork Inst Technol, Dept Phys Sci, Cork, Ireland.
[Ahnen, M. L.; Biland, A.; Hughes, G.] ETH, CH-8093 Zurich, Switzerland.
[Ansoldi, S.; Berti, A.; Biasuzzi, B.; De Lotto, B.; Longo, F.; Palatiello, M.; Peresano, M.; Persic, M.; Treves, A.] Univ Udine, I-33100 Udine, Italy.
[Ansoldi, S.; Berti, A.; Biasuzzi, B.; De Lotto, B.; Longo, F.; Palatiello, M.; Peresano, M.; Persic, M.; Treves, A.] INFN Trieste, I-33100 Udine, Italy.
[Antonelli, L. A.; Carosi, A.; Covino, S.; Di Pierro, F.; Giammaria, P.; Lombardi, S.; Maraschi, L.; Perri, L.; Stamerra, A.; Tavecchio, F.] INAF Natl Inst Astrophys, I-00136 Rome, Italy.
[Flinders, A.; Antoranz, P.; Bonnoli, G.; Carosi, R.; Da Vela, P.; Paoletti, R.] Univ Siena, I-53100 Siena, Italy.
[Antoranz, P.; Bonnoli, G.; Carosi, R.; Da Vela, P.; Paoletti, R.] INFN Pisa, I-53100 Siena, Italy.
[Arcaro, C.; De Angelis, A.; Doro, M.; Hahn, A.; Mariotti, M.; Paiano, S.; Prandini, E.; Reichardt, I.; Tescaro, D.] Univ Padua, I-35131 Padua, Italy.
[Arcaro, C.; De Angelis, A.; Doro, M.; Mariotti, M.; Paiano, S.; Prandini, E.; Reichardt, I.] Ist Nazl Fis Nucl, I-35131 Padua, Italy.
[Babic, A.; Prester, D. Dominis; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Suric, T.; Terzic, T.] Univ Rijeka, Rudjer Boskov Inst, Croatian MAGIC Consortium, Rijeka, Croatia.
[Babic, A.; Prester, D. Dominis; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Suric, T.; Terzic, T.] Univ Split, Split, Croatia.
[Babic, A.; Prester, D. Dominis; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Suric, T.; Terzic, T.] Univ Zagreb, Zagreb, Croatia.
[Banerjee, B.; Chatterjee, A.; Majumdar, P.] Saha Inst Nucl Phys, 1-AF Bidhannagar,Sect 1, Kolkata 700064, India.
[Bangale, P.; de Almeida, U. Barres; Borracci, F.; Colin, P.; Dazzi, F.; Fruck, C.; Hahn, A.; Hose, J.; Mazin, D.; Menzel, U.; Mirzoyan, R.; Moretti, E.; Noda, K.; Paneque, D.; Garcia, J. R.; Schweizer, T.; Strzys, M.; Teshima, M.; Toyama, T.; Vovk, I.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Barrio, J. A.; Bonnefoy, S.; Contreras, J. L.; Dominguez, A.; Fidalgo, D.; Fonseca, M. V.; Lopez, M.; Nievas Rosillo, M.] Univ Complutense, E-28040 Madrid, Spain.
[Becerra Gonzalez, J.; Colombo, E.; Garcia Lopez, R. J.; Herrera, J.; Manganaro, M.; Vanzo, G.; Vazquez Acosta, M.; Will, M.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain.
[Becerra Gonzalez, J.; Colombo, E.; Garcia Lopez, R. J.; Herrera, J.; Vanzo, G.; Vazquez Acosta, M.; Will, M.] Univ La Laguna, Dept Astrofis, E-38206 San Cristobal la Laguna, Tenerife, Spain.
[Bednarek, W.; Idec, W.; Niedzwiecki, A.; Sitarek, J.; Sobczynska, D.] Univ Lodz, PL-90236 Lodz, Poland.
[Bernardini, E.; Garczarczyk, M.; Gora, D.; Mallot, K.; Pedaletti, G.; Satalecka, K.] DESY, D-15738 Zeuthen, Germany.
[Bernardini, E.] Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany.
[Blanch, O.; Cortina, J.; Cumani, P.; Fernandez-Barral, A.; Guberman, D.; Hassan, T.; Lopez-Coto, R.; Martinez, M.; Moralejo, A.; Nogues, L.; Palacio, J.; Rico, J.; Ward, J. E.] Barcelona Inst Sci & Technol, Inst Fis Altes Energies, Campus UAB, E-08193 Bellaterra, Barcelona, Spain.
[Bretz, T.; Dorner, D.; Glawion, D. Eisenacher; Mannheim, K.] Univ Wurzburg, D-97074 Wurzburg, Germany.
[de Ona Wilhelmi, E.; Torres, D. F.; Wu, M. H.] CSIC IEEC, Inst Space Sci, E-08193 Barcelona, Spain.
[Weinstein, A.; Doert, M.; Elsaesser, D.; Engelkemeier, M.; Noethe, M.; Rhode, W.; Schroeder, S.] Tech Univ Dortmund, D-44221 Dortmund, Germany.
[Ramazani, V. Fallah; Lindfors, E.; Neustroev, V.; Nilsson, K.; Poutanen, J.; Sillanpaa, A.; Takalo, L.] Univ Turku, Tuorla Observ, Finnish MAGIC Consortium, Turku, Finland.
[Ramazani, V. Fallah; Lindfors, E.; Neustroev, V.; Nilsson, K.; Poutanen, J.; Sillanpaa, A.; Takalo, L.] Univ Oulu, Astron Div, Oulu, Finland.
[Font, L.; Gaug, M.] Univ Autonoma Barcelona, Dept Fis, Unitat Fis Radiac, E-08193 Barcelona, Spain.
[Font, L.; Gaug, M.] Univ Autonoma Barcelona, CERES IEEC, E-08193 Barcelona, Spain.
[Galindo, D.; Marcote, B.; Paredes, J. M.; Paredes-Fortuny, X.; Ribo, M.; Torres-Alba, N.; Zanin, R.] Univ Barcelona, ICC, IEEC UB, E-08028 Barcelona, Spain.
[Hadasch, D.; Hayashida, M.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Nakajima, D.; Nishijima, K.; Saito, T.] Univ Tokyo, Japanese MAGIC Consortium, ICRR, Tokyo, Japan.
[Hadasch, D.; Hayashida, M.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Nakajima, D.; Nishijima, K.; Saito, T.] Kyoto Univ, Dept Phys, Kyoto, Japan.
[Hadasch, D.; Hayashida, M.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Nakajima, D.; Nishijima, K.; Saito, T.] Kyoto Univ, Hakubi Ctr, Kyoto, Japan.
[Hadasch, D.; Hayashida, M.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Nakajima, D.; Nishijima, K.; Saito, T.] Tokai Univ, Tokai, Ibaraki, Japan.
[Hadasch, D.; Hayashida, M.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Nakajima, D.; Nishijima, K.; Saito, T.] Univ Tokushima, Tokushima, Japan.
[Makariev, M.; Maneva, G.; Temnikov, P.] Inst Nucl Energy Res, BG-1784 Sofia, Bulgaria.
[Moroni, P. G. Prada; Shore, S. N.] Univ Pisa, I-56126 Pisa, Italy.
[Moroni, P. G. Prada; Shore, S. N.] INFN Pisa, I-56126 Pisa, Italy.
[Torres, D. F.] ICREA, E-08193 Barcelona, Spain.
[Hovatta, T.] Aalto Univ, Metsahovi Radio Observ, Metsahovintie 114, Kylmala 02540, Finland.
[Hovatta, T.] Aalto Univ, Dept Radio Sci & Engn, POB 13000, FI-00076 Aalto, Finland.
[de la Calle Perez, I.; Racero, E.] European Space Agcy, European Space Astron Ctr INSA ESAC, Satellite Tracking Stn, POB Apdo 50727, E-28080 Madrid, Spain.
[Smith, P. S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Balokovic, M.] CALTECH, Cahill Ctr Astron & Astrophys, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
[Ansoldi, S.; Dominguez, A.] Kyoto Univ, Dept Phys, Kyoto, Japan.
[de Almeida, U. Barres] Ctr Brasileiro Pesquisas Fis CBPF MCTI, R Dr Xavier Sigaud,150 Urca, BR-22290180 Rio De Janeiro, RJ, Brazil.
[Becerra Gonzalez, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Becerra Gonzalez, J.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Becerra Gonzalez, J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Berti, A.; Longo, F.] Univ Trieste, I-34127 Trieste, Italy.
[Bretz, T.] Ecole Polytech Fed Lausanne, Lausanne, Switzerland.
[Lopez-Coto, R.] Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany.
[Mazin, D.; Teshima, M.] Japanese MAGIC Consortium, Kyoto, Japan.
[Nilsson, K.] ESO FINCA, Finnish Ctr Astron, Turku, Finland.
[Persic, M.] Univ Bologna, INAF Trieste, Bologna, Italy.
[Persic, M.] Univ Bologna, Dept Phys & Astron, Bologna, Italy.
RP Abeysekara, AU (reprint author), Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
RI Manganaro, Marina/B-7657-2011; Puljak, Ivica/D-8917-2017;
OI Manganaro, Marina/0000-0003-1530-3031; Becerra Gonzalez,
Josefa/0000-0002-6729-9022; Bird, Ralph/0000-0002-4596-8563; Doro,
Michele/0000-0001-9104-3214; Prandini, Elisa/0000-0003-4502-9053
FU U.S. Department of Energy Office of Science; U.S. National Science
Foundation; Smithsonian Institution; NSERC in Canada; German BMBF;
German MPG; Italian INFN; Italian INAF; Swiss National Fund SNF; ERDF
under the Spanish MINECO [FPA2015-69818-P, FPA2012-36668,
FPA2015-68278-P, FPA2015-69210-C6-2-R, FPA2015-69210-C6-4-R,
FPA2015-69210-C6-6-R, AYA2013-47447-C3-1-P, AYA2015-71042-P,
ESP2015-71662-C2-2-P, CSD2009-00064]; Japanese JSPS; Japanese MEXT;
Spanish Centro de Excelencia "Severo Ochoa" [SEV-2012-0234,
SEV-2015-0548]; Unidad de Excelencia "Maria de Maeztu" [MDM-2014-0369];
Academy of Finland [268740]; Croatian Science Foundation (HrZZ) Project
[09/176]; University of Rijeka Project [13.12.1.3.02]; DFG Collaborative
Research Centers [SFB823/C4, SFB876/C3]; Polish MNiSzW
[745/N-HESS-MAGIC/2010/0]; Fermi Guest Investigator grants - NASA
[NNX12AO93G, NNX15AU81G]; NASA [NNX08AW31G, NNX11A043G]; NSF
[AST-0808050, AST-1109911]; International Fulbright Science and
Technology Award; NASA Headquarters under the NASA Earth and Space
Science Fellowship Program [NNX14AQ07H]
FX VERITAS is supported by grants from the U.S. Department of Energy Office
of Science, the U.S. National Science Foundation and the Smithsonian
Institution, and by NSERC in Canada. We acknowledge the excellent work
of the technical support staff at the Fred Lawrence Whipple Observatory
and at the collaborating institutions in the construction and operation
of the instrument.; The MAGIC collaboration would like to thank the
Instituto de Astrofisica de Canarias for the excellent working
conditions at the Observatorio del Roque de los Muchachos in La Palma.
The financial support of the German BMBF and MPG, the Italian INFN and
INAF, the Swiss National Fund SNF, the he ERDF under the Spanish MINECO
(FPA2015-69818-P, FPA2012-36668, FPA2015-68278-P, FPA2015-69210-C6-2-R,
FPA2015-69210-C6-4-R, FPA2015-69210-C6-6-R, AYA2013-47447-C3-1-P,
AYA2015-71042-P, ESP2015-71662-C2-2-P, CSD2009-00064), and the Japanese
JSPS and MEXT is gratefully acknowledged. This work was also supported
by the Spanish Centro de Excelencia "Severo Ochoa" SEV-2012-0234 and
SEV-2015-0548, and Unidad de Excelencia "Maria de Maeztu" MDM-2014-0369,
by grant 268740 of the Academy of Finland, by the Croatian Science
Foundation (HrZZ) Project 09/176 and the University of Rijeka Project
13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and
SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0.; This
work used data from the Fermi-LAT archive and from the Steward
Observatory spectropolarimetric monitoring project, which is supported
by Fermi Guest Investigator grants NNX12AO93G and NNX15AU81G funded by
NASA.; The OVRO 40-m monitoring program is supported in part by NASA
grants NNX08AW31G and NNX11A043G, and NSF grants AST-0808050 and
AST-1109911.; M. B. acknowledges support from the International
Fulbright Science and Technology Award, and NASA Headquarters under the
NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H.
NR 72
TC 0
Z9 0
U1 8
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 1
PY 2017
VL 834
IS 1
AR 2
DI 10.3847/1538-4357/834/1/2
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EH2BT
UT WOS:000391573000002
ER
PT J
AU Karpen, JT
DeVore, CR
Antiochos, SK
Pariat, E
AF Karpen, J. T.
DeVore, C. R.
Antiochos, S. K.
Pariat, E.
TI RECONNECTION-DRIVEN CORONAL-HOLE JETS WITH GRAVITY AND SOLAR WIND
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetic reconnection; magnetohydrodynamics (MHD); solar wind; stars:
jets; Sun: activity; Sun: corona
ID X-RAY JETS; EXTREME-ULTRAVIOLET JETS; POLAR JETS; MAGNETIC RECONNECTION;
FILAMENT ERUPTIONS; CHROMOSPHERIC JET; EXPLOSIVE EVENTS; FLUX EMERGENCE;
FINE-STRUCTURE; WHITE-LIGHT
AB Coronal-hole jets occur ubiquitously in the Sun's coronal holes, at EUV and X-ray bright points associated with intrusions of minority magnetic polarity. The embedded-bipole model for these jets posits that they are driven by explosive, fast reconnection between the stressed closed field of the embedded bipole and the open field of the surrounding coronal hole. Previous numerical studies in Cartesian geometry, assuming uniform ambient magnetic field and plasma while neglecting gravity and solar wind, demonstrated that the model is robust and can produce jet-like events in simple configurations. We have extended these investigations by including spherical geometry, gravity, and solar wind in a nonuniform, coronal hole-like ambient atmosphere. Our simulations confirm that the jet is initiated by the onset of a kink-like instability of the internal closed field, which induces a burst of reconnection between the closed and external open field, launching a helical jet. Our new results demonstrate that the jet propagation is sustained through the outer corona, in the form of a traveling nonlinear Alfven wave front trailed by slower-moving plasma density enhancements that are compressed and accelerated by the wave. This finding agrees well with observations of white-light coronal-hole jets, and can explain microstreams and torsional Alfven waves detected in situ in the solar wind. We also use our numerical results to deduce scaling relationships between properties of the coronal source region and the characteristics of the resulting jet, which can be tested against observations.
C1 [Karpen, J. T.; DeVore, C. R.; Antiochos, S. K.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Pariat, E.] Univ Paris Diderot, UPMC Univ Paris 06, Sorbonne Univ, LESIA,Observ Paris,PSL Res Univ,CNRS,Sorbonne Par, 5 Pl Jules Janssen, F-92195 Meudon, France.
RP Karpen, JT (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
FU NASA
FX We thank Kevin Dalmasse and Peter Wyper for many helpful discussions of
the results developed in this paper. Our research was supported by NASA
Living With a Star grants to understand reconnection-driven solar jets
and their heliospheric consequences, and to prepare for the
investigation of the inner heliosphere by Solar Probe Plus. The
numerical simulations were supported by grants to C.R.D. of High-End
Computing resources at NASA's Center for Climate Simulation.
NR 65
TC 1
Z9 1
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 1
PY 2017
VL 834
IS 1
AR 62
DI 10.3847/1538-4357/834/1/62
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EH4MM
UT WOS:000391745300007
ER
PT J
AU Rho, J
Hewitt, JW
Bieging, J
Reach, WT
Andersen, M
Gusten, R
AF Rho, J.
Hewitt, J. W.
Bieging, J.
Reach, W. T.
Andersen, M.
Guesten, R.
TI DISCOVERY OF BROAD MOLECULAR LINES AND OF SHOCKED MOLECULAR HYDROGEN
FROM THE SUPERNOVA REMNANT G357.7+0.3: HHSMT, APEX, SPITZER, AND SOFIA
OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: ISM; ISM: individual objects (G357.7+0.3); ISM: supernova
remnants; radio lines: ISM
ID GAMMA-RAY EMISSION; LARGE-AREA TELESCOPE; MHZ MASER EMISSION; FERMI-LAT;
INTERSTELLAR SHOCKS; GALACTIC-CENTER; WATER EMISSION; X-RAY; CLOUDS; GAS
AB We report a discovery of shocked gas from the supernova remnant (SNR) G357.7+0.3. Our millimeter and submillimeter observations reveal broad molecular lines of CO(2-1), CO(3-2), CO(4-3), (CO)-C-13 (2-1), and (CO)-C-13 (3-2), HCO+, and HCN using the Heinrich Hertz Submillimeter Telescope, the Arizona 12 m Telescope, APEX, and the MOPRA Telescope. The widths of the broad lines are 15-30 km s(-1), and the detection of such broad lines is unambiguous, dynamic evidence showing that the SNR G357.7+0.3 is interacting with molecular clouds. The broad lines appear in extended regions (>4'.5 x 5'). We also present the detection of shocked H-2 emission in the mid-infrared but lacking ionic lines using Spitzer/IRS observations to map a few-arcminute area. The H2 excitation diagram shows a best fit with a two-temperature local thermal equilibrium model with the temperatures of similar to 200 and 660 K. We observed [C II] at 158 mu m and high-J CO(11-10) with the German Receiver for Astronomy at Terahertz Frequencies (GREAT) on the Stratospheric Observatory for Infrared Astronomy. The GREAT spectrum of [C II], a 3 sigma detection, shows a broad line profile with a width of 15.7 km(-1) that is similar to those of broad CO molecular lines. The line width of [C II] implies that ionic lines can come from a low-velocity C-shock. Comparison of H2 emission with shock models shows that a combination of two C-shock models is favored over a combination of C- and J-shocks or a single shock. We estimate the CO density, column density, and temperature using a RADEX model. The best-fit model with n(H-2) = 1.7 x 10(4) cm(-3), N(CO) = 5.6 x 10(16) cm(-2), and T = 75 K can reproduce the observed millimeter CO brightnesses.
C1 [Rho, J.] SETI Inst, 189 N Bernardo Ave, Mountain View, CA 94043 USA.
[Rho, J.] NASA, SOFIA Sci Ctr, Ames Res Ctr, MS211-1, Moffett Field, CA 94043 USA.
[Hewitt, J. W.] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA.
[Hewitt, J. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hewitt, J. W.] Univ North Florida, Dept Phys, Jacksonville, FL 32224 USA.
[Bieging, J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Reach, W. T.] NASA, Univ Space Res Assoc, SOFIA Sci Ctr, Ames Res Ctr, MS 232, Moffett Field, CA 94034 USA.
[Andersen, M.] Gemini Observ, Casilla 603, La Serena, Chile.
[Guesten, R.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
RP Rho, J (reprint author), SETI Inst, 189 N Bernardo Ave, Mountain View, CA 94043 USA.; Rho, J (reprint author), NASA, SOFIA Sci Ctr, Ames Res Ctr, MS211-1, Moffett Field, CA 94043 USA.
EM jrho@seti.org; john.w.hewitt@unf.edu; jbieging@as.arizona.edu;
wreach@sofia.usra.edu; manderse@gemini.edu; guesten@mpifr-bonn.mpg.de
OI Reach, William/0000-0001-8362-4094
FU National Science Foundation; NASA [NAS2-97001]; Deutsches SOFIA Institut
under DLR [50 OK 0901]
FX We thank Sebastien Bardeau, a staff scientist at IRAM for helping with
various issues of CLASS softwares, and Miguel Angel Requena Torres and
Friedrich Wyrowski for helping with SOFIA and APEX observations and data
processing, respectively. We thank the anonymous referee for helpful
comments. The Arizona Radio Observatory is part of the Steward
Observatory at the University of Arizona and receives partial support
from the National Science Foundation. Based (in part) on observations
made with the NASA/DLR Stratospheric Observatory for Infrared Astronomy.
SOFIA Science Mission Operations are conducted jointly by the
Universities Space Research Association, Inc., under NASA contract
NAS2-97001, and the Deutsches SOFIA Institut under DLR contract 50 OK
0901. APEX is a collaboration between the Max-Planck-Institut fur
Radioastronomie, the European Southern Observatory, and the Onsala Space
Observatory.
NR 70
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 1
PY 2017
VL 834
IS 1
AR 12
DI 10.3847/1538-4357/834/1/12
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EH2BT
UT WOS:000391573000012
ER
PT J
AU Majid, WA
Pearlman, AB
Dobreva, T
Horiuchi, S
Kocz, J
Lippuner, J
Prince, TA
AF Majid, Walid A.
Pearlman, Aaron B.
Dobreva, Tatyana
Horiuchi, Shinji
Kocz, Jonathon
Lippuner, Jonas
Prince, Thomas A.
TI POST-OUTBURST RADIO OBSERVATIONS OF THE HIGH MAGNETIC FIELD PULSAR PSR
J1119-6127
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE ISM: individual objects (G292.2-0.5); ISM: supernova remnants; pulsars:
individual (PSR J1119-6127); stars: magnetars; stars: neutron
ID SUPERNOVA REMNANT G292.2-0.5; YOUNG PULSAR; TELESCOPE; EMISSION; GLITCH;
DENSITY; CATALOG
AB We have carried out high-frequency radio observations of the high magnetic field pulsar PSR. J1119-6127 following its recent X-ray outburst. While initial observations showed no evidence of significant radio emission, subsequent observations detected pulsed emission across a large frequency band. In this Letter, we report on the initial disappearance of the pulsed emission and its prompt reactivation and dramatic evolution over several months of observation. The periodic pulse profile at S-band (2.3 GHz) after reactivation exhibits a multi-component emission structure, while the simultaneous X-band (8.4 GHz) profile shows a single emission peak. Single pulses were also detected at S-band near the main emission peaks. We present measurements of the spectral index across a wide frequency bandwidth, which captures the underlying changes in the radio emission profile of the neutron star. The high-frequency radio detection, unusual emission profile, and observed variability suggest similarities with magnetars, which may independently link the high-energy outbursts to magnetar-like behavior.
C1 [Majid, Walid A.; Pearlman, Aaron B.; Dobreva, Tatyana; Kocz, Jonathon; Prince, Thomas A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Majid, Walid A.; Pearlman, Aaron B.; Prince, Thomas A.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Horiuchi, Shinji] CSIRO Astron & Space Sci, Canberra Deep Space Commun Complex, POB 1035, Tuggeranong, ACT 2901, Australia.
[Lippuner, Jonas] CALTECH, Walter Burke Inst Theoret Phys, TAPIR, MC 350-17, Pasadena, CA 91125 USA.
RP Majid, WA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
OI Lippuner, Jonas/0000-0002-5936-3485
FU Department of Defense (DoD) through the National Defense Science and
Engineering Graduate Fellowship (NDSEG) Program; National Science
Foundation Graduate Research Fellowship [DGE-1144469]; Jet Propulsion
Laboratory Graduate Fellowship program; Jet Propulsion Laboratory,
California Institute of Technology under a Research and Technology
Development Grant; Jet Propulsion Laboratory, California Institute of
Technology under National Aeronautics and Space Administration
Government
FX We thank V. Kaspi and R. Archibald for alerting us to the initial
outburst and for providing an ephemeris for PSR J1119-6127. We also
thank V. Kaspi for a careful reading of the manuscript and detailed
comments. We acknowledge support from the DSN team for scheduling the
observations. A. B. Pearlman acknowledges support by the Department of
Defense (DoD) through the National Defense Science and Engineering
Graduate Fellowship (NDSEG) Program and by the National Science
Foundation Graduate Research Fellowship under Grant No. DGE-1144469. J.
Lippuner acknowledges support from the Jet Propulsion Laboratory
Graduate Fellowship program. A portion of this research was performed at
the Jet Propulsion Laboratory, California Institute of Technology under
a Research and Technology Development Grant and under a contract with
the National Aeronautics and Space Administration Government sponsorship
is acknowledged.
NR 29
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JAN 1
PY 2017
VL 834
IS 1
AR L2
DI 10.3847/2041-8213/834/1/L2
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EH6LX
UT WOS:000391885700001
ER
PT J
AU Kidd, C
Becker, A
Huffman, GJ
Muller, CL
Joe, P
Skofronick-Jackson, G
Kirschbaum, DB
AF Kidd, Chris
Becker, Andreas
Huffman, George J.
Muller, Catherine L.
Joe, Paul
Skofronick-Jackson, Gail
Kirschbaum, Dalia B.
TI SO, HOW MUCH OF THE EARTH'S SURFACE IS COVERED BY RAIN GAUGES?
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID PRECIPITATION MEASUREMENT; TROPICAL RAINFALL; NETWORK; SNOW; DATABASE;
CLIMATE; SPACE; WIND
AB The total area measured globally by all currently available rain gauges is surprisingly small, equivalent to less than half a football field or soccer pitch.
C1 [Kidd, Chris] Univ Maryland, College Pk, MD 20742 USA.
[Kidd, Chris; Huffman, George J.; Skofronick-Jackson, Gail; Kirschbaum, Dalia B.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Becker, Andreas] Deutsch Wetterdienst, Offenbach, Germany.
[Muller, Catherine L.] Univ Birmingham, Reading, Royal Meteorol Soc, Birmingham, W Midlands, England.
[Muller, Catherine L.] Univ Birmingham, Sch Geog Earth & Environm Sci, Birmingham, W Midlands, England.
[Joe, Paul] Environm & Climate Change Canada, Meteorol Res Div, Toronto, ON, Canada.
RP Kidd, C (reprint author), Univ Maryland, College Pk, MD 20742 USA.; Kidd, C (reprint author), NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM chris.kidd@nasa.gov
NR 47
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U1 2
U2 2
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
EI 1520-0477
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD JAN
PY 2017
VL 98
IS 1
BP 69
EP +
DI 10.1175/BAMS-D-14-00283.1
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EH6UW
UT WOS:000391910400012
ER
PT J
AU Pan, LL
Atlas, EL
Salawitch, RJ
Honomichl, SB
Bresch, JF
Randel, WJ
Apel, EC
Hornbrook, RS
Weinheimer, AJ
Anderson, DC
Andrews, SJ
Baidar, S
Beaton, SP
Campos, TL
Carpenter, LJ
Chen, D
Dix, B
Donets, V
Hall, SR
Hanisco, TF
Homeyer, CR
Huey, LG
Jensen, JB
Kaser, L
Kinnison, DE
Koenig, TK
Lamarque, JF
Liu, C
Luo, J
Luo, ZJ
Montzka, DD
Nicely, JM
Pierce, RB
Riemer, DD
Robinson, T
Romashkin, P
Saiz-Lopez, A
Schauffler, S
Shieh, O
Stell, MH
Ullmann, K
Vaughan, G
Volkamer, R
Wolfe, G
AF Pan, L. L.
Atlas, E. L.
Salawitch, R. J.
Honomichl, S. B.
Bresch, J. F.
Randel, W. J.
Apel, E. C.
Hornbrook, R. S.
Weinheimer, A. J.
Anderson, D. C.
Andrews, S. J.
Baidar, S.
Beaton, S. P.
Campos, T. L.
Carpenter, L. J.
Chen, D.
Dix, B.
Donets, V.
Hall, S. R.
Hanisco, T. F.
Homeyer, C. R.
Huey, L. G.
Jensen, J. B.
Kaser, L.
Kinnison, D. E.
Koenig, T. K.
Lamarque, J-F
Liu, C.
Luo, J.
Luo, Z. J.
Montzka, D. D.
Nicely, J. M.
Pierce, R. B.
Riemer, D. D.
Robinson, T.
Romashkin, P.
Saiz-Lopez, A.
Schauffler, S.
Shieh, O.
Stell, M. H.
Ullmann, K.
Vaughan, G.
Volkamer, R.
Wolfe, G.
TI THE CONVECTIVE TRANSPORT OF ACTIVE SPECIES IN THE TROPICS (CONTRAST)
EXPERIMENT
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID ZERO OZONE CONCENTRATIONS; WEST PACIFIC; IN-SITU; AIRCRAFT MEASUREMENTS;
TROPOSPHERIC OZONE; AEROSOL EXTINCTION; LOWER STRATOSPHERE; TROPOPAUSE
LAYER; PEM-TROPICS; AIR
C1 [Pan, L. L.; Honomichl, S. B.; Bresch, J. F.; Randel, W. J.; Apel, E. C.; Hornbrook, R. S.; Weinheimer, A. J.; Beaton, S. P.; Campos, T. L.; Hall, S. R.; Jensen, J. B.; Kaser, L.; Kinnison, D. E.; Lamarque, J-F; Luo, J.; Montzka, D. D.; Romashkin, P.; Schauffler, S.; Stell, M. H.; Ullmann, K.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
[Atlas, E. L.; Donets, V.; Riemer, D. D.] Univ Miami, Coral Gables, FL 33124 USA.
[Salawitch, R. J.; Anderson, D. C.; Nicely, J. M.] Univ Maryland, College Pk, MD 20742 USA.
[Andrews, S. J.; Carpenter, L. J.] Univ York, York, N Yorkshire, England.
[Baidar, S.; Dix, B.; Koenig, T. K.; Volkamer, R.] Univ Colorado, Boulder, CO 80309 USA.
[Chen, D.; Huey, L. G.] Georgia Inst Technol, Atlanta, GA 30332 USA.
[Hanisco, T. F.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Homeyer, C. R.] Univ Oklahoma, Norman, OK 73019 USA.
[Liu, C.] Texas A&M Univ Corpus Christi, Corpus Christi, TX USA.
[Luo, Z. J.] CUNY City Coll, New York, NY 10031 USA.
[Pierce, R. B.] NOAA Satellite & Informat Serv NESDIS, Ctr Satellite Applicat & Res STAR, Madison, WI USA.
[Robinson, T.; Shieh, O.] Univ Hawaii Manoa, Honolulu, HI 96822 USA.
[Saiz-Lopez, A.] CSIC, Inst Phys Chem Rocasolano, Madrid, Spain.
[Stell, M. H.] Metropolitan State Univ, Denver, CO USA.
[Vaughan, G.] Univ Manchester, Manchester, Lancs, England.
[Wolfe, G.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Wolfe, G.] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA.
[Luo, J.] Lanzhou Univ, Lanzhou, Peoples R China.
RP Pan, LL (reprint author), Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
EM liwen@ucar.edu
RI Saiz-Lopez, Alfonso/B-3759-2015; Wolfe, Glenn/D-5289-2011; Volkamer,
Rainer/B-8925-2016; Salawitch, Ross/B-4605-2009; Anderson,
Daniel/I-4398-2014; Manager, CSD Publications/B-2789-2015;
OI Saiz-Lopez, Alfonso/0000-0002-0060-1581; Volkamer,
Rainer/0000-0002-0899-1369; Salawitch, Ross/0000-0001-8597-5832;
Anderson, Daniel/0000-0002-9826-9811; Nicely, Julie/0000-0003-4828-0032
NR 64
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U1 5
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PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
EI 1520-0477
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD JAN
PY 2017
VL 98
IS 1
BP 106
EP +
DI 10.1175/BAMS-D-14-00272.1
PG 25
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EH6UW
UT WOS:000391910400015
ER
PT J
AU Jensen, EJ
Pfister, L
Jordan, DE
Bui, TV
Ueyama, R
Singh, HB
Thornberry, TD
Rollins, AW
Gao, RS
Fahey, DW
Rosenlof, KH
Elkins, JW
Diskin, GS
DiGangi, JP
Lawson, RP
Woods, S
Atlas, EL
Rodriguez, MAN
Wofsy, SC
Pittman, J
Bardeen, CG
Toon, OB
Kindel, BC
Newman, PA
McGill, MJ
Hlavka, DL
Lait, LR
Schoeberl, MR
Bergman, JW
Selkirk, HB
Alexander, MJ
Kim, JE
Lim, BH
Stutz, J
Pfeilsticker, K
AF Jensen, Eric J.
Pfister, Leonhard
Jordan, David E.
Bui, Thaopaul V.
Ueyama, Rei
Singh, Hanwant B.
Thornberry, Troy D.
Rollins, Andrew W.
Gao, Ru-Shan
Fahey, David W.
Rosenlof, Karen H.
Elkins, James W.
Diskin, Glenn S.
DiGangi, Joshua P.
Lawson, R. Paul
Woods, Sarah
Atlas, Elliot L.
Rodriguez, Maria A. Navarro
Wofsy, Steven C.
Pittman, Jasna
Bardeen, Charles G.
Toon, Owen B.
Kindel, Bruce C.
Newman, Paul A.
McGill, Matthew J.
Hlavka, Dennis L.
Lait, Leslie R.
Schoeberl, Mark R.
Bergman, John W.
Selkirk, Henry B.
Alexander, M. Joan
Kim, Ji-Eun
Lim, Boon H.
Stutz, Jochen
Pfeilsticker, Klaus
TI THE NASA AIRBORNE TROPICAL TROPOPAUSE EXPERIMENT High-Altitude Aircraft
Measurements in the Tropical Western Pacific
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID LOWER-STRATOSPHERE; WATER-VAPOR; MICROPHYSICAL PROPERTIES;
UPPER-TROPOSPHERE; CIRRUS CLOUDS; DEHYDRATION; LAYER; WAVE
AB We describe the Global Hawk flights and the measurements made during the NASA Airborne Tropical Tropopause Experiment (ATTREX) 2014 western Pacific campaign based in Guam.
C1 [Jensen, Eric J.; Pfister, Leonhard; Jordan, David E.; Bui, Thaopaul V.; Ueyama, Rei; Singh, Hanwant B.] NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
[Thornberry, Troy D.; Rollins, Andrew W.; Gao, Ru-Shan; Fahey, David W.; Rosenlof, Karen H.; Elkins, James W.] NOAA Earth Syst Res Lab, Boulder, CO USA.
[Thornberry, Troy D.; Rollins, Andrew W.] Cooperat Inst Res Environm Sci, Boulder, CO USA.
[Diskin, Glenn S.; DiGangi, Joshua P.] NASA Langley Res Ctr, Hampton, VA USA.
[Lawson, R. Paul; Woods, Sarah] SPEC Inc, Boulder, CO USA.
[Atlas, Elliot L.; Rodriguez, Maria A. Navarro] Univ Miami, Miami, FL USA.
[Wofsy, Steven C.; Pittman, Jasna] Harvard Univ, Cambridge, MA 02138 USA.
[Bardeen, Charles G.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
[Toon, Owen B.; Kindel, Bruce C.] Univ Colorado, Boulder, CO 80309 USA.
[Newman, Paul A.; McGill, Matthew J.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Hlavka, Dennis L.] Sci Syst & Applicat Inc, Greenbelt, MD USA.
[Lait, Leslie R.] Morgan State Univ, Baltimore, MD 21239 USA.
[Schoeberl, Mark R.] Sci & Technol Corp, Columbia, MD USA.
[Bergman, John W.] Bay Area Environm Res Inst, Sonoma, CA USA.
[Selkirk, Henry B.] Univ Space Res Assoc, Greenbelt, MD USA.
[Alexander, M. Joan; Kim, Ji-Eun] Colorado Res Associates Off, North West Res Associates, Boulder, CO USA.
[Lim, Boon H.] Jet Prop Lab, Pasadena, CA USA.
[Stutz, Jochen] Univ Calif Los Angeles, Los Angeles, CA USA.
[Pfeilsticker, Klaus] Heidelberg Univ, Heidelberg, Germany.
RP Jensen, EJ (reprint author), NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
EM eric.j.jensen@nasa.gov
RI Fahey, David/G-4499-2013; Rosenlof, Karen/B-5652-2008; Manager, CSD
Publications/B-2789-2015
OI Fahey, David/0000-0003-1720-0634; Rosenlof, Karen/0000-0002-0903-8270;
FU Deutsche Forschungsgemeinschaft (DFG) [PF 384 12/1]
FX We thank the Global Hawk project managers, pilots, and crew. Without
their hard work overcoming numerous challenges, collection of the
excellent data described here would not have been possible. Additional
funding from the Deutsche Forschungsgemeinschaft (DFG) Grant PF 384 12/1
in support of the DOAS measurements and data processing is acknowledged.
NR 29
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PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
EI 1520-0477
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD JAN
PY 2017
VL 98
IS 1
BP 129
EP +
DI 10.1175/BAMS-D-14-00263.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EH6UW
UT WOS:000391910400016
ER
PT J
AU Vitart, F
Ardilouze, C
Bonet, A
Brookshaw, A
Chen, M
Codorean, C
Deque, M
Ferranti, L
Fucile, E
Fuentes, M
Hendon, H
Hodgson, J
Kang, HS
Kumar, A
Lin, H
Liu, G
Liu, X
Malguzzi, P
Mallas, I
Manoussakis, M
Mastrangelo, D
MacLachlan, C
McLean, P
Minami, A
Mladek, R
Nakazawa, T
Najm, S
Nie, Y
Rixen, M
Robertson, AW
Ruti, P
Sun, C
Takaya, Y
Tolstykh, M
Venuti, F
Waliser, D
Woolnough, S
Wu, T
Won, DJ
Xiao, H
Zaripov, R
Zhang, L
AF Vitart, F.
Ardilouze, C.
Bonet, A.
Brookshaw, A.
Chen, M.
Codorean, C.
Deque, M.
Ferranti, L.
Fucile, E.
Fuentes, M.
Hendon, H.
Hodgson, J.
Kang, H-S
Kumar, A.
Lin, H.
Liu, G.
Liu, X.
Malguzzi, P.
Mallas, I.
Manoussakis, M.
Mastrangelo, D.
MacLachlan, C.
McLean, P.
Minami, A.
Mladek, R.
Nakazawa, T.
Najm, S.
Nie, Y.
Rixen, M.
Robertson, A. W.
Ruti, P.
Sun, C.
Takaya, Y.
Tolstykh, M.
Venuti, F.
Waliser, D.
Woolnough, S.
Wu, T.
Won, D-J
Xiao, H.
Zaripov, R.
Zhang, L.
TI THE SUBSEASONAL TO SEASONAL (S2S) PREDICTION PROJECT DATABASE
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID MADDEN-JULIAN OSCILLATION; WEATHER FORECASTS; SIMULATION; ENSEMBLE;
MANAGERS; IMPACTS; SYSTEM
AB A database containing subseasonal to seasonal forecasts from II operational centers is available to the research community and will help advance our understanding of predictability at the subseasonal to seasonal time range.
C1 [Vitart, F.; Bonet, A.; Brookshaw, A.; Codorean, C.; Ferranti, L.; Fucile, E.; Fuentes, M.; Mallas, I.; Manoussakis, M.; Mladek, R.; Najm, S.; Venuti, F.] ECMWF, Reading, Berks, England.
[Ardilouze, C.; Deque, M.] CNRM, Meteo France, Toulouse, France.
[Brookshaw, A.; MacLachlan, C.; McLean, P.] Hadley Ctr, Met Off, Exeter, Devon, England.
[Chen, M.; Kumar, A.] NCEP, College Pk, MD USA.
[Hendon, H.; Liu, G.] Bur Meteorol, Melbourne, Vic, Australia.
[Hodgson, J.; Lin, H.] Environm & Climate Change Canada, Montreal, PQ, Canada.
[Kang, H-S; Nakazawa, T.; Won, D-J] Korea Meteorol Agcy, Seoul, South Korea.
[Liu, X.; Nie, Y.; Sun, C.; Wu, T.; Xiao, H.; Zhang, L.] China Meteorol Adm, Beijing, Peoples R China.
[Malguzzi, P.; Mastrangelo, D.] CNR, ISAC, Bologna, Italy.
[Minami, A.; Takaya, Y.] Japan Meteorol Agcy, Tokyo, Japan.
[Rixen, M.; Ruti, P.] World Meteorol Org, Geneva, Switzerland.
[Robertson, A. W.] Columbia Univ, Int Res Inst Climate & Soc, Palisades, NY USA.
[Tolstykh, M.] Russian Acad Sci, Inst Numer Math, Moscow, Russia.
[Waliser, D.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Woolnough, S.] Univ Reading, Dept Meteorol, Natl Ctr Atmospher Sci, Reading, Berks, England.
[Zaripov, R.] Hydrometeorol Res Ctr, Moscow, Russia.
RP Vitart, F (reprint author), ECMWF, Reading, Berks, England.
EM frederic.vitart@ecmwf.int
OI Mastrangelo, Daniele/0000-0001-9438-5439
FU NASA; Russian Science Support Foundation [14-37-00053]
FX Duane Waliser's contribution was carried out on behalf of the Jet
Propulsion Laboratory, California Institute Of Technology, under a
contract with NASA. The part of Mikhail Tolstykh's contribution (HMCR
model diagnostics) was funded by the Russian Science Support Foundation
(Grant 14-37-00053). The authors thank Gilbert Brunet and two anonymous
reviewers for their suggestions and comments, which helped improve this
manuscript.
NR 22
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U1 5
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PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
EI 1520-0477
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD JAN
PY 2017
VL 98
IS 1
BP 163
EP +
DI 10.1175/BAMS-D-16-0017.1
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EH6UW
UT WOS:000391910400018
ER
PT J
AU Jin, D
Oreopoulos, L
Lee, D
AF Jin, Daeho
Oreopoulos, Lazaros
Lee, Dongmin
TI Regime-based evaluation of cloudiness in CMIP5 models
SO CLIMATE DYNAMICS
LA English
DT Article
DE CMIP5 evaluation; CFMIP; COSP; ISCCP simulator; Cloud assessment; Cloud
climatology; Cloud regime
ID CLIMATE MODELS; GLOBAL OCEANS; CLOUDS; ISCCP; MODIS; WATER; MULTISENSOR;
RETRIEVALS; SIMULATOR; ECMWF
AB The concept of cloud regimes (CRs) is used to develop a framework for evaluating the cloudiness of 12 fifth Coupled Model Intercomparison Project (CMIP5) models. Reference CRs come from existing global International Satellite Cloud Climatology Project (ISCCP) weather states. The evaluation is made possible by the implementation in several CMIP5 models of the ISCCP simulator generating in each grid cell daily joint histograms of cloud optical thickness and cloud top pressure. Model performance is assessed with several metrics such as CR global cloud fraction (CF), CR relative frequency of occurrence (RFO), their product [long-term average total cloud amount (TCA)], cross-correlations of CR RFO maps, and a metric of resemblance between model and ISCCP CRs. In terms of CR global RFO, arguably the most fundamental metric, the models perform unsatisfactorily overall, except for CRs representing thick storm clouds. Because model CR CF is internally constrained by our method, RFO discrepancies yield also substantial TCA errors. Our results support previous findings that CMIP5 models underestimate cloudiness. The multi-model mean performs well in matching observed RFO maps for many CRs, but is still not the best for this or other metrics. When overall performance across all CRs is assessed, some models, despite shortcomings, apparently outperform Moderate Resolution Imaging Spectroradiometer cloud observations evaluated against ISCCP like another model output. Lastly, contrasting cloud simulation performance against each model's equilibrium climate sensitivity in order to gain insight on whether good cloud simulation pairs with particular values of this parameter, yields no clear conclusions.
C1 [Jin, Daeho] Univ Space Res Assoc, Columbia, MD 21046 USA.
[Jin, Daeho; Oreopoulos, Lazaros; Lee, Dongmin] NASA, Goddard Space Flight Ctr, Code 613, Greenbelt, MD 20771 USA.
[Lee, Dongmin] Morgan State Univ, Baltimore, MD 21239 USA.
RP Jin, D (reprint author), Univ Space Res Assoc, Columbia, MD 21046 USA.; Jin, D (reprint author), NASA, Goddard Space Flight Ctr, Code 613, Greenbelt, MD 20771 USA.
EM Daeho.Jin@nasa.gov
FU NASA's Modeling Analysis and Prediction (MAP) program
FX We acknowledge the World Climate Research Programme's Working Group on
Coupled Modeling, which is responsible for CMIP, and we thank the
climate modeling groups (listed in Table 1 of this paper) for producing
and making available their model output. For CMIP, the U.S. Department
of Energy's Program for Climate Model Diagnosis and Intercomparison
provides coordinating support and led development of software
infrastructure in partnership with the Global Organization for Earth
System Science Portals. Lastly, funding by NASA's Modeling Analysis and
Prediction (MAP) program is gratefully acknowledged.
NR 43
TC 1
Z9 1
U1 0
U2 0
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
EI 1432-0894
J9 CLIM DYNAM
JI Clim. Dyn.
PD JAN
PY 2017
VL 48
IS 1-2
BP 89
EP 112
DI 10.1007/s00382-016-3064-0
PG 24
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EI2HK
UT WOS:000392307300006
ER
PT J
AU Jin, D
Oreopoulos, L
Lee, D
AF Jin, Daeho
Oreopoulos, Lazaros
Lee, Dongmin
TI Simplified ISCCP cloud regimes for evaluating cloudiness in CMIP5 models
SO CLIMATE DYNAMICS
LA English
DT Article
DE CMIP5 evaluation; CFMIP; COSP; ISCCP simulator; Cloud assessment; Cloud
climatology; Cloud regime
ID INSTRUMENT SIMULATORS; ECMWF
AB We take advantage of ISCCP simulator data available for many models that participated in CMIP5, in order to introduce a framework for comparing model cloud output with corresponding ISCCP observations based on the cloud regime (CR) concept. Simplified global CRs are employed derived from the co-variations of three variables, namely cloud optical thickness, cloud top pressure and cloud fraction (tau, p (c) , CF). Following evaluation criteria established in a companion paper of ours (Jin et al. 2016), we assess model cloud simulation performance based on how well the simplified CRs are simulated in terms of similarity of centroids, global values and map correlations of relative-frequency-of-occurrence, and long-term total cloud amounts. Mirroring prior results, modeled clouds tend to be too optically thick and not as extensive as in observations. CRs with high-altitude clouds from storm activity are not as well simulated here compared to the previous study, but other regimes containing near-overcast low clouds show improvement. Models that have performed well in the companion paper against CRs defined by joint tau-p (c) histograms distinguish themselves again here, but improvements for previously underperforming models are also seen. Averaging across models does not yield a drastically better picture, except for cloud geographical locations. Cloud evaluation with simplified regimes seems thus more forgiving than that using histogram-based CRs while still strict enough to reveal model weaknesses.
C1 [Jin, Daeho] Univ Space Res Assoc, Columbia, MD 21046 USA.
[Jin, Daeho; Oreopoulos, Lazaros; Lee, Dongmin] NASA, Goddard Space Flight Ctr, Code 613, Greenbelt, MD 20771 USA.
[Lee, Dongmin] Morgan State Univ, Baltimore, MD 21239 USA.
RP Jin, D (reprint author), Univ Space Res Assoc, Columbia, MD 21046 USA.; Jin, D (reprint author), NASA, Goddard Space Flight Ctr, Code 613, Greenbelt, MD 20771 USA.
EM Daeho.Jin@nasa.gov
FU NASA's Modeling Analysis and Prediction (MAP) program
FX We acknowledge the World Climate Research Programme's Working Group on
Coupled Modeling, which is responsible for CMIP, and we thank the
climate modeling groups (listed in Table 1 of this paper) for producing
and making available their model output. For CMIP, the U.S. Department
of Energy's Program for Climate Model Diagnosis and Intercomparison
provides coordinating support and led development of software
infrastructure in partnership with the Global Organization for Earth
System Science Portals. Lastly, funding by NASA's Modeling Analysis and
Prediction (MAP) program is gratefully acknowledged.
NR 25
TC 0
Z9 0
U1 1
U2 1
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
EI 1432-0894
J9 CLIM DYNAM
JI Clim. Dyn.
PD JAN
PY 2017
VL 48
IS 1-2
BP 113
EP 130
DI 10.1007/s00382-016-3107-6
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EI2HK
UT WOS:000392307300007
ER
PT J
AU Li, KF
Su, H
Mak, SN
Chang, TM
Jiang, JH
Norris, JR
Yung, YL
AF Li, King-Fai
Su, Hui
Mak, Sze-Ning
Chang, Tiffany M.
Jiang, Jonathan H.
Norris, Joel R.
Yung, Yuk L.
TI An analysis of high cloud variability: imprints from the El Nio-Southern
Oscillation
SO CLIMATE DYNAMICS
LA English
DT Article
DE Sea surface temperature; Cloud fraction; Interannual variability;
Principal component analysis
ID SEA-SURFACE TEMPERATURE; OUTGOING LONGWAVE RADIATION; CLIMATE
SENSITIVITY; DEEP CONVECTION; DIURNAL CYCLE; MODEL; CIRCULATION;
FEEDBACK; OCEAN; ISCCP
AB Using data from the International Satellite Cloud Climatology Project (ISCCP), we examine how near-global (60A degrees N-60A degrees S) high cloud fraction varies over time in the past three decades. Our focus is on identifying dominant modes of variability and associated spatial patterns, and how they are related to sea surface temperature. By performing the principal component analysis, we find that the first two principal modes of high cloud distribution show strong imprints of the two types of El Nio-Southern Oscillation (ENSO)-the canonical ENSO and the ENSO Modoki. Comparisons between ISCCP data and 14 models from the Atmospheric Model Intercomparison Project Phase 5 (AMIP5) show that models simulate the spatial pattern and the temporal variations of high cloud fraction associated with the canonical ENSO very well but the magnitudes of the canonical ENSO vary among the models. Furthermore, the multi-model mean of the second principal mode in the AMIP5 simulations appears to capture the temporal behavior of the second mode but individual AMIP5 models show large discrepancies in capturing observed temporal variations. A new metric, defined by the relative variances of the first two principal components, suggests that most of the AMIP5 models overestimate the second principal mode of high clouds.
C1 [Li, King-Fai] Univ Washington, Dept Appl Math, Seattle, WA 98195 USA.
[Su, Hui; Jiang, Jonathan H.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Mak, Sze-Ning] Chinese Univ Hong Kong, Dept Phys, Shatin, Hong Kong, Peoples R China.
[Chang, Tiffany M.] Brown Univ, Div Appl Math, Providence, RI 02912 USA.
[Norris, Joel R.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
[Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Li, KF (reprint author), Univ Washington, Dept Appl Math, Seattle, WA 98195 USA.
EM kfli@uw.edu
OI Li, King-Fai/0000-0003-0150-2910
FU California Institute of Technology; Chinese University of Hong Kong;
NASA Energy and Water Cycle Study (NEWS) program; Jack Eddy Fellowship;
NASA [NNX14AR40G]; University of Houston to Caltech [UHOUST.130027]
FX TMC was supported by the 2013 Summer Undergraduate Research Fellowships
at the California Institute of Technology. SNM was supported by the 2014
Summer Undergraduate Research Exchange Program at the Chinese University
of Hong Kong. We thank Katie Antilla, Run-Lie Shia, and Edmund K.-M.
Chang for their technical support and invaluable comments. We also thank
Qiong Zhang, Sally Newman, and Mimi Gerstell for reading the manuscript.
HS and JHJ acknowledge funding support from NASA Energy and Water Cycle
Study (NEWS) program. They performed the work at Jet Propulsion
Laboratory, California Institute of Technology, under contract with
NASA. KFL was supported partly by the Jack Eddy Fellowship managed by
the University Corporation for Atmospheric Research and party by the
NASA Grant NNX14AR40G. YLY was supported by UHOUST.130027 subcontract
from the University of Houston to Caltech. The monthly SST data and
monthly ENSO index were provided by NOAA/OAR/ESRL, Boulder, Colorado,
from their website (http://esrl.noaa.gov/psd/). The monthly ENSO Modoki
index was provided by the Japan Agency for Marine-Earth Science and
Technology
(http://www.jamstec.go.jp/frcgc/research/d1/iod/modoki_home.html.en).
The AMIP5 models were obtained from the CMIP5 model archive
(http://cmip-pcmdi.llnl.gov/cmip5/).
NR 57
TC 0
Z9 0
U1 2
U2 2
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
EI 1432-0894
J9 CLIM DYNAM
JI Clim. Dyn.
PD JAN
PY 2017
VL 48
IS 1-2
BP 447
EP 457
DI 10.1007/s00382-016-3086-7
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EI2HK
UT WOS:000392307300025
ER
PT J
AU Pahlevan, N
Sarkar, S
Devadiga, S
Wolfe, RE
Roman, M
Vermote, E
Lin, GQ
Xiong, XX
AF Pahlevan, Nima
Sarkar, Sudipta
Devadiga, Sadashiva
Wolfe, Robert E.
Roman, Miguel
Vermote, Eric
Lin, Guoqing
Xiong, Xiaoxiong
TI Impact of Spatial Sampling on Continuity of MODIS-VIIRS Land Surface
Reflectance Products: A Simulation Approach
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Biosphere; consistency; geometry; land surface; spatial resolution
ID DIFFERENCE VEGETATION INDEX; RESOLUTION; PERFORMANCE; VALIDATION;
SATELLITE; SCIENCE; SENSORS; COVER
AB With the increasing need to construct long-term climate-quality data records to understand, monitor, and predict climate variability and change, it is vital to continue systematic satellite measurements along with the development of new technology for more quantitative and accurate observations. The Suomi National Polar-orbiting Partnership mission provides continuity in monitoring the Earth's surface and its atmosphere in a similar fashion as the heritage MODIS instruments onboard the National Aeronautics and Space Administration's Terra and Aqua satellites. In this paper, we aim at quantifying the consistency of Aqua MODIS and Suomi-NPP Visible Infrared Imaging Radiometer Suite (VIIRS) Land Surface Reflectance (LSR) and NDVI products as related to their inherent spatial sampling characteristics. To avoid interferences from sources of measurement and/or processing errors other than spatial sampling, including calibration, atmospheric correction, and the effects of the bidirectional reflectance distribution function, the MODIS and VIIRS LSR products were simulated using the Landsat-8's Operational Land Imager (OLI) LSR products. The simulations were performed using the instruments' point spread functions on a daily basis for various OLI scenes over a 16-day orbit cycle. It was found that the daily mean differences due to discrepancies in spatial sampling remain below 0.0015 (1%) in absolute surface reflectance at subgranule scale (i.e., OLI scene size). We also found that the MODIS-VIIRS product intercomparisons appear to be minimally impacted when differences in the corresponding view zenith angles (VZAs) are within the range of -15 degrees to -35 degrees (VZA(V) - VZA(M)), where VIIRS and MODIS footprints resemble in size. In general, depending on the spatial heterogeneity of the OLI scene contents, per-grid-cell differences can reach up to 20%. Further spatial analysis of the simulated NDVI and LSR products revealed that, depending on the user accuracy requirements for product intercomparisons, spatial aggregations may be used. It was found that if per-grid-cell differences on the order of 10% (in LSR or NDVI) are tolerated, the product intercomparisons are expected to be immune from differences in spatial sampling.
C1 [Pahlevan, Nima; Sarkar, Sudipta; Devadiga, Sadashiva; Wolfe, Robert E.; Roman, Miguel; Vermote, Eric; Lin, Guoqing; Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Pahlevan, Nima; Sarkar, Sudipta; Devadiga, Sadashiva; Lin, Guoqing] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
RP Pahlevan, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Pahlevan, N (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
EM nima.pahlevan@nasa.gov
OI Pahlevan, Nima/0000-0002-5454-5212
NR 29
TC 1
Z9 1
U1 9
U2 9
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD JAN
PY 2017
VL 55
IS 1
BP 183
EP 196
DI 10.1109/TGRS.2016.2604214
PG 14
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA EH1LJ
UT WOS:000391527900015
ER
PT J
AU Platnick, S
Meyer, KG
King, MD
Wind, G
Amarasinghe, N
Marchant, B
Arnold, GT
Zhang, ZB
Hubanks, PA
Holz, RE
Yang, P
Ridgway, WL
Riedi, J
AF Platnick, Steven
Meyer, Kerry G.
King, Michael D.
Wind, Galina
Amarasinghe, Nandana
Marchant, Benjamin
Arnold, G. Thomas
Zhang, Zhibo
Hubanks, Paul A.
Holz, Robert E.
Yang, Ping
Ridgway, William L.
Riedi, Jerome
TI The MODIS Cloud Optical and Microphysical Products: Collection 6 Updates
and Examples From Terra and Aqua
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Aqua; cloud remote sensing; clouds; MOD06; moderate resolution imaging
spectroradiometer (MODIS); MYD06; satellite applications; Terra;
terrestrial atmosphere
ID SOLAR-RADIATION MEASUREMENTS; EFFECTIVE PARTICLE RADIUS; INDO-GANGETIC
PLAINS; LIQUID WATER CLOUDS; A-TRAIN; HIMALAYAN FOOTHILLS; AEROSOL
PROPERTIES; THICKNESS; RETRIEVALS; VAPOR
AB The Moderate-Resolution Imaging Spectroradiometer (MODIS) level-2 (L2) cloud product (earth science data set names MOD06 and MYD06 for Terra and Aqua MODIS, respectively) provides pixel-level retrievals of cloud top properties (day and night pressure, temperature, and height) and cloud optical properties (optical thickness, effective particle radius, and water path for both liquid water and ice cloud thermodynamic phases-daytime only). Collection 6 (C6) reprocessing of the product was completed in May 2014 and March 2015 for MODIS Aqua and Terra, respectively. Here we provide an overview of major C6 optical property algorithm changes relative to the previous Collection 5 (C5) product. Notable C6 optical and microphysical algorithm changes include: 1) new ice cloud optical property models and a more extensive cloud radiative transfer code lookup table (LUT) approach; 2) improvement in the skill of the shortwave-derived cloud thermodynamic phase; 3) separate cloud effective radius retrieval data sets for each spectral combination used in previous collections; 4) separate retrievals for partly cloudy pixels and those associated with cloud edges; 5) failure metrics that provide diagnostic information for pixels having observations that fall outside the LUT solution space; and 6) enhanced pixel-level retrieval uncertainty calculations. The C6 algorithm changes can collectively result in significant changes relative to C5, though the magnitude depends on the data set and the pixel's retrieval location in the cloud parameter space. Example L2 granule and level-3 gridded data set differences between the two collections are shown. While the emphasis is on the suite of cloud optical property data sets, other MODIS cloud data sets are discussed when relevant.
C1 [Platnick, Steven] NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD 20771 USA.
[Meyer, Kerry G.; Marchant, Benjamin] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21046 USA.
[King, Michael D.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.
[King, Michael D.] Texas A&M Univ, Inst Adv Study, College Stn, TX 77843 USA.
[Wind, Galina; Amarasinghe, Nandana; Arnold, G. Thomas; Ridgway, William L.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Zhang, Zhibo] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Hubanks, Paul A.] ADNET Syst Inc, Bethesda, MD 20817 USA.
[Holz, Robert E.] Univ Wisconsin Madison, Space Sci & Engn Ctr, Madison, WI 53706 USA.
[Yang, Ping] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77845 USA.
[Riedi, Jerome] Univ Lille Sci & Technol, Opt Atmospher Lab, F-59655 Villeneuve Dascq, France.
RP Platnick, S (reprint author), NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD 20771 USA.
EM steven.platnick@nasa.gov
RI King, Michael/C-7153-2011; Yang, Ping/B-4590-2011; Meyer,
Kerry/E-8095-2016
OI King, Michael/0000-0003-2645-7298; Meyer, Kerry/0000-0001-5361-9200
FU Nataionl Aeronautics and Space Administration (NASA) through MODIS
Science Team; Nataionl Aeronautics and Space Administration (NASA)
through Radiation Sciences Program; NASA [NNX14AO70G, NNX14AO69G]
FX This work was supported by the Nataionl Aeronautics and Space
Administration (NASA) through the MODIS Science Team and the Radiation
Sciences Program. The work of M. D. King was supported by NASA to the
University of Colorado under Grant NNX14AO70G. The work of R. E. Holz
was supported by NASA to the University of Wisconsin under Grant
NNX14AO69G.
NR 71
TC 3
Z9 3
U1 11
U2 11
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD JAN
PY 2017
VL 55
IS 1
BP 502
EP 525
DI 10.1109/TGRS.2016.2610522
PG 24
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA EH1LJ
UT WOS:000391527900040
ER
PT J
AU Islam, T
Hulley, GC
Malakar, NK
Radocinski, RG
Guillevic, PC
Hook, SJ
AF Islam, Tanvir
Hulley, Glynn C.
Malakar, Nabin K.
Radocinski, Robert G.
Guillevic, Pierre C.
Hook, Simon J.
TI A Physics-Based Algorithm for the Simultaneous Retrieval of Land Surface
Temperature and Emissivity From VIIRS Thermal Infrared Data
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Cross validation; intercomparison; Joint Polar Satellite System
(JPSS)/NPOESS satellites; land surface temperature (LST); multispectral
remote sensing; radiative transfer; spectral emissivity retrieval; Suomi
National Polar-Orbiting Partnership (NPP) satellite
ID RADIATIVE-TRANSFER MODEL; MODIS DATA; EARTH-SCIENCE; VALIDATION; ASTER;
RADIOMETER; SATELLITE; PRODUCTS; SEPARATION; ASSIMILATION
AB Land surface temperature (LST) is a key climate variable for studying the energy and water balance of the earth surface and monitoring the effects of climate change. This paper presents a physics-based temperature emissivity separation (TES) algorithm for the simultaneous retrieval of LST and emissivity (LST&E) from the thermal infrared bands of the Suomi National Polar-Orbiting Partnership's Visible Infrared Imaging Radiometer Suite (VIIRS) payload. The new VIIRS LST&E product (VNP21) was developed to provide continuity with the Moderate-Resolution Imaging Spectroradiometer (MODIS) equivalent LST&E product (MxD21) product, which is available in Collection 6, and to address inconsistencies between the current MODIS and VIIRS split-window LST products. The TES algorithm uses full radiative transfer simulations to isolate the surface emitted radiance, and an emissivity calibration curve based on the variability in the surface radiance data to dynamically retrieve both LST and spectral emissivity. Furthermore, an improved water vapor scaling model was implemented to improve the accuracy and stability of the atmospheric correction for conditions with high atmospheric water vapor content. An independent assessment of the VIIRS LST retrievals was performed against in situ LST measurements over two dedicated validation sites at Lake Tahoe and Salton Sea in the Southwestern USA, while the VIIRS emissivity retrievals were evaluated with the latest ASTER Global Emissivity Dataset Version 3 (GEDv3). The bias and root-mean-square error (RMSE) in retrieved VIIRS LST were 0.50 and 1.40 K, respectively for the two sites combined, while mean emissivity differences between VIIRS and ASTER GEDv3 were 0.2%, 0.1%, and 0.3% for bands M14 (8.55 mu m), M15 (10.76 mu m), and M16 (12.01 mu m), respectively, with an RMSE of 1%. We further demonstrate close agreement between the MODIS and VIIRS TES algorithm LST products to within similar to 0.3 K difference, as opposed to the current MODIS and VIIRS split window products, which had an average difference of 3 K.
C1 [Islam, Tanvir; Hulley, Glynn C.; Malakar, Nabin K.; Radocinski, Robert G.; Hook, Simon J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Guillevic, Pierre C.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Guillevic, Pierre C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Islam, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM tanvir.islam@jpl.nasa.gov
NR 53
TC 0
Z9 0
U1 12
U2 12
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD JAN
PY 2017
VL 55
IS 1
BP 563
EP 576
DI 10.1109/TGRS.2016.2611566
PG 14
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA EH1LJ
UT WOS:000391527900044
ER
PT J
AU Zheng, G
Ma, LX
Eitel, JUH
He, W
Magney, TS
Moskal, LM
Li, MS
AF Zheng, Guang
Ma, Lixia
Eitel, Jan U. H.
He, Wei
Magney, Troy S.
Moskal, Ludmila Monika
Li, Mingshi
TI Retrieving Directional Gap Fraction, Extinction Coefficient, and
Effective Leaf Area Index by Incorporating Scan Angle Information From
Discrete Aerial Lidar Data
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Aerial laser scanning (ALS); directional gap fraction (DGF); effective
leaf area index (LAIe); scan angle
ID DISCONTINUOUS VEGETATION CANOPIES; RADIATIVE-TRANSFER MODEL; PLANT
CANOPIES; LASER SCANNER; WAVE-FORMS; COVER; ARCHITECTURE; DISTRIBUTIONS;
FORESTS; IMPACTS
AB The scan angle information implicitly contained within the 3-D point cloud data (PCD) generated from light detection and ranging strongly affects the retrieval accuracy of the forest canopy structural parameters. Using information generated from overlapping aerial laser scanning (ALS) flight paths with multiple scan angles over a forest canopy can help to remove the occlusion effects between foliage elements, ultimately creating a relative comprehensive PCD. In this paper, we develop a novel physically based scan angle correction algorithm to retrieve the effective leaf area index (LAIe) of a forest canopy using ALS. Furthermore, we investigate the effects of scan angle and the number of ALS overpass lines from adjacent flight paths over a forest canopy on directional gap fraction (DGF) estimates. Our results suggest that ALS-based LAIe estimates capture 71.35% of the variations in LAIe derived from digital hemispherical photography. A forest canopy point cloud created using PCD from multiple overlapping ALS flight paths was sufficient to quantitatively reveal the anisotropy characteristics of DGF variations. These results suggest that scan angle information should not be neglected in retrieving forest canopy structural parameters, especially when using ALS data collected with a wide scan angle ( i.e., -30 degrees to 30 degrees in this paper). Finally, this paper provides a solid foundation to characterize the 3-D spatial distribution of a forest radiation regime using ALS-based forest PCD.
C1 [Zheng, Guang; Ma, Lixia] Nanjing Univ, Int Inst Earth Syst Sci, Jiangsu Prov Key Lab Geog Informat Sci & Technol, Nanjing 210023, Jiangsu, Peoples R China.
[Ma, Lixia; He, Wei] Jiangsu Ctr Collaborat Innovat Geog Informat Reso, Nanjing 210023, Jiangsu, Peoples R China.
[Eitel, Jan U. H.] Univ Idaho, Geospatial Lab Environm Dynam, Moscow, ID 83844 USA.
[Eitel, Jan U. H.] Univ Idaho, McCall Outdoor Sci Sch, Mccall, ID 83638 USA.
[Magney, Troy S.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Moskal, Ludmila Monika] Univ Washington, Sch Environm & Forest Sci, Remote Sensing & Geospatial Anal Lab, Precis Forestry Cooperat, Seattle, WA 98195 USA.
[Li, Mingshi] Nanjing Forestry Univ, Coll Forestry, Nanjing 210037, Jiangsu, Peoples R China.
RP Zheng, G (reprint author), Nanjing Univ, Int Inst Earth Syst Sci, Jiangsu Prov Key Lab Geog Informat Sci & Technol, Nanjing 210023, Jiangsu, Peoples R China.
EM zhengguang@nju.edu.cn
FU University of Washington Precision Forestry Cooperative
FX This research was conducted at the International Institute for Earth
System Science, Nanjing University. The authors also want to thank N.
Hackman, Dr. J. Richardson, and P. Johnsey for their help in field data
collection and for the University of Washington Precision Forestry
Cooperative for facilitating and funding the data collection.
NR 47
TC 0
Z9 0
U1 6
U2 6
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD JAN
PY 2017
VL 55
IS 1
BP 577
EP 590
DI 10.1109/TGRS.2016.2611651
PG 14
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA EH1LJ
UT WOS:000391527900045
ER
PT J
AU Mao, W
Thill, M
Hassibi, B
AF Mao, Wei
Thill, Matthew
Hassibi, Babak
TI On Ingleton-Violating Finite Groups
SO IEEE TRANSACTIONS ON INFORMATION THEORY
LA English
DT Article
DE Finite groups; entropy vectors; Ingleton inequality; network coding;
group network codes
ID INFORMATION INEQUALITIES; ENTROPY
AB Given n discrete random variables, its entropy vector is the 2(n) - 1-dimensional vector obtained from the joint entropies of all non-empty subsets of the random variables. It is well known that there is a close relation between such an entropy vector and a certain group-characterizable vector obtained from a finite group and n of its subgroups; indeed, roughly speaking, knowing the region of all such group-characterizable vectors is equivalent to knowing the region of all entropy vectors. This correspondence may be useful for characterizing the space of entropic vectors and for designing network codes. If one restricts attention to abelian groups then not all entropy vectors can be obtained. This is an explanation for the fact shown by Dougherty et al. that linear network codes cannot achieve capacity in general network coding problems (since linear network codes come from abelian groups). All abelian group-characterizable vectors, and by fiat all entropy vectors generated by linear network codes, satisfy a linear inequality called the Ingleton inequality. General entropy vectors, however, do not necessarily have this property. It is, therefore, of interest to identify groups that violate the Ingleton inequality. In this paper, we study the problem of finding nonabelian finite groups that yield characterizable vectors, which violate the Ingleton inequality. Using a refined computer search, we find the symmetric group S-5 to be the smallest group that violates the Ingleton inequality. Careful study of the structure of this group, and its subgroups, reveals that it belongs to the Ingleton-violating family PGL(2, q) with a prime power q >= 5, i.e., the projective group of 2 x 2 nonsingular matrices with entries in F-q. We further interpret this family of groups, and their subgroups, using the theory of group actions and identify the subgroups as certain stabilizers. We also extend the construction to more general groups such as PGL(n, q) and GL(n, q). The families of groups identified here are therefore good candidates for constructing network codes more powerful than linear network codes, and we discuss some considerations for constructing such group network codes.
C1 [Mao, Wei; Thill, Matthew; Hassibi, Babak] CALTECH, Dept Elect Engn, Pasadena, CA 91125 USA.
[Mao, Wei] Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90095 USA.
[Thill, Matthew] Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mao, W (reprint author), CALTECH, Dept Elect Engn, Pasadena, CA 91125 USA.; Mao, W (reprint author), Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90095 USA.
EM wmao.tsinghua@gmail.com; mthill@caltech.edu; hassibi@caltech.edu
FU National Science Foundation [CNS-0932428, CCF-1018927, CCF-1423663,
CCF-1409204]; Qualcomm Inc.; NASA's Jet Propulsion Laboratory through
the President and Director's Fund; King Abdulaziz University; King
Abdullah University of Science and Technology
FX This work was supported in part by the National Science Foundation under
Grant CNS-0932428, Grant CCF-1018927, Grant CCF-1423663, and Grant
CCF-1409204, in part by Qualcomm Inc., in part by the NASA's Jet
Propulsion Laboratory through the President and Director's Fund, in part
by King Abdulaziz University, and in part by the King Abdullah
University of Science and Technology. This work was presented at the
2009 Forty-Seventh Annual Allerton Conference on Communication, Control,
and Computing [1] and the 2010 IEEE International Symposium on
Information Theory [2].
NR 37
TC 0
Z9 0
U1 1
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9448
EI 1557-9654
J9 IEEE T INFORM THEORY
JI IEEE Trans. Inf. Theory
PD JAN
PY 2017
VL 63
IS 1
BP 183
EP 200
DI 10.1109/TIT.2016.2627530
PG 18
WC Computer Science, Information Systems; Engineering, Electrical &
Electronic
SC Computer Science; Engineering
GA EH4KL
UT WOS:000391740000016
ER
PT J
AU Loeb, NG
Wang, HL
Liang, LS
Kato, SJ
Rose, FG
AF Loeb, Norman G.
Wang, Hailan
Liang, Lusheng
Kato, Seiji
Rose, Fred G.
TI Surface energy budget changes over Central Australia during the early
21st century drought
SO INTERNATIONAL JOURNAL OF CLIMATOLOGY
LA English
DT Article
DE energy budget; drought; radiation; albedo; precipitation; latent heat;
sensible heat
ID DATA ASSIMILATION SYSTEM; SOIL-MOISTURE; ATMOSPHERE RADIATION; LAND;
CLIMATE; ALBEDO; REGIONS; PRECIPITATION; REFLECTANCE; VARIABILITY
AB Satellite observations are used to investigate surface energy budget variability over central Australia during the early 21st century drought. Over a large expanse of open shrubland and savanna, surface albedo exhibits a multiyear increase of 0.06 during the drought followed by a sharp decline of 0.08 after heavy rainfall in 2010 broke the drought. The surface albedo variations are associated with increased normalized difference vegetation index (NDVI) during wet years before and after the drought and decreased NDVI during drought years. During the worst drought years (2002-2009), the surface albedo increase is most pronounced in the shortwave infrared region (wavelengths between 1 and 3 mu m), implying soil moisture content variability is the likely cause of the albedo changes. At interannual timescales, surface albedo variability is associated with near-surface soil moisture, controlled by episodic precipitation events, whereas the multiyear increase in surface albedo is more closely linked with decreases in soil moisture in deeper surface layers. In addition to a higher surface albedo and lower soil moisture content during the drought, the observations show less evaporation, enhanced reflected shortwave radiation, increased upward emission of thermal infrared radiation, lower downwelling longwave (LW) radiation, reduced net total downward radiation, and higher sensible heating compared with the rainy period following the drought. Upward emission of thermal infrared radiation decreases sharply after the drought with increased surface evaporation. However, the surface energy budget changes during the worst drought years show a stronger relationship between upward emission of thermal radiation and reflected shortwave flux. During this period, evaporative fraction is extremely low and surface albedo is steadily increasing. In such extreme conditions, the surface albedo appears to modulate surface upward LW radiation, preventing it from getting too high. The change in upward LW radiation thus represents a negative feedback as it offsets further decreases in surface net radiation.
C1 [Loeb, Norman G.; Kato, Seiji] NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA.
[Wang, Hailan; Liang, Lusheng; Rose, Fred G.] Sci Syst & Applicat Inc, Hampton, VA USA.
RP Loeb, NG (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA.
EM norman.g.loeb@nasa.gov
FU NASA CERES Project
FX This research has been supported by the NASA CERES Project. The CERES
datasets were obtained from http://ceres.larc.nasa.gov/order_data.php.
The NASA Langley Atmospheric Sciences Data Center processed the
instantaneous single scanner footprint and monthly SYNIdeg_Edition3 data
used to produce ERNE Ed2.8. ERA-interim mass-corrected-derived
components were downloaded from the NCAR Climate Data Guide at
https://climatedataguide.ucar.edu. GPCP precipitation data were obtained
from http://precip.gsfc.nasa.gov/gpcp_v2.2_data.html. The authors would
like to thank Professor Michael L. Roderick for his helpful comments.
NR 37
TC 1
Z9 1
U1 3
U2 3
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0899-8418
EI 1097-0088
J9 INT J CLIMATOL
JI Int. J. Climatol.
PD JAN
PY 2017
VL 37
IS 1
BP 159
EP 168
DI 10.1002/joc.4694
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EI3TY
UT WOS:000392415700012
ER
PT J
AU Reale, O
Achuthavarier, D
Fuentes, M
Putman, WM
Partyka, G
AF Reale, Oreste
Achuthavarier, Deepthi
Fuentes, Marangelly
Putman, William M.
Partyka, Gary
TI Tropical Cyclones in the 7-km NASA Global Nature Run for Use in
Observing System Simulation Experiments
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID AFRICAN EASTERLY JET; WESTERN NORTH PACIFIC; AUSTRALIAN REGION;
EXTRATROPICAL TRANSITION; 3-DIMENSIONAL STRUCTURE; SOMALI-JET; PART I;
SOUTHERN OSCILLATION; INTERACTIVE AEROSOL; FORECASTING SYSTEM
AB The National Aeronautics and Space Administration (NASA) nature run (NR), released for use in observing system simulation experiments (OSSEs), is a 2-yr-long global nonhydrostatic free-running simulation at a horizontal resolution of 7 km, forced by observed sea surface temperatures (SSTs) and sea ice, and inclusive of interactive aerosols and trace gases. This article evaluates the NR with respect to tropical cyclone (TC) activity. It is emphasized that to serve as an NR, a long-term simulation must be able to produce realistic TCs, which arise out of realistic large-scale forcings. The presence in the NR of the relevant dynamical features over the African monsoon region and the tropical Atlantic is confirmed, along with realistic African easterly wave activity. The NR Atlantic TC seasons, produced with 2005 and 2006 SSTs, show interannual variability consistent with observations, with much stronger activity in 2005. An investigation of TC activity over all the other basins (eastern and western North Pacific Ocean, north and south Indian Ocean, and Australian region), together with important elements of the atmospheric circulation, such as the Somali jet and westerly bursts, reveals that the model captures the fundamental aspects of TC seasons in every basin, producing a realistic number of TCs with realistic tracks, life spans, and structures. This confirms that the NASA NR is a very suitable tool for OSSEs targeting TCs and represents an improvement with respect to previous long simulations that have served the global atmospheric OSSE community.
C1 [Reale, Oreste; Achuthavarier, Deepthi; Fuentes, Marangelly; Putman, William M.; Partyka, Gary] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Reale, Oreste; Achuthavarier, Deepthi] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21046 USA.
[Fuentes, Marangelly; Partyka, Gary] Sci Syst & Applicat Inc, Greenbelt, MD USA.
RP Reale, O (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.; Reale, O (reprint author), Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21046 USA.
EM oreste.reale-1@nasa.gov
FU NASA Modeling, Analysis, and Prediction (MAP) program
FX The GEOS-5 atmospheric general circulation model development in the
Global Modeling and Assimilation Office is funded by David Considine,
under the NASA Modeling, Analysis, and Prediction (MAP) program. The NR
was produced at the NASA Center for Climate Simulation (NCCS). The
authors thank Dr. Ross Hoffman and one anonymous reviewer for their
helpful suggestions.
NR 83
TC 0
Z9 0
U1 2
U2 2
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
EI 1520-0426
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD JAN
PY 2017
VL 34
IS 1
BP 73
EP 100
DI 10.1175/JTECH-D-16-0094.1
PG 28
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA EH5PW
UT WOS:000391826300007
ER
PT J
AU Elsaesser, GS
Del Genio, AD
Jiang, JH
Van Lier-Walqui, M
AF Elsaesser, Gregory S.
Del Genio, Anthony D.
Jiang, Jonathan H.
Van Lier-Walqui, Marcus
TI An Improved Convective Ice Parameterization for the NASA GISS Global
Climate Model and Impacts on Cloud Ice Simulation
SO JOURNAL OF CLIMATE
LA English
DT Article
ID SIZE DISTRIBUTIONS; WATER-CONTENT; SATELLITE-OBSERVATIONS; TROPICAL
CIRRUS; STRATIFORM RAIN; PARTICLE-SIZE; IN-SITU; A-TRAIN; SENSITIVITY;
PROBE
AB Partitioning of convective ice into precipitating and detrained condensate presents a challenge for GCMs since partitioning depends on the strength and microphysics of the convective updraft. It is an important issue because detrainment of ice from updrafts influences the development of stratiform anvils, impacts radiation, and can affect GCM climate sensitivity. Recent studies have shown that the CMIP5 configurations of the Goddard Institute for Space Studies (GISS) GCM simulated upper-tropospheric ice water content (IWC) that exceeded an estimated upper bound by a factor of 2. Partly in response to this bias, a new GCM parameterization of convective cloud ice has been developed that incorporates new ice particle fall speeds and convective outflow particle size distributions (PSDs) from the NASA African Monsoon Multidisciplinary Analyses (NAMMA), NASA Tropical Composition, Cloud and Climate Coupling (TC4), DOE ARM-NASA Midlatitude Continental Convective Clouds Experiment (MC3E), and DOE ARM Small Particles in Cirrus (SPARTICUS) field campaigns. The new parameterization assumes a normalized gamma PSD with two novel developments: no explicit assumption for particle habit in the calculation of mass distributions, and a formulation for translating ice particle fall speeds as a function of maximum diameter into fall speeds as a function of melted-equivalent diameter. Two parameters (particle volume-and projected area-weighted equivalent diameter) are diagnosed as a function of temperature and IWC in the convective plume, and these parameters constrain the shape and scale of the normalized gamma PSD. The diagnosed fall speeds and PSDs are combined with the GCM's parameterized convective updraft vertical velocity to partition convective updraft condensate into precipitating and detrained components. A 5-yr prescribed sea surface temperature GCM simulation shows a 30%-50% decrease in upper-tropospheric deep convective IWC, bringing the tropical and global mean ice water path into closer agreement with CloudSat best estimates.
C1 [Elsaesser, Gregory S.] Columbia Univ, Dept Appl Phys & Math, New York, NY USA.
[Elsaesser, Gregory S.; Del Genio, Anthony D.; Van Lier-Walqui, Marcus] NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
[Jiang, Jonathan H.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Van Lier-Walqui, Marcus] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
RP Elsaesser, GS (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.; Elsaesser, GS (reprint author), Columbia Univ, Dept Appl Phys & Appl Math, 2880 Broadway, New York, NY 10025 USA.
EM gregory.elsaesser@columbia.edu
FU NASA; NASA [RTOP WBS 281945.02.04.02.55, RTOP WBS 573945.04.18.02.41,
RTOP WBS 967701.02.02.01.76]; DOE [DE-SC0014382, DE-SC0006988]
FX We thank Andrew Ackerman and Ann Fridlind for discussion during the
early portion of this analysis (and thank David Mitchell for access to
TC4 PSDs used in the early portion of this work). We thank Greg
McFarquhar for providing MC3E aircraft data, and for a critical review
of this manuscript. We thank Andy Heymsfield for providing the NAMMA and
TC4 field campaign PIP instrument data. Computing resources were
provided by the NASA High-End Computing (HEC) Program through the NASA
Center for Climate Simulation (NCCS) at the Goddard Space Flight Center,
with additional support by NASA GISS and by the Jet Propulsion
Laboratory, California Institute of Technology, under contract with
NASA. This research was funded by the NASA Modeling, Analysis, and
Prediction (MAP) program under RTOP WBS 281945.02.04.02.55 (JJ, AD, and
GE), Precipitation Measurement Missions under RTOP WBS
573945.04.18.02.41 (AD and GE), CloudSat/CALIPSO Mission RTOP WBS
967701.02.02.01.76 (AD), and the DOE Atmospheric System Research Program
(Cooperative Agreement DE-SC0014382 with DOE for AD and GE; Grant
DE-SC0006988 for MVLM). We are grateful to David Considine for his
encouragement and support.
NR 87
TC 0
Z9 0
U1 2
U2 2
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD JAN
PY 2017
VL 30
IS 1
BP 317
EP 336
DI 10.1175/JCLI-D-16-0346.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EH6AW
UT WOS:000391855700019
ER
PT J
AU Yu, S
Pearson, JC
Amano, T
Matsushima, F
AF Yu, S.
Pearson, J. C.
Amano, T.
Matsushima, F.
TI THz spectroscopy of D2H+
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE THz spectra; Tunable FIR; Molecular Ion; Interstellar molecule
ID ROTATIONAL SPECTRA; H2D+; EMISSION; CORE
AB We extended the measurements of the rotational transitions of D2H+ up to 3 THz by using the JPL frequency multiplier chains and a TuFIR system at Toyama. D2H+ was generated in an extended negative glow discharge cell cooled to liquid nitrogen temperature. We observed five new THz lines. All the available rotational transition frequencies together with the combination differences derived from the three fundamental bands were subject to least square analysis to determine the molecular constants. New THz measurements are definitely useful for better characterization of spectroscopic properties. The improved molecular constants provide better predictions of other unobserved rotational transitions. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Yu, S.; Pearson, J. C.; Amano, T.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Matsushima, F.] Toyama Univ, Dept Phys, Toyama 9308555, Japan.
RP Amano, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM shanshan.yu@jpl.nasa.gov; john.c.pearson@jpl.nasa.gov;
tamano@jpl.nasa.gov; matsushi@sci.u-toyama.ac.jp
RI Yu, Shanshan/D-8733-2016
FU JSPS (The Japan Society for Promotion of Science)
FX A part of the research was performed at Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration. This research was also supported
in part by the grants from JSPS (The Japan Society for Promotion of
Science). Participation in part in TuFIR experiment at Toyama by Mari
Suzuki and Mizuki Fujita are gratefully acknowledged.
NR 20
TC 0
Z9 0
U1 0
U2 0
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0022-2852
EI 1096-083X
J9 J MOL SPECTROSC
JI J. Mol. Spectrosc.
PD JAN
PY 2017
VL 331
BP 6
EP 8
DI 10.1016/j.jms.2016.10.012
PG 3
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA EH6UG
UT WOS:000391908800002
ER
PT J
AU Devi, VM
Benner, DC
Sung, K
Crawford, TJ
Gamache, RR
Renaud, CL
Smith, MAH
Mantz, AW
Villanuev, GL
AF Devi, V. Malathy
Benner, D. Chris
Sung, Keeyoon
Crawford, Timothy J.
Gamache, Robert R.
Renaud, Candice L.
Smith, Mary Ann H.
Mantz, Arlan W.
Villanuev, Geronimo L.
TI Line parameters for CO2 broadening in the nu(2) band of (HDO)-O-16
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE HDO-CO2 widths; HDO-CO2 shifts; HDO-CO2 calculated line list;
Temperature dependence of widths; Off-diagonal relaxation matrix element
coefficients; Mars atmosphere
ID ROBERT-BONAMY FORMALISM; INTERMOLECULAR POTENTIAL PARAMETERS;
DIODE-LASER MEASUREMENTS; RANGE DISPERSION ENERGY; WATER-VAPOR;
HALF-WIDTHS; COLLISIONAL PARAMETERS; SHIFT COEFFICIENTS; H2O LINES;
COMBINATION RULES
AB CO2-rich planetary atmospheres such as those of Mars and Venus require accurate knowledge of CO2 broadened HDO half-width coefficients and their temperature dependence exponents for reliable abundance determination. Although a few calculated line lists have recently been published on HDO-CO2 line shapes and their temperature dependences, laboratory measurements of those parameters are thus far non-existent. In this work, we report the first measurements of CO2-broadened half-width and pressure-shift coefficients and their temperature dependences for over 220 transitions in the nu(2) band. First measurements of self-broadened half-width and self-shift coefficients at room temperature are also obtained for majority of these transitions. In addition, the first experimental determination of collisional line mixing has been reported for 11 transition pairs for HDO-CO2 and HDO-HDO systems. These results were obtained by analyzing ten high-resolution spectra of HDO and HDO-CO2 mixtures at various sample temperatures and pressures recorded with the Bruker IFS-125HR Fourier transform spectrometer at the Jet Propulsion Laboratory (JPL). Two coolable absorption cells with path lengths of 2038 cm and 20.941 m were used to record the spectra. The various line parameters were retrieved by fitting all ten spectra simultaneously using a multispectrum nonlinear least squares fitting algorithm.
The HDO transitions in the 1100-4100 cm(-1) range were extracted from the HITRAN2012 database. For the nu(2) and 2 nu(2) -nu(2) bands there were 2245 and 435 transitions, respectively. Modified Complex Robert-Bonamy formalism (MCRB) calculations were made for the half-width coefficients, their temperature dependence and the pressure shift coefficients for the HDO-CO2 and HDO-HDO collision systems. MCRB calculations are compared with the measured values. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Devi, V. Malathy; Benner, D. Chris] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA.
[Sung, Keeyoon; Crawford, Timothy J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Gamache, Robert R.; Renaud, Candice L.] Univ Massachusetts Lowell, Dept Environm Earth & Atmospher Sci, Lowell, MA USA.
[Smith, Mary Ann H.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23665 USA.
[Mantz, Arlan W.] Connecticut Coll, Dept Phys Astron & Geophys, New London, CT 06320 USA.
[Villanuev, Geronimo L.] NASA, Goddard Space Flight Ctr, Astrochem, Greenbelt, MD USA.
RP Devi, VM (reprint author), Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA.
RI Sung, Keeyoon/I-6533-2015
FU NASA's Mars Fundamental Research Program [NNX13AG66G]; National Science
Foundation [AGS-1156862, AGS-1622676]
FX The research performed at the College of William and Mary is supported
by a Grant from NASA's Mars Fundamental Research Program (NNX13AG66G).
The research at the Jet propulsion Laboratory, California Institute of
Technology, Connecticut College and NASA Langley Research Center was
conducted under contracts and cooperative agreements with the National
Aeronautics and Space Administration. Research performed at the
University of Massachusetts Lowell is supported by the National Science
Foundation through Grant No. AGS-1156862 and AGS-1622676. One of the
authors (VM Devi) sincerely thanks Linda Brown from JPL for many useful
discussions and help during the course of the data analysis. She also
acknowledges and thanks Olga Naumenko for providing a part of the line
list from the Supplemental file published in Ref. [17].
NR 74
TC 0
Z9 0
U1 1
U2 1
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD JAN
PY 2017
VL 187
BP 472
EP 488
DI 10.1016/j.jqsrt.2016.10.004
PG 17
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA EH6QP
UT WOS:000391899300044
ER
PT J
AU Kleinbohl, A
Friedson, AJ
Schofield, JT
AF Kleinbohl, Armin
Friedson, A. James
Schofield, John T.
TI Two-dimensional radiative transfer for the retrieval of limb emission
measurements in the martian atmosphere
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE 2D; Radiative transfer; Limb geometry; Mars; MCS
ID 3-D TOMOGRAPHIC RETRIEVAL; MIDDLE-ATMOSPHERE; SOUNDING OBSERVATIONS;
IMAGER GLORIA; MARS; SPECTRA; SENSITIVITY; MODEL
AB The remote sounding of infrared emission from planetary atmospheres using limb-viewing geometry is a powerful technique for deriving vertical profiles of structure and composition on a global scale. Compared with nadir viewing, limb geometry provides enhanced vertical resolution and greater sensitivity to atmospheric constituents. However, standard limb profile retrieval techniques assume spherical symmetry and are vulnerable to biases produced by horizontal gradients in atmospheric parameters. We present a scheme for the correction of horizontal gradients in profile retrievals from limb observations of the martian atmosphere. It characterizes horizontal gradients in temperature, pressure, and aerosol extinction along the line-of-sight of a limb view through neighboring measurements, and represents these gradients by means of two-dimensional radiative transfer in the forward model of the retrieval. The scheme is applied to limb emission measurements from the Mars Climate Sounder instrument on Mars Reconnaissance Orbiter. Retrieval simulations using data from numerical models indicate that biases of up to 10 K in the winter polar region, obtained with standard retrievals using spherical symmetry, are reduced to about 2 K in most locations by the retrieval with two-dimensional radiative transfer. Retrievals from Mars atmospheric measurements suggest that the two-dimensional radiative transfer greatly reduces biases in temperature and aerosol opacity caused by observational geometry, predominantly in the polar winter regions. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Kleinbohl, Armin; Friedson, A. James; Schofield, John T.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Kleinbohl, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 34
TC 0
Z9 0
U1 3
U2 3
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD JAN
PY 2017
VL 187
BP 511
EP 522
DI 10.1016/j.jqsrt.2016.07.009
PG 12
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA EH6QP
UT WOS:000391899300047
ER
PT J
AU Clebone, A
Burian, BK
Polaner, DM
AF Clebone, Anna
Burian, Barbara K.
Polaner, David M.
TI A Time-Out Checklist for Pediatric Regional Anesthetics
SO REGIONAL ANESTHESIA AND PAIN MEDICINE
LA English
DT Article
ID NETWORK PRAN; BLOCKS
AB Background and Objectives: Although pediatric regional anesthesia has a demonstrated record of safety, adverse events, especially those related to block performance issues, still may occur. To reduce the frequency of those events, we developed a Regional Anesthesia Time-Out Checklist using expert opinion and the Delphi method.
Methods: A content development and review was performed by the authors and the Society for Pediatric Anesthesia Quality and Safety Committee. The expert panel was composed of 12 pediatric anesthesiologists, who achieved consensus after 2 rounds of amodified Delphi method. Finally, an author who is an expert in checklist design (B.B.) provided guidance on the formatting and layout of the checklist items to ensure clarity and ease of use. The resulting checklist was trialed in a small pilot study to solicit feedback in a real-life setting.
Results: Sixteen items were included in the checklist sent to the expert panel for the first round of Delphi. Items that had an average rating of 3 or more, with fewer than 3 negative comments, were retained (n = 15). Feedback led to combining several items and dividing the checklist into 2 sections based on the following temporal implementation criteria: "preoperatively" or "immediately before procedure." All remaining 12 checklist items received a positive response from more than 50% of expert panel members and therefore were retained after the second and final round of Delphi. No significant alterations were suggested in the pilot trial.
Conclusions: The Delphi method and human factors principles enabled the creation of a Regional Anesthesia Time-Out Checklist based on published and experiential knowledge of adverse events. Usability of the checklist was supported through the results of a pilot study.
C1 [Clebone, Anna] Univ Chicago, Dept Anesthesia & Crit Care, 5841 S Maryland Ave, Chicago, IL 60637 USA.
[Burian, Barbara K.] NASA, Ames Res Ctr, Human Syst Integrat Div, Moffett Field, CA 94035 USA.
[Polaner, David M.] Univ Colorado, Dept Anesthesiol, Sch Med, Childrens Hosp Colorado, Aurora, CO USA.
[Polaner, David M.] Univ Colorado, Dept Pediat, Sch Med, Childrens Hosp Colorado, Aurora, CO USA.
RP Clebone, A (reprint author), Univ Chicago, Dept Anesthesia & Crit Care, 5841 S Maryland Ave, Chicago, IL 60637 USA.
EM aclebone@gmail.com
NR 12
TC 0
Z9 0
U1 0
U2 0
PU LIPPINCOTT WILLIAMS & WILKINS
PI PHILADELPHIA
PA TWO COMMERCE SQ, 2001 MARKET ST, PHILADELPHIA, PA 19103 USA
SN 1098-7339
EI 1532-8651
J9 REGION ANESTH PAIN M
JI Region. Anesth. Pain Med.
PD JAN-FEB
PY 2017
VL 42
IS 1
BP 105
EP 108
DI 10.1097/AAP.0000000000000509
PG 4
WC Anesthesiology
SC Anesthesiology
GA EH6DA
UT WOS:000391861700015
PM 27831957
ER
PT J
AU Koshimoto, N
Udalski, A
Beaulieu, JP
Sumi, T
Bennett, DP
Bond, IA
Rattenbury, N
Fukui, A
Batista, V
Marquette, JB
Brillant, S
Abe, F
Asakura, Y
Bhattacharya, A
Donachie, M
Freeman, M
Hirao, Y
Itow, Y
Li, MCA
Ling, CH
Masuda, K
Matsubara, Y
Matsuo, T
Muraki, Y
Nagakane, M
Ohnishi, K
Oyokawa, H
Saito, T
Sharan, A
Shibai, H
Sullivan, DJ
Suzuki, D
Tristram, PJ
Yonehara, A
Kozlowski, S
Pietrukowicz, P
Poleski, R
Skowron, J
Soszynski, I
Szymanski, MK
Ulaczyk, K
Wyrzykowski, L
AF Koshimoto, N.
Udalski, A.
Beaulieu, J. P.
Sumi, T.
Bennett, D. P.
Bond, I. A.
Rattenbury, N.
Fukui, A.
Batista, V.
Marquette, J. B.
Brillant, S.
Abe, F.
Asakura, Y.
Bhattacharya, A.
Donachie, M.
Freeman, M.
Hirao, Y.
Itow, Y.
Li, M. C. A.
Ling, C. H.
Masuda, K.
Matsubara, Y.
Matsuo, T.
Muraki, Y.
Nagakane, M.
Ohnishi, K.
Oyokawa, H.
Saito, To.
Sharan, A.
Shibai, H.
Sullivan, D. J.
Suzuki, D.
Tristram, P. J.
Yonehara, A.
Kozlowski, S.
Pietrukowicz, P.
Poleski, R.
Skowron, J.
Soszynski, I.
Szymanski, M. K.
Ulaczyk, K.
Wyrzykowski, L.
CA MOA Collaboration
Ogle Collaboration
TI OGLE-2012-BLG-0950Lb: THE FIRST PLANET MASS MEASUREMENT FROM ONLY
MICROLENS PARALLAX AND LENS FLUX
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE gravitational lensing: micro; planetary systems
ID PARSEC EVOLUTIONARY TRACKS; M-CIRCLE-DOT; OR-EQUAL-TO; GALACTIC BULGE;
HIGH-MAGNIFICATION; EARTH-MASS; SNOW LINE; OGLE-III; M DWARF;
JUPITER/SATURN ANALOG
AB We report the discovery of a microlensing planet OGLE-2012-BLG-0950Lb with a planet/host mass ratio of q similar or equal to 2 x 10(-4). A long term distortion detected in both MOA and OGLE light curve can be explained by the microlens parallax due to the Earth's orbital motion around the Sun. Although the finite source effect is not detected, we obtain the lens flux by the high resolution Keck AO observation. Combining the microlens parallax and the lens flux reveal the nature of the lens: a planet with mass of M-p = 35(-9)(+17)M(circle plus) is orbiting around an M-dwarf with mass of M-host = 0.560(-0.16)(+0.12)M(circle dot) with a planet-host projected separation of r(perpendicular to) = 2.7(-0.7)(+0.6) au located at D-L = 3.0(-1.1)(+0.8) kpc from us. This is the first mass measurement from only microlens parallax and the lens flux without the finite source effect. In the coming space observation-era with Spitzer, K2, Euclid, and WFIRST, we expect many such events for which we will not be able to measure any finite source effect. This work demonstrates an ability of mass measurements in such events.
C1 [Koshimoto, N.; Sumi, T.; Hirao, Y.; Matsuo, T.; Nagakane, M.; Shibai, H.] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, 1-1 Machikaneyama, Toyonaka, Osaka 5600043, Japan.
[Udalski, A.; Kozlowski, S.; Pietrukowicz, P.; Poleski, R.; Skowron, J.; Soszynski, I.; Szymanski, M. K.; Ulaczyk, K.; Wyrzykowski, L.] Univ Warsaw Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland.
[Beaulieu, J. P.; Batista, V.; Marquette, J. B.] UPMC Univ Paris 06, Sorbonne Univ, CNRS, Inst Astrophys Paris,UMR 7095, F-75014 Paris, France.
[Bennett, D. P.; Bhattacharya, A.; Suzuki, D.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Bennett, D. P.; Bhattacharya, A.; Suzuki, D.] NASA, Goddard Space Flight Ctr, Lab Exoplanets & Stellar Astrophys, Greenbelt, MD 20771 USA.
[Bond, I. A.; Ling, C. H.] Massey Univ, Inst Informat & Math Sci, North Shore Mail Ctr, Private Bag 102-904, Auckland, New Zealand.
[Rattenbury, N.; Donachie, M.; Freeman, M.; Li, M. C. A.; Sharan, A.] Univ Auckland, Dept Phys, Private Bag 92019, Auckland, New Zealand.
[Fukui, A.] Natl Astron Observ, Okayama Astrophys Observ, 3037-5 Honjo, Asakuchi, Okayama 7190232, Japan.
[Brillant, S.] ESO, Karl Schwarzschildst 2, D-85748 Garching, Germany.
[Abe, F.; Asakura, Y.; Itow, Y.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Oyokawa, H.] Nagoya Univ, Inst Space Earth Environm Res, Nagoya, Aichi 4648601, Japan.
[Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan.
[Saito, To.] Tokyo Metropolitan Coll Ind Technol, Tokyo 1168523, Japan.
[Sullivan, D. J.] Victoria Univ, Sch Chem & Phys Sci, Wellington, New Zealand.
[Tristram, P. J.] Mt John Observ, POB 56, Lake Tekapo 8770, New Zealand.
[Yonehara, A.] Kyoto Sangyo Univ, Fac Sci, Dept Phys, Kyoto 6038555, Japan.
[Poleski, R.] Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA.
RP Koshimoto, N (reprint author), Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, 1-1 Machikaneyama, Toyonaka, Osaka 5600043, Japan.
FU JSPS KAKENHI [JP15J01676]; National Science Centre, Poland [MAESTRO
2014/14/A/ST9/00121]; CNES; DIM ACAV, Region lle-de-France; PERSU
Sorbonne Universite Programme National de Planetologie; labex ESEP;
[JSPS25103508]; [23340064]
FX We acknowledge the following support: Work by N.K. is supported by JSPS
KAKENHI Grant Number JP15J01676. The MOA project is supported by the
grant JSPS25103508 and 23340064. N.J.R. is a Royal Society of New
Zealand Rutherford Discovery Fellow. OGLE Team thanks Profs. M. Kubiak
and G. Pietrzynski, former members of the OGLE team, for their
contribution to the collection of the OGLE photometric data over the
past years. The OGLE project has received funding from the National
Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to A.U. V.B.
was supported by the CNES and the DIM ACAV, Region lle-de-France. V.B.,
J.P.B., and J.B.M. acknowledge the support of PERSU Sorbonne Universite
the Programme National de Planetologie and the labex ESEP.
NR 89
TC 0
Z9 0
U1 3
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD JAN
PY 2017
VL 153
IS 1
AR 1
DI 10.3847/1538-3881/153/1/1
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EH1OQ
UT WOS:000391536900001
ER
PT J
AU Daneshvar, MRM
Freund, FT
AF Daneshvar, Mohammad Reza Mansouri
Freund, Friedemann T.
TI Remote Sensing of Atmospheric and Ionospheric Signals Prior to the Mw
8.3 Illapel Earthquake, Chile 2015
SO PURE AND APPLIED GEOPHYSICS
LA English
DT Article
DE Illapel earthquake; Chile; Atmospheric anomalies; Ionospheric anomalies;
Satellite observations; Remote sensing; Earthquake precursors; Peroxy
defects; Positive hole charge carriers
ID TOTAL ELECTRON-CONTENT; PRECURSORY SIGNALS; GEOMAGNETIC STORM; TEC
RESPONSE; ANOMALIES; CIRCUIT; CONDUCTIVITY; THUNDERSTORM; SATELLITE;
DEMETER
AB In the present study, a number of atmospheric and some ionospheric anomalies are analyzed, which were recorded prior to the Mw 8.3 Illapel earthquake of September 16, 2015. This very large earthquake occurred in Central Chile, close to the coast, as the result of thrust faulting on the interface between the Nazca Plate and South American continent. Using remotely sensed data extracted from NASA/Giovanni, NOAA/NCEP, and NOAA/NGDC, atmospheric and ionospheric anomalies were observed that co-registered 35-40 and 25-30 days prior to the main shock, respectively. With reference to long-term time series over the epicentral area, significant atmospheric anomalies were recorded for cloud cover, geopotential height, precipitation rates, surface air pressure, omega, stream function, and wind vectors-all in the time window of August 5-10, 2015, 35-40 days prior to the main shock. Anomalous TEC maps were recorded for the same time period. Satellite images indicate the formation of an unusual cyclone, presumably triggered by air turbulences and abnormal atmospheric conditions over the epicentral area, including strong vertical winds. Data from the Jicamarca radio observatory in Peru, more than 2000 km to the North, reveal anomalous ionospheric variations on August 15-20, 2015 with respect to international reference ionosphere thickness parameters and the altitude of the F layer. The observed anomalies are consistent with processes that occur at the ground-to-air interface due to the stress activation of peroxy defects in the hypocentral volume. The flow of positive hole charge carriers to the Earth surface expected to have led to massive air ionization, generating at first primarily positive airborne ions, then negative air ions plus ozone. Understanding the sequence of processes inside the Earth's crust and at the ground-to-air interface provides information not previously available about the causal and temporal linkages between the various pre-earthquake phenomena and the future seismic event.
C1 [Daneshvar, Mohammad Reza Mansouri] Res Inst Shakhes Pajouh, Dept Geog & Nat Hazards, Esfahan, Iran.
[Freund, Friedemann T.] NASA, Ames Res Ctr, Code SCR, Mountain View, CA 94035 USA.
[Freund, Friedemann T.] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
[Freund, Friedemann T.] San Jose State Univ, Dept Phys, San Jose, CA 95192 USA.
RP Daneshvar, MRM (reprint author), Res Inst Shakhes Pajouh, Dept Geog & Nat Hazards, Esfahan, Iran.
EM mrm_danesh-var2012@yahoo.com; friedemann.t.freund@nasa.gov
FU NASA ESI grant through the San Jose State University Foundation
[NNX12AL71G]
FX We wish to acknowledge the NASA and NOAA online data centers for global
transmission of reanalysis data. Friedemann T. Freund acknowledges
support from the NASA ESI grant NNX12AL71G through the San Jose State
University Foundation.
NR 69
TC 0
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U1 5
U2 5
PU SPRINGER BASEL AG
PI BASEL
PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND
SN 0033-4553
EI 1420-9136
J9 PURE APPL GEOPHYS
JI Pure Appl. Geophys.
PD JAN
PY 2017
VL 174
IS 1
BP 11
EP 45
DI 10.1007/s00024-016-1366-0
PG 35
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EG9EV
UT WOS:000391362100002
ER
PT J
AU Needham, AW
Messenger, S
Han, J
Keller, LP
AF Needham, Andrew W.
Messenger, Scott
Han, Jangmi
Keller, Lindsay P.
TI Corundum-hibonite inclusions and the environments of high temperature
processing in the early Solar System
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
DE Corundum; Hibonite; CAI; Chondrite; Oxygen isotopes; 26Al; Magnesium
isotopes; Solar nebula; Condensation
ID MURCHISON CARBONACEOUS CHONDRITE; OXYGEN ISOTOPIC COMPOSITION;
SHORT-LIVED RADIONUCLIDES; REFRACTORY INCLUSIONS; PROTOPLANETARY DISK;
RICH INCLUSIONS; ION MICROPROBE; HETEROGENEOUS DISTRIBUTION; ORIGIN;
AL-26
AB Corundum-bearing Ca-Al-rich inclusions (CAIs) are a rare class of high-temperature condensates from the inner regions of the protoplanetary disk. Their mineralogy is intermediate between isolated corundum grains and CAIs where corundum has been replaced by lower-temperature phases. These inclusions sample a critical transitional period of the inner nebula where both the Sun and protoplanetary disk were rapidly evolving. We conducted O isotopic, Al-Mg chronological, petrographic, and crystallographic studies of four corundum-bearing inclusions in the Murchison CM2 and ALHA 77307 CO3.0 carbonaceous chondrites. Within each inclusion, corundum, hibonite, and spinel have indistinguishable 16 O-rich compositions. The O isotopic compositions from all inclusions fall within a narrow range of Delta(17) O = -22.8 +/- 3.6% that matches values of most previously studied micrometer-sized corundum grains and mineralogically pristine CAIs. These data indicate that, with few exceptions, the most refractory inclusions in carbonaceous chondrites formed from the same O isotopic reservoir. One CAI from ALHA 77307, ALH-61, exhibits a continuous corundum mantle overlying a hibonite core, opposite the equilibrium condensation sequence at typical nebular pressures and dust/gas ratios. Transmission electron microscopy examination of the hibonite-corundum interface suggests that the corundum condensed on the hibonite and was itself then partially overlain with spinel. Additionally, high dust/gas ratios are interpreted from the W-and Mo-depleted composition of a refractory metal nugget within a second corundum-bearing CAI, ALH-160. Together, these observations show that the primary formation conditions of some corundum-bearing CAIs involved non-equilibrium condensation in environments with elevated dust-gas ratios.
The corundum-bearing CAIs studied here have inferred initial Al-26/(27) Al ratios that fall within the roughly bimodal distribution of values observed in most CAIs. ALH-160 retains no resolvable excess Mg-26 while ALH-61 has a well-resolved initial Al-26/Al-27 ratio of 4.2 +/- 0.4 x 10(-5). The presence or absence of live Al-26 at the time of CAI formation may record distinct chronology if Al-26 was initially homogeneously distributed in the early Solar System. Alternatively, variations in Al-26/Al-27 ratios may reflect late injection and/or heterogeneous distribution of Al-26. Regardless of which model for Al-26 distribution is correct, the data presented here indicate that formation of corundum-bearing CAIs was repeated during multiple heating and non-equilibrium condensation events throughout early Solar System history and within a single oxygen isotopic reservoir. (C) 2016 Published by Elsevier Ltd.
C1 [Needham, Andrew W.; Messenger, Scott; Keller, Lindsay P.] NASA JSC, EISD Directorate, ARES, Robert M Walker Lab Space Sci, 2101 NASA Pkwy, Houston, TX 77058 USA.
[Needham, Andrew W.; Han, Jangmi] Lunar & Planetary Inst, 3600 Bay Area Blvd, Houston, TX 77058 USA.
RP Needham, AW (reprint author), NASA JSC, EISD Directorate, ARES, Robert M Walker Lab Space Sci, 2101 NASA Pkwy, Houston, TX 77058 USA.; Needham, AW (reprint author), Carnegie Inst Sci, Geophys Lab, 5251 Broad Branch Rd NW, Washington, DC 20015 USA.
EM aneedham@carnegiescience.edu
FU NASA Cosmochemistry grant [COS13-0018]; NASA Emerging Worlds grant
[EW14-0122]
FX This work was funded by a NASA Cosmochemistry grant COS13-0018 (SM) and
a NASA Emerging Worlds grant EW14-0122 (LPK). Editorial handling by Yuri
Amelin and constructive reviews by Sasha Krot, Steve Simon and an
anonymous reviewer are all gratefully acknowledged. LPI contribution No.
1916.
NR 70
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U1 3
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
EI 1872-9533
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JAN 1
PY 2017
VL 196
BP 18
EP 35
DI 10.1016/j.gca.2016.04.022
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EG3QG
UT WOS:000390959200002
ER
PT J
AU Kebukawa, Y
Zolensky, ME
Chan, QHS
Nagao, K
Kilcoyne, ALD
Bodnar, RJ
Farley, C
Rahman, Z
Le, L
Cody, GD
AF Kebukawa, Yoko
Zolensky, Michael E.
Chan, Queenie H. S.
Nagao, Keisuke
Kilcoyne, A. L. David
Bodnar, Robert J.
Farley, Charles
Rahman, Zia
Le, Loan
Cody, George D.
TI Characterization of carbonaceous matter in xenolithic clasts from the
Sharps (H3.4) meteorite: Constraints on the origin and thermal
processing
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
DE Ordinary chondrites; FTIR spectroscopy; Raman spectroscopy; TEM; Noble
gases; XANES; Organic matter
ID EARLY SOLAR-SYSTEM; ORGANIC-MATTER; RAMAN-SPECTROSCOPY; ORDINARY
CHONDRITES; NOBLE-GASES; PARENT-BODY; MATERIAL GEOTHERMOMETER;
AROMATIC-HYDROCARBONS; PRIMITIVE METEORITES; ISOTOPIC COMPOSITION
AB Primitive xenolithic clasts, often referred to as `` dark clasts", are well known in many regolith breccias. The Sharps H3.4 ordinary chondrite contains unusually large dark clasts up to similar to 1 cm across. Poorly-graphitized carbon (PGC), with Fe, Ni metal and described as `` carbon-rich aggregates", has been reported in these clasts (Brearley, 1990). We report detailed analyses of carbonaceous matter in several identical Sharps clasts using FTIR, Raman, C-XANES, and TEM that provide insight on the extent of thermal processing and possible origin of such clasts. We also prepared acid residues of the clasts using the HCl/HF method and conducted mass spectrometric analysis of the entrained noble gases.
Carbonaceous matter is often used to infer thermal history due to its sensitivity to thermal processes. The FTIR spectra of the acid residue from the Sharps clast suggest that carbonaceous matter in the clast contains less hydrogen and oxygen compared to acid residues from typical type 3.4 ordinary chondrites. The metamorphic temperatures obtained by Raman spectroscopy ranges between similar to 380 degrees C and similar to 490 degrees C. TEM observations indicate that the clasts experienced a peak temperature of 300 degrees C to 400 degrees C, based on the carbon d(002) layer lattice spacing of C-rich aggregates. These estimates are consistent with an earlier estimate of 330 +/- 50 degrees C, that is also estimated by the d(002) layer lattice spacing (Brearley, 1990). It should be noted that the lattice spacing thermometer is based on terrestrial metamorphose rocks, and thus temperature was probably underestimated. Meanwhile, the C-XANES spectra of the C-rich aggregates show high exciton intensities, indicative of graphene structures that developed at around 700-800 degrees C following an extensive period of time (millions of years), however, the surrounding matrix areas experienced lower temperatures of less than 300-500 degrees C. Noble gas analysis of the acid residue from the Sharps clasts shows that the residue is almost identical with some material reported in carbonaceous chondrites, i.e., heavily enriched in the Q-gas component as well as HL-gas from presolar diamonds and Ne-E(H) from presolar SiC.
These results indicate that the C-rich aggregates in the Sharps clasts formed under relatively high temperature conditions, up to 800 degrees C, and were subsequently mixed with lower temperature matrix, probably in a different parent body, before they were incorporated into the final Sharps lithology by collision. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Kebukawa, Yoko] Yokohama Natl Univ, Fac Engn, Hodogaya Ku, 79-5 Tokiwadai, Yokohama, Kanagawa 2408501, Japan.
[Zolensky, Michael E.; Chan, Queenie H. S.] NASA Johnson Space Ctr, ARES, 2101 NASA Pkwy, Houston, TX 77058 USA.
[Nagao, Keisuke] Univ Tokyo, Grad Sch Sci, Geochem Res Ctr, Bunkyo Ku, Tokyo 1130033, Japan.
[Kilcoyne, A. L. David] Lawrence Berkeley Natl Lab, Adv Light Source, 1 Cyclotron Rd, Berkeley, CA 94720 USA.
[Bodnar, Robert J.; Farley, Charles] Virginia Tech, Dept Geosci, Blacksburg, VA 24061 USA.
[Rahman, Zia; Le, Loan] Jacobs NASA Johnson Space Ctr, Houston, TX 77058 USA.
[Cody, George D.] Carnegie Inst Sci, Geophys Lab, 5251 Broad Branch Rd NW, Washington, DC 20015 USA.
[Nagao, Keisuke] Korea Polar Res Inst, 26 Songdomirae Ro, Inchon 21990, South Korea.
RP Kebukawa, Y (reprint author), Yokohama Natl Univ, Fac Engn, Hodogaya Ku, 79-5 Tokiwadai, Yokohama, Kanagawa 2408501, Japan.
EM kebukawa@ynu.ac.jp
RI Kilcoyne, David/I-1465-2013
FU NASA Astrobiology Institute; Japan Society for the Promotion of Science
(JSPS); KAKENHI [15K17794]; Astrobiology Program of National Institutes
of Natural Sciences (NINS); W. M. Keck Foundation; Office of Science,
Department of Energy [DE-AC02-05CH11231]; NASA Cosmochemistry Program;
LARS Program; NASA Postdoctoral Program at the Johnson Space Center;
Ministry of Science, ICT and Planning (MSIP) of Korea
FX We are very grateful to three anonymous reviewers and Associate Editor,
Dr. Eric Quirico for their fruitful comments for this manuscript. We
thank Marc Fries for valuable comments and discussion. We thank Dr.
Bjorn O. Mysen for providing access to the FTIR. This research was
supported by the NASA Astrobiology Institute. YK acknowledges supports
through the Japan Society for the Promotion of Science (JSPS)
Postdoctoral Fellowships and KAKENHI grant (No. 15K17794), and the
Astrobiology Program of National Institutes of Natural Sciences (NINS).
The FTIR facility at the Geophysical Laboratory was supported by the W.
M. Keck Foundation. STXM-XANES data were acquired at beamline 5.3.2.2 at
the ALS, which is supported by the Director of the Office of Science,
Department of Energy, under Contract No. DE-AC02-05CH11231. MEZ was
supported by the NASA Cosmochemistry and LARS Programs. QHSC
acknowledges support from the NASA Postdoctoral Program at the Johnson
Space Center, administered by Oak Ridge Associated Universities. KN
acknowledges the Ministry of Science, ICT and Planning (MSIP) of Korea,
for support to prepare the paper.
NR 115
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U1 5
U2 5
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
EI 1872-9533
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JAN 1
PY 2017
VL 196
BP 74
EP 101
DI 10.1016/j.gca.2016.09.024
PG 28
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EG3QG
UT WOS:000390959200005
ER
PT J
AU Parker, PA
AF Parker, Peter A.
TI Discussion of "Optimizing in a complex world: A statistician's role in
decision making"
SO QUALITY ENGINEERING
LA English
DT Editorial Material
C1 [Parker, Peter A.] Natl Aeronaut & Space Adm, Mail Stop 238, Hampton, VA 23681 USA.
RP Parker, PA (reprint author), Natl Aeronaut & Space Adm, Mail Stop 238, Hampton, VA 23681 USA.
EM peter.a.parker@nasa.gov
NR 5
TC 0
Z9 0
U1 0
U2 0
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA
SN 0898-2112
EI 1532-4222
J9 QUAL ENG
JI Qual. Eng.
PY 2017
VL 29
IS 1
BP 48
EP 50
DI 10.1080/08982112.2016.1217130
PG 3
WC Engineering, Industrial; Statistics & Probability
SC Engineering; Mathematics
GA EG2SR
UT WOS:000390894900009
ER
PT S
AU England, S
Rajulu, S
AF England, Scott
Rajulu, Sudhakar
BE Duffy, VG
TI Application of Strength Requirements to Complex Loading Scenarios
SO ADVANCES IN APPLIED DIGITAL HUMAN MODELING AND SIMULATION
SE Advances in Intelligent Systems and Computing
LA English
DT Proceedings Paper
CT International Conference on Digital Human Modeling and Simulation
CY JUL 27-31, 2016
CL FL
DE NASA; Strength; Requirements; Biomechanics; Ergonomics; Human-systems
integration; Spacesuits
AB NASA's endeavors in human spaceflight rely on extensive volumes of human-systems integration requirements to ensure mission success. These requirements protect space hardware accommodation for the full range of potential crewmembers, but cannot cover every possible action and contingency in detail. This study was undertaken in response to questions from various strength requirement users who were unclear how to apply idealized strength requirements that did not map well to the complex loading scenarios that crewmembers would encounter. Three of the most commonly occurring questions from stakeholders were selected to be investigated by human testing and human modeling. Preliminary findings indicate that deviation from nominal postures can affect compliance with strength requirements positively or negatively, depending on the nature of the deviation. Human modeling offers some avenues for quickly addressing requirement verification questions, but is limited by the fidelity of the model and environment.
C1 [England, Scott] MEI Technol Inc, 2525 Bay Area Blvd Suite 300, Houston, TX 77058 USA.
[Rajulu, Sudhakar] NASA Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA.
RP England, S (reprint author), MEI Technol Inc, 2525 Bay Area Blvd Suite 300, Houston, TX 77058 USA.
EM scott.a.england@nasa.gov
NR 6
TC 0
Z9 0
U1 0
U2 0
PU SPRINGER INT PUBLISHING AG
PI CHAM
PA GEWERBESTRASSE 11, CHAM, CH-6330, SWITZERLAND
SN 2194-5357
BN 978-3-319-41627-4; 978-3-319-41626-7
J9 ADV INTELL SYST
PY 2017
VL 481
BP 155
EP 168
DI 10.1007/978-3-319-41627-4_15
PG 14
WC Computer Science, Artificial Intelligence; Engineering, Industrial
SC Computer Science; Engineering
GA BG6RN
UT WOS:000390837100015
ER
PT S
AU Schutte, P
Goodrich, K
Williams, R
AF Schutte, Paul
Goodrich, Kenneth
Williams, Ralph
BE Stanton, NA
Landry, S
DiBucchianico, G
Vallicelli, A
TI Synergistic Allocation of Flight Expertise on the Flight Deck
(SAFEdeck): A Design Concept to Combat Mode Confusion, Complacency, and
Skill Loss in the Flight Deck
SO ADVANCES IN HUMAN ASPECTS OF TRANSPORTATION
SE Advances in Intelligent Systems and Computing
LA English
DT Proceedings Paper
CT International Conference on Human Factors in Transportation
CY JUL 27-31, 2016
CL FL
DE Human factors; Human-systems integration; Function allocation; Flight
deck; Aviation; Human error; Skill loss
AB This paper presents a new design and function allocation philosophy between pilots and automation that seeks to support the human in mitigating innate weaknesses (e.g., memory, vigilance) while enhancing their strengths (e.g., adaptability, resourcefulness). In this new allocation strategy, called Synergistic Allocation of Flight Expertise in the Flight Deck (SAFEdeck), the automation and the human provide complementary support and backup for each other. Automation is designed to be compliant with the practices of Crew Resource Management. The human takes a more active role in the normal operation of the aircraft without adversely increasing workload over the current automation paradigm. This designed involvement encourages the pilot to be engaged and ready to respond to unexpected situations. As such, the human may be less prone to error than the current automation paradigm.
C1 [Schutte, Paul; Goodrich, Kenneth] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Williams, Ralph] Analyt Mech Associates, Hampton, VA 23666 USA.
RP Schutte, P (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM Paul.C.Schutte@nasa.gov; Kenneth.H.Goodrich@nasa.gov;
Ralph.A.Williams@nasa.gov
NR 14
TC 0
Z9 0
U1 0
U2 0
PU SPRINGER INT PUBLISHING AG
PI CHAM
PA GEWERBESTRASSE 11, CHAM, CH-6330, SWITZERLAND
SN 2194-5357
BN 978-3-319-41682-3; 978-3-319-41681-6
J9 ADV INTELL SYST
PY 2017
VL 484
BP 899
EP 911
DI 10.1007/978-3-319-41682-3_74
PG 13
WC Computer Science, Artificial Intelligence; Transportation Science &
Technology
SC Computer Science; Transportation
GA BG6RL
UT WOS:000390836900074
ER
PT S
AU Caddick, ZA
Gregory, K
Flynn-Evans, EE
AF Caddick, Zachary A.
Gregory, Kevin
Flynn-Evans, Erin E.
BE Stanton, NA
Landry, S
DiBucchianico, G
Vallicelli, A
TI Sleep Environment Recommendations for Future Spaceflight Vehicles
SO ADVANCES IN HUMAN ASPECTS OF TRANSPORTATION
SE Advances in Intelligent Systems and Computing
LA English
DT Proceedings Paper
CT International Conference on Human Factors in Transportation
CY JUL 27-31, 2016
CL FL
DE Extreme environments; Habitability; Human factors; Sleep
ID HIGH-ALTITUDE; CIRCADIAN PACEMAKER; OXYGEN ENRICHMENT; BODY-TEMPERATURE;
IMPROVES SLEEP; NREM SLEEP; REM-SLEEP; HUMANS; LIGHT; NOISE
AB Evidence from spaceflight and ground-based missions demonstrate that sleep loss and circadian desynchronization occur among astronauts, leading to reduced performance and, increased risk of injuries and accidents. We conducted a comprehensive literature review to determine the optimal sleep environment for lighting, temperature, airflow, humidity, comfort, noise, privacy and security in the sleep environment. We reviewed the design and use of sleep environments in a wide range of cohorts including among aquanauts, expeditioners, pilots, military personnel, and ship operators. We also reviewed sleep quality from every NASA spaceflight mission. We found that the optimal sleep environment is cool, dark, quiet, and is perceived as safe and private. There are wide individual differences in the preferred sleep environment; therefore modifiable sleeping compartments are necessary to ensure all crewmembers are able to select personalized configurations for optimal sleep. We provide recommendations to aid in the design of deep space sleep chambers.
C1 [Caddick, Zachary A.; Gregory, Kevin] San Jose State Univ, Res Fdn, San Jose, CA USA.
[Flynn-Evans, Erin E.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Flynn-Evans, EE (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM erin.e.flynn-evans@nasa.gov
NR 95
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U1 0
U2 0
PU SPRINGER INT PUBLISHING AG
PI CHAM
PA GEWERBESTRASSE 11, CHAM, CH-6330, SWITZERLAND
SN 2194-5357
BN 978-3-319-41682-3; 978-3-319-41681-6
J9 ADV INTELL SYST
PY 2017
VL 484
BP 923
EP 933
DI 10.1007/978-3-319-41682-3_76
PG 11
WC Computer Science, Artificial Intelligence; Transportation Science &
Technology
SC Computer Science; Transportation
GA BG6RL
UT WOS:000390836900076
ER
PT S
AU Lyons, JB
Sadler, GG
Koltai, K
Battiste, H
Ho, NT
Hoffmann, LC
Smith, D
Johnson, W
Shively, R
AF Lyons, Joseph B.
Sadler, Garrett G.
Koltai, Kolina
Battiste, Henri
Ho, Nhut T.
Hoffmann, Lauren C.
Smith, David
Johnson, Walter
Shively, Robert
BE SavageKnepshield, P
Chen, J
TI Shaping Trust Through Transparent Design: Theoretical and Experimental
Guidelines
SO ADVANCES IN HUMAN FACTORS IN ROBOTS AND UNMANNED SYSTEMS
SE Advances in Intelligent Systems and Computing
LA English
DT Proceedings Paper
CT 7th International Conference on Applied Human Factors and Ergonomics /
International Conference on Human Factors in Robots and Unmanned Systems
CY JUL 27-31, 2016
CL Bay Lake, FL
DE Trust; Transparency; Automation
ID AUTOMATION; RELIANCE
AB The current research discusses transparency as a means to enable trust of automated systems. Commercial pilots (N = 13) interacted with an automated aid for emergency landings. The automated aid provided decision support during a complex task where pilots were instructed to land several aircraft simultaneously. Three transparency conditions were used to examine the impact of transparency on pilot's trust of the tool. The conditions were: baseline (i.e., the existing tool interface), value (where the tool provided a numeric value for the likely success of a particular airport for that aircraft), and logic (where the tool provided the rationale for the recommendation). Trust was highest in the logic condition, which is consistent with prior studies in this area. Implications for design are discussed in terms of promoting understanding of the rationale for automated recommendations.
C1 [Lyons, Joseph B.] US Air Force, Res Lab, Dayton, OH 45433 USA.
[Sadler, Garrett G.; Koltai, Kolina; Battiste, Henri; Ho, Nhut T.; Hoffmann, Lauren C.] NVH Human Syst Integrat, Canoga Pk, Los Angeles, CA USA.
[Smith, David; Johnson, Walter; Shively, Robert] NASA, Ames Res Ctr, Los Angeles, CA USA.
RP Lyons, JB (reprint author), US Air Force, Res Lab, Dayton, OH 45433 USA.
EM joseph.lyons.6@us.af.mi; garrett.g.sadler@gmail.com;
kolina.koltai@gmail.com; hbattiste@gmail.com; nhut.ho.51@gmail.com;
lauren.c.hoffmann@gmail.com; david.smith@nasa.gov;
walter.johnson@nasa.gov; robert.shively@nasa.gov
NR 11
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U1 1
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PU SPRINGER INT PUBLISHING AG
PI CHAM
PA GEWERBESTRASSE 11, CHAM, CH-6330, SWITZERLAND
SN 2194-5357
BN 978-3-319-41959-6; 978-3-319-41958-9
J9 ADV INTELL SYST
PY 2017
VL 499
BP 127
EP 136
DI 10.1007/978-3-319-41959-6_11
PG 10
WC Automation & Control Systems; Computer Science, Artificial Intelligence;
Robotics
SC Automation & Control Systems; Computer Science; Robotics
GA BG6SB
UT WOS:000390838400011
ER
PT S
AU Trujillo, AC
Puig-Navarro, J
Mehdi, SB
McQuarry, AK
AF Trujillo, Anna C.
Puig-Navarro, Javier
Mehdi, S. Bilal
McQuarry, A. Kyle
BE SavageKnepshield, P
Chen, J
TI Using Natural Language to Enable Mission Managers to Control Multiple
Heterogeneous UAVs
SO ADVANCES IN HUMAN FACTORS IN ROBOTS AND UNMANNED SYSTEMS
SE Advances in Intelligent Systems and Computing
LA English
DT Proceedings Paper
CT 7th International Conference on Applied Human Factors and Ergonomics /
International Conference on Human Factors in Robots and Unmanned Systems
CY JUL 27-31, 2016
CL Bay Lake, FL
DE Unmanned aerial vehicles; Voice commands; Autonomy; Coordinated flight;
Mission operator
AB The availability of highly capable, yet relatively cheap, unmanned aerial vehicles (UAVs) is opening up new areas of use for hobbyists and for commercial activities. This research is developing methods beyond classical control-stick pilot inputs, to allow operators to manage complex missions without in-depth vehicle expertise. These missions may entail several heterogeneous UAVs flying coordinated patterns or flying multiple trajectories deconflicted in time or space to pre-defined locations. This paper describes the functionality and preliminary usability measures of an interface that allows an operator to define a mission using speech inputs. With a defined and simple vocabulary, operators can input the vast majority of mission parameters using simple, intuitive voice commands. Although the operator interface is simple, it is based upon autonomous algorithms that allow the mission to proceed with minimal input from the operator. This paper also describes these underlying algorithms that allow an operator to manage several UAVs.
C1 [Trujillo, Anna C.] NASA, Langley Res Ctr, MS 492, Hampton, VA 23681 USA.
[Puig-Navarro, Javier; Mehdi, S. Bilal] Univ Illinois, Urbana, IL 61801 USA.
[McQuarry, A. Kyle] Analyt Mech Associates Inc, Hampton, VA 23681 USA.
RP Trujillo, AC (reprint author), NASA, Langley Res Ctr, MS 492, Hampton, VA 23681 USA.
EM anna.c.trujillo@nasa.gov; puignav2@illinois.edu; mehdi1@illinois.edu;
andrew.k.mcquarry@nasa.gov
NR 35
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U1 0
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PU SPRINGER INT PUBLISHING AG
PI CHAM
PA GEWERBESTRASSE 11, CHAM, CH-6330, SWITZERLAND
SN 2194-5357
BN 978-3-319-41959-6; 978-3-319-41958-9
J9 ADV INTELL SYST
PY 2017
VL 499
BP 267
EP 280
DI 10.1007/978-3-319-41959-6_22
PG 14
WC Automation & Control Systems; Computer Science, Artificial Intelligence;
Robotics
SC Automation & Control Systems; Computer Science; Robotics
GA BG6SB
UT WOS:000390838400022
ER
PT S
AU Chandarana, M
Trujillo, A
Shimada, K
Allen, BD
AF Chandarana, Meghan
Trujillo, Anna
Shimada, Kenji
Allen, B. Danette
BE SavageKnepshield, P
Chen, J
TI A Natural Interaction Interface for UAVs Using Intuitive Gesture
Recognition
SO ADVANCES IN HUMAN FACTORS IN ROBOTS AND UNMANNED SYSTEMS
SE Advances in Intelligent Systems and Computing
LA English
DT Proceedings Paper
CT 7th International Conference on Applied Human Factors and Ergonomics /
International Conference on Human Factors in Robots and Unmanned Systems
CY JUL 27-31, 2016
CL Bay Lake, FL
DE Natural interaction; Gesture; Trajectory; Flight path; UAV; Non-expert
user
ID ROBOT
AB The popularity of unmanned aerial vehicles (UAVs) is increasing as technological advancements boost their favorability for a broad range of applications. One application is science data collection. In fields like earth and atmospheric science, researchers are seeking to use UAVs to augment their current portfolio of platforms and increase their accessibility to geographic areas of interest. By increasing the number of data collection platforms, UAVs will significantly improve system robustness and allow for more sophisticated studies. Scientists would like the ability to deploy an available fleet of UAVs to traverse a desired flight path and collect sensor data without needing to understand the complex low-level controls required to describe and coordinate such a mission. A natural interaction interface for a Ground Control System (GCS) using gesture recognition is developed to allow non-expert users (e.g., scientists) to define a complex flight path for a UAV using intuitive hand gesture inputs from the constructed gesture library. The GCS calculates the combined trajectory on-line, verifies the trajectory with the user, and sends it to the UAV controller to be flown.
C1 [Chandarana, Meghan; Shimada, Kenji] Carnegie Mellon Univ, Pittsburgh, PA 15213 USA.
[Trujillo, Anna; Allen, B. Danette] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Chandarana, M (reprint author), Carnegie Mellon Univ, Pittsburgh, PA 15213 USA.
EM mchandar@cmu.edu; a.c.trujillo@nasa.gov; shimada@cmu.edu;
danette.allen@nasa.gov
NR 28
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U1 2
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PU SPRINGER INT PUBLISHING AG
PI CHAM
PA GEWERBESTRASSE 11, CHAM, CH-6330, SWITZERLAND
SN 2194-5357
BN 978-3-319-41959-6; 978-3-319-41958-9
J9 ADV INTELL SYST
PY 2017
VL 499
BP 387
EP 398
DI 10.1007/978-3-319-41959-6_32
PG 12
WC Automation & Control Systems; Computer Science, Artificial Intelligence;
Robotics
SC Automation & Control Systems; Computer Science; Robotics
GA BG6SB
UT WOS:000390838400032
ER
PT J
AU Mazzuca, GM
Pickering, KE
Clark, RD
Loughner, CP
Fried, A
Zweers, DCS
Weinheimer, AJ
Dickerson, RR
AF Mazzuca, Gina M.
Pickering, Kenneth E.
Clark, Richard D.
Loughner, Christopher P.
Fried, Alan
Zweers, Deborah C. Stein
Weinheimer, Andrew J.
Dickerson, Russell R.
TI Use of tethersonde and aircraft profiles to study the impact of
mesoscale and microscale meteorology on air quality
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Ozone; Bay breeze; Gulf breeze; DISCOVER-AQ campaign; Pollution
ID LOWER-TROPOSPHERE; CHESAPEAKE BAY; SURFACE OZONE; BREEZE; POLLUTION
AB Highly-resolved vertical profiles of ozone and reactive nitrogen in the lower troposphere were obtained using Millersville University's tethered balloon system and NASA's P-3B aircraft during the July 2011 Baltimore, MD/Washington DC and the September 2013 Houston, TX deployments of the NASA DISCOVER-AQ air quality field mission. The tethered balloon and surface measurement sites were located at Edgewood, MD and Smith Point, TX. The balloon profiles are used to connect aircraft data from the lowest portion of NASA's P-3B spirals (300 m AGL) to the surface thus creating complete profiles from the surface to 3-5 km AGL. The highest concentrations of surface ozone at these coastal sites resulted from mean flow transport of polluted air over an adjacent body of water followed by advection back over land several hours later, due to a bay or gulf breeze. Several meteorological processes including horizontal advection, vertical mixing, thermally direct circulation (i.e., bay, gulf, and, sea breezes) combined with chemical processes like photochemical production and deposition played a role in the local ozone maxima. Several small-scale, but highly polluted layers from the Chesapeake Bay advected landward over Edgewood, MD. The Houston Metro area was subject to large-scale recirculation of emissions from petrochemical sources by the Gulf of Mexico and Galveston Bay breezes. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Mazzuca, Gina M.; Pickering, Kenneth E.; Dickerson, Russell R.] Univ Maryland, Dept Atmospher & Ocean Sci, 4254 Stadium Dr, College Pk, MD 20742 USA.
[Pickering, Kenneth E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Clark, Richard D.] Millersville Univ Pennsylvania, Dept Earth Sci, Millersville, PA 17551 USA.
[Zweers, Deborah C. Stein] KNMI Royal Netherlands Meteorol Inst, De Bilt, Netherlands.
[Fried, Alan] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA.
[Weinheimer, Andrew J.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
[Loughner, Christopher P.] Natl Ocean & Atmospher Adm, Air Resources Lab, College Pk, MD 20740 USA.
[Loughner, Christopher P.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
RP Mazzuca, GM (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, 4254 Stadium Dr, College Pk, MD 20742 USA.
EM gmazzuca@umd.edu
RI Dickerson, Russell/F-2857-2010
OI Dickerson, Russell/0000-0003-0206-3083
FU NASA's AQAST [NNX10AR39G]; MDE; RAMMPP
FX The work presented here was supported under [NNX10AR39G], by NASA's
AQAST, and by MDE, and RAMMPP. The authors would like to thank James
Crawford, Gao Chen, Mary Kleb, and all of the DISCOVER-AQ participants.
Thanks to Edwin Gluth (MDE), Anne Thompson, Douglas Martins, Ryan
Stauffer (PSU), Clare Flynn (UMD), Michael Charnick (Millersville), and
Millersville University undergraduate students who participated in the
tethered balloon and surface operation during DISCOVER-AQ
NR 31
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PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD JAN
PY 2017
VL 149
BP 55
EP 69
DI 10.1016/j.atmosenv.2016.10.025
PG 15
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA EF7MQ
UT WOS:000390514100006
ER
PT J
AU Schnase, JL
Duffy, DQ
Tamkin, GS
Nadeau, D
Thompson, JH
Grieg, CM
McInerney, MA
Webster, WP
AF Schnase, John L.
Duffy, Daniel Q.
Tamkin, Glenn S.
Nadeau, Denis
Thompson, John H.
Grieg, Cristina M.
McInerney, Mark A.
Webster, William P.
TI MERRA Analytic Services: Meeting the Big Data challenges of climate
science through cloud-enabled Climate Analytics-as-a-Service
SO COMPUTERS ENVIRONMENT AND URBAN SYSTEMS
LA English
DT Article
DE MapReduce; Hadoop; Data analytics; Data services; Cloud Computing;
Generativity; iRODS; MERRA; ESGF; BAER
AB Climate science is a Big Data domain that is experiencing unprecedented growth. In our efforts to address the Big Data challenges of climate science, we are moving toward a notion of Climate Analytics-as-a-Service (CAaaS). We focus on analytics, because it is the knowledge gained from our interactions with Big Data that ultimately produce societal benefits. We focus on CAaaS because we believe it provides a useful way of thinking about the problem: a specialization of the concept of business process-as-a-service, which is an evolving extension of IaaS, PaaS, and SaaS enabled by Cloud Computing. Within this framework, Cloud Computing plays an important role; however, we see it as only one element in a constellation of capabilities that are essential to delivering climate analytics as a service. These elements are essential because in the aggregate they lead to generativity, a capacity for self assembly that we feel is the key to solving many of the Big Data challenges in this domain. MERRA Analytic Services (MERRA/AS) is an example of cloud-enabled CAaaS built on this principle. MERRA/AS enables MapReduce analytics over NASA's Modern-Era Retrospective Analysis for Research and Applications (MERRA) data collection. The MERRA reanalysis integrates observational data with numerical models to produce a global temporally and spatially consistent synthesis of 26 key climate variables. It represents a type of data product that is of growing importance to scientists doing climate change research and a wide range of decision support applications. MERRA/AS brings together the following generative elements in a full, end-to-end demonstration of CAaaS capabilities: (1) high-performance, data proximal analytics, (2) scalable data management, (3) software appliance virtualization, (4) adaptive analytics, and (5) a domain-harmonized API. The effectiveness of MERRA/AS has been demonstrated in several applications. In our experience, Cloud Computing lowers the barriers and risk to organizational change, fosters innovation and experimentation, facilitates technology transfer, and provides the agility required to meet our customers' increasing and changing needs. Cloud Computing is providing a new tier in the data services stack that helps connect earthbound, enterprise-level data and computational resources to new customers and new mobility-driven applications and modes of work. For climate science, Cloud Computing's capacity to engage communities in the construction of new capabilities is perhaps the most important link between Cloud Computing and Big Data. Published by Elsevier Ltd.
C1 [Schnase, John L.; Tamkin, Glenn S.; Nadeau, Denis; McInerney, Mark A.; Webster, William P.] NASA, Off Computat & Informat Sci & Technol, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Duffy, Daniel Q.; Thompson, John H.] NASA, Ctr Climate Simulat, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Grieg, Cristina M.] George Mason Univ, Dept Computat Data Sci, Fairfax, VA 22030 USA.
RP Schnase, JL (reprint author), NASA, Off Computat & Informat Sci & Technol, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM John.L.Schnase@NASA.gov
FU NASA
FX We thank Scott Sinno, Ben Bledsoe, Ed Luczak, Mike Little, and Tsengdar
Lee for their many contributions to this effort. Roger Gill, Keith
Weber, Mark Carroll, George Haskett, and Tess Gardiner were instrumental
in making the RECOVER project possible. Thanks also to the iRODS
development team at the University of North Carolina at Chapel Hill's
Renaissance Computing Institute (RENCI) for their indispensable
technical advice on the work we do with iRODS. Readers who wish to
access the applications described in this paper are invited to contact
the authors to make arrangements. This work has been funded in part by
grants from NASA's High-End Computing Program and NASA's Applied
Sciences Program.
NR 31
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PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0198-9715
EI 1873-7587
J9 COMPUT ENVIRON URBAN
JI Comput. Environ. Urban Syst.
PD JAN
PY 2017
VL 61
SI SI
BP 198
EP 211
DI 10.1016/j.compenvurbsys.2013.12.003
PG 14
WC Computer Science, Interdisciplinary Applications; Engineering,
Environmental; Environmental Studies; Geography; Operations Research &
Management Science
SC Computer Science; Engineering; Environmental Sciences & Ecology;
Geography; Operations Research & Management Science
GA EG1YL
UT WOS:000390830200009
ER
PT J
AU Minello, TJ
AF Minello, Thomas J.
TI Environmental factors affecting burrowing by brown shrimp
Farfantepenaeus aztecus and white shrimp Litopenaeus setiferus and their
susceptibility to capture in towed nets
SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY
LA English
DT Article
DE Burrowing; Penaeid shrimp; Catch efficiency; Trawls
ID JUVENILE PENAEID PRAWNS; ACTIVITY PATTERNS; PINK SHRIMP; DECAPOD
CRUSTACEANS; DUORARUM; LIGHT; EFFICIENCY; BEHAVIOR; FISH; METAPENAEUS
AB Laboratory experiments were conducted under simulated daytime conditions to examine the effects of salinity, sediment texture, size, density, and hunger on burrowing behavior of juvenile brown shrimp Farfantepenaeus aztecus and white shrimp Litopenaeus setiferus. Over all experimental conditions (20,929 observations of 2411 individual shrimp), 77.5% of brown shrimp and 21.4% of white shrimp were observed burrowed with more than half of their body beneath the substrate. The tendency of burrowed shrimp to emerge from burrows when disturbed also was tested. When burrowing rates were examined in combination with this tendency to emerge upon disturbance, only 46.7% of brown shrimp would be susceptible to capture in towed nets, while almost all (97%) white shrimp would be susceptible. All environmental factors examined in this study, except salinity for white shrimp, significantly affected burrowing of these species. When these environmental effects on burrowing were combined with the likelihood of emergence, however, the effects of salinity and substrate type on brown shrimp behavior appeared most likely to affect capture by towed nets. Estuarine abundance indices from resource surveys using towed nets could be adjusted using such vulnerability estimates. Published by Elsevier B.V.
C1 [Minello, Thomas J.] NOAA, Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, 4700 Ave U, Galveston, TX 77551 USA.
RP Minello, TJ (reprint author), NOAA, Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, 4700 Ave U, Galveston, TX 77551 USA.
EM tom.minello@noaa.gov
FU NOAA, National Marine Fisheries Service, Southeast Fisheries Science
Center
FX This research was funded by the NOAA, National Marine Fisheries Service,
Southeast Fisheries Science Center. Experiments were conducted by
personnel from the Fishery Ecology Branch (FEB) located at the Galveston
Laboratory. The assistance of everyone in the FEB was essential for the
successful completion of this project. In particular, I would like to
thank Edward Klima, Roger Zimmerman, Eduardo Martinez, and Pamela Baker
for support and assistance in conducting these experiments. Lawrence
Rozas, Alex Chester, and Jeff Pulver reviewed earlier versions of the
manuscript. The findings and conclusions reported here do not
necessarily represent the views of the National Marine Fisheries
Service. [SW]
NR 38
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PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-0981
EI 1879-1697
J9 J EXP MAR BIOL ECOL
JI J. Exp. Mar. Biol. Ecol.
PD JAN
PY 2017
VL 486
BP 265
EP 273
DI 10.1016/j.jembe.2016.10.010
PG 9
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA EF7FP
UT WOS:000390495800032
ER
PT J
AU Rocha, C
Meseguer, J
Munoz, C
AF Rocha, Camilo
Meseguer, Jose
Munoz, Cesar
TI Rewriting modulo SMT and open system analysis
SO JOURNAL OF LOGICAL AND ALGEBRAIC METHODS IN PROGRAMMING
LA English
DT Article
ID SYMBOLIC EXECUTION; MODEL CHECKING; LOGIC; REACHABILITY; UNIFICATION;
AUTOMATA
AB This paper proposes rewriting modulo SMT, a new technique that combines the power of SMT solving, rewriting modulo theories, and model checking. Rewriting modulo SMT is ideally suited to model and analyze reachability properties of infinite-state open systems, i.e., systems that interact with a nondeterministic environment. Such systems exhibit both internal nondeterminism, which is proper to the system, and external nondeterminism, which is due to the environment. In a reflective formalism, such as rewriting logic, rewriting modulo SMT can be reduced to standard rewriting. Hence, rewriting modulo SMT naturally extends rewriting-based reachability analysis techniques, which are available for closed systems, to open systems. Furthermore, a single state expression with symbolic constraints can now denote an infinite set of concrete states. The proposed technique is illustrated with the formal analysis of: (i) a real-time system that is beyond the scope of timed-automata methods and (ii) automatic detection of reachability violations in a synchronous language developed to support autonomous spacecraft operations. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Rocha, Camilo] Pontificia Univ Javeriana, Dept Elect & Comp Sci, Cali, Colombia.
[Meseguer, Jose] Univ Illinois, Dept Comp Sci, 1304 W Springfield Ave, Urbana, IL 61801 USA.
[Munoz, Cesar] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Rocha, C (reprint author), Pontificia Univ Javeriana, Dept Elect & Comp Sci, Cali, Colombia.
EM camilo.rocha@javerianacali.edu.co; meseguer@cs.illinois.edu;
cesar.a.munoz@nasa.gov
FU NSF [CNS 13-19109]; Assurance of Flight Critical System's project of
NASA's Aviation Safety Program at Langley Research Center [NNL09AA00A]
FX The authors would like to thank S. Eker for fruitful discussions on
these ideas and their implementation in Maude, and the anonymous
referees for their very helpful comments that helped us improve the
paper. This work was partially supported by NSF Grant CNS 13-19109. The
first author would like to thank the National Institute of Aerospace for
a short visit supported by the Assurance of Flight Critical System's
project of NASA's Aviation Safety Program at Langley Research Center
under Research Cooperative Agreement No. NNL09AA00A.
NR 68
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PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 2352-2208
J9 J LOG ALGEBR METHODS
JI J. Log. Algebr. Methods Program
PD JAN
PY 2017
VL 86
IS 1
SI SI
BP 269
EP 297
DI 10.1016/j.jlamp.2016.10.001
PG 29
WC Computer Science, Theory & Methods; Logic
SC Computer Science; Science & Technology - Other Topics
GA EF7GI
UT WOS:000390497700011
ER
PT J
AU Masci, FJ
Laher, RR
Rebbapragada, UD
Doran, GB
Miller, AA
Bellm, E
Kasliwal, M
Ofek, EO
Surace, J
Shupe, DL
Grillmair, CJ
Jackson, E
Barlow, T
Yan, L
Cao, Y
Cenko, SB
Storrie-Lombardi, LJ
Helou, G
Prince, TA
Kulkarni, SR
AF Masci, Frank J.
Laher, Russ R.
Rebbapragada, Umaa D.
Doran, Gary B.
Miller, Adam A.
Bellm, Eric
Kasliwal, Mansi
Ofek, Eran O.
Surace, Jason
Shupe, David L.
Grillmair, Carl J.
Jackson, Ed
Barlow, Tom
Yan, Lin
Cao, Yi
Cenko, S. Bradley
Storrie-Lombardi, Lisa J.
Helou, George
Prince, Thomas A.
Kulkarni, Shrinivas R.
TI The IPAC Image Subtraction and Discovery Pipeline for the Intermediate
Palomar Transient Factory
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
DE methods: analytical; methods: data analysis; methods: statistical;
techniques: image processing; techniques: photometric
ID DIGITAL SKY SURVEY; ASTROMETRIC CALIBRATION; VARIABLE-STARS;
CLASSIFICATION; CATALOG; SEARCH; KERNEL; PHOTOMETRY; SUPERNOVAE;
ALGORITHM
AB We describe the near real-time transient-source discovery engine for the intermediate Palomar Transient Factory (iPTF), currently in operations at the Infrared Processing and Analysis Center (IPAC), Caltech. We coin this system the IPAC/iPTF Discovery Engine (or IDE). We review the algorithms used for PSF-matching, image subtraction, detection, photometry, and machine-learned (ML) vetting of extracted transient candidates. We also review the performance of our ML classifier. For a limiting signal-to-noise ratio of 4 in relatively unconfused regions, bogus candidates from processing artifacts and imperfect image subtractions outnumber real transients by; 10:1. This can be considerably higher for image data with inaccurate astrometric and/or PSF-matching solutions. Despite this occasionally high contamination rate, the ML classifier is able to identify real transients with an efficiency (or completeness) of; 97% for a maximum tolerable false-positive rate of 1% when classifying raw candidates. All subtraction-image metrics, source features, ML probability-based real-bogus scores, contextual metadata from other surveys, and possible associations with known Solar System objects are stored in a relational database for retrieval by the various science working groups. We review our efforts in mitigating false-positives and our experience in optimizing the overall system in response to the multitude of science projects underway with iPTF.
C1 [Masci, Frank J.; Shupe, David L.; Yan, Lin; Helou, George] CALTECH, Ctr Infrared Proc & Anal, MS 100-22, Pasadena, CA 91125 USA.
[Laher, Russ R.; Surace, Jason; Grillmair, Carl J.; Jackson, Ed; Storrie-Lombardi, Lisa J.] CALTECH, Spitzer Sci Ctr, MS 314-6, Pasadena, CA 91125 USA.
[Rebbapragada, Umaa D.; Doran, Gary B.; Miller, Adam A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Miller, Adam A.; Bellm, Eric; Kasliwal, Mansi; Barlow, Tom; Cao, Yi; Prince, Thomas A.; Kulkarni, Shrinivas R.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Ofek, Eran O.] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel.
[Cenko, S. Bradley] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, MC 661, Greenbelt, MD 20771 USA.
RP Masci, FJ (reprint author), CALTECH, Ctr Infrared Proc & Anal, MS 100-22, Pasadena, CA 91125 USA.
EM fmasci@caltech.edu
FU iPTF project at the California Institute of Technology; ZTF project at
the California Institute of Technology; National Science Foundation
[AST-144034]; National Science Foundation PIRE GROWTH award; NASA from
Hubble Fellowship grant [HST-HF-51325.01]; STScI; NASA [NAS 5-26555];
NASA
FX This work was funded in part by the iPTF and ZTF projects at the
California Institute of Technology. iPTF is a partnership led by the
California Institute of Technology and includes the Infrared Processing
& Astronomical Center; Los Alamos National Laboratory; University of
Wisconsin at Milwaukee; Oskar-Klein Center of the University of
Stockholm, Sweden; Weizmann Institute of Sciences, Israel; University
System of Taiwan, Taiwan; the Institute for Physics & Mathematics of the
universe, Japan; Lawrence Berkeley National Laboratory and the
University of California, Berkeley. ZTF is funded by the National
Science Foundation under grant no. AST-144034. M.M.K. acknowledges
support from the National Science Foundation PIRE GROWTH award. A.A.M.
acknowledges support for this work by NASA from a Hubble Fellowship
grant: HST-HF-51325.01, awarded by STScI, operated by AURA, Inc., for
NASA, under contract NAS 5-26555. Part of the research was carried out
at the Jet Propulsion Laboratory, California Institute of Technology,
under a contract with NASA.
NR 68
TC 4
Z9 4
U1 6
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6280
EI 1538-3873
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD JAN 1
PY 2017
VL 129
IS 971
AR 014002
DI 10.1088/1538-3873/129/971/014002
PG 48
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EG1RS
UT WOS:000390810500001
ER
PT J
AU Greaves, HE
Vierling, LA
Eitel, JUH
Boelman, NT
Magney, TS
Prager, CM
Griffin, KL
AF Greaves, Heather E.
Vierling, Lee A.
Eitel, Jan U. H.
Boelman, Natalie T.
Magney, Troy S.
Prager, Case M.
Griffin, Kevin L.
TI Applying terrestrial lidar for evaluation and calibration of airborne
lidar-derived shrub biomass estimates in Arctic tundra
SO REMOTE SENSING LETTERS
LA English
DT Article
ID ABOVEGROUND BIOMASS; LEAF-AREA
AB Monitoring of climate-driven expansion of low-stature shrubs in Arctic tundra can be improved through application of high-resolution remote sensing. However, the destructive nature of harvest sampling that is usually performed for validation of these data is resource intensive and can limit future comparisons by destroying benchmark measurements. We compared aboveground shrub biomass estimates derived from terrestrial laser scanning (TLS) and airborne laser scanning (ALS) with the goal of determining whether TLS data can be used to accurately calibrate ALS estimates of shrub biomass in Arctic tundra. We used a leave-one-out cross-validation calibration of canopy volume against harvested shrub biomass to establish predictive relationships between TLS canopy volume and harvested shrub biomass, and between ALS canopy volume and TLS-derived shrub biomass estimates. TLS produced more accurate predictions of shrub biomass (R-2 = 0.78; root mean square deviation [RMSD] = 102 g) than did ALS, but the accuracy of ALS-derived shrub biomass predictions was the same whether they were calibrated directly against harvest biomass or against TLS-derived estimates of biomass (R-2 = 0.62; RMSD = 140 g). Our results suggest that once the initial TLS-harvest relationship is known, TLS can provide valid ground reference data for calibration of ALS-derived estimates of shrub biomass without the need for additional destructive harvest.
C1 [Greaves, Heather E.; Vierling, Lee A.; Eitel, Jan U. H.] Univ Idaho, Dept Nat Resources & Soc, Geospatial Lab Environm Dynam, Moscow, ID 83843 USA.
[Vierling, Lee A.; Eitel, Jan U. H.] Univ Idaho, McCall Outdoor Sci Sch, Mccall, ID USA.
[Boelman, Natalie T.; Griffin, Kevin L.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
[Boelman, Natalie T.; Griffin, Kevin L.] Columbia Univ, Dept Earth & Environm Sci, New York, NY USA.
[Magney, Troy S.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Prager, Case M.; Griffin, Kevin L.] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY USA.
RP Greaves, HE (reprint author), Univ Idaho, Dept Nat Resources & Soc, 875 Perimeter Dr MS 1142, Moscow, ID 83844 USA.
EM hgreaves@uidaho.edu
RI Griffin, Kevin/B-2629-2013
OI Griffin, Kevin/0000-0003-4124-3757
FU National Aeronautics and Space Administration (NASA) Terrestrial Ecology
grant [NNX12AK83G]; NASA Earth Science Fellowship [NNX15AP04H]; NASA
Idaho Space Grant Fellowship [NNX10AM75H]; NASA [EAR-0735156]
FX This work was supported by National Aeronautics and Space Administration
(NASA) Terrestrial Ecology grant NNX12AK83G (LAV, PI), NASA Earth
Science Fellowship NNX15AP04H awarded to HEG, and NASA Idaho Space Grant
Fellowship NNX10AM75H awarded to TSM. Riegl VZ-400 and accessories were
provided by the UNAVCO Facility with support from the National Science
Foundation (NSF) and NASA under NSF Cooperative Agreement No.
EAR-0735156.
NR 15
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Z9 0
U1 10
U2 10
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND
SN 2150-704X
EI 2150-7058
J9 REMOTE SENS LETT
JI Remote Sens. Lett.
PY 2017
VL 8
IS 2
BP 175
EP 184
DI 10.1080/2150704X.2016.1246770
PG 10
WC Remote Sensing; Imaging Science & Photographic Technology
SC Remote Sensing; Imaging Science & Photographic Technology
GA EF8IU
UT WOS:000390573300008
ER
PT J
AU Baker, EH
Painter, TH
Schneider, D
Meddens, AJH
Hicke, JA
Molotch, NP
AF Baker, Emily H.
Painter, Thomas H.
Schneider, Dominik
Meddens, Arjan J. H.
Hicke, Jeffrey A.
Molotch, Noah P.
TI Quantifying insect-related forest mortality with the remote sensing of
snow
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Snow cover; Forest mortality; MODIS; Mountain pine beetle
ID WESTERN UNITED-STATES; PINE-BEETLE INFESTATION; TREE MORTALITY;
BRITISH-COLUMBIA; ROCKY-MOUNTAINS; MODIS DATA; OUTBREAK; COLORADO;
IMAGERY; COVER
AB Greenhouse gas emissions have altered global climate significantly, increasing the frequency of drought, fire, and insect- and pathogen-related mortality in forests across the western United States. The accuracy of satellite-based estimates of canopy change has been limited by difficulties associated with discriminating overstory canopy from understory vegetation. To overcome this issue, we developed a method to quantify forest canopy cover using winter-season fractional snow covered area (F-SCA) data from NASA's Moderate Resolution Imaging Spectroradiometer (MODIS) snow covered area and grain size (MODSCAG) algorithm. The method utilizes time series of Fscp, data to identify images with continuous ground snow coverage and a snow-free overstory, effectively masking out the influence of understory vegetation. Using this method, we determined that MODSCAGretrieved viewable gap fraction (VGF; i.e. fraction of pixel sub-canopy viewable area) was significantly correlated with an independent product of yearly crown mortality caused by mountain pine beetles derived from Landsat imagery at 25 high-mortality sites in northern Colorado ((r) over bar = 0.96 +/- 0.03, p<0.03). Additionally, we determined the temporal lag between tree mortality and needlefall, showing that needlefall occurred an average of 2.6 +/- 1.2 years after year of attack. The canopy change detection method described herein is the first to utilize snow cover to mask understory impacts on overstory detection. The method can be applied anywhere in the seasonal snow zone and therefore has wide applicability given that 30% of the global land surface is seasonally snow covered. In this regard, the approach addresses significant limitations of previously published methods of canopy change detection and has broad implications with regard to understanding forest mortality and the representation of disturbance within hydrologic, land surface, and climate models. (C) 2016 Published by Elsevier Inc.
C1 [Baker, Emily H.; Schneider, Dominik; Molotch, Noah P.] Univ Colorado, Dept Geog, Inst Arctic & Alpine Res, Boulder, CO 80303 USA.
[Painter, Thomas H.; Molotch, Noah P.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Meddens, Arjan J. H.] Univ Idaho, Coll Nat Resources, Moscow, ID 83844 USA.
[Hicke, Jeffrey A.] Univ Idaho, Dept Geog, Moscow, ID 83844 USA.
RP Molotch, NP (reprint author), Univ Colorado, Dept Geog, Inst Arctic & Alpine Res, Boulder, CO 80303 USA.
EM noah.molotch@colorado.edu
RI Painter, Thomas/B-7806-2016;
OI MOLOTCH, NOAH/0000-0003-4733-8060; Baker, Emily/0000-0002-0938-3496
FU NASA [NNXIIAK35A]; NSF-U.S. Department of Agriculture (USDA) joint
program for Water Sustainability and Climate (USDA) [2012-67003-19802];
NSF Hydrological Sciences Program (NSF) [EAR1141764]; NASA Earth and
Space Science Fellowship
FX This material is based upon work supported by NASA grant NNXIIAK35A, the
NSF-U.S. Department of Agriculture (USDA) joint program for Water
Sustainability and Climate (USDA Grant: 2012-67003-19802), and the NSF
Hydrological Sciences Program (NSF Grant: EAR1141764). Part of this work
was performed at the Jet Propulsion Laboratory, California Institute of
Technology under a contract with NASA. D. Schneider was supported by a
NASA Earth and Space Science Fellowship. We also thank GDAL developers
(GDAL Development Team, 2016) and the R Core Team (R Core Team, 2016);
in particular authors of the raster (Hijmans, 2016) and rgdal (Bivand et
al., 2016) packages. All code and data is available upon request from
the corresponding author.
NR 70
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U1 21
U2 21
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD JAN
PY 2017
VL 188
BP 26
EP 36
DI 10.1016/j.rse.2016.11.001
PG 11
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA EF9BY
UT WOS:000390626900004
ER
PT J
AU Kim, B
Sarkar, S
AF Kim, Bokhwa
Sarkar, Sudipta
TI Impact of wildfires on some greenhouse gases over continental USA: A
study based on satellite data
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Fire; Aqua; AIRS; Trace-gas; Ozone; Methane; Carbon monoxide; Water
vapor; USA; Spring; Summer
ID TROPOSPHERIC OZONE; EMISSIONS; CLIMATE; FIRES; SEA
AB Wildfire episodes are becoming more rampant with global warming and climate change. Every year it causes lot of damage in terms of burnt acres and also impacts the air quality and climate through emission of various trace greenhouse gases. As emissions from large fires increase with time, it is essential to monitor the extent and spatial distribution of such changes that can have both short term and long-term implications in terms of human health and feedback on global radiative forcing. In this paper we have used the vertical profile distributions of some of the key trace gases, from AQUA-AIRS sensor to better understand the impact of wildfires in terms of magnitude, spatial and seasonal distribution. Our study shows the impact of season on fire emission in the planetary boundary layer and the free troposphere and also highlights areas in the continental United States (CONUS) where different trace gas emissions are more preponderant. Overall it successfully demonstrates the applicability of satellite-based sensors for regular monitoring of fire related trace gas emissions. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Kim, Bokhwa] George Mason Univ, Sch Computat Sci & Informat, 4400 Univ Dr, Fairfax, VA 22030 USA.
[Sarkar, Sudipta] NASA Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Sarkar, Sudipta] Sci Syst & Applicat Inc, 10210 Greenbelt Rd,Suite 600, Lanham, MD 20706 USA.
RP Sarkar, S (reprint author), NASA Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM Sudipta.sarkar@nasa.gov
OI Sarkar, Sudipta/0000-0003-0551-6543
NR 29
TC 0
Z9 0
U1 28
U2 28
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD JAN
PY 2017
VL 188
BP 118
EP 126
DI 10.1016/j.rse.2016.10.047
PG 9
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA EF9BY
UT WOS:000390626900011
ER
PT J
AU Nelson, R
Margolis, H
Montesano, P
Sun, GQ
Cook, B
Corp, L
Andersen, HE
deJong, B
Pellat, FP
Fickel, T
Kauffman, J
Prisley, S
AF Nelson, Ross
Margolis, Hank
Montesano, Paul
Sun, Guoqing
Cook, Bruce
Corp, Larry
Andersen, Hans-Erik
deJong, Ben
Paz Pellat, Fernando
Fickel, Thaddeus
Kauffman, Jobriath
Prisley, Stephen
TI Lidar-based estimates of aboveground biomass in the continental US and
Mexico using ground, airborne, and satellite observations
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE ICESat/GLAS; Hybrid 3-phase sampling; Model-based; Forest biomass
ID LEAF-AREA INDEX; FOREST BIOMASS; HEDMARK COUNTY; BOREAL FOREST;
SPACEBORNE LIDAR; NATIONAL FOREST; NORWAY; UNCERTAINTY; ICESAT/GLAS;
ACCURACY
AB Existing national forest inventory plots, an airborne lidar scanning (ALS) system, and a space profiling lidar system (ICESat-GLAS) are used to generate circa 2005 estimates of total aboveground dry biomass (AGB) in forest strata, by state, in the continental United States (CONUS) and Mexico. The airborne lidar is used to link ground observations of AGB to space lidar measurements. Two sets of models are generated, the first relating ground estimates of AGB to airborne laser scanning (ALS) measurements and the second set relating ALS estimates of AGB (generated using the first model set) to GLAS measurements. GLAS then, is used as a sampling tool within a hybrid estimation framework to generate stratum-, state-, and national-level AGB estimates. A two-phase variance estimator is employed to quantify GLAS sampling variability and, additively, ALS-GLAS model variability in this current, three-phase (ground-ALS-space lidar) study. The model variance component characterizes the variability of the regression coefficients used to predict ALS-based estimates of biomass as a function of GLAS measurements. Three different types of predictive models are considered in CONUS to determine which produced biomass totals closest to ground-based national forest inventory estimates - (1) linear (LIN), (2) linear-no-intercept (LNI), and (3) log-linear. For CONUS at the national level, the GLAS LNI model estimate (23.95 +/- 0.45 Gt AGB), agreed most closely with the US national forest inventory ground estimate, 24.17 +/- 0.06 Gt, i.e., within 1%. The national biomass total based on linear ground-ALS and ALS-GLAS models (25.87 +/- 0.49 Gt) overestimated the national ground-based estimate by 7.5%. The comparable log -linear model result (63.29 +/- 1.36 Gt) overestimated ground results by 261%. All three national biomass GLAS estimates, LIN, LNI, and log -linear, are based on 241,718 pulses collected on 230 orbits. The US national forest inventory (ground) estimates are based on 119,414 ground plots. At the US state level, the average absolute value of the deviation of LNI GLAS estimates from the comparable ground estimate of total biomass was 18.8% (range: Oregon, -40.8% to North Dakota, 128.6%). Log-linear models produced gross overestimates in the continental US, i.e., >2.6x, and the use of this model to predict regional biomass using GLAS data in temperate, western hemisphere forests is not appropriate. The best model form, LNI, is used to produce biomass estimates in Mexico. The average biomass density in Mexican forests is 53.10 +/- 0.88 t/ha, and the total biomass for the country, given a total forest area of 688,096 km(2), is 3.65 +/- 0.06 Gt. In Mexico, our GLAS biomass total underestimated a 2005 FAO estimate (4.152 Gt) by 12% and overestimated a 2007/8 radar study's figure (3.06 Gt) by 19%. (C) Published by Elsevier Inc.
C1 [Nelson, Ross; Margolis, Hank; Montesano, Paul; Sun, Guoqing; Cook, Bruce; Corp, Larry] NASA GSFC, Biospher Sci Lab, Code 618, Greenbelt, MD 20771 USA.
[Margolis, Hank] Univ Laval, Ctr Etud Foret, Quebec City, PQ G1V0A6, Canada.
[Margolis, Hank] NASA Headquarters, Div Earth Sci, 300 E St SW, Washington, DC 20546 USA.
[Montesano, Paul; Corp, Larry] Sci Syst & Applicat Inc, 10210 Greenbelt Rd, Lanham, MD 20706 USA.
[Sun, Guoqing] Univ Maryland, Dept Geog Sci, Lefrak Hall, College Pk, MD 20742 USA.
[Andersen, Hans-Erik] Univ Washington, US Forest Serv, Pacific Northwest Res Stn, 107 Anderson Hall,POB 352100, Seattle, WA 98195 USA.
[deJong, Ben] El Colegio Frontera Sur, Av Ranco Pollgono 2-A, Lerma 24500, Campeche, Mexico.
[Paz Pellat, Fernando] Colegio Postgrad Ciencias Agr, Km 36-5,Texcoco 5, Montecillo 56230, Estado De Mexic, Mexico.
[Fickel, Thaddeus] Infrared Baron Inc, 2372 North 1st St, Hermiston, OR 97838 USA.
[Kauffman, Jobriath; Prisley, Stephen] Virginia Tech, Dept Forest Resources & Environm Conservat, Cheatham Hall,310 West Campus Dr, Blacksburg, VA 24061 USA.
RP Nelson, R (reprint author), NASA GSFC, Biospher Sci Lab, Code 618, Greenbelt, MD 20771 USA.
EM rfn104@gmail.com; hank.a.margolis@nasa.gov; paul.m.montesano@nasa.gov;
quoging.sun-1@nasa.gov; bruce.cook@nasa.gov; lawrence.a.corp@nasa.gov;
handersen@fs.fed.us; bjong@ecosur.mx; pellat@colpos.mx;
tad@infraredbaron.com; jkauffma@vt.edu; prisley@vt.edu
FU NASA's Carbon Cycle Science Program within the Science Mission
Directorate Earth Science Division [NNH10ZDA001N-CARBON(2010)]
FX This research was funded by NASA's Carbon Cycle Science Program within
the Science Mission Directorate Earth Science
Division-NNH10ZDA001N-CARBON(2010).
NR 44
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U1 18
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PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD JAN
PY 2017
VL 188
BP 127
EP 140
DI 10.1016/j.rse.2016.10.038
PG 14
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA EF9BY
UT WOS:000390626900012
ER
PT J
AU Lindsay, MR
Anderson, C
Fox, N
Scofield, G
Allen, J
Anderson, E
Bueter, L
Poudel, S
Sutherland, K
Munson-McGee, JH
Van Nostrand, JD
Zhou, J
Spear, JR
Baxter, BK
Lageson, DR
Boyd, ES
AF Lindsay, M. R.
Anderson, C.
Fox, N.
Scofield, G.
Allen, J.
Anderson, E.
Bueter, L.
Poudel, S.
Sutherland, K.
Munson-McGee, J. H.
Van Nostrand, J. D.
Zhou, J.
Spear, J. R.
Baxter, B. K.
Lageson, D. R.
Boyd, E. S.
TI Microbialite response to an anthropogenic salinity gradient in Great
Salt Lake, Utah
SO GEOBIOLOGY
LA English
DT Article
ID MARINE STROMATOLITES; ALGAL STROMATOLITES; WESTERN-AUSTRALIA;
NATIONAL-PARK; SHARK BAY; USA; DIVERSITY; LITHIFICATION; COMMUNITIES;
WATER
AB A railroad causeway across Great Salt Lake, Utah (GSL), has restricted water flow since its construction in 1959, resulting in a more saline North Arm (NA; 24%-31% salinity) and a less saline South Arm (SA; 11%-14% salinity). Here, we characterized microbial carbonates collected from the SA and the NA to evaluate the effect of increased salinity on community composition and abundance and to determine whether the communities present in the NA are still actively precipitating carbonate or if they are remnant features from prior to causeway construction. SSU rRNA gene abundances associated with the NA microbialite were three orders of magnitude lower than those associated with the SA microbialite, indicating that the latter community is more productive. SSU rRNA gene sequencing and functional gene microarray analyses indicated that SA and NA microbialite communities are distinct. In particular, abundant sequences affiliated with photoautotrophic taxa including cyanobacteria and diatoms that may drive carbonate precipitation and thus still actively form microbialites were identified in the SA microbialite; sequences affiliated with photoautotrophic taxa were in low abundance in the NA microbialite. SA and NA microbialites comprise smooth prismatic aragonite crystals. However, the SA microbialite also contained micritic aragonite, which can be formed as a result of biological activity. Collectively, these observations suggest that NA microbialites are likely to be remnant features from prior to causeway construction and indicate a strong decrease in the ability of NA microbialite communities to actively precipitate carbonate minerals. Moreover, the results suggest a role for cyanobacteria and diatoms in carbonate precipitation and microbialite formation in the SA of GSL.
C1 [Lindsay, M. R.; Anderson, E.; Bueter, L.; Poudel, S.; Munson-McGee, J. H.; Boyd, E. S.] Montana State Univ, Dept Microbiol & Immunol, Bozeman, MT 59717 USA.
[Anderson, C.; Fox, N.; Scofield, G.; Allen, J.; Sutherland, K.; Lageson, D. R.] Montana State Univ, Dept Earth Sci, Bozeman, MT 59717 USA.
[Van Nostrand, J. D.; Zhou, J.] Univ Oklahoma, Dept Microbiol & Plant Biol, Norman, OK 73019 USA.
[Zhou, J.] Tsinghua Univ, Sch Environm, State Key Joint Lab Environm Simulat & Pollut Con, Beijing, Peoples R China.
[Zhou, J.] Lawrence Berkeley Natl Lab, Earth Sci Div, Berkeley, CA USA.
[Spear, J. R.] Colorado Sch Mines, Dept Civil & Environm Engn, Golden, CO 80401 USA.
[Baxter, B. K.] Westminster Coll, Dept Biol, Salt Lake City, UT USA.
[Spear, J. R.; Boyd, E. S.] NASA, Astrobiol Inst, Mountain View, CA USA.
RP Boyd, ES (reprint author), Montana State Univ, Dept Microbiol & Immunol, Bozeman, MT 59717 USA.
EM eboyd@montana.edu
FU Utah Department of Natural Resources Division of Forestry, Fire State
Lands; NASA Astrobiology Institute [NNA15BB02A]
FX The authors thank Laura Kellerman for her assistance and expertise with
the field emission scanning electron microscope, Dr. Karlene Hoo, Dean
of the Montana State University Graduate School, for providing funds to
help defray costs associated with our Precambrian Biosphere graduate
class project, Dr. Mark Jutila for providing funds that enabled a class
field trip to the Bridger Mountains to observe a stromatolite fossil
bed, Donald L. Clark from the Utah Geologic Survey for careful review of
this manuscript, and Charles G. Oviatt for helpful discussions regarding
the geologic history of GSL. This work was supported by a grant from the
Utah Department of Natural Resources Division of Forestry, Fire & State
Lands (BKB and ESB) and a grant (NNA15BB02A) from the NASA Astrobiology
Institute (JRS and ESB).
NR 97
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U1 9
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PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1472-4677
EI 1472-4669
J9 GEOBIOLOGY
JI Geobiology
PD JAN
PY 2017
VL 15
IS 1
BP 131
EP 145
DI 10.1111/gbi.12201
PG 15
WC Biology; Environmental Sciences; Geosciences, Multidisciplinary
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Geology
GA EF3AD
UT WOS:000390195900009
PM 27418462
ER
PT J
AU Singh, SK
Srivastava, PK
Szabo, S
Petropoulos, GP
Gupta, M
Islam, T
AF Singh, Sudhir Kumar
Srivastava, Prashant K.
Szabo, Szilard
Petropoulos, George P.
Gupta, Manika
Islam, Tanvir
TI Landscape transform and spatial metrics for mapping spatiotemporal land
cover dynamics using Earth Observation data-sets
SO GEOCARTO INTERNATIONAL
LA English
DT Article
DE Protected ecosystem; remote sensing; landscape pattern; fragmentation;
ecological metrics; geographic information system
ID MAXIMUM-LIKELIHOOD CLASSIFICATION; REMOTE-SENSING DATA; GROUNDWATER
QUALITY; RANDOM FORESTS; INDIA; FRAGMENTATION; GIS; IDENTIFICATION;
FRAGSTATS; SELECTION
AB Analysis of Earth observation (EO) data, often combined with geographical information systems (GIS), allows monitoring of land cover dynamics over different ecosystems, including protected or conservation sites. The aim of this study is to use contemporary technologies such as EO and GIS in synergy with fragmentation analysis, to quantify the changes in the landscape of the Rajaji National Park (RNP) during the period of 19years (1990-2009). Several statistics such as principal component analysis (PCA) and spatial metrics are used to understand the results. PCA analysis has produced two principal components (PC) and explained 84.1% of the total variance, first component (PC1) accounted for the 57.8% of the total variance while the second component (PC2) has accounted for the 26.3% of the total variance calculated from the core area metrics, distance metrics and shape metrics. Our results suggested that notable changes happened in the RNP landscape, evidencing the requirement of taking appropriate measures to conserve this natural ecosystem.
C1 [Singh, Sudhir Kumar] Univ Allahabad, Nehru Sci Ctr, IIDS, K Banerjee Ctr Atmospher & Ocean Studies, Allahabad, Uttar Pradesh, India.
[Srivastava, Prashant K.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Srivastava, Prashant K.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Srivastava, Prashant K.] Banaras Hindu Univ, Inst Environm & Sustainable Dev, Varanasi, Uttar Pradesh, India.
[Szabo, Szilard] Univ Debrecen, Dept Phys Geog & Geoinformat, Debrecen, Hungary.
[Petropoulos, George P.] Aberystwyth Univ, Dept Geog & Earth Sci, Aberystwyth, Dyfed, Wales.
[Gupta, Manika] Indian Inst Technol, Dept Civil Engn, New Delhi, India.
[Islam, Tanvir] NOAA NESDIS Ctr Satellite Applicat & Res, College Pk, MD USA.
[Islam, Tanvir] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA.
RP Srivastava, PK (reprint author), NASA Goddard Space Flight Ctr, Greenbelt, MD USA.; Srivastava, PK (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.; Srivastava, PK (reprint author), Banaras Hindu Univ, Inst Environm & Sustainable Dev, Varanasi, Uttar Pradesh, India.
EM prashant.k.srivastava@nasa.gov
FU K. Banerjee, Centre of Atmospheric and Ocean Studies, IIDS, Nehru
Science Centre, University of Allahabad, Allahabad, India
FX This research work is supported by K. Banerjee, Centre of Atmospheric
and Ocean Studies, IIDS, Nehru Science Centre, University of Allahabad,
Allahabad, India. Authors also thank USGS
(http://www.usgs.gov/pubprod/aerial.html#satellite) for providing the
Landsat satellite data-sets. The views expressed here are those of the
authors solely and do not constitute a statement of policy, decision, or
position on behalf of NOAA/NASA or the authors' affiliated institutions.
NR 60
TC 1
Z9 1
U1 18
U2 18
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND
SN 1010-6049
EI 1752-0762
J9 GEOCARTO INT
JI Geocarto Int.
PY 2017
VL 32
IS 2
BP 113
EP 127
DI 10.1080/10106049.2015.1130084
PG 15
WC Environmental Sciences; Geosciences, Multidisciplinary; Remote Sensing;
Imaging Science & Photographic Technology
SC Environmental Sciences & Ecology; Geology; Remote Sensing; Imaging
Science & Photographic Technology
GA EF5QI
UT WOS:000390384300001
ER
PT J
AU Liu, JB
Kummerow, CD
Elsaesser, GS
AF Liu, Jianbo
Kummerow, Christian D.
Elsaesser, Gregory S.
TI Identifying and analysing uncertainty structures in the TRMM microwave
imager precipitation product over tropical ocean basins
SO INTERNATIONAL JOURNAL OF REMOTE SENSING
LA English
DT Article
ID RAIN-PROFILING ALGORITHM; MEASURING MISSION TRMM; RETRIEVAL ALGORITHM;
RADAR; ERROR; CONVECTION; MODEL; RADIOMETRY; AIRBORNE; REGIMES
AB Despite continuous improvements in microwave sensors and retrieval algorithms, our understanding of precipitation uncertainty is quite limited, due primarily to inconsistent findings in studies that compare satellite estimates to in situ observations over different parts of the world. This study seeks to characterize the temporal and spatial properties of uncertainty in the Tropical Rainfall Measuring Mission Microwave Imager surface rainfall product over tropical ocean basins. Two uncertainty analysis frameworks are introduced to qualitatively evaluate the properties of uncertainty under a hierarchy of spatiotemporal data resolutions. The first framework (i.e. 'climate method') demonstrates that, apart from random errors and regionally dependent biases, a large component of the overall precipitation uncertainty is manifested in cyclical patterns that are closely related to large-scale atmospheric modes of variability. By estimating the magnitudes of major uncertainty sources independently, the climate method is able to explain 45-88% of the monthly uncertainty variability. The percentage is largely resolution dependent (with the lowest percentage explained associated with a 1 degrees x 1 degrees spatial/1 month temporal resolution, and highest associated with a 3 degrees x 3 degrees spatial/3 month temporal resolution). The second framework (i.e. 'weather method') explains regional mean precipitation uncertainty as a summation of uncertainties associated with individual precipitation systems. By further assuming that self-similar recurring precipitation systems yield qualitatively comparable precipitation uncertainties, the weather method can consistently resolve about 50% of the daily uncertainty variability, with only limited dependence on the regions of interest.
C1 [Liu, Jianbo; Kummerow, Christian D.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Elsaesser, Gregory S.] Columbia Univ, NASA Goddard Inst Space Studies, New York, NY USA.
[Elsaesser, Gregory S.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA.
RP Liu, JB (reprint author), Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
EM jianbo@atmos.colostate.edu
FU NOAA National Centers for Environmental Information [NA14OAR4320125]
FX This work was supported by the NOAA National Centers for Environmental
Information [Grant Number: NA14OAR4320125].
NR 43
TC 1
Z9 1
U1 5
U2 5
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND
SN 0143-1161
EI 1366-5901
J9 INT J REMOTE SENS
JI Int. J. Remote Sens.
PY 2017
VL 38
IS 1
BP 23
EP 42
DI 10.1080/01431161.2016.1259676
PG 20
WC Remote Sensing; Imaging Science & Photographic Technology
SC Remote Sensing; Imaging Science & Photographic Technology
GA EF2AI
UT WOS:000390126200002
ER
PT J
AU Kim, D
Chin, M
Remer, LA
Diehl, T
Bian, HS
Yu, HB
Brown, ME
Stockwell, WR
AF Kim, Dongchul
Chin, Mian
Remer, Lorraine A.
Diehl, Thomas
Bian, Huisheng
Yu, Hongbin
Brown, Molly E.
Stockwell, William R.
TI Role of surface wind and vegetation cover in multi-decadal variations of
dust emission in the Sahara and Sahel
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Dust emission; Surface wind; NDVI; GOCART model; North Africa; Sahel
ID CONVECTION-PERMITTING SIMULATIONS; ATLANTIC CLIMATE VARIABILITY; DESERT
DUST; GOCART MODEL; MINERAL DUST; AFRICAN DUST; CIRCULATION PATTERNS;
NORTHERN-HEMISPHERE; AEROSOL VARIATIONS; WEATHER ANOMALIES
AB North Africa, the world's largest dust source, is non-uniform, consisting of a permanently arid region (Sahara), a semi-arid region (Sahel), and a relatively moist vegetated region (Savanna), each with very different rainfall patterns and surface conditions. This study aims to better understand the controlling factors that determine the variation of dust emission in North Africa over a 27-year period from 1982 to 2008, using observational data and model simulations. The results show that the model-derived Saharan dust emission is only correlated with the 10-rn winds (W10m) obtained from reanalysis data, but the model-derived Sahel dust emission is correlated with both W10m and the Normalized Difference Vegetation Index (NDVI) that is obtained from satellite. While the Saharan dust accounts for 82% of the continental North Africa dust emission (1340-1570 Tg year in the 27-year average, the Sahel accounts for 17% with a larger seasonal and inter-annual variation (230-380 Tg year(-1)), contributing about a quarter of the transatlantic dust transported to the northern part of South America. The decreasing dust emission trend over the 27-year period is highly correlated with W10m over the Sahara (R = 0.92). Over the Sahel, the dust emission is correlated with WIOm (R = 0.69) but is also anti-correlated with the trend of NDVI (R =-0.65). WIOm is decreasing over both the Sahara and the Sahel between 1982 and 2008, and the trends are correlated (R = 0.53), suggesting that Saharan/Sahelian surface winds are a coupled system, driving the inter-annual variation of dust emission. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Kim, Dongchul; Diehl, Thomas] Univ Space Res Assoc, Columbia, MD 21046 USA.
[Kim, Dongchul; Chin, Mian; Diehl, Thomas; Bian, Huisheng; Yu, Hongbin; Brown, Molly E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Remer, Lorraine A.; Bian, Huisheng] JCET UMBC, Baltimore, MD USA.
[Yu, Hongbin; Brown, Molly E.] Univ Maryland, College Pk, MD 20742 USA.
[Stockwell, William R.] Howard Univ, Washington, DC 20059 USA.
[Diehl, Thomas] European Commiss, Joint Res Ctr, Ispra, Italy.
RP Kim, D (reprint author), Univ Space Res Assoc, Columbia, MD 21046 USA.
EM dongchul.kim@nasa.gov
RI Yu, Hongbin/C-6485-2008
OI Yu, Hongbin/0000-0003-4706-1575
FU NASA Modeling, Analysis and Prediction (MAP); EOS Programs [NNX11AH66G];
National Aeronautics and Space Administration; National Oceanic and
Atmospheric Administration
FX This work is supported by NASA Modeling, Analysis and Prediction (MAP)
and EOS Programs (NNX11AH66G). We would like to thank the MISR, MODIS,
and AERONET team for the data used in this study. William Stockwell
thanks the National Aeronautics and Space Administration for the grant
"Howard University Beltsville Center for Climate System Observation" and
a grant from the National Oceanic and Atmospheric Administration to
Howard University's NOAA Center for Atmospheric Sciences for supporting
his participation in this work.
NR 83
TC 0
Z9 0
U1 15
U2 15
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
EI 1873-2844
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD JAN
PY 2017
VL 148
BP 282
EP 296
DI 10.1016/j.atmosenv.2016.10.051
PG 15
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA EE2DW
UT WOS:000389394900026
ER
PT J
AU Janka, O
Zaikina, JV
Bux, SK
Tabatabaifar, H
Yang, H
Browning, ND
Kauzlarich, SM
AF Janka, Oliver
Zaikina, Julia V.
Bux, Sabah K.
Tabatabaifar, Hosna
Yang, Hao
Browning, Nigel D.
Kauzlarich, Susan M.
TI Microstructure investigations of Yb- and Bi-doped Mg2Si prepared from
metal hydrides for thermoelectric applications
SO JOURNAL OF SOLID STATE CHEMISTRY
LA English
DT Article
DE Magnesium silicide; Thermoelectric materials; Ytterbium; Bismuth
ID SILICON; SEMICONDUCTORS; YTTERBIUM; SYSTEM; MGH2
AB Within the field of thermoelectric materials for energy conversion magnesium silicide, Mg2Si, is an outstanding candidate due to its low density, abundant constituents and low toxicity. However electronic and thermal tuning of the material is a required necessity to improve its Figure of Merit, zT. Doping of Yb via reactive YbH2 into the structure is performed with the goal of reducing the thermal conductivity. Hydrogen is released as a by-product at high temperatures allowing for facile incorporation of Yb into the structure. We report on the properties of Yb-and Bi-doped Mg2Si prepared with MgH2 and YbH2 with the focus on the synthetic conditions, and samples' microstructure, investigated by various electron microscopy techniques. Yb is found in the form of both Yb3Si5 inclusions and Yb dopant segregated at the grain boundary substituting for Mg. The addition of 1 at% Yb concentration reduced the thermal conductivity, providing a value of 30 mW/cm K at 800 K. In order to adjust carrier concentration, the sample is additionally doped with Bi. The impact of the microstructure on the transport properties of the obtained material is studied. Idealy, the reduction of the thermal conductivity is achieved by doping with Yb and the electronic transport is adjusted by doping with Bi. Large grain microstructure facilitates the electronic transport. However, the synthetic conditions that provide the optimized microstructure for electrical transport do not facilitate the additional Yb dopant incorporation. Therefore, the Yb and Bi containing sample with the optimized microstructure provides a zT=0.46 at 800 K.
C1 [Janka, Oliver; Zaikina, Julia V.; Tabatabaifar, Hosna; Kauzlarich, Susan M.] Univ Calif Davis, Dept Chem, One Shields Ave, Davis, CA 95616 USA.
[Bux, Sabah K.] CALTECH, Jet Prop Lab, Thermal Energy Convers Technol Grp, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
[Yang, Hao; Browning, Nigel D.] Pacific Northwest Natl Lab, Div Chem & Mat Sci, Richland, WA 99352 USA.
[Janka, Oliver] Westfalische Wilhelms Univ, Inst Anorgan & Analyt Chem, Corrensstr 28-30, D-48161 Munster, Germany.
RP Kauzlarich, SM (reprint author), Univ Calif Davis, Dept Chem, One Shields Ave, Davis, CA 95616 USA.
FU NSF/DOE Partnership [CBET-1048799, DMR-1405973]; UC Davis; Department of
Energy's Office of Biological and Environmental Research (DOE BER)
located at PNNL; Battelle Memorial Institute for the DOE
[DE-AC05-76RL01830]; NASA Science Missions Directorate's Radioisotope
Power Systems Thermoelectric Technology Development Project
FX We thank Greg Baxter for sample preparation for microprobe analysis and
Nick Botto for the measurements. We gratefully acknowledge financial
support from NSF/DOE Partnership CBET-1048799, DMR-1405973, and UC
Davis.; A portion of this research is part of the Chemical Imaging
Initiative conducted under the Laboratory Directed Research and
Development (LDRD) Program at Pacific Northwest National Laboratory
(PNNL) and was performed at the Environmental Molecular Sciences
Laboratory (EMSL), a national scientific user facility sponsored by the
Department of Energy's Office of Biological and Environmental Research
(DOE BER) located at PNNL, a multiprogram national laboratory operated
by Battelle Memorial Institute for the DOE under Contract
DE-AC05-76RL01830.; Part of this work was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. This
work supported by the NASA Science Missions Directorate's Radioisotope
Power Systems Thermoelectric Technology Development Project.
NR 33
TC 0
Z9 0
U1 16
U2 16
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0022-4596
EI 1095-726X
J9 J SOLID STATE CHEM
JI J. Solid State Chem.
PD JAN
PY 2017
VL 245
BP 152
EP 159
DI 10.1016/j.jssc.2016.10.011
PG 8
WC Chemistry, Inorganic & Nuclear; Chemistry, Physical
SC Chemistry
GA EE4IU
UT WOS:000389566300021
ER
PT J
AU Yoon, J
Lee, J
Choi, B
Lee, D
Kim, DH
Kim, DM
Moon, DI
Lim, M
Kim, S
Choi, SJ
AF Yoon, Jinsu
Lee, Juhee
Choi, Bongsik
Lee, Dongil
Kim, Dae Hwan
Kim, Dong Myong
Moon, Dong-Il
Lim, Meehyun
Kim, Sungho
Choi, Sung-Jin
TI Flammable carbon nanotube transistors on a nitrocellulose paper
substrate for transient electronics
SO NANO RESEARCH
LA English
DT Article
DE carbon nanotube; paper substrate; flammable; transient; security
ID THIN-FILM TRANSISTORS; FUNCTIONAL TRANSFORMATION; INTEGRATED-CIRCUITS;
SILK FIBROIN; DEGRADATION; DEVICES; BIOCOMPATIBILITY; CHEMISTRY;
NETWORKS; TUNGSTEN
AB Transient electronics represent an emerging class of technology comprising materials that can vanish in a controlled manner in response to stimuli. In contrast to conventional electronic devices that are designed to operate over the longest possible period, transient electronics are defined by operation typically over a short and well-defined period; when no longer needed, transient electronics undergo self-deconstruction and disappear completely. In this work, we demonstrate the fabrication of thermally triggered transient electronic devices based on a paper substrate, specifically, a nitrocellulose paper. Nitrocellulose paper is frequently used in acts of magic because it consists of highly flammable components that are formed by nitrating cellulose by exposure to nitric acid. Therefore, a complete and rapid destruction of electronic devices fabricated on nitrocellulose paper is possible without producing any residue (i.e., ash). The transience rates can be modified by controlling radio frequency signal-induced voltages that are applied to a silver (Ag) resistive heater, which is stamped on the backside of the nitrocellulose paper. The Ag resistive heater was prepared by a simple, low-cost stamping fabrication, which requires no harsh chemicals or complex thermal treatments. For the electronics on the nitrocellulose paper substrate, we employed semiconducting carbon nanotube (CNT) network channels in the transistor for superior electrical and mechanical properties.
C1 [Yoon, Jinsu; Lee, Juhee; Choi, Bongsik; Kim, Dae Hwan; Kim, Dong Myong; Choi, Sung-Jin] Kookmin Univ, Sch Elect Engn, Seoul 02707, South Korea.
[Lee, Dongil] Korea Adv Inst Sci & Technol, Sch Elect Engn, Daejeon 34141, South Korea.
[Moon, Dong-Il] NASA Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
[Lim, Meehyun] Mech R&D Ctr, Samsung Elect, Test&Package Technol Grp, Gyeonggi Do 18448, South Korea.
[Kim, Sungho] Sejong Univ, Dept Elect Engn, Seoul 05006, South Korea.
RP Choi, SJ (reprint author), Kookmin Univ, Sch Elect Engn, Seoul 02707, South Korea.; Kim, S (reprint author), Sejong Univ, Dept Elect Engn, Seoul 05006, South Korea.
EM sungho85kim@sejong.ac.kr; sjchoiee@kookmin.ac.kr
FU National Research Foundation of Korea through the Ministry of Education,
Science and Technology, Korean Government [2013R1A1A1057870,
2016R1A2B4011366]; [2016R1A5A1012966]
FX The work was supported by the National Research Foundation of Korea
through the Ministry of Education, Science and Technology, Korean
Government (Nos. 2013R1A1A1057870 and 2016R1A2B4011366) and partially
supported by No. 2016R1A5A1012966. We thank Professor Jeffrey Bokor for
useful discussions.
NR 42
TC 0
Z9 0
U1 10
U2 10
PU TSINGHUA UNIV PRESS
PI BEIJING
PA TSINGHUA UNIV, RM A703, XUEYAN BLDG, BEIJING, 100084, PEOPLES R CHINA
SN 1998-0124
EI 1998-0000
J9 NANO RES
JI Nano Res.
PD JAN
PY 2017
VL 10
IS 1
BP 87
EP 96
DI 10.1007/s12274-016-1268-6
PG 10
WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science,
Multidisciplinary; Physics, Applied
SC Chemistry; Science & Technology - Other Topics; Materials Science;
Physics
GA EF1DT
UT WOS:000390066000008
ER
PT J
AU Singh, MK
Gautam, R
Gatebe, CK
Poudyal, R
AF Singh, Manoj K.
Gautam, Ritesh
Gatebe, Charles K.
Poudyal, Rajesh
TI PolarBRDF: A general purpose Python package for visualization and
quantitative analysis of multi-angular remote sensing measurements (vol
96, pg 173, 2016)
SO COMPUTERS & GEOSCIENCES
LA English
DT Correction
C1 [Singh, Manoj K.; Gautam, Ritesh] Indian Inst Technol, Ctr Studies Resources Engn, Bombay 400076, Maharashtra, India.
[Gautam, Ritesh] Indian Inst Technol, Interdisciplinary Program Climate Studies, Mumbai 400076, Maharashtra, India.
[Gatebe, Charles K.] Univ Space Res Assoc, Columbia, MD 21046 USA.
[Gatebe, Charles K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Poudyal, Rajesh] Sci Syst & Applicat Inc, Lanham, MD USA.
RP Singh, MK; Gautam, R (reprint author), Indian Inst Technol, Ctr Studies Resources Engn, Bombay 400076, Maharashtra, India.; Gautam, R (reprint author), Indian Inst Technol, Interdisciplinary Program Climate Studies, Mumbai 400076, Maharashtra, India.; Gatebe, CK (reprint author), Univ Space Res Assoc, Columbia, MD 21046 USA.; Gatebe, CK (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM manojks@iitb.ac.in
NR 1
TC 0
Z9 0
U1 6
U2 6
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0098-3004
EI 1873-7803
J9 COMPUT GEOSCI-UK
JI Comput. Geosci.
PD JAN
PY 2017
VL 98
BP 93
EP 93
DI 10.1016/j.cageo.2016.09.012
PG 1
WC Computer Science, Interdisciplinary Applications; Geosciences,
Multidisciplinary
SC Computer Science; Geology
GA EE0UL
UT WOS:000389294300011
ER
PT J
AU Glaze, LS
Self, S
Schmidt, A
Hunter, SJ
AF Glaze, Lori S.
Self, Stephen
Schmidt, Anja
Hunter, Stephen J.
TI Assessing eruption column height in ancient flood basalt eruptions
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE flood basalt; climate; Roza; sulfur dioxide; Columbia River Basalt
Group; plume heights
ID LARGE IGNEOUS PROVINCES; 1783-1784 LAKI ERUPTION; FISSURE ERUPTIONS;
EXPLOSIVE VOLCANISM; MASS EXTINCTIONS; SULFATE AEROSOL; KILAUEA VOLCANO;
CLIMATE MODEL; SKAFTAR-FIRES; PLUME HEIGHTS
AB A buoyant plume model is used to explore the ability of flood basalt eruptions to inject climate-relevant gases into the stratosphere. An example from the 1986 Izu-Oshima basaltic fissure eruption validates the model's ability to reproduce the observed maximum plume heights of 12-16 km above sea level, sustained above fire-fountains. The model predicts maximum plume heights of 13-17 km for source widths of between 4-16 m when 32% (by mass) of the erupted magma is fragmented and involved in the buoyant plume (effective volatile content of 6 wt%). Assuming that the Miocene-age Roza eruption (part of the Columbia River Basalt Group) sustained fire-fountains of similar height to Izu-Oshima (1.6 km above the vent), we show that the Roza eruption could have sustained buoyant ash and gas plumes that extended into the stratosphere at similar to 45 degrees N. Assuming 5 km long active fissure segments and 9000 Mt of SO2 released during explosive phases over a 10-15 year duration; the similar to 180 km of known Roza fissure length could have supported similar to 36 explosive events/phases, each with a duration of 3-4 days. Each 5 km fissure segment could have emitted 62 Mt of SO2 per day into the stratosphere while actively fountaining, the equivalent of about three 1991 Mount Pinatubo eruptions per day. Each fissure segment could have had one to several vents, which subsequently produced lava without significant fountaining for a longer period within the decades-long eruption. Sensitivity of plume rise height to ancient atmospheric conditions is explored. Although eruptions in the Deccan Traps (similar to 66 Ma) may have generated buoyant plumes that rose to altitudes in excess of 18 km, they may not have reached the stratosphere because the tropopause was substantially higher in the late Cretaceous. Our results indicate that some flood basalt eruptions, such as Roza, were capable of repeatedly injecting large masses of SO2 into the stratosphere. Thus sustained flood basalt eruptions could have influenced climate on time scales of decades to centuries but the location (i.e., latitude) of the province and relevant paleoclimate is important and must be considered. (C) 2016 Published by Elsevier B.V.
C1 [Glaze, Lori S.] NASA, Goddard Space Flight Ctr, Code 690,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Self, Stephen] Open Univ, Dept Environm Earth & Ecosyst, Walton Hall, Milton Keynes MK7 6AA, Bucks, England.
[Self, Stephen] Univ Calif Berkeley, Earth & Planetary Sci, 307 McCone Hall, Berkeley, CA 94720 USA.
[Schmidt, Anja; Hunter, Stephen J.] Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England.
RP Glaze, LS (reprint author), NASA, Goddard Space Flight Ctr, Code 690,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM Lori.S.Glaze@nasa.gov; Steve.self1815@gmail.com; A.Schmidt@leeds.ac.uk;
S.Hunter@leeds.ac.uk
RI Glaze, Lori/D-1314-2012;
OI Schmidt, Anja/0000-0001-8759-2843
FU NASA Planetary Geology and Geophysics [WBS 811073.02.01.05.80]; UK-NERC
research grants [NER/B/S/2003/00246, GR3/11474]; Academic Research
Fellowship from the School of Earth and Environment, University Of
Leeds; European Research Council under the European Union's Seventh
Framework Programme (FP7)/ERC [278636]
FX L. Glaze was funded by NASA Planetary Geology and Geophysics (WBS
811073.02.01.05.80) and S. Self was funded by UK-NERC research grants
NER/B/S/2003/00246 and GR3/11474 for part of this research. A. Schmidt
was funded by an Academic Research Fellowship from the School of Earth
and Environment, University Of Leeds. S. Hunter is funded by the
European Research Council under the European Union's Seventh Framework
Programme (FP7/2007-2013)/ERC grant agreement no. 278636. We thank Steve
Baloga and Luke Oman for providing comments on an early version of this
manuscript, and Tim Elliott, Laszlo Kestay, and two anonymous reviewers
for providing constructive reviews.
NR 70
TC 2
Z9 2
U1 5
U2 5
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
EI 1385-013X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD JAN 1
PY 2017
VL 457
BP 263
EP 270
DI 10.1016/j.epsl.2014.07.043
PG 8
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EE2FB
UT WOS:000389398000024
ER
PT J
AU Zoogman, P
Liu, X
Suleiman, RM
Pennington, WF
Flittner, DE
Al-Saadi, JA
Hilton, BB
Nicks, DK
Newchurch, MJ
Carr, JL
Janz, SJ
Andraschko, MR
Arola, A
Baker, BD
Canova, BP
Miller, CC
Cohen, RC
Davis, JE
Dussault, ME
Edwards, DP
Fishman, J
Ghulam, A
Abad, GG
Grutter, M
Herman, JR
Houck, J
Jacob, DJ
Joiner, J
Kerridge, BJ
Kim, J
Krotkov, NA
Lamsal, L
Li, C
Lindfors, A
Martin, RV
McElroy, CT
McLinden, C
Natraj, V
Neil, DO
Nowlan, CR
O'Sullivan, EJ
Palmer, PI
Pierce, RB
Pippin, MR
Saiz-Lopez, A
Spurr, RJD
Szykman, JJ
Torres, O
Veefkind, JP
Veihelmann, B
Wang, H
Wang, J
Chance, K
AF Zoogman, P.
Liu, X.
Suleiman, R. M.
Pennington, W. F.
Flittner, D. E.
Al-Saadi, J. A.
Hilton, B. B.
Nicks, D. K.
Newchurch, M. J.
Carr, J. L.
Janz, S. J.
Andraschko, M. R.
Arola, A.
Baker, B. D.
Canova, B. P.
Miller, C. Chan
Cohen, R. C.
Davis, J. E.
Dussault, M. E.
Edwards, D. P.
Fishman, J.
Ghulam, A.
Abad, G. Gonzalez
Grutter, M.
Herman, J. R.
Houck, J.
Jacob, D. J.
Joiner, J.
Kerridge, B. J.
Kim, J.
Krotkov, N. A.
Lamsal, L.
Li, C.
Lindfors, A.
Martin, R. V.
McElroy, C. T.
McLinden, C.
Natraj, V.
Neil, D. O.
Nowlan, C. R.
O'Sullivan, E. J.
Palmer, P. I.
Pierce, R. B.
Pippin, M. R.
Saiz-Lopez, A.
Spurr, R. J. D.
Szykman, J. J.
Torres, O.
Veefkind, J. P.
Veihelmann, B.
Wang, H.
Wang, J.
Chance, K.
TI Tropospheric emissions: Monitoring of pollution (TEMPO)
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
ID ROTATIONAL RAMAN-SCATTERING; BACKSCATTER ULTRAVIOLET MEASUREMENTS; OZONE
PROFILE RETRIEVALS; SURFACE UV IRRADIANCE; SATELLITE-OBSERVATIONS;
AIR-QUALITY; NO2 RETRIEVAL; FORMALDEHYDE COLUMNS; GLOBAL OBSERVATIONS;
NORTH-AMERICA
AB TEMPO was selected in 2012 by NASA as the first Earth Venture Instrument, for launch between 2018 and 2021. It will measure atmospheric pollution for greater North America from space using ultraviolet and visible spectroscopy. TEMPO observes from Mexico City, Cuba, and the Bahamas to the Canadian oil sands, and from the Atlantic to the Pacific, hourly and at high spatial resolution (similar to 2.1 km N/S x 4.4 km E/W at 36.5 degrees N, 100 degrees W). TEMPO provides a tropospheric measurement suite that includes the key elements of tropospheric air pollution chemistry, as well as contributing to carbon cycle knowledge. Measurements are made hourly from geostationary (GEO) orbit, to capture the high variability present in the diurnal cycle of emissions and chemistry that are unobservable from current low-Earth orbit (LEO) satellites that measure once per day. The small product spatial footprint resolves pollution sources at sub-urban scale. Together, this temporal and spatial resolution improves emission inventories, monitors population exposure, and enables effective emission-control strategies.
TEMPO takes advantage of a commercial GEO host spacecraft to provide a modest cost mission that measures the spectra required to retrieve ozone (O-3), nitrogen dioxide (NO2), sulfur dioxide (SO2), formaldehyde (H2CO), glyoxal (C2H2O2), bromine monoxide (BrO), IO (iodine monoxide), water vapor, aerosols, cloud parameters, ultraviolet radiation, and foliage properties. TEMPO thus measures the major elements, directly or by proxy, in the tropospheric O-3 chemistry cycle. Multi-spectral observations provide sensitivity to O-3 in the lowermost troposphere, substantially reducing uncertainty in air quality predictions. TEMPO quantifies and tracks the evolution of aerosol loading. It provides these near-realtime air quality products that will be made publicly available. TEMPO will launch at a prime time to be the North American component of the global geostationary constellation of pollution monitoring together with the European Sentinel-4 (S4) and Korean Geostationary Environment Monitoring Spectrometer (GEMS) instruments. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Zoogman, P.; Liu, X.; Suleiman, R. M.; Davis, J. E.; Dussault, M. E.; Abad, G. Gonzalez; Houck, J.; Martin, R. V.; Nowlan, C. R.; O'Sullivan, E. J.; Wang, H.; Chance, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Pennington, W. F.; Flittner, D. E.; Al-Saadi, J. A.; Hilton, B. B.; Andraschko, M. R.; Neil, D. O.; Pippin, M. R.] NASA, Langley Res Ctr, Hampton, VA USA.
[Nicks, D. K.; Baker, B. D.; Canova, B. P.] Ball Aerosp & Technol Corp, Boulder, CO USA.
[Newchurch, M. J.] Univ Alabama, Huntsville, AL USA.
[Carr, J. L.] Carr Astronaut, Greenbelt, MD USA.
[Janz, S. J.; Joiner, J.; Krotkov, N. A.; Lamsal, L.; Torres, O.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Arola, A.; Lindfors, A.] Finnish Meteorol Inst, Helsinki, Finland.
[Miller, C. Chan; Jacob, D. J.] Harvard Univ, Cambridge, MA 02138 USA.
[Cohen, R. C.] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Edwards, D. P.] Natl Ctr Atmospher Res, Boulder, CO USA.
[Fishman, J.; Ghulam, A.] St Louis Univ, St Louis, MO 63103 USA.
[Grutter, M.] Univ Nacl Autonoma Mexico, Mexico City 04510, DF, Mexico.
[Herman, J. R.] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA.
[Kerridge, B. J.] Rutherford Appleton Lab, Chilton, Oxon, England.
[Kim, J.] Yonsei Univ, Seoul 120749, South Korea.
[Lamsal, L.] Univ Space Res Assoc, GESTAR, Greenbelt, MD USA.
[Martin, R. V.] Dalhousie Univ, Halifax, NS B3H 3J5, Canada.
[McElroy, C. T.] York Univ, N York, ON M3J 1P3, Canada.
[McLinden, C.] Environm & Climate Change Canada, Gatineau, PQ, Canada.
[Natraj, V.] NASA, Jet Prop Lab, Pasadena, CA USA.
[Palmer, P. I.] Univ Edinburgh, Edinburgh EH8 9YL, Midlothian, Scotland.
[Pierce, R. B.] NOAA, Silver Spring, MD USA.
[Saiz-Lopez, A.] CSIC, Inst Quim Fis Rocasolano, Madrid, Spain.
[Spurr, R. J. D.] RT Solut Inc, Cambridge, MA USA.
[Szykman, J. J.] US EPA, Washington, DC USA.
[Veefkind, J. P.] Koninklijk Nederlands Meteorolog Inst, De Bilt, Netherlands.
[Veihelmann, B.] European Space Agcy, F-75738 Paris 15, France.
[Wang, J.] Univ Nebraska, Lincoln, NE 68583 USA.
RP Zoogman, P (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RI Cohen, Ronald/A-8842-2011; Saiz-Lopez, Alfonso/B-3759-2015; Lindfors,
Anders/C-6727-2012; Wang, Jun/A-2977-2008;
OI Cohen, Ronald/0000-0001-6617-7691; Saiz-Lopez,
Alfonso/0000-0002-0060-1581; Wang, Jun/0000-0002-7334-0490; Gonzalez
Abad, Gonzalo/0000-0002-8090-6480; Arola, Antti/0000-0002-9220-0194
NR 129
TC 4
Z9 4
U1 27
U2 27
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD JAN
PY 2017
VL 186
SI SI
BP 17
EP 39
DI 10.1016/j.jqsrt.2016.05.008
PG 23
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA ED7BP
UT WOS:000389011000003
ER
PT J
AU Sheese, PE
Walker, KA
Boone, CD
Bernath, PF
Froidevaux, L
Funke, B
Raspollini, P
von Clarmann, T
AF Sheese, Patrick E.
Walker, Kaley A.
Boone, Chris D.
Bernath, Peter F.
Froidevaux, Lucien
Funke, Bernd
Raspollini, Piera
von Clarmann, Thomas
TI ACE-FTS ozone, water vapour, nitrous oxide, nitric acid, and carbon
monoxide profile comparisons with MIPAS and MLS
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE ACE-FIE; MIPAS; MLS; Profile comparison; Stratospheric and mesospheric
trace gases; Satellite limb sounding
ID FOURIER-TRANSFORM SPECTROMETER; VALIDATION; RETRIEVAL; N2O; INSTRUMENT;
SATELLITE; CLONO2; HNO3
AB The atmospheric limb sounders, ACE-FTS on the SCISAT satellite, MIPAS on ESA's Envisat satellite, and MLS on NASA's Aura satellite, take measurements used to retrieve atmospheric profiles of O-3, N2O, H2O, HNO3, and CO. Each was taking measurements between February 2004 and April 2012 (ACE-FTS and MLS are currently operational), providing hundreds of profile coincidences in the Northern and Southern hemispheres, and during local morning and evening. Focusing on determining diurnal and hemispheric biases in the ACE-FTS data, this study compares ACE-FTS version 3.5 profiles that are collocated with MIPAS and MLS, and analyzes the differences between instrument retrievals for Northern and Southern hemispheres and for local morning and evening data. For O-3, ACE-FTS is typically within 5% of mid-stratospheric MIPAS and MLS data and exhibits a positive bias of similar to 10 to 20% in the upper stratosphere - lower mesosphere. For H2O, ACEFTS exhibits an average bias of 5% between 20 and 60 km. For N2O, ACE-FTS agrees with MIPAS and MLS within 20 to +10% up to 45 km and 35 km, respectively. For HNO3, ACEFTS typically agrees within +/- 10% below 30 km, and exhibits a positive bias of similar to 10 to 20% above 30 km. With respect to MIPAS CO, ACE-FTS exhibits an average - 11% bias between 28 and 50 km, and at higher altitudes a positive bias on the order of 10% ( > 100%) in the winter (summer). With respect to winter MLS CO, ACE-FTS is typically within 10% between 25 and 40 km, and has an average bias of - 11% above 40 km. (C) 2016 Elsevier Ltd. All rights reserved:
C1 [Sheese, Patrick E.; Walker, Kaley A.] Univ Toronto, Dept Phys, 60 St George St, Toronto, ON M5S 1A7, Canada.
[Walker, Kaley A.; Boone, Chris D.] Univ Waterloo, Dept Chem, 200 Univ Ave W, Waterloo, ON N2L 3G1, Canada.
[Bernath, Peter F.] Old Dominion Univ, Dept Chem & Biochem, 4541 Hampton Blvd, Norfolk, VA 23529 USA.
[Froidevaux, Lucien] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Funke, Bernd] CSIC, Inst Astrofis Andalucia, Apartado 3004, E-18080 Granada, Spain.
[Raspollini, Piera] CNR, Inst Appl Phys Nello Carrara, Via Madonna del Piano 10, I-50019 Florence, Italy.
[von Clarmann, Thomas] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, H v Helmholtz Pl 1, D-76344 Karlsruhe, Germany.
RP Walker, KA (reprint author), Univ Toronto, Dept Phys, 60 St George St, Toronto, ON M5S 1A7, Canada.
EM kwalker@atmosp.physics.utoronto.ca
RI Funke, Bernd/C-2162-2008
OI Funke, Bernd/0000-0003-0462-4702
NR 24
TC 2
Z9 2
U1 7
U2 7
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD JAN
PY 2017
VL 186
SI SI
BP 63
EP 80
DI 10.1016/j.jqsrt.2016.06.026
PG 18
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA ED7BP
UT WOS:000389011000006
ER
PT J
AU Mahieu, E
Lejeune, B
Bovy, B
Servais, C
Toon, GC
Bernath, PF
Boone, CD
Walker, KA
Reimann, S
Vollmer, MK
O'Doherty, S
AF Mahieu, Emmanuel
Lejeune, Bernard
Bovy, Benoit
Servais, Christian
Toon, Geoffrey C.
Bernath, Peter F.
Boone, Christopher D.
Walker, Kaley A.
Reimann, Stefan
Vollmer, Martin K.
O'Doherty, Simon
TI Retrieval of HCFC-142b (CH3CClF2) from ground-based high-resolution
infrared solar spectra: Atmospheric increase since 1989 and comparison
with surface and satellite measurements
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE HCFC-142b; FTIR spectroscopy; Jungfraujoch; NDACC; ACE-FTS; AGAGE
ID MAX-DOAS OBSERVATIONS; IN-SITU; JUNGFRAUJOCH STATION; FTIR; TRENDS;
SPECTROSCOPY; FORMALDEHYDE; NETWORK; VAPOR; CO
AB We have developed an approach for retrieving HCFC-142b (CH3CCLF2) from ground-based high-resolution infrared solar spectra, using its v(7) band Q branch in the 900-906 cm(-1) interval. Interferences by HNO3, CO2 and H2O have to be accounted for. Application of this approach to observations recorded within the framework of long-term monitoring activities carried out at the northern mid-latitude, high-altitude Jungfraujoch station in Switzerland (46.5 degrees N, 8.0 degrees E, 3580 m above sea level) has provided a total column times series spanning the 1989 to mid-2015 time period. A fit to the HCFC-142b daily mean total column time series shows a statistically-significant long-term trend of (1.23 +/- 0.08 x 10(13) molec cm(-2)) per year from 2000 to 2010, at the 2-sigma confidence level. This corresponds to a significant atmospheric accumulation of (0.94 +/- 0.06) ppt (1 ppt =1/10(12)) per year for the mean tropospheric mixing ratio, at the 2-sigma confidence level. Over the subsequent time period (2010-2014), we note a significant slowing down in the HCFC-142b buildup. Our ground-based FTIR (Fourier Transform Infrared) results are compared with relevant data sets derived from surface in situ measurements at the Mace Head and Jungfraujoch sites of the AGAGE (Advanced Global Atmospheric Gases Experiment) network and from occultation measurements by the ACE-FTS (Atmospheric Chemistry Experiment-Fourier Transform Spectrometer) instrument on-board the SCISAT satellite. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Mahieu, Emmanuel; Lejeune, Bernard; Bovy, Benoit; Servais, Christian] Univ Liege, Inst Astrophys & Geophys, Liege, Belgium.
[Toon, Geoffrey C.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Bernath, Peter F.] Old Dominion Univ, Dept Chem & Biochem, Norfolk, VA USA.
[Boone, Christopher D.] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada.
[Walker, Kaley A.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A1, Canada.
[Reimann, Stefan; Vollmer, Martin K.] Swiss Fed Labs Mat Sci & Technol, Lab Air Pollut & Environm Technol, Empa, Dubendorf, Switzerland.
[O'Doherty, Simon] Univ Bristol, Sch Chem, Bristol BS8 1TH, Avon, England.
RP Mahieu, E (reprint author), Univ Liege Quartier Agora, Inst Astrophys & Geophys, Allee Six Aout 19, B-4000 Liege, Sart Tilman, Belgium.
EM emmanuel.mahieu@ulg.ac.be
RI Reimann, Stefan/A-2327-2009;
OI Reimann, Stefan/0000-0002-9885-7138; Mahieu,
Emmanuel/0000-0002-5251-0286
NR 38
TC 0
Z9 0
U1 7
U2 7
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD JAN
PY 2017
VL 186
SI SI
BP 96
EP 105
DI 10.1016/j.jqsrt.2016.03.017
PG 10
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA ED7BP
UT WOS:000389011000008
ER
PT J
AU Hashemi, R
Predoi-Cross, A
Nikitin, AV
Tyuterev, VG
Sung, K
Smith, MAH
Devi, VM
AF Hashemi, R.
Predoi-Cross, A.
Nikitin, A. V.
Tyuterev, Vi. G.
Sung, K.
Smith, M. A. H.
Devi, V. Malathy
TI Spectroscopic line parameters of (CH4)-C-12 for atmospheric composition
retrievals in the 4300-4500 cm(-1) region
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Methane; CH4-CH4 & CH4-air half-width coefficient; Relaxation matrix
coefficients; CH4-air & CH4-CH4 shift coefficient
ID PRESSURE-SHIFT COEFFICIENTS; DIODE-LASER MEASUREMENTS; LORENTZ
BROADENING COEFFICIENTS; MULTISPECTRUM ANALYSIS; HALF-WIDTHS; MU-M;
TEMPERATURE DEPENDENCES; MIXING COEFFICIENTS; FITTING TECHNIQUE;
SPECTRAL REGION
AB Due to the importance of methane as a trace atmospheric gas and a greenhouse gas, we have carried out a precise line-shape study to obtain the CH4-CH4 and CH4-air half-width coefficients, CH4-CH4 and CH4-air shift coefficients and off-diagonal relaxation matrix element coefficients for methane transitions in the spectral range known as the "methane Octad". In addition, the associated temperature dependences of these coefficients have been measured in the 4300-4500 cm(-1) region of the Octad. The high signal to noise ratio spectra of pure methane and of dilute mixtures of methane in dry air with high resolution have been recorded at temperatures from 148 K to room temperature using the Bruker IFS 125 HR Fourier transform spectrometer (FTS) at the Jet Propulsion Laboratory, Pasadena, California. The analysis of spectra was done using a multispectrum non-linear least squares curve fitting technique. Theoretical calculations have been performed and the results are compared with the previously published line positions, intensities and with the line parameters available in the GEISA and HITRAN2012 databases. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Hashemi, R.; Predoi-Cross, A.] Univ Lethbridge, Dept Phys & Astron, Lethbridge, AB T1K 3M4, Canada.
[Nikitin, A. V.] Tomsk State Univ, Russian Acad Sci, VE Zuev Inst Atmospher Opt, Lab Theoret Spect, Tomsk, Russia.
[Nikitin, A. V.] Tomsk State Univ, QUAMER Lab, Tomsk, Russia.
[Tyuterev, Vi. G.] Univ Reims, Grp Spectrometrie Mol & Atmospher, UMR CNRS 6089, UFR Sci, Reims 2, France.
[Sung, K.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Smith, M. A. H.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23665 USA.
[Devi, V. Malathy] Coll William & Mary, Dept Phys, Williamsburg, VA 23185 USA.
RP Hashemi, R (reprint author), Univ Lethbridge, Dept Phys & Astron, Lethbridge, AB T1K 3M4, Canada.
RI Nikitin, Andrei/K-2624-2013; Sung, Keeyoon/I-6533-2015
OI Nikitin, Andrei/0000-0002-4280-4096;
NR 60
TC 1
Z9 1
U1 5
U2 5
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD JAN
PY 2017
VL 186
SI SI
BP 106
EP 117
DI 10.1016/j.jqsrt.2016.03.024
PG 12
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA ED7BP
UT WOS:000389011000009
ER
PT J
AU Drouin, BJ
Benner, DC
Brown, LR
Cich, MJ
Crawford, TJ
Devi, VM
Guillaume, A
Hodges, JT
Mlawer, EJ
Robichaud, DJ
Oyafuso, F
Payne, VH
Sung, KY
Wishnow, EH
Yu, SS
AF Drouin, Brian J.
Benner, D. Chris
Brown, Linda R.
Cich, Matthew J.
Crawford, Timothy J.
Devi, V. Malathy
Guillaume, Alexander
Hodges, Joseph T.
Mlawer, Eli J.
Robichaud, David J.
Oyafuso, Fabiano
Payne, Vivienne H.
Sung, Keeyoon
Wishnow, Edward H.
Yu, Shanshan
TI Multispectrum analysis of the oxygen A-band
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Oxygen; Atmospheric absorption; Collision-induced absorption;
Multispectrum fitting; Spectral lineshapes
ID MOLECULAR SPECTROSCOPIC DATABASE; RING-DOWN SPECTROSCOPY;
FOURIER-TRANSFORM SPECTROMETER; CO2 RETRIEVAL ALGORITHM; LINE
PARAMETERS; MU-M; O-2; ABSORPTION; TRANSITIONS; INTENSITIES
AB Retrievals of atmospheric composition from near-infrared measurements require measurements of airmass to better than the desired precision of the composition. The oxygen bands are obvious choices to quantify airmass since the mixing ratio of oxygen is fixed over the full range of atmospheric conditions. The OCO-2 mission is currently retrieving carbon dioxide concentration using the oxygen A-band for airmass normalization. The 0.25% accuracy desired for the carbon dioxide concentration has pushed the required state-of-the-art for oxygen spectroscopy. To measure 02 A-band cross-sections with such accuracy through the full range of atmospheric pressure requires a sophisticated line shape model (Rautian or Speed-Dependent Voigt) with line mixing (LM) and collision induced absorption (CIA). Models of each of these phenomena exist, however, this work presents an integrated self-consistent model developed to ensure the best accuracy.
It is also important to consider multiple sources of spectroscopic data for such a study in order to improve the dynamic range of the model and to minimize effects of instrumentation and associated systematic errors. The techniques of Fourier Transform Spectroscopy (FTS) and Cavity Ring-Down Spectroscopy (CRDS) allow complimentary information for such an analysis. We utilize multispectrum fitting software to generate a comprehensive new database with improved accuracy based on these datasets. The extensive information will be made available as a multi-dimensional cross-section (ABSCO) table and the parameterization will be offered for inclusion in the HITRANonline database. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Drouin, Brian J.; Brown, Linda R.; Cich, Matthew J.; Crawford, Timothy J.; Guillaume, Alexander; Oyafuso, Fabiano; Payne, Vivienne H.; Sung, Keeyoon; Yu, Shanshan] CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Benner, D. Chris; Devi, V. Malathy] Coll William & Mary, Dept Phys, Williamsburg, VA 23185 USA.
[Hodges, Joseph T.] NIST, Mat Measurement Lab, 100 Bur Dr, Gaithersburg, MD 20899 USA.
[Mlawer, Eli J.] Atmospher & Environm Res, Lexington, MA USA.
[Robichaud, David J.] Natl Renewable Energy Lab, 15013 Denver West Pkwy, Golden, CO 80401 USA.
[Wishnow, Edward H.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Wishnow, Edward H.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
RP Drouin, BJ (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM brian.j.drouin@jpl.nasa.gov
RI Sung, Keeyoon/I-6533-2015; Yu, Shanshan/D-8733-2016
FU Intramural NIST DOC [9999-NIST]
NR 69
TC 0
Z9 0
U1 12
U2 12
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD JAN
PY 2017
VL 186
SI SI
BP 118
EP 138
DI 10.1016/j.jqsrt.2016.03.037
PG 21
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA ED7BP
UT WOS:000389011000010
PM 27840454
ER
PT J
AU Li, ZL
Hu, F
Schnase, JL
Duffy, DQ
Lee, T
Bowen, MK
Yang, CW
AF Li, Zhenlong
Hu, Fei
Schnase, John L.
Duffy, Daniel Q.
Lee, Tsengdar
Bowen, Michael K.
Yang, Chaowei
TI A spatiotemporal indexing approach for efficient processing of big
array-based climate data with MapReduce
SO INTERNATIONAL JOURNAL OF GEOGRAPHICAL INFORMATION SCIENCE
LA English
DT Article
DE Spatiotemporal index; big climate data; array-based; Hadoop MapReduce;
HDFS; NASA MERRA; climate change
AB Climate observations and model simulations are producing vast amounts of array-based spatiotemporal data. Efficient processing of these data is essential for assessing global challenges such as climate change, natural disasters, and diseases. This is challenging not only because of the large data volume, but also because of the intrinsic high-dimensional nature of geoscience data. To tackle this challenge, we propose a spatiotemporal indexing approach to efficiently manage and process big climate data with MapReduce in a highly scalable environment. Using this approach, big climate data are directly stored in a Hadoop Distributed File System in its original, native file format. A spatiotemporal index is built to bridge the logical array-based data model and the physical data layout, which enables fast data retrieval when performing spatiotemporal queries. Based on the index, a data-partitioning algorithm is applied to enable MapReduce to achieve high data locality, as well as balancing the workload. The proposed indexing approach is evaluated using the National Aeronautics and Space Administration (NASA) Modern-Era Retrospective Analysis for Research and Applications (MERRA) climate reanalysis dataset. The experimental results show that the index can significantly accelerate querying and processing (similar to 10x speedup compared to the baseline test using the same computing cluster), while keeping the index-to-data ratio small (0.0328%). The applicability of the indexing approach is demonstrated by a climate anomaly detection deployed on a NASA Hadoop cluster. This approach is also able to support efficient processing of general array-based spatiotemporal data in various geoscience domains without special configuration on a Hadoop cluster.
C1 [Li, Zhenlong; Hu, Fei; Yang, Chaowei] George Mason Univ, NSF Spatiotemporal Innovat Ctr, Fairfax, VA 22030 USA.
[Li, Zhenlong] Univ South Carolina, Dept Geog, Columbia, SC 29208 USA.
[Schnase, John L.] NASA Goddard Space Flight Ctr, Off Computat & Informat Sci & Technol, Greenbelt, MD USA.
[Duffy, Daniel Q.; Bowen, Michael K.] NASA, Goddard Space Flight Ctr, Ctr Climate Simulat, Greenbelt, MD USA.
[Lee, Tsengdar] NASA, Earth Sci Div, Washington, DC 20546 USA.
RP Yang, CW (reprint author), George Mason Univ, NSF Spatiotemporal Innovat Ctr, Fairfax, VA 22030 USA.
EM cyang3@gmu.edu
RI Yang, Chaowei/A-9881-2017
FU NSF [PLR-1349259, IIP-1338925, CNS-1117300, ICER-1343759]; NASA
[NNG12PP37I, NNG14HH38I]
FX This research was supported by NSF [PLR-1349259], [IIP-1338925],
[CNS-1117300], [ICER-1343759]; and NASA [NNG12PP37I], [NNG14HH38I].
NR 22
TC 2
Z9 2
U1 17
U2 17
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND
SN 1365-8816
EI 1362-3087
J9 INT J GEOGR INF SCI
JI Int. J. Geogr. Inf. Sci.
PY 2017
VL 31
IS 1
BP 17
EP 35
DI 10.1080/13658816.2015.1131830
PG 19
WC Computer Science, Information Systems; Geography; Geography, Physical;
Information Science & Library Science
SC Computer Science; Geography; Physical Geography; Information Science &
Library Science
GA EB3MJ
UT WOS:000387268600002
ER
PT J
AU Merkel, AW
Cassidy, TA
Vervack, RJ
McClintock, WE
Sarantos, M
Burger, MH
Killen, RM
AF Merkel, Aimee W.
Cassidy, Timothy A.
Vervack, Ronald J., Jr.
McClintock, William E.
Sarantos, Menelaos
Burger, Matthew H.
Killen, Rosemary M.
TI Seasonal variations of Mercury's magnesium dayside exosphere from
MESSENGER observations
SO ICARUS
LA English
DT Article
ID CALCIUM EXOSPHERE; INPUT FUNCTION; IMPACT; ATMOSPHERE; ENVIRONMENT;
DISCOVERY; SODIUM; FLYBY; MOON
AB The Ultraviolet and Visible Spectrometer channel of the Mercury Atmospheric and Surface Composition Spectrometer instrument aboard the MErcury Surface, Space ENvironment, GEochemistry, and Ranging spacecraft made near-daily observations of solar-scattered resonant emission from magnesium in Mercury's exosphere during the mission's orbital phase (March 2011-April 2015, similar to 17 Mercury years). In this paper, a subset of these data (March 2013-April 2015) is described and analyzed to illustrate Mg's spatial and temporal variations. Dayside altitude profiles of emission are used to make estimates of the Mg density and temperature. The main characteristics of the Mg exosphere are (a) a predominant enhancement of emission in the morning (6 am-10 am) near perihelion, (b) a bulk temperature of 6000 K, consistent with impact vaporization as the predominant ejection process, (c) a near-surface density that varies from 5 cm(-3) to 50 cm(-3) and (d) a production rate that is strongest in the morning on the inbound leg of Mercury's orbit with rates ranging from 1 x 10(5) cm(-2) s(-1) to 8 x 10(5) cm(-2) s(-1). (C) 2016 Elsevier Inc. All rights reserved.
C1 [Merkel, Aimee W.; Cassidy, Timothy A.; McClintock, William E.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.
[Vervack, Ronald J., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Sarantos, Menelaos] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 22118 USA.
[Sarantos, Menelaos] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Burger, Matthew H.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Killen, Rosemary M.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
RP Merkel, AW (reprint author), Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.
EM aimee.merkel@colorado.edu
RI Vervack, Ronald/C-2702-2016
OI Vervack, Ronald/0000-0002-8227-9564
FU NASA [NAS5-97271, NASW-00002]; MES-SENGER Participating Scientist
Program
FX The MESSENGER project is supported by the NASA Discovery Program under
contracts NAS5-97271 to The Johns Hopkins University Applied Physics
Laboratory and NASW-00002 to the Carnegie Institution of Washington. RJV
and RMK are supported by the MES-SENGER Participating Scientist Program.
All original data reported in this paper are archived by the NASA
Planetary Data System
(http://pds-geosciences/wustl.edu/missions/messenger/index.htm).
NR 29
TC 2
Z9 2
U1 11
U2 11
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JAN 1
PY 2017
VL 281
BP 46
EP 54
DI 10.1016/j.icarus.2016.08.032
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DY9TN
UT WOS:000385478100004
ER
PT J
AU Neish, CD
Hamilton, CW
Hughes, SS
Nawotniak, SK
Garry, WB
Skok, JR
Elphic, RC
Schaefer, E
Carter, LM
Bandfield, JL
Osinski, GR
Lim, D
Heldmann, JL
AF Neish, C. D.
Hamilton, C. W.
Hughes, S. S.
Nawotniak, S. Kobs
Garry, W. B.
Skok, J. R.
Elphic, R. C.
Schaefer, E.
Carter, L. M.
Bandfield, J. L.
Osinski, G. R.
Lim, D.
Heldmann, J. L.
TI Terrestrial analogues for lunar impact melt flows
SO ICARUS
LA English
DT Article
DE Earth; Impact processes; Moon, surface; Radar observations; Volcanism
ID SYNTHETIC-APERTURE; SURFACE-ROUGHNESS; RADAR SCATTERING; LAVA; CRATERS;
EMPLACEMENT; PAHOEHOE; EJECTA; MOON; MORPHOLOGY
AB Lunar impact melt deposits have unique physical properties. They have among the highest observed radar returns at S-Band (12.6 cm wavelength), implying that they are rough at the decimeter scale. However, they are also observed in high-resolution optical imagery to be quite smooth at the meter scale. These characteristics distinguish them from well-studied terrestrial analogues, such as Hawaiian pahoehoe and 'a' (a) over bar lava flows. The morphology of impact melt deposits can be related to their emplacement conditions, so understanding the origin of these unique surface properties will help to inform us as to the circumstances under which they were formed. In this work, we seek to find a terrestrial analogue for well-preserved lunar impact melt flows by examining fresh lava flows on Earth. We compare the radar return and high-resolution topographic variations of impact melt flows to terrestrial lava flows with a range of surface textures. The lava flows examined in this work range from smooth Hawaiian pahoehoe to transitional basaltic flows at Craters of the Moon (COTM) National Monument and Preserve in Idaho to rubbly and spiny pahoehoe-like flows at the recent eruption at Holuhraun in Iceland. The physical properties of lunar impact melt flows appear to differ from those of all the terrestrial lava flows studied in this work. This may be due to (a) differences in post-emplacement modification processes or (b) fundamental differences in the surface texture of the melt flows due to the melts' unique emplacement and/or cooling environment. Information about the surface properties of lunar impact melt deposits will be critical for future landed missions that wish to sample these materials. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Neish, C. D.; Osinski, G. R.] Univ Western Ontario, Dept Earth Sci, London, ON N6A 5B7, Canada.
[Neish, C. D.; Osinski, G. R.] Univ Western Ontario, Ctr Planetary Sci & Explorat, London, ON N6A 5B7, Canada.
[Hamilton, C. W.; Schaefer, E.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Hughes, S. S.; Nawotniak, S. Kobs] Idaho State Univ, Pocatello, ID 83209 USA.
[Garry, W. B.; Carter, L. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Skok, J. R.] SETI Inst, Mountain View, CA 94043 USA.
[Elphic, R. C.; Lim, D.; Heldmann, J. L.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
[Bandfield, J. L.] Space Sci Inst, Boulder, CO 80301 USA.
[Lim, D.] Bay Area Environm Res Inst, Petaluma, CA 94952 USA.
RP Neish, CD (reprint author), Univ Western Ontario, Dept Earth Sci, London, ON N6A 5B7, Canada.; Neish, CD (reprint author), Univ Western Ontario, Ctr Planetary Sci & Explorat, London, ON N6A 5B7, Canada.
EM cneish@uwo.ca
RI Carter, Lynn/D-2937-2012
FU National Sciences and Engineering Research Council of Canada; NASA Solar
System Workings (SSW) Program [NNX15AL60G]
FX We thank the LRO, AIRSAR, and UAVSAR projects for their effort in
returning the data presented here. Data from the LRO mission is made
publicly available through the Planetary Data System (pds.nasa.gov).
Data from the AIRSAR and UAVSAR projects were freely obtained at
http://airsar.jpl.nasa.gov/ and http://uavsar.jpl.nasa.gov,
respectively. The fieldwork in Idaho was conducted in conjunction with
the FINESSE (Field Investigations to Enable Solar System Science and
Exploration) project of the Solar System Exploration Research Virtual
Institute (SSERVI), led by PI J. Heldmann. Fieldwork in the Hawaii
Volcanoes National Park was conducted under Scientific Research and
Collecting Permit # HAVO-2006-SCI-0003. Assistance with the dGPS surveys
was provided by J. Carlin, S. Squyres, B. Caldwell, A. Bramson, L.
Kestay, C. Dundas, A. Ryan, M. Sori, and A. Keske. Topographic profiles
from Idaho, Hawaii, and Iceland may be obtained from CDN
(cneish@uwo.ca). CDN acknowledges support from the National Sciences and
Engineering Research Council of Canada and CWH acknowledges support from
the NASA Solar System Workings (SSW) Program (Grant #NNX15AL60G). We
thank two anonymous reviewers for comments that helped to improve the
manuscript.
NR 71
TC 0
Z9 0
U1 12
U2 12
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JAN 1
PY 2017
VL 281
BP 73
EP 89
DI 10.1016/j.icarus.2016.08.008
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DY9TN
UT WOS:000385478100006
ER
PT J
AU Nachon, M
Mangold, N
Forni, O
Kah, LC
Cousin, A
Wiens, RC
Anderson, R
Blaney, D
Blank, JG
Calef, F
Clegg, SM
Fabre, C
Fisk, MR
Gasnault, O
Grotzinger, JP
Kronyak, R
Lanza, NL
Lasue, J
Le Deit, L
Le Mouelic, S
Maurice, S
Meslin, PY
Oehler, DZ
Payre, V
Rapin, W
Schroder, S
Stack, K
Sumner, D
AF Nachon, M.
Mangold, N.
Forni, O.
Kah, L. C.
Cousin, A.
Wiens, R. C.
Anderson, R.
Blaney, D.
Blank, J. G.
Calef, F.
Clegg, S. M.
Fabre, C.
Fisk, M. R.
Gasnault, O.
Grotzinger, J. P.
Kronyak, R.
Lanza, N. L.
Lasue, J.
Le Deit, L.
Le Mouelic, S.
Maurice, S.
Meslin, P. -Y.
Oehler, D. Z.
Payre, V.
Rapin, W.
Schroeder, S.
Stack, K.
Sumner, D.
TI Chemistry of diagenetic features analyzed by ChemCam at Pahrump Hills,
Gale crater, Mars
SO ICARUS
LA English
DT Article
DE Mars surface; Geological processes; Mineralogy
ID INDUCED BREAKDOWN SPECTROSCOPY; INSTRUMENT SUITE; ROVER; SULFATE;
TARGETS; ROCKS; UNIT
AB The Curiosity rover's campaign at Pahrump Hills provides the first analyses of lower Mount Sharp strata. Here we report ChemCam elemental composition of a diverse assemblage of post-depositional features embedded in, or cross-cutting, the host rock. ChemCam results demonstrate their compositional diversity, especially compared to the surrounding host rock: (i) Dendritic aggregates and relief enhanced features, characterized by a magnesium enhancement and sulfur detection, and interpreted as Mg-sulfates; (ii) A localized observation that displays iron enrichment associated with sulfur, interpreted as Fe-sulfate; (iii) Dark raised ridges with varying Mg- and Ca-enriched compositions compared to host rock; (iv) Several dark-toned veins with calcium enhancement associated with fluorine detection, interpreted as fluorite veins. (v) Light-toned veins with enhanced calcium associated with sulfur detection, and interpreted as Ca-sulfates. The diversity of the Pahrump Hills diagenetic assemblage suggests a complex post depositional history for fine-grained sediments for which the origin has been interpreted as fluvial and lacustrine. Assessment of the spatial and relative temporal distribution of these features shows that the Mg-sulfate features are predominant in the lower part of the section, suggesting local modification of the sediments by early diagenetic fluids. In contrast, light-toned Ca-sulfate veins occur in the whole section and cross-cut all other features. A relatively late stage shift in geochemical conditions could explain this observation. The Pahrump Hills diagenetic features have no equivalent compared to targets analyzed in other locations at Gale crater. Only the light-toned Ca-sulfate veins are present elsewhere, along Curiosity's path, suggesting they formed through a common late-stage process that occurred at over a broad area. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Nachon, M.; Mangold, N.; Le Deit, L.; Le Mouelic, S.] Univ Nantes, CNRS, Lab Planetol & Geodynam Nantes, UMR6112, F-44322 Nantes, France.
[Forni, O.; Cousin, A.; Gasnault, O.; Lasue, J.; Maurice, S.; Meslin, P. -Y.; Rapin, W.; Schroeder, S.] Univ Toulouse, Inst Rech Astrophys & Planetol, UPS OMP, Toulouse, France.
[Kah, L. C.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN USA.
[Wiens, R. C.; Clegg, S. M.; Lanza, N. L.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Anderson, R.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Blaney, D.; Calef, F.; Stack, K.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
[Blank, J. G.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Fabre, C.; Payre, V.] Univ Lorraine, GeoRessources, Nancy, France.
[Fisk, M. R.] Oregon State Univ, Coll Earth Ocean & Atmospher Sci, Corvallis, OR 97331 USA.
[Grotzinger, J. P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Oehler, D. Z.] NASA, Astromat Res & Explorat Sci Div, Johnson Space Ctr, Houston, TX 77058 USA.
[Schroeder, S.] Inst Opt Sensorsyst, German Aerosp Ctr DLR, Berlin, Germany.
[Sumner, D.] Univ Calif Davis, Earth & Planetary Sci, Davis, CA 95616 USA.
RP Nachon, M (reprint author), Univ Nantes, CNRS, Lab Planetol & Geodynam Nantes, UMR6112, F-44322 Nantes, France.
EM marion.nachon@univ-nantes.fr
OI Clegg, Sam/0000-0002-0338-0948
FU NASA's Mars Exploration Program; Centre National de la Recherche
Scientifique; Centre National d'Etudes Spatiales; Observatoire des
Sciences de l'Univers Nord Atlantique
FX Data used in the study are available at the NASA Planetary Data System
(https://pds.jpl.nasa.gov). We are grateful to the MSL and especially
ChemCam science and engineering Teams for the data collection, which is
supported in the US by NASA's Mars Exploration Program. We acknowledge
Jean-Pierre Lorand (LPGNantes) for providing us with the NiS sample. We
also acknowledge the IRAP and the CNES Team members for their
contribution on the laboratory analysis. Insightful comments provided by
two anonymous reviewers were appreciated. French authors are granted by
the Centre National de la Recherche Scientifique, the Centre National
d'Etudes Spatiales, and the Observatoire des Sciences de l'Univers Nord
Atlantique.
NR 50
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U1 15
U2 15
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JAN 1
PY 2017
VL 281
BP 121
EP 136
DI 10.1016/j.icarus.2016.08.026
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DY9TN
UT WOS:000385478100010
ER
PT J
AU Kerber, L
Dickson, JL
Head, JW
Grosfils, EB
AF Kerber, Laura
Dickson, James L.
Head, James W.
Grosfils, Eric B.
TI Polygonal ridge networks on Mars: Diversity of morphologies and the
special case of the Eastern Medusae Fossae Formation
SO ICARUS
LA English
DT Article
DE Mars; Surface; Geological processes; Mars; Volcanism; Hydrology
ID FINE-GRAINED SEDIMENTS; FAN-SHAPED DEPOSIT; GALE CRATER; MARTIAN
SURFACE; EVOLUTION; EROSION; ORIGIN; FAULTS; HELLAS; HISTORY
AB Polygonal ridge networks, also known as boxwork or reticulate ridges, are found in numerous locations and geological contexts across Mars. Distinguishing the morphologies and geological context of the ridge networks sheds light on their potential as astrobiological and mineral resource sites of interest. The most widespread type of ridge morphology is characteristic of the Nili Fossae and Nilosyrtis region and consists of thin, criss-crossing ridges with a variety of heights, widths, and intersection angles. They are found in ancient Noachian terrains at a variety of altitudes (between -2500 and 2200 m) and geographic locations and are likely to be chemically altered fracture planes or mineral veins. They occur in the same general areas as valley networks and ancient lake basins, but they are not more numerous where these water-related features are concentrated, and can appear in places where th morphologies are absent. Similarly, some of the ridge networks are located near hydrated mineral detections, but there is not a one-to-one correlation. Smaller, light-toned ridges of variable widths have been found in Gale Crater and other rover sites and are interpreted to be smaller versions of the Nili-like ridges, mostly formed by the mineralization of fractures. This type of ridge is likely to be found in many other places on Mars as more high-resolution data become available. Sinus Meridiani contains many flat-topped ridges arranged into quasi-circular patterns. The ridges are eroding from a clay-rich unit, and could be formed by a similar process as the Nili-type ridges, but at a much larger scale and controlled by fractures made through a different process. Hellas Basin is host to a fourth type of ridge morphology consisting of large, thick, light-toned ridges forming regular polygons at several superimposed scales. While still enigmatic, these are most likely to be the result of sediment-filled fractures. The Eastern Medusae Fossae Formation contains large swaths of a fifth, previously undocumented, ridge network type. The dark ridges, reaching up to 50m in height, enclose regular polygons and erode into dark boulders. These ridge networks are interpreted to form as a result of lava flow embayment of deeply fractured Medusae Fossae Formation outcrops. (C) 2016 Published by Elsevier Inc.
C1 [Kerber, Laura] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Dickson, James L.; Head, James W.] Brown Univ, Dept Geol Sci, Box 1846, Providence, RI 02912 USA.
[Grosfils, Eric B.] Pomona Coll, Dept Geol, 185 E 6th St, Claremont, CA 91711 USA.
RP Kerber, L (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM kerber@lmd.jussieu.fr
NR 66
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U1 9
U2 9
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JAN 1
PY 2017
VL 281
BP 200
EP 219
DI 10.1016/j.icarus.2016.08.020
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DY9TN
UT WOS:000385478100014
ER
PT J
AU Ramirez, RM
Kasting, JF
AF Ramirez, Ramses M.
Kasting, James F.
TI Could cirrus clouds have warmed early Mars?
SO ICARUS
LA English
DT Article
DE Mars; Atmosphere; Mars; Climate; Atmospheres; Evolution
ID CARBON-DIOXIDE CLOUDS; EARLY MARTIAN CLIMATE; RUNAWAY GREENHOUSE; ICE
CLOUDS; CO2; ABSORPTION; ATMOSPHERE; MODEL; RADIATION; MIXTURES
AB The presence of the ancient valley networks on Mars indicates that the climate at 3.8 Ga was warm enough to allow substantial liquid water to flow on the martian surface for extended periods of time. However, the mechanism for producing this warming continues to be debated. One hypothesis is that Mars could have been kept warm by global cirrus cloud decks in a CO2-H2O atmosphere containing at least 0.25 bar of CO2 (Urata and Toon, 2013). Initial warming from some other process, e.g., impacts, would be required to make this model work. Those results were generated using the CAM 3-D global climate model. Here, we use a single-column radioactive-convective climate model to further investigate the cirrus cloud warming hypothesis. Our calculations indicate that cirrus cloud decks could have produced global mean surface temperatures above freezing, but only if cirrus cloud cover approaches similar to 75 - 100% and if other cloud properties (e.g., height, optical depth, particle size) are chosen favorably. However, at more realistic cirrus cloud fractions, or if cloud parameters are not optimal, cirrus clouds do not provide the necessary warming, suggesting that other greenhouse mechanisms are needed. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Ramirez, Ramses M.] Cornell Univ, Carl Sagan Inst, Ithaca, NY 14853 USA.
[Ramirez, Ramses M.] Cornell Univ, Cornell Ctr Astrophys & Planetary Sci, Ithaca, NY 14853 USA.
[Kasting, James F.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
[Kasting, James F.] Penn State Univ, Penn State Astrobiol Res Ctr, University Pk, PA 16802 USA.
[Kasting, James F.] Univ Washington, NASA, Astrobiol Inst, Virtual Planetary Lab, Seattle, WA 98195 USA.
RP Ramirez, RM (reprint author), Cornell Univ, Carl Sagan Inst, Ithaca, NY 14853 USA.; Ramirez, RM (reprint author), Cornell Univ, Cornell Ctr Astrophys & Planetary Sci, Ithaca, NY 14853 USA.
EM ramsesny@gmail.com
FU Simons Foundation [SCOL 290357]; Carl Sagan Institute; Cornell Center of
Astrophysics and Planetary Science; NASA Emerging Worlds; NASA Habitable
Worlds; Astrobiology Institute
FX We would like to thank Richard Urata and Brian Toon for kindly providing
the cloud optical data. RR acknowledges support by the Simons Foundation
(SCOL 290357, LK), Carl Sagan Institute, and the Cornell Center of
Astrophysics and Planetary Science. JK acknowledges support from NASA's
Emerging Worlds, Habitable Worlds, and the Astrobiology Institute.
NR 48
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PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JAN 1
PY 2017
VL 281
BP 248
EP 261
DI 10.1016/j.icarus.2016.08.016
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DY9TN
UT WOS:000385478100018
ER
PT J
AU Kim, SJ
Geballe, TR
Greathouse, TK
Yung, YL
Miller, S
Orton, GS
Minh, YC
AF Kim, Sang Joon
Geballe, Thomas R.
Greathouse, Thomas K.
Yung, Yuk L.
Miller, Steve
Orton, G. S.
Minh, Y. C.
TI Temperatures and CH4 mixing ratios near the homopause of the 8 mu m
north polar hot spot of Jupiter
SO ICARUS
LA English
DT Article
DE Jupiter; Atmosphere; Aurora; Infrared; Spectroscopy
ID UPPER-ATMOSPHERE; BRIGHTENINGS; STRATOSPHERE; CHEMISTRY; EMISSION;
CASSINI; REGIONS; WAVES
AB We have derived homopause temperatures of 180-250 K for the 8-mu m north-polar hot spot (8NPHS) of Jupiter by fitting CH4 emission models to 3 and 8 mu m spectra of the 8NPHS obtained 24 days apart in 2013. From the fits, we find that CH4 mixing ratios at the 8NPHS are consistent with those reported by Kim et al. (2014) in equatorial regions. We propose possible mechanisms to account for the temperature of the 8NPHS homopause, which is relatively cool compared with the temperatures of other auroral regions, including locally-fixed and transient but energetic auroral particle precipitation. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Kim, Sang Joon] Kyung Hee Univ, Sch Space Res, Yongin 446701, South Korea.
[Geballe, Thomas R.] Gemini Observ, 670 N Aohoku Pl, Hilo, HI 96720 USA.
[Greathouse, Thomas K.] Southwest Res Inst, 6220 Culebra Rd, San Antonio, TX 78228 USA.
[Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Miller, Steve] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Orton, G. S.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Minh, Y. C.] Korea Astron & Space Sci Inst, Daejeon 305348, South Korea.
RP Kim, SJ (reprint author), Kyung Hee Univ, Sch Space Res, Yongin 446701, South Korea.
EM sjkim1@khu.ac.kr
FU Space Core Technology program through NRF - Ministry of Education,
Science and Technology; KASI under RD program; NASA
FX SJK acknowledges support from the Space Core Technology program through
NRF funded by the Ministry of Education, Science and Technology, and
from KASI under the R&D program supervised by the Ministry of Science,
ICT and Future Planning. Support for GSO was provided, in part, by an
award from NASA to the Jet Propulsion Laboratory, California Institute
of Technology. The research is based in part on observations obtained at
the Gemini Observatory, which is operated by the Association of
Universities for Research in Astronomy, Inc., under a cooperative
agreement with the NSF on behalf of the Gemini partnership: the National
Science Foundation (United States), the National Research Council
(Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnologia e
Innovacion Productiva (Argentina), and Ministerio da Ciencia, Tecnologia
e Inovacao (Brazil).
NR 22
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U1 7
U2 7
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JAN 1
PY 2017
VL 281
BP 281
EP 285
DI 10.1016/j.icarus.2016.09.017
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DY9TN
UT WOS:000385478100021
ER
PT J
AU Lainey, V
Jacobson, RA
Tajeddine, R
Cooper, NJ
Murray, C
Robert, V
Tobie, G
Guillot, T
Mathis, S
Remus, F
Desmars, J
Arlot, JE
De Cuyper, JP
Dehant, V
Pascu, D
Thuillot, W
Le Poncin-Lafitte, C
Zahn, JP
AF Lainey, Valery
Jacobson, Robert A.
Tajeddine, Radwan
Cooper, Nicholas J.
Murray, Carl
Robert, Vincent
Tobie, Gabriel
Guillot, Tristan
Mathis, Stephane
Remus, Francoise
Desmars, Josselin
Arlot, Jean-Eudes
De Cuyper, Jean-Pierre
Dehant, Veronique
Pascu, Dan
Thuillot, William
Le Poncin-Lafitte, Christophe
Zahn, Jean-Paul
TI New constraints on Saturn's interior from Cassini astrometric data
SO ICARUS
LA English
DT Article
DE Astrometry; Interior; Saturn
ID STRONG TIDAL DISSIPATION; GIANT PLANETS; SOLAR-SYSTEM; SATELLITES;
MODELS; ENCELADUS; EVOLUTION; JUPITER; MOONS; EARTH
AB Using astrometric observations spanning more than a century and including a large set of Cassini data, we determine Saturn's tidal parameters through their current effects on the orbits of the eight main and four coorbital Moons. We have used the latter to make the first determination of Saturn's Love number from observations, k(2)=0.390 +/- 0.024, a value larger than the commonly used theoretical value of 0.341 (Gavrilov & Zharkov, 1977), but compatible with more recent models (Helled & Guillot, 2013) for which the static k(2) ranges from 0.355 to 0382. Depending on the assumed spin for Saturn's interior, the new constraint can lead to a significant reduction in the number of potential models, offering great opportunities to probe the planet's interior. In addition, significant tidal dissipation within Saturn is confirmed (Lainey et al., 2012) corresponding to a high present-day tidal ratio k(2)/Q=(1.59 +/- 0.74)x10(-4) and implying fast orbital expansions of the Moons. This high dissipation, with no obvious variations for tidal frequencies corresponding to those of Enceladus and Dione, may be explained by viscous friction in a solid core, implying a core viscosity typically ranging between 10(14) and 10(16) Pa.s (Remus et al., 2012). However, a dissipation increase by one order of magnitude at Rhea's frequency could suggest the existence of an additional, frequency-dependent, dissipation process, possibly from turbulent friction acting on tidal waves in the fluid envelope of Saturn (Ogilvie & Lin, 2004; Fuller et al. 2016). (C) 2016 Elsevier Inc. All rights reserved.
C1 [Lainey, Valery; Tajeddine, Radwan; Cooper, Nicholas J.; Robert, Vincent; Remus, Francoise; Desmars, Josselin; Arlot, Jean-Eudes; Thuillot, William] Univ Paris 06, Sorbonne Univ, PSL Res Univ, IMCCE,Observ Paris,CNRS,Univ Lille, F-75252 Paris 05, France.
[Jacobson, Robert A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Tajeddine, Radwan] Cornell Univ, Ctr Astrophys & Planetary Sci, Ithaca, NY 14853 USA.
[Cooper, Nicholas J.; Murray, Carl] Queen Mary Univ London, Mile End Rd, London E1 4NS, England.
[Robert, Vincent] IPSA, 7-9 Rue Maurice Grandcoing, F-94200 Ivry, France.
[Tobie, Gabriel] Univ Nantes, CNRS, Lab Planetol & Geodynam Nantes, UMR 6112, 2 Rue Houssiniere, F-44322 Nantes 3, France.
[Guillot, Tristan] Univ Nice Sophia Antipolis, CNRS UMR 7293, Lab Lagrange, Observ Cote Azur, BP 4229, F-06304 Nice 4, France.
[Mathis, Stephane; Remus, Francoise] Univ Paris Diderot, CEA DRF, CNRS, Lab AIM Paris Saclay,IRFU SAp Ctr Saclay, F-91191 Gif Sur Yvette, France.
[Remus, Francoise; Zahn, Jean-Paul] LUTH Observ Paris, UMR CNRS 8102, 5 Pl Jules Janssen, F-92195 Meudon, France.
[Desmars, Josselin] Observ Nacl, Rua Jose Cristino 77, BR-20921400 Sao Cristovao, RJ, Brazil.
[De Cuyper, Jean-Pierre; Dehant, Veronique] Royal Observ Belgium, Ave Circulaire 3, B-1180 Brussels, Belgium.
[Pascu, Dan] USNO, 3450 Massachusetts Ave NW, Washington, DC 20392 USA.
[Le Poncin-Lafitte, Christophe] Univ Paris 06, Sorbonne Univ, PSL Res Univ, SYRTE,Observ Paris,CNRS,LNE, 61 Ave Observ, F-75014 Paris, France.
RP Lainey, V (reprint author), Univ Paris 06, Sorbonne Univ, PSL Res Univ, IMCCE,Observ Paris,CNRS,Univ Lille, F-75252 Paris 05, France.
EM lainey@imcce.fr
OI Guillot, Tristan/0000-0002-7188-8428; Robert,
Vincent/0000-0002-4517-5213
FU European Community's Seventh Framework Program [263466]; International
Space Science Institute (ISSI); PNP (INSU/CNES); AS GRAM
(INSU/CNES/INP); UK Science and Technology Facilities Council
[ST/M001202/1]; Leverhulme Trust; Scientific Council of the Paris
Observatory; European Research Council through ERC grant SPIRE [647383];
European Research Council under European Community's Seventh Framework
Programme [259285]; European Research Council under European Community's
Seventh Framework Programme (ERC EXOATER)
FX The authors are indebted to all participants of the Encelade WG. V.L.
would like to thank Michael Efroimsky for fruitful discussions. This
work has been supported by the European Community's Seventh Framework
Program (FP7/2007-2013) under grant agreement 263466 for the FP7-ESPaCE
project, the International Space Science Institute (ISSI), PNP
(INSU/CNES) and AS GRAM (INSU/CNES/INP). The work of R. A. J. was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA. N.C. and C.M. were supported by
the UK Science and Technology Facilities Council (Grant No.
ST/M001202/1) and are grateful to them for financial assistance. C.M. is
also grateful to the Leverhulme Trust for the award of a Research
Fellowship. N.C. thanks the Scientific Council of the Paris Observatory
for funding. S. Mathis acknowledges funding by the European Research
Council through ERC grant SPIRE 647383. G. Tobie acknowledges funding
from the European Research Council under the European Community's
Seventh Framework Programme (FP7/2007-2013 Grant Agreement no. 259285,
ERC EXOATER). The authors are indebted to the Cassini project and the
Imaging Science Subsystem Team for making this collaboration possible.
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SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JAN 1
PY 2017
VL 281
BP 286
EP 296
DI 10.1016/j.icarus.2016.07.014
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DY9TN
UT WOS:000385478100022
ER
PT J
AU Zhang, Z
Hayes, AG
Janssen, MA
Nicholson, PD
Cuzzi, JN
de Pater, I
Dunn, DE
Estrada, PR
Hedman, MM
AF Zhang, Z.
Hayes, A. G.
Janssen, M. A.
Nicholson, P. D.
Cuzzi, J. N.
de Pater, I.
Dunn, D. E.
Estrada, P. R.
Hedman, M. M.
TI Cassini microwave observations provide clues to the origin of Saturn's C
ring
SO ICARUS
LA English
DT Article
DE Saturn, rings; Planetary rings; Radar observations; Origin, Solar system
ID DENSE PLANETARY RINGS; INFRARED OBSERVATIONS; PARTICLE COMPOSITION; SIZE
DISTRIBUTION; SOLAR-SYSTEM; BOMBARDMENT; SATELLITE; ACCRETION;
EVOLUTION; IMPACTS
AB Despite considerable study, Saturn's rings continue to challenge current theories for their provenance. Water ice comprises the bulk of Saturn's rings, yet it is the small fraction of non-icy material that is arguably more valuable in revealing clues about the system's origin and age. Herein, we present new measurements of the non-icy material fraction in Saturn's C ring, determined from microwave radiometry observations acquired by the Cassini spacecraft. Our observations show an exceptionally high brightness at near-zero azimuthal angles, suggesting a high porosity of 70-75% for the C ring particles. Furthermore, our results show that most regions in the C ring contain about 1-2% silicates. These results are consistent with an initially nearly pure-ice ring system that has been continuously contaminated by in-falling microwmeteoroids over similar to 15-90 million years, using the currently accepted value of the micrometeoroid flux at infinity of similar to 4.5 x 10(-17)g cm(-2) s(-1), and assuming that the C ring optical depth and surface density has not changed significantly during that time. This absolute time scale is inversely proportional not only to the flux at infinity, but also to the amount of gravitational focusing by Saturn the micrometeoroids experience before encountering the rings. We also find an enhanced abundance of non-icy material concentrated in the middle C ring. When assumed to be mixed volumetrically ("intramixed") with water ice, this enhanced contamination reaches a maximum concentration of 6-11% silicates by volume around a ring radius of 83,000 km, depending on the volume mixing model used. This is significantly higher than the inner and outer C ring. As opposed to an intramixing model, we also consider a silicate-core, icy mantle model to address the fact that silicates may be present in chunks instead of fine powder in the ring particles. Such a model naturally helps to account for the observed opacity distribution. We propose several models to explain the radially varied non-icy material contamination. Our preferred model is that the C ring has been continuously polluted by meteoroid bombardment since it first formed, while the middle C ring was further contaminated by an incoming Centaur, a rocky object torn apart by tides and ultimately broken into pieces that currently reside in the middle C ring. If correct, the spatial extent of the enhanced non-icy material fraction suggests that the Centaur was likely to be captured and integrated into the rings perhaps as recently as similar to 10-20 million years ago. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Zhang, Z.; Hayes, A. G.; Nicholson, P. D.] Cornell Univ, Dept Astron, Ithaca, NY 14850 USA.
[Janssen, M. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Cuzzi, J. N.; Estrada, P. R.] NASA, Div Space Sci, Ames Res Ctr, Moffett Field, CA 94035 USA.
[de Pater, I.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Dunn, D. E.] Sierra Coll, Dept Astron, Rocklin, CA 95677 USA.
[Estrada, P. R.] SETI Inst, Moffett Field, CA 94035 USA.
[Hedman, M. M.] Univ Idaho, Dept Phys, Moscow, ID 83844 USA.
RP Zhang, Z (reprint author), Cornell Univ, Dept Astron, Ithaca, NY 14850 USA.
EM zz246@cornell.edu
FU NASA Outer Planets Research Program [NNX14AR27G]; NASA
FX We thank NASA Outer Planets Research Program (Grant Number NNX14AR27G)
for funding this work. We thank Luke Dones for providing an estimate for
the timescale of catastrophic breakup of Saturnian fragments. We thank
Joseph Burns, Matthew Tiscareno and Michael Evans for helpful
conversations. Finally we gratefully acknowledge those who designed,
developed and operate the Cassini/Huygens mission, which is a joint
endeavor of NASA, the European Space Agency (ESA), and the Italian Space
Agency (ASI) and is managed by JPL/Caltech under a contract with NASA.
NR 92
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U2 8
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JAN 1
PY 2017
VL 281
BP 297
EP 321
DI 10.1016/j.icarus.2016.07.020
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DY9TN
UT WOS:000385478100023
ER
PT J
AU Aglyamov, Y
Schroeder, DM
Vance, SD
AF Aglyamov, Yury
Schroeder, Dustin M.
Vance, Steven D.
TI Bright prospects for radar detection of Europa's ocean
SO ICARUS
LA English
DT Article
DE Radar sounding; Regolith; Ocean; Volume scattering; Icy moon
ID ICY GALILEAN SATELLITES
AB The surface of Europa has been hypothesized to include an ice regolith layer from hundreds of meters to kilometers in thickness. However, contrary to previous claims, it does not present a significant obstacle to searching for Europa's ocean with radar sounding. This note corrects prior volume scattering loss analyses and expands them to includes observational and thermo-mechanical constraints on pore size and regolith depth. This provides a more physically realistic range of potential ice-regolith volume-scattering losses for radar sounding observations of Europa's ice shell in the HF and VHF frequency bands. We conclude that, for the range of physical processes and material properties observed or hypothesized for Europa, volume scattering losses are not likely to pose a major obstacle to radar penetration. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Aglyamov, Yury] CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Schroeder, Dustin M.] Stanford Univ, Dept Geophys, Stanford, CA 94305 USA.
[Vance, Steven D.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Schroeder, DM (reprint author), Stanford Univ, Dept Geophys, Stanford, CA 94305 USA.
EM dustin.m.schroeder@stanford.edu
OI Schroeder, Dustin/0000-0003-1916-3929
FU National Aeronautics and Space Administration
FX A portion of this research was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration.
NR 20
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PI SAN DIEGO
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SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JAN 1
PY 2017
VL 281
BP 334
EP 337
DI 10.1016/j.icarus.2016.08.014
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DY9TN
UT WOS:000385478100025
ER
PT J
AU Gautier, T
Trainer, MG
Loeffler, MJ
Sebree, JA
Anderson, CM
AF Gautier, Thomas
Trainer, Melissa G.
Loeffler, Mark J.
Sebree, Joshua A.
Anderson, Carrie M.
TI Environmental temperature effect on the far-infrared absorption features
of aromatic-based Titan's aerosol analogs
SO ICARUS
LA English
DT Article
DE Titan; Atmosphere; Photochemistry; Atmosphere; Chemistry
ID UPPER-ATMOSPHERE; SPECTROSCOPY; THOLINS; SPECTRA; STRATOSPHERE;
MOLECULES; CHEMISTRY; PLASMA
AB Benzene detection has been reported in Titan's atmosphere both in the stratosphere at ppb levels by remote sensing (Coustenis et al., 2007; Vinatier et al., 2007) and in the thermosphere at ppm levels by the Cassini's Ion and Neutral Mass Spectrometer (Waite et al., 2007). This detection supports the idea that aromatic and heteroaromatic reaction pathways may play an important role in Titan's atmospheric chemistry, especially in the formation of aerosols. Indeed, aromatic molecules are easily dissociated by ultraviolet radiation and can therefore contribute significantly to aerosol formation. It has been shown recently that aerosol analogs produced from a gas mixture containing a low concentration of aromatic and/or heteroaromatic molecules (benzene, naphthalene, pyridine, quinoline and isoquinoline) have spectral signatures below 500 cm(-1), a first step towards reproducing the aerosol spectral features observed by Cassini's Composite InfraRed Spectrometer (CIRS) in the far infrared (Anderson and Samuelson 2011, and references therein). In this work we investigate the influence of environmental temperature on the absorption spectra of such aerosol samples, simulating the temperature range to which aerosols, once formed, are exposed during their transport through Titan's stratosphere. Our results show that environmental temperature does not have any major effect on the spectral shape of these aerosol analogs in the far-infrared, which is consistent with the CIRS observations. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Gautier, Thomas; Trainer, Melissa G.; Loeffler, Mark J.; Anderson, Carrie M.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Sebree, Joshua A.] Univ Northern Iowa, Dept Chem & Biochem, Cedar Falls, IA 50614 USA.
RP Gautier, T (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
EM thomas.j.gautier@nasa.gov
FU National Aeronautics and Space Administration [10-PATM10-0027]
FX This work was supported by the National Aeronautics and Space
Administration under Grant 10-PATM10-0027 issued through the Planetary
Atmospheres Program. T.G. was supported by an appointment to the NASA
Postdoctoral Program at the Goddard Space Flight Center, administered by
Oak Ridge Associated Universities through a contract with NASA.
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SN 0019-1035
EI 1090-2643
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JI Icarus
PD JAN 1
PY 2017
VL 281
BP 338
EP 341
DI 10.1016/j.icarus.2016.07.015
PG 4
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SC Astronomy & Astrophysics
GA DY9TN
UT WOS:000385478100026
ER
PT J
AU Shepard, MK
Richardson, J
Taylor, PA
Rodriguez-Ford, LA
Conrad, A
de Pater, I
Adamkovics, M
de Kleer, K
Males, JR
Morzinski, KM
Close, LM
Kaasalainen, M
Viikinkoski, M
Timerson, B
Reddy, V
Magri, C
Nolan, MC
Howell, ES
Benner, LAM
Giorgini, JD
Warner, BD
Harris, AW
AF Shepard, Michael K.
Richardson, James
Taylor, Patrick A.
Rodriguez-Ford, Linda A.
Conrad, Al
de Pater, Imke
Adamkovics, Mate
de Kleer, Katherine
Males, Jared R.
Morzinski, Katie M.
Close, Laird M.
Kaasalainen, Mikko
Viikinkoski, Matti
Timerson, Bradley
Reddy, Vishnu
Magri, Christopher
Nolan, Michael C.
Howell, Ellen S.
Benner, Lance A. M.
Giorgini, Jon D.
Warner, Brian D.
Harris, Alan W.
TI Radar observations and shape model of asteroid 16 Psyche
SO ICARUS
LA English
DT Article
DE Asteroids; Asteroids Composition; Surfaces Asteroids; Radar
ID MAIN-BELT ASTEROIDS; INDUCED SEISMIC ACTIVITY; LIGHTCURVE INVERSION;
OPTIMIZATION METHODS; ASTROMETRIC MASSES; 21 LUTETIA; DENSITY;
METEORITE; GRAVITY; SIZE
AB Using the S-band radar at Arecibo Observatory, we observed 16 Psyche, the largest M-class asteroid in the main belt. We obtained 18 radar imaging and 6 continuous wave runs in November and December 2015, and combined these with 16 continuous wave runs from 2005 and 6 recent adaptive-optics (AO) images (Drummond et al., 2016) to generate a three-dimensional shape model of Psyche. Our model is consistent with a previously published AO image (Hanus et al., 2013) and three multi-chord occultations. Our shape model has dimensions 279 x 232 x 189 km (+/- 10%), D-eff =226 +/- 23 km, and is 6% larger than, but within the uncertainties of, the most recently published size and shape model generated from the inversion of lightcurves (Hanus et al., 2013). Psyche is roughly ellipsoidal but displays a mass-deficit over a region spanning 90 degrees of longitude. There is also evidence for two similar to 50-70 km wide depressions near its south pole. Our size and published masses lead to an overall bulk density estimate of 4500 +/- 1400 kgm(-3). Psyche's mean radar albedo of 0.37 +/- 0.09 is consistent with a near-surface regolith composed largely of iron-nickel and similar to 40% porosity. Its radar reflectivity varies by a factor of 1.6 as the asteroid rotates, suggesting global variations in metal abundance or bulk density in the near surface. The variations in radar albedo appear to correlate with large and small-scale shape features. Our size and Psyche's published absolute magnitude lead to an optical albedo of p(v)=0.15 +/- 0.03, and there is evidence for albedo variegations that correlate with shape features. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Shepard, Michael K.] Bloomsburg Univ, 400 E Second St, Bloomsburg, PA 17815 USA.
[Richardson, James; Taylor, Patrick A.; Rodriguez-Ford, Linda A.] Arecibo Observ, USRA Arecibo, Arecibo, PR 00612 USA.
[Conrad, Al] Univ Arizona, Large Binocular Telescope Obs, Tucson, AZ 85721 USA.
[de Pater, Imke; Adamkovics, Mate; de Kleer, Katherine] Univ Calif Berkeley, Berkeley, CA 94720 USA.
[Males, Jared R.; Morzinski, Katie M.; Close, Laird M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Kaasalainen, Mikko; Viikinkoski, Matti] Tampere Univ Technol, FIN-33101 Tampere, Finland.
[Timerson, Bradley] Int Occultat Timing Assoc, 623 Bell Rd, Newark, NY 14513 USA.
[Reddy, Vishnu; Nolan, Michael C.; Howell, Ellen S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Magri, Christopher] Univ Maine Farmington, Farmington, ME 04938 USA.
[Benner, Lance A. M.; Giorgini, Jon D.] Jet Prop Lab, Pasadena, CA 91109 USA.
[Warner, Brian D.] More Data Inc, Eaton, CO 80615 USA.
[Harris, Alan W.] More Data Inc, La Caliada, CA 91011 USA.
RP Shepard, MK (reprint author), Bloomsburg Univ, 400 E Second St, Bloomsburg, PA 17815 USA.
EM mshepard@bloomu.edu
RI Kaasalainen, Mikko/G-4236-2014
FU National Aeronautics and Space Administration [NNX12AF24G]; National
Aeronautics and Space Administration (NASA) under Science Mission
Directorate Research and Analysis Programs; NASA grant [NNX13AP56G];
National Science Foundation [AST-1507535]
FX The Arecibo Observatory is operated by SRI International under a
cooperative agreement with the National Science Foundation
(AST-1100968), and in alliance with Ana G. Mendez-Universidad
Metropolitana, and the Universities Space Research Association. The
Arecibo Planetary Radar Program is supported by the National Aeronautics
and Space Administration under Grant No. NNX12AF24G issued through the
Near Earth Object Observations program. We thank the Arecibo operators
and staff for their help in observing. Some of this work was performed
at the Jet Propulsion Laboratory, California Institute of Technology,
under contract with the National Aeronautics and Space Administration.
This material is based in part upon work supported by the National
Aeronautics and Space Administration (NASA) under the Science Mission
Directorate Research and Analysis Programs. Some of the data presented
herein were obtained at the W.M. Keck Observatory, which is operated as
a scientific partnership among the California Institute of Technology,
the University of California and the National Aeronautics and Space
Administration. The Observatory was made possible by the generous
financial support of the W.M. Keck Foundation. The authors wish to
recognize and acknowledge the very significant cultural role and
reverence that the summit of Mauna Kea has always had within the
indigenous Hawaiian community. We are most fortunate to have the
opportunity to conduct observations from this mountain. This paper also
includes data gathered with the 6.5 m Magellan Telescopes located at Las
Campanas Observatory, Chile. Funding for PDS observations, analysis, and
publication was provided by NASA grant NNX13AP56G. Work on the asteroid
lightcurve database (LCDB) was also funded in part by National Science
Foundation grant AST-1507535.
NR 55
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JAN 1
PY 2017
VL 281
BP 388
EP 403
DI 10.1016/j.icarus.2016.08.011
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DY9TN
UT WOS:000385478100030
ER
PT J
AU Morishima, R
AF Morishima, Ryuji
TI Onset of oligarchic growth and implication for accretion histories of
dwarf planets
SO ICARUS
LA English
DT Article
DE Accretion; Planetary formation; Origin; Solar System; Asteroids; Kuiper
belt
ID KUIPER-BELT OBJECTS; PLANETESIMAL-DRIVEN MIGRATION; SOLAR
GRAVITATIONAL-FIELD; TRANS-NEPTUNIAN OBJECTS; N-BODY SIMULATIONS; SIZE
DISTRIBUTION; RUNAWAY GROWTH; COLLISIONAL EVOLUTION; TERRESTRIAL
PLANETS; GIANT PLANETS
AB We investigate planetary accretion that starts from equal-mass planetesimals using an analytic theory and numerical simulations. We particularly focus on how the planetary mass M-oli at the onset of oligarchic growth depends on the initial mass m(0) of a planetesimal. Oligarchic growth commences when the velocity dispersion relative to the Hill velocity of the protoplanet takes its minimum. We find that if m(0) is small enough, this normalized velocity dispersion becomes as low as unity during the intermediate stage between the runaway and oligarchic growth stages. In this case, M-oli is independent of m(0). If m(0) is large, on the other hand, oligarchic growth commences directly after runaway growth, and M-oli alpha m(0)(3/7). The planetary mass M-oli for the solid surface density of the Minimum Mass Solar Nebula is close to the masses of the dwarf planets in a reasonable range of m(0). This indicates that they are likely to be the largest remnant planetesimals that failed to become planets. The power-law exponent q of the differential mass distribution of remnant planetesimals is typically -2.0 and -2.7 to -2.5 for small and large m(0). The slope, q similar or equal to -2.7, and the bump at 10(21) g (or 50 km in radius) for the mass distribution of hot Kuiper belt objects are reproduced if m(0) is the bump mass. On the other hand, small initial planetesimals with m(0) similar to 10(13) g or less are favored to explain the slope of large asteroids, q similar or equal to -2.0, while the bump at 10(21) g can be reproduced by introducing a small number of asteroid seeds each with mass of 10(19) g. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Morishima, Ryuji] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Morishima, Ryuji] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Morishima, R (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
EM Ryuji.Morishima@jpl.nasa.gov
NR 90
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PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD JAN 1
PY 2017
VL 281
BP 459
EP 475
DI 10.1016/j.icarus.2016.07.019
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DY9TN
UT WOS:000385478100034
ER
PT J
AU Sung, K
Toon, GC
Crawford, TJ
AF Sung, Keeyoon
Toon, Geoffrey C.
Crawford, Timothy J.
TI N-2- and (H-2+He)-broadened cross sections of benzene (C6H6) in the 7-15
mu m region for the Titan and Jovian atmospheres (vol 271, pg 438, 2016)
SO ICARUS
LA English
DT Correction
C1 [Sung, Keeyoon; Toon, Geoffrey C.; Crawford, Timothy J.] CALTECH, Jet Prop Lab, 4800 Oak Grove, Pasadena, CA 91109 USA.
RP Sung, K (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove, Pasadena, CA 91109 USA.
EM keeyoon.sung@jpl.nasa.gov
RI Sung, Keeyoon/I-6533-2015
NR 1
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SN 0019-1035
EI 1090-2643
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JI Icarus
PD JAN 1
PY 2017
VL 281
BP 476
EP 476
DI 10.1016/j.icarus.2016.08.018
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DY9TN
UT WOS:000385478100035
ER
PT J
AU Smialek, JL
AF Smialek, James L.
TI Environmental resistance of a Ti2AlC-type MAX phase in a high pressure
burner rig
SO JOURNAL OF THE EUROPEAN CERAMIC SOCIETY
LA English
DT Article
DE Ti2AlC MAX phase; Oxidation; Scale volatility; Water vapor; Burner rig
ID SIO2 SCALE VOLATILITY; WATER-VAPOR; OXIDATION BEHAVIOR; COMBUSTION
CONDITIONS; NITRIDE MATERIALS; SILICON-NITRIDE; GAS-TURBINE; AIR;
TI3ALC2; RECESSION
AB Alumina-forming commercial Ti2AlC (MAXthal 211)(TM) phase samples were exposed in a jet-fueled, high pressure burner rig (HPBR) at 1100 degrees, 1200 degrees, and 1300 degrees C, operating at 6 atm (bar) and 25 m/s, in similar to 10% water vapor. Weight change exhibited a rapid initial uptake associated with a TiO2 transient phase followed by cubic kinetics of a slow-growing alpha-Al2O3 underlayer. The cubic rate constants, k(c), were approximately 20% of those measured in static thermo-balance furnace tests. A small recession rate of -0.012 mg/cm(2)/h was measured at 1300 degrees C for a pre-oxidized sample. The loss rate was similar to 15% that observed for SiO2 scales subject to volatile Si(OH)(4) formation for SiC tested under similar conditions. These kinetic features were fitted in a modified cubic-linear law. From thermodynamic, XRD, and SEM analyses, it is proposed that volatile TiO(OH)(2) was formed by the reaction of water vapor with TiO2 and TiAl2O5 outer layers. Published by Elsevier Ltd.
C1 [Smialek, James L.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Smialek, JL (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM James.L.Smialek@nasa.gov
OI Smialek, James/0000-0003-4310-5569
FU NASA Aeronautics Research Mission Directorate hot section and
transformational technologies research programs
FX The author acknowledges Robert Pastel for his dedicated and expert
maintenance and operation of the NASA Glenn Research Center High
Pressure Burner Rig Facility, as well as conducting all MAX phase sample
exposures presented here. Dr. Nathan S. Jacobson is thanked for his
extensive and detailed thermodynamic/gaseous diffusion model
calculations in the Appendix and for helpful comments on the manuscript.
Insightful SEM characterizations were provided by Dr. Anita Garg and
X-ray diffraction analyses by Dr. Richard Rogers. This study was
supported by the NASA Aeronautics Research Mission Directorate hot
section and transformational technologies research programs. The HPBR
has since been decommissioned.
NR 43
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U1 22
U2 22
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0955-2219
EI 1873-619X
J9 J EUR CERAM SOC
JI J. Eur. Ceram. Soc.
PD JAN
PY 2017
VL 37
IS 1
BP 23
EP 34
DI 10.1016/j.jeurceramsoc.2016.07.038
PG 12
WC Materials Science, Ceramics
SC Materials Science
GA DY1JX
UT WOS:000384852400003
ER
PT J
AU Li, ZJ
Cheng, XP
Gustafson, WI
Vogelmann, AM
AF Li, Zhijin
Cheng, Xiaoping
Gustafson, William I., Jr.
Vogelmann, Andrew M.
TI Spectral characteristics of background error covariance and multiscale
data assimilation
SO INTERNATIONAL JOURNAL FOR NUMERICAL METHODS IN FLUIDS
LA English
DT Article
DE Variational data assimilation; Kalman Filter; atmospheric and oceanic
models; multiscale algorithm; background error covariance; spectral
power density
ID VARIATIONAL DATA ASSIMILATION; ENSEMBLE KALMAN FILTER; ATMOSPHERIC DATA
ASSIMILATION; PART I; ANALYSIS SYSTEM; SCHEME; FORMULATION; CLOUD;
IMPLEMENTATION; PREDICTION
AB The spatial resolutions of numerical atmospheric and oceanic circulation models have steadily increased over the past decades. Horizontal grid spacing down to the order of 1 km is now often used to resolve cloud systems in the atmosphere and sub-mesoscale circulation systems in the ocean. These fine resolution models encompass a wide range of temporal and spatial scales, across which dynamical and statistical properties vary. In particular, dynamic flow systems at small scales can be spatially localized and temporarily intermittent. Difficulties of current data assimilation algorithms for such fine resolution models are numerically and theoretically examined. An analysis shows that the background error correlation length scale is larger than 75 km for streamfunctions and is larger than 25 km for water vapor mixing ratios, even for a 2-km resolution model. A theoretical analysis suggests that such correlation length scales prevent the currently used data assimilation schemes from constraining spatial scales smaller than 150 km for streamfunctions and 50 km for water vapor mixing ratios. These results highlight the need to fundamentally modify currently used data assimilation algorithms for assimilating high-resolution observations into the aforementioned fine resolution models. Within the framework of four-dimensional variational data assimilation, a multiscale methodology based on scale decomposition is suggested and challenges are discussed. Copyright (C) 2016 John Wiley & Sons, Ltd.
C1 [Li, Zhijin] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
[Cheng, Xiaoping] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA USA.
[Gustafson, William I., Jr.] Pacific Northwest Natl Lab, Richland, WA USA.
[Vogelmann, Andrew M.] Brookhaven Natl Lab, Upton, NY 11973 USA.
RP Li, ZJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM Zhijin.Li@jpl.nasa.gov
RI Gustafson, William/A-7732-2008; Vogelmann, Andrew/M-8779-2014
OI Gustafson, William/0000-0001-9927-1393; Vogelmann,
Andrew/0000-0003-1918-5423
FU National Aeronautics and Space Administration (NASA); U.S. Department of
Energy Atmospheric Radiation Measurement Climate Research Facility via
Pacific Northwest National Laboratory (PNNL); DOE [DE-AC05-76RL01830];
Atmospheric System Research Program [DE-SC00112704]
FX The research described in this publication was carried out, in part, at
the Jet Propulsion Laboratory (JPL), California Institute of Technology,
under a contract with the National Aeronautics and Space Administration
(NASA). This research was supported in part by the U.S. Department of
Energy Atmospheric Radiation Measurement Climate Research Facility via a
subcontract from the Pacific Northwest National Laboratory (PNNL). PNNL
is operated for DOE by Battelle Memorial Institute under contract
DE-AC05-76RL01830 and the BNL contribution is through the Atmospheric
System Research Program via DE-SC00112704. ZL is deeply grateful to
Prof. I. Michael Navon for his continued encouragement, invaluable
advice, and gracious support since the days when ZL was a postdoc
working with him 20 years ago. The authors thank the anonymous reviewers
for comments that were very helpful for improving the manuscript.
NR 51
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Z9 0
U1 5
U2 5
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0271-2091
EI 1097-0363
J9 INT J NUMER METH FL
JI Int. J. Numer. Methods Fluids
PD DEC 30
PY 2016
VL 82
IS 12
BP 1035
EP 1048
DI 10.1002/fld.4253
PG 14
WC Computer Science, Interdisciplinary Applications; Mathematics,
Interdisciplinary Applications; Mechanics; Physics, Fluids & Plasmas
SC Computer Science; Mathematics; Mechanics; Physics
GA ED4CW
UT WOS:000388796000013
ER
PT J
AU Schiller, Q
Kanekal, SG
Jian, LK
Li, X
Jones, A
Baker, DN
Jaynes, A
Spence, HE
AF Schiller, Q.
Kanekal, S. G.
Jian, L. K.
Li, X.
Jones, A.
Baker, D. N.
Jaynes, A.
Spence, H. E.
TI Prompt injections of highly relativistic electrons induced by
interplanetary shocks: A statistical study of Van Allen Probes
observations
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID ENERGETIC PARTICLE INJECTIONS; 24 MARCH 1991; DRIFT ECHOES; INNER
MAGNETOSPHERE; ACCELERATION; SUBSTORMS; TRANSPORT; ENERGIZATION;
SIMULATION; ENERGIES
AB We conduct a statistical study on the sudden response of outer radiation belt electrons due to interplanetary (IP) shocks during the Van Allen Probes era, i.e., 2012 to 2015. Data from the Relativistic Electron-Proton Telescope instrument on board Van Allen Probes are used to investigate the highly relativistic electron response (E > 1.8 MeV) within the first few minutes after shock impact. We investigate the relationship of IP shock parameters, such as Mach number, with the highly relativistic electron response, including spectral properties and radial location of the shock-induced injection. We find that the driving solar wind structure of the shock does not affect occurrence for enhancement events, 25% of IP shocks are associated with prompt energization, and 14% are associated with MeV electron depletion. Parameters that represent IP shock strength are found to correlate best with highest levels of energization, suggesting that shock strength may play a key role in the severity of the enhancements. However, not every shock results in an enhancement, indicating that magnetospheric preconditioning may be required.
C1 [Schiller, Q.; Kanekal, S. G.; Jian, L. K.; Jones, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Jian, L. K.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Li, X.; Baker, D. N.; Jaynes, A.] Univ Colorado Boulder, Lab Atmospher & Space Sci, Boulder, CO USA.
[Spence, H. E.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
RP Schiller, Q (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM quintin.schiller@nasa.gov
OI Jones, Ashley/0000-0002-7394-3638; Jian, Lan/0000-0002-6849-5527;
Spence, Harlan/0000-0002-2526-2205; LI, XINLIN/0000-0002-1683-3192
FU NASA
FX The results presented in this paper rely on data collected at ground
magnetic observatories; we thank the national institutes that support
them and INTERMAGNET for promoting high standards of magnetic
observatory practice (www.intermagnet.org). This paper also uses data
from the Heliospheric Shock Database, generated and maintained at the
University of Helsinki. The authors would like to acknowledge the ACE
and Wind teams for supplying solar wind and interplanetarymagnetic field
information and the Van Allen Probes REPT team and the Van Allen Probe
online database http://rbspgway.jhuapl.edu/data_instrumentationSOC.
Additionally, the authors would like to thank David Sibeck for
insightful discussion regarding this work. This study was supported by
an appointment to the NASA Postdoctoral Program at Goddard Space Flight
Center, administered by the Universities Space Research Association
through a contract with NASA.
NR 29
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U1 2
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD DEC 28
PY 2016
VL 43
IS 24
BP 12317
EP 12324
DI 10.1002/2016GL071628
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA EI8FT
UT WOS:000392741900002
ER
PT J
AU Otto, KA
Jaumann, R
Krohn, K
Spahn, F
Raymond, CA
Russell, CT
AF Otto, K. A.
Jaumann, R.
Krohn, K.
Spahn, F.
Raymond, C. A.
Russell, C. T.
TI The Coriolis effect on mass wasting during the Rheasilvia impact on
asteroid Vesta
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID ACOUSTIC FLUIDIZATION; DAWN; GRAVITY; LANDSLIDES; MOBILITY; PHYSICS;
MODELS; SHAPE; POLE
AB We investigate the influence of the Coriolis force on mass motion related to the Rheasilvia impact on asteroid Vesta. Observations by the NASA Dawn mission revealed a pattern of curved radial ridges, which are related to Coriolis-deflected mass-wasting during the initial modification stage of the crater. Utilizing the projected curvature of the mass-wasting trajectories, we developed a method that enabled investigation of the initial mass wasting of the Rheasilvia impact by observational means. We demonstrate that the Coriolis force can strongly affect the crater formation processes on rapidly rotating objects, and we derive the material's velocities (28.9 +/- 22.5 m/s), viscosities (1.5-9.0 x 10(6) Pa s) and coefficients of friction (0.02-0.81) during the impact modification stage. The duration of the impact modification stage could be estimated to (1.1 +/- 0.5) h. By analyzing the velocity distribution with respect to the topography, we deduce that the Rheasilvia impactor hit a heterogeneous target and that the initial crater walls were significantly steeper during the modification stage.
C1 [Otto, K. A.; Jaumann, R.; Krohn, K.] Deutsch Zentrum Luft & Raumfahrt, Inst Planetary Res, Berlin, Germany.
[Jaumann, R.] Free Univ Berlin, Inst Geol Sci, Berlin, Germany.
[Spahn, F.] Univ Potsdam, Inst Phys & Astron, Potsdam, Germany.
[Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Russell, C. T.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA.
RP Otto, KA (reprint author), Deutsch Zentrum Luft & Raumfahrt, Inst Planetary Res, Berlin, Germany.
EM katharina.otto@dlr.de
OI Russell, Christopher/0000-0003-1639-8298; Krohn,
Katrin/0000-0001-8518-4985
NR 28
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U1 1
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD DEC 28
PY 2016
VL 43
IS 24
BP 12340
EP 12347
DI 10.1002/2016GL071539
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA EI8FT
UT WOS:000392741900005
ER
PT J
AU Chu, W
Schroeder, DM
Seroussi, H
Creyts, TT
Palmer, SJ
Bell, RE
AF Chu, Winnie
Schroeder, Dustin M.
Seroussi, Helene
Creyts, Timothy T.
Palmer, Steven J.
Bell, Robin E.
TI Extensive winter subglacial water storage beneath the Greenland Ice
Sheet
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID LAND-TERMINATING SECTOR; WEST GREENLAND; DRAINAGE SYSTEM; SURFACE
MELTWATER; RADAR ATTENUATION; FLOW VARIABILITY; BASAL CONDITIONS; EAST
ANTARCTICA; RUSSELL GLACIER; GROUNDING-ZONE
AB Surface meltwater that reaches the base of the Greenland Ice Sheet exerts a fundamental impact on ice flow, but observations of catchment-wide movement and distribution of subglacial water remain limited. Using radar-sounding data from two seasons, we identify the seasonal distribution of subglacial water in western Greenland. Our analysis provides evidence of widespread subglacial water storage beneath Greenland in the wintertime. The winter storage is located primarily on bedrock ridges with higher bed elevations in excess of 200 m. During the melt season water moves to the subglacial troughs. This inverse relationship with topography indicates that the material properties of the glacier bed strongly influence subglacial drainage development. Both the spatial variations in bed properties and the initial state of the subglacial hydrology system at the start of the melt season lead to differing glacier dynamical responses to surface melting across the Greenland Ice Sheet.
C1 [Chu, Winnie; Creyts, Timothy T.; Bell, Robin E.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Schroeder, Dustin M.] Stanford Univ, Dept Geophys, Sch Earth Energy & Environm Sci, Stanford, CA 94305 USA.
[Seroussi, Helene] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Palmer, Steven J.] Univ Exeter, Coll Life & Environm Sci, Exeter, Devon, England.
RP Chu, W (reprint author), Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
EM wchu@ldeo.columbia.edu
OI Palmer, Steven/0000-0003-3977-8509; Chu, Winnie/0000-0002-8107-7450;
Schroeder, Dustin/0000-0003-1916-3929
FU NASA Earth and Space Science Fellowship; NASA Cryospheric Sciences
Program; NASA Sea Level Rise Program; National Science Foundation (NSF);
NASA Cryospheric Sciences; Natural Environment Research Council's Centre
for Polar Observation
FX W.C. is a recipient of the NASA Earth and Space Science Fellowship.
D.M.S. is supported by a grant from the NASA Cryospheric Sciences
Program. H.S. is supported by grants from the NASA Cryospheric Sciences
and Sea Level Rise Programs. T.T.C and R.E.B are supported by grants
from National Science Foundation (NSF) and NASA Cryospheric Sciences.
S.P. is supported by the Natural Environment Research Council's Centre
for Polar Observation. The radar data central to this work are provided
by CReSIS from the University of Kansas. We thank Julienne Stroeve,
Joseph MacGregor, and an anonymous referee for their constructive
comments on this manuscript. We are grateful to Indrani Das, Jonathan
Kingslake, Kirsty Tinto, and Timothy Bartholomaus for their suggestions
for this work. Results produced in the paper are available upon request
to the corresponding author. Radar data are available on the CReSIS data
repository at https://data.cresis.ku.edu/data/rds/.
NR 79
TC 0
Z9 0
U1 7
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD DEC 28
PY 2016
VL 43
IS 24
BP 12484
EP 12492
DI 10.1002/2016GL071538
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA EI8FT
UT WOS:000392741900022
ER
PT J
AU Brown, PT
Li, WH
Jiang, JH
Su, H
AF Brown, Patrick T.
Li, Wenhong
Jiang, Jonathan H.
Su, Hui
TI Spread in the magnitude of climate model interdecadal global temperature
variability traced to disagreements over high-latitude oceans
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID MERIDIONAL OVERTURNING CIRCULATION; DECADAL VARIABILITY; DEEP
CONVECTION; HIATUS PERIODS; WARMING HIATUS; PACIFIC; ATLANTIC;
MECHANISMS; DRIVER
AB Unforced variability in global mean surface air temperature can obscure or exaggerate global warming on interdecadal time scales; thus, understanding both the magnitude and generating mechanisms of such variability is of critical importance for both attribution studies as well as decadal climate prediction. Coupled atmosphere-ocean general circulation models (climate models) simulate a wide range of magnitudes of unforced interdecadal variability in global mean surface air temperature (UITglobal), hampering efforts to quantify the influence of UITglobal on contemporary global temperature trends. Recently, a preliminary consensus has emerged that unforced interdecadal variability in local surface temperatures (UITlocal) over the tropical Pacific Ocean is particularly influential on UITglobal. Therefore, a reasonable hypothesis might be that the large spread in the magnitude of UITglobal across climate models can be explained by the spread in the magnitude of simulated tropical Pacific UITlocal. Here we show that this hypothesis is mostly false. Instead, the spread in the magnitude of UITglobal is linked much more strongly to the spread in the magnitude of UITlocal over high-latitude regions characterized by significant variability in oceanic convection, sea ice concentration, and energy flux at both the surface and the top of the atmosphere. Thus, efforts to constrain the climate model produced range of UITglobal magnitude would be best served by focusing on the simulation of air-sea interaction at high latitudes.
C1 [Brown, Patrick T.; Li, Wenhong] Duke Univ, Nicholas Sch Environm, Earth & Ocean Sci, Durham, NC 27708 USA.
[Jiang, Jonathan H.; Su, Hui] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Brown, PT (reprint author), Duke Univ, Nicholas Sch Environm, Earth & Ocean Sci, Durham, NC 27708 USA.
EM Patrick.Brown@duke.edu
OI Brown, Patrick/0000-0002-5058-1718
FU NIH [NIH-1R21AG044294-01A1]; NASA MAP program; NASA NEWS program; NASA
FX We acknowledge the World Climate Research Programme's Working Group on
Coupled Modelling, which is responsible for CMIP, and we thank the
climate modeling groups for producing and making available their model
output. For CMIP the U.S. Department of Energy's Program for Climate
Model Diagnosis and Intercomparison provides coordinating support and
led development of software infrastructure in partnership with the
Global Organization for Earth System Science Portals. The CMIP5 data
used for this study can be downloaded at
http://cmip-pcmdi.llnl.gov/cmip5/data_portal.html. Contact Patrick Brown
(patrick.brown@duke.edu) for other data and code requests. This work was
partially supported by the NIH grant NIH-1R21AG044294-01A1 and NASA MAP
and NEWS programs. J.H.J. and H.S. conducted the work at the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with NASA.
NR 31
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U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD DEC 28
PY 2016
VL 43
IS 24
BP 12543
EP 12549
DI 10.1002/2016GL071442
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA EI8FT
UT WOS:000392741900029
ER
PT J
AU Garay, MJ
Davis, AB
Diner, DJ
AF Garay, Michael J.
Davis, Anthony B.
Diner, David J.
TI Tomographic reconstruction of an aerosol plume using passive multiangle
observations from the MISR satellite instrument
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID COMPUTED-TOMOGRAPHY; RETRIEVALS; ALGORITHM
AB We present initial results using computed tomography to reconstruct the three-dimensional structure of an aerosol plume from passive observations made by the Multi-angle Imaging SpectroRadiometer (MISR) instrument on NASA's Terra satellite. MISR views the Earth from nine different angles at four visible and near-infrared wavelengths. Adopting the 672 nm channel, we treat each view as an independent measure of aerosol optical thickness along the line of sight at 1.1 km resolution. A smoke plume over dark water is selected as it provides a more tractable lower boundary condition for the retrieval. A tomographic algorithm is used to reconstruct the horizontal and vertical aerosol extinction field for one along-track slice from the path of all camera rays passing through a regular grid. The results compare well with ground-based lidar observations from a nearby Micropulse Lidar Network site.
C1 [Garay, Michael J.; Davis, Anthony B.; Diner, David J.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Garay, MJ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Michael.J.Garay@jpl.nasa.gov
OI Davis, Anthony/0000-0003-1279-1420
FU NASA's MISR Science Activity; Remote Sensing Theory (RST) program;
Advanced Information Systems Technology (AIST) program; National
Aeronautics and Space Administration (NASA); NASA Radiation Science
Program; Earth Observing System
FX The authors acknowledge support from NASA's MISR Science Activity, the
Remote Sensing Theory (RST), and Advanced Information Systems Technology
(AIST) programs. This work was performed at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration (NASA). The MISR data
used in this work were obtained from the NASA Langley Research Center
Atmospheric Science Data Center. The MPLNET project is funded by the
NASA Radiation Science Program and Earth Observing System. We thank the
MPLNET PIs, Judd Welton and John Barnes, for their efforts in
establishing and maintaining the Trinidad Head site. We also thank Brent
Holben for his effort in establishing and maintaining the Trinidad Head
AERONET site. Many thanks to Michele Cappellari, University of Oxford,
for his IDL (TM) port of the BLVS code. Copyright 2016 California
Institute of Technology. U.S. Government sponsorship acknowledged.
NR 19
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U1 0
U2 0
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD DEC 28
PY 2016
VL 43
IS 24
BP 12590
EP 12596
DI 10.1002/2016GL071479
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA EI8FT
UT WOS:000392741900034
ER
PT J
AU Solomon, S
Kinnison, D
Garcia, RR
Bandoro, J
Mills, M
Wilka, C
Neely, RR
Schmidt, A
Barnes, JE
Vernier, JP
Hopfner, M
AF Solomon, Susan
Kinnison, Doug
Garcia, Rolando R.
Bandoro, Justin
Mills, Michael
Wilka, Catherine
Neely, Ryan R., III
Schmidt, Anja
Barnes, John E.
Vernier, Jean-Paul
Hoepfner, Michael
TI Monsoon circulations and tropical heterogeneous chlorine chemistry in
the stratosphere
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID IN-SITU MEASUREMENTS; WATER-VAPOR; OZONE DEPLETION; AIRCRAFT
MEASUREMENTS; HALOGEN CHEMISTRY; SUMMER MONSOON; AEROSOL; TRANSPORT;
EXTINCTION; CLIMATE
AB Model simulations presented in this paper suggest that transport processes associated with the summer monsoons bring increased abundances of hydrochloric acid into contact with liquid sulfate aerosols in the cold tropical lowermost stratosphere, leading to heterogeneous chemical activation of chlorine species. The calculations indicate that the spatial and seasonal distributions of chlorine monoxide and chlorine nitrate near the monsoon regions of the northern hemisphere tropical and subtropical lowermost stratosphere could provide indicators of heterogeneous chlorine processing. In the model, these processes impact the local ozone budget and decrease ozone abundances, implying a chemical contribution to longer-term northern tropical ozone profile changes at 16-19 km.
C1 [Solomon, Susan; Bandoro, Justin; Wilka, Catherine] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Kinnison, Doug; Garcia, Rolando R.; Mills, Michael] Natl Ctr Atmospher Res, Atmospher Chem Observat & Modeling Lab, POB 3000, Boulder, CO 80307 USA.
[Neely, Ryan R., III; Schmidt, Anja] Univ Leeds, Sch Earth & Environm, Leeds, W Yorkshire, England.
[Neely, Ryan R., III] Univ Leeds, Natl Ctr Atmospher Sci, Leeds, W Yorkshire, England.
[Barnes, John E.] NOAA, Mauna Loa Observ, Hilo, HI USA.
[Vernier, Jean-Paul] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Vernier, Jean-Paul] Sci Syst & Applicat Inc, Hampton, VA USA.
[Hoepfner, Michael] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, Karlsruhe, Germany.
RP Solomon, S (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
EM solos@mit.edu; mmills@ucar.edu
OI Neely, Ryan/0000-0003-4560-4812; Wilka, Catherine/0000-0002-2917-1140;
Schmidt, Anja/0000-0001-8759-2843; Mills, Michael/0000-0002-8054-1346;
Kinnison, Douglas/0000-0002-3418-0834
FU Natural Environment Research Council through National Centre for
Atmospheric Science in the UK; Academic Research Fellowship from
University of Leeds; National Center for Atmospheric Research (NCAR);
NOAA/ESRL/GMD; U.S. National Science Foundation; National Science
Foundation (NSF); Office of Science of the U.S. Department of Energy;
NSF; [NSF-1539972]; [NSF-1419667]
FX We thank Dan Murphy and Brian Toon for their helpful discussions. S.S.
and J.B. acknowledge funding under NSF-1539972 and NSF-1419667. R.N. is
supported by the Natural Environment Research Council through the
National Centre for Atmospheric Science in the UK. A.S. was supported by
an Academic Research Fellowship from the University of Leeds and a
National Center for Atmospheric Research (NCAR) visiting researcher
grant. J.E.B. is funded by NOAA/ESRL/GMD. NCAR is sponsored by the U.S.
National Science Foundation. Any opinions, findings, and conclusions or
recommendations expressed in the publication are those of the author(s)
and do not necessarily reflect the views of the National Science
Foundation. WACCM is a component of the Community Earth System Model
(CESM), which is supported by the National Science Foundation (NSF) and
the Office of Science of the U.S. Department of Energy. Computing
resources were provided by NCAR's Climate Simulation Laboratory,
sponsored by NSF and other agencies. This research was enabled by the
computational and storage resources of NCAR's Computational and
Information System Laboratory. We thank NASA Goddard Space Flight Center
for the MERRA data (accessed freely online at
http://disc.sci.gsfc.nasa.gov/) and the Aura MLS team for HCl data
(accessed freely online at
http://disc.sci.gsfc.nasa.gov/Aura/data-holdings/MLS). Mauna Loa lidar
data shown in this paper may be accessed at http://ndacc-lidar.org/.
Model results shown in this paper are available on request to the WACCM
liaison, Michael Mills mmills@ucar.edu.
NR 50
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Z9 0
U1 1
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD DEC 28
PY 2016
VL 43
IS 24
BP 12624
EP 12633
DI 10.1002/2016GL071778
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA EI8FT
UT WOS:000392741900038
ER
PT J
AU Deng, ZX
Scheidler, JJ
Asnani, VM
Dapino, MJ
AF Deng, Zhangxian
Scheidler, Justin J.
Asnani, Vivake M.
Dapino, Marcelo J.
TI Quasi-static major and minor strain-stress loops in textured
polycrystalline Fe81.6Ga18.4 Galfenol
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
ID IRON-GALLIUM ALLOYS; HYSTERESIS; VIBRATION; BEHAVIOR; FIELD; MODEL
AB The Delta E effect (Young's modulus variation of magnetostrictive materials) is useful for tunable vibration absorption and stiffness control. The Delta E effect of iron-gallium (Galfenol) has not been fully characterized. In this study, major and minor strain-stress loops were measured under different bias magnetic fields in solid, research grade, < 100 >-oriented, highly-textured polycrystalline Fe81.6Ga18.4 Galfenol. A 1 Hz, constant amplitude compressive stress was applied from 0.5 MPa to 63.3 MPa for major loop responses. Minor loops were generated by simultaneously applying a 4 Hz, 2.88 MPa amplitude sinusoidal stress and different bias stresses ranging from 5.7 MPa to 41.6 MPa in increments of about 7.2 MPa. Bias magnetic fields were applied in two ways, a constant field in the sample obtained using a proportional-integral (PI) controller and a constant current in the excitation coils. The Delta E effect was quantified from major and minor loop measurements. The maximum Delta E effect is 54.84% and 39.01% for constant field and constant current major loops, respectively. For constant field and constant current minor loops, the maximum Delta E effect is 37.90% and 27.46%, respectively. A laminated sample of the same material was tested under constant current conditions. The saturation modulus of this material is 59.54 GPa, or 82.65% of the solid rod's saturation modulus, due in part to the soft adhesive layers. The minimum modulus calculated from major loops is 36.31 GPa, which corresponds to a 39.02% Delta E effect. A new optimization procedure is presented on the basis of an existing discrete energy-averaged model to incorporate measurement uncertainties. The model was optimized to both major and minor loop data; model parameters with 95% confidence intervals are presented. Published by AIP Publishing.
C1 [Deng, Zhangxian; Dapino, Marcelo J.] Ohio State Univ, Dept Mech & Aerosp Engn, Columbus, OH 43210 USA.
[Scheidler, Justin J.] NASA, Univ Space Res Assoc, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Asnani, Vivake M.] NASA, Rotating & Drive Syst Branch, Mat & Struct Div, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Dapino, MJ (reprint author), Ohio State Univ, Dept Mech & Aerosp Engn, Columbus, OH 43210 USA.
EM dapino.1@osu.edu
FU NASA Aeronautics Scholarship Program [NNX14AE24H]; NASA Aeronautics
Research Mission Directorate Seedling Fund; Smart Vehicle Concepts
Center, a National Science Foundation Industry/University Cooperative
Research Center created under NSF [IIP-1238286]
FX This work was supported by the NASA Aeronautics Scholarship Program
(Grant No. NNX14AE24H). Additional support was provided by the NASA
Aeronautics Research Mission Directorate Seedling Fund and the Smart
Vehicle Concepts Center, a National Science Foundation
Industry/University Cooperative Research Center created under NSF Grant
IIP-1238286.
NR 34
TC 0
Z9 0
U1 6
U2 6
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0021-8979
EI 1089-7550
J9 J APPL PHYS
JI J. Appl. Phys.
PD DEC 28
PY 2016
VL 120
IS 24
AR 243901
DI 10.1063/1.4972479
PG 11
WC Physics, Applied
SC Physics
GA EI0OO
UT WOS:000392174000007
ER
PT J
AU Klocko, AD
Ormsby, T
Galazka, JM
Leggett, NA
Uesaka, M
Honda, S
Freitag, M
Selker, EU
AF Klocko, Andrew D.
Ormsby, Tereza
Galazka, Jonathan M.
Leggett, Neena A.
Uesaka, Miki
Honda, Shinji
Freitag, Michael
Selker, Eric U.
TI Normal chromosome conformation depends on subtelomeric facultative
heterochromatin in Neurospora crassa
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE Hi-C; facultative heterochromatin; H3K27me2/3; PRC2; Neurospora crassa
ID DNA METHYLATION; DROSOPHILA GENOME; HISTONE; PRINCIPLES; HP1;
ORGANIZATION; ARCHITECTURE; RECOGNITION; ARABIDOPSIS; MECHANISMS
AB High-throughput chromosome conformation capture (Hi-C) analyses revealed that the 3D structure of the Neurospora crassa genome is dominated by intra-and interchromosomal links between regions of heterochromatin, especially constitutive heterochromatin. Elimination of trimethylation of lysine 9 on histone H3 (H3K9me3) or its binding partner Heterochromatin Protein 1 (HP1)-both prominent features of constitutive heterochromatin-have little effect on the HiC pattern. It remained possible that di- or trimethylation of lysine 27 on histone H3 (H3K27me2/3), which becomes localized in regions of constitutive heterochromatin when H3K9me3 or HP1 are lost, plays a critical role in the 3D structure of the genome. We found that H3K27me2/3, catalyzed by the Polycomb Repressive Complex 2 (PRC2) member SET-7 (SET domain protein-7), does indeed play a prominent role in the Hi-C pattern of WT, but that its presence in regions normally occupied by H3K9me3 is not responsible for maintenance of the genome architecture when H3K9me3 is lost. The Hi-C pattern of a mutant defective in the PRC2 member N. crassa p55 (NPF), which is predominantly required for subtelomeric H3K27me2/3, was equivalent to that of the set-7 deletion strain, suggesting that subtelomeric facultative heterochromatin is paramount for normal chromosome conformation. Both PRC2 mutants showed decreased heterochromatin-heterochromatin contacts and increased euchromatin-heterochromatin contacts. Cytological observations suggested elimination of H3K27me2/3 leads to partial displacement of telomere clusters from the nuclear periphery. Transcriptional profiling of Delta dim-5, Delta set-7, Delta set-7; Delta dim-5, and Delta npf strains detailed anticipated changes in gene expression but did not support the idea that global changes in genome architecture, per se, led to altered transcription.
C1 [Klocko, Andrew D.; Ormsby, Tereza; Leggett, Neena A.; Selker, Eric U.] Univ Oregon, Inst Mol Biol, Eugene, OR 97403 USA.
[Galazka, Jonathan M.; Freitag, Michael] Oregon State Univ, Dept Biochem & Biophys, Corvallis, OR 97331 USA.
[Uesaka, Miki; Honda, Shinji] Univ Fukui, Div Chromosome Biol, Fac Med Sci, Fukui 9101193, Japan.
[Galazka, Jonathan M.] NASA, Ames Res Ctr, Space Biosci Div, Moffett Field, CA 94035 USA.
RP Selker, EU (reprint author), Univ Oregon, Inst Mol Biol, Eugene, OR 97403 USA.
EM selker@uoregon.edu
FU NIH [GM035690, GM093061, GM097637, GM097821]; Competitive Funds in
Program to Disseminate Tenure Tracking System, Ministry of Education,
Culture, Sports, Science and Technology (MEXT), Japan; NASA
FX We thank Vince Bicocca (University of Oregon) for the use of unpublished
ChIP-seq data, Diana Libuda (University of Oregon) for the use of the
deconvolution microscope, and Ayumi Yokoyama (University of Fukui) for
technical support. This study was supported by NIH Grants GM035690 (to
E.U.S.), GM093061 (to E.U.S.), and GM097637 (to M.F.); a Competitive
Funds in Program to Disseminate Tenure Tracking System, Ministry of
Education, Culture, Sports, Science and Technology (MEXT), Japan, grant
(to S.H.); NIH Postdoctoral Fellowship GM097821 (to A.D.K.); and a NASA
postdoctoral fellowship (to J.M.G.).
NR 41
TC 2
Z9 2
U1 9
U2 9
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD DEC 27
PY 2016
VL 113
IS 52
BP 15048
EP 15053
DI 10.1073/pnas.1615546113
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EG5NL
UT WOS:000391090800049
PM 27856763
ER
PT J
AU He, M
Hu, YX
Huang, JP
Stamnes, K
AF He, Min
Hu, Yongxiang
Huang, Jian Ping
Stamnes, Knut
TI Aerosol optical depth under "clear" sky conditions derived from sea
surface reflection of lidar signals
SO OPTICS EXPRESS
LA English
DT Article
ID ATMOSPHERIC CORRECTION; RAYLEIGH-SCATTERING; WIND-SPEED; SATELLITE;
OCEAN; DEPOLARIZATION; ALGORITHMS
AB There are considerable demands for accurate atmospheric correction of satellite observations of the sea surface or subsurface signal. Surface and sub-surface reflection under "clear" atmospheric conditions can be used to study atmospheric correction for the simplest possible situation. Here "clear" sky means a cloud-free atmosphere with sufficiently small aerosol particles. The "clear" aerosol concept is defined according to the spectral dependence of the scattering cross section on particle size. A 5-year combined CALIPSO and AMSR-E data set was used to derive the aerosol optical depth (AOD) from the lidar signal reflected from the sea surface. Compared with the traditional lidar-retrieved AOD, which relies on lidar backscattering measurements and an assumed lidar ratio, the AOD retrieved through the surface reflectance method depends on both scattering and absorption because it is based on two-way attenuation of the lidar signal transmitted to and then reflected from the surface. The results show that the clear sky AOD derived from the surface signal agrees with the clear sky AOD available in the CALIPSO level 2 database in the westerly wind belt located in the southern hemisphere, but yields significantly higher aerosol loadings in the tropics and in the northern hemisphere. (C) 2016 Optical Society of America
C1 [He, Min; Stamnes, Knut] Stevens Inst Technol, Hoboken, NJ 07030 USA.
[Hu, Yongxiang] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Huang, Jian Ping] Lanzhou Univ, Coll Atmospher Sci, Minist Educ, Key Lab Semiarid Climate Change, Lanzhou 730000, Peoples R China.
RP He, M (reprint author), Stevens Inst Technol, Hoboken, NJ 07030 USA.
EM mhe1@stevens.edu
RI Hu, Yongxiang/K-4426-2012
NR 43
TC 0
Z9 0
U1 3
U2 3
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD DEC 26
PY 2016
VL 24
IS 26
BP A1618
EP A1634
DI 10.1364/OE.24.0A1618
PG 17
WC Optics
SC Optics
GA EG1RE
UT WOS:000390809100012
PM 28059358
ER
PT J
AU Yang, QG
Liu, X
Wu, W
Kizer, S
Baize, RR
AF Yang, Qiguang
Liu, Xu
Wu, Wan
Kizer, Susan
Baize, Rosemary R.
TI Fast and accurate hybrid stream PCRTM-SOLAR radiative transfer model for
reflected solar spectrum simulation in the cloudy atmosphere
SO OPTICS EXPRESS
LA English
DT Article
ID DISCRETE-ORDINATE-METHOD; MULTIPLE-SCATTERING; PLANETARY-ATMOSPHERES;
POLARIZED-LIGHT; REGION; BAND
AB A hybrid stream PCRTM-SOLAR model has been proposed for fast and accurate radiative transfer simulation. It calculates the reflected solar (RS) radiances with a fast coarse way and then, with the help of a pre-saved matrix, transforms the results to obtain the desired high accurate RS spectrum. The methodology has been demonstrated with the hybrid stream discrete ordinate (HSDO) radiative transfer (RT) model. The HSDO method calculates the monochromatic radiances using a 4-stream discrete ordinate method, where only a small number of monochromatic radiances are simulated with both 4-stream and a larger N-stream (N >= 16) discrete ordinate RT algorithm. The accuracy of the obtained channel radiance is comparable to the result from N-stream moderate resolution atmospheric transmission version 5 (MODTRAN5). The root-mean-square errors are usually less than 5x 10(-4) mW/cm(2)/sr/cm(-1). The computational speed is three to four-orders of magnitude faster than the medium speed correlated-k option MODTRAN5. This method is very efficient to simulate thousands of RS spectra under multi-layer clouds/aerosols and solar radiation conditions for climate change study and numerical weather prediction applications. (C) 2016 Optical Society of America
C1 [Yang, Qiguang; Wu, Wan; Kizer, Susan] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
[Liu, Xu; Baize, Rosemary R.] NASA Langley Res Ctr, Hampton, VA 23681 USA.
RP Liu, X (reprint author), NASA Langley Res Ctr, Hampton, VA 23681 USA.
EM xu.liu-1@nasa.gov
FU NASA CLARREO project; NASA NPP program; NASA SMD high-End Computing
(HEC) resources
FX The authors thank for the NASA CLARREO project, the NASA NPP program,
and the NASA SMD high-End Computing (HEC) resources for supporting this
work.
NR 19
TC 0
Z9 0
U1 0
U2 0
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD DEC 26
PY 2016
VL 24
IS 26
BP A1514
EP A1527
DI 10.1364/OE.24.0A1514
PG 14
WC Optics
SC Optics
GA EG1RE
UT WOS:000390809100003
PM 28059282
ER
PT J
AU Ryan, STJ
del Barrio, J
Suardiaz, R
Ryan, DF
Rosta, E
Scherman, OA
AF Ryan, Sean T. J.
del Barrio, Jesus
Suardiaz, Reynier
Ryan, Daniel F.
Rosta, Edina
Scherman, Oren A.
TI A Dynamic and Responsive Host in Action: Light-Controlled Molecular
Encapsulation
SO ANGEWANDTE CHEMIE-INTERNATIONAL EDITION
LA English
DT Article
DE host-guest systems; hydrogen bonds; macrocycles; photochemistry;
supramolecular chemistry
ID GUEST; RECOGNITION; RELEASE; AZOBENZENE; RECEPTORS; CAPTURE; BINDING;
REDOX
AB The rational design of a flexible molecular box, oAzoBox(4+), incoporating both photochromic and supramolecular recognition motifs is described. We exploit the EZ photoisomerization properties of azobenzenes to alter the shape of the cavity of the macrocycle upon absorption of light. Imidazolium motifs are used as hydrogen-bonding donor components, allowing for sequestration of small molecule guests in acetonitrile. Upon EZ photoisomerization of oAzoBox(4+) the guest is expelled from the macrocyclic cavity.
C1 [Ryan, Sean T. J.; del Barrio, Jesus; Scherman, Oren A.] Univ Cambridge, Dept Chem, Melville Lab Polymer Synth, Lensfield Rd, Cambridge CB2 1EW, England.
[del Barrio, Jesus] Schlumberger Gould Res, Madingley Rd, Cambridge CB3 0EL, England.
[Ryan, Daniel F.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Suardiaz, Reynier; Rosta, Edina] Kings Coll London, Dept Chem, London SE1 1DB, England.
RP del Barrio, J; Scherman, OA (reprint author), Univ Cambridge, Dept Chem, Melville Lab Polymer Synth, Lensfield Rd, Cambridge CB2 1EW, England.; del Barrio, J (reprint author), Schlumberger Gould Res, Madingley Rd, Cambridge CB3 0EL, England.
EM JBarrio2@slb.com; oas23@cam.ac.uk
RI Suardiaz, Reynier/B-2962-2008
OI Suardiaz, Reynier/0000-0002-1035-9020
FU Cambridge Home and European Scholarship Scheme; Robert Gardiner memorial
scholarship; Marie Curie IEF [273807]; EC for a Marie Curie fellowship
[622711]; NASA Postdoctoral Program; EPSRC [EP/G060649/1]; ERC Starting
Investigator Grant [240629]; Walters-Kundert Foundation; HECBioSim
(EPSRC) [EP/L000253/1]
FX S.T.J.R acknowledges the Cambridge Home and European Scholarship Scheme
and the Robert Gardiner memorial scholarship. J.D.B. thanks Marie Curie
IEF (project number 273807). R.S. acknowledges the EC for a Marie Curie
fellowship (project number 622711). D.F.R is supported by the NASA
Postdoctoral Program administered by the Universities Space Research
Association. This work was supported by the EPSRC (reference number
EP/G060649/1), an ERC Starting Investigator Grant (project number
240629), and a Next Generation Fellowship from the Walters-Kundert
Foundation. The authors thank HECBioSim (EPSRC grant number
EP/L000253/1) via ARCHER, and the Ada Kings HPC3 service.
Felix Cosmin Mocanu is gratefully acknowledged for assistance in the
synthesis of compound 1.
NR 37
TC 0
Z9 0
U1 9
U2 9
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA POSTFACH 101161, 69451 WEINHEIM, GERMANY
SN 1433-7851
EI 1521-3773
J9 ANGEW CHEM INT EDIT
JI Angew. Chem.-Int. Edit.
PD DEC 23
PY 2016
VL 55
IS 52
BP 16096
EP 16100
DI 10.1002/anie.201607693
PG 5
WC Chemistry, Multidisciplinary
SC Chemistry
GA EJ0CH
UT WOS:000392875700024
PM 27791303
ER
PT J
AU Zhang, Y
Xiao, XM
Guanter, L
Zhou, S
Ciais, P
Joiner, J
Sitch, S
Wu, XC
Nabel, J
Dong, JW
Kato, E
Jain, AK
Wiltshire, A
Stocker, BD
AF Zhang, Yao
Xiao, Xiangming
Guanter, Luis
Zhou, Sha
Ciais, Philippe
Joiner, Joanna
Sitch, Stephen
Wu, Xiaocui
Nabel, Julia
Dong, Jinwei
Kato, Etsushi
Jain, Atul K.
Wiltshire, Andy
Stocker, Benjamin D.
TI Precipitation and carbon-water coupling jointly control the interannual
variability of global land gross primary production
SO SCIENTIFIC REPORTS
LA English
DT Article
ID INDUCED CHLOROPHYLL FLUORESCENCE; USE EFFICIENCY; SEMIARID ECOSYSTEMS;
CLIMATE EXTREMES; DIOXIDE UPTAKE; MODELS; CYCLE; PHOTOSYNTHESIS;
FRAMEWORK; DRIVERS
AB Carbon uptake by terrestrial ecosystems is increasing along with the rising of atmospheric CO2 concentration. Embedded in this trend, recent studies suggested that the interannual variability (IAV) of global carbon fluxes may be dominated by semi-arid ecosystems, but the underlying mechanisms of this high variability in these specific regions are not well known. Here we derive an ensemble of gross primary production (GPP) estimates using the average of three data-driven models and eleven processbased models. These models are weighted by their spatial representativeness of the satellite-based solar-induced chlorophyll fluorescence (SIF). We then use this weighted GPP ensemble to investigate the GPP variability for different aridity regimes. We show that semi-arid regions contribute to 57% of the detrended IAV of global GPP. Moreover, in regions with higher GPP variability, GPP fluctuations are mostly controlled by precipitation and strongly coupled with evapotranspiration (ET). This higher GPP IAV in semi-arid regions is co-limited by supply (precipitation)-induced ET variability and GPP-ET coupling strength. Our results demonstrate the importance of semi-arid regions to the global terrestrial carbon cycle and posit that there will be larger GPP and ET variations in the future with changes in precipitation patterns and dryland expansion.
C1 [Zhang, Yao; Xiao, Xiangming; Wu, Xiaocui; Dong, Jinwei] Univ Oklahoma, Ctr Spatial Anal, Dept Microbiol & Plant Biol, Norman, OK 73019 USA.
[Xiao, Xiangming] Fudan Univ, Inst Biodivers Sci, Shanghai 200433, Peoples R China.
[Guanter, Luis] German Res Ctr Geosci GFZ, Helmholtz Ctr Potsdam, Telegrafenberg A17, D-14473 Potsdam, Germany.
[Zhou, Sha] Tsinghua Univ, Dept Hydraul Engn, State Key Lab Hydrosci & Engn, Beijing, Peoples R China.
[Ciais, Philippe] UVSQ, CNRS, CEA, Lab Sci Climat & Environm, F-91190 Gif Sur Yvette, France.
[Joiner, Joanna] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Sitch, Stephen] Univ Exeter, Coll Life & Environm Sci, Exeter EX4 4RJ, Devon, England.
[Nabel, Julia] Max Planck Inst Meteorol, Bundesstr 53, D-20146 Hamburg, Germany.
[Kato, Etsushi] Inst Appl Energy, Global Environm Program, Minato Ku, Tokyo 1050003, Japan.
[Jain, Atul K.] Univ Illinois, Dept Atmospher Sci, Urbana, IL 61821 USA.
[Wiltshire, Andy] Met Off Hadley Ctr, FitzRoy Rd, Exeter EX1 3PB, Devon, England.
[Stocker, Benjamin D.] Imperial Coll London, Dept Life Sci, Silwood Pk, Ascot SL5 7PY, Berks, England.
RP Zhang, Y; Xiao, XM (reprint author), Univ Oklahoma, Ctr Spatial Anal, Dept Microbiol & Plant Biol, Norman, OK 73019 USA.; Xiao, XM (reprint author), Fudan Univ, Inst Biodivers Sci, Shanghai 200433, Peoples R China.
EM yaozhang@ou.edu; xiangming.xiao@ou.edu
RI Jain, Atul/D-2851-2016
OI Jain, Atul/0000-0002-4051-3228
FU USDA National Institute for Food and Agriculture (NIFA)'s Agriculture
and Food Research Initiative (AFRI) [2013-69002]; Regional Approaches
for Adaptation to and Mitigation of Climate Variability and Change;
National Science Foundation EPSCoR [IIA-1301789]
FX We thank the Numerical Terradynamic Simulation Group at the University
of Montana for providing the improved MOD17 GPP and MOD16 ET datasets.
We thank the TRENDY-v4 modelers for contributing model outputs. We thank
Dr. Kaiyu Guan for discussion on the early version of the manuscript.
This study by Y.Z., X.X., X.W., and J.D. is partially supported by a
research grant (Project No. 2013-69002) through the USDA National
Institute for Food and Agriculture (NIFA)'s Agriculture and Food
Research Initiative (AFRI), Regional Approaches for Adaptation to and
Mitigation of Climate Variability and Change, and a research grant
(IIA-1301789) from the National Science Foundation EPSCoR. We thank Ms.
Sarah Xiao at Yale University for the English editing of the manuscript.
NR 56
TC 1
Z9 1
U1 13
U2 13
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2045-2322
J9 SCI REP-UK
JI Sci Rep
PD DEC 23
PY 2016
VL 6
AR 39748
DI 10.1038/srep39748
PG 9
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EG0XB
UT WOS:000390754500001
PM 28008960
ER
PT J
AU Filacchione, G
Raponi, A
Capaccioni, F
Ciarniello, M
Tosi, F
Capria, MT
De Sanctis, MC
Migliorini, A
Piccioni, G
Cerroni, P
Barucci, MA
Fornasier, S
Schmitt, B
Quirico, E
Erard, S
Bockelee-Morvan, D
Leyrat, C
Arnold, G
Mennella, V
Ammannito, E
Bellucci, G
Benkhoff, J
Bibring, JP
Blanco, A
Blecka, MI
Carlson, R
Carsenty, U
Colangeli, L
Combes, M
Combi, M
Crovisier, J
Drossart, P
Encrenaz, T
Federico, C
Fink, U
Fonti, S
Fulchignoni, M
Ip, WH
Irwin, P
Jaumann, R
Kuehrt, E
Langevin, Y
Magni, G
McCord, T
Moroz, L
Mottola, S
Palomba, E
Schade, U
Stephan, K
Taylor, F
Tiphene, D
Tozzi, GP
Beck, P
Biver, N
Bonal, L
Combe, JP
Despan, D
Flamini, E
Formisano, M
Frigeri, A
Grassi, D
Gudipati, MS
Kappel, D
Longobardo, A
Mancarella, F
Markus, K
Merlin, F
Orosei, R
Rinaldi, G
Cartacci, M
Cicchetti, A
Hello, Y
Henry, F
Jacquinod, S
Reess, JM
Noschese, R
Politi, R
Peter, G
AF Filacchione, G.
Raponi, A.
Capaccioni, F.
Ciarniello, M.
Tosi, F.
Capria, M. T.
De Sanctis, M. C.
Migliorini, A.
Piccioni, G.
Cerroni, P.
Barucci, M. A.
Fornasier, S.
Schmitt, B.
Quirico, E.
Erard, S.
Bockelee-Morvan, D.
Leyrat, C.
Arnold, G.
Mennella, V.
Ammannito, E.
Bellucci, G.
Benkhoff, J.
Bibring, J. P.
Blanco, A.
Blecka, M. I.
Carlson, R.
Carsenty, U.
Colangeli, L.
Combes, M.
Combi, M.
Crovisier, J.
Drossart, P.
Encrenaz, T.
Federico, C.
Fink, U.
Fonti, S.
Fulchignoni, M.
Ip, W. -H.
Irwin, P.
Jaumann, R.
Kuehrt, E.
Langevin, Y.
Magni, G.
McCord, T.
Moroz, L.
Mottola, S.
Palomba, E.
Schade, U.
Stephan, K.
Taylor, F.
Tiphene, D.
Tozzi, G. P.
Beck, P.
Biver, N.
Bonal, L.
Combe, J. -Ph.
Despan, D.
Flamini, E.
Formisano, M.
Frigeri, A.
Grassi, D.
Gudipati, M. S.
Kappel, D.
Longobardo, A.
Mancarella, F.
Markus, K.
Merlin, F.
Orosei, R.
Rinaldi, G.
Cartacci, M.
Cicchetti, A.
Hello, Y.
Henry, F.
Jacquinod, S.
Reess, J. M.
Noschese, R.
Politi, R.
Peter, G.
TI Seasonal exposure of carbon dioxide ice on the nucleus of comet
67P/Churyumov-Gerasimenko
SO SCIENCE
LA English
DT Article
ID IMAGING SPECTROMETER; OPTICAL-CONSTANTS; ONBOARD ROSETTA; CASSINI-VIMS;
WATER ICE; SURFACE; VIRTIS; ROTATION; TRITON; SHAPE
AB Carbon dioxide (CO2) is one of the most abundant species in cometary nuclei, but because of its high volatility, CO2 ice is generally only found beneath the surface. We report the infrared spectroscopic identification of a CO2 ice-rich surface area located in the Anhur region of comet 67P/ Churyumov-Gerasimenko. Spectral modeling shows that about 0.1% of the 80-by 60-meter area is CO2 ice. This exposed ice was observed a short time after the comet exited local winter; following the increased illumination, the CO2 ice completely disappeared over about 3 weeks. We estimate the mass of the sublimated CO2 ice and the depth of the eroded surface layer. We interpret the presence of CO2 ice as the result of the extreme seasonal changes induced by the rotation and orbit of the comet.
C1 [Filacchione, G.; Raponi, A.; Capaccioni, F.; Ciarniello, M.; Tosi, F.; Capria, M. T.; De Sanctis, M. C.; Migliorini, A.; Piccioni, G.; Cerroni, P.; Bellucci, G.; Magni, G.; Palomba, E.; Formisano, M.; Frigeri, A.; Grassi, D.; Longobardo, A.; Rinaldi, G.; Cartacci, M.; Cicchetti, A.; Noschese, R.; Politi, R.] INAF IAPS, Rome, Italy.
[Barucci, M. A.; Fornasier, S.; Erard, S.; Bockelee-Morvan, D.; Leyrat, C.; Combes, M.; Crovisier, J.; Drossart, P.; Encrenaz, T.; Fulchignoni, M.; Biver, N.; Despan, D.; Merlin, F.; Hello, Y.; Henry, F.; Jacquinod, S.; Reess, J. M.] Univ Paris Diderot, UPMC Univ Paris 06,Sorbonne Paris Cite, Sorbonne Univ,Observ Paris,Paris Sci & Letters Re, Lab Etud Spatiales & Instrumentat Astrophys,CNRS, Paris, France.
[Schmitt, B.; Quirico, E.; Carsenty, U.; Beck, P.; Bonal, L.] Univ Grenoble Alpes, CNRS, Inst Planetol & Astrophys Grenoble, Grenoble, France.
[Arnold, G.; Jaumann, R.; Kuehrt, E.; Moroz, L.; Mottola, S.; Stephan, K.; Kappel, D.; Markus, K.] DLR Deutsch Zentrums Luft & Raumfahrt, Inst Planetary Res, Berlin, Germany.
[Mennella, V.] INAF Osservatorio Capodimonte, Naples, Italy.
[Ammannito, E.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, 603 Charles Young Dr, Los Angeles, CA 90095 USA.
[Benkhoff, J.; Colangeli, L.] ESA, European Space Res & Technol Ctr, Noordwjik, Netherlands.
[Bibring, J. P.; Langevin, Y.] CNRS, Inst Astrophys Spatial, Orsay, France.
[Blanco, A.; Fonti, S.; Mancarella, F.] Univ Salento, Dipartimento Matemat & Fis Ennio De Giorgi, Lecce, Italy.
[Blecka, M. I.] Polish Acad Sci, Space Res Ctr, Warsaw, Poland.
[Carlson, R.; Gudipati, M. S.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Combi, M.] Univ Michigan, Space Phys Res Lab, Ann Arbor, MI 48109 USA.
[Federico, C.] Univ Perugia, Perugia, Italy.
[Fink, U.] Univ Arizona, Lunar Planetary Lab, Tucson, AZ 85721 USA.
[Ip, W. -H.] Natl Cent Univ, Taipei, Taiwan.
[Irwin, P.; Taylor, F.] Univ Oxford, Dept Phys, Oxford, England.
[McCord, T.; Combe, J. -Ph.] Bear Fight Inst, Winthrop, WA 98862 USA.
[Schade, U.] Helmholtz Zentrum Berlin Mat & Energie, Berlin, Germany.
[Tozzi, G. P.] INAF Osservatorio Astrofis Arcetri, Florence, Italy.
[Flamini, E.] Agenzia Spaziale Italiana, Rome, Italy.
[Orosei, R.] INAF Ist Radioastron, Bologna, Italy.
[Peter, G.] DLR, Inst Opt Sensor Syst, Berlin, Germany.
RP Filacchione, G (reprint author), INAF IAPS, Rome, Italy.
EM gianrico.filacchione@iaps.inaf.it
RI Beck, Pierre/F-3149-2011; Schmitt, Bernard/A-1064-2009; quirico,
eric/K-9650-2013; Combi, Michael/J-1697-2012;
OI Schmitt, Bernard/0000-0002-1230-6627; quirico, eric/0000-0003-2768-0694;
Combi, Michael/0000-0002-9805-0078; Palomba,
Ernesto/0000-0002-9101-6774; Tosi, Federico/0000-0003-4002-2434
FU Italian Space Agency (ASI); Centre National d'Etudes Spatiales (CNES,
France); DLR (Germany); NASA (USA); ASI; CNES; NASA JPL; National
Science Council of Taiwan [102-2112-M-008-013-MY3]; Science and
Technology Development Fund of Macao Special Administrative Region
[017/2014/A1]; Deutsche Forschungsgemeinschaft [MO 3007/1-1]
FX The authors thank the institutions and agencies that supported this
work: the Italian Space Agency (ASI), Centre National d'Etudes Spatiales
(CNES, France), DLR (Germany), and NASA (USA). VIRTIS was built by a
consortium from Italy, France, and Germany, under the scientific
responsibility of INAF-IAPS, Rome, Italy, which also led the scientific
operations. The VIRTIS instrument development for ESA has been funded
and managed by ASI, with contributions from Observatoire de Meudon
(financed by CNES) and DLR. The VIRTIS instrument industrial prime
contractor was formerly Officine Galileo and is now Leonardo SpA in
Campi Bisenzio, Florence, Italy. The authors thank the Rosetta Liaison
Scientists, the Rosetta Science Ground Segment, and the Rosetta Mission
Operations Centre for their support in planning the VIRTIS observations.
T.M. acknowledges additional funding from NASA JPL, W.-H.I. from the
National Science Council of Taiwan (grant 102-2112-M-008-013-MY3) and
Science and Technology Development Fund of Macao Special Administrative
Region (grant 017/2014/A1), and L.M. from Deutsche
Forschungsgemeinschaft (grant MO 3007/1-1). The VIRTIS calibrated data
are available through ESA's Planetary Science Archive
(www.cosmos.esa.int/web/psa/rosetta). This research has made use of
NASA's Astrophysics Data System.
NR 31
TC 2
Z9 2
U1 15
U2 15
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD DEC 23
PY 2016
VL 354
IS 6319
BP 1563
EP 1566
DI 10.1126/science.aag3161
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EF3VZ
UT WOS:000390254300046
PM 27856846
ER
PT J
AU Fornasier, S
Mottola, S
Keller, HU
Barucci, MA
Davidsson, B
Feller, C
Deshapriya, JDP
Sierks, H
Barbieri, C
Lamy, PL
Rodrigo, R
Koschny, D
Rickman, H
A'Hearn, M
Agarwal, J
Bertaux, JL
Bertini, I
Besse, S
Cremonese, G
Da Deppo, V
Debei, S
De Cecco, M
Deller, J
El-Maarry, MR
Fulle, M
Groussin, O
Gutierrez, PJ
Guttler, C
Hofmann, M
Hviid, SF
Ip, WH
Jorda, L
Knollenberg, J
Kovacs, G
Kramm, R
Kuhrt, E
Kuppers, M
Lara, ML
Lazzarin, M
Moreno, JJL
Marzari, F
Massironi, M
Naletto, G
Oklay, N
Pajola, M
Pommerol, A
Preusker, F
Scholten, F
Shi, X
Thomas, N
Toth, I
Tubiana, C
Vincent, JB
AF Fornasier, S.
Mottola, S.
Keller, H. U.
Barucci, M. A.
Davidsson, B.
Feller, C.
Deshapriya, J. D. P.
Sierks, H.
Barbieri, C.
Lamy, P. L.
Rodrigo, R.
Koschny, D.
Rickman, H.
A'Hearn, M.
Agarwal, J.
Bertaux, J. -L.
Bertini, I.
Besse, S.
Cremonese, G.
Da Deppo, V.
Debei, S.
De Cecco, M.
Deller, J.
El-Maarry, M. R.
Fulle, M.
Groussin, O.
Gutierrez, P. J.
Guettler, C.
Hofmann, M.
Hviid, S. F.
Ip, W. -H.
Jorda, L.
Knollenberg, J.
Kovacs, G.
Kramm, R.
Kuehrt, E.
Kuppers, M.
Lara, M. L.
Lazzarin, M.
Moreno, J. J. Lopez
Marzari, F.
Massironi, M.
Naletto, G.
Oklay, N.
Pajola, M.
Pommerol, A.
Preusker, F.
Scholten, F.
Shi, X.
Thomas, N.
Toth, I.
Tubiana, C.
Vincent, J. -B.
TI Rosetta's comet 67P/Churyumov-Gerasimenko sheds its dusty mantle to
reveal its icy nature
SO SCIENCE
LA English
DT Article
ID EXPOSED WATER ICE; H2O ICE; NUCLEUS; SURFACE; OSIRIS; INSTRUMENTS;
MORPHOLOGY; VIRTIS
AB The Rosetta spacecraft has investigated comet 67P/Churyumov-Gerasimenko from large heliocentric distances to its perihelion passage and beyond. We trace the seasonal and diurnal evolution of the colors of the 67P nucleus, finding changes driven by sublimation and recondensation of water ice. The whole nucleus became relatively bluer near perihelion, as increasing activity removed the surface dust, implying that water ice is widespread underneath the surface. We identified large (1500 square meters) ice-rich patches appearing and then vanishing in about 10 days, indicating small-scale heterogeneities on the nucleus. Thin frosts sublimating in a few minutes are observed close to receding shadows, and rapid variations in color are seen on extended areas close to the terminator. These cyclic processes are widespread and lead to continuously, slightly varying surface properties.
C1 [Fornasier, S.; Barucci, M. A.; Feller, C.; Deshapriya, J. D. P.] Sorbonne Univ, UPMC Univ Paris 06,Sorbonne Paris Cite, Univ Paris Diderot,PSL Res Univ, CNRS,Observ Paris,LESIA, 5 Pl J Janssen, F-92125 Meudon, France.
[Mottola, S.; Keller, H. U.; Hviid, S. F.; Kuehrt, E.; Preusker, F.; Scholten, F.] Inst Planetenforschung Asteroiden & Kometen, Deutsches Zentrum Luft & Raumfahrt DLR, Rutherfordstrafle 2, D-12489 Berlin, Germany.
[Keller, H. U.] Tech Univ Carolo Wilhelmina Braunschweig, IGEP, Mendelssohnstr 3, D-38106 Braunschweig, Germany.
[Davidsson, B.] Jet Prop Lab, M-S 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Sierks, H.; Agarwal, J.; Deller, J.; Guettler, C.; Hofmann, M.; Kovacs, G.; Kramm, R.; Oklay, N.; Shi, X.; Tubiana, C.; Vincent, J. -B.] Max Planck Inst Sonnensyst Forsch, Justus von Liebig Weg 3, D-37077 Gottingen, Germany.
[Barbieri, C.; Bertini, I.; Lazzarin, M.; Marzari, F.] Univ Padua, Dept Phys & Astron, Vicolo dellOsservatorio 3, I-35122 Padua, Italy.
[Lamy, P. L.] CNRS, Lab Astrophys Marseille, UMR 7326, 38 Rue Frederic Joliot Curie, F-13388 Marseille 13, France.
[Lamy, P. L.] Univ Aix Marseille, 38 Rue Frederic Joliot Curie, F-13388 Marseille 13, France.
[Rodrigo, R.; Gutierrez, P. J.; Lara, M. L.; Moreno, J. J. Lopez] Inst Astrofis Andalucia CSIC, C Glorieta Astron S N, Granada 18008, Spain.
[Rodrigo, R.] Int Space Sci Inst, Hallerstr 6, CH-3012 Bern, Switzerland.
[Koschny, D.] European Space Res & Technol Centre ESA, Sci Support Off, Keplerlaan 1,Postbus 299, NL-2201 AZ Noordwijk, Netherlands.
[Rickman, H.] Uppsala Univ, Dept Phys & Astron, Box 516, S-75120 Uppsala, Sweden.
[Rickman, H.] Polish Acad Sci, Space Res Ctr, Bartycka 18A, PL-00716 Warsaw, Poland.
[A'Hearn, M.] Univ Maryland, Dept Phys & Astron, College Pk, MD 20742 USA.
[Bertaux, J. -L.] CNRS UVSQ IPSL, Lab Atmospheres Milieux Observ Spati LATMOS, 11 Blvd Alembert, F-78280 Guyancourt, France.
[Besse, S.; Kuppers, M.] European Space Astron Ctr ESA, Operat Dept, POB 78, F-28691 Madrid, Spain.
[Cremonese, G.] INAF, Osservatorio Via Venezia 1, I-35122 Padua, Italy.
[Da Deppo, V.; Naletto, G.] CNR, IFN UOS Padova LUXOR, Via Trasea 7, I-35131 Padua, Italy.
[Debei, S.] Univ Padua, Dept Mech Engn, Via Venezia 1, I-35131 Trento, Italy.
[De Cecco, M.] Univ Trent, Via Mesiano 77, I-38100 Trento, Italy.
[El-Maarry, M. R.; Pommerol, A.; Thomas, N.] Univ Bern, Phys Inst, Sidlerstr 5, CH-3012 Bern, Switzerland.
[Fulle, M.] Osserv Astron Trieste, INAF, Via Tiepolo 11, I-34014 Trieste, Italy.
[Groussin, O.; Jorda, L.] Aix Marseille Univ, CNRS, LAM, UMR 7326, 38 Rue Frederic Joliot Curie, F-13388 Marseille 13, France.
[Ip, W. -H.] Natl Cent Univ, Grad Inst Astron, 300 Chung Da Rd, Chungli 32054, Taiwan.
[Ip, W. -H.] Macau Univ Sci & Technol, Space Sci Inst, Macau, Peoples R China.
[Kovacs, G.] Budapest Univ Technol & Econ, Budapest, Hungary.
[Massironi, M.] Univ Padua, Dipartimento Geosci, Via G Gradenigo 6, I-35131 Padua, Italy.
[Massironi, M.; Naletto, G.; Pajola, M.] Univ Padua, Ctr Studies & Act Space CISAS, Via Venezia 15, I-35131 Padua, Italy.
[Naletto, G.] Univ Padua, Dept Informat Engn, Via Gradenigo 6-B, I-35131 Padua, Italy.
[Pajola, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Toth, I.] MTA CSFK Konkoly Observ, Konkoly Thege M Ut 15-17, H-1121 Budapest, Hungary.
RP Fornasier, S (reprint author), Sorbonne Univ, UPMC Univ Paris 06,Sorbonne Paris Cite, Univ Paris Diderot,PSL Res Univ, CNRS,Observ Paris,LESIA, 5 Pl J Janssen, F-92125 Meudon, France.
EM sonia.fornasier@obspm.fr
OI fulle, marco/0000-0001-8435-5287; Massironi, Matteo/0000-0002-7757-8818;
Besse, Sebastien/0000-0002-1052-5439
FU Germany (DLR); France (CNES); Italy (ASI); Spain (MEC); Sweden (SNSB);
ESA Technical Directorate; NASA through Jet Propulsion Laboratory
[1267923]; Akademie der Wissenschaften zu Gottingen; Ministry of Science
and Technology, Taiwan [NSC 102-2112-M-008]; Macau University of Science
and Technology [FDCT 017/2014/A1]
FX OSIRIS was built by a consortium led by the Max-Planck-Institut fur
Sonnensystemforschung, Gottingen, Germany, in collaboration with CISAS,
University of Padova, Italy; the Laboratoire d'Astrophysique de
Marseille, France; the Instituto de Astrofisica de Andalucia, CSIC,
Granada, Spain; the Scientific Support Office of the European Space
Agency (ESA), Noordwijk, The Netherlands; the Instituto Nacional de
Tecnica Aeroespacial, Madrid, Spain; the Universidad Politechnica de
Madrid, Spain; the Department of Physics and Astronomy of Uppsala
University, Sweden; and the Institut fur Datentechnik und
Kommunikationsnetze der Technischen Universitat Braunschweig, Germany.
The support of the contributing research institutes of the OSIRIS
consortium and of the national funding agencies of Germany (DLR), France
(CNES), Italy (ASI), Spain (MEC), Sweden (SNSB), and the ESA Technical
Directorate is gratefully acknowledged. M.A. acknowledges NASA funding
through Jet Propulsion Laboratory contract no. 1267923 and from the
Akademie der Wissenschaften zu Gottingen. W.-H.I, acknowledges the
Ministry of Science and Technology, Taiwan (grant no. NSC
102-2112-M-008), and Macau University of Science and Technology (grant
no. FDCT 017/2014/A1). We thank the ESA teams at European Space
Astronomy Centre, European Space Operations Centre, and European Space
Research and Technology Centre for their work in support of the Rosetta
mission. P. H. Hasselmann and D. Perna are acknowledged for helpful
discussion. Rosetta/OSIRIS data are available through the ESA's
Planetary Science Archive (PSA) at www.cosmos.esa.int/web/psa/rosetta.
Some images used in this paper that are not yet available at PSA can be
downloaded from the MPS OSIRIS website at
https://planetgate.mps.mpg.de/WebFileShare/Released_Images/Fornasier+Sci
ence.
NR 24
TC 3
Z9 3
U1 17
U2 17
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD DEC 23
PY 2016
VL 354
IS 6319
BP 1566
EP 1570
DI 10.1126/science.aag2671
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EF3VZ
UT WOS:000390254300047
PM 27856849
ER
PT J
AU Schroeder, JR
Beyer, KD
AF Schroeder, Jason R.
Beyer, Keith D.
TI Deliquescence Relative Humidities of Organic and Inorganic Salts
Important in the Atmosphere
SO JOURNAL OF PHYSICAL CHEMISTRY A
LA English
DT Article
ID AMMONIUM-SULFATE; MINERAL DUST; MALONIC-ACID; OXALIC-ACID; PARTICLES;
WATER; AEROSOLS; SODIUM; TROPOSPHERE; SOLUBILITY
AB The deliquescence relative humidities (DRH) as a function of temperature have been determined for several salts of atmospheric importance using humidity controlled thermogravimetric analysis (HTGA): sodium hydrogen oxalate monohydrate (NaHC2O4H2O), sodium oxalate (Na2C2O4), sodium ammonium sulfate dihydrate (NaNH4SO4.2H(2)O, lecontite), sodium hydrogen malonate monohydrate (NaHC3H2O4.H2O), sodium malonate monohydrate (Na2C3H2O4.H2O), and ammonium hydrogen malonate (NH4HC3H2O4). The temperature dependent onset DRH values (where a dry mixture begins to take up water) were also determined for mixtures of ammonium sulfate with malonic acid, and ammonium sulfate with sodium oxalates and sodium malonates, respectively. We demonstrate that the onset DRH is independent of the ratio of solids in the mixture. In general, onset DRH values were always lower than the pure component DRH values.
C1 [Schroeder, Jason R.; Beyer, Keith D.] Univ Wisconsin, Dept Chem & Biochem, La Crosse, WI 54601 USA.
[Schroeder, Jason R.] NASA, Langley Res Ctr, NASA Postdoctoral Program, Hampton, VA 23665 USA.
RP Beyer, KD (reprint author), Univ Wisconsin, Dept Chem & Biochem, La Crosse, WI 54601 USA.
EM kbeyer@uwlax.edu
FU NSF Atmospheric Chemistry Program [AGS-1361592]
FX We wish to thank Anastasiya Vinokur and Dr. Ilia Guzei at the University
of Wisconsin Madison for running and analyzing the X-ray crystallography
experiments, Lukas Buttke for performing some of the HTGA experiments,
and anonymous reviewers for helpful comments on our manuscript. This
work was supported by the NSF Atmospheric Chemistry Program
(AGS-1361592).
NR 41
TC 0
Z9 0
U1 9
U2 9
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1089-5639
J9 J PHYS CHEM A
JI J. Phys. Chem. A
PD DEC 22
PY 2016
VL 120
IS 50
BP 9948
EP 9957
DI 10.1021/acs.jpca.6b08725
PG 10
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA EG0PW
UT WOS:000390735700007
PM 27966359
ER
PT J
AU Nowicki, SMJ
Payne, A
Larour, E
Seroussi, H
Goelzer, H
Lipscomb, W
Gregory, J
Abe-Ouchi, A
Shepherd, A
AF Nowicki, Sophie M. J.
Payne, Anthony
Larour, Eric
Seroussi, Helene
Goelzer, Heiko
Lipscomb, William
Gregory, Jonathan
Abe-Ouchi, Ayako
Shepherd, Andrew
TI Ice Sheet Model Intercomparison Project (ISMIP6) contribution to CMIP6
SO GEOSCIENTIFIC MODEL DEVELOPMENT
LA English
DT Article
ID SURFACE MASS-BALANCE; FUTURE SEA-LEVEL; EARTH-SYSTEM-MODEL; REGIONAL
CLIMATE MODELS; MULTIMODEL PROJECTIONS; SPATIAL SENSITIVITIES;
ENVIRONMENTAL-CHANGE; EXPERIMENTAL-DESIGN; ELEVATION FEEDBACK; GREENLAND
AB Reducing the uncertainty in the past, present, and future contribution of ice sheets to sea-level change requires a coordinated effort between the climate and glaciology communities. The Ice Sheet Model Intercomparison Project for CMIP6 (ISMIP6) is the primary activity within the Coupled Model Intercomparison Project - phase 6 (CMIP6) focusing on the Greenland and Antarctic ice sheets. In this paper, we describe the framework for ISMIP6 and its relationship with other activities within CMIP6. The ISMIP6 experimental design relies on CMIP6 climate models and includes, for the first time within CMIP, coupled ice-sheet-climate models as well as standalone ice-sheet models. To facilitate analysis of the multi-model ensemble and to generate a set of standard climate inputs for standalone ice-sheet models, ISMIP6 defines a protocol for all variables related to ice sheets. ISMIP6 will provide a basis for investigating the feedbacks, impacts, and sea-level changes associated with dynamic ice sheets and for quantifying the uncertainty in ice-sheet-sourced global sea-level change.
C1 [Nowicki, Sophie M. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Payne, Anthony] Univ Bristol, Sch Geog Sci, Bristol BS8 1SS, Avon, England.
[Larour, Eric; Seroussi, Helene] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Goelzer, Heiko] Univ Utrecht, Inst Marine & Atmospher Res, NL-3584 CC Utrecht, Netherlands.
[Goelzer, Heiko] Univ Libre Bruxelles, Lab Glaciol, CP160-03,Ave Roosevelt 50, B-1050 Brussels, Belgium.
[Lipscomb, William] Los Alamos Natl Lab, Los Alamos, NM 87544 USA.
[Gregory, Jonathan] Univ Reading, Dept Meteorol, Reading RG6 6BB, Berks, England.
[Gregory, Jonathan] Met Off Hadley Ctr, Exeter EX1 3BP, Devon, England.
[Abe-Ouchi, Ayako] Univ Tokyo, Atmosphere & Ocean Res Inst, Kashiwa, Chiba 2778564, Japan.
[Abe-Ouchi, Ayako] Japan Agcy Marine Earth Sci & Technol, Yokohama, Kanagawa, Japan.
[Shepherd, Andrew] Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England.
RP Nowicki, SMJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM sophie.nowicki@nasa.gov
OI Gregory, Jonathan/0000-0003-1296-8644; Goelzer,
Heiko/0000-0002-5878-9599
FU Climate and Cryosphere (CliC) Project; World Climate Research Programme
(WCRP); Netherlands Earth System Science Centre (NESSC); Dutch Ministry
of Education, Culture and Science (OCW) [024.002.001]; NASA Cryospheric
Science Program; NASA Modeling Analysis and Prediction Program; Regional
and Global Climate Modeling program of the Office of Biological and
Environmental Research within the US Department of Energy's Office of
Science; NERC Centre for Polar Observation and Modelling (CPOM)
FX We thank the CMIP6 panel members for their continuous leadership of the
CMIP6 effort, the Working Group on Coupled Modeling (WGCM)
Infrastructure Panel (WIP) for overseeing the CMIP6 and ISMIP6
infrastructure, and in particular Martin Juckes and Alison Pamment for
their help with the ISMIP6 data request, and Karl Taylor for sharing his
wisdom on CMIP experiment protocols. We thank the current ISMIP6
members, the modeling groups, and the wider glaciology community for
their contribution in the ISMIP6 design. We acknowledge the Climate and
Cryosphere (CliC) Project and the World Climate Research Programme
(WCRP) for their guidance, support, and sponsorship. Heiko Goelzer has
received funding from the program of the Netherlands Earth System
Science Centre (NESSC), financially supported by the Dutch Ministry of
Education, Culture and Science (OCW) under grant no. 024.002.001. Sophie
Nowicki, Helene Seroussi, and Eric Larour were supported by grants from
the NASA Cryospheric Science Program and the NASA Modeling Analysis and
Prediction Program. William Lipscomb was supported by the Regional and
Global Climate Modeling program of the Office of Biological and
Environmental Research within the US Department of Energy's Office of
Science. Anthony Payne is supported by the NERC Centre for Polar
Observation and Modelling (CPOM). We thank our topical editor Philippe
Huybrechts, our reviewers Christian Rodehacke and Xylar Asay-Davis, and
everyone who contributed to the open discussion for constructive
comments.
NR 133
TC 0
Z9 0
U1 4
U2 4
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1991-959X
EI 1991-9603
J9 GEOSCI MODEL DEV
JI Geosci. Model Dev.
PD DEC 21
PY 2016
VL 9
IS 12
BP 4521
EP 4545
DI 10.5194/gmd-9-4521-2016
PG 25
WC Geosciences, Multidisciplinary
SC Geology
GA EH2EF
UT WOS:000391579600002
ER
PT J
AU Kirnosov, V
Chang, LC
Pulkkinen, A
AF Kirnosov, Vladimir
Chang, Lin-Ching
Pulkkinen, Antti
TI Combining STEREO SECCHI COR2 and HI1 images for automatic CME front edge
tracking
SO JOURNAL OF SPACE WEATHER AND SPACE CLIMATE
LA English
DT Article
DE STEREO SECCHI; CME; Front edge tracking; COR2; HI1
ID CORONAL MASS EJECTIONS; CATALOG; RECONSTRUCTION; PROPAGATION;
KINEMATICS; MISSION; STORMS
AB COR2 coronagraph images are the most commonly used data for coronal mass ejection (CME) analysis among the various types of data provided by the STEREO (Solar Terrestrial Relations Observatory) SECCHI (Sun-Earth Connection Coronal and Heliospheric Investigation) suite of instruments. The field of view (FOV) in COR2 images covers 2-15 solar radii (Rs) that allow for tracking the front edge of a CME in its initial stage to forecast the lead-time of a CME and its chances of reaching the Earth. However, estimating the lead-time of a CME using COR2 images gives a larger lead-time, which may be associated with greater uncertainty. To reduce this uncertainty, CME front edge tracking should be continued beyond the FOV of COR2 images. Therefore, heliospheric imager (HI1) data that covers 15-90 Rs FOV must be included. In this paper, we propose a novel automatic method that takes both COR2 and HI1 images into account and combine the results to track the front edges of a CME continuously. The method consists of two modules: pre-processing and tracking. The pre-processing module produces a set of segmented images, which contain the signature of a CME, for both COR2 and HI1 separately. In addition, the HI1 images are resized and padded, so that the center of the Sun is the central coordinate of the resized HI1 images. The resulting COR2 and HI1 image set is then fed into the tracking module to estimate the position angle (PA) and track the front edge of a CME. The detected front edge is then used to produce a height-time profile that is used to estimate the speed of a CME. The method was validated using 15 CME events observed in the period from January 1, 2008 to August 31, 2009. The results demonstrate that the proposed method is effective for CME front edge tracking in both COR2 and HI1 images. Using this method, the CME front edge can now be tracked automatically and continuously in a much larger range, i.e., from 2 to 90 Rs, for the first time. These improvements can greatly help in making the quantitative CME analysis more accurate and have the potential to assist in space weather forecasting.
C1 [Kirnosov, Vladimir; Chang, Lin-Ching] Catholic Univ Amer, Elect Engn & Comp Sci Dept, 620 Michigan Ave N-E, Washington, DC 20064 USA.
[Pulkkinen, Antti] NASA, Goddard Space Flight Ctr, Code 674, Greenbelt, MD 20771 USA.
RP Kirnosov, V (reprint author), Catholic Univ Amer, Elect Engn & Comp Sci Dept, 620 Michigan Ave N-E, Washington, DC 20064 USA.
EM 57kirnosov@cua.edu
NR 41
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U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 2115-7251
J9 J SPACE WEATHER SPAC
JI J. Space Weather Space Clim.
PD DEC 21
PY 2016
VL 6
AR A41
DI 10.1051/swsc/2016037
PG 10
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA EG4EO
UT WOS:000390996600001
ER
PT J
AU Lindblom, L
Cutler, C
AF Lindblom, Lee
Cutler, Curt
TI Model waveform accuracy requirements for the Allen chi(2) discriminator
SO PHYSICAL REVIEW D
LA English
DT Article
AB This paper derives accuracy standards for model gravitational waveforms required to ensure proper use of the Allen chi(2) discriminator in gravitational wave data analysis. These standards are different from previously established requirements for detection and waveform parameter measurement based on signal-to-noise optimization. We present convenient formulas for evaluating and interpreting the contribution of model errors to measured values of this chi(2) statistic. The new accuracy standards derived here are needed to ensure the reliability of measured values of the Allen chi(2) statistic, both in their traditional role as vetoes and in their current role as elements in evaluating the significance of candidate detections.
C1 [Lindblom, Lee] Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr, La Jolla, CA 92093 USA.
[Cutler, Curt] CALTECH, Theoret Astrophys 350 17, Pasadena, CA 91125 USA.
[Cutler, Curt] Jet Prop Lab, M-S 169-327,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Lindblom, L (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr, La Jolla, CA 92093 USA.
FU National Science Foundation [PHY1404569, PHY-1604244, DMS-1620366]
FX We thank Jolien Creighton, Benjamin Owen, and Xavier Siemens for helpful
comments on this work. C. C.' s research was supported in part by Grant
No. PHY1404569 to the California Institute of Technology from the
National Science Foundation. L. L.' s research was supported in part by
Grants No. PHY-1604244 and No. DMS-1620366 to the University of
California at San Diego from the National Science Foundation.
NR 10
TC 0
Z9 0
U1 0
U2 0
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2470-0010
EI 2470-0029
J9 PHYS REV D
JI Phys. Rev. D
PD DEC 20
PY 2016
VL 94
IS 12
AR 124030
DI 10.1103/PhysRevD.94.124030
PG 5
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA EO9KS
UT WOS:000397008200009
ER
PT J
AU Domenech, JL
Drouin, BJ
Cernicharo, J
Herrero, VJ
Tanarro, I
AF Domenech, J. L.
Drouin, B. J.
Cernicharo, J.
Herrero, V. J.
Tanarro, I.
TI THE HIGH-RESOLUTION INFRARED SPECTRUM OF HCl+
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE ISM: molecules; methods: laboratory: molecular; molecular data;
techniques: spectroscopic
ID INTERSTELLAR CHLORONIUM; LINE CATALOG; SUBMILLIMETER; MILLIMETER
AB The chloroniumyl cation, HCl+, has been recently identified in space from Herschel's spectra. A joint analysis of extensive vis-UV spectroscopy emission data together with a few high-resolution and high-accuracy millimeter-wave data provided the necessary rest frequencies to support the astronomical identification. Nevertheless, the analysis did not include any infrared (IR) vibration-rotation data. Furthermore, with the end of the Herschel mission, IR observations from the ground may be one of the few available means to further study this ion in space. In this work, we provide a set of accurate rovibrational transition wavenumbers, as well as a new and improved global fit of vis-UV, IR, and millimeter-wave spectroscopy laboratory data, that will aid in future studies of this molecule.
C1 [Domenech, J. L.; Herrero, V. J.; Tanarro, I.] CSIC, Inst Estruct Mat IEM, Dept Mol Phys, Serrano 123, E-28006 Madrid, Spain.
[Drouin, B. J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Cernicharo, J.] CSIC, Inst Ciencia Mat Madrid ICMM, Mol Astrophys Grp, Sor Juana Ines de la Cruz 3, E-28049 Madrid, Spain.
RP Domenech, JL (reprint author), CSIC, Inst Estruct Mat IEM, Dept Mol Phys, Serrano 123, E-28006 Madrid, Spain.
EM jl.domenech@csic.es
OI Cernicharo, Jose/0000-0002-3518-2524
FU Spanish MINECO [CSD2009-00038]; ERC [ERC-2013-SyG NANOCOSMOS];
[FIS2012-38175]; [FIS2013-408087-C2-1P]; [AYA2012-32032]
FX J.L.D., J.C., V.J.H., and I.T. acknowledge financial support from the
Spanish MINECO through the Consolider ASTRO-MOL project, grant
CSD2009-00038, and from the ERC through the Synergy Grant ERC-2013-SyG
NANOCOSMOS. Additional support through grants FIS2012-38175 (J.L.D.),
FIS2013-408087-C2-1P (V.J.H., I.T.), and AYA2012-32032 (J.C.) is also
acknowledged. We thank J.R. Goicoechea for his reading and comments on
the manuscript. Portions of the research described in this Letter were
performed at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration. Government sponsorship acknowledged.
NR 18
TC 0
Z9 0
U1 2
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD DEC 20
PY 2016
VL 833
IS 2
AR L32
DI 10.3847/2041-8213/833/2/L32
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EH2OU
UT WOS:000391607900007
ER
PT J
AU Falconer, DA
Tiwari, SK
Moore, RL
Khazanov, I
AF Falconer, David A.
Tiwari, Sanjiv K.
Moore, Ronald L.
Khazanov, Igor
TI A NEW METHOD TO QUANTIFY AND REDUCE THE NET PROJECTION ERROR IN
WHOLE-SOLAR-ACTIVE-REGION PARAMETERS MEASURED FROM VECTOR MAGNETOGRAMS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: activity; Sun: magnetic fields; Sun: photosphere
ID MAGNETIC-FIELD DATA
AB Projection errors limit the use of vector magnetograms of active regions (ARs) far from the disk center. In this Letter, for ARs observed up to 60 degrees from the disk center, we demonstrate a method for measuring and reducing the projection error in the magnitude of any whole-AR parameter that is derived from a vector magnetogram that has been deprojected to the disk center. The method assumes that the center-to-limb curve of the average of the parameter's absolute values, measured from the disk passage of a large number of ARs and normalized to each AR's absolute value of the parameter at central meridian, gives the average fractional projection error at each radial distance from the disk center. To demonstrate the method, we use a large set of large-flux ARs and apply the method to a whole-AR parameter that is among the simplest to measure: whole-AR magnetic flux. We measure 30,845 SDO/Helioseismic and Magnetic Imager vector magnetograms covering the disk passage of 272 large-flux ARs, each having whole-AR flux > 10(22) Mx. We obtain the center-to-limb radial-distance run of the average projection error in measured whole-AR flux from a Chebyshev fit to the radial-distance plot of the 30,845 normalized measured values. The average projection error in the measured whole-AR flux of an AR at a given radial distance is removed by multiplying the measured flux by the correction factor given by the fit. The correction is important for both the study of the evolution of ARs and for improving the accuracy of forecasts of an AR's major flare/coronal mass ejection productivity.
C1 [Falconer, David A.; Tiwari, Sanjiv K.; Moore, Ronald L.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Falconer, David A.; Moore, Ronald L.; Khazanov, Igor] Univ Alabama Huntsville, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA.
[Khazanov, Igor] Archarithms Inc, Huntsville, AL 35801 USA.
RP Falconer, DA (reprint author), NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.; Falconer, DA (reprint author), Univ Alabama Huntsville, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA.
EM David.a.Falconer@nasa.gov
OI Tiwari, Sanjiv/0000-0001-7817-2978
FU NASA's Game Changing Development Program; Johnson Space Center's Space
Radiation Analysis Group (SRAG); NextGen Federal Systems; NASA
FX We thank the referee for leading us to make several improvements in the
paper. Support for MAG4 development came from NASA's Game Changing
Development Program, and the Johnson Space Center's Space Radiation
Analysis Group (SRAG). In particular, the authors want to gratefully
acknowledge the continued support and guidance of Dan Fry (NASA-JSC) and
David Moore (NASA-LaRC). D.F. acknowledges support from NextGen Federal
Systems for the completion of this work. S.K.T. is supported by an
appointment to the NASA Postdoctoral Program at the NASA/MSFC,
administered by USRA through a contract with NASA.
NR 14
TC 0
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U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD DEC 20
PY 2016
VL 833
IS 2
AR L31
DI 10.3847/2041-8213/833/2/L31
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EH2OU
UT WOS:000391607900006
ER
PT J
AU Chipperfield, MP
Liang, Q
Rigby, M
Hossaini, R
Montzka, SA
Dhomse, S
Feng, WH
Prinn, RG
Weiss, RF
Harth, CM
Salameh, PK
Muhle, J
O'Doherty, S
Young, D
Simmonds, PG
Krummel, PB
Fraser, PJ
Steele, LP
Happell, JD
Rhew, RC
Butler, J
Yvon-Lewis, SA
Hall, B
Nance, D
Moore, F
Miller, BR
Elkins, J
Harrison, JJ
Boone, CD
Atlas, EL
Mahieu, E
AF Chipperfield, Martyn P.
Liang, Qing
Rigby, Matthew
Hossaini, Ryan
Montzka, Stephen A.
Dhomse, Sandip
Feng, Wuhu
Prinn, Ronald G.
Weiss, Ray F.
Harth, Christina M.
Salameh, Peter K.
Muhle, Jens
O'Doherty, Simon
Young, Dickon
Simmonds, Peter G.
Krummel, Paul B.
Fraser, Paul J.
Steele, L. Paul
Happell, James D.
Rhew, Robert C.
Butler, James
Yvon-Lewis, Shari A.
Hall, Bradley
Nance, David
Moore, Fred
Miller, Ben R.
Elkins, JamesW.
Harrison, Jeremy J.
Boone, Chris D.
Atlas, Elliot L.
Mahieu, Emmanuel
TI Model sensitivity studies of the decrease in atmospheric carbon
tetrachloride
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID CHEMISTRY EXPERIMENT ACE; SOIL SINK; EMISSIONS; CCL4; GASES; TRANSPORT;
TRENDS; FUTURE
AB Carbon tetrachloride (CCl4) is an ozone-depleting substance, which is controlled by the Montreal Protocol and for which the atmospheric abundance is decreasing. However, the current observed rate of this decrease is known to be slower than expected based on reported CCl4 emissions and its estimated overall atmospheric lifetime. Here we use a three-dimensional (3-D) chemical transport model to investigate the impact on its predicted decay of uncertainties in the rates at which CCl4 is removed from the atmosphere by photolysis, by ocean uptake and by degradation in soils. The largest sink is atmospheric photolysis (74% of total), but a reported 10% uncertainty in its combined photolysis cross section and quantum yield has only a modest impact on the modelled rate of CCl4 decay. This is partly due to the limiting effect of the rate of transport of CCl4 from the main tropospheric reservoir to the stratosphere, where photolytic loss occurs. The model suggests large interannual variability in the magnitude of this stratospheric photolysis sink caused by variations in transport. The impact of uncertainty in the minor soil sink (9% of total) is also relatively small. In contrast, the model shows that uncertainty in ocean loss (17% of total) has the largest impact on modelled CCl4 decay due to its sizeable contribution to CCl4 loss and large lifetime uncertainty range (147 to 241 years). With an assumed CCl4 emission rate of 39 Gg year(-1), the reference simulation with the best estimate of loss processes still underestimates the observed CCl4 (overestimates the decay) over the past 2 decades but to a smaller extent than previous studies. Changes to the rate of CCl4 loss processes, in line with known uncertainties, could bring the model into agreement with in situ surface and remote-sensing measurements, as could an increase in emissions to around 47 Gg year(-1). Further progress in constraining the CCl4 budget is partly limited by systematic biases between observational datasets. For example, surface observations from the National Oceanic and Atmospheric Administration (NOAA) network are larger than from the Advanced Global Atmospheric Gases Experiment (AGAGE) network but have shown a steeper decreasing trend over the past 2 decades. These differences imply a difference in emissions which is significant relative to uncertainties in the magnitudes of the CCl4 sinks.
C1 [Chipperfield, Martyn P.; Dhomse, Sandip; Feng, Wuhu] Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England.
[Chipperfield, Martyn P.] Univ Leeds, Natl Ctr Earth Observat, Leeds LS2 9JT, W Yorkshire, England.
[Liang, Qing] NASA Goddard Space Flight Ctr, Atmospher Chem & Dynam, Greenbelt, MD 20771 USA.
[Liang, Qing] Univ Space Res Assoc, GESTAR, Columbia, MD 21046 USA.
[Rigby, Matthew; O'Doherty, Simon; Young, Dickon; Simmonds, Peter G.] Univ Bristol, Sch Chem, Atmospher Chem Res Grp, Bristol BS8 1TS, Avon, England.
[Hossaini, Ryan] Univ Lancaster, Lancaster Environm Ctr, Lancaster LA1 4YQ, England.
[Montzka, Stephen A.; Butler, James; Hall, Bradley; Nance, David; Moore, Fred; Miller, Ben R.; Elkins, JamesW.] NOAA Earth Syst Res Lab, Global Monitoring Div, Boulder, CO 80305 USA.
[Feng, Wuhu] Univ Leeds, Natl Ctr Atmospher Sci, Leeds LS2 9JT, W Yorkshire, England.
[Prinn, Ronald G.] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Weiss, Ray F.; Harth, Christina M.; Salameh, Peter K.; Muhle, Jens] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
[Krummel, Paul B.; Fraser, Paul J.; Steele, L. Paul] CSIRO Oceans & Atmosphere, Aspendale, Vic 3195, Australia.
[Happell, James D.] Univ Miami, Dept Ocean Sci, Miami, FL 33149 USA.
[Rhew, Robert C.] Univ Calif Berkeley, Dept Geog, Berkeley, CA 94720 USA.
[Yvon-Lewis, Shari A.] Texas A&M Univ, Dept Oceanog, College Stn, TX 77840 USA.
[Harrison, Jeremy J.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Harrison, Jeremy J.] Univ Leicester, Natl Ctr Earth Observat, Leicester LE1 7RH, Leics, England.
[Boone, Chris D.] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada.
[Atlas, Elliot L.] Univ Miami, Dept Atmospher Sci, Miami, FL 33149 USA.
[Mahieu, Emmanuel] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium.
RP Chipperfield, MP (reprint author), Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England.; Chipperfield, MP (reprint author), Univ Leeds, Natl Ctr Earth Observat, Leeds LS2 9JT, W Yorkshire, England.
EM m.chipperfield@leeds.ac.uk
RI Steele, Paul/B-3185-2009; Liang, Qing/B-1276-2011; Dhomse,
Sandip/C-8198-2011;
OI Steele, Paul/0000-0002-8234-3730; Dhomse, Sandip/0000-0003-3854-5383;
Mahieu, Emmanuel/0000-0002-5251-0286
FU UK Natural Environment Research Council (NERC) through the TROPHAL
project [NE/J02449X/1]; NERC National Centre for Earth Observation
(NCEO); Canadian Space Agency; F.R.S.-FNRS; Federation
Wallonie-Bruxelles; GAW-CH programme of Meteoswiss; NASA (USA);
Department of Energy and Climate Change (DECC, UK); NOAA (USA); CSIRO
(Australia); BoM (Australia); DECC [GA01103]; Royal Society Wolfson
Merit award; ASA Atmospheric Composition Campaign Data Analysis and
Modeling (ACCDAM) programme; NOAA Atmospheric Chemistry, Carbon Cycle,
and Climate (AC4) programme; National Science Foundation AGS Program
[ATM0849086, AGS0959853]
FX This work was supported by the UK Natural Environment Research Council
(NERC) through the TROPHAL project (NE/J02449X/1). The TOMCAT modelling
work was supported by the NERC National Centre for Atmospheric Science
(NCAS). The ACE-FTS CCl4 work was supported by the NERC
National Centre for Earth Observation (NCEO). The ACE mission is funded
primarily by the Canadian Space Agency. The University of Liege
involvement has primarily been supported by the F.R.S.-FNRS, the
Federation Wallonie-Bruxelles and the GAW-CH programme of Meteoswiss.
Emmanuel Mahieu is a research associate with F.R.S.-FNRS. We thank the
International Foundation High Altitude Research Stations Jungfraujoch
and Gornergrat (HFSJG, Bern) for supporting the facilities needed to
perform the FTIR observations and the many colleagues who contributed to
FTIR data acquisition. AGAGE is supported principally by NASA (USA)
grants to MIT and SIO, as well as by Department of Energy and Climate
Change (DECC, UK) and NOAA (USA) grants to Bristol University and by
CSIRO and BoM (Australia). The operation of the station at Mace Head was
funded by DECC through contract GA01103. Martyn P. Chipperfield is
supported by a Royal Society Wolfson Merit award. Qing Liang is
supported by the NASA Atmospheric Composition Campaign Data Analysis and
Modeling (ACCDAM) programme. NOAA observations were made possible with
technical and sampling assistance from station personnel (D. Mondeel, C.
Siso, C. Sweeney, S. Wolter, D. Neff, J. Higgs, M. Crotwell, D.
Guenther, P. Lang and G. Dutton) and were supported, in part, through
the NOAA Atmospheric Chemistry, Carbon Cycle, and Climate (AC4)
programme. Elliot L. Atlas acknowledges X. Zhu and L. Pope for technical
support and the National Science Foundation AGS Program for support
under grants ATM0849086 and AGS0959853.
NR 37
TC 0
Z9 0
U1 5
U2 5
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PD DEC 20
PY 2016
VL 16
IS 24
BP 15741
EP 15754
DI 10.5194/acp-16-15741-2016
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EH1VL
UT WOS:000391555600002
ER
PT J
AU Ade, PAR
Ahmed, Z
Aikin, RW
Alexander, KD
Barkats, D
Benton, SJ
Bischoff, CA
Bock, JJ
Bowens-Rubin, R
Brevik, JA
Buder, I
Bullock, E
Buza, V
Connors, J
Crill, BP
Duband, L
Dyorkin, C
Filippini, JP
Fliescher, S
Grayson, J
Halpern, M
Harrison, S
Hildebrandt, SR
Hilton, GC
Hui, H
Irwin, KD
Kang, J
Karkare, KS
Karpel, E
Kaufman, JP
Keating, BG
Kefeli, S
Kernasoyskiy, SA
Kovac, JM
Kuo, CL
Leitch, EM
Lueker, M
Megerian, KG
Namikawa, T
Netterfield, CB
Nguyen, HT
O'Brient, R
Ogburn, RW
Orlando, A
Pryke, C
Richter, S
Schwarz, R
Sheehy, CD
Staniszewski, ZK
Steinbach, B
Sudiwala, RV
Teply, GP
Thompson, KL
Tolan, JE
Tucker, C
Turner, AD
Vieregg, AG
Weber, AC
Wiebe, DV
Willmert, J
Wong, CL
Wu, WLK
Yoon, KW
AF Ade, P. A. R.
Ahmed, Z.
Aikin, R. W.
Alexander, K. D.
Barkats, D.
Benton, S. J.
Bischoff, C. A.
Bock, J. J.
Bowens-Rubin, R.
Brevik, J. A.
Buder, I.
Bullock, E.
Buza, V.
Connors, J.
Crill, B. P.
Duband, L.
Dyorkin, C.
Filippini, J. P.
Fliescher, S.
Grayson, J.
Halpern, M.
Harrison, S.
Hildebrandt, S. R.
Hilton, G. C.
Hui, H.
Irwin, K. D.
Kang, J.
Karkare, K. S.
Karpel, E.
Kaufman, J. P.
Keating, B. G.
Kefeli, S.
Kernasoyskiy, S. A.
Kovac, J. M.
Kuo, C. L.
Leitch, E. M.
Lueker, M.
Megerian, K. G.
Namikawa, T.
Netterfield, C. B.
Nguyen, H. T.
O'Brient, R.
Ogburn, R. W.
Orlando, A.
Pryke, C.
Richter, S.
Schwarz, R.
Sheehy, C. D.
Staniszewski, Z. K.
Steinbach, B.
Sudiwala, R. V.
Teply, G. P.
Thompson, K. L.
Tolan, J. E.
Tucker, C.
Turner, A. D.
Vieregg, A. G.
Weber, A. C.
Wiebe, D. V.
Willmert, J.
Wong, C. L.
Wu, W. L. K.
Yoon, K. W.
CA Keck Array Bicep2 Collaborations
TI BICEP2/KECK ARRAY VIII: MEASUREMENT OF GRAVITATIONAL LENSING FROM
LARGE-SCALE B-MODE POLARIZATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations; gravitational
lensing: weak; polarization
ID MICROWAVE; CMB; RECONSTRUCTION; MASS
AB We present measurements of polarization lensing using the 150 GHz maps, which include all data taken by the BICEP2 and Keck Array Cosmic Microwave Background polarization experiments up to and including the 2014 observing season (BK14). Despite their modest angular resolution (similar to 0 degrees.5), the excellent sensitivity (similar to 3 mu K-arcmin) of these maps makes it possible to directly reconstruct the lensing potential using only information at larger angular scales (l <= 700). From the auto-spectrum of the reconstructed potential, we measure an amplitude of the spectrum to be A(L)(phi phi) = 1.15 +/- 0.36 (Planck CDM prediction corresponds to A(L)(phi phi) = 1) and reject the no-lensing hypothesis at 5.8s, which is the highest significance achieved to date using an EB lensing estimator. Taking the cross-spectrum of the reconstructed potential with the Planck 2015 lensing map yields A(L)(phi phi) = 1.13 +/- 0.20. These direct measurements of A(L)(phi phi) are consistent with the CDM cosmology and with that derived from the previously reported BK14 B-mode auto-spectrum (A(L)(BB) = 1.20 +/- 0.17). We perform a series of null tests and consistency checks to show that these results are robust against systematics and are insensitive to analysis choices. These results unambiguously demonstrate that the B modes previously reported by BICEP / Keck at intermediate angular scales (150 less than or similar to l less than or similar to 350) are dominated by gravitational lensing. The good agreement between the lensing amplitudes obtained from the lensing reconstruction and B-mode spectrum starts to place constraints on any alternative cosmological sources of B modes at these angular scales.
C1 [Ade, P. A. R.; Kernasoyskiy, S. A.; Sudiwala, R. V.; Tucker, C.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Ahmed, Z.; Buza, V.; Grayson, J.; Irwin, K. D.; Kang, J.; Karpel, E.; Kuo, C. L.; Namikawa, T.; Ogburn, R. W.; Thompson, K. L.; Tolan, J. E.; Wu, W. L. K.; Yoon, K. W.; Keck Array Bicep2 Collaborations] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Ahmed, Z.; Irwin, K. D.; Kang, J.; Kuo, C. L.; Namikawa, T.; Ogburn, R. W.; Thompson, K. L.] Kavli Inst Particle Astrophys & Cosmol, SLAC Natl Accelerator Lab, 2575 Sand Hill Rd, Menlo Pk, CA 94025 USA.
[Aikin, R. W.] CALTECH, Dept Phys, Pasadena, CA 91125 USA.
[Alexander, K. D.; Barkats, D.; Bischoff, C. A.; Bowens-Rubin, R.; Buder, I.; Connors, J.; Harrison, S.; Karkare, K. S.; Kovac, J. M.; Richter, S.; Vieregg, A. G.; Wong, C. L.] Harvard Smithsonian Ctr Astrophys, 60 Garden St MS 42, Cambridge, MA 02138 USA.
[Benton, S. J.; Netterfield, C. B.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Bock, J. J.; Brevik, J. A.; Filippini, J. P.; Hildebrandt, S. R.; O'Brient, R.; Orlando, A.; Teply, G. P.] CALTECH, Dept Phys, Pasadena, CA 91125 USA.
[Bock, J. J.; Crill, B. P.; Hildebrandt, S. R.; Megerian, K. G.; Nguyen, H. T.; O'Brient, R.; Orlando, A.; Turner, A. D.] Jet Prop Lab, Pasadena, CA 91109 USA.
[Bullock, E.; Fliescher, S.; Pryke, C.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA.
[Dyorkin, C.; Kovac, J. M.; Wong, C. L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Duband, L.] Commissariat Energie Atom, Serv Basses Temp, F-38054 Grenoble, France.
[Filippini, J. P.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
[Halpern, M.; Wiebe, D. V.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Hilton, G. C.] NIST, Boulder, CO 80305 USA.
[Kaufman, J. P.; Keating, B. G.; Teply, G. P.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA.
[Leitch, E. M.; Sheehy, C. D.; Vieregg, A. G.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Hui, H.; Kefeli, S.; Lueker, M.; Netterfield, C. B.; Staniszewski, Z. K.; Steinbach, B.] Canadian Inst Adv Res, Toronto, ON M5G 1Z8, Canada.
[Pryke, C.; Schwarz, R.; Sheehy, C. D.; Staniszewski, Z. K.; Weber, A. C.; Willmert, J.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Vieregg, A. G.] Univ Chicago, Enrico Fermi Inst, Dept Phys, Chicago, IL 60637 USA.
[Wu, W. L. K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
RP Namikawa, T (reprint author), Stanford Univ, Dept Phys, Stanford, CA 94305 USA.; Namikawa, T (reprint author), Kavli Inst Particle Astrophys & Cosmol, SLAC Natl Accelerator Lab, 2575 Sand Hill Rd, Menlo Pk, CA 94025 USA.
EM namikawa@slac.stanford.edu
OI Bischoff, Colin/0000-0001-9185-6514; Alexander, Kate/0000-0002-8297-2473
FU National Science Foundation [ANT-1145172, ANT-1145143, ANT-1145248];
Keck Foundation (Caltech); JPL Research and Technology Development Fund;
NASA APRA program [06-ARPA206-0040, 10-SAT10-0017]; NASA SAT program
[06-ARPA206-0040, 10-SAT10-0017]; Gordon and Betty Moore Foundation at
Caltech; Canada Foundation for Innovation grant; FAS Science Division
Research Computing Group at Harvard University; U.S. Department of
Energy Office of Science; Japan Society for the Promotion of Science
FX The Keck Array project has been made possible through support from the
National Science Foundation under Grants ANT-1145172 (Harvard),
ANT-1145143 (Minnesota), and ANT-1145248 (Stanford), and from the Keck
Foundation (Caltech). The development of antenna-coupled detector
technology was supported by the JPL Research and Technology Development
Fund and grant Nos. 06-ARPA206-0040 and 10-SAT10-0017 from the NASA APRA
and SAT programs. The development and testing of focal planes were
supported by the Gordon and Betty Moore Foundation at Caltech. Readout
electronics were supported by a Canada Foundation for Innovation grant
to UBC. The computations in this paper were run on the Odyssey cluster
supported by the FAS Science Division Research Computing Group at
Harvard University. The analysis effort at Stanford and SLAC is
partially supported by the U.S. Department of Energy Office of Science.
We thank the staff of the U.S. Antarctic Program and in particular the
South Pole Station without whose help this research would not have been
possible. Special thanks go to our heroic winter-overs Robert Schwarz
and Steffen Richter. We thank all those who have contributed past
efforts to the BICEP-Keck Array series of experiments, including the
BICEP1 team. T.N. acknowledges support from Japan Society for the
Promotion of Science Postdoctoral Fellowships for Research Abroad.
NR 75
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 20
PY 2016
VL 833
IS 2
AR 228
DI 10.3847/1538-4357/833/2/228
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EG6PY
UT WOS:000391169600103
ER
PT J
AU Boorman, PG
Gandhi, P
Alexander, DM
Annuar, A
Ballantyne, DR
Bauer, F
Boggs, SE
Brandt, WN
Brightman, M
Christensen, FE
Craig, WW
Farrah, D
Hailey, CJ
Harrison, FA
Honig, SF
Koss, M
LaMassa, SM
Masini, A
Ricci, C
Risaliti, G
Stern, D
Zhang, WW
AF Boorman, Peter G.
Gandhi, P.
Alexander, D. M.
Annuar, A.
Ballantyne, D. R.
Bauer, F.
Boggs, S. E.
Brandt, W. N.
Brightman, M.
Christensen, F. E.
Craig, W. W.
Farrah, D.
Hailey, C. J.
Harrison, F. A.
Honig, S. F.
Koss, M.
LaMassa, S. M.
Masini, A.
Ricci, C.
Risaliti, G.
Stern, D.
Zhang, W. W.
TI IC 3639-A NEW BONA FIDE COMPTON-THICK AGN UNVEILED BY NuSTAR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: nuclei; galaxies: Seyfert; techniques:
spectroscopic; X-rays: galaxies; X-rays: individual (IC 3639)
ID ACTIVE GALACTIC NUCLEI; SEYFERT 2 GALAXIES; X-RAY CORRELATION;
SUBARCSECOND MIDINFRARED VIEW; K-ALPHA EMISSION; XMM-NEWTON; MU-M;
EXTREME ABSORPTION; IRON LINES; BLACK-HOLE
AB We analyze high-quality NuSTAR observations of the local (z = 0.011) Seyfert 2 active galactic nucleus (AGN) IC 3639, in conjunction with archival Suzaku and Chandra data. This provides the first broadband X-ray spectral analysis of the source, spanning nearly two decades in energy (0.5-30 keV). Previous X-ray observations of the source below 10 keV indicated strong reflection/obscuration on the basis of a pronounced iron fluorescence line at 6.4 keV. The hard X-ray energy coverage of NuSTAR, together with self-consistent toroidal reprocessing models, enables direct broadband constraints on the obscuring column density of the source. We find the source to be heavily Compton-thick (CTK) with an obscuring column in excess of 3.6 x 10(24) cm(-2), unconstrained at the upper end. We further find an intrinsic 2-10 keV luminosity of log(10) (L2-10keV[erg s(-1)] = 43.4(-1.1)(+0.6) to 90% confidence, almost 400 times the observed flux, and consistent with various multiwavelength diagnostics. Such a high ratio of intrinsic to observed flux, in addition to an Fe-K alpha fluorescence line equivalent width exceeding 2 keV, is extreme among known bona fide CTK AGNs, which we suggest are both due to the high level of obscuration present around IC 3639. Our study demonstrates that broadband spectroscopic modeling with NuSTAR enables large corrections for obscuration to be carried out robustly and emphasizes the need for improved modeling of AGN tori showing intense iron fluorescence.
C1 [Boorman, Peter G.; Gandhi, P.; Honig, S. F.] Univ Southampton, Fac Phys Sci & Engn, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Alexander, D. M.; Annuar, A.] Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England.
[Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Bauer, F.; Ricci, C.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Casilla 306, Santiago 22, Chile.
[Bauer, F.; Ricci, C.] Pontificia Univ Catolica Chile, Fac Fis, Ctr Astroingn, Casilla 306, Santiago 22, Chile.
[Bauer, F.] Millennium Inst Astrophys MAS, Nuncio Monsenor Sotero Sanz 100, Santiago, Chile.
[Bauer, F.] Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA.
[Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Brandt, W. N.] Penn State Univ, Davey Lab 525, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Brandt, W. N.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Brandt, W. N.] Penn State Univ, Dept Phys, Davey Lab 104, University Pk, PA 16802 USA.
[Brightman, M.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Christensen, F. E.; Craig, W. W.] Tech Univ Denmark, DTU Space Natl Space Inst, Elektrovej 327, DK-2800 Lyngby, Denmark.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Craig, W. W.] Dept Phys, Virginia Tech, Blacksburg, VA 24061 USA.
[Farrah, D.] Dept Phys, Virginia Tech, Blacksburg, VA 24061 USA.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Koss, M.] Swiss Fed Inst Technol, Inst Astron, Dept Phys, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.
[Harrison, F. A.] NASA Postdoctoral Program Fellow, NASA Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA.
[Masini, A.] Univ Bologna, Dipartimento Fis Astron DIFA, Viale Berti Pichat 6-2, I-40127 Bologna, Italy.
[Risaliti, G.] INAFArcetri Observ, Largo Fermi 5, I-50126 Florence, Italy.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Stern, D.] NASA Goddard Space Flight Ctr, X Ray Astrophys Lab, Greenbelt, MD 20771 USA.
RP Boorman, PG (reprint author), Univ Southampton, Fac Phys Sci & Engn, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England.
EM p.g.boorman@soton.ac.uk
OI Ballantyne, David/0000-0001-8128-6976
FU National Aeronautics and Space Administration; STFC [ST/J003697/2]; RAS;
Majlis Amanah Rakyat (MARA), Malaysia; Caltech NuSTAR [44A-1092750];
European Research Council [ERC-2015-StG-677117]; Swiss National Science
Foundation (SNSF) [PZOOP2_154799/1]; NASA; ASI/INAF grant
[I/037/12/0-011/13]; NASA NuSTAR A01 Award [NNX15AV27G]; CONICYT-Chile
[Basal-CATA PFB-06/2007]; FONDECYT Regular [1141218, 1151408];
China-CONICYT; Ministry of Economy, Development, and Tourism's
Millennium Science Initiative [IC120009]
FX We thank the anonymous referee for the invaluable comments that helped
to improve this paper. This work made use of data from the NuSTAR
mission, a project led by the California Institute of Technology,
managed by the Jet Propulsion Laboratory, and funded by the National
Aeronautics and Space Administration. We thank the NuSTAR Operations,
Software, and Calibration teams for support with the execution and
analysis of these observations. This research has made use of the NuSTAR
Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science
Data Center (ASDC, Italy) and the California Institute of Technology
(USA). The scientific results reported in this article are based on
observations made by the ChandraX-ray Observatory.; This publication
makes use of data products from the Wide field Infrared Survey Explorer,
which is a joint project of the University of California, Los Angeles,
and the Jet Propulsion Laboratory/California Institute of Technology,
funded by the National Aeronautics and Space Administration.; P.B.
thanks STFC and the RAS for funding.; P.G. thanks STFC for support
(grant reference ST/J003697/2).; A.A. acknowledges financial support
from Majlis Amanah Rakyat (MARA), Malaysia.; W.N.B. acknowledges Caltech
NuSTAR subcontract 44A-1092750 and the VM Willaman Endowment.; S.F.H.
acknowledges support from the European Research Council under Horizon
2020 grant ERC-2015-StG-677117.; M.K. acknowledges support from the
Swiss National Science Foundation (SNSF) through the Ambizione
fellowship grant PZOOP2_154799/1.; S.M.L. acknowledges support by an
appointment to the NASA Postdoctoral Program at the NASA Goddard Space
Flight Center, administered by the Universities Space Research
Association under contract with NASA.; A.M. acknowledges support from
the ASI/INAF grant I/037/12/0-011/13.; F.E.B. and C.R. acknowledge
support from NASA NuSTAR A01 Award NNX15AV27G, CONICYT-Chile grants
Basal-CATA PFB-06/2007, FONDECYT Regular 1141218 and 1151408, "EMBIGGEN"
Anillo ACT1101, the China-CONICYT, and the Ministry of Economy,
Development, and Tourism's Millennium Science Initiative through grant
IC120009, awarded to The Millennium Institute of Astrophysics, MAS.
NR 89
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 20
PY 2016
VL 833
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PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EG6PY
UT WOS:000391169600120
ER
PT J
AU Clemens, DP
Tassis, K
Goldsmith, PF
AF Clemens, Dan P.
Tassis, K.
Goldsmith, Paul F.
TI THE MAGNETIC FIELD OF L1544. I. NEAR-INFRARED POLARIMETRY AND THE
NON-UNIFORM ENVELOPE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Galaxy: disk; ISM: individual objects (L1544); ISM: magnetic fields;
magnetic fields; polarization; techniques: polarimetric
ID POLARIZATION SURVEY GPIPS; CLERK MAXWELL TELESCOPE; OH-ZEEMAN
OBSERVATIONS; MOLECULAR CLOUD CORES; STAR-FORMATION; DARK CLOUDS;
AMBIPOLAR-DIFFUSION; DENSE CORES; INTERSTELLAR CLOUDS; PRESTELLAR CORES
AB The magnetic field (B-field) of the starless dark cloud L1544 has been studied using near-infrared (NIR) background starlight polarimetry (BSP) and archival data in order to characterize the properties of the plane-of-sky B-field. NIR linear polarization measurements of over 1700 stars were obtained in the H band and 201 of these were also measured in the K band. The NIR BSP properties are correlated with reddening, as traced using the Rayleigh-Jeans color excess (H-M) method, and with thermal dust emission from the L1544 cloud and envelope seen in Herschel maps. The NIR polarization position angles change at the location of the cloud and exhibit their lowest dispersion there, offering strong evidence that NIR polarization traces the plane-of-sky B-field of L1544. In this paper, the uniformity of the plane-of-sky B-field in the envelope region of L1544 is quantitatively assessed. This allows evaluation of the approach of assuming uniform field geometry when measuring relative mass-to-flux ratios in the cloud envelope and core based on averaging of the radio Zeeman observations in the envelope, as done by Crutcher et al. In L1544, the NIR BSP shows the envelope B-field to be significantly non-uniform and likely not suitable for averaging Zeeman properties without treating intrinsic variations. Deeper analyses of the NIR BSP and related data sets, including estimates of the B-field strength and testing how it varies with position and gas density, are the subjects of later papers in this series.
C1 [Clemens, Dan P.] Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02215 USA.
[Tassis, K.] Univ Crete, Dept Phys, Iraklion 71003, Greece.
[Tassis, K.] Univ Crete, ITCP, Iraklion 71003, Greece.
[Tassis, K.] Fdn Res & Technol Hellas, IESL, POB 1527, GR-71110 Iraklion, Greece.
[Goldsmith, Paul F.] Jet Prop Lab, M-S 169-504,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Clemens, DP (reprint author), Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02215 USA.
EM clemens@bu.edu; tassis@physics.uoc.gr; paul.f.goldsmith@jpl.nasa.gov
RI Tassis, Konstantinos/C-3155-2011
FU NASA; NSF; FP7 through Marie Curie Career Integration Grant "SFOnset"
[PCIG-GA-2011- 293531]; EU FP7 Grant "EuroCal" [PIRSES-GA-2012-31578];
W.M. Keck Foundation; NSF/MPS [AST 06-07500, 09-07790, 14-12269]; NASA
ADAP [NNX15AE51G]; BU-LO
FX The authors thank Dick Crutcher and Tom Troland for answering questions
concerning their Zeeman observations of L1544 and thank the two
reviewers for their sincere efforts to improve the paper. Brian Taylor
rebuilt a key Mimir computer just in time to enable the 2016 January
observations on the last clear night of the run. This publication makes
use of data products from the Two Micron All Sky Survey, which is a
joint project of the University of Massachusetts and the Infrared
Processing and Analysis Center/California Institute of Technology
(CalTech), funded by NASA and NSF. AllWISE makes use of data from WISE,
which is a joint project of the University of California, Los Angeles,
and the Jet Propulsion Laboratory (JPL)/CalTech, and NEOWISE, which is a
project of JPL/CalTech. WISE and NEOWISE are funded by NASA. This
research has made use of the VizieR catalog access tool, CDS,
Strasbourg, France. VizieR is a joint effort of CDS (Centre de Donnees
astronomiques de Strasbourg) and ESA-ESRIN (Information Systems
Division).; This research was conducted in part at JPL, which is
operated for NASA by CalTech. K.T. acknowledges support by FP7 through
Marie Curie Career Integration Grant PCIG-GA-2011- 293531 "SFOnset," and
partial support from the EU FP7 Grant PIRSES-GA-2012-31578 "EuroCal."
This research was conducted in part using the Mimir instrument, jointly
developed at Boston University (BU) and Lowell Observatory (LO) and
supported by NASA, NSF, and the W.M. Keck Foundation. Mimir observations
and analyses have been made possible by grants AST 06-07500, 09-07790,
and 14-12269 from NSF/MPS, by NASA ADAP grant NNX15AE51G, and by grants
of significant observing time from the BU-LO partnership.
NR 85
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 20
PY 2016
VL 833
IS 2
AR 176
DI 10.3847/1538-4357/833/2/176
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EG6PY
UT WOS:000391169600051
ER
PT J
AU Darnley, MJ
Henze, M
Bode, MF
Haciusu, I
Hernanz, M
Hornoch, K
Hounsell, R
Kato, M
Ness, JU
Osborne, JP
Page, KL
Ribeiro, VARM
Rodriguez-Gil, P
Shafter, AW
Shara, MM
Steele, IA
Williams, SC
Arai, A
Arcavi, I
Barsukova, EA
Boumis, P
Chen, T
Fabrika, S
Figueira, J
Gao, X
Gehrels, N
Godon, P
Goranskij, VP
Harman, DJ
Hartmann, DH
Hosseinzade, G
Horst, JC
Itagam, K
Jose, J
Kabashima, F
Kaur, A
Kawm, N
Kennea, JA
Kiyota, S
Kucakkova, H
Lau, KM
Maehara, H
Naito, H
Nakajima, K
Nishiyama, K
O'Brien, TJ
Quimby, R
Sala, G
Sano, Y
Sion, EM
Valeev, AF
Watanabe, F
Watanabe, M
Williams, BF
Xu, Z
AF Darnley, M. J.
Henze, M.
Bode, M. F.
Haciusu, I.
Hernanz, M.
Hornoch, K.
Hounsell, R.
Kato, M.
Ness, J. -U.
Osborne, J. P.
Page, K. L.
Ribeiro, V. A. R. M.
Rodriguez-Gil, P.
Shafter, A. W.
Shara, M. M.
Steele, I. A.
Williams, S. C.
Arai, A.
Arcavi, I.
Barsukova, E. A.
Boumis, P.
Chen, T.
Fabrika, S.
Figueira, J.
Gao, X.
Gehrels, N.
Godon, P.
Goranskij, V. P. .
Harman, D. J.
Hartmann, D. H.
Hosseinzade, G.
Horst, J. Chuck
Itagam, K.
Jose, J.
Kabashima, F.
Kaur, A.
Kawm, N.
Kennea, J. A.
Kiyota, S.
Kucakkova, H.
Lau, K. M.
Maehara, H.
Naito, H.
Nakajima, K.
Nishiyama, K.
O'Brien, T. J.
Quimby, R.
Sala, G.
Sano, Y.
Sion, E. M.
Valeev, A. F.
Watanabe, F.
Watanabe, M.
Williams, B. F.
Xu, Z.
TI M31N 2008-12a-THE REMARKABLE RECURRENT NOVA IN M31: PANCHROMATIC
OBSERVATIONS OF THE 2015 ERUPTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (M31); novae cataclysmic variables; stars:
individual (M31N 2008-12a); ultraviolet: stars; X-rays: binaries
ID X-RAY OBSERVATIONS; MULTIWAVELENGTH LIGHT-CURVE; AGAPE MICROLENSING
SURVEY; UNIVERSAL DECLINE LAW; UBV COLOR EVOLUTION; SUPER-SOFT PHASE; RS
OPHIUCHI 1985; CLASSICAL NOVAE; 2006 OUTBURST; WHITE-DWARFS
AB The Andromeda Galaxy recurrent nova M31N 2008-12a had been observed in eruption 10 times, including yearly eruptions from 2008 to 2014. With a measured recurrence period of P-rec = 351 +/- 13 days (we believe the true value to be half of this) and a white dwarf very close to the Chandrasekhar limit, M31N 2008-12a has become the leading pre-explosion supernova type Ia progenitor candidate. Following multi-wavelength follow-up observations of the 2013 and 2014 eruptions, we initiated a campaign to ensure early detection of the predicted 2015 eruption, which triggered ambitious ground and space-based follow-up programs. In this paper we present the 2015 detection, visible to near-infrared photometry and visible spectroscopy, and ultraviolet and X-ray observations from the Swift. observatory. The LCOGT 2 m (Hawaii) discovered the 2015 eruption, estimated to have commenced at August 28.28 +/- 0.12 UT. The 2013-2015 eruptions are remarkably similar at all wavelengths. New early spectroscopic observations reveal short-lived emission from material with velocities similar to 13,000 km s(-1), possibly collimated outflows. Photometric and spectroscopic observations of the eruption provide strong evidence supporting a red giant donor. An apparently stochastic variability during the early supersoft X-ray phase was comparable in amplitude and duration to past eruptions, but the 2013 and 2015 eruptions show evidence of a brief flux dip during this phase. The multi-eruption Swift/XRT spectra show tentative evidence of high-ionization emission lines above a high-temperature continuum. Following Henze et al. (2015a), the updated recurrence period based on all known eruptions is P-rec = 174 +/- 10 days, and we expect the next eruption of M31N 2008-12a. to occur around 2016 mid-September.
C1 [Darnley, M. J.; Bode, M. F.; Steele, I. A.; Williams, S. C.; Harman, D. J.] Liverpool John Moores Univ, Astrophys Res Inst, IC2 Liverpool Sci Pk, Liverpool L3 5RF, Merseyside, England.
[Henze, M.; Hernanz, M.] CSIC IEEC, Inst Ciencies Espai, Campus UAB,C Can Magrans S-N, E-08193 Cerdanyola Del Valles, Spain.
[Haciusu, I.] Univ Tokyo, Dept Earth Sci & Astron, Coll Arts & Sci, Meguro Ku, 3-8-1 Komaba, Tokyo 1538902, Japan.
[Hornoch, K.] Acad Sci, Astron Inst, CZ-25165 Ondrejov, Czech Republic.
[Hounsell, R.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA.
[Kato, M.] Keio Univ, Dept Astron, Yokohama, Kanagawa 2238521, Japan.
[Ness, J. -U.] European Space Astron Ctr, Camino Bajo Castillo S-N, E-28692 Madrid, Spain.
[Osborne, J. P.; Page, K. L.] Univ Leicester, Dept Phys & Astron, Xray & Observat Astron Grp, Leicester LE1 7RH, Leics, England.
[Ribeiro, V. A. R. M.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands.
[Rodriguez-Gil, P.] Inst Astrofis Canarias, Via Lactea S-N, E-38205 San Cristobal la Laguna, Santa Cruz De T, Spain.
[Rodriguez-Gil, P.] Univ La Laguna, Dept Astrofis, E-38205 San Cristobal la Laguna, Santa Cruz De T, Spain.
[Shafter, A. W.; Horst, J. Chuck; Quimby, R.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Shara, M. M.] Amer Museum Nat Hist, 79th St & Cent Pk West, New York, NY 10024 USA.
[Williams, S. C.] Univ Lancaster, Dept Phys, Lancaster LA1 4YB, England.
[Arai, A.] Kyoto Sangyo Univ, Koyama Astron Observ, Kita Ku, Kyoto, Kyoto 6038555, Japan.
[Arcavi, I.; Hosseinzade, G.] Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA.
[Barsukova, E. A.] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA.
[Fabrika, S.; Valeev, A. F.] Russian Acad Sci, Special Astrophys Observ, Nizhnii Arkhyz 369167, Karachai Cherke, Russia.
[Boumis, P.] Natl Observ Athens, Inst Astron Astrophys Space Applicat & Remote, Penteli 15236, Greece.
[Chen, T.; Lau, K. M.] Corona Borealis Observ, Ngari, Tibet, Peoples R China.
[Fabrika, S.; Valeev, A. F.] Kazan Fed Univ, Kazan 420008, Russia.
[Figueira, J.; Jose, J.; Sala, G.] Univ Politecn Cataluna, EUETIB, Dept Fis, C-Compte dUrgell 187, E-08036 Barcelona, Spain.
[Figueira, J.; Jose, J.; Sala, G.] Inst dEstudis Espacials Catalunya, C-Gran Capita 2-4,Ed Nexus-201, E-08034 Barcelona, Spain.
[Gao, X.] Xingming Observ, Urumqi, Xinjiang, Peoples R China.
[Gehrels, N.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Godon, P.; Sion, E. M.] Villanova Univ, Dept Astron & Astrophys, 800 Lancaster Ave, Villanova, PA 19085 USA.
[Goranskij, V. P. .] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Univ Prospect 13, Moscow 119899, Russia.
[Hartmann, D. H.; Kaur, A.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA.
[Hosseinzade, G.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Itagam, K.] Itagaki Astron Observ, Teppo, Yamagata 9902492, Japan.
[Kabashima, F.; Nishiyama, K.] MiyakiArgenteus Observ, Miyaki, Saga 8401102, Japan.
[Kawm, N.] Tokyo Inst Technol, Dept Phys, Meguro Ku, 2-12-1 Ookayama, Tokyo 1528551, Japan.
[Kennea, J. A.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
[Kiyota, S.] VSOLJ, 7-1 Kitahatsutomi, Kamagaya 2730126, Japan.
[Kucakkova, H.] Charles Univ Prague, Fac Mathemath & Phys, Astron Inst, Holesovickach 2, CR-18000 Prague 8, Czech Republic.
[Maehara, H.] Natl Inst Nat Sci, NAOJ, Okayama Astrophys Observ, 3037-5 Honjo, Okayama 7190232, Japan.
[Naito, H.; Nakajima, K.; Sano, Y.; Watanabe, F.] Nayoro Observ, 157-1 Nisshin, Nayoro, Hokkaido 0960066, Japan.
[Nakajima, K.] Rikubetsu Space & Earth Sci Museum, Ashoro, Hokkaido 0894301, Japan.
[O'Brien, T. J.] Univ Manchester, Jodrell Bank Ctr Astrophys, Alan Turing Bldg, Manchester M13 9PL, Lancs, England.
[Sano, Y.] Hokkaido Univ, Fac Sci, Observat & Data Ctr Cosmosci, Kita Ku, Sapporo, Hokkaido 0600810, Japan.
[Watanabe, M.] Hokkaido Univ, Dept Cosmosci, Kita Ku, Kita 10,Nishi 8, Sapporo, Hokkaido 0600810, Japan.
[Watanabe, M.] Okayama Univ Sci, Dept Appl Phys, Kita Ku, 1-1 Ridai cho, Okayama, Okayama 7000005, Japan.
[Williams, B. F.] Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
[Xu, Z.] Nanjing Putian Telecommun Co Ltd, 1 Putian Rd, Nanjing, Jiangsu 210012, Peoples R China.
RP Darnley, MJ (reprint author), Liverpool John Moores Univ, Astrophys Res Inst, IC2 Liverpool Sci Pk, Liverpool L3 5RF, Merseyside, England.; Henze, M (reprint author), CSIC IEEC, Inst Ciencies Espai, Campus UAB,C Can Magrans S-N, E-08193 Cerdanyola Del Valles, Spain.
EM M.J.Darnley@ljmu.ac.uk; henze@ice.cat
OI Darnley, Matt/0000-0003-0156-3377; Williams, Steven/0000-0001-8178-0202;
Henze, Martin/0000-0001-9985-3406
FU RFBR [16 February 00758]; Spanish Ministry of Economy and
Competitiveness (MINECO) [AYA2014-59084-P]; E.U. FEDER funds;
AGAUR/Generalitat de Catalunya [SGR0038/2014]; Russian Scientific
Foundation [14-50-00043]; Russian Government Program of Competitive
Growth of Kazan Federal University; Spanish MINECO [FDPI-2013-16933];
MINECO [ESP2014-56003-R]; UK Space Agency; Radboud Excellence
Initiative; LJMU; NSF [AST-1009566]; NASA [HST-Go-14125.012]; STFC; MEXT
of Japan; National Aeronautics and Space Administration; National
Science Foundation; [RVO:67985815]
FX E.A.B., A.F.V., and V.P.G. acknowledge support from RFBR Grant No. 16
February 00758. J.F., J.J., and G.S. acknowledge support from Spanish
Ministry of Economy and Competitiveness (MINECO) grant AYA2014-59084-P,
the E.U. FEDER funds, and AGAUR/Generalitat de Catalunya grant
SGR0038/2014. S.F. acknowledges support from the Russian Scientific
Foundation (grant N 14-50-00043) and the Russian Government Program of
Competitive Growth of Kazan Federal University. M. Henze acknowledges
the support of the Spanish MINECO under grant FDPI-2013-16933. M.
Hernanz acknowledges MINECO support under grant ESP2014-56003-R. K.H.
was supported by the project RVO:67985815. J.P.O. and K.L.P. acknowledge
funding from the UK Space Agency. VARMR acknowledges financial support
from the Radboud Excellence Initiative. S.C.W. acknowledges a visiting
research fellowship at LJMU. This work has been supported in part by NSF
grant AST-1009566 and NASA grant HST-Go-14125.012.; The Liverpool
Telescope is operated on the island of La Palma by Liverpool John Moores
University (LJMU) in the Spanish Observatorio del Roque de los Muchachos
of the Instituto de Astrofisica de Canarias with financial support from
STFC. This work makes use of observations from the LCOGT network. The
Pirka telescope is operated by the Graduate School of Science, Hokkaido
University, which also participates in the Optical and Near-Infrared
Astronomy Inter University Cooperation Program, supported by the MEXT of
Japan. This research made use of data supplied by the UK Swift Science
Data Centre at the University of Leicester. This publication makes use
of data products from the Two Micron All Sky Survey (2MASS), which is a
joint project of the University of Massachusetts and the Infrared
Processing and Analysis Center/California Institute of Technology,
funded by the National Aeronautics and Space Administration and the
National Science Foundation. This research has made use of NASA's
Astrophysics Data System Bibliographic Services.
NR 228
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 20
PY 2016
VL 833
IS 2
AR 149
DI 10.3847/1538-4357/833/2/149
PG 38
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EG6PY
UT WOS:000391169600024
ER
PT J
AU Dodson-Robinson, SE
Su, KYL
Bryden, G
Harvey, P
Green, JD
AF Dodson-Robinson, Sarah E.
Su, Kate Y. L.
Bryden, Geoff
Harvey, Paul
Green, Joel D.
TI HERSCHEL OBSERVATIONS AND UPDATED SPECTRAL ENERGY DISTRIBUTIONS OF FIVE
SUNLIKE STARS WITH DEBRIS DISKS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; infrared: planetary systems; stars: individual
(eta Cru, HD 33636, HD 50554, HD 52265)
ID SPITZER INFRARED SPECTROGRAPH; SOLAR-TYPE STAR; COLLISIONAL CASCADES;
RADIATIVE-TRANSFER; EPSILON-ERIDANI; AU MICROSCOPII; KUIPER-BELT; HR
8799; DUST; PLANETS
AB Observations from the Herschel Space Observatory have more than doubled the number of wide debris disks orbiting Sunlike stars to include over 30 systems with R > 100 AU. Here we present new Herschel PACS and re-analyzed Spitzer MIPS photometry of five Sunlike stars with wide debris disks, from Kuiper belt size to R > 150 AU. The disk surrounding HD 105211 is well resolved, with an angular extent of >14" along the major axis, and the disks of HD 33636, HD 50554, and HD 52265 are extended beyond the PACS PSF size (50% of energy enclosed within radius 4.23"). HD 105211 also has a 24 mu m infrared excess that was previously overlooked because of a poorly constrained photospheric model. Archival Spitzer IRS observations indicate that the disks have small grains of minimum radius a(min) similar to 3 mu m, although the a(min) is larger than the radiation pressure blowout size in all systems. If modeled as single-temperature blackbodies, the disk temperatures would all be <60 K. Our radiative transfer models predict actual disk radii approximately twice the radius of model blackbody disks. We find that the Herschel photometry traces dust near the source population of planetesimals. The disk luminosities are in the range 2 x 10(-5) <= L/L-circle dot <= 2 x 10(-4) , consistent with collisions in icy planetesimal belts stirred by Pluto-size dwarf planets.
C1 [Dodson-Robinson, Sarah E.] Univ Delaware, Dept Phys & Astron, 217 Sharp Lab, Newark, DE 19716 USA.
[Su, Kate Y. L.] Univ Arizona, Dept Astron, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.
[Bryden, Geoff] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Harvey, Paul; Green, Joel D.] Univ Texas Austin, Dept Astron, 4800 Oak Grove Dr, Austin, TX 78712 USA.
[Green, Joel D.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
RP Dodson-Robinson, SE (reprint author), Univ Delaware, Dept Phys & Astron, 217 Sharp Lab, Newark, DE 19716 USA.
EM sdr@udel.edu
OI Green, Joel/0000-0003-1665-5709
FU NASA [1524391]; National Aeronautics and Space Administration
FX Funding for this work was provided by NASA research support agreement
1524391. We thank Roberta Paladini of the HASA Herschel Science Center
for guidance on data reduction and Sebastian Wolf for developing the
publicly available Debris Disk Simulator tool. John Gizis and Neal Evans
provided helpful input on data analysis methods. This research has made
use of the following resources: (1) Herschel Interactive Processing
Environment (HIPE) and the ipipe scripts for data reduction. (2) VizieR
catalogue access tool, CDS, Strasbourg, France. The original description
of the VizieR service was published in A&AS 143, 23. (3) NASA/IPAC
Infrared Science Archive, which is operated by the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
NASA. (4) SIMBAD database, operated at CDS, Strasbourg, France; Wenger
et al. (2000). (5) Herschel Science Archive,
www.cosmos.esa.int/web/herschel/science-archive. (6) Astropy python
library for astronomy, www.astropy.org. (7) APLpy (Astronomical Plotting
Library in Python), aplpy.github.io. (8) Data products from the
Wide-field Infrared Survey Explorer, which is a joint project of the
University of California, Los Angeles, and the Jet Propulsion
Laboratory/California Institute of Technology, funded by the National
Aeronautics and Space Administration.
NR 81
TC 0
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U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 20
PY 2016
VL 833
IS 2
AR 183
DI 10.3847/1538-4357/833/2/183
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EG6PY
UT WOS:000391169600058
ER
PT J
AU Gopalswamy, N
Yashiro, S
Thakur, N
Makela, P
Xie, H
Akiyama, S
AF Gopalswamy, N.
Yashiro, S.
Thakur, N.
Maekelae, P.
Xie, H.
Akiyama, S.
TI THE 2012 JULY 23 BACKSIDE ERUPTION: AN EXTREME ENERGETIC PARTICLE EVENT?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE shock waves; Sun: coronal mass ejections (CMEs); Sun: filaments,
prominences; Sun: flares; Sun: particle emission; Sun: radio radiation
ID CORONAL MASS EJECTIONS; SOLAR-CYCLE 24; GROUND-LEVEL EVENTS; SPACE
WEATHER EVENT; INTERPLANETARY SPACE; SHOCK FORMATION; STEREO MISSION;
RELEASE TIMES; SEP EVENT; NEAR-SUN
AB The backside coronal mass ejection (CME) of 2012 July 23 had a short Sun-to-Earth shock transit time (18.5 hr). The associated solar energetic particle (SEP) event had a >10 MeV proton flux peaking at similar to 5000 pfu, and the energetic storm particle event was an order of magnitude larger, making it the most intense event in the space era at these energies. By a detailed analysis of the CME, shock, and SEP characteristics, we find that the July 23 event is consistent with a high-energy SEP event (accelerating particles to gigaelectronvolt. energies). The times of maximum and fluence spectra in the range 10-100 MeV were very hard, similar to those of ground-level enhancement (GLE) events. We found a hierarchical relationship between the CME initial speeds and the fluence spectral indices: CMEs with low initial speeds had SEP events with the softest spectra, while those with the. highest initial speeds had SEP events with the hardest spectra. CMEs attaining intermediate speeds result in moderately hard spectra. The July 23 event was in the group of hard-spectrum events. During the July 23 event, the shock speed (>2000 km s(-1)), the initial acceleration (similar to 1.70 km s(-2)), and the shock-formation height (similar to 1.5 solar radii) were all typical of GLE events. The associated type II burst had emission components from meter. to kilometer. wavelengths, suggesting a strong shock. These observations confirm that the 2012 July 23 event is likely to be an extreme event in terms of the energetic particles it accelerated.
C1 [Gopalswamy, N.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Code 671, Greenbelt, MD 20771 USA.
[Yashiro, S.; Thakur, N.; Maekelae, P.; Xie, H.; Akiyama, S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Yashiro, S.; Thakur, N.; Maekelae, P.; Xie, H.; Akiyama, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Solar Phys Lab, Code 671, Greenbelt, MD 20771 USA.
EM nat.gopalswamy@nasa.gov
OI Makela, Pertti/0000-0002-8182-4559
FU NASA/LWS program; H-GI program; NSF [AGS-1358274, AGS-1622377]; NASA
[NNX15AB77G, NNX15AB70G]
FX We thank NOAA/NGDC for making the GOES proton data available and the
Oulu Cosmic Ray Station for the GLE list used in this paper. This work
benefitted greatly from the open data policy of NASA in using SDO,
SAMPEX, SOHO, STEREO, and Wind data. The SWAP data were obtained via the
Helioviewer website. STEREO is a mission in NASA's Solar Terrestrial
Probes program. SOHO is a project of international collaboration between
ESA and NASA. We thank the anonymous referee for the comments that
helped improve the paper. The work of NG, SY, and SA was supported by
NASA/LWS and H-GI programs. PM was partially supported by NSF grant
AGS-1358274 and NASA grant NNX15AB77G. HX was partially supported by
NASA grant NNX15AB70G. NT was partially supported by NSF grant
AGS-1622377.
NR 81
TC 0
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U1 0
U2 0
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 20
PY 2016
VL 833
IS 2
AR 216
DI 10.3847/1538-4357/833/2/216
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EG6PY
UT WOS:000391169600091
ER
PT J
AU Inglis, AR
Ireland, J
Dennis, BR
Hayes, L
Gallagher, P
AF Inglis, A. R.
Ireland, J.
Dennis, B. R.
Hayes, L.
Gallagher, P.
TI A LARGE-SCALE SEARCH FOR EVIDENCE OF QUASI-PERIODIC PULSATIONS IN SOLAR
FLARES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: statistical; Sun: corona; Sun: flares; Sun: oscillations; Sun:
X-rays, gamma rays
ID GAMMA-RAY BURST; HARD X-RAY; MAGNETIC RECONNECTION; MAGNETOHYDRODYNAMIC
OSCILLATIONS; PARTICLE-ACCELERATION; ENERGETIC PARTICLES; FOOTPOINT
MOTIONS; RED NOISE; EMISSION; MICROWAVE
AB The nature of quasi-periodic pulsations (QPP) in solar flares is poorly constrained, and critically the general prevalence of such signals in solar flares is unknown. Therefore, we perform a large-scale search for evidence of signals consistent with QPP in solar flares, focusing on the 1-300 s timescale. We analyze 675 M- and X-class flares observed by the Geostationary Operational Environmental Satellite (GOES) series in 1-8 angstrom soft X-rays between 2011 February 1 and 2015 December 31. Additionally, over the same era we analyze Fermi/Gamma-ray Burst Monitor (GBM) 15-25 keV X-ray data for each of these flares associated with a Fermi/GBM solar flare trigger, a total of 261 events. Using a model comparison method, we determine whether there is evidence for a substantial enhancement in the Fourier power spectrum that may be consistent with a QPP signature, based on three tested models; a power-law plus a constant, a broken power-law plus constant, and a power-law-plus-constant with an additional QPP signature component. From this, we determine that similar to 30% of GOES events and similar to 8% of Fermi/GBM events show strong signatures consistent with classical interpretations of QPP. For the remaining events either two or more tested models cannot be strongly distinguished from each other, or the events are well-described by single power-law or broken power-law Fourier power spectra. For both instruments, a preferred characteristic timescale of similar to 5-30 s was found in the QPP-like events, with no dependence on flare magnitude in either GOES or GBM data. We also show that individual events in the sample show similar characteristic timescales in both GBM and GOES data sets. We discuss the implications of these results for our understanding of solar flares and possible QPP mechanisms.
C1 [Inglis, A. R.; Ireland, J.; Dennis, B. R.] NASA, Solar Phys Lab, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Inglis, A. R.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Hayes, L.; Gallagher, P.] Trinity Coll Dublin, Dublin, Ireland.
[Ireland, J.] ADNET Syst Inc, Bethesda, MD USA.
RP Inglis, AR (reprint author), NASA, Solar Phys Lab, Heliophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Inglis, AR (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
OI Gallagher, Peter/0000-0001-9745-0400
NR 62
TC 1
Z9 1
U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 20
PY 2016
VL 833
IS 2
AR 284
DI 10.3847/1538-4357/833/2/284
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EG6PY
UT WOS:000391169600159
ER
PT J
AU Klingler, N
Rangelov, B
Kargaltsev, O
Pavlov, GG
Romani, RW
Posselt, B
Slane, P
Temim, T
Ng, CY
Bucciantini, N
Bykov, A
Swartz, DA
Buehler, R
AF Klingler, Noel
Rangelov, Blagoy
Kargaltsev, Oleg
Pavlov, George G.
Romani, Roger W.
Posselt, Bettina
Slane, Patrick
Temim, Tea
Ng, C. -Y.
Bucciantini, Niccolo
Bykov, Andrei
Swartz, Douglas A.
Buehler, Rolf
TI DEEP CHANDRA OBSERVATIONS OF THE PULSAR WIND NEBULA CREATED BY PSR
B0355+54
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: individual (PSR B0355+54); stars: neutron; X-rays: general
ID X-RAY OBSERVATIONS; SUPERNOVA REMNANT; IGR J11014-6103; CRAB-NEBULA;
EMISSION; SPECTROSCOPY; SIMULATIONS; DISCOVERY; BUBBLES; SHOCKS
AB We report on Chandra X-ray Observatory (CXO) observations of the pulsar wind nebula (PWN) associated with PSR B0355+54 (eight observations with a 395 ks total exposure, performed over an eight. month period). We investigated the spatial and spectral properties of the emission coincident with the pulsar, compact nebula (CN), and extended tail. We find that the CN morphology can be interpreted in a way that suggests a small angle between the pulsar spin axis and our line of sight, as inferred from the radio data. On larger scales, emission from the 7' (approximate to 2 pc) tail is clearly seen. We also found hints of two faint extensions nearly orthogonal to the direction of the pulsar's proper motion. The spectrum extracted at the pulsar position can be described with an absorbed power-law + blackbody model. The nonthermal component can be attributed to magnetospheric emission, while the thermal component can be attributed to emission from either a hot spot (e.g., a polar cap) or the entire neutron star surface. Surprisingly, the spectrum of the tail shows only a slight hint of cooling with increasing distance from the pulsar. This implies either a low magnetic field with fast flow speed, or particle reacceleration within the tail. We estimate physical properties of the PWN and compare the morphologies of the CN and the extended tail with those of other bow shock PWNe observed with long CXO exposures.
C1 [Klingler, Noel; Rangelov, Blagoy; Kargaltsev, Oleg] George Washington Univ, Dept Phys, 725 21st St NW, Washington, DC 20052 USA.
[Pavlov, George G.; Posselt, Bettina] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Romani, Roger W.] Stanford Univ, Dept Phys, 382 Via Pueblo, Stanford, CA 94305 USA.
[Slane, Patrick] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Temim, Tea] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA.
[Temim, Tea] Univ Maryland, CRESST, College Pk, MD 20742 USA.
[Ng, C. -Y.] Univ Hong Kong, Dept Phys, Pokfulam Rd, Hong Kong, Hong Kong, Peoples R China.
[Bucciantini, Niccolo] INAF Osservatorio Astrofis Arcetri, Lgo E Fermi 5, I-50125 Florence, Italy.
[Bucciantini, Niccolo] INFN Sez Firenze, Via G Sansone 1, I-150019 Sesto Fiorentino, Firenze, Italy.
[Bykov, Andrei] Ioffe Inst Phys & Technol, St Petersburg 194021, Russia.
[Bykov, Andrei] St Petersburg Polytech Univ, St Petersburg 195251, Russia.
[Bykov, Andrei] Int Space Sci Inst, Hallerstr 6, CH-3012 Bern, Switzerland.
[Swartz, Douglas A.] NASA, Marshall Space Flight Ctr, ZP12,320 Sparkman Dr, Huntsville, AL 35805 USA.
[Buehler, Rolf] DESY, Platanenallee 6, D-15738 Zeuthen, Germany.
RP Klingler, N (reprint author), George Washington Univ, Dept Phys, 725 21st St NW, Washington, DC 20052 USA.
RI Bykov, Andrei/E-3131-2014;
OI /0000-0002-5847-2612; Posselt, Bettina/0000-0003-2317-9747; Rangelov,
Blagoy/0000-0002-9282-5207; Buehler, Rolf/0000-0003-4425-6641; Temim,
Tea/0000-0001-7380-3144
FU National Aeronautics and Space Administration [G03-14082]; National
Aeronautics Space Administration [NAS8-03060]; NASA [NNX08AD71G]; RSF
grant [16-12-10225]
FX We would like to thank Martin Weisskopf, Maxim Lyutikov, Giovanni
Morlino, and Marina Romanova for the very helpful discussions. We are
also grateful to the anonymous referee for the helpful suggestions and a
careful reading of the paper. Support for this work was provided by the
National Aeronautics and Space Administration through Chandra Award
Number G03-14082 issued by the Chandra X-ray Observatory Center, which
is operated by the Smithsonian Astrophysical Observatory for and on
behalf of the National Aeronautics Space Administration under contract
NAS8-03060. The work was also partly supported by NASA grant NNX08AD71G.
A.M.B.. was supported by RSF grant 16-12-10225.
NR 46
TC 0
Z9 0
U1 2
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 20
PY 2016
VL 833
IS 2
AR 253
DI 10.3847/1538-4357/833/2/253
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EG6PY
UT WOS:000391169600128
ER
PT J
AU Larsson, J
Fransson, C
Spyromilio, J
Leibundgut, B
Challis, P
Chevalier, RA
France, K
Jerkstrand, A
Kirshner, RP
Lundqvist, P
Matsuura, M
McCray, R
Smith, N
Sollerman, J
Garnavich, P
Heng, K
Lawrence, S
Mattila, S
Migotto, K
Sonneborn, G
Taddia, F
Wheeler, JC
AF Larsson, J.
Fransson, C.
Spyromilio, J.
Leibundgut, B. .
Challis, P.
Chevalier, R. A.
France, K.
Jerkstrand, A.
Kirshner, R. P.
Lundqvist, P.
Matsuura, M.
McCray, R.
Smith, N.
Sollerman, J.
Garnavich, P.
Heng, K.
Lawrence, S.
Mattila, S.
Migotto, K.
Sonneborn, G.
Taddia, F.
Wheeler, J. C.
TI THREE-DIMENSIONAL DISTRIBUTION OF EJECTA IN SUPERNOVA 1987A AT 10,000
DAYS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE supernovae: general; supernovae: individual (SN 1987A)
ID CORE-COLLAPSE SUPERNOVAE; LATE SPECTRAL EVOLUTION;
HUBBLE-SPACE-TELESCOPE; SN 1987A; REVERSE SHOCK; LINE EMISSION;
CASSIOPEIA-A; ASYMMETRIC EXPLOSION; CIRCUMSTELLAR RING;
STRIPPED-ENVELOPE
AB Due to its proximity, SN. 1987A offers a unique opportunity to directly observe the geometry of a stellar explosion as it unfolds. Here we present spectral and imaging observations of SN. 1987A obtained similar to 10,000 days after the explosion with HST/STIS and VLT/SINFONI at optical and near-infrared wavelengths. These observations allow us to produce the most detailed 3D map of Ha to date, the first 3D maps for [Ca II] lambda lambda 7292, 7324, [O I] lambda lambda 6300, 6364, and Mg. II lambda lambda 9218, 9244, as well as new maps for [Si I]+[Fe II] 1.644 mu m and He I 2.058 mu m. A comparison with previous observations shows that the [Si I]+[Fe II] flux and morphology have not changed significantly during the past ten years, providing evidence that this line is powered by Ti-44. The time evolution of Ha shows that it is predominantly powered by X-rays from the ring, in agreement with previous findings. All lines that have sufficient signal show a similar large-scale 3D structure, with a north-south asymmetry that resembles a broken dipole. This structure correlates with early observations of asymmetries, showing that there is a global asymmetry that extends from the inner core to the outer envelope. On smaller scales, the two brightest lines, Ha and [Si I]+[Fe II] 1.644 mu m, show substructures at the level of similar to 200-1000 km s(-1) and clear differences in their 3D geometries. We discuss these results in the context of explosion models and the properties of dust in the ejecta.
C1 [Larsson, J.] AlbaNova, Dept Phys, KTH, SE-10691 Stockholm, Sweden.
[Larsson, J.] AlbaNova, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Fransson, C.; Lundqvist, P.; Sollerman, J.; Migotto, K.; Taddia, F.] Stockholm Univ, AlbaNova, Dept Astron, SE-10691 Stockholm, Sweden.
[Fransson, C.; Lundqvist, P.; Sollerman, J.; Migotto, K.; Taddia, F.] Stockholm Univ, AlbaNova, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Spyromilio, J.; Leibundgut, B. .] ESO, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Challis, P.; Kirshner, R. P.] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-78, Cambridge, MA 02138 USA.
[Chevalier, R. A.] Univ Virginia, Dept Astron, POB 400325, Charlottesville, VA 22904 USA.
[France, K.] Univ Colorado, Lab Atmospher & Space Phys, 392 UCB, Boulder, CO 80309 USA.
[France, K.] Univ Colorado, Ctr Astrophys & Space Astron, 389 UCB, Boulder, CO 80309 USA.
[Jerkstrand, A.] Queens Univ Belfast, Sch Maths & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Matsuura, M.] Cardiff Univ, Sch Phys & Astron, Queens Bldg, Cardiff CF24 3AA, S Glam, Wales.
[McCray, R.] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
[Smith, N.] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.
[Garnavich, P.] Univ Notre Dame, Nieuwland Sci, Notre Dame, IN 46556 USA.
[Heng, K.] Univ Bern, Ctr Space & Habitabil, Sidlerstr 5, CH-3012 Bern, Switzerland.
[Lawrence, S.] Hofstra Univ, Dept Phys & Astron, Hempstead, NY 11549 USA.
[Lawrence, S.] Univ Turku, Dept Phys & Astron, Tuorla Observ, Vislntie 20, FI-21500 Piikki, Finland.
[Lawrence, S.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Sonneborn, G.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab Code 665, Greenbelt, MD 20771 USA.
[Wheeler, J. C.] Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA.
RP Larsson, J (reprint author), AlbaNova, Dept Phys, KTH, SE-10691 Stockholm, Sweden.; Larsson, J (reprint author), AlbaNova, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
OI Fransson, Claes/0000-0001-8532-3594; Lundqvist,
Peter/0000-0002-3664-8082; /0000-0003-0065-2933; FRANCE,
KEVIN/0000-0002-1002-3674
FU Swedish National Space Board; NASA through grants from the Space
Telescope Science Institute [13401, 13405]; NASA [NAS5-26555]; European
Organization for Astronomical Research in the Southern Hemisphere, Chile
(ESO Program) [094.D-0505(C)]; Swedish Research Council
FX We are grateful to Hans-Thomas Janka and Michael Gabler for discussions
about their explosion models. This work was supported by the Swedish
National Space Board and Swedish Research Council. Support for HST GO
program numbers 13401 and 13405 was provided by NASA through grants from
the Space Telescope Science Institute, which is operated by the
Association of Universities for Research in Astronomy, Inc., under NASA
contract NAS5-26555. The ground-based observations were collected at the
European Organization for Astronomical Research in the Southern
Hemisphere, Chile (ESO Program 094.D-0505(C)).
NR 81
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 20
PY 2016
VL 833
IS 2
AR 147
DI 10.3847/1538-4357/833/2/147
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EG6PY
UT WOS:000391169600022
ER
PT J
AU Reisenfeld, DB
Bzowski, M
Funsten, HO
Fuselier, SA
Galli, A
Janzen, PH
Karna, N
Kubiak, MA
McComas, DJ
Schwadron, NA
Sokol, JM
AF Reisenfeld, D. B.
Bzowski, M.
Funsten, H. O.
Fuselier, S. A.
Galli, A.
Janzen, P. H.
Karna, N.
Kubiak, M. A.
McComas, D. J.
Schwadron, N. A.
Sokol, J. M.
TI TRACKING THE SOLAR CYCLE THROUGH IBEX OBSERVATIONS OF ENERGETIC NEUTRAL
ATOM FLUX VARIATIONS AT THE HELIOSPHERIC POLES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: general; magnetohydrodynamics (MHD); plasmas; solar wind; Sun:
heliosphere
ID INTERSTELLAR-BOUNDARY-EXPLORER; 1ST 5 YEARS; TERMINATION SHOCK; OUTER
HELIOSPHERE; MAGNETIC-FIELD; WIND; HELIOSHEATH; RIBBON; HYDROGEN;
SPECTRA
AB With seven years of Interstellar Boundary Explorer (IBEX) observations, from 2009 to 2015, we can now trace the time evolution of heliospheric energetic neutral atoms (ENAs) through over half a solar cycle. At the north and south ecliptic poles, the spacecraft attitude allows for continuous coverage of the ENA flux; thus, signal from these regions has much higher statistical accuracy and time resolution than anywhere else in the sky. By comparing the solar wind dynamic pressure measured at 1 au with the heliosheath plasma pressure derived from the observed ENA fluxes, we show that the heliosheath pressure measured at the poles correlates well with the solar cycle. The analysis requires time-shifting the ENA measurements to account for the travel time out and back from the heliosheath, which allows us to estimate the scale size of the heliosphere in the polar directions. We arrive at an estimated distance to the center of the ENA source region in the north of 220 au. and in the south. a distance of 190 au. We also find a good correlation between the solar cycle and the ENA energy spectra at the poles. In particular, the ENA flux for the highest IBEX energy channel (4.3 keV) is quite closely correlated with the areas of the polar coronal holes, in both the north and south, consistent with the notion that polar ENAs at this energy originate from pickup ions of the very high speed wind (similar to 700 km s(-1)) that emanates from polar coronal holes.
C1 [Reisenfeld, D. B.; Janzen, P. H.] Univ Montana, Missoula, MT 59812 USA.
[Bzowski, M.; Kubiak, M. A.; Sokol, J. M.] Polish Acad Sci CBK PAN, Space Res Ctr, Bartycka 18A, PL-00716 Warsaw, Poland.
[Funsten, H. O.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Fuselier, S. A.] Southwest Res Inst, San Antonio, TX 78228 USA.
[Fuselier, S. A.] Univ Texas San Antonio, San Antonio, TX 78228 USA.
[Galli, A.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland.
[Karna, N.] George Mason Univ, Fairfax, VA 22306 USA.
[Karna, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[McComas, D. J.] Princeton Univ, Peyton Hall, Princeton, NJ 08544 USA.
[Schwadron, N. A.] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA.
RP Reisenfeld, DB (reprint author), Univ Montana, Missoula, MT 59812 USA.
EM dan.reisenfeld@umontana.edu; bzowski@cbk.waw.pl; hfunsten@lanl.gov;
sfuselier@swri.edu; andre.galli@space.unibe.ch;
paul.janzen@umontana.edu; nkarna@masonlive.gmu.edu; mkubiak@cbk.waw.pl;
dmccomas@prineeton.edu; n.schwadron@unh.edu; jsokol@cbk.waw.pl
RI Sokol, Justyna/K-2892-2015;
OI Galli, Andre/0000-0003-2425-3793
FU NASA's Explorer Program; US Department of Energy; National Science
Center, Poland [2015-19-B-ST9-01328]; Schlumberger Foundation Faculty
for the Future Program
FX We give our sincere thanks to all of the outstanding professionals who
have made the IBEX mission a success. We would also like to thank Dr.
John Steinberg for productive conversations regarding the latitude
dependence of the ENA energy spectra, and the reviewer for very
substantive and thoughtful comments. This work was carried out as part
of NASA's IBEX Mission, with support from NASA's Explorer Program. Work
at Los Alamos was performed under the auspices of the US Department of
Energy. M.B., M.A.K. and J.M.S. acknowledge the support by the grant
2015-19-B-ST9-01328 from the National Science Center, Poland. N.K. is
supported by the Schlumberger Foundation Faculty for the Future Program.
NR 60
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U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 20
PY 2016
VL 833
IS 2
AR 277
DI 10.3847/1538-4357/833/2/277
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EG6PY
UT WOS:000391169600152
ER
PT J
AU Serra, P
Dore, O
Lagache, G
AF Serra, Paolo
Dore, Olivier
Lagache, Guilaine
TI DISSECTING THE HIGH-z INTERSTELLAR MEDIUM THROUGH INTENSITY MAPPING
CROSS-CORRELATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: ISM; infrared: diffuse background; large-scale structure of
universe
ID STAR-FORMING GALAXIES; C II EMISSION; INFRARED BACKGROUND ANISOTROPIES;
SINGLY IONIZED NITROGEN; NEUTRAL ATOMIC PHASES; GALACTIC PLANE SURVEY;
FINE-STRUCTURE LINES; DARK-MATTER HALOS; 158 MU-M; HIGH-REDSHIFT
AB We explore the detection, with upcoming spectroscopic surveys, of three-dimensional power spectra of emission line fluctuations produced in different phases of the interstellar medium (ISM) by forbidden transitions of ionized carbon [C II] (157.7 mu m), ionized nitrogen [N II] (121.9 and 205.2 mu m), and neutral oxygen [O I] (145.5 mu m) at redshift z > 4. These lines are important coolants of both the neutral and the ionized medium, and probe multiple phases of the ISM. In the framework of the halo model, we compute predictions of the three-dimensional power spectra for two different surveys, showing that they have the required sensitivity to detect cross-power spectra between the [C II] line and both the [O I] line and the [N II] lines with sufficient signal-to-noise ratio. The importance of cross-correlating multiple lines with the intensity mapping technique is twofold. On the one hand, we will have multiple probes of the different phases of the ISM, which is key to understanding the interplay between energetic sources, and the gas and dust at high redshift. This kind of study will be useful for a next-generation space observatory such as the NASA Far-IR Surveyor, which will probe the global star formation and the ISM of galaxies from the peak of star formation to the epoch of reionization. On the other hand, emission lines from external galaxies are an important foreground when measuring spectral distortions of the cosmic microwave background spectrum with future space-based experiments like PIXIE; measuring fluctuations in the intensity mapping regime will help constrain the mean amplitude of these lines, and will allow us to better handle this important foreground.
C1 [Serra, Paolo; Dore, Olivier] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Serra, Paolo; Dore, Olivier] CALTECH, Pasadena, CA 91125 USA.
[Lagache, Guilaine] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
RP Serra, P (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.; Serra, P (reprint author), CALTECH, Pasadena, CA 91125 USA.
EM Paolo.Serra@jpl.nasa.gov
FU "Programme National de Cosmologie and Galaxies" (PNCG) of CNRS/INSU,
France; OCEVU Labex [ANR-11-LABX-0060]; A*MIDEX project -
"Investissements d'Avenir" French government program
[ANR-11-IDEX-0001-02]
FX We thank Phil Bull, Tzu-Ching Chang, Abigail Crites, Roland de Putter
and Paul Goldsmith for insightful discussions, and the organizers of the
stimulating workshop "Opportunities and Challenges in Intensity Mapping"
in Stanford. We acknowledge financial support from "Programme National
de Cosmologie and Galaxies" (PNCG) of CNRS/INSU, France. P.S.
acknowledges hospitality from the Laboratoire d'Astrophysique de
Marseille, where part of this work was completed. Part of the research
described in this paper was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration. Part of this work has
been carried out thanks to the support of the OCEVU Labex
(ANR-11-LABX-0060) and the A*MIDEX project (ANR-11-IDEX-0001-02) funded
by the "Investissements d'Avenir" French government program managed by
the ANR.
NR 123
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 20
PY 2016
VL 833
IS 2
AR 153
DI 10.3847/1538-4357/833/2/153
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EG6PY
UT WOS:000391169600028
ER
PT J
AU Suzuki, D
Bennett, DP
Sumi, T
Bond, IA
Rogers, LA
Abe, F
Asakura, Y
Bhattacharya, A
Donachie, M
Freeman, M
Fukui, A
Hirao, Y
Itow, Y
Koshimoto, N
Li, MCA
Ling, CH
Masuda, K
Matsubara, Y
Muraki, Y
Nagakane, M
Onishi, K
Oyokawa, H
Rattenbury, N
Saito, T
Sharan, A
Shibai, H
Sullivan, DJ
Tristram, PJ
Yonehara, A
AF Suzuki, D.
Bennett, D. P.
Sumi, T.
Bond, I. A.
Rogers, L. A.
Abe, F.
Asakura, Y.
Bhattacharya, A.
Donachie, M.
Freeman, M.
Fukui, A.
Hirao, Y.
Itow, Y.
Koshimoto, N.
Li, M. C. A.
Ling, C. H.
Masuda, K.
Matsubara, Y.
Muraki, Y.
Nagakane, M.
Onishi, K.
Oyokawa, H.
Rattenbury, N.
Saito, To.
Sharan, A.
Shibai, H.
Sullivan, D. J.
Tristram, P. J.
Yonehara, A.
CA MOA Collaboration
TI THE EXOPLANET MASS-RATIO FUNCTION FROM THE MOA-II SURVEY: DISCOVERY OF A
BREAK AND LIKELY PEAK AT A NEPTUNE MASS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gravitational lensing: micro; planetary systems
ID MAGNIFICATION MICROLENSING EVENTS; SURFACE BRIGHTNESS RELATIONS; PARSEC
EVOLUTIONARY TRACKS; FREE-FLOATING PLANET; ORBITING M DWARFS; SOLAR-TYPE
STARS; M-CIRCLE-DOT; GALACTIC BULGE; EXTRASOLAR PLANETS; BROWN DWARF
AB We report the results of the statistical analysis of planetary signals discovered in MOA-II microlensing survey alert system events from 2007 to 2012. We determine the survey sensitivity as a function of planet-star mass ratio, q, and projected planet-star separation, s, in Einstein radius units. We find that the. mass-ratio function is not a single power. law, but has a change in slope at q similar to 10(-4), corresponding to similar to 20M(circle plus) for the median host-star mass of similar to 0.6 M-circle plus. We find significant planetary signals in 23 of the 1474 alert events that are well-characterized by the MOA-II survey data alone. Data from other groups are used only to characterize planetary signals that have been identified in the MOA data alone. The distribution of mass ratios and separations of the planets found in our sample are. well fit by a broken power-law model of the form dN(pl)/(dlog q d logs)= A(q/q(br))(p) s(m) dex(-2) for q > q(br) and dN(pl)/(dlog q d logs)= A(q/q(br))(n) s(m) dex(-2) for q < q(br), where q(br) is the mass ratio of the break. We also combine this analysis with the previous analyses of Gould et al. and Cassan et al., bringing the total sample to 30 planets. This combined analysis yields A =0.61(-0.16)(+0.21), n = -0.93 +/- 0.13, m = 0.49(-0.49)(+0.47), and p = 0.6(-0.4)(+0.5) for q(br) =1.7 x 10(-4). The unbroken power-law model is disfavored with a p-value of 0.0022, which corresponds to a Bayes factor of 27 favoring the broken power-law model. These results imply that cold Neptunes are likely to be the most common type of planets beyond the snow line.
C1 [Suzuki, D.; Bennett, D. P.; Bhattacharya, A.] NASA, Goddard Space Flight Ctr, Lab Exoplanets & Stellar Astrophys, Greenbelt, MD 20771 USA.
[Bennett, D. P.; Bhattacharya, A.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Sumi, T.; Hirao, Y.; Koshimoto, N.; Nagakane, M.; Shibai, H.] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, 1-1 Machikaneyama, Toyonaka, Osaka 5600043, Japan.
[Bond, I. A.; Ling, C. H.] Massey Univ, Inst Informat & Math Sci, North Shore Mail Ctr, Private Bag 102-904, Auckland, New Zealand.
[Rogers, L. A.] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
[Abe, F.; Asakura, Y.; Itow, Y.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Oyokawa, H.] Nagoya Univ, Inst Space Earth Environm Res, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648601, Japan.
[Donachie, M.; Freeman, M.; Li, M. C. A.; Rattenbury, N.; Sharan, A.] Univ Auckland, Dept Phys, Private Bag 92019, Auckland, New Zealand.
[Fukui, A.] Natl Astron Observ, Okayama Astrophys Observ, 3037-5 Honjo, Okayama 7190232, Japan.
[Onishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan.
[Saito, To.] Tokyo Metropolitan Coll Ind Technol, Tokyo 1168523, Japan.
[Sullivan, D. J.] Victoria Univ, Sch Chem & Phys Sci, Wellington, New Zealand.
[Tristram, P. J.] Mt John Univ Observ, POB 56, Lake Tekapo 8770, New Zealand.
[Yonehara, A.] Kyoto Sangyo Univ, Fac Sci, Dept Phys, Kyoto 6038555, Japan.
[Rogers, L. A.] Univ Calif Berkeley, Dept Earth & Planetary Sci, 501 Campbell Hall 3411, Berkeley, CA 94720 USA.
RP Suzuki, D (reprint author), NASA, Goddard Space Flight Ctr, Lab Exoplanets & Stellar Astrophys, Greenbelt, MD 20771 USA.
OI Rogers, Leslie/0000-0003-0638-3455
FU NASA [NNX13AF64G, NNX14AG49G, NNX15AJ76G]; JSPS [JSPS23103002,
JSPS24253004, JSPS26247023, JSPS25870893]; NASA through the Sagan
Fellowship Program; [JSPS25103508]; [23340064]
FX D.S. and D.P.B. acknowledge support from NASA grants NNX13AF64G,
NNX14AG49G, and NNX15AJ76G. T.S. acknowledges the financial support from
the JSPS, JSPS23103002, JSPS24253004, and JSPS26247023. D.S. was
supported by Grant-in-Aid for JSPS Fellows. A.Y. acknowleges the
financial support from the JSPS, JSPS25870893. The MOA project is
supported by the grant JSPS25103508 and 23340064. This work was
performed in part under contract with the California Institute of
Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA
through the Sagan Fellowship Program executed by the NASA Exoplanet
Science Institute. The authors thank OGLE, mu FUN, MiNDSTEp, PLNAET, and
RoboNet collaborations for letting us use their data to characterize the
alerted events.
NR 135
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 20
PY 2016
VL 833
IS 2
AR 145
DI 10.3847/1538-4357/833/2/145
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EG6PY
UT WOS:000391169600020
ER
PT J
AU Tinyanont, S
Kasliwal, MM
Fox, OD
Lau, R
Smith, N
Williams, R
Jencson, J
Perley, D
Dykhoff, D
Gehrz, R
Johansson, J
Van Dyk, SD
Masci, F
Cody, AM
Prince, T
AF Tinyanont, Samaporn
Kasliwal, Mansi M.
Fox, Ori D.
Lau, Ryan
Smith, Nathan
Williams, Robert
Jencson, Jacob
Perley, Daniel
Dykhoff, Devin
Gehrz, Robert
Johansson, Joel
Van Dyk, Schuyler D.
Masci, Frank
Cody, Ann Marie
Prince, Thomas
TI A SYSTEMATIC STUDY OF MID-INFRARED EMISSION FROM CORE-COLLAPSE
SUPERNOVAE WITH SPIRITS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE supernovae: general; supernovae: individual (SN 2011ja, SN 2014C, SN
2014bi)
ID SPITZER-SPACE-TELESCOPE; NEAR-INFRARED OBSERVATIONS; RICH CIRCUMSTELLAR
MEDIUM; MAJOR DUST FACTORIES; MASSIVE STARS; SN 2006JC; IIN SUPERNOVAE;
LIGHT CURVES; EVOLUTION; PROGENITOR
AB We present a systematic study of mid-infrared emission from 141 nearby supernovae (SNe). observed with Spitzer/IRAC as part of the ongoing SPIRITS survey. We detect 8 Type Ia and 36 core-collapse SNe. All Type. Ia/Ibc SNe. become undetectable within three. years of explosion, whereas 22 +/- 11% of Type. II SNe. continue to be detected. Five Type. II SNe are detected even two decades after discovery (SN 1974E, 1979C, 1980K, 1986J, and 1993J). Warm dust luminosity, temperature, and a lower limit on mass are obtained by fitting the two IRAC bands, assuming an optically thin dust shell. We derive warm dust masses between 10(-6) and 10(-2) M-circle dot and dust color temperatures between 200 and 1280 K. This observed warm dust could be pre-existing or newly created, but in either case represents a lower limit to the dust mass because cooler dust may be present. We present three case studies of extreme SNe.. SN 2011ja (II-P) was over-luminous ([4.5] = -15.6 mag) at 900 days post explosion with increasing hot dust mass, suggesting either an episode of dust formation or intensifying circumstellar material (CSM) interactions heating up pre-existing dust. SN 2014bi (II-P) showed a factor of 10 decrease in dust mass over one month, suggesting either dust destruction or reduced dust heating. The IR luminosity of SN 2014C (Ib) stayed. constant over 800 days, possibly due to strong CSM interaction with an. H-rich shell, which is rare among stripped-envelope SNe. The observations suggest that this CSM shell originated from an LBV-like eruption roughly 100 years pre-explosion. The observed diversity demonstrates the power of mid-IR observations of a large sample of SNe.
C1 [Tinyanont, Samaporn; Kasliwal, Mansi M.; Lau, Ryan; Jencson, Jacob; Prince, Thomas] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Fox, Ori D.; Williams, Robert] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Lau, Ryan] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Smith, Nathan] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Dykhoff, Devin] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark.
[Dykhoff, Devin; Gehrz, Robert] Univ Minnesota, Sch Phys & Astron, Minnesota Inst Astrophys, 116 Church St,SE, Minneapolis, MN 55455 USA.
[Johansson, Joel] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel.
[Van Dyk, Schuyler D.; Masci, Frank] CALTECH, Infrared Proc & Anal Ctr, M-S 100-22, Pasadena, CA 91125 USA.
[Cody, Ann Marie] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Tinyanont, S (reprint author), CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
EM st@astro.caltech.edu
FU NASA Spitzer mission grants [10136, 11063]; Royal Thai Scholarship;
NASA; United States Air Force
FX This work made use of observations from the Spitzer Space Telescope
operated by the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA. We acknowledge the use of some
data from PIDs 70207 (PI Helou); 80239 and 90178 (PI Andrews); 10139 (PI
Fox); and 10046 (PI Sanders). Ground-based observations presented were
obtained at the Palomar Observatory, operated by California Institute of
Technology. The Mount Lemmon Observing Facility is operated by the
University of Minnesota. The Nordic Optical Telescope is operated by the
Nordic Optical Telescope Scientific Association at the Observatorio del
Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica
de Canarias. We are grateful for support from the NASA Spitzer mission
grants to the SPIRITS program (PIDs 10136 & 11063). This research made
use of Astropy, a community-developed core Python package for Astronomy
Astropy Collaboration et al. (2013). We thank the anonymous referee for
comments and suggestions. S.T. thanks Bill Scanlon for a close read of
the manuscript. S.T. was supported by the Royal Thai Scholarship and a
portion of this work was done while under the Claremont-Carnegie
Astrophysics Research Program. R.D.G. was supported by NASA and the
United States Air Force.
NR 114
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 20
PY 2016
VL 833
IS 2
AR 231
DI 10.3847/1538-4357/833/2/231
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EG6PY
UT WOS:000391169600106
ER
PT J
AU Vican, L
Schneider, A
Bryden, G
Melis, C
Zuckerman, B
Rhee, J
Song, I
AF Vican, Laura
Schneider, Adam
Bryden, Geoff
Melis, Carl
Zuckerman, B.
Rhee, Joseph
Song, Inseok
TI HERSCHEL OBSERVATIONS OF DUSTY DEBRIS DISKS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; infrared: planetary systems
ID SPITZER-SPACE-TELESCOPE; A-TYPE STARS; TERRESTRIAL PLANET FORMATION;
MAIN-SEQUENCE STARS; SUN-LIKE STARS; WARM DUST; MOVING GROUP; HR 8799;
INFRARED SPECTROGRAPH; HIPPARCOS STARS
AB We present results from two Herschel observing programs using the Photodetector Array Camera and Spectrometer. During three separate campaigns, we obtained Herschel data for 24 stars at 70, 100, and 160 mu m. We chose stars that were already known or suspected to have circumstellar dust based on excess infrared (IR) emission previously measured with the InfraRed Astronomical Satellite (IRAS) or Spitzer and used Herschel to examine long-wavelength properties of the dust. Fifteen stars were found to be uncontaminated by background sources and possess IR emission most likely due to a circumstellar debris disk. We analyzed the properties of these debris disks to better understand the physical mechanisms responsible for dust production and removal. Seven targets were spatially resolved in the Herschel images. Based on fits to their spectral energy distributions, nine disks appear to have two temperature components. Of these nine, in three cases, the warmer dust component is likely the result of a transient process rather than a steady-state collisional cascade. The dust belts at four stars are likely stirred by an unseen planet and merit further investigation.
C1 [Vican, Laura; Zuckerman, B.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Schneider, Adam] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA.
[Bryden, Geoff] Caltech, JPL, Pasadena, CA 01109 USA.
[Melis, Carl] Univ Calif San Diego, Ctr Astrophys & Space Sci, San Diego, CA 92093 USA.
[Rhee, Joseph] Calif State Polytech Univ Pomona, 3801 West Temple Ave, Pomona, CA 91768 USA.
[Song, Inseok] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA.
RP Vican, L (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
OI Song, Inseok/0000-0002-5815-7372
FU NASA; NSF Graduate Research Fellowship
FX This research has made use of the Exoplanet Orbit Database, the
Exoplanet Data Explorer at exoplanets.org, the SIMBAD database, and
VizieR search engine, operated by CDS in France. Partial support for
this work was provided by a NASA grant to UCLA and by an NSF Graduate
Research Fellowship to Laura Vican.
NR 77
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U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 20
PY 2016
VL 833
IS 2
AR 263
DI 10.3847/1538-4357/833/2/263
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EG6PY
UT WOS:000391169600138
ER
PT J
AU Zoghbi, A
Miller, JM
King, AL
Miller, MC
Proga, D
Kallman, T
Fabian, AC
Harrison, FA
Kaastra, J
Raymond, J
Reynolds, CS
Boggs, SE
Christensen, FE
Craig, W
Hailey, CJ
Stern, D
Zhang, WW
AF Zoghbi, Abderahmen
Miller, J. M.
King, A. L.
Miller, M. C.
Proga, D.
Kallman, T.
Fabian, A. C.
Harrison, F. A.
Kaastra, J.
Raymond, J.
Reynolds, C. S.
Boggs, S. E.
Christensen, F. E.
Craig, W.
Hailey, C. J.
Stern, D.
Zhang, W. W.
TI DISK-WIND CONNECTION DURING THE HEARTBEATS OF GRS 1915+105
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; instabilities; X-rays: binaries; X-rays:
individual (GRS 1915+105)
ID DOMINATED ACCRETION DISKS; BLACK-HOLE SPIN; TIMING-EXPLORER
OBSERVATIONS; X-RAY BINARIES; RADIATION PRESSURE; UNIFIED MODEL;
REFLECTION; INSTABILITY; SPECTRA; MASS
AB Disk and wind signatures are seen in the soft state of Galactic black holes, while the jet is seen in the hard state. Here we study the disk-wind connection in the rho class of variability in GRS 1915+105 using a joint NuSTAR-Chandra observation. The source shows 50 s limit cycle oscillations. By including new information provided by the reflection spectrum. and using phase-resolved spectroscopy, we find that the change in the inner disk inferred from the blackbody emission is not matched by reflection measurements. The latter is almost constant, independent of the continuum model. The two radii are comparable only if the disk temperature color correction factor changes, an effect that could be due to the changing opacity of the disk caused by changes in metal abundances. The disk inclination is similar to that inferred from the jet axis, and oscillates by similar to 10 degrees. The simultaneous Chandra data show the presence of two wind components with velocities between 500 and 5000 km s(-1), and possibly two more with velocities reaching 20,000 km s(-1) (similar to 0.06 c). The column densities are similar to 5 x 10(22) cm(-2). An upper limit to the wind response time of 2 s is measured, implying a launch radius of < 6 x 10(10) cm. The changes in wind velocity and absorbed flux require the geometry of the wind to change during the oscillations, constraining the wind to be launched from a distance of 290-1300 r(g) from the black hole. Both data sets support fundamental model predictions in which a bulge originates in the inner disk and moves outward as the instability progresses.
C1 [Zoghbi, Abderahmen; Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[King, A. L.] Stanford Univ, KIPAC, 452 Lomita Mall, Stanford, CA 94305 USA.
[Miller, M. C.; Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Proga, D.] Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA.
[Kallman, T.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA.
[Fabian, A. C.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 OHA, England.
[Harrison, F. A.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA.
[Kaastra, J.] SRON, Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands.
[Kaastra, J.] Univ Utrecht, Dept Phys & Astron, POB 80000, NL-3508 TA Utrecht, Netherlands.
[Raymond, J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Boggs, S. E.; Craig, W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, Elektrovej 327, DK-2800 Lyngby, Denmark.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Zoghbi, A (reprint author), Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
EM abzoghbi@umich.edu
FU National Aeronautics and Space Administration
FX This work made use of data from the NuSTAR mission, a project led by the
California Institute of Technology, managed by the Jet Propulsion
Laboratory, and funded by the National Aeronautics and Space
Administration. This work is also based on observations made by the
Chandra X-ray Observatory.
NR 65
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U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 20
PY 2016
VL 833
IS 2
AR 165
DI 10.3847/1538-4357/833/2/165
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EG6PY
UT WOS:000391169600040
ER
PT J
AU Aguilera-Gomez, C
Chaname, J
Pinsonneault, MH
Carlberg, JK
AF Aguilera-Gomez, Claudia
Chaname, Julio
Pinsonneault, Marc H.
Carlberg, Joleen K.
TI ON LITHIUM-RICH RED GIANTS: ENGULFMENT ON THE GIANT BRANCH OF TRUMPLER
20
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE open clusters and associations: individual (Trumpler 20); planet-star
interactions; stars: abundances; stars: chemically peculiar
ID OPEN CLUSTER; LI; STARS; COMPANIONS; DEPLETION; STELLAR; I.
AB The Gaia-ESO survey recently reported on a large sample of lithium (Li) abundance determinations for evolved stars in the rich open cluster Trumpler 20. They argue for a scenario where virtually all stars experience post-main-sequence mixing and Li is preserved in only two objects. We present an alternate explanation, where Li is normal in the vast majority of cluster stars and anomalously high in these two cases. We demonstrate that the Li upper limits in the red giants can be explained with a combination of mainsequence depletion and standard dredge-up and that they are close to the detected levels in other systems of similar age. In our framework, two of the detected giants are anomalously Li-rich, and we propose that both could have been produced by the engulfment of a substellar mass companion of 16(-10)(+6) M-J. This would imply that similar to 5% of 1.8 M-circle dot stars in this system, and by extension elsewhere, should have substellar mass companions of high mass that could be engulfed at some point in their lifetimes. We discuss future tests that could confirm or refute this scenario.
C1 [Aguilera-Gomez, Claudia; Chaname, Julio] Pontificia Univ Catolica Chile, Inst Astrofis, Ave Vicuna Mackenna 4860, Santiago 7820436, Chile.
[Aguilera-Gomez, Claudia; Chaname, Julio] Millennium Inst Astrophys, Santiago, Chile.
[Pinsonneault, Marc H.] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA.
[Pinsonneault, Marc H.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Carlberg, Joleen K.] NASA, Goddard Space Flight Ctr, Code 667, Greenbelt, MD 20771 USA.
RP Aguilera-Gomez, C (reprint author), Pontificia Univ Catolica Chile, Inst Astrofis, Ave Vicuna Mackenna 4860, Santiago 7820436, Chile.; Aguilera-Gomez, C (reprint author), Millennium Inst Astrophys, Santiago, Chile.
FU CONICYT-PCHA Doctorado Nacional [2013-21130353]; Chilean Ministry for
the Economy, Development, and Tourism's Programa Iniciativa Cientifica
Milenio [IC120009]; Centro de Astronomia y Tecnologias Afines [PFB-06];
NASA [NNX15AF13G]
FX We thank the anonymous referee for a very useful report that helped
improve the quality of the science presented in this work. We thank Luca
Sbordone for helpful discussion, Jamie Tayar and Joel Zinn for guidance
on horizontal branch models, and Elisa Delgado-Mena for comments to
improve Figure 2 and its interpretation. Support for C.A.-G. is provided
by CONICYT-PCHA Doctorado Nacional 2013-21130353. C.A.-G. and J.C.
acknowledge support from the Chilean Ministry for the Economy,
Development, and Tourism's Programa Iniciativa Cientifica Milenio,
through grant IC120009 awarded to the Millenium Institute of
Astrophysics (MAS) and from PFB-06 Centro de Astronomia y Tecnologias
Afines. M.H.P. acknowledges support from NASA grant NNX15AF13G. J.K.C.
was supported by an appointment to the NASA Postdoctoral Program at the
Goddard Space Flight Center, administered by Universities Space Research
Association under contract with NASA.
NR 28
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U1 3
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD DEC 20
PY 2016
VL 833
IS 2
AR L24
DI 10.3847/2041-8213/833/2/L24
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EG8IM
UT WOS:000391300100001
ER
PT J
AU Koppelmans, V
Bloomberg, JJ
Mulavara, AP
Seidler, RD
AF Koppelmans, Vincent
Bloomberg, Jacob J.
Mulavara, Ajitkumar P.
Seidler, Rachael D.
TI Brain structural plasticity with spaceflight
SO NPJ MICROGRAVITY
LA English
DT Article
ID NORMAL-PRESSURE HYDROCEPHALUS; VOXEL-BASED MORPHOMETRY; HEAD-DOWN TILT;
BED REST; SENSORIMOTOR PERFORMANCE; SPACE MISSION; MOTOR CORTEX;
ADAPTATION; WEIGHTLESSNESS; DIAGNOSIS
AB Humans undergo extensive sensorimotor adaptation during spaceflight due to altered vestibular inputs and body unloading. No studies have yet evaluated the effects of spaceflight on human brain structure despite the fact that recently reported optic nerve structural changes are hypothesized to occur due to increased intracranial pressure occurring with microgravity. This is the first report on human brain structural changes with spaceflight. We evaluated retrospective longitudinal T2-weighted MRI scans and balance data from 27 astronauts (thirteen similar to 2-week shuttle crew members and fourteen similar to 6-month International Space Station crew members) to determine spaceflight effects on brain structure, and whether any pre to postflight brain changes are associated with balance changes. Data were obtained from the NASA Lifetime Surveillance of Astronaut Health. Brain scans were segmented into gray matter maps and normalized into MNI space using a stepwise approach through subject specific templates. Non-parametric permutation testing was used to analyze pre to postflight volumetric gray matter changes. We found extensive volumetric gray matter decreases, including large areas covering the temporal and frontal poles and around the orbits. This effect was larger in International Space Station versus shuttle crew members in some regions. There were bilateral focal gray matter increases within the medial primary somatosensory and motor cortex; i.e., the cerebral areas where the lower limbs are represented. These intriguing findings are observed in a retrospective data set; future prospective studies should probe the underlying mechanisms and behavioral consequences.
C1 [Koppelmans, Vincent; Seidler, Rachael D.] Univ Michigan, Sch Kinesiol, 401 Washtenaw Ave, Ann Arbor, MI 48109 USA.
[Bloomberg, Jacob J.] NASA Johnson Space Ctr, Houston, TX 77058 USA.
[Mulavara, Ajitkumar P.] KBRwyle, Houston, TX 77058 USA.
[Seidler, Rachael D.] Univ Michigan, Dept Psychol, 580 Union Dr, Ann Arbor, MI 48109 USA.
RP Seidler, RD (reprint author), Univ Michigan, Sch Kinesiol, 401 Washtenaw Ave, Ann Arbor, MI 48109 USA.; Seidler, RD (reprint author), Univ Michigan, Dept Psychol, 580 Union Dr, Ann Arbor, MI 48109 USA.
EM rseidler@umich.edu
FU National Aeronautics and Space Administration (NASA) [NNX11AR02G]
FX This work was supported by a grant from the National Aeronautics and
Space Administration (NASA; NNX11AR02G). We thank NASA Lifetime
Surveillance of Astronaut Health for providing these data and all
astronauts who volunteered their time.
NR 58
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U1 1
U2 1
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 2373-8065
J9 NPJ MICROGRAVITY
JI NPJ Microgravity
PD DEC 19
PY 2016
VL 2
AR 2
DI 10.1038/s41526-016-0001-9
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EH2XG
UT WOS:000391631400001
ER
PT J
AU Haskins, JB
Thompson, AE
Lawson, JW
AF Haskins, Justin B.
Thompson, Alexander E.
Lawson, John W.
TI Ab initio simulations of phase stability and martensitic transitions in
NiTi
SO PHYSICAL REVIEW B
LA English
DT Article
ID TOTAL-ENERGY CALCULATIONS; AUGMENTED-WAVE METHOD; SHAPE-MEMORY ALLOYS;
MOLECULAR-DYNAMICS; B19' STRUCTURE; BASIS-SET; METALS; TINI
AB For NiTi-based alloys, the shape memory effect is governed by a transition from a low-temperature martensite phase to a high-temperature austenite phase. Despite considerable experimental and computational work, basic questions regarding the stability of the phases and the martensitic phase transition remain unclear even for the simple case of binary, equiatomic NiTi. We perform ab initio molecular dynamics simulations to describe the temperature-dependent behavior of NiTi and resolve several of these outstanding issues. Structural correlation functions and finite temperature phonon spectra are evaluated to determine phase stability. We show that finite temperature, entropic effects stabilize the experimentally observed martensite (B19') and austenite (B2) phases while destabilizing the theoretically predicted (B33) phase. Free energy computations based on ab initio thermodynamic integration confirm these results and permit estimates of the transition temperature between the phases. In addition to the martensitic phase transition, we predict a new transition between the B33 and B19' phases. The role of defects in suppressing phase transformation temperatures is discussed.
C1 [Haskins, Justin B.] NASA, Ames Res Ctr, AMA Inc, Thermal Protect Mat Branch, Moffett Field, CA 94035 USA.
[Thompson, Alexander E.] NASA, Ames Res Ctr, USRA, Thermal Protect Mat Branch, Moffett Field, CA 94035 USA.
[Lawson, John W.] NASA, Ames Res Ctr, Thermal Protect Mat Branch, Moffett Field, CA 94035 USA.
RP Lawson, JW (reprint author), NASA, Ames Res Ctr, Thermal Protect Mat Branch, Moffett Field, CA 94035 USA.
EM john.w.lawson@nasa.gov
FU NASA Aeronautics Research Mission Directorate's Transformational Tools &
Technologies (TTT) project
FX This work was supported by funding from the NASA Aeronautics Research
Mission Directorate's Transformational Tools & Technologies (TTT)
project. We benefited from discussions with Charles Bauschlicher, Ronald
Noebe, and Othmane Benafan. J. B. Haskins and A. E. Thompson contributed
equally to this work.
NR 46
TC 0
Z9 0
U1 9
U2 9
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-9950
EI 2469-9969
J9 PHYS REV B
JI Phys. Rev. B
PD DEC 19
PY 2016
VL 94
IS 21
AR 214110
DI 10.1103/PhysRevB.94.214110
PG 10
WC Physics, Condensed Matter
SC Physics
GA EF3TM
UT WOS:000390247300001
ER
PT J
AU Hoffman, MJ
Andrews, LC
Price, SA
Catania, GA
Neumann, TA
Luthi, MP
Gulley, J
Ryser, C
Hawley, RL
Morriss, B
AF Hoffman, Matthew J.
Andrews, Lauren C.
Price, Stephen A.
Catania, Ginny A.
Neumann, Thomas A.
Luthi, Martin P.
Gulley, Jason
Ryser, Claudia
Hawley, Robert L.
Morriss, Blaine
TI Greenland subglacial drainage evolution regulated by weakly connected
regions of the bed
SO NATURE COMMUNICATIONS
LA English
DT Article
ID SUPRAGLACIAL LAKE DRAINAGE; HAUT GLACIER DAROLLA; ICE-SHEET;
WATER-PRESSURE; SURFACE MELT; SOUTHWEST GREENLAND; SEASONAL-CHANGES;
WEST GREENLAND; SYSTEM; VELOCITY
AB Penetration of surface meltwater to the bed of the Greenland Ice Sheet each summer causes an initial increase in ice speed due to elevated basal water pressure, followed by slowdown in late summer that continues into fall and winter. While this seasonal pattern is commonly explained by an evolution of the subglacial drainage system from an inefficient distributed to efficient channelized configuration, mounting evidence indicates that subglacial channels are unable to explain important aspects of hydrodynamic coupling in late summer and fall. Here we use numerical models of subglacial drainage and ice flow to show that limited, gradual leakage of water and lowering of water pressure in weakly connected regions of the bed can explain the dominant features in late and post melt season ice dynamics. These results suggest that a third weakly connected drainage component should be included in the conceptual model of subglacial hydrology.
C1 [Hoffman, Matthew J.; Price, Stephen A.] Los Alamos Natl Lab, Fluid Dynam & Solid Mech Grp, Los Alamos, NM 87545 USA.
[Andrews, Lauren C.; Neumann, Thomas A.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD 20771 USA.
[Catania, Ginny A.] Univ Texas Austin, Jackson Sch Geosci, Inst Geophys, Austin, TX 78758 USA.
[Catania, Ginny A.] Univ Texas Austin, Dept Geol Sci, Jackson Sch Geosci, Austin, TX 78758 USA.
[Luthi, Martin P.] Univ Zurich, Glaciol & Geomorphodynam Grp, Dept Geog, CH-8057 Zurich, Switzerland.
[Gulley, Jason] Univ S Florida, Sch Geosci, Tampa, FL 33620 USA.
[Ryser, Claudia] Swiss Fed Inst Technol, Lab Hydraul Hydrol & Glaciol, CH-8093 Zurich, Switzerland.
[Hawley, Robert L.] Dartmouth Coll, Dept Earth Sci, Hanover, NH 03755 USA.
[Morriss, Blaine] Cold Reg Res & Engn Lab, Hanover, NH 03755 USA.
RP Hoffman, MJ (reprint author), Los Alamos Natl Lab, Fluid Dynam & Solid Mech Grp, Los Alamos, NM 87545 USA.
EM mhoffman@lanl.gov
RI Neumann, Thomas/D-5264-2012; Catania, Ginny/B-9787-2008; Andrews,
Lauren/D-8274-2017
OI Andrews, Lauren/0000-0003-3727-4737
FU Laboratory Directed Research and Development Early Career Research
Program (LDRD-ECR) at Los Alamos National Laboratory, Climate Modeling
Programs within the U.S. Department of Energy Office of Science;
National Science Foundation [ANT-0424589]; National Science Foundation
Division of Earth Sciences (EAR) Postdoctoral Fellowship [0946767];
United States National Science Foundation [OPP-0908156, OPP-0909454];
Swiss National Science Foundation [200021_127197]; National Geographic
Society [9067-12]; NASA Cryospheric Sciences
FX This work was supported by a grant to M.J.H. from the Laboratory
Directed Research and Development Early Career Research Program
(LDRD-ECR) at Los Alamos National Laboratory, Climate Modeling Programs
within the U.S. Department of Energy Office of Science, and by the
National Science Foundation, under grant ANT-0424589 to the Center for
Remote Sensing of Ice Sheets (CReSIS). L.C.A. was supported by an
appointment to the NASA Postdoctoral Program at the Goddard Space Flight
Center, administered by Universities Space Research Association under
contract with NASA, and UTIG Ewing-Worzel and Gale White Graduate
Student Fellowships. J.G. was supported by National Science Foundation
Division of Earth Sciences (EAR) Postdoctoral Fellowship (No. 0946767).
Fieldwork resulting in the presented observations was supported by
United States National Science Foundation grants OPP-0908156 and
OPP-0909454, Swiss National Science Foundation grant 200021_127197,
National Geographic Society grant 9067-12 and NASA Cryospheric Sciences.
NR 65
TC 1
Z9 1
U1 19
U2 19
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2041-1723
J9 NAT COMMUN
JI Nat. Commun.
PD DEC 19
PY 2016
VL 7
AR 13903
DI 10.1038/ncomms13903
PG 11
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EE8NJ
UT WOS:000389882400001
PM 27991518
ER
PT J
AU Porter, SE
Parkinson, CL
Mosley-Thompson, E
AF Porter, Stacy E.
Parkinson, Claire L.
Mosley-Thompson, Ellen
TI Bellingshausen Sea ice extent recorded in an Antarctic Peninsula ice
core
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SOUTHERN ANNULAR MODE; CLIMATE-CHANGE; OSCILLATION INDEX; WEST
ANTARCTICA; EXTRATROPICAL CIRCULATION; ACCUMULATION VARIABILITY; ENSO
TELECONNECTION; HEMISPHERE CLIMATE; OCEAN; 20TH-CENTURY
AB Annual net accumulation (A(n)) from the Bruce Plateau (BP) ice core retrieved from the Antarctic Peninsula exhibits a notable relationship with sea ice extent (SIE) in the Bellingshausen Sea. Over the satellite era, both BP A(n) and Bellingshausen SIE are influenced by large-scale climatic factors such as the Amundsen Sea Low, Southern Annular Mode, and Southern Oscillation. In addition to the direct response of BP A(n) to Bellingshausen SIE (e.g., more open water as a moisture source), these large-scale climate phenomena also link the BP and the Bellingshausen Sea indirectly such that they exhibit similar responses (e.g., northerly wind anomalies advect warm, moist air to the Antarctic Peninsula and neighboring Bellingshausen Sea, which reduces SIE and increases A(n)). Comparison with a time series of fast ice at South Orkney Islands reveals a relationship between BP A(n) and sea ice in the northern Weddell Sea that is relatively consistent over the twentieth century, except when it is modulated by atmospheric wave patterns described by the Trans-Polar Index. The trend of increasing accumulation on the Bruce Plateau since similar to 1970 agrees with other climate records and reconstructions in the region and suggests that the current rate of sea ice loss in the Bellingshausen Sea is unrivaled in the twentieth century.
C1 [Porter, Stacy E.; Mosley-Thompson, Ellen] Ohio State Univ, Byrd Polar & Climate Res Ctr, Columbus, OH 43210 USA.
[Parkinson, Claire L.] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Greenbelt, MD USA.
[Mosley-Thompson, Ellen] Ohio State Univ, Dept Geog, Atmospher Sci Program, Columbus, OH 43210 USA.
RP Porter, SE (reprint author), Ohio State Univ, Byrd Polar & Climate Res Ctr, Columbus, OH 43210 USA.
EM porter.573@osu.edu
FU NSF [ANT-0732655]; NASA Earth Science Division
FX The Bruce Plateau field project, laboratory analyses, and partial
support for S.E.P. and E.M.T. were provided by NSF award ANT-0732655 to
Ellen Mosley-Thompson as part of NSF's IPY LARISSA Project. Support for
C.L.P. was provided through the NASA Earth Science Division. We thank
Aaron Wilson for valuable and insightful discussions and three anonymous
reviewers for their thoughtful and constructive reviews. The ice core
data used in this study are archived at NOAA's National Climatic Data
Center/Paleoclimatology
(https://www.ncdc.noaa.gov/cdo/f?p=519:1:0::::P1_STUDY_ID:20350). This
is Byrd Polar and Climate Research Center contribution 1549.
NR 78
TC 0
Z9 0
U1 2
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD DEC 16
PY 2016
VL 121
IS 23
BP 13886
EP 13900
DI 10.1002/2016JD025626
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EL3LJ
UT WOS:000394520300004
ER
PT J
AU Martins, DK
Najjar, RG
Tzortziou, M
Abuhassan, N
Thompson, AM
Kollonige, DE
AF Martins, Douglas K.
Najjar, Raymond G.
Tzortziou, Maria
Abuhassan, Nader
Thompson, Anne M.
Kollonige, Debra E.
TI Spatial and temporal variability of ground and satellite column
measurements of NO2 and O-3 over the Atlantic Ocean during the
Deposition of Atmospheric Nitrogen to Coastal Ecosystems Experiment
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID TROPOSPHERIC NO2; OMI; RETRIEVALS
AB In situ measurements of O-3 and nitrogen oxides (NO + NO2 = NOx) and remote sensing measurements of total column NO2 and O-3 were collected on a ship in the North Atlantic Ocean as part of the Deposition of Atmospheric Nitrogen to Coastal Ecosystems (DANCE) campaign in July- August 2014, similar to 100 km east of the mid-Atlantic United States. Relatively clean conditions for both surface in situ mixing ratio and total column O-3 and NO2 measurements were observed throughout the campaign. Increased surface and column NO2 and O-3 amounts were observed when a terrestrial air mass was advected over the study region. Relative to ship-based total column measurements using a Pandora over the entire study, satellite measurements overestimated total column NO2 under these relatively clean atmospheric conditions over offshore waters by an average of 16%. Differences are most likely due to proximity, or lack thereof, to surface emissions; spatial averaging due to the field of view of the satellite instrument; and the lack of sensitivity of satellite measurements to the surface concentrations of pollutants. Total column O-3 measurements from the shipboard Pandora showed good correlation with the satellite measurements (r = 0.96), but satellite measurements were 3% systematically higher than the ship measurements, in agreement with previous studies. Derived values of boundary layer height using the surface in situ and total column measurements of NO2 are much lower than modeled and satellite-retrieved boundary layer heights, which highlight the differences in the vertical distribution between terrestrial and marine environments.
C1 [Martins, Douglas K.; Najjar, Raymond G.] Penn State Univ, Dept Meteorol & Atmospher Sci, University Pk, PA 16802 USA.
[Martins, Douglas K.] FLIR Detect Inc, W Lafayette, IN 47906 USA.
[Tzortziou, Maria] CUNY, Dept Earth & Atmospher Sci, New York, NY 10021 USA.
[Abuhassan, Nader; Thompson, Anne M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Abuhassan, Nader] Univ Maryland, Joint Ctr Earth Sci Technol, Baltimore, MD 21201 USA.
[Kollonige, Debra E.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
RP Martins, DK (reprint author), Penn State Univ, Dept Meteorol & Atmospher Sci, University Pk, PA 16802 USA.; Martins, DK (reprint author), FLIR Detect Inc, W Lafayette, IN 47906 USA.
EM douglas.martins@flir.com; rgn1@psu.edu
RI Thompson, Anne /C-3649-2014
OI Thompson, Anne /0000-0002-7829-0920
FU National Science Foundation Division of Ocean Sciences [1260574]; NASA's
DISCOVER-AQ [NNX10AR39G]; AQAST [NNXAQ44G]; NASA's Pandora work
[NNX13AL86G]
FX This work was funded by the National Science Foundation Division of
Ocean Sciences (1260574), NASA's DISCOVER-AQ (NNX10AR39G), AQAST
(NNXAQ44G), and NASA's Pandora work (NNX13AL86G). We thank the captain
and the crew of the R/V Hugh R. Sharp. We thank James Szykman and
Winston Luke for their collaborations. The authors gratefully
acknowledge the NOAA Air Resources Laboratory (ARL) for the provision of
the HYSPLIT transport and dispersion model and/or READY website
(http://www.ready.noaa.gov) used in this publication. For data access,
please contact the project Principal Investigator Raymond Najjar,
rgn1@psu.edu.
NR 26
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U1 4
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD DEC 16
PY 2016
VL 121
IS 23
BP 14175
EP 14187
DI 10.1002/2016JD024998
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EL3LJ
UT WOS:000394520300023
ER
PT J
AU Loughner, CP
Tzortziou, M
Shroder, S
Pickering, KE
AF Loughner, Christopher P.
Tzortziou, Maria
Shroder, Shulamit
Pickering, Kenneth E.
TI Enhanced dry deposition of nitrogen pollution near coastlines: A case
study covering the Chesapeake Bay estuary and Atlantic Ocean coastline
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID UNITED-STATES; DISCOVER-AQ; AIR-QUALITY; ATMOSPHERIC DEPOSITION; IMPACT;
OZONE; BREEZE; CMAQ; TRANSFORMATION; POLLUTANTS
AB Atmospheric deposition of nitrogen pollution is one of the major sources of nitrogen to many terrestrial and aquatic ecosystems, worldwide. This modeling study suggests that coastlines frequently experience disproportionally high dry deposition of reactive nitrogen. High concentrations of air pollution from coastal cities often accumulate over adjacent estuaries and coastal waters due to low dry deposition rates over the water and a shallow marine boundary layer trapping marine emissions. As high concentrations of pollutants over the water are transported inland, enhanced dry deposition occurs onshore along the coastlines. Large spatial gradients in air pollutants and deposition totals are simulated along the coastline with decreasing concentrations/deposition as the distance from the water increases. As pollutants are transported onshore, air pollution mixing ratios near the surface decrease due to removal by dry deposition, vertical dilution due to deeper mixing layer heights, and decrease in friction velocity as a function of distance inland from the coastline. Ammonium nitrate formation near agricultural ammonia sources, sodium nitrate formation near coastal areas with atmospheric sea-salt loadings, and particulate growth via water uptake also contribute to large nitrate dry deposition totals at the coastline. Gradients in dry N deposition are evident over a monthly time scale and are enhanced during sea and bay breeze events. Current existing N-deposition monitoring networks do not capture the large spatial gradients of ammonium, nitrate, and nitric acid concentrations near coastlines predicted by the model due to the coarse spatial density distribution of monitoring sites.
C1 [Loughner, Christopher P.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Loughner, Christopher P.; Tzortziou, Maria; Pickering, Kenneth E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Tzortziou, Maria] CUNY, Dept Earth & Atmospher Sci, New York, NY 10021 USA.
[Shroder, Shulamit] Univ Maryland, Environm Sci & Policy Program, College Pk, MD 20742 USA.
RP Loughner, CP (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.; Loughner, CP (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM christopher.p.loughner@nasa.gov
OI Loughner, Christopher/0000-0002-3833-2014
FU NASA [NNX12AD03A, NNX10AQ79G, NNX11AP07G]
FX This work was supported under the NASA Earth Venture-1 DISCOVER-AQ
project (NASA Grant Reference NNX12AD03A) and NASA grants NNX10AQ79G and
NNX11AP07G. CASTNET data can be downloaded via www.epa.gov/castnet.
CASTNET data are available at https://www.epa.gov/castnet, and
DISCOVER-AQ data are available at
http://www-air.larc.nasa.gov/missions/discover-aq/discover-aq.html. The
WRF model is available at http://www.wrf-model.org, and the CMAQ model
is available at https://www.cmascenter.org/cmaq. Model inputs and
outputs are available free of charge by contacting Chris Loughner
(christopher.p.loughner@nasa.gov).
NR 66
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U2 14
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD DEC 16
PY 2016
VL 121
IS 23
BP 14221
EP 14238
DI 10.1002/2016JD025571
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EL3LJ
UT WOS:000394520300026
ER
PT J
AU Mlynczak, MG
Hunt, LA
Russell, JM
Marshall, BT
Mertens, CJ
Thompson, RE
AF Mlynczak, Martin G.
Hunt, Linda A.
Russell, James M., III
Marshall, B. Thomas
Mertens, Christopher J.
Thompson, R. Earl
TI The global infrared energy budget of the thermosphere from 1947 to 2016
and implications for solar variability
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE thermosphere; energy budget; infrared; climate; solar variability
ID SABER EXPERIMENT; CYCLE
AB We present an empirical model of the global infrared energy budget of the thermosphere over the past 70years. The F-10.7, Ap, and Dst indices are used in linear regression fits to the 14.5year time series of radiative cooling by carbon dioxide and nitric oxide measured by the Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) instrument on the TIMED satellite. Databases of these indices are used to develop the radiative cooling time series from 1947. No consistent relation between the occurrence of peak sunspot number and peak infrared cooling is found over the past six solar cycles. The total infrared energy radiated by the thermosphere, integrated over a solar cycle, is nearly constant over five complete solar cycles studied. This is a direct consequence of the geoeffective solar energy also being nearly constant over the same intervals. These results provide a new metric for assessing the terrestrial context of the long-term record of solar-related indices.
C1 [Mlynczak, Martin G.; Mertens, Christopher J.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Hunt, Linda A.] Sci Syst & Applicat Inc, Hampton, VA USA.
[Russell, James M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA.
[Marshall, B. Thomas; Thompson, R. Earl] GATS Inc, Newport News, VA USA.
RP Mlynczak, MG (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
EM m.g.mlynczak@nasa.gov
OI Hunt, Linda/0000-0002-5330-541X
FU NASA TIMED project
FX The Ap and F10.7 data are from the geomagnetic and solar
databases at the NOAA Space Weather Prediction Center. The Dst data are
from the University of Oulu, Finland, . The daily sunspot data are from
the World Data Center for Sunspot Index and Long-term Solar Observations
at Royal Observatory of Belgium, Brussels. The NO and CO2
power data are available from the first author of this article. The
authors acknowledge support from the NASA TIMED project.
NR 16
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U1 3
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD DEC 16
PY 2016
VL 43
IS 23
BP 11934
EP 11940
DI 10.1002/2016GL070965
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA EI5DU
UT WOS:000392515000002
ER
PT J
AU Zhao, C
Russell, CT
Strangeway, RJ
Petrinec, SM
Paterson, WR
Zhou, M
Anderson, BJ
Baumjohann, W
Bromund, KR
Chutter, M
Fischer, D
Le, G
Nakamura, R
Plaschke, F
Slavin, JA
Torbert, RB
Wei, HY
AF Zhao, C.
Russell, C. T.
Strangeway, R. J.
Petrinec, S. M.
Paterson, W. R.
Zhou, M.
Anderson, B. J.
Baumjohann, W.
Bromund, K. R.
Chutter, M.
Fischer, D.
Le, G.
Nakamura, R.
Plaschke, F.
Slavin, J. A.
Torbert, R. B.
Wei, H. Y.
TI Force balance at the magnetopause determined with MMS: Application to
flux transfer events
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE flux transfer events; force free; pressure balance; MMS
ID MAGNETOSPHERIC MULTISCALE; DAYSIDE MAGNETOPAUSE; VENUS
AB The Magnetospheric Multiscale mission (MMS) consists of four identical spacecraft forming a closely separated (10km) and nearly regular tetrahedron. This configuration enables the decoupling of spatial and temporal variations and allows the calculation of the spatial gradients of plasma and electromagnetic field quantities. We make full use of the well cross-calibrated MMS magnetometers and fast plasma instruments measurements to calculate both the magnetic and plasma forces in flux transfer events (FTEs) and evaluate the relative contributions of different forces to the magnetopause momentum variation. This analysis demonstrates that some but not all FTEs, consistent with previous studies, are indeed force-free structures in which the magnetic pressure force balances the magnetic curvature force. Furthermore, we contrast these events with FTE events that have non-force-free signatures.
C1 [Zhao, C.; Russell, C. T.; Strangeway, R. J.; Wei, H. Y.] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA.
[Petrinec, S. M.] Lockheed Martin ATC, Palo Alto, CA USA.
[Paterson, W. R.; Bromund, K. R.; Le, G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Zhou, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA USA.
[Anderson, B. J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Baumjohann, W.; Fischer, D.; Nakamura, R.; Plaschke, F.] Austrian Acad Sci, Space Res Inst, Graz, Austria.
[Chutter, M.; Torbert, R. B.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA.
[Slavin, J. A.] Univ Michigan, Dept Climate Space Sci & Engn, Ann Arbor, MI 48109 USA.
RP Zhao, C (reprint author), Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA.
EM czhao@igpp.ucla.edu
OI Baumjohann, Wolfgang/0000-0001-6271-0110; Russell,
Christopher/0000-0003-1639-8298
FU NASA Magnetospheric Multiscale Mission; NASA [NNG04EB99C]; University of
New Hampshire [06-001]; CNES; CNRS
FX This research was supported by the NASA Magnetospheric Multiscale
Mission in association with NASA contract NNG04EB99C. The work at UCLA
was supported through subcontract 06-001 with the University of New
Hampshire. IRAP contributions to MMS FPI was supported by CNES and CNRS.
We thank the entire MMS team and instrument leads for data access and
support. The data presented in this paper are the L2 data of MMS and can
be accessed from MMS Science Data Center
(https://lasp.colorado.edu/mms/sdc/public/).
NR 19
TC 0
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U1 1
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD DEC 16
PY 2016
VL 43
IS 23
BP 11941
EP 11947
DI 10.1002/2016GL071568
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA EI5DU
UT WOS:000392515000007
ER
PT J
AU Schmedemann, N
Kneissl, T
Neesemann, A
Stephan, K
Jaumann, R
Krohn, K
Michael, GG
Matz, KD
Otto, KA
Raymond, CA
Russell, CT
AF Schmedemann, Nico
Kneissl, T.
Neesemann, A.
Stephan, K.
Jaumann, R.
Krohn, K.
Michael, G. G.
Matz, K. D.
Otto, K. A.
Raymond, C. A.
Russell, C. T.
TI Timing of optical maturation of recently exposed material on Ceres
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Ceres; maturation; crater; weathering; age
ID CASSINI-VIMS; SURFACE; CHRONOLOGY; VESTA; RAY
AB On Ceres, multispectral imaging data from the Dawn spacecraft show a distinct bluish characteristic for recently exposed material from the subsurface in, for example, crater ejecta. Ejecta blankets of presumably old craters show a more reddish spectrum. We selected areas in which fresh material from the Cerean subsurface was exposed at a specific time in the past, and no later geologic process is expected to have changed its surface composition or its cratering record. For each area, we determined two color ratios and the crater retention age. The measured color ratios show an exponential diminishment of the bluish characteristic over time. Although the cause of the color change remains uncertain, the time-dependent change in spectral properties is evident, which could help identify the process.
C1 [Schmedemann, Nico; Kneissl, T.; Neesemann, A.; Jaumann, R.; Michael, G. G.] Free Univ Berlin, Inst Geol Sci, Berlin, Germany.
[Stephan, K.; Jaumann, R.; Krohn, K.; Matz, K. D.; Otto, K. A.] German Aerosp Ctr, Inst Planetary Res, Berlin, Germany.
[Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
RP Schmedemann, N (reprint author), Free Univ Berlin, Inst Geol Sci, Berlin, Germany.
EM nico.schmedemann@fu-berlin.de
OI Krohn, Katrin/0000-0001-8518-4985
FU German Space Agency (DLR) on behalf of the Federal Ministry for Economic
Affairs and Energy, Germany [50 OW 1505, 50 QM 1301];
Helmholtz-Gemeinschaft (Helmholtz Association) [PD-207]
FX This work has been supported by the German Space Agency (DLR) on behalf
of the Federal Ministry for Economic Affairs and Energy, Germany, grants
50 OW 1505 (N.S., T.K., and A.N.) and 50 QM 1301 (G.M.), and
Helmholtz-Gemeinschaft (Helmholtz Association) PD-207 (K.K.). We thank
the Dawn flight team for their excellent job of navigating and
maintaining the probe and the reviewers Stephanie Werner and Carolyn van
der Bogert for their constructive and valuable comments. The global
color mosaics of Ceres and their respective description used in this
study are available at
http://sbn.psi.edu/archive/dawn/fc/certified/DWNCHFFC2_2/ Geometry data
of the mapped areas and craters are listed in the supporting information
Tables S3-S18. Alternatively, geometry data are also available from the
lead author of this work.
NR 38
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U1 1
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD DEC 16
PY 2016
VL 43
IS 23
BP 11987
EP 11993
DI 10.1002/2016GL071143
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA EI5DU
UT WOS:000392515000003
ER
PT J
AU Krohn, K
Jaumann, R
Stephan, K
Otto, KA
Schmedemann, N
Wagner, RJ
Matz, KD
Tosi, F
Zambon, F
von der Gathen, I
Schulzeck, F
Schroder, SE
Buczkowski, DL
Hiesinger, H
McSween, HY
Pieters, CM
Preusker, F
Roatsch, T
Raymond, CA
Russell, CT
Williams, DA
AF Krohn, K.
Jaumann, R.
Stephan, K.
Otto, K. A.
Schmedemann, N.
Wagner, R. J.
Matz, K. -D.
Tosi, F.
Zambon, F.
von der Gathen, I.
Schulzeck, F.
Schroeder, S. E.
Buczkowski, D. L.
Hiesinger, H.
McSween, H. Y.
Pieters, C. M.
Preusker, F.
Roatsch, T.
Raymond, C. A.
Russell, C. T.
Williams, D. A.
TI Cryogenic flow features on Ceres: Implications for crater-related
cryovolcanism
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE cryovolcanism; impact melt; dwarf planet Ceres; subsurface materials;
flow features; coefficient of friction
ID LIQUID-WATER; ORIGIN; AVALANCHES; GANYMEDE; MISSION; STATE; VESTA
AB Craters on Ceres, such as Haulani, Kupalo, Ikapati, and Occator show postimpact modification by the deposition of extended plains material with pits, multiple lobate flows, and widely dispersed deposits that form a diffuse veneer on the preexisting surface. Bright material units in these features have a negative spectral slope in the visible range, making it appear bluish with respect to the grey-toned overall surface of Ceres. We calculate the drop height-to-runout length ratio of several flow features and obtain a coefficient of friction of<0.1: The results imply higher flow efficiency for flow features on Ceres than for similar features on other planetary bodies with similar gravity, suggesting low-viscosity material. The special association of flow features with impact craters could either point to an impact melt origin or to an exogenic triggering of cryovolcanic processes.
C1 [Krohn, K.; Jaumann, R.; Stephan, K.; Otto, K. A.; Wagner, R. J.; Matz, K. -D.; von der Gathen, I.; Schulzeck, F.; Schroeder, S. E.; Preusker, F.; Roatsch, T.] Deutsch Zentrum Luft & Raumfahrt, Inst Planetary Res, Berlin, Germany.
[Jaumann, R.; Schmedemann, N.] Free Univ Berlin, Inst Geol Sci Planetary Sci & Remote Sensing, Berlin, Germany.
[Tosi, F.; Zambon, F.] Natl Inst Astrophys, INAF IAPS, Rome, Italy.
[Buczkowski, D. L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Hiesinger, H.] Westfalische Wilhelms Univ Munster, Inst Planetol, Munster, Germany.
[McSween, H. Y.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN USA.
[Pieters, C. M.] Brown Univ, Providence, RI 02912 USA.
[Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Russell, C. T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
[Williams, D. A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, TX USA.
RP Krohn, K (reprint author), Deutsch Zentrum Luft & Raumfahrt, Inst Planetary Res, Berlin, Germany.
EM katrin.krohn@dlr.de
OI Krohn, Katrin/0000-0001-8518-4985; Tosi, Federico/0000-0003-4002-2434;
Zambon, Francesca/0000-0002-4190-6592
FU Helmholtz Association (HGF) through the research Helmholtz Postdoc
Program
FX We thank the Dawn team for the development, cruise, orbital insertion,
and operations of the Dawn spacecraft at Ceres. Portions of this work
were performed at the DLR Institute of Planetary Research, at the Jet
Propulsion Laboratory (JPL) under contract with NASA. Dawn data are
archived with the NASA Planetary Data System (http://sbn.pds.nasa.gov/).
K. Krohn is supported by the Helmholtz Association (HGF) through the
research Helmholtz Postdoc Program.
NR 53
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U1 4
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD DEC 16
PY 2016
VL 43
IS 23
BP 11994
EP 12003
DI 10.1002/2016GL070370
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA EI5DU
UT WOS:000392515000009
ER
PT J
AU Nelson, RR
Crisp, D
Ott, LE
O'Dell, CW
AF Nelson, Robert R.
Crisp, David
Ott, Lesley E.
O'Dell, Christopher W.
TI High-accuracy measurements of total column water vapor from the Orbiting
Carbon Observatory-2
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE OCO-2; water vapor; TCWV; remote sensing; hyperspectral; near-infrared
ID RESOLUTION IMAGING SPECTRORADIOMETER; RETRIEVAL; VALIDATION; ALGORITHM;
MODIS; OCO-2; SPECTROMETER; PERFORMANCE; HUMIDITY; NETWORK
AB Accurate knowledge of the distribution of water vapor in Earth's atmosphere is of critical importance to both weather and climate studies. Here we report on measurements of total column water vapor (TCWV) from hyperspectral observations of near-infrared reflected sunlight over land and ocean surfaces from the Orbiting Carbon Observatory-2 (OCO-2). These measurements are an ancillary product of the retrieval algorithm used to measure atmospheric carbon dioxide concentrations, with information coming from three highly resolved spectral bands. Comparisons to high-accuracy validation data, including ground-based GPS and microwave radiometer data, demonstrate that OCO-2 TCWV measurements have maximum root-mean-square deviations of 0.9-1.3mm. Our results indicate that OCO-2 is the first space-based sensor to accurately and precisely measure the two most important greenhouse gases, water vapor and carbon dioxide, at high spatial resolution (1.3 x 2.3 km(2)) and that OCO-2 TCWV measurements may be useful in improving numerical weather predictions and reanalysis products.
C1 [Nelson, Robert R.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Crisp, David] Jet Prop Lab, Pasadena, CA USA.
[Ott, Lesley E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[O'Dell, Christopher W.] Cooperat Inst Res Atmosphere, Ft Collins, CO USA.
RP Nelson, RR (reprint author), Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
EM rrnelson@atmos.colostate.edu
FU Jet Propulsion Laboratory [1439002]
FX The Colorado State University and Cooperative Institute for Research in
the Atmosphere contributions to this work were supported by Jet
Propulsion Laboratory subcontract 1439002. A portion of the research
described in this paper was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration. The OCO-2 water vapor
data used in this study are contained in the level-2 OCO-2 "Lite" files,
available at the NASA Goddard Earth Sciences Data and Information
Services Center (GES DISC,
http://disc.sci.gsfc.nasa.gov/uui/datasets/OCO2_L2_Lite_FP_V7r/summary).
The authors would like to thank Thomas H. Vonder Haar, Andrew I.
Manaster, and Heather Q. Cronk for their contributions to this work.
NR 42
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U1 5
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD DEC 16
PY 2016
VL 43
IS 23
BP 12261
EP 12269
DI 10.1002/2016GL071200
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA EI5DU
UT WOS:000392515000012
ER
PT J
AU Indo, HP
Majima, HJ
Terada, M
Suenaga, S
Tomita, K
Yamada, S
Higashibata, A
Ishioka, N
Kanekura, T
Nonaka, I
Hawkins, CL
Davies, MJ
St Clair, DK
Mukai, C
AF Indo, Hiroko P.
Majima, Hideyuki J.
Terada, Masahiro
Suenaga, Shigeaki
Tomita, Kazuo
Yamada, Shin
Higashibata, Akira
Ishioka, Noriaki
Kanekura, Takuro
Nonaka, Ikuya
Hawkins, Clare L.
Davies, Michael J.
St Clair, Daret K.
Mukai, Chiaki
TI Changes in mitochondrial homeostasis and redox status in astronauts
following long stays in space
SO SCIENTIFIC REPORTS
LA English
DT Article
ID SIMULATED MICROGRAVITY; LYMPHOBLASTOID-CELLS; SUPEROXIDE-DISMUTASE;
HUMAN-LYMPHOCYTES; SKELETAL-MUSCLE; FREE-RADICALS; STEM-CELLS;
RAT-LIVER; DNA; SPACEFLIGHT
AB The effects of long-term exposure to extreme space conditions on astronauts were investigated by analyzing hair samples from ten astronauts who had spent six months on the International Space Station (ISS). Two samples were collected before, during and after their stays in the ISS; hereafter, referred to as Preflight, Inflight and Postflight, respectively. The ratios of mitochondrial (mt) to nuclear (n) DNA and mtRNA to nRNA were analyzed via quantitative PCR. The combined data of Preflight, Inflight and Postflight show a significant reduction in the mtDNA/nDNA in Inflight, and significant reductions in the mtRNA/nRNA ratios in both the Inflight and Postflight samples. The mtRNA/mtDNA ratios were relatively constant, except in the Postflight samples. Using the same samples, the expression of redox and signal transduction related genes, MnSOD, CuZnSOD, Nrf2, Keap1, GPx4 and Catalase was also examined. The results of the combined data from Preflight, Inflight and Postflight show a significant decrease in the expression of all of the redox-related genes in the samples collected Postflight, with the exception of Catalase, which show no change. This decreased expression may contribute to increased oxidative stress Inflight resulting in the mitochondrial damage that is apparent Postflight.
C1 [Indo, Hiroko P.; Majima, Hideyuki J.; Suenaga, Shigeaki; Tomita, Kazuo; Higashibata, Akira; Ishioka, Noriaki] Kagoshima Univ, Grad Sch Med & Dent Sci, Dept Oncol & Space Environm Med, Kagoshima, Kagoshima 8908544, Japan.
[Terada, Masahiro] Jikei Univ, Div Aerosp Med, Sch Med, Minato Ku, Tokyo 1058461, Japan.
[Terada, Masahiro; Yamada, Shin; Higashibata, Akira; Ishioka, Noriaki; Mukai, Chiaki] Japan Aerosp Explorat Agcy, Tsukuba, Ibaraki 3058505, Japan.
[Terada, Masahiro] NASA, Ames Res Ctr, Space Biosci Div, Moffett Field, CA 94035 USA.
[Ishioka, Noriaki] Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan.
[Ishioka, Noriaki] SOKENDAI Grad Univ Adv Studies, Sch Phys Sci, Dept Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan.
[Kanekura, Takuro] Kagoshima Univ, Grad Sch Med & Dent Sci, Dept Dermatol, Kagoshima, Kagoshima 8908544, Japan.
[Nonaka, Ikuya] Natl Ctr Hosp Mental Nervous & Muscular Disorders, Kodaira, Tokyo 1878551, Japan.
[Hawkins, Clare L.] Heart Res Inst, 7 Eliza St, Sydney, NSW 2042, Australia.
[Hawkins, Clare L.] Univ Sydney, Sydney Med Sch, Sydney, NSW 2006, Australia.
[Davies, Michael J.] Univ Copenhagen, Panum Inst, Dept Biomed Sci, Blegdamsvej 3, DK-2200 Copenhagen, Denmark.
[St Clair, Daret K.] Univ Kentucky, Coll Med, Dept Toxicol & Canc Biol, Lexington, KY 40536 USA.
[Mukai, Chiaki] Tokyo Univ Sci, Shinjuku Ku, Tokyo 1620825, Japan.
RP Majima, HJ (reprint author), Kagoshima Univ, Grad Sch Med & Dent Sci, Dept Oncol & Space Environm Med, Kagoshima, Kagoshima 8908544, Japan.
EM hmajima@dent.kagoshima-u.ac.jp
RI Davies, Michael/H-4939-2011; Hawkins, Clare/F-6696-2014
OI Davies, Michael/0000-0002-5196-6919; Hawkins, Clare/0000-0003-2738-5089
FU JAXA-ISS Space Medicine Program Grant from the Japan Aerospace
Exploration Agency
FX This study was supported in part by the JAXA-ISS Space Medicine Program
Grant from the Japan Aerospace Exploration Agency. The authors
gratefully thank the astronaut who took part in this study, especially
Dr. Satoshi Furukawa of JAXA who provided encouragement to complete this
study, and Professor John Tremarco of Kagoshima University for his help
and guidance during the preparation of this manuscript.
NR 65
TC 0
Z9 0
U1 7
U2 7
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2045-2322
J9 SCI REP-UK
JI Sci Rep
PD DEC 16
PY 2016
VL 6
AR 39015
DI 10.1038/srep39015
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EE8OM
UT WOS:000389885400001
PM 27982062
ER
PT J
AU Bi, JR
Huang, JP
Holben, B
Zhang, GL
AF Bi, Jianrong
Huang, Jianping
Holben, Brent
Zhang, Guolong
TI Comparison of key absorption and optical properties between pure and
transported anthropogenic dust over East and Central Asia
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID SKY RADIANCE MEASUREMENTS; DESERT DUST; RADIATIVE PROPERTIES;
LIGHT-ABSORPTION; NORTHWEST CHINA; MINERAL DUST; ATMOSPHERIC AEROSOL;
SEMIARID CLIMATE; LOESS PLATEAU; AEOLIAN DUST
AB Asian dust particulate is one of the primary aerosol constituents in the Earth-atmosphere system that exerts profound influences on environmental quality, human health, the marine biogeochemical cycle, and Earth's climate. To date, the absorptive capacity of dust aerosol generated from the Asian desert region is still an open question. In this article, we compile columnar key absorption and optical properties of mineral dust over East and Central Asian areas by utilizing the multiyear quality-assured datasets observed at 13 sites of the Aerosol Robotic Network (AERONET). We identify two types of Asian dust according to threshold criteria from previously published literature. (1) The particles with high aerosol optical depth at 440 nm (AOD(440) >= 0.4) and a low Angstrom wavelength exponent at 440-870 nm (alpha < 0.2) are defined as Pure Dust (PDU), which decreases disturbance of other non-dust aerosols and keeps high accuracy of pure Asian dust. (2) The particles with AOD(440) >= 0.4 and 0.2 < alpha < 0.6 are designated as Transported Anthropogenic Dust (TDU), which is mainly dominated by dust aerosol and might mix with other anthropogenic aerosol types. Our results reveal that the primary components of high AOD days are predominantly dust over East and Central Asian regions, even if their variations rely on different sources, distance from the source, emission mechanisms, and meteorological characteristics. The overall mean and standard deviation of single-scattering albedo, asymmetry factor, real part and imaginary part of complex refractive index at 550 nm for Asian PDU are 0.935 +/- 0.014, 0.742 +/- 0.008, 1.526 +/- 0.029, and 0.00226 +/- 0.00056, respectively, while corresponding values are 0.921 +/- 0.021, 0.723 +/- 0.009, 1.521 +/- 0.025, and 0.00364 +/- 0.0014 for Asian TDU. Aerosol shortwave direct radiative effects at the top of the atmosphere (TOA), at the surface (SFC), and in the atmospheric layer (ATM) for Asian PDU (alpha < 0.2) and TDU (0.2 < alpha < 0.6) computed in this study, are a factor of 2 smaller than the results of Optical Properties of Aerosols and Clouds (OPAC) mineral-accumulated (mineral-acc.) and mineral-transported (mineral-tran.) modes. Therefore, we are convinced that our results hold promise for updating and improving accuracies of Asian dust characteristics in present-day remote sensing applications and regional or global climate models.
C1 [Bi, Jianrong; Huang, Jianping; Zhang, Guolong] Lanzhou Univ, Coll Atmospher Sci, Minist Educ, Key Lab Semiarid Climate Change, Lanzhou 730000, Peoples R China.
[Holben, Brent] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Huang, JP (reprint author), Lanzhou Univ, Coll Atmospher Sci, Minist Educ, Key Lab Semiarid Climate Change, Lanzhou 730000, Peoples R China.
EM hjp@lzu.edu.cn
FU National Science Foundation of China [41521004, 41305025, 41575015,
41405113]; Fundamental Research Funds for the Central Universities
[lzujbky-2015-4, lzujbky-2016-k01]; China 111 Project [B 13045]
FX This work was jointly supported by the National Science Foundation of
China (41521004, 41305025, 41575015 and 41405113), the Fundamental
Research Funds for the Central Universities lzujbky-2015-4 and
lzujbky-2016-k01, and the China 111 Project (No. B 13045). We thank the
GSFC/NASA AERONET group for processing the AERONET data
(http://aeronet.gsfc.nasa.gov). The authors would like to express
special thanks to the principal investigators (Hong-Bin Chen, Philippe
Goloub, Bernadette Chatenet, Xiao-Ye Zhang, Laurent Gomes, Sabur F.
Abdullaev, and Hamid Khalesifard) and their staff for effort in
establishing and maintaining the instruments at AERONET sites used in
this work. We appreciate the MODIS and TOMS teams for supplying the
satellite data. We would also like to thank all anonymous reviewers for
their constructive and insightful comments.
NR 100
TC 0
Z9 0
U1 8
U2 8
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PD DEC 15
PY 2016
VL 16
IS 24
BP 15501
EP 15516
DI 10.5194/acp-16-15501-2016
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EH0XG
UT WOS:000391486900005
ER
PT J
AU Gurgiolo, C
Goldstein, ML
AF Gurgiolo, Chris
Goldstein, Melvyn L.
TI Observations of diffusion in the electron halo and strahl
SO ANNALES GEOPHYSICAE
LA English
DT Article
DE Interplanetary physics (solar wind plasma)
ID HELIOS PLASMA-EXPERIMENT; SOLAR-WIND; FIELD; CORONA; WAVES
AB Observations of the three-dimensional solar wind electron velocity distribution functions (VDF) using phi-theta plots often show a tongue of electrons that begins at the strahl and stretches toward a new population of electrons, termed the proto-halo, that exists near the projection of the magnetic field opposite that associated with the strahl. The energy range in which the tongue and proto-halo are observed forms a "diffusion zone". The tongue first appears in energy generally near the lower-energy range of the strahl and in the absence of any clear core/halo signature. While the phi-theta plots give the appearance that the tongue and proto-halo are derived from the strahl, a close examination of their density suggests that their source is probably the upper-energy core/halo electrons which have been scattered by one or more processes into these populations.
C1 [Gurgiolo, Chris] Bitterroot Basic Res, Hamilton, MT 59840 USA.
[Goldstein, Melvyn L.] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Code 672, Greenbelt, MD USA.
RP Gurgiolo, C (reprint author), Bitterroot Basic Res, Hamilton, MT 59840 USA.
EM chris@gurgiolo.com
FU NASA [NNX15AI88G]
FX The authors would like to acknowledge the work and role of the Cluster
Science Archive (CSA) and thank the EFW and FGM teams for providing the
data used in this study. We would also like to acknowledge the PEACE
team at MSSL who worked on and are constantly improving the instrument
calibration. Both of us would like to acknowledge support from NASA
Grant NNX15AI88G.
NR 37
TC 0
Z9 0
U1 0
U2 0
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 0992-7689
EI 1432-0576
J9 ANN GEOPHYS-GERMANY
JI Ann. Geophys.
PD DEC 15
PY 2016
VL 34
IS 12
BP 1175
EP 1189
DI 10.5194/angeo-34-1175-2016
PG 15
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA EH0YH
UT WOS:000391489700001
ER
PT J
AU Steiner, MH
Hausrath, EM
Madden, MEE
Tschauner, O
Ehlmann, BL
Olsen, AA
Gainey, SR
Smith, JS
AF Steiner, M. H.
Hausrath, E. M.
Madden, M. E. Elwood
Tschauner, O.
Ehlmann, B. L.
Olsen, A. A.
Gainey, S. R.
Smith, J. S.
TI Dissolution of nontronite in chloride brines and implications for the
aqueous history of Mars
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
DE Mars; Nontronite; Clay minerals; Dissolution; Brines; Habitability;
Chlorides
ID KAOLINITE DISSOLUTION; MONTMORILLONITE DISSOLUTION; PRECIPITATION
KINETICS; SILICATE MINERALS; ACIDIC CONDITIONS; ROOM-TEMPERATURE;
ORGANIC-LIGANDS; WATER ACTIVITY; PH; 25-DEGREES-C
AB Increasing evidence suggests the presence of recent liquid water, including brines, on Mars. Brines have therefore likely impacted clay minerals such as the Fe-rich mineral nontronite found in martian ancient terrains. To interpret these interactions, we conducted batch experiments to measure the apparent dissolution rate constant of nontronite at 25.0 degrees C at activities of water (aH(2)O) of 1.00 (0.01 M CaCl2 or NaCl), 0.75 (saturated NaCl or 3.00 mol kg x 1 CaCl2), and 0.50 (5.00 mol kg x 1 CaCl2). Experiments at aH(2)O = 1.00 (0.01 M CaCl2) were also conducted at 4.0 C, 25.0 C, and 45.0 degrees C to measure an apparent activation energy for the dissolution of nontronite.
Apparent dissolution rate constants at 25.0 degrees C in CaCl2-containing solutions decrease with decreasing activity of water as follows: 1.18 x 10(-12) +/- 9 x 10(-14) mol mineral m(-2) s(-1) (aH(2)O = 1.00) > 2.36 x 10(-13) +/- 3.1 x 10(-14) mol mineral m(-2) s(-1) (aH(2)O = 0.75) > 2.05 x 10(-14) +/- 2.9 x 10(-15) mol mineral m(-2) s(-1) (aH(2)O = 0.50). Similar results were observed at 25.0 degrees C in NaCl-containing solutions: 1.89 x 10(-12) +/- 1 x 10(-13) mol mineral m(-2) s(-1) (aH(2)O = 1.00) > 1.98 x 10(-13) +/- 2.3 x 10(-14) mol mineral m(-2) s(-1) (aH(2)O = 0.75). This decrease in apparent dissolution rate constants with decreasing activity of water follows a relationship of the form: log k(diss) = 3.70 +/- 0.20 x aH(2)O x 15.49, where k(diss) is the apparent dissolution rate constant, and aH(2)O is the activity of water. The slope of this relationship (3.70 x 0.20) is within uncertainty of that of other minerals where the relationship between dissolution rates and activity of water has been tested, including forsteritic olivine (log R = 3.27 +/- 0.91 x aH(2)O x 11.00) (Olsen et al., 2015) and jarosite (log R = 3.85 +/- 0.43 x aH(2)O-12.84) (Dixon et al., 2015), where R is the mineral dissolution rate. This result allows prediction of mineral dissolution as a function of activity of water and suggests that with decreasing activity of water, mineral dissolution will decrease due to the role of water as a ligand in the reaction.
Apparent dissolution rate constants in the dilute NaCl solution (1.89 x 10(-12) +/- 1 x 10(-13) mol mineral m(-2) s(-1)) are slightly greater than those in the dilute CaCl2 solutions (1.18 x 10(-12) +/- 9 x 10(-14) mol mineral m(-2) s(-1)). We attribute this effect to the exchange of Na with Ca in the nontronite interlayer. An apparent activation energy of 54.6 +/- 1.0 kJ/mol was calculated from apparent dissolution rate constants in dilute CaCl2-containing solutions at temperatures of 4.0 degrees C, 25.0 degrees C, and 45.0 C: 2.33 x 10(-13) +/- 1.3 x 10(-14) mol mineral m(-2) s(-1) (4.0 degrees C), 1.18 x 10(-12) +/- 9 x 10(-14) mol mineral m(-2) s(-1) (25.0 degrees C), and 4.98 x 10(-12) +/- 3.8 x 10(-13) mol mineral m(-2) s(-1) (45.0 degrees C).
The greatly decreased dissolution of nontronite in brines and at low temperatures suggests that any martian nontronite found to be perceptibly weathered may have experienced very long periods of water-rock interaction with brines at the low temperatures prevalent on Mars, with important implications for the paleoclimate and long-term potential habitability of Mars. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Steiner, M. H.; Hausrath, E. M.; Tschauner, O.; Gainey, S. R.] Univ Nevada Las Vegas, Dept Geosci, 4505 S Maryland Pkwy, Las Vegas, NV 89154 USA.
[Madden, M. E. Elwood] Univ Oklahoma, Sch Geol & Geophys, 100 E Boyd,Suite 710, Norman, OK 73019 USA.
[Ehlmann, B. L.] CALTECH, Div Planetary Sci, 1200 East Calif Blvd, Pasadena, CA 91125 USA.
[Olsen, A. A.] Univ Maine, Sch Earth & Climate Sci, 5790 Bryand Global Sci Ctr, Orono, ME 04469 USA.
[Smith, J. S.] Carnegie Inst Sci, Geophys Lab, HPCAT, Argonne, IL 60439 USA.
[Ehlmann, B. L.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Hausrath, EM (reprint author), Univ Nevada Las Vegas, Dept Geosci, 4505 S Maryland Pkwy, Las Vegas, NV 89154 USA.
EM Elisabeth.Hausrath@unlv.edu
FU Mars Fundamental Research Program grant [NNX12AH96G]; UNLV Faculty
Opportunity Award; UNLV Graduate and Professional Student Association;
U.S. DOE [DE-AC02-06CH11357]; Office of Science, Office of Basic Energy
Sciences, of the U.S. Department of Energy [DE-AC02-05CH11231]; COMPRES,
the Consortium for Materials Properties Research in Earth Sciences under
NSF Cooperative Agreement [EAR 11-57758]; DOE-NNSA [DE-NA0001974];
DOE-BES [DE-FG02-99ER45775]; NSF; National Nuclear Security
Administration under the Stewardship Science Academic Alliances program
through DOE Cooperative Agreement [DE-NA0001982]
FX We would like to acknowledge the Mars Fundamental Research Program grant
NNX12AH96G, the UNLV Faculty Opportunity Award, and the UNLV Graduate
and Professional Student Association for travel funding. The authors
would like to thank Chris Adcock, Kirellos Sefein, Valerie Tu, Renee
Schofield, Courtney Bartlett, and Angela Garcia for insightful
conversation and lab assistance, and Minghua Ren and Michael Strange for
aid in FE-SEM imaging. Part of the work was conducted at the HPCAT
(Sector 16) of the Advanced Photon Source (APS), Argonne National
Laboratory and the 12.2.2 beamline of the Advanced Light Source. Use of
the Advanced Photon Source, an Office of Science User Facility operated
for the U.S. Department of Energy (DOE) Office of Science by Argonne
National Laboratory, was supported by the U.S. DOE under Contract No.
DE-AC02-06CH11357. The Advanced Light Source is supported by the
Director, Office of Science, Office of Basic Energy Sciences, of the
U.S. Department of Energy under Contract No. DE-AC02-05CH11231. ALS
beamline 12.2.2 is partially supported by COMPRES, the Consortium for
Materials Properties Research in Earth Sciences under NSF Cooperative
Agreement EAR 11-57758. HPCAT operations are supported by DOE-NNSA under
Award No. DE-NA0001974 and DOE-BES under Award No. DE-FG02-99ER45775,
with partial instrumentation funding by NSF. This work was in part
supported by the National Nuclear Security Administration under the
Stewardship Science Academic Alliances program through DOE Cooperative
Agreement #DE-NA0001982. We also appreciate thoughtful reviews by four
anonymous reviewers that greatly strengthened the paper.
NR 100
TC 0
Z9 0
U1 8
U2 8
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
EI 1872-9533
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD DEC 15
PY 2016
VL 195
BP 259
EP 276
DI 10.1016/j.gca.2016.08.035
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EG3QD
UT WOS:000390958900014
ER
PT J
AU Nandan, V
Geldsetzer, T
Islam, T
Yackel, JJ
Gill, JPS
Fuller, MC
Gunn, G
Duguay, C
AF Nandan, Vishnu
Geldsetzer, Torsten
Islam, Tanvir
Yackel, John. J.
Gill, Jagvijay P. S.
Fuller, Mark. C.
Gunn, Grant
Duguay, Claude
TI Ku-, X- and C-band measured and modeled microwave backscatter from a
highly saline snow cover on first-year sea ice
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Active microwaves; Snow; Sea ice; Microwave scattering
ID APERTURE RADAR DATA; SURFACE-AREA; INFRARED REFLECTANCE; SCATTEROMETER;
SIGNATURES; FREQUENCIES; SCATTERING; BRINE; MELT
AB In this study, we inter-compare observed and modeled Ku-, X- and C-band microwave backscatter for two snow temperature conditions for a highly saline snow cover on smooth first-year sea ice. A new surface-based multi frequency (Ku-, X- and C-bands) microwave scatterometer system is used quasi-coincident with in situ geophysical snow measurements. A multilayer snow and ice backscatter model is used to calculate the total co-polarized backscatter coefficient for two snow temperature conditions. The model provides the surface and volume scattering contributions for each snow layer, as well as the frequency-dependent penetration depth. These results aid interpretation of observed backscatter. Joint use of Ku-, X- and C-band microwaves provide an enhanced understanding of diverse variations in geophysical, thermodynamic and electrical state of snow/sea ice system. Our results indicate that the effect of dielectric loss associated with highly saline snow covers is the dominant factor affecting microwave penetration and backscatter from all three frequencies. The observed and modeled C band backscatter shows good agreement, followed by X- and Ku-bands, at both snow temperature conditions. Microwave backscatter shows greater sensitivity to variations in plot-scale surface roughness, for all three frequencies. Additionally, Ku-band wavelength exhibits greater sensitivity to snow grain radius, over X-, and C bands. Our results demonstrate the future potential of a multi-frequency approach towards the development of snow thickness and snow water equivalent algorithms on first-year sea ice. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Nandan, Vishnu; Geldsetzer, Torsten; Yackel, John. J.; Gill, Jagvijay P. S.; Fuller, Mark. C.] Univ Calgary, Dept Geog, Cryosphere Climate Res Grp, 2500 Univ Dr NW, Calgary, AB T2N 1N4, Canada.
[Islam, Tanvir] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Gunn, Grant; Duguay, Claude] Univ Waterloo, Dept Geog & Environm Management, Waterloo, ON N2L 3G1, Canada.
RP Nandan, V (reprint author), Univ Calgary, Dept Geog, Cryosphere Climate Res Grp, 2500 Univ Dr NW, Calgary, AB T2N 1N4, Canada.
EM vishnunandan.nandaku@ucalgary.ca
FU NSERC
FX The authors would like to thank ProSensing, Inc for providing UWScat
system to obtain scatterometer data; Dr. Randall Scharien, Jack Landy,
Megan Shields of the Center for Earth Observation Science, University of
Manitoba for their technical and logistical assistance; NSERC Discovery,
PCSP and NRS Research grants for project funding; All four
peer-reviewers for spending substantial time and effort for providing
valuable feedback and suggestions improve the standard of this
manuscript; Liv Waldorf and Patrick Duke for proof reading.
NR 52
TC 1
Z9 1
U1 3
U2 3
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD DEC 15
PY 2016
VL 187
BP 62
EP 75
DI 10.1016/j.rse.2016.10.004
PG 14
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA EF7EX
UT WOS:000390494000005
ER
PT J
AU Middleton, EM
Huemmrich, KF
Landis, DR
Black, TA
Barr, AG
McCaughey, JH
AF Middleton, E. M.
Huemmrich, K. F.
Landis, D. R.
Black, T. A.
Barr, A. G.
McCaughey, J. H.
TI Photosynthetic efficiency of northern forest ecosystems using a
MODIS-derived Photochemical Reflectance Index (PRI)
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Light use efficiency, LUE; MODIS; MODIS GPP; PRI; Terra, Aqua; Canadian
Carbon Program; Boreal forests; Forward scatter
ID LIGHT-USE EFFICIENCY; GROSS PRIMARY PRODUCTION; RADIATION-USE
EFFICIENCY; NET PRIMARY PRODUCTION; CARBON-DIOXIDE FLUXES; BLACK SPRUCE
FOREST; BOREAL ASPEN FOREST; DOUGLAS-FIR FOREST; LEAF-AREA INDEX;
DECIDUOUS FOREST
AB This study evaluates a direct remote sensing approach from space for the determination of ecosystem photosynthetic light use efficiency (LUE), through measurement of vegetation reflectance changes expressed with the Photochemical Reflectance Index (PRI). The PRI is a normalized difference index based on spectral changes at a physiologically active wavelength (similar to 531 nm) as compared to a reference waveband, and is only available from a very few satellites. These include the two Moderate-Resolution Imaging Spectroradiometers (MODIS) on the Aqua and Terra satellites each of which have a narrow (10 nm) ocean band centered at 531 nm. We examined several PRI variations computed with candidate reference bands, since MODIS lacks the traditional 570 nm reference band. The PRI computed using MODIS land band 1 (620-670 nm) gave the best performance for daily LUE estimation. Through rigorous statistical analyses over a large image collection (n = 420), the success of relating in situ daily tower-derived LUE to MODIS observations for northern forests was strongly influenced by satellite viewing geometry. LUE was calculated from CO2 fluxes (mol C mol(-1) absorbed quanta) measured at instrumented Canadian Carbon Program flux towers in four Canadian forests: a mature fir site in British Columbia, mature aspen and black spruce sites in Saskatchewan, and a mixed deciduous/coniferous forest site in Ontario. All aspects of the viewing geometry had significant effects on the MODIS-PRI, including the view zenith angle (VZA), the view azimuth angle, and the displacement of the view azimuth relative to the solar principal plane, in addition to illumination related variables. Nevertheless, we show that forward scatter sector views (VZA, 16 degrees-45 degrees) provided the strongest relationships to daily LUE, especially those collected in the early afternoon by Aqua (r(2) = 0.83, RMSE = 0.003 mol C mol(-1) absorbed quanta). Nadir (VZA, 0 15) and backscatter views (VZA, 16 to 45) had lower performance in estimating LUE (nadir: r(2) similar to 0.62-0.67; bacicscatter: r(2) similar to 0.54-0.59) and similar estimation error (RMSE = 0.004-0.005). When directional effects were not considered, only a moderately successful MODIS-PRI vs. LUE relationship (r(2) = 0.34, RMSE = 0.007) was obtained in the full dataset (all views & sites, both satellites), but site-specific relationships were able to discriminate between coniferous and deciduous forests. Overall, MODIS-PRI values from Terra (late morning) were higher than those from Aqua (early afternoon), before/after the onset of diurnal stress responses expressed spectrally. Therefore, we identified ninety-two Terra-Aqua "same day" pairs, for which the sum of Terra morning and Aqua afternoon MODIS-PRI values (PRIsum) using all available directional observations was linearly correlated with daily tower LUE (r(2) = 0.622, RMSE = 0.013) and independent of site differences or meteorological information. Our study highlights the value of off-nadir directional reflectance observations, and the value of pairing morning and afternoon satellite observations to monitor stress responses that inhibit carbon uptake in Canadian forest ecosystems.
In addition, we show that MODIS-PRI values, when derived from either: (i) forward views only, or (ii) Terra/Aqua same day (any view) combined observations, provided more accurate estimates of tower-measured daily LUE than those derived from either nadir or backscatter views or those calculated by the widely used semi-operational MODIS GPP model (MOD17) which is based on a theoretical maximum LUE and environmental data. Consequently, we demonstrate the importance of diurnal as well as off-nadir satellite observations for detecting vegetation physiological processes. (C) 2016 Published by Elsevier Inc.
C1 [Middleton, E. M.] NASA, Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Huemmrich, K. F.] Univ Maryland Baltimore Cty, Joint Ctr Earth Tech, Baltimore, MD 21228 USA.
[Landis, D. R.] Global Sci & Technol Inc, Greenbelt, MD 20770 USA.
[Black, T. A.] Univ British Columbia, Vancouver, BC, Canada.
[Barr, A. G.] Meteorol Serv Canada, Climate Res Branch, Saskatoon, SK, Canada.
[McCaughey, J. H.] Queens Univ, Kingston, ON, Canada.
RP Landis, DR (reprint author), Global Sci & Technol Inc, Greenbelt, MD 20770 USA.
EM elizabeth.m.middleton@nasa.gov; david.r.landis@nasa.gov
FU NASA; Canadian Foundation for Climate and Atmospheric Science (CFCAS);
Natural Sciences and Engineering Research Council (NSERC) of Canada;
BIOCAP Canada; Environment Canada; Natural Resources Canada
FX We would like to thank Dr. Forrest G. Hall (UMBC) for his advocacy of
multi-angle reflectance observations of ecosystems. We would also like
to acknowledge the research on PRI conducted by Dr. Thomas Hilker
(Oregon State Univ., in memorium). Our research was supported by NASA
funding on Carbon Cycle Science and the Science of Terra & Aqua. Thanks
also to Fluxnet Canada and the Canadian Carbon Program which was
supported by the Canadian Foundation for Climate and Atmospheric Science
(CFCAS), the Natural Sciences and Engineering Research Council (NSERC)
of Canada, and BIOCAP Canada. Additional support was from Environment
Canada and Natural Resources Canada.
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PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD DEC 15
PY 2016
VL 187
BP 345
EP 366
DI 10.1016/j.rse.2016.10.021
PG 22
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA EF7EX
UT WOS:000390494000025
ER
PT J
AU Eitel, JUH
Magney, TS
Vierling, LA
Greaves, HE
Zheng, G
AF Eitel, Jan U. H.
Magney, Troy S.
Vierling, Lee A.
Greaves, Heather E.
Zheng, Guang
TI An automated method to quantify crop height and calibrate
satellite-derived biomass using hypertemporal lidar
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Autonomously operating terrestrial laser scanner(ATLS); Leaf area index
(LAI); Hypertemporal lidar; Crop biomass; Biomass scaling; Error
accounting; Laser allometry
ID TERRESTRIAL LASER SCANNER; LEAF-AREA INDEX; WHEAT NITROGEN STATUS;
CHLOROPHYLL CONTENT; VEGETATION INDEXES; SPECTRAL INDEX; REFLECTANCE;
TRANSFERABILITY; DYNAMICS; LIMITATIONS
AB Crop biomass information is of great importance for a variety of applications, ranging from supporting farm management decisions to modeling the crop-environment system. Dimensionless spectral vegetation index values derived from satellite imagery are commonly used to derive crop biomass. However, the highly empirical nature of spectrally derived biomass estimates requires frequent and costly calibration with manually collected ground data. Recently, low cost, autonomously operating terrestrial laser scanners (ATLSs) have become available for near-surface applications. In contrast to the dimensionless nature of spectral index values, autonomous light detection and ranging (lidar) technology measures physical vegetation structure by recording the x, y, z coordinates of canopy components at very high spatial (<10 cm), and temporal (<2 days) resolution. The objective of this study was to assess the suitability of an ATLS to i) monitor crop growth dynamics and ii) calibrate satellite imagery for estimating crop biomass. Wheat (Triticum aestivum spp.) growth was monitored by acquiring hypertemporal (every 28 h for a full growing season) ATLS data at three different field sites across a range of experimentally manipulated crop growth conditions. The ATLS-derived crop height explained nearly three-quarters of the variability in destructively sampled wheat biomass (r(2) = 0.74, RMSE = 514.20 kg ha(-1)), showing a slightly stronger correlation to crop biomass than did leaf area index (LAI) measurements collected in the field using a LAI-2000 Plant Canopy Analyzer (r(2) = 0.71, RMSE = 546 kg ha(-1)). Satellite-based crop biomass estimates calibrated with ATLS data captured the variability in wheat biomass throughout a farm field with a biomass error of 730.96 and 727.60 kg ha(-1) (RMSE) during the jointing (Development stage: Zadoks 37) and heading (Development stage: Zadoks 50) growth stages, respectively. These findings suggest that the hypertemporal lidar information provided via ATLS technology could constitute a major step forward in operational monitoring and mapping of crop biomass. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Eitel, Jan U. H.; Vierling, Lee A.; Greaves, Heather E.] Univ Idaho, Geospatial Lab Environm Dynam, Moscow, ID 83844 USA.
[Eitel, Jan U. H.; Vierling, Lee A.] Univ Idaho, McCall Outdoor Sci Sch, Coll Nat Resources, Mccall, ID 83638 USA.
[Magney, Troy S.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Zheng, Guang] Nanjing Univ, Int Inst Earth Syst Sci, Nanjing 210023, Jiangsu, Peoples R China.
RP Eitel, JUH (reprint author), Univ Idaho, Geospatial Lab Environm Dynam, Moscow, ID 83844 USA.; Eitel, JUH (reprint author), Univ Idaho, McCall Outdoor Sci Sch, Coll Nat Resources, Mccall, ID 83638 USA.
EM jeitel@uidaho.edu
FU Department of the Interior, United States Geological Survey
[G14AP00002]; USDA-NIFA [2011-67003-3034, 2011-68002-30191]; NASA
[NNX10AM75H]
FX We thank two anonymous reviewers for their thoughtful comments that
helped to considerably improve the quality of the manuscript. We further
thank Dr. David Huggins for his help with the experimental design and
Jyoti Jennewein and Samuel Finch for their assistance in the field. We
also thank Dr. Christopher Williams for his help with the bootstrap
resampling procedure. This work was supported by Grant Number G14AP00002
from the Department of the Interior, United States Geological Survey to
AmericaView and USDA-NIFA Award Nos. 2011-67003-3034 and
2011-68002-30191. TSM was funded by NASA Idaho Space Grant Fellowship
(#NNX10AM75H). Mention of trade names and commercial products does not
constitute their endorsement by the University of Idaho or the U.S.
Government.
NR 59
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PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD DEC 15
PY 2016
VL 187
BP 414
EP 422
DI 10.1016/j.rse.2016.10.044
PG 9
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA EF7EX
UT WOS:000390494000029
ER
PT J
AU Lemoine, FG
Schrama, EJO
AF Lemoine, F. G.
Schrama, E. J. O.
TI Preface - Scientific applications of DORIS in space geodesy
SO ADVANCES IN SPACE RESEARCH
LA English
DT Editorial Material
C1 [Lemoine, F. G.] NASA, Goddard Space Flight Ctr, Geodesy & Geophys Lab, Code 61A, Greenbelt, MD 20771 USA.
[Schrama, E. J. O.] Delft Univ Technol, Fac Aerosp Engn, Kluyverweg 1, NL-2629 HS Delft, Netherlands.
RP Lemoine, FG (reprint author), NASA, Goddard Space Flight Ctr, Geodesy & Geophys Lab, Code 61A, Greenbelt, MD 20771 USA.
EM Frank.G.Lemoine@nasa.gov; e.j.o.schrama@tudelft.nl
NR 0
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PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD DEC 15
PY 2016
VL 58
IS 12
BP 2477
EP 2478
DI 10.1016/j.asr.2016.11.002
PG 2
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA EF1HS
UT WOS:000390076500001
ER
PT J
AU Moreaux, G
Lemoine, FG
Capdeville, H
Kuzin, S
Otten, M
Stepanek, P
Willis, P
Ferrage, P
AF Moreaux, Guilhem
Lemoine, Frank G.
Capdeville, Hugues
Kuzin, Sergey
Otten, Michiel
Stepanek, Petr
Willis, Pascal
Ferrage, Pascale
TI The International DORIS Service contribution to the 2014 realization of
the International Terrestrial Reference Frame
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE DORIS; Intra-technique combination; Terrestrial Reference Frame; ITRF;
Polar motion
ID RADIAL ORBIT ERROR; THERMOSPHERIC MODEL; SERIES; CONSTRAINTS; ALTIMETRY;
ITRF2008; JASON-1; SYSTEM; TRENDS
AB In preparation of the 2014 realization of the International Terrestrial Reference Frame (ITRF2014), the International DORIS Service delivered to the International Earth Rotation and Reference Systems Service a set of 1140 weekly solution files including station coordinates and Earth orientation parameters, covering the time period from 1993.0 to 2015.0. The data come from eleven DORIS satellites: TOPEX/Poseidon, SPOT2, SPOT3, SPOT4, SPOTS, Envisat, Jason-1, Jason-2, Cryosat-2, Saral and HY-2A. In their processing, the six analysis centers which contributed to the DORIS combined solution used the latest time variable gravity models and estimated DORIS ground beacon frequency variations. Furthermore, all the analysis centers but one excepted included in their processing phase center variations for ground antennas. The main objective of this study is to present the combination process and to analyze the impact of the new modeling on the performance of the new combined solution. Comparisons with the IDS contribution to ITRF2008 show that (i) the application of the DORIS ground phase center variations in the data processing shifts the combined scale upward by nearly 711 mm and (ii) thanks to estimation of DORIS ground beacon frequency variations, the new combined solution no longer shows any scale discontinuity in early 2002 and does not present unexplained vertical discontinuities in any station position time series. However, analysis of the new series with respect to ITRF2008 exhibits a scale increase late 2011 which is not yet explained. A new DORIS Terrestrial Reference Frame was computed to evaluate the intrinsic quality of the new combined solution. That evaluation shows that the addition of data from the new missions equipped with the latest generation of DORIS receiver (Jason-2, Cryosat-2, HY-2A, Saral), results in an internal position consistency of 10 mm or better after mid-2008. (C) 2015 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Moreaux, Guilhem; Capdeville, Hugues] Collette Localisat Satellites, 8-10 Rue Hermes,Parc Technol Canal, F-31520 Ramonville St Agne, France.
[Lemoine, Frank G.] NASA, Goddard Space Flight Ctr, Code 698, Greenbelt, MD 20771 USA.
[Kuzin, Sergey] Russian Acad Sci, Inst Astron, 48 Pjatnitskaya St, Moscow 119017, Russia.
[Otten, Michiel] ESA, European Space Operat Ctr, Robert Boch Str 5, D-64293 Darmstadt, Germany.
[Stepanek, Petr] Res Inst Geodesy Topog & Cartog, Geodet Observ Pecny, Ondrejov 244, Zdiby 25165, Czech Republic.
[Willis, Pascal] Inst Natl Informat Geog & Forestiere, St Mande, France.
[Willis, Pascal] Univ Paris Diderot, Inst Phys Globe Paris, UMR 7154, Sorbonne Paris Cite,Gravimetrie & Geodesie Spatia, Paris, France.
[Ferrage, Pascale] Ctr Natl Etud Spatiales, 18 Ave Edouard Belin, F-31401 Toulouse 9, France.
RP Moreaux, G (reprint author), Collette Localisat Satellites, 8-10 Rue Hermes,Parc Technol Canal, F-31520 Ramonville St Agne, France.
EM Guilhem.Moreaux@cls.fr
RI Willis, Pascal/A-8046-2008
OI Willis, Pascal/0000-0002-3257-0679
FU Czech grant agency project [15-24730J]
FX Part of this work was performed at CLS under contract with the Centre
National d'Etudes Spatiales (CNES). The authors are grateful to all the
Agencies hosting DORIS stations.The IDS CC would like to thank Zuheir
Altamimi (IGN) for his assist both on CATREF use and realization and
improvements of the DORIS combined solution.We also thank Mathis
Blossfeld (DGFI) and Claudio Abbondanza (JPL) for their collaboration on
the determination of the DORIS time series discontinuities. Part of the
work corresponding to GOP AC solutions was supported by Czech grant
agency project 15-24730J. All the data used in this study are freely
available and downloadable from the IDS data centers: CDDIS
(ftp://cddis.gsfc.nasa.gov/doris/productsh and IGN
(ftp://doris.ensg.ign.fr/pub/dorish/).
NR 52
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD DEC 15
PY 2016
VL 58
IS 12
BP 2479
EP 2504
DI 10.1016/j.asr.2015.12.021
PG 26
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA EF1HS
UT WOS:000390076500002
ER
PT J
AU Lemoine, FG
Chinn, DS
Zelensky, NP
Beall, JW
Le Bail, K
AF Lemoine, F. G.
Chinn, D. S.
Zelensky, N. P.
Beall, J. W.
Le Bail, K.
TI The development of the GSFC DORIS contribution to ITRF2014
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE DORIS; Terrestrial Reference Frame; ITRF2014; Precise orbit
determination; Polar motion
ID GRAVITY-FIELD MODELS; RADIAL ORBIT ERROR; CORRECTIVE MODEL; JASON-1;
TOPEX/POSEIDON; SPACECRAFT; PRESSURE; SERVICE; SERIES
AB The NASA GSFC DORIS analysis center has processed data from January 1993 to December 2014 and provided 1141 weekly solutions in the form of normal equations for incorporation into the DORIS solution for ITRF2014. The solution time series, designated as gscwd26, were based on tracking data to eleven DORIS satellites divided generally into seven-day arcs. With respect to the ITRF2008 submission (Le Bail et al., 2010), the measurement model was updated to model the beacon frequency variations at certain DORIS sites, to apply the DORIS antenna phase law for the Starec and Alcatel antennae, and to apply the antenna offset corrections in the NASA GSFC orbit determination software rather than using the data-supplied corrections. We show that computing the antenna offset corrections in the orbit determination software is superior to using the offset corrections that are supplied with the DORIS data, and that this improves the RMS of fit for SPOT-2, Envisat, SPOT-4, and SPOT-5. The updates for the force model included: (1) the development of improved nonconservative force modeling for SPOT-2, SPOT-3, SPOT-5, Envisat, and HY-2A, and (2) the application of an updated static gravity model based on GRACE and GOCE data, and weekly models of the variations in the low degree gravity field deduced independently from tracking by Satellite Laser Ranging (SLR) and DORIS. The post-ITRF2008 DORIS coordinate WRMS after the launch of Envisat and SPOT-5 is improved from 11.20 to 12.45 mm with ITRF2008 (Le Bail et al., 2010), to between 8.50 and 9.99 mm with the gscwd26 SINEX solution. The application of the DORIS antenna phase laws shifts the DORIS scale wrt DPOD2008 by +6.0 mm from 1993/01/03 to 2002/06/06, and. by +11.4 mm from 2002/06/13 to 2011/10/30. The application of more detailed models of time-variable gravity reduces the slopes in the Helmert transformation parameters Tx, and Ty (w.r.t. DPOD2008) after 2005. The annual amplitude in these parameters is reduced from 3.2 mm (for Tx), 4.1 mm (for Ty), to 1.7 mm (for Tx) and 2.8 mm (for Ty). Published by Elsevier Ltd. on behalf of COSPAR. This is an open access article under the CC BY-NC-ND license.
C1 [Lemoine, F. G.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Code 698, Greenbelt, MD 20771 USA.
[Chinn, D. S.; Zelensky, N. P.] SGT Inc, 7701 Greenbelt Rd, Greenbelt, MD 20770 USA.
[Beall, J. W.] Emergent Space Technol, 6411 Ivy Lane, Greenbelt, MD 20770 USA.
[Le Bail, K.] NVI Inc, 7527 Hanover Pkwy, Greenbelt, MD 20770 USA.
RP Lemoine, FG (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Code 698, Greenbelt, MD 20771 USA.
EM Frank.G.Lemoine@nasa.gov
FU U.S. National Aeronautics and Space Administration
FX This work was suppported by the U.S. National Aeronautics and Space
Administration, under following the programs: Interdisciplinary Research
in Earth Science, Ocean Surface Topography Science Team (OSTST), and
Making Earth System data records for Use in Research Environments
(MEaSUREs).
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD DEC 15
PY 2016
VL 58
IS 12
BP 2520
EP 2542
DI 10.1016/j.asr.2015.12.043
PG 23
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA EF1HS
UT WOS:000390076500004
ER
PT J
AU Willis, P
Heflin, MB
Haines, BJ
Bar-Sever, YE
Bertiger, WI
Mandea, M
AF Willis, Pascal
Heflin, Michael B.
Haines, Bruce J.
Bar-Sever, Yoaz E.
Bertiger, Willy I.
Mandea, Mioara
TI Is the Jason-2 DORIS oscillator also affected by the South Atlantic
Anomaly?
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE DORIS; GPS; South Atlantic Anomaly (SAA); Jason-2 satellite; Maule
earthquake
ID ORBIT DETERMINATION; CORRECTIVE MODEL; SEA-LEVEL; GPS DATA; NETWORK;
SERIES; TOPEX; ERROR
AB We analyzed time series of daily DORIS and GPS station coordinate estimates derived from Precise Point Positioning (PPP). The DORIS coordinates were estimated using Jason-2 precise orbits based on GPS data only, implying that the station positions from the two techniques are expressed in the same GPS-based terrestrial reference frame. Comparisons of 3-D vectors of such co-located stations show systematic biases in position around South America when compared to local geodetic ties. We conclude that these results could be explained by a sensitivity of the Jason-2/DORIS oscillator to radiation when the satellite passes over the South Atlantic Anomaly (SAA). The effect for Jason-2 manifests mainly as an offset in station coordinates, though there is also evidence of a drift at the start of the mission that diminishes in time. This contrasts with the experience on Jason-1, wherein large, persistent drifts were observed for stations in this same (SAA) region. The spurious drift is much (similar to 90%) smaller for Jason-2, which may be attributable to the steps taken prior to launch to harden the oscillator. Analysis of DORIS Doppler residuals may indicate some small degradation after 2009 for these stations. (C) 2016 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Willis, Pascal] Inst Natl Informat Geog & Forestiere, Direct Rech & Enseignement, F-77455 Marne La Vallee, France.
[Willis, Pascal] Univ Paris Diderot, Inst Phys Globe Paris, Gravimetrie & Geodesie Spatiale, UMR7154,Sorbonne Paris Cite, F-75013 Paris, France.
[Heflin, Michael B.; Haines, Bruce J.; Bar-Sever, Yoaz E.; Bertiger, Willy I.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Mandea, Mioara] Ctr Natl Etud Spatiales, F-75001 Paris, France.
RP Willis, P (reprint author), Inst Natl Informat Geog & Forestiere, Direct Rech & Enseignement, F-77455 Marne La Vallee, France.
EM pascal.willis@ign.fr
RI Willis, Pascal/A-8046-2008; MANDEA, Mioara/E-4892-2012
OI Willis, Pascal/0000-0002-3257-0679;
FU Centre National d'Etudes Spatiales (CNES)
FX Part of this was supported by the Centre National d'Etudes Spatiales
(CNES) and based on observations with DORIS embarked on Jason-2
satellite. Part of this research was performed at jet Propulsion
Laboratory, California Institute of Technology, under contract with
NASA.
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD DEC 15
PY 2016
VL 58
IS 12
BP 2617
EP 2627
DI 10.1016/j.asr.2016.09.015
PG 11
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA EF1HS
UT WOS:000390076500010
ER
PT J
AU Zelensky, NP
Lemoine, FG
Chinn, DS
Beckley, BD
Bordyugov, O
Yang, X
Wimert, J
Pavlis, D
AF Zelensky, Nikita P.
Lemoine, Frank G.
Chinn, Douglas S.
Beckley, Brian D.
Bordyugov, Oleg
Yang, Xu
Wimert, Jesse
Pavlis, Despina
TI Towards the 1-cm SARAL orbit
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE SARAL; POD; DORIS; SLR; Altimetry; Satellite orbit
ID MEAN SEA-LEVEL; GEOCENTER MOTION; TOPEX/POSEIDON; ALTIMETRY; GRAVITY;
JASON-1; ERROR; MODEL; GPS; MISSIONS
AB We have investigated the quality of precise orbits for the SARAL altimeter satellite using Satellite Laser Ranging (SLR) and Doppler Orbitography and Radiopositioning Integrated by Satellite (DORIS) data from March 14, 2013 to August 10, 2014. We have identified a 4.31 +/- 0.14 cm error in the Z (cross-track) direction that defines the center-of-mass of the SARAL satellite in the spacecraft coordinate system, and we have tuned the SLR and DORIS tracking point offsets. After these changes, we reduce the average RMS of the SLR residuals for seven-day arcs from 1.85 to 1.38 cm. We tuned the non-conservative force model for SARAL, reducing the amplitude of the daily adjusted empirical accelerations by eight percent. We find that the best dynamic orbits show altimeter crossover residuals of 5.524 cm over cycles 7-15. Our analysis offers a unique illustration that high-elevation SLR residuals will not necessarily provide an accurate estimate of radial error at the 1-cm level, and that other supporting orbit tests are necessary for a better estimate. Through the application of improved models for handling time-variable gravity, the use of reduced-dynamic orbits, and through an arc-by-arc estimation of the C-22 and S-22 coefficients, we find from analysis of independent SLR residuals and other tests that we achieve 1.1-1.2 cm radial orbit accuracies for SARAL. The limiting errors stem from the inadequacy of the DPOD2008 and SLRF2008 station complements, and inadequacies in radiation force modeling, especially with respect to spacecraft self-shadowing and modeling of thermal variations due to eclipses. (C) 2015 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Zelensky, Nikita P.; Lemoine, Frank G.; Chinn, Douglas S.; Beckley, Brian D.; Bordyugov, Oleg; Yang, Xu; Wimert, Jesse; Pavlis, Despina] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Code 698, Greenbelt, MD 20771 USA.
[Zelensky, Nikita P.; Chinn, Douglas S.; Beckley, Brian D.; Bordyugov, Oleg; Yang, Xu; Wimert, Jesse; Pavlis, Despina] SGT Inc, 7701 Greenbelt Rd, Greenbelt, MD 20770 USA.
RP Zelensky, NP (reprint author), SGT Inc, 7701 Greenbelt Rd, Greenbelt, MD 20770 USA.
EM nzelensky@sgt-inc.com
FU International DORIS Service (IDS); International Laser Ranging Service
(ILRS); U.S. National Aeronautics and Space Administration (NASA) under
MEASURES (Making Earth System data records for use in Research
Environments) program
FX We acknowledge the International DORIS Service (IDS) and International
Laser Ranging Service (ILRS) for their support and leadership in
providing DORIS and Satellite Laser Ranging data (Willis et al., 2010;
Pearlman et al., 2002), as well as the providers of SARAL satellite
information and altimeter data (Vernon et al., 2015). We thank David
Rowlands (NASA/GSFC) for the valuable discussions and comments, and the
three anonymous reviewers for the very useful comments. This research
was supported by the U.S. National Aeronautics and Space Administration
(NASA) under the auspices of the MEASURES (Making Earth System data
records for use in Research Environments) program.
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PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD DEC 15
PY 2016
VL 58
IS 12
BP 2651
EP 2676
DI 10.1016/j.asr.2015.12.011
PG 26
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA EF1HS
UT WOS:000390076500012
ER
PT J
AU De Lannoy, GJM
Reichle, RH
AF De Lannoy, Gabrielle J. M.
Reichle, Rolf H.
TI Assimilation of SMOS brightness temperatures or soil moisture retrievals
into a land surface model
SO HYDROLOGY AND EARTH SYSTEM SCIENCES
LA English
DT Article
ID CLIMATE REFERENCE NETWORK; RADIATIVE-TRANSFER MODEL; L-BAND;
HIGH-RESOLUTION; NONFROZEN LAND; PRECIPITATION; CALIBRATION; FIELDS
AB Three different data products from the Soil Moisture Ocean Salinity (SMOS) mission are assimilated separately into the Goddard Earth Observing System Model, version 5 (GEOS-5) to improve estimates of surface and root-zone soil moisture. The first product consists of multi-angle, dual-polarization brightness temperature (Tb) observations at the bottom of the atmosphere extracted from Level 1 data. The second product is a derived SMOS Tb product that mimics the data at a 40 degrees incidence angle from the Soil Moisture Active Passive (SMAP) mission. The third product is the operational SMOS Level 2 surface soil moisture (SM) retrieval product. The assimilation system uses a spatially distributed ensemble Kalman filter (EnKF) with seasonally varying climatological bias mitigation for Tb assimilation, whereas a time-invariant cumulative density function matching is used for SM retrieval assimilation. All assimilation experiments improve the soil moisture estimates compared to model-only simulations in terms of unbiased root-mean-square differences and anomaly correlations during the period from 1 July 2010 to 1 May 2015 and for 187 sites across the US. Especially in areas where the satellite data are most sensitive to surface soil moisture, large skill improvements (e.g., an increase in the anomaly correlation by 0.1) are found in the surface soil moisture. The domain-average surface and root-zone skill metrics are similar among the various assimilation experiments, but large differences in skill are found locally. The observation-minus-forecast residuals and analysis increments reveal large differences in how the observations add value in the Tb and SM retrieval assimilation systems. The distinct patterns of these diagnostics in the two systems reflect observation and model errors patterns that are not well captured in the assigned EnKF error parameters. Consequently, a localized optimization of the EnKF error parameters is needed to further improve Tb or SM retrieval assimilation.
C1 [De Lannoy, Gabrielle J. M.] Katholieke Univ Leuven, Dept Earth & Environm Sci, Heverlee, Belgium.
[Reichle, Rolf H.] NASA Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD USA.
RP De Lannoy, GJM (reprint author), Katholieke Univ Leuven, Dept Earth & Environm Sci, Heverlee, Belgium.
EM gabrielle.delannoy@kuleuven.be
RI Reichle, Rolf/E-1419-2012
FU NASA Soil Moisture Active Passive (SMAP) mission
FX The NASA Soil Moisture Active Passive (SMAP) mission supported this
study. The NASA Center for Climate Simulation (NCCS) at the Goddard
Space Flight Center provided computational resources through the NASA
High-End Computing (HEC) program. The authors thank the editors and
reviewers for their input.
NR 49
TC 0
Z9 0
U1 15
U2 15
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1027-5606
EI 1607-7938
J9 HYDROL EARTH SYST SC
JI Hydrol. Earth Syst. Sci.
PD DEC 15
PY 2016
VL 20
IS 12
BP 4895
EP 4911
DI 10.5194/hess-20-4895-2016
PG 17
WC Geosciences, Multidisciplinary; Water Resources
SC Geology; Water Resources
GA EF6IM
UT WOS:000390434500001
ER
PT J
AU Matheou, G
Dimotakis, PE
AF Matheou, Georgios
Dimotakis, Paul E.
TI Scalar excursions in large-eddy simulations
SO JOURNAL OF COMPUTATIONAL PHYSICS
LA English
DT Article
DE Large eddy simulation; Numerical methods; Numerical model error; Scalar
mixing; Turbulent mixing
ID ATMOSPHERIC BOUNDARY-LAYER; FINITE-DIFFERENCE SCHEMES; TURBULENT CHANNEL
FLOW; STRETCHED-VORTEX MODEL; SUBGRID-STRESS MODEL; NUMERICAL ERRORS;
UPSTREAM INTERPOLATION; INCOMPRESSIBLE-FLOW; MIXING TRANSITION;
DISSIPATION
AB The range of values of scalar fields in turbulent flows is bounded by their boundary values, for passive scalars, and by a combination of boundary values, reaction rates, phase changes, etc., for active scalars. The current investigation focuses on the local conservation of passive scalar concentration fields and the ability of the large-eddy simulation (LES) method to observe the boundedness of passive scalar concentrations. In practice, as a result of numerical artifacts, this fundamental constraint is often violated with scalars exhibiting unphysical excursions. The present study characterizes passive-scalar excursions in LES of a shear flow and examines methods for diagnosis and assesment of the problem. The analysis of scalar-excursion statistics provides support of the main hypothesis of the current study that unphysical scalar excursions in LES result from dispersive errors of the convection-term discretization where the subgrid-scale model (SGS) provides insufficient dissipation to produce a sufficiently smooth scalar field. In the LES runs three parameters are varied: the discretization of the convection terms, the SGS model, and grid resolution. Unphysical scalar excursions decrease as the order of accuracy of non-dissipative schemes is increased, but the improvement rate decreases with increasing order of accuracy. Two SGS models are examined, the stretched-vortex and a constant-coefficient Smagorinsky. Scalar excursions strongly depend on the SGS model. The excursions are significantly reduced when the characteristic SGS scale is set to double the grid spacing in runs with the stretched-vortex model. The maximum excursion and volume fraction of excursions outside boundary values show opposite trends with respect to resolution. The maximum unphysical excursions increase as resolution increases, whereas the volume fraction decreases. The reason for the increase in the maximum excursion is statistical and traceable to the number of grid points (sample size) which increases with resolution. In contrast, the volume fraction of unphysical excursions decreases with resolution because the SGS models explored perform better at higher grid resolution. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Matheou, Georgios] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Matheou, Georgios; Dimotakis, Paul E.] CALTECH, Grad Aerosp Labs, Pasadena, CA 91125 USA.
RP Matheou, G (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.; Matheou, G (reprint author), CALTECH, Grad Aerosp Labs, Pasadena, CA 91125 USA.
EM georgios.matheou@jpl.nasa.gov
FU AFOSR [FA9550-12-1-0461]; DOE [DE-NA0002382]; John K. Northrop Chair of
the California Institute of Technology
FX This work was supported by AFOSR Grant No. FA9550-12-1-0461, DOE Grant
No. DE-NA0002382, and the John K. Northrop Chair of the California
Institute of Technology. The authors would also like to acknowledge
discussions and collaborations with Prof. G. Candler and his research
group at the University of Minnesota, and Prof. D. Meiron and Prof. D.
Pullin at Caltech. We would like to thank Dr. D. Chung (University of
Melbourne) for making available the spectral code used in this study.
This research was carried out at the California Institute of Technology
and the Jet Propulsion Laboratory, California Institute of Technology,
the latter under a contract with the National Aeronautics and Space
Administration.
NR 68
TC 0
Z9 0
U1 6
U2 6
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0021-9991
EI 1090-2716
J9 J COMPUT PHYS
JI J. Comput. Phys.
PD DEC 15
PY 2016
VL 327
BP 97
EP 120
DI 10.1016/j.jcp.2016.08.035
PG 24
WC Computer Science, Interdisciplinary Applications; Physics, Mathematical
SC Computer Science; Physics
GA DZ7TH
UT WOS:000386069200005
ER
PT J
AU Yang, WD
Marshak, A
McBride, PJ
Chiu, JC
Knyazikhin, Y
Schmidt, KS
Flynn, C
Lewis, ER
Eloranta, EW
AF Yang, Weidong
Marshak, Alexander
McBride, Patrick J.
Chiu, J. Christine
Knyazikhin, Yuri
Schmidt, K. Sebastian
Flynn, Connor
Lewis, Ernie R.
Eloranta, Edwin W.
TI Observation of the spectrally invariant properties of clouds in
cloudy-to-clear transition zones during the MAGIC field campaign
SO ATMOSPHERIC RESEARCH
LA English
DT Article
DE Transition zone; Cloud; Cloud-aerosol interaction; Air entrainment and
mixing; Spectral invariance; MAGIC field campaign
ID TRADE-WIND CUMULUS; RADIATIVE-TRANSFER; OPTICAL-THICKNESS; ZENITH
RADIANCE; ENTRAINMENT; HUMIDITY; MODEL
AB We use the spectrally invariant method to study the variability of cloud optical thickness tau and droplet effective radius r(eff) in transition zones (between the cloudy and clear sky columns) observed from Solar Spectral Flux Radiometer (SSFR) and Shortwave Array Spectroradiometer-Zenith (SASZe) during the Marine ARM GPCI Investigation of Clouds (MAGIC) field campaign. The measurements from the SSFR and the SASZe are different, however inter-instrument differences of self-normalized measurements (divided by their own spectra at a fixed time) are small. The spectrally invariant method approximates the spectra in the cloud transition zone as a linear combination of definitely clear and cloudy spectra, where the coefficients, slope and intercept, characterize the spectrally invariant properties of the transition zone. Simulation results from the SBDART (Santa Barbara DISORT Atmospheric Radiative Transfer) model demonstrate that (1) the slope of the visible band is positively correlated with the cloud optical thickness tau while the intercept of the near-infrared band has high negative correlation with the cloud drop effective radius r(eff) even without the exact knowledge of tau; (2) the above relations hold for all Solar Zenith Angle (SZA) and for cloud-contaminated skies. In observations using redundant measurements from SSFR and SASZe, we find that during cloudy-to-clear transitions, (a) the slopes of the visible band decrease, and (b) the intercepts of the near-infrared band remain almost constant near cloud edges. The finding in simulations and observations suggest that, while the optical thickness decreases during the cloudy-to-clear transition, the cloud drop effective radius does not change when cloud edges are approached. These results support the hypothesis that inhomogeneous mixing dominates near cloud edges in the studied cases. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Yang, Weidong; Marshak, Alexander] NASA, Goddard Space Flight Ctr, Climate & Radiat Branch, Code 661, Greenbelt, MD 20771 USA.
[Yang, Weidong] Univ Space Res Assoc, Columbia, MD USA.
[McBride, Patrick J.] ASTRA, Boulder, CO USA.
[Chiu, J. Christine] Univ Reading, Dept Meteorol, Reading, Berks, England.
[Knyazikhin, Yuri] Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA.
[Schmidt, K. Sebastian] Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
[Flynn, Connor] Pacific Northwest Natl Lab, POB 999,MSIN K4-28, Richland, WA 99352 USA.
[Lewis, Ernie R.] Brookhaven Natl Lab, Environm & Climate Sci Dept, Upton, NY 11973 USA.
[Eloranta, Edwin W.] Univ Wisconsin, Space Sci & Engn Ctr, Madison, WI USA.
RP Yang, WD (reprint author), NASA, Goddard Space Flight Ctr, Climate & Radiat Branch, Code 661, Greenbelt, MD 20771 USA.
EM weidong.yang@nasa.gov
RI Chiu, Christine/E-5649-2013; Marshak, Alexander/D-5671-2012;
OI Chiu, Christine/0000-0002-8951-6913; SCHMIDT, KONRAD
SEBASTIAN/0000-0003-3899-228X
FU Office of Science (BER), U.S. Department of Energy (DOE) [DE-SC0005457,
DE-SC0011666]; U.S. Department of Energy's Atmospheric System Research
Program (Office of Science, BER) [DE-SC00112704]; Horizon Lines; Captain
and crew of the Horizon Spirit
FX This research was supported by the Office of Science (BER), U.S.
Department of Energy (DOE), under grant DE-SC0005457. J. C. Chiu was
supported by the Office of Science (BER), U.S. Department of Energy
(DOE) under grant DE-SC0011666. E. Lewis was supported by the U.S.
Department of Energy's Atmospheric System Research Program (Office of
Science, BER) under Contract No. DE-SC00112704. Thanks to Warren Gore of
NASA Ames Research Center for his support of the SSFR during MAGIC. We
thank Horizon Lines and the Captain and crew of the Horizon Spirit for
their support and hospitality during MAGIC. We would also like to thank
David Troyan and Tami Toto for ship movement correction; and Laurie
Gregory, Richard Wagener and Cimel Electronique for their help with
deploying the Cimel sun photometer on the ship. The MAGIC data can be
found at http://www.arm.gov/campaigns/amf2012magic.
NR 35
TC 0
Z9 0
U1 9
U2 9
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0169-8095
EI 1873-2895
J9 ATMOS RES
JI Atmos. Res.
PD DEC 15
PY 2016
VL 182
BP 294
EP 301
DI 10.1016/j.atmosres.2016.08.004
PG 8
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DY1QG
UT WOS:000384868900025
ER
PT J
AU Kazadzis, S
Raptis, P
Kouremeti, N
Amiridis, V
Arola, A
Gerasopoulos, E
Schuster, GL
AF Kazadzis, Stelios
Raptis, Panagiotis
Kouremeti, Natalia
Amiridis, Vassilis
Arola, Antti
Gerasopoulos, Evangelos
Schuster, Gregory L.
TI Aerosol absorption retrieval at ultraviolet wavelengths in a complex
environment
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID SINGLE SCATTERING ALBEDO; SURFACE UV IRRADIANCE; LIGHT-ABSORPTION;
PHOTOCHEMICAL SMOG; OPTICAL-PROPERTIES; ORGANIC-CARBON; GROUND ALBEDO;
MEXICO-CITY; DESERT DUST; RADIATION
AB We have used total and diffuse UV irradiance measurements from a multi-filter rotating shadow-band radiometer (UVMFR) in order to investigate aerosol absorption in the UV range for a 5-year period in Athens, Greece. This dataset was used as input to a radiative transfer model and the single scattering albedo (SSA) at 368 and 332 nm was calculated. Retrievals from a collocated CIMEL sun photometer were used to evaluate the products and study the absorption spectral behavior of retrieved SSA values. The UVMFR SSA, together with synchronous, CIMEL-derived retrievals of SSA at 440 nm, had a mean of 0.90, 0.87 and 0.83, with lowest values (higher absorption) encountered at the shorter wavelengths. In addition, noticeable diurnal variation of the SSA in all wavelengths is shown, with amplitudes up to 0.05. Strong SSA wavelength dependence is revealed for cases of low Angstrom exponents, accompanied by a SSA decrease with decreasing extinction optical depth, suggesting varying influence under different aerosol composition. However, part of this dependence for low aerosol optical depths is masked by the enhanced SSA retrieval uncertainty. Dust and brown carbon UV absorbing properties were also investigated to explain seasonal patterns.
C1 [Kazadzis, Stelios; Kouremeti, Natalia] WRC, PMOD, Dorfstr 33, CH-7260 Davos, Switzerland.
[Kazadzis, Stelios; Raptis, Panagiotis; Gerasopoulos, Evangelos] Natl Observ Athens, Inst Environm Res & Sustainable Dev, Athens, Greece.
[Amiridis, Vassilis] Natl Observ Athens, Inst Astron Astrophys Space Applicat & Remote Sen, Athens, Greece.
[Arola, Antti] Finnish Meteorol Inst, Kuopio Unit, Kuopio, Finland.
[Schuster, Gregory L.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Kazadzis, S (reprint author), WRC, PMOD, Dorfstr 33, CH-7260 Davos, Switzerland.; Kazadzis, S (reprint author), Natl Observ Athens, Inst Environm Res & Sustainable Dev, Athens, Greece.
EM stelios.kazadzis@pmodwrc.ch
OI Arola, Antti/0000-0002-9220-0194
FU project "European Union's Horizon 2020 Research and Innovation Programme
ACTRIS-2" [654109]
FX Panagiotis Raptis would like to acknowledge the project Aristotelis
SOLAR (50561), "Investigation on the factors affecting the solar
radiation field in Greece". Vassilis Amiridis, Stelios Kazadzis and
Evangelos Gerasopoulos would like to acknowledge the project "European
Union's Horizon 2020 Research and Innovation Programme ACTRIS-2" (grant
agreement no. 654109).
NR 76
TC 1
Z9 1
U1 5
U2 5
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1867-1381
EI 1867-8548
J9 ATMOS MEAS TECH
JI Atmos. Meas. Tech.
PD DEC 13
PY 2016
VL 9
IS 12
BP 5997
EP 6011
DI 10.5194/amt-9-5997-2016
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EG8BC
UT WOS:000391279600003
ER
PT J
AU Saunois, M
Bousquet, P
Poulter, B
Peregon, A
Ciais, P
Canadell, JG
Dlugokencky, EJ
Etiope, G
Bastviken, D
Houweling, S
Janssens-Maenhout, G
Tubiello, FN
Castaldi, S
Jackson, RB
Alexe, M
Arora, VK
Beerling, DJ
Bergamaschi, P
Blake, DR
Brailsford, G
Brovkin, V
Bruhwiler, L
Crevoisier, C
Crill, P
Covey, K
Curry, C
Frankenberg, C
Gedney, N
Hoglund-Isaksson, L
Ishizawa, M
Ito, A
Joos, F
Kim, HS
Kleinen, T
Krummel, P
Lamarque, JF
Langenfelds, R
Locatelli, R
Machida, T
Maksyutov, S
McDonald, KC
Marshall, J
Melton, JR
Morino, I
Naik, V
O'Doherty, S
Parmentier, FJW
Patra, PK
Peng, CH
Peng, SS
Peters, GP
Pison, I
Prigent, C
Prinn, R
Ramonet, M
Riley, WJ
Saito, M
Santini, M
Schroeder, R
Simpson, IJ
Spahni, R
Steele, P
Takizawa, A
Thornton, BF
Tian, HQ
Tohjima, Y
Viovy, N
Voulgarakis, A
van Weele, M
van der Werf, GR
Weiss, R
Wiedinmyer, C
Wilton, DJ
Wiltshire, A
Worthy, D
Wunch, D
Xu, XY
Yoshida, Y
Zhang, B
Zhang, Z
Zhu, Q
AF Saunois, Marielle
Bousquet, Philippe
Poulter, Ben
Peregon, Anna
Ciais, Philippe
Canadell, Josep G.
Dlugokencky, Edward J.
Etiope, Giuseppe
Bastviken, David
Houweling, Sander
Janssens-Maenhout, Greet
Tubiello, Francesco N.
Castaldi, Simona
Jackson, Robert B.
Alexe, Mihai
Arora, Vivek K.
Beerling, David J.
Bergamaschi, Peter
Blake, Donald R.
Brailsford, Gordon
Brovkin, Victor
Bruhwiler, Lori
Crevoisier, Cyril
Crill, Patrick
Covey, Kristofer
Curry, Charles
Frankenberg, Christian
Gedney, Nicola
Hoeglund-Isaksson, Lena
Ishizawa, Misa
Ito, Akihiko
Joos, Fortunat
Kim, Heon-Sook
Kleinen, Thomas
Krummel, Paul
Lamarque, Jean-Francois
Langenfelds, Ray
Locatelli, Robin
Machida, Toshinobu
Maksyutov, Shamil
McDonald, Kyle C.
Marshall, Julia
Melton, Joe R.
Morino, Isamu
Naik, Vaishali
O'Doherty, Simon
Parmentier, Frans-Jan W.
Patra, Prabir K.
Peng, Changhui
Peng, Shushi
Peters, Glen P.
Pison, Isabelle
Prigent, Catherine
Prinn, Ronald
Ramonet, Michel
Riley, William J.
Saito, Makoto
Santini, Monia
Schroeder, Ronny
Simpson, Isobel J.
Spahni, Renato
Steele, Paul
Takizawa, Atsushi
Thornton, Brett F.
Tian, Hanqin
Tohjima, Yasunori
Viovy, Nicolas
Voulgarakis, Apostolos
van Weele, Michiel
van der Werf, Guido R.
Weiss, Ray
Wiedinmyer, Christine
Wilton, David J.
Wiltshire, Andy
Worthy, Doug
Wunch, Debra
Xu, Xiyan
Yoshida, Yukio
Zhang, Bowen
Zhang, Zhen
Zhu, Qiuan
TI The global methane budget 2000-2012
SO EARTH SYSTEM SCIENCE DATA
LA English
DT Article
ID PROCESS-BASED MODEL; INTERCOMPARISON PROJECT ACCMIP; ATMOSPHERIC
HYDROXYL RADICALS; BIOMASS BURNING EMISSIONS; GREENHOUSE-GAS EMISSIONS;
PAST 2 DECADES; NATURAL-GAS; TRACE GASES; TROPOSPHERIC METHANE; ISOTOPIC
COMPOSITION
AB The global methane (CH4) budget is becoming an increasingly important component for managing realistic pathways to mitigate climate change. This relevance, due to a shorter atmospheric lifetime and a stronger warming potential than carbon dioxide, is challenged by the still unexplained changes of atmospheric CH4 over the past decade. Emissions and concentrations of CH4 are continuing to increase, making CH4 the second most important human-induced greenhouse gas after carbon dioxide. Two major difficulties in reducing uncertainties come from the large variety of diffusive CH4 sources that overlap geographically, and from the destruction of CH4 by the very short-lived hydroxyl radical (OH). To address these difficulties, we have established a consortium of multi-disciplinary scientists under the umbrella of the Global Carbon Project to synthesize and stimulate research on the methane cycle, and producing regular (similar to biennial) updates of the global methane budget. This consortium includes atmospheric physicists and chemists, biogeochemists of surface and marine emissions, and socio-economists who study anthropogenic emissions. Following Kirschke et al. (2013), we propose here the first version of a living review paper that integrates results of top-down studies (exploiting atmospheric observations within an atmospheric inverse-modelling framework) and bottom-up models, inventories and data-driven approaches (including process-based models for estimating land surface emissions and atmospheric chemistry, and inventories for anthropogenic emissions, data-driven extrapolations).
For the 2003-2012 decade, global methane emissions are estimated by top-down inversions at 558 TgCH(4) yr(-1), range 540-568. About 60% of global emissions are anthropogenic (range 50-65 %). Since 2010, the bottom-up global emission inventories have been closer to methane emissions in the most carbon-intensive Representative Concentrations Pathway (RCP8.5) and higher than all other RCP scenarios. Bottom-up approaches suggest larger global emissions (736 TgCH(4) yr(-1), range 596-884) mostly because of larger natural emissions from individual sources such as inland waters, natural wetlands and geological sources. Considering the atmospheric constraints on the top-down budget, it is likely that some of the individual emissions reported by the bottom-up approaches are overestimated, leading to too large global emissions. Latitudinal data from top-down emissions indicate a predominance of tropical emissions (similar to 64% of the global budget, <30 degrees N) as compared to mid (similar to 32 %, 30-60 degrees N) and high northern latitudes (similar to 4 %, 60-90 degrees N). Top-down inversions consistently infer lower emissions in China (similar to 58 TgCH(4) yr(-1), range 51-72, -14 %) and higher emissions in Africa (86 TgCH(4) yr(-1), range 73-108, + 19 %) than bottom-up values used as prior estimates. Overall, uncertainties for anthropogenic emissions appear smaller than those from natural sources, and the uncertainties on source categories appear larger for top-down inversions than for bottom-up inventories and models.
The most important source of uncertainty on the methane budget is attributable to emissions from wetland and other inland waters. We show that the wetland extent could contribute 30-40% on the estimated range for wetland emissions. Other priorities for improving the methane budget include the following: (i) the development of process-based models for inland-water emissions, (ii) the intensification of methane observations at local scale (flux measurements) to constrain bottom-up land surface models, and at regional scale (surface networks and satellites) to constrain top-down inversions, (iii) improvements in the estimation of atmospheric loss by OH, and (iv) improvements of the transport models integrated in top-down inversions. The data presented here can be downloaded from the Carbon Dioxide Information Analysis Center (http://doi.org/10.3334/CDIAC/GLOBAL_METHANE_BUDGET_2016_V1.1) and the Global Carbon Project.
C1 [Saunois, Marielle; Bousquet, Philippe; Peregon, Anna; Ciais, Philippe; Locatelli, Robin; Peng, Shushi; Pison, Isabelle; Ramonet, Michel; Viovy, Nicolas] Univ Paris Saclay, LSCE IPSL CEA CNRS UVSQ, Lab Sci Climat & Environm, F-91191 Gif Sur Yvette, France.
[Poulter, Ben; Zhang, Zhen] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Canadell, Josep G.] CSIRO Oceans & Atmosphere, Global Carbon Project, Canberra, ACT 2601, Australia.
[Dlugokencky, Edward J.; Bruhwiler, Lori] NOAA ESRL, 325 Broadway, Boulder, CO 80305 USA.
[Etiope, Giuseppe] Ist Nazl Geofis & Vulcanol, Sez Roma 2, Via V Murata 605, I-00143 Rome, Italy.
[Bastviken, David] Linkoping Univ, Dept Themat Studies Environm Change, S-58183 Linkoping, Sweden.
[Houweling, Sander] SRON, Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands.
[Houweling, Sander] Inst Marine & Atmospher Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands.
[Janssens-Maenhout, Greet; Alexe, Mihai; Bergamaschi, Peter] European Commiss Joint Res Ctr, Ispra, VA, Italy.
[Tubiello, Francesco N.] Food & Agr Org United Nations FAO, Stat Div, Viale Terme Caracalla, I-00153 Rome, Italy.
[Castaldi, Simona] Seconda Univ Napoli, Dipartimento Sci Ambientali Biol & Farmaceut, Via Vivaldi 43, I-81100 Caserta, Italy.
[Castaldi, Simona] FEFU, Vladivostok, Russky Island, Russia.
[Castaldi, Simona; Santini, Monia] Euromediterranean Ctr Climate Change, Via Augusto Imperatore 16, I-73100 Lecce, Italy.
[Jackson, Robert B.] Stanford Univ, Sch Earth Energy & Environm Sci, Stanford, CA 94305 USA.
[Arora, Vivek K.] Environm & Climate Change Canada, Div Climate Res, Canadian Ctr Climate Modelling & Anal, Victoria, BC V8W 2Y2, Canada.
[Beerling, David J.; Wilton, David J.] Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England.
[Blake, Donald R.; Simpson, Isobel J.] Univ Calif Irvine, Dept Chem, 570 Rowland Hall, Irvine, CA 92697 USA.
[Brailsford, Gordon] Natl Inst Water & Atmospher Res, 301 Evans Bay Parade, Wellington, New Zealand.
[Brovkin, Victor; Kleinen, Thomas] Max Planck Inst Meteorol, Bundesstr 53, D-20146 Hamburg, Germany.
[Crevoisier, Cyril] Ecole Polytech, LMD IPSL, Meteorol Dynam Lab, F-91120 Palaiseau, France.
Dept Geol Sci, Svante Arrhenius Vag 8, S-10691 Stockholm, Sweden.
[Crill, Patrick; Thornton, Brett F.] Bolin Ctr Climate Res, Svante Arrhenius Vag 8, S-10691 Stockholm, Sweden.
[Covey, Kristofer] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA.
[Curry, Charles] Univ Victoria, Sch Earth & Ocean Sci, POB 1700 STN CSC, Victoria, BC V8W 2Y2, Canada.
[Frankenberg, Christian] Jet Prop Lab, M-S 183-601,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Gedney, Nicola; Morino, Isamu] Joint Ctr Hydrometeorol Res, Met Off Hadley Ctr, Maclean Bldg, Wallingford OX10 8BB, Oxon, England.
[Hoeglund-Isaksson, Lena] Int Inst Appl Syst Anal, Air Qual & Greenhouse Gases Program AIR, A-2361 Laxenburg, Austria.
Natl Inst Environm Studies, Ctr Global Environm Res, Onogawa 16-2, Tsukuba, Ibaraki 3058506, Japan.
[Joos, Fortunat; Spahni, Renato] Univ Bern, Inst Phys, Climate & Environm Phys, Sidlerstr 5, CH-3012 Bern, Switzerland.
[Joos, Fortunat; Spahni, Renato] Univ Bern, Oeschger Ctr Climate Change Res, Sidlerstr 5, CH-3012 Bern, Switzerland.
[Krummel, Paul; Langenfelds, Ray; Steele, Paul] CSIRO, Oceans & Atmosphere, Aspendale, Vic 3195, Australia.
[Lamarque, Jean-Francois; Wiedinmyer, Christine] NCAR, POB 3000, Boulder, CO 80307 USA.
[McDonald, Kyle C.; Schroeder, Ronny] CUNY, Dept Earth & Atmospher Sci, New York, NY 10031 USA.
[Marshall, Julia] Max Planck Inst Biogeochem, Hans Knoll Str 10, D-07745 Jena, Germany.
[Melton, Joe R.] Environm & Climate Change Canada, Div Climate Res, Victoria, BC V8W 2Y2, Canada.
[Naik, Vaishali] NOAA, GFDL, 201 Forrestal Rd, Princeton, NJ 08540 USA.
[O'Doherty, Simon] Univ Bristol, Sch Chem, Cantocks Close, Bristol BS8 1TS, Avon, England.
[Parmentier, Frans-Jan W.] Lund Univ, Dept Phys Geog & Ecosyst Sci, Solvegatan 12, S-22362 Lund, Sweden.
[Patra, Prabir K.] JAMSTEC, Dept Environm Geochem Cycle Res, Kanazawa Ku, 3173-25 Showa Machi, Yokohama, Kanagawa 2360001, Japan.
[Peng, Changhui] Univ Quebec, Inst Environm Sci, Dept Biol Sci, Montreal, PQ H3C 3P8, Canada.
[Peters, Glen P.] CICERO, Pb 1129 Blindern, N-0318 Oslo, Norway.
[Prigent, Catherine] Observ Paris, CNRS, LERMA, 61 Ave Observ, F-75014 Paris, France.
[Prinn, Ronald] MIT, Dept Earth Atmospher & Planetary Sci, Bldg 54-1312, Cambridge, MA 02139 USA.
[Riley, William J.; Xu, Xiyan] Lawrence Berkeley Natl Lab, Div Earth Sci, 1 Cyclotron Rd, Berkeley, CA 94720 USA.
[Schroeder, Ronny] Univ Hohenheim, Inst Bot, D-70593 Stuttgart, Germany.
[Takizawa, Atsushi] JMA, Chiyoda Ku, 1-3-4 Otemachi, Tokyo 1008122, Japan.
[Tian, Hanqin; Zhang, Bowen] Auburn Univ, Sch Forestry & Wildlife Sci, Int Ctr Climate & Global Change Res, 602 Duncan Dr, Auburn, AL 36849 USA.
[Voulgarakis, Apostolos] Imperial Coll London, Blackett Lab, Space & Atmospher Phys, London SW7 2AZ, England.
[van Weele, Michiel] KNMI, POB 201, NL-3730 AE De Bilt, Netherlands.
[van der Werf, Guido R.] Vrije Univ Amsterdam, Earth & Climate Cluster, Fac Earth & Life Sci, Amsterdam, Netherlands.
[Weiss, Ray] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
[Wiltshire, Andy] Met Off Hadley Ctr, FitzRoy Rd, Exeter EX1 3PB, Devon, England.
[Worthy, Doug] Environm Canada, 4905 Rue Dufferin, Toronto, ON, Canada.
[Wunch, Debra] Univ Toronto, Dept Phys, 60 St George St, Toronto, ON, Canada.
[Zhang, Zhen] Swiss Fed Res Inst WSL, CH-8059 Birmensdorf, Switzerland.
[Zhu, Qiuan] Northwest A&F Univ, State Key Lab Soil Eros & Dryland Farming Loess P, Yangling 712100, Shaanxi, Peoples R China.
RP Saunois, M (reprint author), Univ Paris Saclay, LSCE IPSL CEA CNRS UVSQ, Lab Sci Climat & Environm, F-91191 Gif Sur Yvette, France.
EM marielle.saunois@lsce.ipsl.fr
RI Parmentier, Frans-Jan/D-9022-2013; Canadell, Josep/E-9419-2010; Brovkin,
Victor/C-2803-2016; Frankenberg, Christian/A-2944-2013; Morino,
Isamu/K-1033-2014; Langenfelds, Raymond/B-5381-2012; Peng,
Shushi/J-4779-2014; Patra, Prabir/B-5206-2009; Maksyutov,
Shamil/G-6494-2011;
OI Parmentier, Frans-Jan/0000-0003-2952-7706; Canadell,
Josep/0000-0002-8788-3218; Brovkin, Victor/0000-0001-6420-3198;
Frankenberg, Christian/0000-0002-0546-5857; Morino,
Isamu/0000-0003-2720-1569; Peng, Shushi/0000-0001-5098-726X; Patra,
Prabir/0000-0001-5700-9389; Maksyutov, Shamil/0000-0002-1200-9577;
Marshall, Julia/0000-0003-2648-128X
FU Swiss National Science Foundation; NASA [NNX14AF93G, NNX14AO73G];
National Environmental Science Program - Earth Systems and Climate
Change Hub; European Commission [283576, 633080]; ESA Climate Change
Initiative Greenhouse Gases Phase 2 project; US Department of Energy,
BER [DE-AC02-05CH11231]; FAO member countries; Environment Research and
Technology Development Fund of the Ministry of the Environment, Japan
[2-1502]; ERC [322998]; NERC [NE/J00748X/1]; Swedish Research Council
VR; Research Council of Norway [244074]; NSF [1243232, 1243220];
National Science and Engineering Research Council of Canada (NSERC);
China's QianRen Program; CSIRO Australia; Australian Bureau of
Meteorology; Australian Institute of Marine Science; Australian
Antarctic Division; NOAA USA; Meteorological Service of Canada; National
Aeronautic and Space Administration (NASA) [NAG5-12669, NNX07AE89G,
NNX11AF17G, NNX07AE87G, NNX07AF09G, NNX11AF15G, NNX11AF16G]; Department
of Energy and Climate Change (DECC, UK) [GA01081]; Commonwealth
Scientific and Industrial Research Organization (CSIRO Australia);
Bureau of Meteorology (Australia); Joint DECC/Defra Met Office Hadley
Centre Climate Programme [GA01101]
FX This collaborative international effort is part of the Global Carbon
Project activity to establish and track greenhouse gas budgets and their
trends. Fortunat Joos and Renato Spahni acknowledge support by the Swiss
National Science Foundation. Heon-Sook Kim and Shamil Maksyutov
acknowledge use of the GOSAT Research Computation Facility. Donald R.
Blake and Isobel J. Simpson (UCI) acknowledge funding support from NASA.
Josep G. Canadell thanks the support from the National Environmental
Science Program - Earth Systems and Climate Change Hub. Marielle Saunois
and Philippe Bousquet acknowledge the Global Carbon Project for the
scientific advice and the computing power of LSCE for data analyses.
Peter Bergamaschi and Mihai Alexe acknowledge the support by the
European Commission Seventh Framework Programme (FP7/2007-2013) project
MACC-II under grant agreement 283576, by the European Commission
Horizon2020 Programme project MACC-III under grant agreement 633080, and
by the ESA Climate Change Initiative Greenhouse Gases Phase 2 project.
William J. Riley and Xiyan Xu acknowledge support by the US Department
of Energy, BER, under contract no. DE-AC02-05CH11231. The FAOSTAT
database is supported by regular programme funding from all FAO member
countries. Prabir K. Patra is supported by the Environment Research and
Technology Development Fund (2-1502) of the Ministry of the Environment,
Japan. David J. Beerling acknowledges support from an ERC Advanced grant
(CDREG, 322998) and NERC (NE/J00748X/1). David Bastviken and Patrick
Crill acknowledge support from the Swedish Research Council VR. Glen P.
Peters acknowledges the support of the Research Council of Norway
project 244074. Hanqin Tian and Bowen Zhang acknowledge funding support
from NASA (NNX14AF93G; NNX14AO73G) and NSF (1243232; 1243220). Changhui
Peng acknowledges the support by National Science and Engineering
Research Council of Canada (NSERC) discovery grant and China's QianRen
Program. The CSIRO and the Australian Government Bureau of Meteorology
are thanked for their ongoing long-term support of the Cape Grim station
and the Cape Grim science programme. The CSIRO flask network is
supported by CSIRO Australia, Australian Bureau of Meteorology,
Australian Institute of Marine Science, Australian Antarctic Division,
NOAA USA, and the Meteorological Service of Canada. The operation of the
AGAGE instruments at Mace Head, Trinidad Head, Cape Matatula, Ragged
Point, and Cape Grim is supported by the National Aeronautic and Space
Administration (NASA) (grants NAG5-12669, NNX07AE89G, and NNX11AF17G to
MIT and grants NNX07AE87G, NNX07AF09G, NNX11AF15G, and NNX11AF16G to
SIO), the Department of Energy and Climate Change (DECC, UK) contract
GA01081 to theUniversity of Bristol, and the Commonwealth Scientific and
Industrial Research Organization (CSIRO Australia), and Bureau of
Meteorology (Australia). Nicola Gedney and Andy Wiltshire acknowledge
support by the Joint DECC/Defra Met Office Hadley Centre Climate
Programme (GA01101).
NR 360
TC 4
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U1 78
U2 78
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1866-3508
EI 1866-3516
J9 EARTH SYST SCI DATA
JI Earth Syst. Sci. Data
PD DEC 12
PY 2016
VL 8
IS 2
BP 697
EP 751
DI 10.5194/essd-8-697-2016
PG 55
WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences
SC Geology; Meteorology & Atmospheric Sciences
GA EF2HL
UT WOS:000390145300001
ER
PT J
AU Isella, A
Guidi, G
Testi, L
Liu, SF
Li, H
Li, ST
Weaver, E
Boehler, Y
Carperter, JM
De Gregorio-Monsalvo, I
Manara, CF
Natta, A
Perez, LM
Ricci, L
Sargent, A
Tazzari, M
Turner, N
AF Isella, Andrea
Guidi, Greta
Testi, Leonardo
Liu, Shangfei
Li, Hui
Li, Shengtai
Weaver, Erik
Boehler, Yann
Carperter, John M.
De Gregorio-Monsalvo, Itziar
Manara, Carlo F.
Natta, Antonella
Perez, Laura M.
Ricci, Luca
Sargent, Anneila
Tazzari, Marco
Turner, Neal
TI Ringed Structures of the HD 163296 Protoplanetary Disk Revealed by ALMA
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID HL TAU DISK; TRANSITIONAL DISKS; ACCRETION DISKS; PLANET; GAP;
SIMULATIONS; INSTABILITY; IONIZATION; VORTICES; PREDICTIONS
AB We present Atacama Large Millimeter and Submillimeter Array observations of the protoplanetary disk around the Herbig Ae star HD 163296 that trace the spatial distribution of millimeter-sized particles and cold molecular gas on spatial scales as small as 25 astronomical units (A. U.). The image of the disk recorded in the 1.3 mm continuum emission reveals three dark concentric rings that indicate the presence of dust depleted gaps at about 60, 100, and 160 A. U. from the central star. The maps of the (CO)-C-12, (CO)-C-13, and (CO)-O-18 J = 2 - 1 emission do not show such structures but reveal a change in the slope of the radial intensity profile across the positions of the dark rings in the continuum image. By comparing the observations with theoretical models for the disk emission, we find that the density of CO molecules is reduced inside the middle and outer dust gaps. However, in the inner ring there is no evidence of CO depletion. From the measurements of the dust and gas densities, we deduce that the gas-to-dust ratio varies across the disk and, in particular, it increases by at least a factor 5 within the inner dust gap compared to adjacent regions of the disk. The depletion of both dust and gas suggests that the middle and outer rings could be due to the gravitational torque exerted by two Saturn-mass planets orbiting at 100 and 160 A. U. from the star. On the other hand, the inner dust gap could result from dust accumulation at the edge of a magnetorotational instability dead zone, or from dust opacity variations at the edge of the CO frost line. Observations of the dust emission at higher angular resolution and of molecules that probe dense gas are required to establish more precisely the origins of the dark rings observed in the HD 163296 disk.
C1 [Isella, Andrea; Liu, Shangfei; Weaver, Erik; Boehler, Yann] Rice Univ, Dept Phys & Astron, 6100 Main St,MS-108, Houston, TX 77005 USA.
[Guidi, Greta; Testi, Leonardo; Natta, Antonella] Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy.
[Testi, Leonardo; Tazzari, Marco] ESO, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Liu, Shangfei; Li, Hui; Li, Shengtai] Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA.
[Carperter, John M.; De Gregorio-Monsalvo, Itziar] Joint ALMA Observ, Alonso de Cordova 3107, Vitacura, Santiago De Chi, Chile.
[Manara, Carlo F.] European Space Res & Technol Ctr ESA ESTEC, Directorate Sci, Sci Support Off, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands.
[Natta, Antonella] Dublin Inst Adv Studies, Sch Cosm Phys, 31 Fitzwilliams Pl, Dublin 2, Ireland.
[Perez, Laura M.] Max Planck Inst Radioastron, Hgel 69, D-53121 Bonn, Germany.
[Ricci, Luca] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Sargent, Anneila] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Turner, Neal] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Isella, A (reprint author), Rice Univ, Dept Phys & Astron, 6100 Main St,MS-108, Houston, TX 77005 USA.
EM isella@rice.edu
OI Tazzari, Marco/0000-0003-3590-5814
FU NSF [AST-1535809]; National Aeronautics and Space Administration
[NNX15AB06G]; NRAO Student Observing Support Grant [AST-0836064];
Laboratory Directed Research and Development program at Los Alamos
National Laboratory
FX We thank Munetake Momose, Misato Fukagawa, and Giovanni Rosotti for the
helpful conversation. This paper makes use of the following Atacama
Large Millimeter and Submillimeter Array (ALMA) data: ADS/JAO.
ALMA#2013.1.00601. S. ALMA is a partnership of European Southern
Observatory (ESO) (representing its member states), National Science
Foundation (USA), and National Institutes of Natural Sciences (Japan),
together with National Research Council (Canada), National Science
Council and Academia Sinica Institute of Astronomy and Astrophysics
(Taiwan), and Korea Astronomy and Space Science Institute (Korea), in
cooperation with Chile. The Joint ALMA Observatory is operated by ESO,
Associated Universities, Inc/National Radio Astronomy Observatory
(NRAO), and National Astronomical Observatory of Japan. The National
Radio Astronomy Observatory is a facility of the National Science
Foundation operated under cooperative agreement by Associated
Universities, Inc. A. I. and Y.B. acknowledge support from the NSF Grant
No. AST-1535809 and the National Aeronautics and Space Administration
Grant No. NNX15AB06G. E.W. acknowledge support from the NRAO Student
Observing Support Grant No. AST-0836064. H.L. and S.L. acknowledge the
support from the Laboratory Directed Research and Development program at
Los Alamos National Laboratory. C.F.M. gratefully acknowledges an
European Space Agency Research Fellowship. Part of this research was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration.
NR 45
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U1 0
U2 0
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
EI 1079-7114
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD DEC 12
PY 2016
VL 117
IS 25
AR 251101
DI 10.1103/PhysRevLett.117.251101
PG 8
WC Physics, Multidisciplinary
SC Physics
GA EF3JO
UT WOS:000390220900001
PM 28036197
ER
PT J
AU Serabyn, E
Liewer, K
Lindensmith, C
Wallace, K
Nadeau, J
AF Serabyn, Eugene
Liewer, Kurt
Lindensmith, Chris
Wallace, Kent
Nadeau, Jay
TI Compact, lensless digital holographic microscope for remote microbiology
SO OPTICS EXPRESS
LA English
DT Article
ID MOTILITY; TRAJECTORIES; TOMOGRAPHY; PHASE; CHIP; CELL
AB In situ investigation of microbial life in extreme environments can be carried out with microscopes capable of imaging 3-dimensional volumes and tracking particle motion. Here we present a lensless digital holographic microscope approach that provides roughly 1.5 micron resolution in a compact, robust package suitable for remote deployment. High resolution is achieved by generating high numerical-aperture input beams with radial gradient-index rod lenses. The ability to detect and track prokaryotes was explored using bacterial strains of two different sizes. In the larger strain, a variety of motions were seen, while the smaller strain was used to demonstrate a detection capability down to micron scales. (C) 2016 Optical Society of America
C1 [Serabyn, Eugene; Liewer, Kurt; Lindensmith, Chris; Wallace, Kent] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Nadeau, Jay] CALTECH, Grad Aerosp Labs, 1200 E Calif Blvd, Pasadena, CA 91125 USA.
RP Serabyn, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM gene.serabyn@jpl.nasa.gov
FU NASA Jet Propulsion Laboratory; Gordon and Betty Moore Foundation [4037,
4038]
FX NASA Jet Propulsion Laboratory; Gordon and Betty Moore Foundation (4037,
4038).
NR 33
TC 0
Z9 0
U1 4
U2 4
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD DEC 12
PY 2016
VL 24
IS 25
BP 28540
EP 28548
DI 10.1364/OE.24.028540
PG 9
WC Optics
SC Optics
GA EE6ZJ
UT WOS:000389763000035
PM 27958498
ER
PT J
AU Lu, XM
Hu, YX
Pelon, J
Trepte, C
Liu, K
Rodier, S
Zeng, S
Lucker, P
Verhappen, R
Wilson, J
Audouy, C
Ferrier, C
Haouchine, S
Hunt, B
Getzewich, B
AF Lu, Xiaomei
Hu, Yongxiang
Pelon, Jacques
Trepte, Charles
Liu, Katie
Rodier, Sharon
Zeng, Shan
Lucker, Patricia
Verhappen, Ron
Wilson, Jamie
Audouy, Claude
Ferrier, Christophe
Haouchine, Said
Hunt, Bill
Getzewich, Brian
TI Retrieval of ocean subsurface particulate backscattering coefficient
from space-borne CALIOP lidar measurements
SO OPTICS EXPRESS
LA English
DT Article
ID VOLUME-SCATTERING FUNCTION; ANGULAR SHAPE; WATERS; REFLECTANCE;
ALTIMETRY; COLOR; SEA
AB A new approach has been proposed to determine ocean subsurface particulate backscattering coefficient b(bp) from CALIOP 30 degrees off-nadir lidar measurements. The new method also provides estimates of the particle volume scattering function at the 180 degrees scattering angle. The CALIOP based layer-integrated lidar backscatter and particulate backscattering coefficients are compared with the results obtained from MODIS ocean color measurements. The comparison analysis shows that ocean subsurface lidar backscatter and particulate backscattering coefficient bbp can be accurately obtained from CALIOP lidar measurements, thereby supporting the use of space-borne lidar measurements for ocean subsurface studies. (C) 2016 Optical Society of America
C1 [Lu, Xiaomei; Rodier, Sharon; Zeng, Shan; Lucker, Patricia; Verhappen, Ron; Wilson, Jamie; Hunt, Bill; Getzewich, Brian] Sci Syst & Applicat Inc, 1 Enterprise Pkwy,Suite 200, Hampton, VA 23666 USA.
[Lu, Xiaomei; Hu, Yongxiang; Trepte, Charles; Rodier, Sharon; Zeng, Shan; Lucker, Patricia; Verhappen, Ron; Wilson, Jamie; Hunt, Bill; Getzewich, Brian] NASA Langley Res Ctr, Hampton, VA 23681 USA.
[Pelon, Jacques] CNRS, Paris, France.
[Liu, Katie] NASA Langley Res Ctr, NIFS Internship, Hampton, VA 23681 USA.
[Audouy, Claude; Haouchine, Said] CNES, Toulouse, France.
[Ferrier, Christophe] CALIPSO Flight Dynam CNES, Toulouse, France.
RP Lu, XM (reprint author), Sci Syst & Applicat Inc, 1 Enterprise Pkwy,Suite 200, Hampton, VA 23666 USA.; Lu, XM (reprint author), NASA Langley Res Ctr, Hampton, VA 23681 USA.
EM xiaomei.lu@nasa.gov
RI Hu, Yongxiang/K-4426-2012
NR 26
TC 0
Z9 0
U1 2
U2 2
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD DEC 12
PY 2016
VL 24
IS 25
BP 29002
EP 29009
DI 10.1364/OE.24.029000
PG 8
WC Optics
SC Optics
GA EE6ZJ
UT WOS:000389763000079
ER
PT J
AU Dutle, A
Kay, B
AF Dutle, Aaron
Kay, Bill
TI Graph odometry
SO DISCRETE APPLIED MATHEMATICS
LA English
DT Article
DE Graph reconstruction; Menger's theorem; Non-backtracking walk
AB We address the problem of determining edge weights on a graph using non-backtracking closed walks from a vertex. We show that the weights of all of the edges can be determined from any starting vertex exactly when the graph has minimum degree at least three. We also determine the minimum number of walks required to reveal all edge weights. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Dutle, Aaron] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Kay, Bill] Emory Univ, Dept Math & Comp Sci, 400 Doman Dr, Atlanta, GA 30329 USA.
RP Kay, B (reprint author), Emory Univ, Dept Math & Comp Sci, 400 Doman Dr, Atlanta, GA 30329 USA.
EM aaron.m.dutle@nasa.gov; bill.w.kay@gmail.com
NR 7
TC 0
Z9 0
U1 1
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0166-218X
EI 1872-6771
J9 DISCRETE APPL MATH
JI Discret Appl. Math.
PD DEC 11
PY 2016
VL 214
BP 108
EP 115
DI 10.1016/j.dam.2016.06.023
PG 8
WC Mathematics, Applied
SC Mathematics
GA DY1NL
UT WOS:000384861600008
ER
PT J
AU Aravena, M
Decarli, R
Walter, F
Da Cunha, E
Bauer, FE
Carilli, CL
Daddi, E
Elbaz, D
Ivison, RJ
Riechers, DA
Smail, I
Swinbank, AM
Weiss, A
Anguita, T
Assef, RJ
Bell, E
Bertoldi, F
Bacon, R
Bouwens, R
Cortes, P
Cox, P
Gonzalez-Lopez, J
Hodge, J
Ibar, E
Inami, H
Infante, L
Karim, A
Le Le Fevre, OL
Magnelli, B
Ota, K
Popping, G
Sheth, K
van der Werf, P
Wagg, J
AF Aravena, M.
Decarli, R.
Walter, F.
Da Cunha, E.
Bauer, F. E.
Carilli, C. L.
Daddi, E.
Elbaz, D.
Ivison, R. J.
Riechers, D. A.
Smail, I.
Swinbank, A. M.
Weiss, A.
Anguita, T.
Assef, R. J.
Bell, E.
Bertoldi, F.
Bacon, R.
Bouwens, R.
Cortes, P.
Cox, P.
Gonzalez-Lopez, J.
Hodge, J.
Ibar, E.
Inami, H.
Infante, L.
Karim, A.
Le Le Fevre, O.
Magnelli, B.
Ota, K.
Popping, G.
Sheth, K.
van der Werf, P.
Wagg, J.
TI THE ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: CONTINUUM
NUMBER COUNTS, RESOLVED 1.2 mm EXTRAGALACTIC BACKGROUND, AND PROPERTIES
OF THE FAINTEST DUSTY STAR-FORMING GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: ISM; galaxies: star formation; galaxies:
statistics; instrumentation: interferometers; submillimeter: galaxies
ID MASS-METALLICITY RELATION; SUBMILLIMETER-SELECTED GALAXIES; CO-TO-H-2
CONVERSION FACTOR; MOLECULAR GAS-RESERVOIRS; AZTEC MILLIMETER SURVEY;
GREATER-THAN 2; GOODS-N FIELD; 850 MU-M; HIGH-REDSHIFT; MAIN-SEQUENCE
AB We present an analysis of a deep (1 sigma = 13 mu Jy) cosmological 1.2 mm continuum map based on ASPECS, the ALMA Spectroscopic Survey in the Hubble Ultra Deep Field. In the 1 arcmin(2) covered by ASPECS we detect nine sources at >3.5 sigma significance at 1.2 mm. Our ALMA-selected sample has a median redshift of z = 1.6 +/- 0.4, with only one galaxy detected at z > 2 within the survey area. This value is significantly lower than that found in millimeter samples selected at a higher flux density cut-off and similar frequencies. Most galaxies have specific star formation rates similar to that of main sequence galaxies at the same epoch, and we find median values of stellar mass and star formation rates of 4.0 x 10(10) M circle dot and similar to 40 M circle dot yr(-1), respectively. Using the dust emission as a tracer for the ISM mass, we derive depletion times that are typically longer than 300 Myr, and we find molecular gas fractions ranging from similar to 0.1 to 1.0. As noted by previous studies, these values are lower than using CO-based ISM estimates by a factor similar to 2. The 1\,mm number counts (corrected for fidelity and completeness) are in agreement with previous studies that were typically restricted to brighter sources. With our individual detections only, we recover 55% +/- 4% of the extragalactic background light (EBL) at 1.2 mm measured by the Planck satellite, and we recover 80% +/- 7% of this EBL if we include the bright end of the number counts and additional detections from stacking. The stacked contribution is dominated by galaxies at z similar to 1-2, with stellar masses of (1-3) x 10(10) M circle dot. For the first time, we are able to characterize the population of galaxies that dominate the EBL at 1.2 mm.
C1 [Aravena, M.] Univ Diego Port, Fac Ingn, Nucleo Astron, Ejercito 441, Santiago, Chile.
[Decarli, R.; Walter, F.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Walter, F.] CALTECH, Dept Astron, MC105-24, Pasadena, CA 91125 USA.
[Walter, F.] NRAO, Pete V Domenici Array Sci Ctr, POB O, Socorro, NM 87801 USA.
[Da Cunha, E.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic, Australia.
[Bauer, F. E.] Pontificia Univ Catolica Chile, Inst Astrofis, Fac Fis, Av Vicuna Mackenna 4860, 7820436 Santiago, Chile.
[Bauer, F. E.] Millennium Inst Astrophys, Santiago, Chile.
[Bauer, F. E.] Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA.
[Carilli, C. L.] Cavendish Lab, Astrophys Grp, JJ Thomson Ave, Cambridge CB3 0HE, England.
[Daddi, E.; Elbaz, D.] Univ Paris Diderot, Irfu Serv Astrophys, Lab AIM, CEA Saclay, F-91191 Gif Sur Yvette, France.
[Ivison, R. J.; Popping, G.] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Ivison, R. J.] Univ Edinburgh, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Riechers, D. A.] Cornell Univ, 220 Space Sci Bldg, Ithaca, NY 14853 USA.
[Smail, I.] Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England.
[Smail, I.] Univ Durham, Inst Computat Cosmol, South Rd, Durham DH1 3LE, England.
[Weiss, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Anguita, T.] Univ Andres Bello, Dept Ciencias Fis, Fernandez Concha 700, Santiago, Chile.
[Bell, E.] Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA.
[Bertoldi, F.] Univ Bonn, Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany.
[Bacon, R.] Univ Lyon 1, 9 Ave Charles Andre, F-69561 St Genis Laval, France.
[Bouwens, R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Bacon, R.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Bouwens, R.] Joint ALMA Observ ESO, Alonso Cordova 3104, Santiago, Chile.
[Cortes, P.; Cox, P.] Univ Valparaiso, Inst Fis Astron, Avda Gran Breta 1111, Valparaiso, Chile.
[Ibar, E.] Marseille Univ, CNRS, LAM UMR 7326, F-13388 Marseille, France.
[Le Le Fevre, O.] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England.
[Ota, K.] Univ Cambridge, Cavendish Lab, 19 JJ Thomson Ave, Cambridge CB3 0HE, England.
[Ota, K.] Sci Miss Directorate, NASA Headquarters, Washington, DC 20546 USA.
[Sheth, K.] SKA Org, Macclesfield SK11 9DL, Cheshire, England.
RP Aravena, M (reprint author), Univ Diego Port, Fac Ingn, Nucleo Astron, Ejercito 441, Santiago, Chile.
EM manuel.aravenaa@mail.udp.cl
OI Daddi, Emanuele/0000-0002-3331-9590; da Cunha,
Elisabete/0000-0001-9759-4797; Bell, Eric/0000-0002-5564-9873
FU FONDECYT [1140099, 1141218, 1151408]; ERC; Conicyt [PFB-06/2007,
ACT1417]; Ministry of Economy, Development, and Tourism's Millennium
Science Initiative [IC120009]; Australian Research Council
[FT150100079]; National Science Foundation [AST-1614213]; STFC
[ST/L00075X/1]; Royal Society/Wolfson Merit award; DFG [1573];
Collaborative Research Council - Deutsche Forschungsgemeinschaft (DFG)
[956]; Conict [PFB-06/2007, ACT1417]; German ARC
FX We thank the anonymous referee for her/his positive feedback and useful
comments. M.A. acknowledges partial support from FONDECYT through grant
1140099. F.W., I.R.S., and R.J.I. acknowledge support through ERC grants
COSMIC-DAWN, DUSTYGAL, and COSMICISM, respectively. F.E.B. and L.I.
acknowledge Conicyt grants Basal-CATA PFB-06/2007 and Anilo ACT1417.
F.E.B. also acknowledges support from FONDECYT Regular 1141218 (FEB) and
the Ministry of Economy, Development, and Tourism's Millennium Science
Initiative through grant IC120009, awarded to the Millennium Institute
of Astrophysics (MAS). E.d.C. gratefully acknowledges the Australian
Research Council as the recipient of a Future Fellowship (project
FT150100079). D.R. acknowledges support from the National Science
Foundation under grant number AST-1614213 to Cornell University. I.R.S.
also acknowledges support from STFC (ST/L00075X/1) and a Royal
Society/Wolfson Merit award. Support for R.D. and B.M. was provided by
the DFG priority program 1573 "The Physics of the Interstellar Medium."
A.K. and F.B. acknowledge support by the Collaborative Research Council
956, sub-project A1, funded by the Deutsche Forschungsgemeinschaft
(DFG). P.I. acknowledges Conict grants Basal-CATA PFB-06/2007 and Anilo
ACT1417. R.J.A. was supported by FONDECYT grant number 1151408. This
paper makes use of the following ALMA data: ADS/JAO.ALMA#2013.1.00146.S
and ADS/JAO.ALMA#2013.1.00718.S. ALMA is a partnership of ESO
(representing its member states), NSF (USA), and NINS (Japan), together
with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea),
in cooperation with the Republic of Chile. The Joint ALMA Observatory is
operated by ESO, AUI/NRAO, and NAOJ. The 3 mm part of the ALMA project
was supported by the German ARC.
NR 145
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 10
PY 2016
VL 833
IS 1
AR 833
DI 10.3847/1538-4357/833/1/68
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EK1HX
UT WOS:000393677500001
ER
PT J
AU Adrian, ML
Vinas, AF
Moya, PS
Wendel, DE
AF Adrian, M. L.
Vinas, A. F.
Moya, P. S.
Wendel, D. E.
TI SOLAR WIND MAGNETIC FLUCTUATIONS AND ELECTRON NON-THERMAL TEMPERATURE
ANISOTROPY: SURVEY OF WIND-SWE-VEIS OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE instabilities; kinematics and dynamics; methods: data analysis; plasmas;
solar wind; turbulence
ID VELOCITY DISTRIBUTION-FUNCTIONS; HELIOS PLASMA-EXPERIMENT; GLOBAL
PROCESSES; SPACECRAFT; WAVES
AB The solar wind electron velocity distribution function (eVDF) exhibits a variety of non-thermal features that deviate from thermal equilibrium. These deviations from equilibrium provide a local source for electromagnetic fluctuation emissions, including the commonly observed electron whistler-cyclotron and firehose instabilities. We present a systematic analysis of Wind-SWE-VEIS observations of solar wind electron plasma and associated Wind-MFI observed magnetic fluctuations. For the first time using the full solar wind electron distribution and its moments, without separation of the various electron components, we show clear evidence that the temperature anisotropy threshold of the parallel electron cyclotron anisotropic instability bounds solar wind electrons during slow solar wind periods. We also demonstrate that during periods of slow solar wind, collisions-while infrequent -are the dominant mechanism by which solar wind electrons are constrained, leading to isotropization. During fast solar wind periods, magnetic fluctuations and solar wind anisotropies are enhanced above the parallel whistler anisotropic threshold boundary and collisional effects are significantly reduced. Preliminary calculations further show that the oblique electron whistler mirror anisotropic instability bounds both the slow and fast solar wind. Regardless of speed, the solar wind electron thermal anisotropy appears globally bounded by the parallel electron firehose instability for anisotropiesT(e)perpendicular to/T-e parallel to < 1. Our results indicate that collisions, while infrequent, play a necessary role in regulating the solar wind eVDFs. In striking contrast to solar wind ions, solar wind electron plasma, when considered globally as a single eVDF, is only marginally stable with respect to parallel propagating instabilities.
C1 [Adrian, M. L.; Vinas, A. F.; Moya, P. S.; Wendel, D. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
[Moya, P. S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Moya, P. S.] Univ Chile, Fac Ciencias, Dept Fis, Santiago, Chile.
RP Adrian, ML (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Heliophys Sci Div,Sci & Explorat Directorate, Mail Code 673,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM Mark.L.Adrian@nasa.gov
RI Moya, Pablo/C-3163-2011
OI Moya, Pablo/0000-0002-9161-0888
FU CONICyT Chile through FONDECyT grant [11150055]; Conicyt PIA project
[ACT1405]
FX The authors gratefully acknowledge Dr. Adam Szabo at NASA/Goddard Space
Flight Center and the Coordinated Data Analysis Web
(CDAWeb-http://cdaweb.gsfc.nasa.gov) for providing access to the
Wind-SWE-VEIS solar wind electron moments data, as well as the
high-resolution Wind-MFI data, that formed the foundation to the work
presented above. Additionally, the authors would like to acknowledge Dr.
Lynn Wilson, III for his numerous insightful discussions and comments.
P.S.M. is grateful for the support of CONICyT Chile through FONDECyT
grant No. 11150055 and Conicyt PIA project ACT1405.
NR 21
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 10
PY 2016
VL 833
IS 1
AR 49
DI 10.3847/1538-4357/833/1/49
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EF8CX
UT WOS:000390557100013
ER
PT J
AU Bucik, R
Innes, DE
Mason, GM
Wiedenbeck, ME
AF Bucik, Radoslav
Innes, Davina E.
Mason, Glenn M.
Wiedenbeck, Mark E.
TI ASSOCIATION OF He-3-RICH SOLAR ENERGETIC PARTICLES WITH LARGE-SCALE
CORONAL WAVES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; shock waves; Sun: coronal mass ejections
(CMEs); Sun: flares; Sun: particle emission; waves
ID ADVANCED COMPOSITION EXPLORER; MAGNETIC-FIELD CONNECTION; ELECTRON
EVENTS; STEREO MISSION; ISOTOPE SPECTROMETER; WIND SPACECRAFT; MASS
EJECTIONS; ALPHA MONITOR; SEP EVENTS; EUV WAVES
AB Small, He-3-rich solar energetic particle (SEP) events have been commonly associated with extreme-ultraviolet (EUV) jets and narrow coronal mass ejections (CMEs) that are believed to be the signatures of magnetic reconnection, involving field lines open to interplanetary space. The elemental and isotopic fractionation in these events are thought to be caused by processes confined to the flare sites. In this study, we identify 32 He-3-rich SEP events observed by the Advanced Composition Explorer, near the Earth, during the solar minimum period 2007-2010, and we examine their solar sources with the high resolution Solar Terrestrial Relations Observatory (STEREO) EUV images. Leading the Earth, STEREO-A has provided, for the first time, a direct view on He-3-rich flares, which are generally located on the Sun's western hemisphere. Surprisingly, we find that about half of the He-3-rich SEP events in this survey are associated with large-scale EUV coronal waves. An examination of the wave front propagation, the source-flare distribution, and the coronal magnetic field connections suggests that the EUV waves may affect the injection of He-3-rich SEPs into interplanetary space.
C1 [Bucik, Radoslav] Georg August Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
[Bucik, Radoslav; Innes, Davina E.] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany.
[Mason, Glenn M.] Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA.
[Wiedenbeck, Mark E.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Innes, Davina E.] Max Planck Princeton Ctr Plasma Phys, Princeton, NJ 08540 USA.
RP Bucik, R (reprint author), Georg August Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.; Bucik, R (reprint author), Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany.
EM bucik@mps.mpg.de
OI Bucik, Radoslav/0000-0001-7381-6949
FU Deutsche Forschungsgemeinschaft (DFG) [BU 3115/2-1]; NASA
[NNX13AR20G/115828]; NASA from the University of California Berkeley
[SA4889-26309]
FX The work of R. B. is supported by the Deutsche Forschungsgemeinschaft
(DFG) under grant BU 3115/2-1. We thank R. J. MacDowall for providing
the Wind/WAVES data and acknowledge the use of the Wind/3DP data. Work
at JPL was supported by NASA. Work at APL (ACE/ULEIS and STEREO/SIT) was
supported by NASA grant NNX13AR20G/115828 and NASA subcontract
SA4889-26309 from the University of California Berkeley.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 10
PY 2016
VL 833
IS 1
AR 63
DI 10.3847/1538-4357/833/1/63
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EF8CX
UT WOS:000390557100027
ER
PT J
AU Guo, YC
Rafelski, M
Faber, SM
Koo, DC
Krumholz, MR
Trump, JR
Willner, SP
Amorin, R
Barro, G
Bell, EF
Gardner, JP
Gawiser, E
Hathi, NP
Koekemoer, AM
Pacifici, C
Perez-Gonzalez, PG
Ravindranath, S
Reddy, N
Teplitz, HI
Yesuf, H
AF Guo, Yicheng
Rafelski, Marc
Faber, S. M.
Koo, David C.
Krumholz, Mark R.
Trump, Jonathan R.
Willner, S. P.
Amorin, Ricardo
Barro, Guillermo
Bell, Eric F.
Gardner, Jonathan P.
Gawiser, Eric
Hathi, Nimish P.
Koekemoer, Anton M.
Pacifici, Camilla
Perez-Gonzalez, Pablo G.
Ravindranath, Swara
Reddy, Naveen
Teplitz, Harry I.
Yesuf, Hassen
TI THE BURSTY STAR FORMATION HISTORIES OF LOW-MASS GALAXIES AT 0.4 < z < 1
REVEALED BY STAR FORMATION RATES MEASURED FROM H beta AND FUV
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: dwarf; galaxies: evolution; galaxies: formation; galaxies:
fundamental parameters; galaxies: starburst; galaxies: star formation
ID SIMILAR-TO 2; HUBBLE-SPACE-TELESCOPE; STELLAR POPULATION SYNTHESIS;
EXTRAGALACTIC LEGACY SURVEY; CONTINUUM ESCAPE FRACTION; FORMATION RATE
INDICATORS; DUST ATTENUATION CURVE; LARGE-MAGELLANIC-CLOUD; GOODS-SOUTH
FIELD; LESS-THAN 1.5
AB We investigate the burstiness of star formation histories (SFHs) of galaxies at 0.4 < z < 1 by using the ratio of star formation rates (SFRs) measured from H beta and FUV (1500 angstrom) (H beta-to-FUV ratio). Our sample contains 164 galaxies down to stellar mass (M-*) of 10(8.5) M-circle dot in the CANDELS GOODS-N region, where Team Keck Redshift Survey Keck/DEIMOS spectroscopy and Hubble Space Telescope/WFC3 F275W images from CANDELS and Hubble Deep UV Legacy Survey are available. When the ratio of H beta-and FUV-derived SFRs is measured, dust extinction correction is negligible (except for very dusty galaxies) with the Calzetti attenuation curve. The H beta-toFUV ratio of our sample increases with M-* and SFR. The median ratio is similar to 0.7 at M-* similar to 10(8.5) M-circle dot (or SFR similar to 0.5M(circle dot) yr(-1)) and increases to similar to 1 at M-* similar to 10(10) M-circle dot (or SFR similar to 10 M-circle dot yr(-1)). At M-* < 10(9.5) M-circle dot, our median H beta-to-FUV ratio is lower than that of local galaxies at the same M*, implying a redshift evolution. Bursty SFH on a timescale of a few tens of megayears on galactic scales provides a plausible explanation for our results, and the importance of the burstiness increases as M* decreases. Due to sample selection effects, our H beta-to-FUV ratio may be an upper limit of the true value of a complete sample, which strengthens our conclusions. Other models, e.g., non-universal initial mass function or stochastic star formation on star cluster scales, are unable to plausibly explain our results.
C1 [Guo, Yicheng; Faber, S. M.; Koo, David C.; Krumholz, Mark R.; Barro, Guillermo; Yesuf, Hassen] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Rafelski, Marc; Gardner, Jonathan P.; Pacifici, Camilla] Goddard Space Flight Ctr, Code 665, Greenbelt, MD USA.
[Krumholz, Mark R.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia.
[Trump, Jonathan R.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
[Trump, Jonathan R.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Willner, S. P.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Amorin, Ricardo] Osserv Astron Roma, INAF, Monte Porzio Catone, Italy.
[Barro, Guillermo] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
[Bell, Eric F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Gawiser, Eric] Rutgers State Univ, Dept Phys & Astron, New Brunswick, NJ USA.
[Hathi, Nimish P.] Aix Marseille Univ, CNRS, LAM, UMR 7326, Marseille, France.
[Rafelski, Marc; Koekemoer, Anton M.; Ravindranath, Swara] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Perez-Gonzalez, Pablo G.] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain.
[Reddy, Naveen] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[Teplitz, Harry I.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
RP Guo, YC (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA.
EM ycguo@ucolick.org
FU NSF [AST-0808133]; NASA [HST-GO-12060, HST-AR-13891, NAS5-26555]; NASA
Postdoctoral Program at Goddard Space Flight Center
FX We thank the anonymous referee for the valuable and constructive
comments, which improve this article. Y.G., S.M.F., D.C.K., G.B., and
H.Y. acknowledge support from NSF Grant AST-0808133. Support for Program
HST-GO-12060 and HST-AR-13891 were provided by NASA through a grant from
the Space Telescope Science Institute, operated by the Association of
Universities for Research in Astronomy, Incorporated, under NASA
contract NAS5-26555. MR acknowledges support from an appointment to the
NASA Postdoctoral Program at Goddard Space Flight Center.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 10
PY 2016
VL 833
IS 1
AR 37
DI 10.3847/1538-4357/833/1/37
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EF8CX
UT WOS:000390557100001
ER
PT J
AU Lau, RM
Werner, M
Sahai, R
Ressler, ME
AF Lau, R. M.
Werner, M.
Sahai, R.
Ressler, M. E.
TI EVIDENCE FROM SOFIA IMAGING OF POLYCYCLIC AROMATIC HYDROCARBON FORMATION
ALONG A RECENT OUTFLOW IN NGC 7027
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; ISM: abundances; ISM: jets and outflows;
photon-dominated region (PDR); planetary nebulae: individual (NGC 7027)
ID PLANETARY-NEBULA NGC-7027; INFRARED-EMISSION; INTERSTELLAR SHOCKS;
MOLECULAR ENVELOPE; GRAIN DESTRUCTION; SPACE-TELESCOPE; DUST;
EXCITATION; MODEL; MASS
AB We report spatially resolved (FWHM similar to 3.'' 8-4.'' 6) mid-IR imaging observations of the planetary nebula (PN) NGC 7027 taken with the 2.5 m telescope on board the Stratospheric Observatory for Infrared Astronomy (SOFIA). Images of NGC 7027 were acquired at 6.3, 6.6, 11.1, 19.7, 24.2, 33.6, and 37.1 mu m using the Faint Object Infrared Camera for the SOFIA Telescope (FORCAST). The observations reveal emission from polycyclic aromatic hydrocarbons (PAHs) and warm dust (T-D similar to 90 K) from the illuminated inner edge of the molecular envelope surrounding the ionized gas and central star. The DustEM code was used to fit the spectral energy distribution of fluxes obtained by FORCAST and the archival infrared spectrum of NGC 7027 acquired by the Short Wavelength Spectrometer (SWS) on the Infrared Space Observatory (ISO). Best-fit dust models provide a total dust mass of 5.8(-2.6)(+2.3) x 10(-3) M-circle dot, where carbonaceous large (a = 1.5 mu m) and very small (a similar to 12 angstrom) grains, and PAHs (3.1 angstrom < a < 12 angstrom) compose 96.5, 2.2, and 1.3% of the dust by mass, respectively. The 37 mu m optical depth map shows minima in the dust column density at regions in the envelope that are coincident with a previously identified collimated outflow from the central star. The optical depth minima are also spatially coincident with enhancements in the 6.2 mu m PAH feature, which is derived from the 6.3 and 6.6 mu m maps. We interpret the spatial anti-correlation of the dust optical depth and PAH 6.2 mu m feature strength and their alignment with the outflow from the central star as evidence of dust processing and rapid PAH formation via grain-grain collisions in the post-shock environment of the dense (n(H) similar to 10(5) cm(-3)) photo-dissociation region and molecular envelope.
C1 [Lau, R. M.; Werner, M.; Sahai, R.; Ressler, M. E.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Lau, RM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
FU Universities Space Research Association, Inc. (USRA) under NASA
[NAS2-97001]; Deutsches SOFIA Institut (DSI) under DLR [50 OK 0901];
NASA by USRA [8500-98-014]
FX We would like to thank the FORCAST team, Terry Herter, Luke Keller, Joe
Adams, George Gull, Justin Schoenwald, and Chuck Henderson, the USRA
Science and Mission Ops teams, and the entire SOFIA staff. We also thank
Peter van Hoof for sharing his models of the emission from NGC 7027, and
the anonymous referee for helpful comments. R.L. would like to thank
Jeronimo Bernard-Salas for insightful discussion on dust processing in
PNe. This work is based on observations made with the NASA/DLR
Stratospheric Observatory for Infrared Astronomy (SOFIA). This work was
also based in part on observations made with the NASA/ESA Hubble Space
Telescope, obtained from the data archive at the Space Telescope Science
Institute, and observations made by the Chandra X-ray Observatory and
published previously in cited articles. This work was carried out at the
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. SOFIA
science mission operations are conducted jointly by the Universities
Space Research Association, Inc. (USRA), under NASA contract NAS2-97001,
and the Deutsches SOFIA Institut (DSI) under DLR contract 50 OK 0901.
Financial support for FORCAST was provided by NASA through award
8500-98-014 issued by USRA.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 10
PY 2016
VL 833
IS 1
AR 115
DI 10.3847/1538-4357/833/1/115
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EG1BG
UT WOS:000390765800011
ER
PT J
AU Rouillard, AP
Plotnikov, I
Pinto, RF
Tirole, M
Lavarra, M
Zucca, P
Vainio, R
Tylka, AJ
Vourlidas, A
De Rosa, ML
Linker, J
Warmuth, A
Mann, G
Cohen, CMS
Mewaldt, RA
AF Rouillard, A. P.
Plotnikov, I.
Pinto, R. F.
Tirole, M.
Lavarra, M.
Zucca, P.
Vainio, R.
Tylka, A. J.
Vourlidas, A.
De Rosa, M. L.
Linker, J.
Warmuth, A.
Mann, G.
Cohen, C. M. S.
Mewaldt, R. A.
TI DERIVING THE PROPERTIES OF CORONAL PRESSURE FRONTS IN 3D: APPLICATION TO
THE 2012 MAY 17 GROUND LEVEL ENHANCEMENT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE shock waves; Sun: coronal mass ejections (CMEs); Sun: particle emission
ID ENERGETIC PARTICLE EVENT; HELIOSPHERIC PLASMA SHEETS; RADIAL
MAGNETIC-FIELD; WHOLE SUN MONTH; MASS EJECTIONS; SOLAR CORONA; STEREO
MISSION; WHITE-LIGHT; ACCELERATION; DRIVEN
AB We study the link between an expanding coronal shock and the energetic particles measured near Earth during the ground level enhancement of 2012 May 17. We developed a new technique based on multipoint imaging to triangulate the three-dimensional (3D) expansion of the shock forming in the corona. It uses images from three vantage points by mapping the outermost extent of the coronal region perturbed by the pressure front. We derive for the first time the 3D velocity vector and the distribution of Mach numbers, M-FM, of the entire front as a function of time. Our approach uses magnetic field reconstructions of the coronal field, full magnetohydrodynamic simulations and imaging inversion techniques. We find that the highest M-FM values appear near the coronal neutral line within a few minutes of the coronal mass ejection onset; this neutral line is usually associated with the source of the heliospheric current and plasma sheet. We illustrate the variability of the shock speed, shock geometry, and Mach number along different modeled magnetic field lines. Despite the level of uncertainty in deriving the shock Mach numbers, all employed reconstruction techniques show that the release time of GeV particles occurs when the coronal shock becomes super-critical (M-FM > 3). Combining in situ measurements with heliospheric imagery, we also demonstrate that magnetic connectivity between the accelerator (the coronal shock of 2012 May 17) and the near-Earth environment is established via a magnetic cloud that erupted from the same active region roughly five days earlier.
C1 [Rouillard, A. P.; Plotnikov, I.; Pinto, R. F.; Tirole, M.; Lavarra, M.] Univ Toulouse III UPS, Inst Rech Astrophys & Planetol, Toulouse, France.
[Rouillard, A. P.; Plotnikov, I.; Pinto, R. F.; Tirole, M.; Lavarra, M.] CNRS, UMR 5277, Toulouse, France.
[Zucca, P.] Univ Paris 06, Observ Paris, LESIA UMR 8109, F-92190 Meudon, France.
[Zucca, P.] Univ Paris 07, F-92190 Meudon, France.
[Vainio, R.] Univ Turku, Turku, Finland.
[Tylka, A. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Vourlidas, A.] Johns Hopkins Appl Phys Lab, Laurel, MD USA.
[De Rosa, M. L.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA USA.
[Linker, J.] Predict Sci Inc, San Diego, CA USA.
[Warmuth, A.; Mann, G.] Leibniz Inst Astrophys Potsdam AIP, Potsdam, Germany.
[Cohen, C. M. S.; Mewaldt, R. A.] CALTECH, Pasadena, CA USA.
RP Rouillard, AP (reprint author), Univ Toulouse III UPS, Inst Rech Astrophys & Planetol, Toulouse, France.; Rouillard, AP (reprint author), CNRS, UMR 5277, Toulouse, France.
EM arouillard@irap.omp.eu
RI Vainio, Rami/A-5590-2009; Vourlidas, Angelos/C-8231-2009;
OI Vainio, Rami/0000-0002-3298-2067; Vourlidas,
Angelos/0000-0002-8164-5948; Ferreira Pinto, Rui/0000-0001-8247-7168
FU HELCATS project under the FP7 EU [606692]; HESPERIA project under the
EU/H2020 [637324]; DLR [50 QL 0001]; CNES; Leibniz Institute fur
Astrophysik Potsdam (AIP)
FX We acknowledge usage of the tools made available by the plasma physics
data center (Centre de Donnes de la Physique des Plasmas; CDPP;
http://cdpp.eu/), the Virtual Solar Observatory (VSO;
http://sdac.virtualsolar.org), the Multi Experiment Data & Operation
Center (MEDOC; https://idoc.ias.u-psud.fr/MEDOC), the French space
agency (Centre National des Etudes Spatiales; CNES; https://cnes.fr/fr),
and the space weather team in Toulouse (Solar-Terrestrial Observations
and Modeling Service; STORMS; https://stormsweb.irap.omp.eu/). This
includes the data mining tools AMDA (http://amda.cdpp.eu/) and CLWEB
(clweb.cesr.fr/) and the propagation tool
(http://propagationtool.cdpp.eu). RFP and IP acknowledge financial
support from the HELCATS project under the FP7 EU contract number
606692. RV acknowledges financial support from the HESPERIA project
under the EU/H2020 contract number 637324. AW acknowledges the support
by DLR under grant No. 50 QL 0001. APR acknowledges funding from CNES
and the Leibniz Institute fur Astrophysik Potsdam (AIP) to visit AIP and
to collaborate with AW and GM on the present project. The STEREO SECCHI
data are produced by a consortium of RAL (UK), NRL (USA), LMSAL (USA),
GSFC (USA), MPS (Germany), CSL (Belgium), IOTA (France), and IAS
(France). The ACE data were obtained from the ACE science center. The
Wind data were obtained from the Space Physics Data Facility.
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 10
PY 2016
VL 833
IS 1
AR 45
DI 10.3847/1538-4357/833/1/45
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EF8CX
UT WOS:000390557100009
ER
PT J
AU Wang, QHS
Markevitch, M
Giacintucci, S
AF Wang, Qian H. S.
Markevitch, Maxim
Giacintucci, Simona
TI THE MERGING GALAXY CLUSTER A520-A BROKEN-UP COOL CORE, A DARK
SUBCLUSTER, AND AN X-RAY CHANNEL
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: individual (A520); intergalactic medium; X-rays:
galaxies: clusters
ID INTRACLUSTER MEDIUM; CHANDRA OBSERVATION; THERMAL CONDUCTION; COMA
CLUSTER; COLD FRONTS; RADIO HALO; BOW SHOCK; GAS; MASS; SAMPLE
AB We present results from a deep. Chandra. X-ray observation of a merging galaxy cluster A520. A high-resolution gas temperature map reveals a long trail of dense, cool clumps-apparently the fragments of a cool core that has been stripped from the infalling subcluster by ram pressure. The clumps should still be connected by the stretched magnetic field lines. The observed temperature variations imply that thermal conductivity is suppressed by a factor >100 across the presumed direction of the magnetic field (as found in other clusters), and is also suppressed along the field lines by a factor of several. Two massive clumps in the periphery of A520, visible in the weak-lensing mass map and the X-ray image, have apparently been completely stripped of gas during the merger, but then reaccreted the surrounding high-entropy gas upon exit from the cluster. The mass clump that hosted the stripped cool core is also reaccreting hotter gas. An X-ray hydrostatic mass estimate for the clump that has the simplest geometry agrees with the lensing mass. Its current gas mass to total mass ratio is very low, 1.5%-3%, which makes it a "dark subcluster." We also found a curious low X-ray brightness channel (likely a low-density sheet in projection) going across the cluster along the direction of an apparent secondary merger. The channel may be caused by plasma depletion in a region of an amplified magnetic field (with plasma beta similar to 10-20). The shock in A520 will be studied in a separate paper.
C1 [Wang, Qian H. S.; Giacintucci, Simona] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Markevitch, Maxim] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Markevitch, Maxim; Giacintucci, Simona] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
RP Wang, QHS (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
OI Giacintucci, Simona/0000-0002-1634-9886
FU Chandra [GO3-14144Z, GO5-16147Z]
FX We thank the referee for useful comments that made the paper clearer.
Q.H.S.W. was supported by Chandra grants GO3-14144Z and GO5-16147Z.
NR 46
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD DEC 10
PY 2016
VL 833
IS 1
AR 99
DI 10.3847/1538-4357/833/1/99
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EG1KU
UT WOS:000390792000011
ER
PT J
AU Gaulme, P
Rowe, JF
Bedding, TR
Benomar, O
Corsaro, E
Davies, GR
Hale, SJ
Howe, R
Garcia, RA
Huber, D
Jimenez, A
Mathur, S
Mosser, B
Appourchaux, T
Boumier, P
Jackiewicz, J
Leibacher, J
Schmider, FX
Hammel, HB
Lissauer, JJ
Marley, MS
Simon, AA
Chaplin, WJ
Elsworth, Y
Guzik, JA
Murphy, N
Aguirre, VS
AF Gaulme, P.
Rowe, J. F.
Bedding, T. R.
Benomar, O.
Corsaro, E.
Davies, G. R.
Hale, S. J.
Howe, R.
Garcia, R. A.
Huber, D.
Jimenez, A.
Mathur, S.
Mosser, B.
Appourchaux, T.
Boumier, P.
Jackiewicz, J.
Leibacher, J.
Schmider, F. -X.
Hammel, H. B.
Lissauer, J. J.
Marley, M. S.
Simon, A. A.
Chaplin, W. J.
Elsworth, Y.
Guzik, J. A.
Murphy, N.
Aguirre, V. Silva
TI A DISTANT MIRROR: SOLAR OSCILLATIONS OBSERVED ON NEPTUNE BY THE KEPLER
K2 MISSION
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planets and satellites: individual (Neptune); stars: oscillations
(including pulsations); Sun: helioseismology; techniques: photometric
ID RED-GIANT STARS; STELLAR OSCILLATIONS; SCALING RELATIONS;
BAYESIAN-APPROACH; MAIN-SEQUENCE; HR DIAGRAM; AMPLITUDES;
ASTEROSEISMOLOGY; COROT; FREQUENCIES
AB Starting in 2014 December, Kepler K2 observed Neptune continuously for 49 days at a 1 minute cadence. The goals consisted of studying its atmospheric dynamics, detecting its global acoustic oscillations, and those of the Sun, which we report on here. We present the first indirect detection of solar oscillations in intensity measurements. Beyond the remarkable technical performance, it indicates how Kepler would see a star like the Sun. The result from the global asteroseismic approach, which consists of measuring the oscillation frequency at maximum amplitude nu(max) and the mean frequency separation between mode overtones Delta nu, is surprising as the nu(max) measured from Neptune photometry is larger than the accepted value. Compared to the usual reference nu(max,circle dot) = 3100 mu Hz, the asteroseismic scaling relations therefore make the solar mass and radius appear larger by 13.8 +/- 5.8% and 4.3 +/- 1.9%, respectively. The higher nu(max) is caused by a combination of the value of nu(max,circle dot), being larger at the time of observations than the usual reference from SOHO/VIRGO/SPM data (3160 +/- 10 mu Hz), and the noise level of the K2 time series, being 10 times larger than VIRGO's. The peak-bagging method provides more consistent results: despite a low signal-to-noise ratio (S/N), we model 10 overtones for degrees l = 0, 1, 2. We compare the K2 data with simultaneous SOHO/VIRGO/SPM photometry and BiSON velocity measurements. The individual frequencies, widths, and amplitudes mostly match those from VIRGO and BiSON within 1 sigma, except for the few peaks with the lowest S/N.
C1 [Gaulme, P.; Jackiewicz, J.] New Mexico State Univ, Dept Astron, POB 30001,MSC 4500, Las Cruces, NM 88003 USA.
[Gaulme, P.] Apache Point Observ, 2001 Apache Point Rd,POB 59, Sunspot, NM 88349 USA.
[Gaulme, P.] New Mexico Inst Min & Technol, Dept Phys, 801 Leroy Pl, Socorro, NM 87801 USA.
[Rowe, J. F.] Univ Montreal, Dept Phys, Inst Rech Exoplanetes, iREx, Montreal, PQ H3C 3J7, Canada.
[Bedding, T. R.; Huber, D.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
[Bedding, T. R.; Davies, G. R.; Hale, S. J.; Howe, R.; Elsworth, Y.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Benomar, O.] New York Univ Abu Dhabi, NYUAD Inst, Ctr Space Sci, POB 129188, Abu Dhabi, U Arab Emirates.
[Corsaro, E.; Garcia, R. A.] Univ Paris 7 Diderot, Lab AIM, Ctr Saclay, CEA,DRF,CNRS,IRFU,SAp, F-91191 Gif Sur Yvette, France.
[Corsaro, E.; Jimenez, A.] Inst Astrofis Canarias, E-38200 Tenerife, Spain.
[Corsaro, E.; Jimenez, A.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain.
[Corsaro, E.; Davies, G. R.] Osserv Astrofis Catania, INAF, Via S Sofia 78, I-95123 Catania, Italy.
[Hale, S. J.; Howe, R.; Huber, D.; Chaplin, W. J.; Elsworth, Y.; Aguirre, V. Silva] Aarhus Univ, Dept Phys & Astron, SAC, Ny Munkegade 120, DK-8000 Aarhus C, Denmark.
[Huber, D.] SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA.
[Mathur, S.] Space Sci Inst, Ctr Extrasolar Planetary Syst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA.
[Mosser, B.] Univ Paris 07, Univ Pierre & Marie Curie, CNRS, LESIA,Observ Paris,PSL Res Univ, F-92195 Meudon, France.
[Appourchaux, T.; Boumier, P.; Leibacher, J.] Univ Paris 11, Inst Astrophys Spatiale, Batiment 121, F-91405 Orsay, France.
[Appourchaux, T.; Boumier, P.; Leibacher, J.] CNRS, UMR 8617, Batiment 121, F-91405 Orsay, France.
[Leibacher, J.] Natl Solar Observ, North Cherry Ave, Tucson, AZ 85718 USA.
[Schmider, F. -X.] Univ Nice Sophia Antipolis, CNRS, Lab Lagrange, Observ Cote Azur, Nice, France.
[Hammel, H. B.] AURA Inc, 1331 Pennsylvania Ave NW,Suite 1475, Washington, DC 20004 USA.
[Lissauer, J. J.; Marley, M. S.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, MS 245-3, Moffett Field, CA 94035 USA.
[Simon, A. A.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div 690 0, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Guzik, J. A.] Los Alamos Natl Lab, XTD NTA, MS T086, Los Alamos, NM 87545 USA.
[Murphy, N.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Gaulme, P (reprint author), New Mexico State Univ, Dept Astron, POB 30001,MSC 4500, Las Cruces, NM 88003 USA.; Gaulme, P (reprint author), Apache Point Observ, 2001 Apache Point Rd,POB 59, Sunspot, NM 88349 USA.; Gaulme, P (reprint author), New Mexico Inst Min & Technol, Dept Phys, 801 Leroy Pl, Socorro, NM 87801 USA.
EM gaulme@nmsu.edu
RI Simon, Amy/C-8020-2012;
OI Simon, Amy/0000-0003-4641-6186; Gaulme, Patrick/0000-0001-8330-5464;
Benomar, Othman/0000-0001-9405-5552; Bedding, Tim/0000-0001-5222-4661
FU CNES GOLF grant; European Community [312844]; European Union's Horizon
2020 research and innovation programme under the Marie Sklodowska-Curie
grant [664931]; Australian Research Council [DE140101364]; National
Aeronautics and Space Administration under Kepler Participating
Scientist Program [NNX14AB92G]; NASA [NNX12AE17G, NNX15AF13G]; NSF
[AST-1411685]
FX T.A., P.B., and R.A.G. acknowledge the support received from the CNES
GOLF grant. E.C. and R.A.G. received funding from the European
Community's Seventh Framework Programme ([FP7/2007-2013]) under grant
agreement No. 312844 (SPACEINN). E.C. has received fundings from the
European Union's Horizon 2020 research and innovation programme under
the Marie Sklodowska-Curie grant agreement No. 664931. D.H. acknowledges
support by the Australian Research Council's Discovery Projects funding
scheme (project number DE140101364) and support by the National
Aeronautics and Space Administration under grant NNX14AB92G issued
through the Kepler Participating Scientist Program. S.M. would like to
acknowledge support from NASA grants NNX12AE17G and NNX15AF13G and NSF
grant AST-1411685.
NR 51
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD DEC 10
PY 2016
VL 833
IS 1
AR L13
DI 10.3847/2041-8213/833/1/L13
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EG1WA
UT WOS:000390822200003
ER
PT J
AU Lindberg, JE
Charnley, SB
Cordiner, MA
AF Lindberg, Johan E.
Charnley, Steven B.
Cordiner, Martin A.
TI ON THE ORIGIN OF C4H AND CH3OH IN PROTOSTELLAR ENVELOPES
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE astrochemistry; ISM: individual objects (Ophiuchus); ISM: molecules;
stars: formation
ID LOW-MASS PROTOSTARS; COMPLEX ORGANIC-MOLECULES; CARBON-CHAIN-CHEMISTRY;
YOUNG STELLAR OBJECTS; STAR-FORMATION; CHEMICAL DIFFERENTIATION; CORONA
AUSTRALIS; CLOUDS; EVOLUTION; ABUNDANCE
AB The formation pathways of different types of organic molecules in protostellar envelopes and other regions of star formation are subjects of intense current interest. We present here observations of C4H and CH3OH, tracing two distinct groups of interstellar organic molecules, toward 16 protostars in the Ophiuchus and Corona Australis molecular clouds. Together with observations in the literature, we present C4H and CH3OH data from single-dish observations of 40 embedded protostars. We find no correlation between the C4H and CH3OH column densities in this large sample. Based on this lack of correlation, a difference in line profiles between C4H and CH3OH, and previous interferometric observations of similar sources, we propose that the emission from these two molecules is spatially separated, with the CH3OH tracing gas that has been transiently heated to high (similar to 70-100 K) temperatures and the C4H tracing the cooler large-scale envelope where CH4 molecules have been liberated from ices. These results provide insight in the differentiation between hot corino and warm carbon-chain chemistry in embedded protostars.
C1 [Lindberg, Johan E.; Charnley, Steven B.; Cordiner, Martin A.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Mail Code 691,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Cordiner, Martin A.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Lindberg, JE (reprint author), NASA, Goddard Space Flight Ctr, Astrochem Lab, Mail Code 691,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM johan.lindberg@nasa.gov
FU NASA's Emerging Worlds Program
FX This research was supported by an appointment to the NASA Postdoctoral
Program at the NASA Goddard Space Flight Center to J.E.L., administered
by Universities Space Research Association through a contract with NASA,
and by NASA's Emerging Worlds Program.
NR 48
TC 1
Z9 1
U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD DEC 10
PY 2016
VL 833
IS 1
AR L14
DI 10.3847/2041-8213/833/1/L14
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EG1BS
UT WOS:000390767100001
ER
PT J
AU Loeffler, MJ
Hudson, RL
AF Loeffler, Mark J.
Hudson, Reggie L.
TI WHAT IS EATING OZONE? THERMAL REACTIONS BETWEEN SO2 AND O-3:
IMPLICATIONS FOR ICY ENVIRONMENTS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE astrochemistry; comets: general; evolution; methods: laboratory: solid
state; planets and satellites: surfaces; radiation mechanisms: thermal
ID INFRARED MAPPING SPECTROMETER; SULFURIC-ACID MONOHYDRATE;
THERMOGRAVIMETRIC DATA; GALILEAN SATELLITES; GANYMEDE; SURFACE; EUROPA;
RELEVANCE; CALLISTO; SPECTRA
AB Laboratory studies are presented, showing for the first time that thermally driven reactions in solid H2O + SO2 + O-3 mixtures can occur below 150 K, with the main sulfur-containing product being bisulfate (HSO4-). Using a technique not previously applied to the low-temperature kinetics of either interstellar or solar-system ice analogs, we estimate an activation energy of 32 kJ mol(-1) for HSO4- formation. These results show that at the temperatures of the Jovian satellites, SO2 and O-3 will efficiently react making detection of these molecules in the same vicinity unlikely. Our results also explain why O-3 has not been detected on Callisto and why the SO2 concentration on Callisto appears to be highest on that world's leading hemisphere. Furthermore, our results predict that the SO2 concentration on Ganymede will be lowest in the trailing hemisphere, where the concentration of O-3 is the highest. Our work suggests that thermal reactions in ices play a much more important role in surface and sub-surface chemistry than generally appreciated, possibly explaining the low abundance of sulfur-containing molecules and the lack of ozone observed in comets and interstellar ices.
C1 [Loeffler, Mark J.; Hudson, Reggie L.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Code 691, Greenbelt, MD 20771 USA.
RP Loeffler, MJ (reprint author), NASA, Goddard Space Flight Ctr, Astrochem Lab, Code 691, Greenbelt, MD 20771 USA.
EM mark.loeffler@nasa.gov
FU NASA's Outer Planets Research Program; NASA Astrobiology Institute's
Goddard Center for Astrobiology
FX This work was supported by NASA's Outer Planets Research Program and the
NASA Astrobiology Institute's Goddard Center for Astrobiology.
NR 30
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U1 3
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD DEC 10
PY 2016
VL 833
IS 1
AR L9
DI 10.3847/2041-8213/833/1/L9
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EF5BI
UT WOS:000390345300001
ER
PT J
AU Mishchenko, MI
Dlugach, JM
Liu, L
AF Mishchenko, Michael I.
Dlugach, Janna M.
Liu, Li
TI Linear depolarization of lidar returns by aged smoke particles
SO APPLIED OPTICS
LA English
DT Article
ID SPECTRAL-RESOLUTION LIDAR; AEROSOL LIGHT-ABSORPTION; OPTICAL-PROPERTIES;
NONSPHERICAL PARTICLES; BLACK CARBON; SOOT; SCATTERING; HYGROSCOPICITY;
DEPENDENCE; MORPHOLOGY
AB We use the numerically exact (superposition) T-matrix method to analyze recent measurements of the backscattering linear depolarization ratio (LDR) for a plume of aged smoke at lidar wavelengths ranging from 355 to 1064 nm. We show that the unique spectral dependence of the measured LDRs can be modeled, but only by assuming expressly nonspherical morphologies of smoke particles containing substantial amounts of nonabsorbing (or weakly absorbing) refractory materials such as sulfates. Our results demonstrate that spectral backscattering LDR measurements can be indicative of the presence of morphologically complex smoke particles, but additional (e.g., passive polarimetric or bistatic lidar) measurements may be required for a definitive characterization of the particle morphology and composition. (C) 2016 Optical Society of America
C1 [Mishchenko, Michael I.; Liu, Li] NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
[Dlugach, Janna M.] Natl Acad Sci Ukraine, Main Astron Observ, 27 Zabolotny Str, UA-03680 Kiev, Ukraine.
[Liu, Li] Columbia Univ, New York, NY 10025 USA.
RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM michael.i.mishchenko@nasa.gov
FU National Aeronautics and Space Administration (NASA) ACE Project;
National Academy of Sciences of Ukraine Main Astronomical Observatory
GRAPE/GPU/GRID Computing Cluster Project; NASA Remote Sensing Theory
Program
FX National Aeronautics and Space Administration (NASA) ACE Project, NASA
Remote Sensing Theory Program; National Academy of Sciences of Ukraine
Main Astronomical Observatory GRAPE/GPU/GRID Computing Cluster Project.
NR 44
TC 0
Z9 0
U1 6
U2 6
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD DEC 10
PY 2016
VL 55
IS 35
BP 9968
EP 9973
DI 10.1364/AO.55.009968
PG 6
WC Optics
SC Optics
GA EE5MQ
UT WOS:000389652600010
PM 27958398
ER
PT J
AU Errera, Q
Ceccherini, S
Christophe, Y
Chabrillat, S
Hegglin, MI
Lambert, A
Menard, R
Raspollini, P
Skachko, S
van Weele, M
Walker, KA
AF Errera, Quentin
Ceccherini, Simone
Christophe, Yves
Chabrillat, Simon
Hegglin, Michaela I.
Lambert, Alyn
Menard, Richard
Raspollini, Piera
Skachko, Sergey
van Weele, Michiel
Walker, Kaley A.
TI Harmonisation and diagnostics of MIPAS ESA CH4 and N2O profiles using
data assimilation
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID STRATOSPHERIC CHEMISTRY; CHEMICAL OBSERVATIONS; 4D-VAR ASSIMILATION;
TRANSPORT MODEL; NITROUS-OXIDE; ERA-INTERIM; METHANE; VALIDATION;
SYSTEM; REANALYSIS
AB This paper discusses assimilation experiments of methane (CH4) and nitrous oxide (N2O) profiles retrieved from the Michelson Interferometer for Passive Atmospheric Sounding (MIPAS). Here we focus on data versions 6 and 7 provided by the ESA processor. These data sets have been assimilated by the Belgian Assimilation System for Chemical ObsErvations (BASCOE). The CH4 and N2O retrieved profiles can oscillate, especially in the tropical lower stratosphere. Using the averaging kernels of the observations and a background error covariance matrix, which has previously been calibrated, allows the system to partly remedy this issue and provide assimilated fields that are more regular vertically. In general, there is a good agreement between the BASCOE analyses and independent observations from ACE-FTS (CH4 and N2O) and MLS (N2O), demonstrating the general good quality of CH4 and N2O retrievals provided by MIPAS ESA. Nevertheless, this study also identifies two issues in these data sets. First, time series of the observations show unexpected discontinuities due to an abrupt change in the gain of MIPAS band B, generally occurring after the instrument decontamination. Since the calibration is performed weekly, the abrupt change in the gain affects the measurements until the subsequent calibration is performed. Second, the correlations between BASCOE analyses and independent observations are poor in the lower stratosphere, especially in the tropics, probably due to the presence of outliers in the assimilated data. In this region, we recommend using MIPAS CH4 and N2O retrievals with caution.
C1 [Errera, Quentin; Christophe, Yves; Chabrillat, Simon; Skachko, Sergey] Belgian Inst Space Aeron BIRA IASB, Brussels, Belgium.
[Ceccherini, Simone] CNR, Ist Fis Applicata N Carrara IFAC, Florence, Italy.
[Hegglin, Michaela I.] Univ Reading, Dept Meteorol, Reading, Berks, England.
[Lambert, Alyn; Raspollini, Piera] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Menard, Richard] Environm & Climate Change Canada, Air Qual Res Div, Dorval, PQ, Canada.
[van Weele, Michiel] Royal Netherlands Meteorol Inst KNMI, De Bilt, Netherlands.
[Walker, Kaley A.] Univ Toronto, Dept Phys, Toronto, ON, Canada.
[Walker, Kaley A.] Univ Waterloo, Dept Chem, Waterloo, ON, Canada.
RP Errera, Q (reprint author), Belgian Inst Space Aeron BIRA IASB, Brussels, Belgium.
EM quentin@oma.be
RI Hegglin, Michaela/D-7528-2017
OI Hegglin, Michaela/0000-0003-2820-9044
FU International Space Science Institute (ISSI); Canadian Space Agency
(CSA)
FX This study was initiated by the study group on the added value of
chemical data assimilation in the stratosphere and upper troposphere,
sponsored by the International Space Science Institute (ISSI). Work at
the Jet Propulsion Laboratory, California Institute of Technology, was
carried out under a contract with the National Aeronautics and Space
Administration. Funding for ACE is provided mainly by the Canadian Space
Agency (CSA). MIPAS L2 ESA v7 products were kindly provided by ESA for
the tests reported in this paper before the official release.
NR 44
TC 0
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U1 2
U2 2
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1867-1381
EI 1867-8548
J9 ATMOS MEAS TECH
JI Atmos. Meas. Tech.
PD DEC 9
PY 2016
VL 9
IS 12
BP 5895
EP 5909
DI 10.5194/amt-9-5895-2016
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EG1CE
UT WOS:000390768400001
ER
PT J
AU Tiranov, A
Strassmann, PC
Lavoie, J
Brunner, N
Huber, M
Verma, VB
Nam, SW
Mirin, RP
Lita, AE
Marsili, F
Afzelius, M
Bussieres, F
Gisin, N
AF Tiranov, Alexey
Strassmann, Peter C.
Lavoie, Jonathan
Brunner, Nicolas
Huber, Marcus
Verma, Varun B.
Nam, Sae Woo
Mirin, Richard P.
Lita, Adriana E.
Marsili, Francesco
Afzelius, Mikael
Bussieres, Felix
Gisin, Nicolas
TI Temporal Multimode Storage of Entangled Photon Pairs
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID ATOMIC ENSEMBLES; QUANTUM MEMORY; LINEAR OPTICS; LIGHT; COMMUNICATION;
REPEATERS; INTERFACE; DISTANCE; FIBER
AB Multiplexed quantum memories capable of storing and processing entangled photons are essential for the development of quantum networks. In this context, we demonstrate and certify the simultaneous storage and retrieval of two entangled photons inside a solid-state quantum memory and measure a temporal multimode capacity of ten modes. This is achieved by producing two polarization-entangled pairs from parametric down-conversion and mapping one photon of each pair onto a rare-earth-ion-doped (REID) crystal using the atomic frequency comb (AFC) protocol. We develop a concept of indirect entanglement witnesses, which can be used as Schmidt number witnesses, and we use it to experimentally certify the presence of more than one entangled pair retrieved from the quantum memory. Our work puts forward REID-AFC as a platform compatible with temporal multiplexing of several entangled photon pairs along with a new entanglement certification method, useful for the characterization of multiplexed quantum memories.
C1 [Tiranov, Alexey; Strassmann, Peter C.; Lavoie, Jonathan; Huber, Marcus; Afzelius, Mikael; Bussieres, Felix; Gisin, Nicolas] Univ Geneva, Grp Phys Appl, CH-1211 Geneva, Switzerland.
[Brunner, Nicolas] Univ Geneva, Dept Phys Theor, CH-1211 Geneva, Switzerland.
[Huber, Marcus] Austrian Acad Sci, IQOQI, Boltzmanngasse 3, A-1090 Vienna, Austria.
[Verma, Varun B.; Nam, Sae Woo; Mirin, Richard P.; Lita, Adriana E.] NIST, 325 Broadway, Boulder, CO 80305 USA.
[Gisin, Nicolas] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Lavoie, Jonathan] Univ Oregon, Dept Phys, Eugene, OR 97403 USA.
[Lavoie, Jonathan] Univ Oregon, Oregon Ctr Opt Mol & Quantum Sci, Eugene, OR 97403 USA.
RP Lavoie, J (reprint author), Univ Geneva, Grp Phys Appl, CH-1211 Geneva, Switzerland.; Lavoie, J (reprint author), Univ Oregon, Dept Phys, Eugene, OR 97403 USA.; Lavoie, J (reprint author), Univ Oregon, Oregon Ctr Opt Mol & Quantum Sci, Eugene, OR 97403 USA.
EM jlavoie@uoregon.edu
RI Huber, Marcus/G-2925-2010; Strassmann, Peter/A-9634-2016; Afzelius,
Mikael/N-5825-2016; Bussieres, Felix/E-5384-2011
OI Huber, Marcus/0000-0003-1985-4623; Strassmann,
Peter/0000-0002-6150-7492; Afzelius, Mikael/0000-0001-8367-6820;
Bussieres, Felix/0000-0003-0234-175X
FU European Research Council (ERC-AG MEC); Swiss National Science
Foundation (SNSF); Natural Sciences and Engineering Research Council of
Canada (NSERC); Swiss National Science Foundation [PP00P2-138917,
AMBIZIONE Z00P2-161351]; Austrian Science Fund (FWF) through the START
Project [Y879-N27]
FX We thank Marc-Olivier Renou and Marc Maetz for useful discussions, Boris
Korzh for help with the detectors, Alban Ferrier and Philippe Goldner
for the crystals and Harald Herrmann and Christine Silberhorn for
lending one of the nonlinear waveguides. This work was financially
supported by the European Research Council (ERC-AG MEC) and the Swiss
National Science Foundation (SNSF). J. L. was supported by the Natural
Sciences and Engineering Research Council of Canada (NSERC). N. B
acknowledges Swiss National Science Foundation (Grant No. PP00P2-138917
and Starting grant DIAQ). M. H would like to acknowledge funding from
the Swiss National Science Foundation (AMBIZIONE Z00P2-161351) and the
Austrian Science Fund (FWF) through the START Project Y879-N27.
NR 45
TC 0
Z9 0
U1 7
U2 7
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
EI 1079-7114
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD DEC 9
PY 2016
VL 117
IS 24
AR 240506
DI 10.1103/PhysRevLett.117.240506
PG 6
WC Physics, Multidisciplinary
SC Physics
GA EE4MO
UT WOS:000389576600001
PM 28009181
ER
PT J
AU Roman, NG
AF Roman, Nancy Grace
TI Following my lucky star
SO SCIENCE
LA English
DT Editorial Material
C1 [Roman, Nancy Grace] NASA, Astron Program, Washington, DC 20024 USA.
[Roman, Nancy Grace] NASA, Relat Program, Washington, DC 20024 USA.
RP Roman, NG (reprint author), NASA, Astron Program, Washington, DC 20024 USA.
NR 0
TC 0
Z9 0
U1 1
U2 1
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD DEC 9
PY 2016
VL 354
IS 6317
BP 1346
EP 1346
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EE4TS
UT WOS:000389598800065
PM 27940878
ER
PT J
AU Scott, VJ
Manohara, H
Toda, R
Del Castillo, L
Murthy, R
Mulder, J
Murty, E
Thompson, MC
AF Scott, Valerie J.
Manohara, Harish
Toda, Risaku
Del Castillo, Linda
Murthy, Rakesh
Mulder, Jerry
Murty, Eshwari
Thompson, M. Clark
TI Robust CNT field emitters: patterning, growth, transfer, and in situ
anchoring
SO NANOTECHNOLOGY
LA English
DT Article
DE carbon nanotubes; field emission; vacuum electronics; low operating
fields; carbon nanotube vacuum triode
ID CARBON NANOTUBE ARRAYS; SILICON; FABRICATION; EMISSION; ATTACHMENT
AB Robust carbon nanotube (CNT)-based cold cathodes were fabricated on titanium (Ti) substrates. Methods to grow vertically aligned CNTs. directly on Ti substrates were developed. These cathodes can be treated post-growth at elevated temperatures under inert atmosphere which causes the surface-grown CNTs to become anchored to the substrate surface. These samples offer improvements in field emission properties over previously studied silicon (Si) substrate-based cathodes with no anchoring, displaying low threshold voltages, high field enhancement factors, and long operating lifetimes. Current densities of 25 mA cm(-2) were held for over 24 h with anchored samples at low electric fields (observed thresholds as low as 0.5 V mu m(-1)) and more current stability. Higher current densities of up to 150 mA cm(-2) could be reached with anchored samples, limited only by the experimental setup. In efforts to generate even more stable and reproducible field emission, a transfer process of CNTs from polished Si to Ti with copper (Cu) was developed (flipCNTs). These cathodes display extreme improvements over previous results, with observed thresholds as low as 0.2 V mu m(-1) and gamma-factors as high as 30 000. To demonstrate the utility of these robust cathodes, a flipCNT-based cathode was assembled into a fully functioning vacuum triode.
C1 [Scott, Valerie J.; Manohara, Harish; Toda, Risaku; Del Castillo, Linda; Murthy, Rakesh; Mulder, Jerry; Murty, Eshwari] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91108 USA.
[Thompson, M. Clark] Chevron Energy Technol Co, Santa Fe, NM USA.
RP Scott, VJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91108 USA.
EM Valerie.j.scott@jpl.nasa.gov
FU Chevron Energy Technology Corporation, a division of Chevron USA, Inc.
(Chevron)
FX This work was carried out with funding from the Chevron Energy
Technology Corporation, a division of Chevron USA, Inc. (Chevron). This
research was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration. We sincerely thank Manuel Gonzalez, Donna
Auzenne, Waqar Qureshi of Chevron for valuable discussions on this
subject, and their deep insight from the application perspective that
helped shape the research. We thank David Charlesworth of Chevron and
Dean Wiberg of JPL for their guidance during the execution of this work.
Our sincere gratitude to Lauren Montemayor who helped with paper
editing.
NR 24
TC 0
Z9 0
U1 13
U2 13
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0957-4484
EI 1361-6528
J9 NANOTECHNOLOGY
JI Nanotechnology
PD DEC 9
PY 2016
VL 27
IS 49
AR 494002
DI 10.1088/0957-4484/27/49/494002
PG 9
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA EC6GD
UT WOS:000388233600001
PM 27827343
ER
PT J
AU Marchenko, SV
DeLand, MT
Lean, JL
AF Marchenko, Sergey V.
DeLand, Matthew T.
Lean, Judith L.
TI Solar spectral irradiance variability in cycle 24: observations and
models
SO JOURNAL OF SPACE WEATHER AND SPACE CLIMATE
LA English
DT Article
DE Sun; Solar activity; Spectral irradiance
ID OZONE MONITORING INSTRUMENT; II SOLSTICE-II; BACKSCATTERED ULTRAVIOLET;
UV IRRADIANCE; NETWORK; SUN; DESIGN; RECONSTRUCTION; VALIDATION;
RESOLUTION
AB Utilizing the excellent stability of the Ozone Monitoring Instrument (OMI), we characterize both short-term (solar rotation) and long-term (solar cycle) changes of the solar spectral irradiance (SSI) between 265 and 500 nm during the ongoing cycle 24. We supplement the OMI data with concurrent observations from the Global Ozone Monitoring Experiment-2 (GOME-2) and Solar Radiation and Climate Experiment (SORCE) instruments and find fair-to-excellent, depending on wavelength, agreement among the observations, and predictions of the Naval Research Laboratory Solar Spectral Irradiance (NRLSSI2) and Spectral And Total Irradiance REconstruction for the Satellite era (SATIRE-S) models.
C1 [Marchenko, Sergey V.; DeLand, Matthew T.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Marchenko, Sergey V.; DeLand, Matthew T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lean, Judith L.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA.
RP Marchenko, SV (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA.; Marchenko, SV (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM sergey_marchenko@ssaihq.com
FU NASA [NNG12HP08C, NNH15CN67C]; NASA SIST Program; NOAA CDR Program
FX We thank the anonymous referees for numerous helpful comments. Part of
this work was supported by NASA Grants NNG12HP08C and NNH15CN67C. J.
Lean acknowledges the support of the NASA SIST and NOAA CDR Programs,
and appreciates ongoing collaboration with Odele Coddington in producing
the NRLSSI2 CDR. We gratefully acknowledge Kok Leng Yeo for discussions
and interpretation of the SATIRE-S model results. The article used the
SATIRE-S data available at
https://www2.mps.mpg.de/projects/sun-climate/data.html. We also used the
Aura/OMI data distributed via http://disc.sci.gsfc.nasa.gov/Aura, as
well as the SSI measurements obtained by SORCE/SIM, SORCE/SOLSTICE
(NASA), and EUMETSAT/GOME-2 (ESA). The editor thanks two anonymous
referees for their assistance in evaluating this paper.
NR 51
TC 0
Z9 0
U1 3
U2 3
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 2115-7251
J9 J SPACE WEATHER SPAC
JI J. Space Weather Space Clim.
PD DEC 8
PY 2016
VL 6
AR A40
DI 10.1051/swsc/2016036
PG 12
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA EG4EN
UT WOS:000390996500001
ER
PT J
AU Bloom, AA
Lauvaux, T
Worden, J
Yadav, V
Duren, R
Sander, SP
Schimel, DS
AF Bloom, A. Anthony
Lauvaux, Thomas
Worden, John
Yadav, Vineet
Duren, Riley
Sander, Stanley P.
Schimel, David S.
TI What are the greenhouse gas observing system requirements for reducing
fundamental biogeochemical process uncertainty? Amazon wetland CH4
emissions as a case study
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID TERRESTRIAL CARBON-CYCLE; METHANE EMISSIONS; ATMOSPHERIC METHANE;
NATURAL WETLANDS; NORTH-AMERICA; SATELLITE-OBSERVATIONS; SENTINEL-5
PRECURSOR; REFERENCE NETWORK; CO2; MODEL
AB Understanding the processes controlling terrestrial carbon fluxes is one of the grand challenges of climate science. Carbon cycle process controls are readily studied at local scales, but integrating local knowledge across extremely heterogeneous biota, landforms and climate space has proven to be extraordinarily challenging. Consequently, top-down or integral flux constraints at process-relevant scales are essential to reducing process uncertainty. Future satellite-based estimates of greenhouse gas fluxes - such as CO2 and CH4 - could potentially provide the constraints needed to resolve biogeochemical process controls at the required scales. Our analysis is focused on Amazon wetland CH4 emissions, which amount to a scientifically crucial and methodologically challenging case study. We quantitatively derive the observing system (OS) requirements for testing wetland CH4 emission hypotheses at a process-relevant scale. To distinguish between hypothesized hydrological and carbon controls on Amazon wetland CH4 production, a satellite mission will need to resolve monthly CH4 fluxes at a similar to 333 km resolution and with a <= 10 mg CH4 m(-2) day(-1) flux precision. We simulate a range of low-earth orbit (LEO) and geostationary orbit (GEO) CH4 OS configurations to evaluate the ability of these approaches to meet the CH4 flux requirements. Conventional LEO and GEO missions resolve monthly similar to 333 km Amazon wetland fluxes at a 17.0 and 2.7 mg CH4 m(-2) day(-1) median uncertainty level. Improving LEO CH4 measurement precision by root 2 would only reduce the median CH4 flux uncertainty to 11.9 mg CH4 m(-2) day(-1). A GEO mission with targeted observing capability could resolve fluxes at a 2.0-2.4 mg CH4 m(-2) day(-1) median precision by increasing the observation density in high cloud-cover regions at the expense of other parts of the domain. We find that residual CH4 concentration biases can potentially reduce the similar to 5-fold flux CH4 precision advantage of a GEO mission to a similar to 2-fold advantage (relative to a LEO mission). For residual CH4 bias correlation lengths of 100 km, the GEO can nonetheless meet the <= 10 mg CH4 m(-2) day(-1) requirements for systematic biases <= 10 ppb. Our study demonstrates that process-driven greenhouse gas OS simulations can enhance conventional uncertainty reduction assessments by quantifying the OS characteristics required for testing biogeochemical process hypotheses.
C1 [Bloom, A. Anthony; Lauvaux, Thomas; Worden, John; Yadav, Vineet; Duren, Riley; Sander, Stanley P.; Schimel, David S.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Lauvaux, Thomas] Penn State Univ, Dept Meteorol, 503 Walker Bldg, University Pk, PA 16802 USA.
RP Bloom, AA (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM abloom@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX The research was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration.
NR 68
TC 0
Z9 0
U1 11
U2 11
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PD DEC 8
PY 2016
VL 16
IS 23
BP 15199
EP 15218
DI 10.5194/acp-16-15199-2016
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EF9KO
UT WOS:000390649300003
ER
PT J
AU Lambert, A
Santee, ML
Livesey, NJ
AF Lambert, Alyn
Santee, Michelle L.
Livesey, Nathaniel J.
TI Interannual variations of early winter Antarctic polar stratospheric
cloud formation and nitric acid observed by CALIOP and MLS
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID LARGE HNO3-CONTAINING PARTICLES; ARCTIC STRATOSPHERE; HETEROGENEOUS
FORMATION; SPECTROSCOPIC EVIDENCE; OPTICAL-CONSTANTS; TRIHYDRATE NAT;
OZONE LOSS; ICE; DENITRIFICATION; NUCLEATION
AB We use satellite-borne measurements collected over the last decade (2006-2015) from the Aura Microwave Limb Sounder (MLS) and the Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) to investigate the nitric acid distribution and the properties of polar stratospheric clouds (PSCs) in the early winter Antarctic vortex. Frequently, at the very start of the winter, we find that synoptic-scale depletion of HNO3 can be detected in the inner vortex before the first lidar detection of geophysically associated PSCs. The generation of "sub-visible" PSCs can be explained as arising from the development of a solid particle population with low number densities and large particle sizes. Assumed to be composed of nitric acid trihydrate (NAT), the sub-visible PSCs form at ambient temperatures well above the ice frost point, but also above the temperature at which supercooled ternary solution (STS) grows out of the background supercooled binary solution (SBS) distribution. The temperature regime of their formation, inferred from the simultaneous uptake of ambient HNO3 into NAT and their Lagrangian temperature histories, is at a depression of a few kelvin with respect to the NAT existence threshold, T-NAT. Therefore, their nucleation requires a considerable supersaturation of HNO3 over NAT, and is consistent with a recently described heterogeneous nucleation process on solid foreign nuclei immersed in liquid aerosol. We make a detailed investigation of the comparative limits of detection of PSCs and the resulting sequestration of HNO3 imposed by lidar, mid-infrared, and microwave techniques. We find that the temperature history of air parcels, in addition to the local ambient temperature, is an important factor in the relative frequency of formation of liquid/solid PSCs. We conclude that the initiation of NAT nucleation and the subsequent development of large NAT particles capable of sedimentation and denitrification in the early winter do not emanate from an ice-seeding process. Finally, we investigate the patterns of interannual variability and compare the relative formation frequency of liquid and solid PSCs in the Antarctic lower polar stratosphere using the results of a cluster analysis to synthesize the combined CALIOP and MLS measurements into a relatively small number of interrelated categories.
C1 [Lambert, Alyn; Santee, Michelle L.; Livesey, Nathaniel J.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Lambert, A (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM alyn.lambert@jpl.nasa.gov
FU National Aeronautics and Space Administration; World Climate Research
Programme; International Space Science Institute (ISSI), Bern,
Switzerland of the Polar Stratospheric Cloud initiative
FX We gratefully acknowledge members of the teams associated with the
CALIOP and MLS instruments, and the GEOS-5 meteorological analyses. Work
at the Jet Propulsion Laboratory, California Institute of Technology,
was carried out under a contract with the National Aeronautics and Space
Administration. We acknowledge the scientific guidance and sponsorship
of the World Climate Research Programme, coordinated in the framework of
the SPARC (Stratosphere-troposphere Processes And their Role in Climate)
Polar Stratospheric Clouds activity. We acknowledge the International
Space Science Institute (ISSI), Bern, Switzerland, for their support of
the Polar Stratospheric Cloud initiative. We thank the anonymous
reviewers for their careful reading of the manuscript and their comments
and suggestions.
NR 65
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Z9 0
U1 2
U2 2
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1680-7316
EI 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PD DEC 8
PY 2016
VL 16
IS 23
BP 15219
EP 15246
DI 10.5194/acp-16-15219-2016
PG 28
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EF9KO
UT WOS:000390649300004
ER
PT J
AU Werner, F
Wind, G
Zhang, ZB
Platnick, S
Di Girolamo, L
Zhao, GY
Amarasinghe, N
Meyer, K
AF Werner, Frank
Wind, Galina
Zhang, Zhibo
Platnick, Steven
Di Girolamo, Larry
Zhao, Guangyu
Amarasinghe, Nandana
Meyer, Kerry
TI Marine boundary layer cloud property retrievals from high-resolution
ASTER observations: case studies and comparison with Terra MODIS
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID SPACEBORNE THERMAL EMISSION; REFLECTION RADIOMETER ASTER; TRADE-WIND
CUMULI; RADIATIVE-TRANSFER; OPTICAL-THICKNESS; LAND-COVER; CLEAR-SKY;
MULTIPLE-SCATTERING; SPATIAL-RESOLUTION; INDEPENDENT PIXEL
AB A research-level retrieval algorithm for cloud optical and microphysical properties is developed for the Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) aboard the Terra satellite. It is based on the operational MODIS algorithm. This paper documents the technical details of this algorithm and evaluates the retrievals for selected marine boundary layer cloud scenes through comparisons with the operational MODIS Data Collection 6 (C6) cloud product. The newly developed, ASTER-specific cloud masking algorithm is evaluated through comparison with an independent algorithm reported in Zhao and Di Girolamo (2006). To validate and evaluate the cloud optical thickness (tau) and cloud effective radius (r(eff)) from ASTER, the high-spatial-resolution ASTER observations are first aggregated to the same 1000m resolution as MODIS. Subsequently, tau(aA) and r(eff, aA) retrieved from the aggregated ASTER radiances are compared with the collocated MODIS retrievals. For overcast pixels, the two data sets agree very well with Pearson's product-moment correlation coefficients of R > 0.970. However, for partially cloudy pixels there are significant differences between r(eff, aA) and the MODIS results which can exceed 10 mu m. Moreover, it is shown that the numerous delicate cloud structures in the example marine boundary layer scenes, resolved by the high-resolution ASTER retrievals, are smoothed by the MODIS observations. The overall good agreement between the research-level ASTER results and the operational MODIS C6 products proves the feasibility of MODIS-like retrievals from ASTER reflectance measurements and provides the basis for future studies concerning the scale dependency of satellite observations and three-dimensional radiative effects.
C1 [Werner, Frank] Joint Ctr Earth Syst Technol, 5523 Res Pk Dr, Baltimore, MD 21228 USA.
[Wind, Galina; Platnick, Steven; Meyer, Kerry] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Zhang, Zhibo] Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21228 USA.
[Di Girolamo, Larry; Zhao, Guangyu] Univ Illinois, Dept Atmospher Sci, 105 South Gregory St, Urbana, IL 61801 USA.
[Amarasinghe, Nandana] NASA, Sci Syst & Applicat Inc, GSFC, Greenbelt, MD 20771 USA.
[Meyer, Kerry] Univ Space Res Assoc, Goddard Earth Sci Technol & Res GESTAR, Columbia, MD 21046 USA.
RP Werner, F (reprint author), Joint Ctr Earth Syst Technol, 5523 Res Pk Dr, Baltimore, MD 21228 USA.
EM frankw@umbc.edu
RI Zhang, Zhibo/D-1710-2010; Meyer, Kerry/E-8095-2016
OI Zhang, Zhibo/0000-0001-9491-1654; Meyer, Kerry/0000-0001-5361-9200
FU NASA [NNX14AJ25G, NNX15AC77G]; U.S. National Science Foundation through
the MRI program [CNS-0821258, CNS-1228778]; U.S. National Science
Foundation through SCREMS program [DMS-0821311]
FX This study is supported by NASA grants NNX14AJ25G and NNX15AC77G. The
hardware used in the computational studies is part of the UMBC High
Performance Computing Facility (HPCF). The facility is supported by the
U.S. National Science Foundation through the MRI program (grant nos.
CNS-0821258 and CNS-1228778) and the SCREMS program (grant no.
DMS-0821311), with additional substantial support from the University of
Maryland, Baltimore County (UMBC).
NR 77
TC 0
Z9 0
U1 1
U2 1
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1867-1381
EI 1867-8548
J9 ATMOS MEAS TECH
JI Atmos. Meas. Tech.
PD DEC 8
PY 2016
VL 9
IS 12
BP 5869
EP 5894
DI 10.5194/amt-9-5869-2016
PG 26
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EF9KT
UT WOS:000390649800002
ER
PT J
AU Barrila, J
Ott, CM
LeBlanc, C
Mehta, SK
Crabbe, A
Stafford, P
Pierson, DL
Nickerson, CA
AF Barrila, Jennifer
Ott, C. Mark
LeBlanc, Carly
Mehta, Satish K.
Crabbe, Aurelie
Stafford, Phillip
Pierson, Duane L.
Nickerson, Cheryl A.
TI Spaceflight modulates gene expression in the whole blood of astronauts
SO NPJ MICROGRAVITY
LA English
DT Article
ID EPSTEIN-BARR-VIRUS; SPACE-FLIGHT; LYMPHOCYTES
AB Astronauts are exposed to a unique combination of stressors during spaceflight, which leads to alterations in their physiology and potentially increases their susceptibility to disease, including infectious diseases. To evaluate the potential impact of the spaceflight environment on the regulation of molecular pathways mediating cellular stress responses, we performed a first-of-its-kind pilot study to assess spaceflight-related gene-expression changes in the whole blood of astronauts. Using an array comprised of 234 well-characterized stress-response genes, we profiled transcriptomic changes in six astronauts (four men and two women) from blood preserved before and immediately following the spaceflight. Differentially regulated transcripts included those important for DNA repair, oxidative stress, and protein folding/degradation, including HSP90AB1, HSP27, GPX1, XRCC1, BAG-1, HHR23A, FAP48, and C-FOS. No gender-specific differences or relationship to number of missions flown was observed. This study provides a first assessment of transcriptomic changes occurring in the whole blood of astronauts in response to spaceflight.
C1 [Barrila, Jennifer; Crabbe, Aurelie; Nickerson, Cheryl A.] Arizona State Univ, Ctr Infect Dis & Vaccinol, Biodesign Inst, Tempe, AZ 85281 USA.
[Ott, C. Mark; Pierson, Duane L.] NASA, Biomed Res & Environm Sci Div, Johnson Space Ctr, Houston, TX USA.
[LeBlanc, Carly; Nickerson, Cheryl A.] Tulane Univ, Dept Microbiol & Immunol, Program Mol Pathogenesis & Immun, Hlth Sci Ctr, New Orleans, LA 70118 USA.
[Mehta, Satish K.] EASI Wyle Labs, Houston, TX USA.
[Stafford, Phillip] Arizona State Univ, Ctr Innovat Med, Biodesign Inst, Tempe, AZ USA.
[Nickerson, Cheryl A.] Arizona State Univ, Sch Life Sci, Tempe, AZ 85281 USA.
[Crabbe, Aurelie] Univ Ghent, Lab Pharmaceut Microbiol, Ottergemsesteenweg 460, Ghent, Belgium.
RP Nickerson, CA (reprint author), Arizona State Univ, Ctr Infect Dis & Vaccinol, Biodesign Inst, Tempe, AZ 85281 USA.; Nickerson, CA (reprint author), Tulane Univ, Dept Microbiol & Immunol, Program Mol Pathogenesis & Immun, Hlth Sci Ctr, New Orleans, LA 70118 USA.; Nickerson, CA (reprint author), Arizona State Univ, Sch Life Sci, Tempe, AZ 85281 USA.
EM cheryl.nickerson@asu.edu
FU USRA Sponsor Award [09930-286-01 (017991-001)]
FX We thank the NASA astronauts who so generously participated in these
flight studies. We apologize to any authors whose work could not be
cited due to space limitations. This work was funded by USRA Sponsor
Award 09930-286-01 (017991-001). We also thank Andrea Throop for helpful
discussions during the writing of this manuscript.
NR 18
TC 0
Z9 0
U1 3
U2 3
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 2373-8065
J9 NPJ MICROGRAVITY
JI NPJ Microgravity
PD DEC 8
PY 2016
VL 2
AR 16039
DI 10.1038/npjmgrav.2016.39
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EF6YD
UT WOS:000390476300001
ER
PT J
AU Armano, M
Audley, H
Auger, G
Baird, J
Binetruy, P
Born, M
Bortoluzzi, D
Brandt, N
Bursi, A
Caleno, M
Cavalleri, A
Cesarini, A
Cruise, M
Danzmann, K
Silva, MD
Desiderio, D
Piersanti, E
Diepholz, I
Dolesi, R
Dunbar, N
Ferraioli, L
Ferroni, V
Fitzsimons, E
Flatscher, R
Freschi, M
Gallegos, J
Marirrodriga, CG
Gerndt, R
Gesa, L
Gibert, F
Giardini, D
Giusteri, R
Grimani, C
Grzymisch, J
Harrison, I
Heinzel, G
Hewitson, M
Hollington, D
Hueller, M
Huesler, J
Inchauspe, H
Jennrich, O
Jetzer, P
Johlander, B
Karnesis, N
Kaune, B
Korsakova, N
Killow, C
Lloro, I
Liu, L
Lopez-Zaragoza, JP
Maarschalkerweerd, R
Madden, S
Mance, D
Martin, V
Martin-Polo, L
Martino, J
Martin-Porqueras, F
Mateos, I
McNamara, PW
Mendes, J
Mendes, L
Moroni, A
Nofrarias, M
Paczkowski, S
Perreur-Lloyd, M
Petiteau, A
Pivato, P
Plagnol, E
Prat, P
Ragnit, U
Ramos-Castro, J
Reiche, J
Perez, JAR
Robertson, D
Rozemeijer, H
Rivas, F
Russano, G
Sarra, P
Schleicher, A
Slutsky, J
Sopuerta, CF
Sumner, T
Texier, D
Thorpe, JI
Tomlinson, R
Trenkel, C
Vetrugno, D
Vitale, S
Wanner, G
Ward, H
Warren, C
Wass, PJ
Wealthy, D
Weber, WJ
Wittchen, A
Zanoni, C
Ziegler, T
Zweifel, P
AF Armano, M.
Audley, H.
Auger, G.
Baird, J.
Binetruy, P.
Born, M.
Bortoluzzi, D.
Brandt, N.
Bursi, A.
Caleno, M.
Cavalleri, A.
Cesarini, A.
Cruise, M.
Danzmann, K.
de Deus Silva, M.
Desiderio, D.
Piersanti, E.
Diepholz, I.
Dolesi, R.
Dunbar, N.
Ferraioli, L.
Ferroni, V.
Fitzsimons, E.
Flatscher, R.
Freschi, M.
Gallegos, J.
Marirrodriga, C. Garcia
Gerndt, R.
Gesa, L.
Gibert, F.
Giardini, D.
Giusteri, R.
Grimani, C.
Grzymisch, J.
Harrison, I.
Heinzel, G.
Hewitson, M.
Hollington, D.
Hueller, M.
Huesler, J.
Inchauspe, H.
Jennrich, O.
Jetzer, P.
Johlander, B.
Karnesis, N.
Kaune, B.
Korsakova, N.
Killow, C.
Lloro, I.
Liu, L.
Lopez-Zaragoza, J. P.
Maarschalkerweerd, R.
Madden, S.
Mance, D.
Martin, V.
Martin-Polo, L.
Martino, J.
Martin-Porqueras, F.
Mateos, I.
McNamara, P. W.
Mendes, J.
Mendes, L.
Moroni, A.
Nofrarias, M.
Paczkowski, S.
Perreur-Lloyd, M.
Petiteau, A.
Pivato, P.
Plagnol, E.
Prat, P.
Ragnit, U.
Ramos-Castro, J.
Reiche, J.
Perez, J. A. Romera
Robertson, D.
Rozemeijer, H.
Rivas, F.
Russano, G.
Sarra, P.
Schleicher, A.
Slutsky, J.
Sopuerta, C. F.
Sumner, T.
Texier, D.
Thorpe, J. I.
Tomlinson, R.
Trenkel, C.
Vetrugno, D.
Vitale, S.
Wanner, G.
Ward, H.
Warren, C.
Wass, P. J.
Wealthy, D.
Weber, W. J.
Wittchen, A.
Zanoni, C.
Ziegler, T.
Zweifel, P.
TI Constraints on LISA Pathfinder's self-gravity: design requirements,
estimates and testing procedures
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article
DE self-gravity; differential accelerometer; LISA; LISA Pathfinder
AB LISA Pathfinder satellite was launched on 3 December 2015 toward the Sun-Earth first Lagrangian point (L1) where the LISA Technology Package (LTP), which is the main science payload, will be tested. LTP achieves measurements of differential acceleration of free-falling test masses (TMs) with sensitivity below 3 x 10(-14) m s(-2) Hz(-1/2) within the 1-30 mHz frequency band in one-dimension. The spacecraft itself is responsible for the dominant differential gravitational field acting on the two TMs. Such a force interaction could contribute a significant amount of noise and thus threaten the achievement of the targeted free-fall level. We prevented this by balancing the gravitational forces to the sub nm s(-2) level, guided by a protocol based on measurements of the position and the mass of all parts that constitute the satellite, via finite element calculation tool estimates. In this paper, we will introduce the gravitational balance requirements and design, and then discuss our predictions for the balance that will be achieved in flight.
C1 [Armano, M.; de Deus Silva, M.; Freschi, M.; Gallegos, J.; Martin-Polo, L.; Martin-Porqueras, F.; Mendes, L.; Texier, D.] European Space Agcy, European Space Astron Ctr, E-28692 Madrid, Spain.
[Audley, H.; Born, M.; Danzmann, K.; Diepholz, I.; Heinzel, G.; Hewitson, M.; Karnesis, N.; Kaune, B.; Korsakova, N.; Paczkowski, S.; Reiche, J.; Wanner, G.; Wittchen, A.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany.
[Audley, H.; Born, M.; Danzmann, K.; Diepholz, I.; Heinzel, G.; Hewitson, M.; Karnesis, N.; Kaune, B.; Korsakova, N.; Paczkowski, S.; Reiche, J.; Wanner, G.; Wittchen, A.] Leibniz Univ Hannover, D-30167 Hannover, Germany.
[Auger, G.; Binetruy, P.; Inchauspe, H.; Martino, J.; Petiteau, A.; Plagnol, E.; Prat, P.] Univ Paris Diderot, APC, UMR7164, Paris, France.
[Baird, J.; Hollington, D.; Sumner, T.; Wass, P. J.] Imperial Coll London, Dept Phys, Blackett Lab, High Energy Phys Grp, Prince Consort Rd, London SW7 2BW, England.
[Bortoluzzi, D.; Zanoni, C.] Univ Trento, Dept Ind Engn, Via Sommarive 9, I-38123 Trento, Italy.
[Bortoluzzi, D.; Bursi, A.; Cavalleri, A.; Cesarini, A.; Dolesi, R.; Ferroni, V.; Gibert, F.; Giusteri, R.; Hueller, M.; Liu, L.; Pivato, P.; Russano, G.; Vetrugno, D.; Vitale, S.; Weber, W. J.; Zanoni, C.] Trento Inst Fundamental Phys & Applicat INFN, Trento, Italy.
[Brandt, N.; Fitzsimons, E.; Flatscher, R.; Gerndt, R.; Schleicher, A.; Ziegler, T.] Airbus Def & Space, Claude Dornier Str, D-88090 Immenstaad, Germany.
[Bursi, A.; Desiderio, D.; Piersanti, E.; Moroni, A.; Sarra, P.] CGS SpA, Compagnia Gen Spazio, Via Gallarate,150, I-20151 Milan, Italy.
[Caleno, M.; Marirrodriga, C. Garcia; Grzymisch, J.; Huesler, J.; Jennrich, O.; Johlander, B.; Madden, S.; McNamara, P. W.; Ragnit, U.; Perez, J. A. Romera; Rozemeijer, H.] European Space Agcy, European Space Technol Ctr, Keplerlaan 1, NL-2200 AG Noordwijk, Netherlands.
[Cavalleri, A.] CNR, Fdn Bruno Kessler, Ist Foton & Nanotecnol, I-38123 Povo, Trento, Italy.
[Cesarini, A.; Dolesi, R.; Ferroni, V.; Gibert, F.; Giusteri, R.; Hueller, M.; Liu, L.; Pivato, P.; Russano, G.; Vetrugno, D.; Vitale, S.; Weber, W. J.] Univ Trento, Dipartimento Fis, I-38123 Povo, Trento, Italy.
[Dunbar, N.; Tomlinson, R.; Trenkel, C.; Warren, C.; Wealthy, D.] Airbus Def & Space, Gunnels Wood Rd, Stevenage SG1 2AS, Herts, England.
[Ferraioli, L.; Giardini, D.; Mance, D.; Zweifel, P.] Swiss Fed Inst Technol, Inst Geophys, Sonneggstr 5, CH-8092 Zurich, Switzerland.
[Gesa, L.; Lloro, I.; Lopez-Zaragoza, J. P.; Martin, V.; Mateos, I.; Nofrarias, M.; Rivas, F.; Sopuerta, C. F.] CSIC, IEEC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-n, E-08193 Cerdanyola Del Valles, Spain.
[Grimani, C.] Univ Urbino Carlo Bo, DiSBeF, Via S Chiara,27, I-61029 Urbino, Italy.
[Harrison, I.; Maarschalkerweerd, R.; Mendes, J.] European Space Agcy, European Space Operat Ctr, D-64293 Darmstadt, Germany.
[Jetzer, P.] Univ Zurich, Phys Inst, Winterthurerstr 190, CH-8057 Zurich, Switzerland.
[Killow, C.; Perreur-Lloyd, M.; Robertson, D.; Ward, H.] Univ Glasgow, Inst Gravitat Res, Sch Phys & Astron, SUPA, Glasgow G12 8QQ, Lanark, Scotland.
[Ramos-Castro, J.] Univ Politecn Cataluna, Dept Enginyeria Elect, E-08034 Barcelona, Spain.
[Ramos-Castro, J.] IEEC, C Gran Capita 2-4, E-08034 Barcelona, Spain.
[Slutsky, J.; Thorpe, J. I.] NASA Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
RP Ferroni, V (reprint author), Trento Inst Fundamental Phys & Applicat INFN, Trento, Italy.; Ferroni, V (reprint author), Univ Trento, Dipartimento Fis, I-38123 Povo, Trento, Italy.
EM valerio.ferroni@unitn.it
RI Pivato, Paolo/K-6641-2015; Wass, Peter/C-5767-2017;
OI Pivato, Paolo/0000-0003-2691-5236; Wass, Peter/0000-0002-2945-399X;
Nofrarias, Miquel/0000-0003-1518-2196; Zanoni,
Carlo/0000-0002-5767-9064; F. Sopuerta, Carlos/0000-0002-1779-4447
FU CNES (Accord Specific de projet) [CNES 1316634/CNRS 103747]; CNRS;
Observatoire de Paris; University Paris-Diderot; UnivEarthS Labex
program at Sorbonne Paris Cit [ANR-10-LABX-0023, ANR-11-IDEX-0005-02];
German Space Agency, DLR; Federal Ministry for Economic Affairs and
Energy [FKZ 50OQ0501, FKZ 50OQ1601]; Agenzia Spaziale Italiana;
Instituto Nazionale di Fisica Nucleare; MICINN [AYA2010-15709]; MINECO
[ESP2013-47637-P, ESP2015-67234-P]; Formacin de Personal Investigador
(MINECO); Swiss Space Office (SSO) via the PRODEX Programme of ESA;
Swiss National Science Foundation; United Kingdom Space Agency (UKSA);
University of Glasgow; University of Birmingham; Imperial College;
Scottish Universities Physics Alliance (SUPA); US National Aeronautics
and Space Administration (NASA)
FX This work has been made possible by the LISA Pathfinder mission, which
is part of the space-science program of the European Space Agency. The
French contribution has been supported by CNES (Accord Specific de
projet CNES 1316634/CNRS 103747), the CNRS, the Observatoire de Paris
and the University Paris-Diderot. EP and HI would also like to
acknowledge the financial support of the UnivEarthS Labex program at
Sorbonne Paris Cit (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02). The
Albert-Einstein-Institut acknowledges the support of the German Space
Agency, DLR. The work is supported by the Federal Ministry for Economic
Affairs and Energy based on a resolution of the German Bundestag (FKZ
50OQ0501 and FKZ 50OQ1601). The Italian contribution has been supported
by Agenzia Spaziale Italiana and Instituto Nazionale di Fisica Nucleare.
The Spanish contribution has been supported by Contracts No.
AYA2010-15709 (MICINN), No. ESP2013-47637-P, and No. ESP2015-67234-P
(MINECO). MN acknowledges support from Fundacion General CSIC (Programa
ComFuturo). FR acknowledges support from a Formacin de Personal
Investigador (MINECO) contract. The Swiss contribution acknowledges the
support of the Swiss Space Office (SSO) via the PRODEX Programme of ESA.
LF acknowledges the support of the Swiss National Science Foundation.
The UK groups wish to acknowledge support from the United Kingdom Space
Agency (UKSA), the University of Glasgow, the University of Birmingham,
Imperial College, and the Scottish Universities Physics Alliance (SUPA).
JIT and JS acknowledge the support of the US National Aeronautics and
Space Administration (NASA).
NR 20
TC 0
Z9 0
U1 6
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0264-9381
EI 1361-6382
J9 CLASSICAL QUANT GRAV
JI Class. Quantum Gravity
PD DEC 8
PY 2016
VL 33
IS 23
AR 235015
DI 10.1088/0264-9381/33/23/235015
PG 14
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA EC9NC
UT WOS:000388470300003
ER
PT J
AU Okojie, RS
Lukco, D
AF Okojie, R. S.
Lukco, D.
TI Simultaneous ohmic contacts to p- and n-type 4H-SiC by phase segregation
annealing of co-sputtered Pt-Ti
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
ID SILICON-CARBIDE; WORK FUNCTION; 4H-SILICON CARBIDE; ION-IMPLANTATION;
TI3SIC2; SILICIDES; BARRIER
AB A new concept, Phase Segregation Annealing (PSA), was investigated for implementing simultaneous ohmic contacts (SOCs) to p- and n-type 4H-SiC. Test structures with selected ratio compositions of co-sputtered Pt:Ti contacts were fabricated in p-type 4H-SiC epitaxial layers having aluminum acceptor concentrations, N-a = 2 x 10(19), 7 x 10(19), and 2.5 x 10(20) cm(-3), and a nitrogen doped n-type epitaxial layer having donor concentration, N-d = 7 x 10(18) cm(-3). The ratios of the co-sputtered Pt-Ti metallization were 80:20, 50:50, and 30:70 at. %. After rapid thermal annealing (RTA) ranging between 800 and 1200 degrees C in vacuum and confirming SOCs by linear current-voltage (I-V) measurement, the specific contact resistance (rho(c)) values were extracted using the Transfer Length Measurement method. SOCs were realized with the Pt80:Ti20 composition starting from 1000 degrees C, and the Pt30:Ti70 composition from 1100 degrees C, with both exhibiting eutectic and segregated phases. The Pt50:Ti50 composition produced no SOC and eutectic and segregated phases were absent. The Pt80:Ti20 composition had the lowest pair of average rho(c) values of 7 x 10(-5) X cm(2) and 7.3 x 10(-4) Omega cm(2) on the highest doped p-type and the n-type samples after RTA at 1000 degrees C, respectively. Auger electron spectroscopy and focused ion beam field emission scanning electron microscopy with energy dispersive x-ray spectroscopy indicated distinct phase segregation via the eutectic-liquidus-eutectic transitions, the coalescence of likely Pt3Si and Pt2Si binary phases, and solid phases of Ti3Si, Ti5Si3, and TiC, with all the active phases maintaining intimate contact to both the p- and n-type 4H-SiC surfaces. The SOC formation was attributed to the disparate work functions of these phases, which was in good agreement with the proposed PSA model. Published by AIP Publishing.
C1 [Okojie, R. S.] NASA Glenn Res Ctr, 21000 Brookpark Rd, Cleveland, OH 44135 USA.
[Lukco, D.] Vantage Partners LLC, 21000 Brookpark Rd, Cleveland, OH 44135 USA.
RP Okojie, RS (reprint author), NASA Glenn Res Ctr, 21000 Brookpark Rd, Cleveland, OH 44135 USA.
NR 41
TC 0
Z9 0
U1 2
U2 2
PU AMER INST PHYSICS
PI MELVILLE
PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA
SN 0021-8979
EI 1089-7550
J9 J APPL PHYS
JI J. Appl. Phys.
PD DEC 7
PY 2016
VL 120
IS 21
AR 215301
DI 10.1063/1.4968572
PG 11
WC Physics, Applied
SC Physics
GA EF8TN
UT WOS:000390602600031
ER
PT J
AU Paredes, P
Choudhari, MM
Li, F
AF Paredes, Pedro
Choudhari, Meelan M.
Li, Fei
TI Transition due to streamwise streaks in a supersonic flat plate boundary
layer
SO PHYSICAL REVIEW FLUIDS
LA English
DT Article
ID PARABOLIZED STABILITY EQUATIONS; SPATIAL OPTIMAL-GROWTH; OPTIMAL
DISTURBANCES; TRANSIENT GROWTH; OPTIMAL PERTURBATIONS; BYPASS
TRANSITION; SECONDARY INSTABILITIES; NUMERICAL SIMULATIONS; ROUGHNESS
ELEMENTS; GORTLER VORTICES
AB Transition induced by stationary streaks undergoing transient growth in a supersonic flat plate boundary layer flow is studied using numerical computations. While the possibility of strong transient growth of small-amplitude stationary perturbations in supersonic boundary layer flows has been demonstrated in previous works, its relation to laminar-turbulent transition cannot be established within the framework of linear disturbances. Therefore, this paper investigates the nonlinear evolution of initially linear optimal disturbances that evolve into finite amplitude streaks in the downstream region, and then studies the modal instability of those streaks as a likely cause for the onset of bypass transition. The nonmodal evolution of linearly optimal stationary perturbations in a supersonic, Mach 3 flat plate boundary layer is computed via the nonlinear plane-marching parabolized stability equations (PSE) for stationary perturbations, or equivalently, the perturbation form of parabolized Navier-Stokes equations. To assess the effect of the nonlinear finite-amplitude streaks on transition, the linear form of plane-marching PSE is used to investigate the instability of the boundary layer flow modified by the spanwise periodic streaks. The onset of transition is estimated using anN-factor criterion based on modal amplification of the secondary instabilities of the streaks. In the absence of transient growth disturbances, first mode instabilities in a Mach 3, zero pressure gradient boundary layer reach N = 10 at Re-x approximate to 10(7). However, secondary instability modes of the stationary streaks undergoing transient growth are able to achieve the same N-factor at Re-x < 2 x 10(6) when the initial streak amplitude is sufficiently large. In contrast to the streak instabilities in incompressible flows, subharmonic instability modes with twice the fundamental spanwise wavelength of the streaks are found to have higher amplification ratios than the streak instabilities at fundamental wavelength. This behavior is shown to be related to the destabilizing influence of the streaks on oblique first mode disturbances, which tend to have longer spanwise wavelengths than those of the optimal stationary disturbances.
C1 [Paredes, Pedro; Choudhari, Meelan M.; Li, Fei] NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA.
RP Paredes, P (reprint author), NASA, Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA.
EM pedro.paredes@nasa.gov
RI Choudhari, Meelan/F-6080-2017
OI Choudhari, Meelan/0000-0001-9120-7362
FU Transformational Tools & Technologies project of the National
Aeronautics and Space Administration (NASA)
FX This work is supported by the Transformational Tools & Technologies
project of the National Aeronautics and Space Administration (NASA).
NR 69
TC 0
Z9 0
U1 4
U2 4
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-990X
J9 PHYS REV FLUIDS
JI Phys. Rev. Fluids
PD DEC 6
PY 2016
VL 1
IS 8
AR 083601
DI 10.1103/PhysRevFluids.1.083601
PG 23
WC Physics, Fluids & Plasmas
SC Physics
GA EF4ZP
UT WOS:000390340800001
ER
PT J
AU Maasakkers, JD
Jacob, DJ
Sulprizio, MP
Turner, AJ
Weitz, M
Wirth, T
Hight, C
DeFigueiredo, M
Desai, M
Schmeltz, R
Hockstad, L
Bloom, AA
Bowman, KW
Jeong, S
Fischer, ML
AF Maasakkers, Joannes D.
Jacob, Daniel J.
Sulprizio, Melissa P.
Turner, Alexander J.
Weitz, Melissa
Wirth, Tom
Hight, Cate
DeFigueiredo, Mark
Desai, Mausami
Schmeltz, Rachel
Hockstad, Leif
Bloom, Anthony A.
Bowman, Kevin W.
Jeong, Seongeun
Fischer, Marc L.
TI Gridded National Inventory of US Methane Emissions
SO ENVIRONMENTAL SCIENCE & TECHNOLOGY
LA English
DT Article
ID SPATIALLY EXPLICIT INVENTORY; BARNETT SHALE REGION; UNITED-STATES;
SATELLITE DATA; GAS; RETRIEVALS; RESOLUTION; SCIAMACHY; SYSTEM; FLUXES
AB We present a gridded inventory of US anthropogenic methane emissions with 0.1 degrees X 0.1 degrees spatial resolution, monthly temporal resolution, and detailed scale-dependent error characterization. The inventory is designed to be consistent with the 2016 US Environmental Protection Agency (EPA) Inventory of US Greenhouse Gas Emissions and Sinks (GHGI) for 2012 The EPA inventory is available only as national totals for different source types. We use a wide range of databases at the state, county, local, and point source level to disaggregate the inventory and allocate the spatial and temporal distribution of emissions for individual source types. Results show large differences with the EDGAR v4.2 global gridded inventory commonly used as a priori estimate in inversions of atmospheric methane observations. We derive grid-dependent error statistics for individual source types from comparison with the Environmental Defense Fund (EDF) regional inventory for Northeast Texas. These error statistics are independently verified by comparison with the California Greenhouse Gas Emissions Measurement (CALGEM) grid-resolved emission inventory. Our gridded, time-resolved inventory provides an improved basis for inversion of atmospheric methane observations to estimate US methane emissions and interpret the results in terms of the underlying processes.
C1 [Maasakkers, Joannes D.; Jacob, Daniel J.; Sulprizio, Melissa P.; Turner, Alexander J.] Harvard Univ, Sch Engn & Appl Sci, Pierce Hall,29 Oxford St, Cambridge, MA 02138 USA.
[Weitz, Melissa; Wirth, Tom; Hight, Cate; DeFigueiredo, Mark; Desai, Mausami; Schmeltz, Rachel; Hockstad, Leif] US EPA, Climate Change Div, Washington, DC 20460 USA.
[Bloom, Anthony A.; Bowman, Kevin W.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Jeong, Seongeun; Fischer, Marc L.] Lawrence Berkeley Natl Lab, Energy Technol Area, Berkeley, CA 94720 USA.
RP Maasakkers, JD (reprint author), Harvard Univ, Sch Engn & Appl Sci, Pierce Hall,29 Oxford St, Cambridge, MA 02138 USA.
EM Maasakkers@fas.harvard.edu
FU NASA Carbon Monitoring System (CMS); Department of Energy (DOE); NASA;
NASA CMS program [NNH13ZDA001N]; California Energy Commission Natural
Gas Research Program under U.S. Department of Energy [DE-AC02-05CH11231]
FX This research was funded by the NASA Carbon Monitoring System (CMS).
A.J. Turner was supported by a Department of Energy (DOE) Computational
Science Graduate Fellowship (CSGF). Part of this research was carried
out at the Jet Propulsion Laboratory, California Institute of Technology
under a contract with NASA. Work by M.L. Fischer and S. Jeong at LBNL
was supported by the NASA CMS program (NNH13ZDA001N) and the California
Energy Commission Natural Gas Research Program under U.S. Department of
Energy Contract No. DE-AC02-05CH11231. We thank D.R. Lyon, D.
Zavala-Araiza, and S.P. Hamburg for providing the EDF methane emissions
over the Barnett Shale. We thank the anonymous reviewers for their
thorough comments.
NR 78
TC 3
Z9 3
U1 16
U2 16
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0013-936X
EI 1520-5851
J9 ENVIRON SCI TECHNOL
JI Environ. Sci. Technol.
PD DEC 6
PY 2016
VL 50
IS 23
BP 13123
EP 13133
DI 10.1021/acs.est.6b02878
PG 11
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA EE4FG
UT WOS:000389557100067
PM 27934278
ER
PT J
AU Milillo, P
Burgmann, R
Lundgren, P
Salzer, J
Perissin, D
Fielding, E
Biondi, F
Milillo, G
AF Milillo, Pietro
Burgmann, Roland
Lundgren, Paul
Salzer, Jacqueline
Perissin, Daniele
Fielding, Eric
Biondi, Filippo
Milillo, Giovanni
TI Space geodetic monitoring of engineered structures: The ongoing
destabilization of the Mosul dam, Iraq
SO SCIENTIFIC REPORTS
LA English
DT Article
ID DIFFERENTIAL SAR INTERFEROMETRY
AB We present a detailed survey of the ongoing destabilization process of the Mosul dam. The dam is located on the Tigris river and is the biggest hydraulic structure in Iraq. From a geological point of view the dam foundation is poor due to a site geology formed by alternating strata of highly soluble materials including gypsum, anhydrite, marl and limestone. Here we present the first multi-sensor cumulative deformation map for the dam generated from space-based interferometric synthetic aperture radar measurements from the Italian constellation COSMO-SkyMed and the European sensor Sentinel-1a over the period 2014-2016 that we compare to an older dataset spanning 2004-2010 acquired with the European Envisat satellite. We found that deformation was rapid during 2004-2010, slowed in 2012-2014 and increased since August 2014 when grouting operations stopped due to the temporary capture of the dam by the self proclaimed Islamic State. We model the inferred deformation using a Markov chain Monte Carlo approach to solve for change in volume for simple tensile dislocations. Results from recent and historical geodetic datasets suggests that the volume dissolution rate remains constant when the equivalent volume of total concrete injected during re-grouting operations is included in the calculations.
C1 [Milillo, Pietro; Lundgren, Paul; Fielding, Eric] CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Burgmann, Roland] Univ Calif Berkeley, Dept Earth & Planetary Sci, 389 McCone Hall, Berkeley, CA 94720 USA.
[Salzer, Jacqueline] GFZ German Res Ctr Geosci Phys Earthquakes & Volc, D-14473 Potsdam, Germany.
[Perissin, Daniele] Purdue Univ, Lyles Sch Civil Engn, 550 Stadium Mall Dr, W Lafayette, IN 47907 USA.
[Biondi, Filippo] Univ Aquila, Laquila, AO, Italy.
[Milillo, Giovanni] Italian Space Agcy, I-75100 Matera, MT, Italy.
RP Milillo, P (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM pietro0milillo@gmail.com
OI Milillo, Giovanni/0000-0002-6045-5686
FU National Aeronautics and Space Administration Postdoctoral Program;
National Aeronautics and Space Administration
FX We thank the Italian Space Agency (ASI) for providing COSMO-SkyMed data
for this project. Original COSMO-SkyMed product ASI Agenzia Spaziale
Italiana (2012-2016). The Envisat-ASAR and Sentinel data were provided
courtesy of the European Space Agency. Mosul Jason Altimeter data
provided by the United States department of agriculture, foreign
agricultural service. The The work of P. Milillo was sponsored by the
National Aeronautics and Space Administration Postdoctoral Program. The
research was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration.
NR 9
TC 0
Z9 0
U1 11
U2 11
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2045-2322
J9 SCI REP-UK
JI Sci Rep
PD DEC 6
PY 2016
VL 6
AR 37408
DI 10.1038/srep37408
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EE1VT
UT WOS:000389372600001
PM 27922128
ER
PT J
AU Lee, BH
Lee, DI
Bae, H
Seong, H
Jeon, SB
Seol, ML
Han, JW
Meyyappan, M
Im, SG
Choi, YK
AF Lee, Byung-Hyun
Lee, Dong-Il
Bae, Hagyoul
Seong, Hyejeong
Jeon, Seung-Bae
Seol, Myung-Lok
Han, Jin-Woo
Meyyappan, M.
Im, Sung-Gap
Choi, Yang-Kyu
TI Foldable and Disposable Memory on Paper
SO Scientific Reports
LA English
DT Article
ID CHEMICAL-VAPOR-DEPOSITION; LIGHT-EMITTING-DIODES; ORGANIC TRANSISTORS;
INTEGRATED-CIRCUITS; FLEXIBLE DISPLAYS; HIGH-PERFORMANCE; ELECTRONICS;
NANOPAPER; DEVICES; SENSORS
AB Foldable organic memory on cellulose nanofibril paper with bendable and rollable characteristics is demonstrated by employing initiated chemical vapor deposition (iCVD) for polymerization of the resistive switching layer and inkjet printing of the electrode, where iCVD based on all-dry and room temperature process is very suitable for paper electronics. This memory exhibits a low operation voltage of 1.5V enabling battery operation compared to previous reports and wide memory window. The memory performance is maintained after folding tests, showing high endurance. Furthermore, the quick and complete disposable nature demonstrated here is attractive for security applications. This work provides an effective platform for green, foldable and disposable electronics based on low cost and versatile materials.
C1 [Lee, Byung-Hyun; Lee, Dong-Il; Bae, Hagyoul; Jeon, Seung-Bae; Choi, Yang-Kyu] Korea Adv Inst Sci & Technol, Sch Elect Engn, 291 Daehak Ro, Daejeon 34141, South Korea.
[Lee, Byung-Hyun] Samsung Elect, Dept Memory Business, San 16 Banwol Dong, Hwasung City 445701, Gyeonggi Do, South Korea.
[Seong, Hyejeong; Im, Sung-Gap] Korea Adv Inst Sci & Technol, Dept Chem & Biomol Engn, 291 Daehak Ro, Daejeon 305701, South Korea.
[Seong, Hyejeong; Im, Sung-Gap] Korea Adv Inst Sci & Technol, KI Nanocentury, Graphene Res Ctr, Daejeon 34141, South Korea.
[Seol, Myung-Lok; Han, Jin-Woo; Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
RP Choi, YK (reprint author), Korea Adv Inst Sci & Technol, Sch Elect Engn, 291 Daehak Ro, Daejeon 34141, South Korea.
EM ykchoi@ee.kaist.ac.kr
FU Center for Integrated Smart Sensors - Ministry of Science, ICT & Future
Planning as Global Frontier Project [CISS-2011-0031848]; Pioneer
Research Center Program through the National Research Foundation of
Korea - Ministry of Science, ICT & Future Planning [2012-0009600];
Center for Advanced Soft-Electronics - Ministry of Science, ICT and
Future Planning as Global Frontier Project [CASE-2011-0031638]
FX This work was partially supported by the Center for Integrated Smart
Sensors funded by the Ministry of Science, ICT & Future Planning as
Global Frontier Project (CISS-2011-0031848); partially supported by the
Pioneer Research Center Program through the National Research Foundation
of Korea funded by the Ministry of Science, ICT & Future Planning (Grant
2012-0009600) and by the Center for Advanced Soft-Electronics funded by
the Ministry of Science, ICT and Future Planning as Global Frontier
Project (CASE-2011-0031638). The authors thank Pia Qvintus of VTT,
Finland for providing nanopaper samples. The authors acknowledge Dr.
Tekla Tammelin and Vesa Kunnari from VTT Technical Research Centre of
Finland for providing the nanocellulose paper samples used in this
study.
NR 49
TC 0
Z9 0
U1 23
U2 23
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2045-2322
J9 SCI REP-UK
JI Sci Rep
PD DEC 6
PY 2016
VL 6
AR 38389
DI 10.1038/srep38389
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EE0AZ
UT WOS:000389237000002
PM 27922094
ER
PT J
AU Huang, MH
Burgmann, R
Hu, JC
AF Huang, Mong-Han
Buergmann, Roland
Hu, Jyr-Ching
TI Fifteen years of surface deformation in Western Taiwan: Insight from SAR
interferometry
SO TECTONOPHYSICS
LA English
DT Article
DE Taiwan; InSAR; Crustal deformation; Land subsidence
ID RIVER ALLUVIAL-FAN; SOUTHWESTERN TAIWAN; SW TAIWAN; TAINAN TABLELAND;
LAND SUBSIDENCE; ACTIVE DEFORMATION; GPS MEASUREMENTS; TECTONIC ESCAPE;
AQUIFER-SYSTEM; VELOCITY-FIELD
AB Geodetically measured surface displacements are produced by a combination of underlying deformation processes acting at different spatial and temporal scales. A complete history of surface measurements in an area can help discriminate contributions from tectonic, hydrologic, and anthropogenic processes. In this study, we use Synthetic Aperture Radar (SAR) images of the active mountain front and adjacent coastal plain of southwestern Taiwan to generate time series of surface deformation from 1995 to 2001 and from 2005 to 2008 based on the InSAR small baseline method. The InSAR measurements agree well with LOS motions estimated from continuous GPS measurements of 3D displacements between 2006 and 2008. A significant range increase in line of sight (LOS) is dominated by land subsidence in the coastal area of Western and southwestern Taiwan. Subsidence rates vary with annual periods and are highly correlated with seasonal precipitation, which are likely associated with groundwater recharge and withdrawal. The long-term deformation is dominated by long-term tectonic loading in SW Taiwan during the interseismic period of the earthquake cycle, including elastic strain along or continuous creep on the active faults. Our results show the ability of InSAR to reveal spatiotemporal crustal deformation in western Taiwan with high spatial resolution and accuracy, which is potentially important for evaluating seismic hazards. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Huang, Mong-Han; Buergmann, Roland] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
[Huang, Mong-Han; Buergmann, Roland] Univ Calif Berkeley, Berkeley Seismol Lab, Berkeley, CA 94720 USA.
[Hu, Jyr-Ching] Natl Taiwan Univ, Dept Geosci, Taipei 10617, Taiwan.
RP Huang, MH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM mong@seismo.berkeley.edu
OI Huang, Mong-Han/0000-0003-2331-3766
FU Larsen fellowship; NASA grant [NNX12AQ32G]; ESA project [28610];
appointment to the NASA Postdoctoral Program at the Jet Propulsion
Laboratory; NSC [98-2628-M-002-016, 101-2116-M-002-012]
FX The authors would like to thank John Suppe, Maryline Le Beon, Ya-Ju Hsu,
and Estelle Chaussard for discussions that significantly improved the
manuscript. Three anonymous reviewers and the associate editor provide
critical reviews and comments that significantly improved the
manuscript. The Larsen fellowship and NASA grant NNX12AQ32G supported
M.-H. Huang for this study, and M.-H. Huang is currently supported by an
appointment to the NASA Postdoctoral Program at the Jet Propulsion
Laboratory, administered by Oak Ridge Associated Universities through a
contract with NASA. The research was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration. The ERS SAR images
were purchased under NSC 98-2628-M-002-016 and NSC 101-2116-M-002-012,
and the Envisat ASAR images are available through ESA project number
28610. Other precipitation data are available at the Center Weather
Bureau, Taiwan website (http://www.cwb.gov.tw). The seismicity data are
downloaded from the Taiwan Earthquake Center
(http://tec.earth.sinica.edu.tw). The continuous GPS time series data
are downloaded from the GPS laboratory at the Institute of Earth
Science, Academia Sinica, Taiwan (http://gps.earth.sinica.edu.tw). This
is BSL contribution #2016-01.
NR 43
TC 2
Z9 2
U1 12
U2 12
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0040-1951
EI 1879-3266
J9 TECTONOPHYSICS
JI Tectonophysics
PD DEC 5
PY 2016
VL 692
BP 252
EP 264
DI 10.1016/j.tecto.2016.02.021
PN B
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EG1WG
UT WOS:000390823700014
ER
PT J
AU Sheese, PE
Walker, KA
Boone, CD
McLinden, CA
Bernath, PF
Bourassa, AE
Burrows, JP
Degenstein, DA
Funke, B
Fussen, D
Manney, GL
McElroy, CT
Murtagh, D
Randall, CE
Raspollini, P
Rozanov, A
Russell, JM
Suzuki, M
Shiotani, M
Urban, J
von Clarmann, T
Zawodny, JM
AF Sheese, Patrick E.
Walker, Kaley A.
Boone, Chris D.
McLinden, Chris A.
Bernath, Peter F.
Bourassa, Adam E.
Burrows, John P.
Degenstein, Doug A.
Funke, Bernd
Fussen, Didier
Manney, Gloria L.
McElroy, C. Thomas
Murtagh, Donal
Randall, Cora E.
Raspollini, Piera
Rozanov, Alexei
Russell, James M., III
Suzuki, Makoto
Shiotani, Masato
Urban, Joachim
von Clarmann, Thomas
Zawodny, Joseph M.
TI Validation of ACE-FTS version 3.5 NOy species profiles using correlative
satellite measurements
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID FOURIER-TRANSFORM SPECTROMETER; HALOGEN OCCULTATION EXPERIMENT;
RETRIEVAL ALGORITHM; VERTICAL PROFILES; STRATOSPHERIC NO2; OPERATIONAL
DATA; ODIN SATELLITE; POLAR OZONE; CLIMATOLOGY; TEMPERATURE
AB The ACE-FTS (Atmospheric Chemistry Experiment - Fourier Transform Spectrometer) instrument on the Canadian SCISAT satellite, which has been in operation for over 12 years, has the capability of deriving stratospheric profiles of many of the NOy (N + NO + NO2 + NO3 + 2 x N2O5 + HNO3 + HNO4 + ClONO2 + BrONO2) species. Version 2.2 of ACE-FTS NO, NO2, HNO3, N2O5, and ClONO2 has previously been validated, and this study compares the most recent version (v3.5) of these five ACE-FTS products to spatially and temporally coincident measurements from other satellite instruments - GOMOS, HALOE, MAESTRO, MIPAS, MLS, OSIRIS, POAM III, SAGE III, SCIAMACHY, SMILES, and SMR. For each ACE-FTS measurement, a photochemical box model was used to simulate the diurnal variations of the NOy species and the ACE-FTS measurements were scaled to the local times of the coincident measurements. The comparisons for all five species show good agreement with correlative satellite measurements. For
C1 [Sheese, Patrick E.; Walker, Kaley A.] Univ Toronto, Dept Phys, Toronto, ON, Canada.
[Walker, Kaley A.; Boone, Chris D.] Univ Waterloo, Dept Chem, Waterloo, ON, Canada.
[McLinden, Chris A.] Environm Canada, Air Qual Res Branch, Toronto, ON, Canada.
[Bernath, Peter F.] Old Dominion Univ, Dept Chem & Biochem, Norfolk, VA USA.
[Bourassa, Adam E.; Degenstein, Doug A.] Univ Saskatchewan, ISAS, Dept Phys & Engn, Saskatoon, SK, Canada.
[Burrows, John P.; Rozanov, Alexei] Univ Bremen, Inst Environm Phys, Bremen, Germany.
[Funke, Bernd] CSIC, Inst Astrofis Andalucia, Granada, Spain.
[Fussen, Didier] IASB, BIRA, Brussels, Belgium.
[Manney, Gloria L.] NorthWest Res Associates Inc, Socorro, NM USA.
[Manney, Gloria L.] New Mexico Inst Min & Technol, Socorro, NM USA.
[McElroy, C. Thomas] York Univ, Dept Earth & Space Sci & Engn, Toronto, ON, Canada.
[Murtagh, Donal; Urban, Joachim] Chalmers, Dept Earth & Space Sci, Gothenburg, Sweden.
[Randall, Cora E.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[Raspollini, Piera] CNR, Ist Fis Applicata Nello Carrara, Florence, Italy.
[Russell, James M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA.
[Suzuki, Makoto] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa, Japan.
[Shiotani, Masato] Kyoto Univ, Res Inst Sustainable Humanosphere, Uji, Kyoto, Japan.
[von Clarmann, Thomas] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, Karlsruhe, Germany.
[Zawodny, Joseph M.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Walker, KA (reprint author), Univ Toronto, Dept Phys, Toronto, ON, Canada.; Walker, KA (reprint author), Univ Waterloo, Dept Chem, Waterloo, ON, Canada.
EM kaley.walker@utoronto.ca
RI Funke, Bernd/C-2162-2008; Burrows, John/B-6199-2014; Randall,
Cora/L-8760-2014
OI Funke, Bernd/0000-0003-0462-4702; Burrows, John/0000-0002-6821-5580;
Randall, Cora/0000-0002-4313-4397
FU Canadian Space Agency (CSA); CSA; Sweden (Swedish National Space Board);
Canada (CSA); France (Centre National d'Etudes Spatiales); Finland
(Tekes); European Space Agency (ESA); NASA [NNX14AH54G]; DLR Space
Agency (Germany); University of Bremen; State of Bremen
FX This project was funded by the Canadian Space Agency (CSA). The
Atmospheric Chemistry Experiment is a Canadian-led mission mainly
supported by the CSA. Odin is a Swedish-led satellite project funded
jointly by Sweden (Swedish National Space Board), Canada (CSA), France
(Centre National d'Etudes Spatiales), and Finland (Tekes), with support
by the third-party mission programme of the European Space Agency (ESA).
Coauthor CER was funded by NASA grant NNX14AH54G. The University of
Bremen team was funded in parts by the DLR Space Agency (Germany) and by
the University and State of Bremen. The authors wish to thank the
anonymous reviewers for their thoughtful comments and valuable insight.
NR 86
TC 1
Z9 1
U1 9
U2 9
PU COPERNICUS GESELLSCHAFT MBH
PI GOTTINGEN
PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY
SN 1867-1381
EI 1867-8548
J9 ATMOS MEAS TECH
JI Atmos. Meas. Tech.
PD DEC 5
PY 2016
VL 9
IS 12
BP 5781
EP 5810
DI 10.5194/amt-9-5781-2016
PG 30
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA ED9RL
UT WOS:000389210200001
ER
PT J
AU Bae, H
Lee, BH
Lee, D
Seol, ML
Kim, D
Han, JW
Kim, CK
Jeon, SB
Ahn, D
Park, SJ
Park, JY
Choi, YK
AF Bae, Hagyoul
Lee, Byung-Hyun
Lee, Dongil
Seol, Myeong-Lok
Kim, Daewon
Han, Jin-Woo
Kim, Choong-Ki
Jeon, Seung-Bae
Ahn, Daechul
Park, Sang-Jae
Park, Jun-Young
Choi, Yang-Kyu
TI Physically Transient Memory on a Rapidly Dissoluble Paper for Security
Application
SO Scientific Reports
LA English
DT Article
ID NONVOLATILE MEMORY; LOW-POWER; ELECTRONICS; DEVICES; PERFORMANCE; ARRAYS
AB We report the transient memory device by means of a water soluble SSG (solid sodium with glycerine) paper. This material has a hydroscopic property hence it can be soluble in water. In terms of physical security of memory devices, prompt abrogation of a memory device which stored a large number of data is crucial when it is stolen because all of things have identified information in the memory device. By utilizing the SSG paper as a substrate, we fabricated a disposable resistive random access memory (RRAM) which has good data retention of longer than 106 seconds and cycling endurance of 300 cycles. This memory device is dissolved within 10 seconds thus it can never be recovered or replicated. By employing direct printing but not lithography technology to aim low cost and disposable applications, the memory capacity tends to be limited less than kilo-bits. However, unlike high memory capacity demand for consumer electronics, the proposed device is targeting for security applications. With this regards, the sub-kilobit memory capacity should find the applications such as one-time usable personal identification, authentication code storage, cryptography key, and smart delivery tag. This aspect is attractive for security and protection system against unauthorized accessibility.
C1 [Bae, Hagyoul; Lee, Byung-Hyun; Lee, Dongil; Kim, Daewon; Kim, Choong-Ki; Jeon, Seung-Bae; Ahn, Daechul; Park, Sang-Jae; Park, Jun-Young; Choi, Yang-Kyu] Korea Adv Inst Sci & Technol, Sch Elect Engn, 291 Daehak Ro, Daejeon 34141, South Korea.
[Seol, Myeong-Lok; Han, Jin-Woo] NASA, Ctr Nanotechnol, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Choi, YK (reprint author), Korea Adv Inst Sci & Technol, Sch Elect Engn, 291 Daehak Ro, Daejeon 34141, South Korea.
EM ykchoi@ee.kaist.ac.kr
OI Seol, Myeong-Lok/0000-0001-5724-2244
FU Center for Integrated Smart Sensors - Ministry of Science, ICT & Future
Planning as Global Frontier Project [CISS-2011-0031848]; Pioneer
Research Center Program through the National Research Foundation of
Korea - Ministry of Science, ICT & Future Planning [2012-0009600]; IDEC
(EDA Tool, MPW); NRF (National Research Foundation of Korea) Grant -
Korea Government [NRF-2014H1A2A1022137]
FX This work was supported by the Center for Integrated Smart Sensors
funded by the Ministry of Science, ICT & Future Planning as Global
Frontier Project (CISS-2011-0031848). This research was partially
supported by the Pioneer Research Center Program through the National
Research Foundation of Korea funded by the Ministry of Science, ICT &
Future Planning (Grant No. 2012-0009600) and IDEC (EDA Tool, MPW). This
work was also supported by NRF (National Research Foundation of Korea)
Grant funded by the Korea Government (NRF-2014H1A2A1022137-Global Ph.D.
Fellowship Program).
NR 44
TC 0
Z9 0
U1 12
U2 12
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2045-2322
J9 SCI REP-UK
JI Sci Rep
PD DEC 5
PY 2016
VL 6
AR 38324
DI 10.1038/srep38324
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA ED9JX
UT WOS:000389187100001
PM 27917910
ER
PT J
AU Motesharrei, S
Rivas, J
Kalnay, E
Asrar, GR
Busalacchi, AJ
Cahalan, RF
Cane, MA
Colwell, RR
Feng, KS
Franklin, RS
Hubacek, K
Miralles-Wilhelm, F
Miyoshi, T
Ruth, M
Sagdeev, R
Shirmohammadi, A
Shukla, J
Srebric, J
Yakovenko, VM
Zeng, N
AF Motesharrei, Safa
Rivas, Jorge
Kalnay, Eugenia
Asrar, Ghassem R.
Busalacchi, Antonio J.
Cahalan, Robert F.
Cane, Mark A.
Colwell, Rita R.
Feng, Kuishuang
Franklin, Rachel S.
Hubacek, Klaus
Miralles-Wilhelm, Fernando
Miyoshi, Takemasa
Ruth, Matthias
Sagdeev, Roald
Shirmohammadi, Adel
Shukla, Jagadish
Srebric, Jelena
Yakovenko, Victor M.
Zeng, Ning
TI Modeling sustainability: population, inequality, consumption, and
bidirectional coupling of the Earth and Human Systems
SO NATIONAL SCIENCE REVIEW
LA English
DT Review
DE Earth and Human System Models; population; migration; inequality; data
assimilation; bidirectional couplings and feedbacks; sustainability
ID AMAZONIAN FOREST FRAGMENTS; NET PRIMARY PRODUCTION;
NINO-SOUTHERN-OSCILLATION; CARBON-DIOXIDE EMISSIONS; ENSEMBLE KALMAN
FILTER; GLOBAL NITROGEN-CYCLE; CLIMATE-CHANGE; INTERNATIONAL-TRADE;
GROUNDWATER DEPLETION; PARAMETER-ESTIMATION
AB Over the last two centuries, the impact of the Human System has grown dramatically, becoming strongly dominant within the Earth System in many different ways. Consumption, inequality, and population have increased extremely fast, especially since about 1950, threatening to overwhelm the many critical functions and ecosystems of the Earth System. Changes in the Earth System, in turn, have important feedback effects on the Human System, with costly and potentially serious consequences. However, current models do not incorporate these critical feedbacks. We argue that in order to understand the dynamics of either system, Earth System Models must be coupled with Human System Models through bidirectional couplings representing the positive, negative, and delayed feedbacks that exist in the real systems. In particular, key Human System variables, such as demographics, inequality, economic growth, and migration, are not coupled with the Earth System but are instead driven by exogenous estimates, such as United Nations population projections. This makes current models likely to miss important feedbacks in the real Earth-Human system, especially those that may result in unexpected or counterintuitive outcomes, and thus requiring different policy interventions from current models. The importance and imminence of sustainability challenges, the dominant role of the Human System in the Earth System, and the essential roles the Earth System plays for the Human System, all call for collaboration of natural scientists, social scientists, and engineers in multidisciplinary research and modeling to develop coupled Earth-Human system models for devising effective science-based policies and measures to benefit current and future generations.
C1 [Motesharrei, Safa; Kalnay, Eugenia; Colwell, Rita R.; Hubacek, Klaus; Miralles-Wilhelm, Fernando; Miyoshi, Takemasa; Sagdeev, Roald; Shirmohammadi, Adel; Srebric, Jelena; Yakovenko, Victor M.; Zeng, Ning] Univ Maryland, College Pk, MD 20742 USA.
[Rivas, Jorge] Inst Global Environm & Soc, Rockville, MD 20852 USA.
[Asrar, Ghassem R.; Miralles-Wilhelm, Fernando] Joint Global Change Res Inst, College Pk, MD 20740 USA.
[Busalacchi, Antonio J.] Univ Corp Atmospheric Res, Boulder, CO 80307 USA.
[Cahalan, Robert F.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Cahalan, Robert F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cane, Mark A.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Franklin, Rachel S.] Brown Univ, Spatial Struct Social Sci, Populat Studies & Training Ctr, Providence, RI 02912 USA.
[Miyoshi, Takemasa] RIKEN, Adv Inst Computat Sci, Kobe, Hyogo 6500047, Japan.
[Ruth, Matthias] Northeastern Univ, Sch Publ Policy & Urban Affairs, Boston, MA 02115 USA.
[Ruth, Matthias] Northeastern Univ, Dept Civil & Environm Engn, Boston, MA 02115 USA.
[Shukla, Jagadish] George Mason Univ, Dept Atmospher Ocean & Earth Sci, Fairfax, VA 22030 USA.
RP Motesharrei, S (reprint author), Univ Maryland, College Pk, MD 20742 USA.
EM ssm@umd.edu
FU University of Maryland Council on the Environment 2014 Seed Grant
[1357928]; National Socio-Environmental Synthesis Center (SESYNC)-US
National Science Foundation (NSF) award [DBI-1052875]; Institute of
Global Environment and Society (IGES); Laboratory Directed Research and
Development award by the Pacific Northwest National Laboratory; Office
of Naval Research [MURI N00014-12-1-0911]; NSF award [CBET-1541642];
Institute for New Economic Thinking (INET)
FX This work was supported by the University of Maryland Council on the
Environment 2014 Seed Grant (1357928). The authors would like to
acknowledge the following grants and institutions: SM, KF, and KH:
National Socio-Environmental Synthesis Center (SESYNC)-US National
Science Foundation (NSF) award DBI-1052875; JR: The Institute of Global
Environment and Society (IGES); GRA: Laboratory Directed Research and
Development award by the Pacific Northwest National Laboratory, which is
managed by the Battelle Memorial Institute for the US Department of
Energy; MAC: Office of Naval Research, research grant MURI
N00014-12-1-0911; FMW: NSF award CBET-1541642; VMY: The Institute for
New Economic Thinking (INET).
NR 320
TC 1
Z9 1
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 2095-5138
EI 2053-714X
J9 NATL SCI REV
JI Natl. Sci. Rev.
PD DEC
PY 2016
VL 3
IS 4
BP 470
EP 494
DI 10.1093/nsr/nww081
PG 25
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA EQ0LP
UT WOS:000397763000018
ER
PT J
AU Storey, J
Roy, DP
Masek, J
Gascon, F
Dwyer, J
Choate, M
AF Storey, James
Roy, David P.
Masek, Jeffrey
Gascon, Ferran
Dwyer, John
Choate, Michael
TI A note on the temporary misregistration of Landsat-8 Operational Land
Imager (OLI) and Sentinel-2 Multi Spectral Instrument (MSI) imagery
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Landsat; Sentinel-2; Image registration
ID MISSION
AB The Landsat-8 and Sentinel-2 sensors provide multi-spectral image data with similar spectral and spatial characteristics that together provide improved temporal coverage globally. Both systems are designed to register Level 1 products to a reference image framework, however, the Landsat-8 framework, based upon the Global Land Survey images, contains residual geolocation errors leading to an expected sensor-to-sensor misregistration of 38 m (24 These misalignments vary geographically but should be stable for a given area. The Landsat framework will be readjusted for consistency with the Sentinel-2 Global Reference Image, with completion expected in 2018. In the interim, users can measure Landsat-to-Sentinel tie points to quantify the misalignment in their area of interest and if appropriate to reproject the data to better alignment. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Storey, James; Choate, Michael] US Geol Survey, Earth Resources Observat & Sci EROS Ctr, Stinger Ghaffarian Technol, Sioux Falls, SD 57030 USA.
[Roy, David P.] South Dakota State Univ, Geospatial Sci Ctr Excellence, Brookings, SD 57007 USA.
[Masek, Jeffrey] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Code 661, Greenbelt, MD 20771 USA.
[Gascon, Ferran] European Space Agcy, European Space Res Inst ESRIN, Frascati, Italy.
[Dwyer, John] US Geol Survey, Earth Resources Observat & Sci EROS Ctr, Sioux Falls, SD 57030 USA.
RP Storey, J (reprint author), US Geol Survey, Earth Resources Observat & Sci EROS Ctr, Stinger Ghaffarian Technol, Sioux Falls, SD 57030 USA.
EM james.storey.cti@usgs.gov; david.roy@sdstate.edu;
jeffrey.g.masek@nasa.gov; ferran.gascon@esa.int; dwyer@usgs.gov;
michael.choate.ctr@usgs.gov
OI Dwyer, John/0000-0002-8281-0896
FU NASA Land Cover/Land Use Change [LCLUCI4-2]; Multi-Source Land Imaging
Science Program [NNX15AK94G]; U.S. Department of the Interior, U.S.
Geological Survey (USGS) [G12PC00069, G15PC00012]
FX This research was funded by the NASA Land Cover/Land Use Change
(LCLUCI4-2), Multi-Source Land Imaging Science Program [Grant
NNX15AK94G], and by the U.S. Department of the Interior, U.S. Geological
Survey (USGS), [Grant G12PC00069 and USGS contract number G15PC00012].
NR 17
TC 0
Z9 0
U1 2
U2 2
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD DEC 1
PY 2016
VL 186
BP 121
EP 122
DI 10.1016/j.rse.2016.08.025
PG 2
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA EO0IW
UT WOS:000396382500009
ER
PT J
AU Jiao, ZT
Schaaf, CB
Dong, YD
Roman, M
Hill, MJ
Chen, JM
Wang, ZS
Zhang, H
Saenz, E
Poudyal, R
Gatebe, C
Breon, FM
Li, XW
Strahler, A
AF Jiao, Ziti
Schaaf, Crystal B.
Dong, Yadong
Roman, Miguel
Hill, Michael J.
Chen, Jing M.
Wang, Zhuosen
Zhang, Hu
Saenz, Edward
Poudyal, Rajesh
Gatebe, Charles
Breon, Francois-Marie
Li, Xiaowen
Strahler, Alan
TI A method for improving hotspot directional signatures in BRDF models
used for MODIS
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE BRDF; CAR; MODIS; POLDER; Multiangle remote sensing; Hotspot signature;
Hotspot kernel; Hotspot effect; Linear RTLSR model; Airborne
measurements
ID BIDIRECTIONAL REFLECTANCE MODEL; KERNEL-DRIVEN MODELS; SPECTRAL
MEASUREMENTS; CANOPY HEIGHT; BOREAL FOREST; AVHRR DATA; HOT-SPOT;
SURFACE; ALBEDO; INDEX
AB The semi-empirical, kernel-driven, linear RossThick-LiSparseReciprocal (RTLSR) Bidirectional Reflectance Distribution Function (BRDF) model is used to generate the routine MODIS BRDF/Albedo product due to its global applicability and the underlying physics. A challenge of this model in regard to surface reflectance anisotropy effects comes from its underestimation of the directional reflectance signatures near the Sun illumination direction; also known as the hotspot effect. In this study, a method has been developed for improving the ability of the RTLSR model to simulate the magnitude and width of the hotspot effect. The method corrects the volumetric scattering component of the RTLSR model using an exponential approximation of a physical hotspot kernel, which recreates the hotspot magnitude and width using two free parameters (C-1 and C-2, respectively). The approach allows one to reconstruct, with reasonable accuracy, the hotspot effect by adjusting or using the prior values of these two hotspot variables. Our results demonstrate that: (1) significant improvements in capturing hotspot effect can be made to this method by using the invested hotspot parameters; (2) the reciprocal nature allow this method to be more adaptive for simulating the hotspot height and width with high accuracy, especially in cases where hotspot signatures are available; and (3) while the new approach is consistent with the heritage RTLSR model inversion used to estimate intrinsic narrowband and broadband albedos, it presents some differences for vegetation clumping index (CI) retrievals. With the hotspot-related model parameters determined a priori, this method offers improved performance for various ecological remote sensing applications; including the estimation of canopy structure parameters. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Jiao, Ziti; Dong, Yadong; Zhang, Hu; Li, Xiaowen] Beijing Normal Univ, Res Ctr Remote Sensing & GIS, State Key Lab Remote Sensing Sci, Beijing 100875, Peoples R China.
[Jiao, Ziti; Dong, Yadong; Zhang, Hu; Li, Xiaowen] Beijing Normal Univ, Sch Geog, Beijing 100875, Peoples R China.
[Jiao, Ziti; Dong, Yadong; Zhang, Hu; Li, Xiaowen] Beijing Normal Univ, Beijing Key Lab Environm Remote Sensing & Digital, Beijing 100875, Peoples R China.
[Schaaf, Crystal B.; Wang, Zhuosen; Saenz, Edward] Univ Massachusetts, Dept Environm Earth & Ocean Sci, Boston, MA 02125 USA.
[Schaaf, Crystal B.; Wang, Zhuosen; Strahler, Alan] Boston Univ, Ctr Remote Sensing, Dept Earth & Environm, Boston, MA 02215 USA.
[Roman, Miguel; Wang, Zhuosen; Gatebe, Charles] NASA, Goddard Space Flight Ctr, Terr Informat Syst Lab, Greenbelt, MD USA.
[Hill, Michael J.] Univ North Dakota, Dept Earth Syst Sci & Policy, Clifford Hall,4149 Univ Ave, Grand Forks, ND 58202 USA.
[Chen, Jing M.] Univ Toronto, Dept Geog & Program Planning, 100 St George St,Room 5047, Toronto, ON M55 3G3, Canada.
[Poudyal, Rajesh] Sci Syst & Applicat Inc, Lanham, MD USA.
[Gatebe, Charles] Univ Space Res Assoc, Columbia, MD USA.
[Breon, Francois-Marie] CEA, DSM, LSCE, F-91191 Gif Sur Yvette, France.
RP Jiao, ZT (reprint author), Beijing Normal Univ, Res Ctr Remote Sensing & GIS, State Key Lab Remote Sensing Sci, Beijing 100875, Peoples R China.; Jiao, ZT (reprint author), Beijing Normal Univ, Sch Geog, Beijing 100875, Peoples R China.
EM jiaort@bnu.edu.cn
FU National Basic Research Program (973 Program) [2013CB733401]; NSFC
[41171261, 41571326]
FX This work was supported by the National Basic Research Program (973
Program, 2013CB733401) and the NSFC (41171261 and 41571326). The
POLDER-3/PARASOL BRDFs databases are elaborated by the LSCE, and
provided by the POSTEL Service Centre.
NR 52
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PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD DEC 1
PY 2016
VL 186
BP 135
EP 151
DI 10.1016/j.rse.2016.08.007
PG 17
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA EO0IW
UT WOS:000396382500011
ER
PT J
AU He, MZ
Kimball, JS
Running, S
Ballantyne, A
Guan, KY
Huemmrich, F
AF He, Mingzhu
Kimball, John S.
Running, Steven
Ballantyne, Ashley
Guan, Kaiyu
Huemmrich, Fred
TI Satellite detection of soil moisture related water stress impacts on
ecosystem productivity using the MODIS-based photochemical reflectance
index
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Photochemical reflectance index (PRI); Soil moisture; Gross primary
production (GPP); MODIS; TCF LUE model
ID LIGHT-USE EFFICIENCY; GROSS PRIMARY PRODUCTION; RADIATION-USE
EFFICIENCY; CARBON-DIOXIDE; VEGETATION INDEXES; OPTICAL INDICATOR;
DECIDUOUS FOREST; GROWING-SEASON; CO2 EXCHANGE; PINE FOREST
AB Satellite remote sensing provides continuous observations of vegetation properties that can be used to estimate global terrestrial ecosystem gross primary production (GPP). The Photochemical Reflectance Index (PRI) has been shown to be sensitive to vegetation photosynthetic light use efficiency (LUE), GPP and canopy water-stress. Here, we use the NASA EOS MODIS (Moderate Resolution Imaging Spectroradiometer) based PRI with eddy covariance CO2 flux measurements and meteorological observations from 20 tower sites representing major plant functional type (PFT) classes within the continental USA (CONUS) to assess GPP sensitivity to soil moisture related water stress. The sPRI (scaled PRI) metric derived using MODIS band 13 as a reference channel (sPRI(13)) shows generally higher correspondence with tower GPP estimates than other potential MODIS reference bands. The sPRI(13) observations were used as a proxy for soil moisture related water supply constraints to LUE within a satellite data driven terrestrial carbon flux model to estimate GPP (GPP(PRI)). The GPP calculations show generally favorable correspondence with tower GPP estimates (0.457 <= R-2 <= 0.818), except for lower GPP(PRI) performance over evergreen needleleaf forest (ENF) sites. A regional model sensitivity analysis using the sPRI(13) as a water supply proxy indicated that water restrictions limit GPP over more than 21% of the CONUS domain, particularly in drier climate areas where atmospheric moisture deficits (VPD) alone are insufficient to represent both atmosphere demand and water supply controls affecting productivity. Our results indicate strong potential of the MODIS 5PRI(13) to represent soil moisture related water supply controls influencing photosynthesis, with enhanced (1-km resolution) delineation of these processes closer to the scale of in situ tower observations. These observations may provide an effective tool for characterizing sub-grid spatial heterogeneity in soil moisture related controls that inform coarser scale observations and estimates determined from other satellite observations and earth system models. (C) 2016 Elsevier Inc. All rights reserved.
C1 [He, Mingzhu; Kimball, John S.; Running, Steven] Univ Montana, Coll Forestry & Conservat, Numer Terradynam Simulat Grp, Missoula, MT 59812 USA.
[Kimball, John S.; Running, Steven; Ballantyne, Ashley] Univ Montana, Coll Forestry & Conservat, Dept Ecosyst & Conservat Sci, Missoula, MT 59812 USA.
[Guan, Kaiyu] Stanford Univ, Dept Earth Syst Sci, Stanford, CA 94305 USA.
[Guan, Kaiyu] Univ Illinois, Dept Nat Resources & Environm Sci, Urbana, IL 61801 USA.
[Huemmrich, Fred] Univ Maryland Baltimore Cty, NASA, Goddard Space Flight Ctr, Joint Ctr Earth Syst Technol, Code 618, Greenbelt, MD 20771 USA.
RP He, MZ (reprint author), Univ Montana, Coll Forestry & Conservat, Numer Terradynam Simulat Grp, Missoula, MT 59812 USA.
EM mingzhu.he@ntsg.umt.edu
FU National Aeronautics and Space Administration [NNX15AB59G, NNX14Al50G];
U.S. Department of Energy, Biological and Environmental Research,
Terrestrial Carbon Program [DE-FG02-04ER63917, DE-FG02-04ER63911];
CarboEuropelP; FAO-GTOS-TCO; iLEAPS; Max Planck Institute for
Biogeochemistry; National Science Foundation; University of Tuscia;
Universite Laval; Environment Canada; U.S. Department of Energy
FX This study was performed at the University of Montana with funding
provided by the National Aeronautics and Space Administration
(NNX15AB59G, NNX14Al50G). This work used eddy covariance data acquired
by the FLUXNET community and in particular by the following networks:
AmeriFlux (U.S. Department of Energy, Biological and Environmental
Research, Terrestrial Carbon Program (DE-FG02-04ER63917 and
DE-FG02-04ER63911). We acknowledge the financial support to the eddy
covariance data harmonization provided by CarboEuropelP, FAO-GTOS-TCO,
iLEAPS, Max Planck Institute for Biogeochemistry, National Science
Foundation, University of Tuscia, Universite Laval, Environment Canada
and U.S. Department of Energy and the database development and technical
support from Berkeley Water Center, Lawrence Berkeley National
Laboratory, Microsoft Research eScience, Oak Ridge National Laboratory,
University of California - Berkeley and the University of Virginia.
NR 75
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U1 1
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PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD DEC 1
PY 2016
VL 186
BP 173
EP 183
DI 10.1016/j.rse.2016.08.019
PG 11
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA EO0IW
UT WOS:000396382500014
ER
PT J
AU Zhang, Q
Middleton, EM
Cheng, YB
Huemmrich, KF
Cook, BD
Corp, LA
Kustas, WP
Russ, AL
Prueger, JH
Yao, T
AF Zhang, Qingyuan
Middleton, Elizabeth M.
Cheng, Yen-Ben
Huemmrich, K. Fred
Cook, Bruce D.
Corp, Lawrence A.
Kustas, William P.
Russ, Andrew L.
Prueger, John H.
Yao, Tian
TI Integrating chlorophyll fAPAR and nadir photochemical reflectance index
from EO-1/Hyperion to predict cornfield daily gross primary production
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Daily GPP; fAPAR(chl); Chlorophyll; PRI; Cornfield; EO-1/Hyperion;
HyspIRI
ID LIGHT-USE EFFICIENCY; NET PRIMARY PRODUCTION; DECIDUOUS BROADLEAF
FOREST; RADIATIVE-TRANSFER MODELS; LEAF-AREA INDEX; MODIS DATA; CANOPY
REFLECTANCE; GLOBAL VEGETATION; CONIFEROUS FOREST; CARBON EXCHANGE
AB The concept of light use efficiency (s) and the concept of fraction of photosynthetically active ration (PAR) absorbed for vegetation photosynthesis (PSN), i.e., fAPAR(PSN), have been widely utilized to estimate vegetation gross primary productivity (GPP). It has been demonstrated that the photochemical reflectance index (PRI) is empirically related to epsilon. An experimental US Department of Agriculture (USDA) cornfield in Maryland was selected as our study field. We explored the potential of integrating fAPAR(chl) (defined as the fraction of PAR absorbed by chlorophyll) and nadir PRI (PRInadir) to predict cornfield daily GPP. We acquired nadir or near-nadir EO-1/Hyperion satellite images that covered the cornfield and took nadir in-situ field spectral measurements. Those data were used to derive the PRInadir and fAPARchi. The fAPARchi is retrieved with the advanced radiative transfer model PROSAIL2 and the Metropolis approach, a type of Markov Chain Monte Carlo (MCMC) estimation procedure. We define chlorophyll light use efficiency (epsilon(chl)) as the ratio of vegetation GPP as measured by eddy covariance techniques to PAR absorbed by chlorophyll (epsilon(chl) = GPP/APAR(chl)). Daily epsilon(chl) retrieved with the EO-1 Hyperion images was regressed with a linear equation of PRInadir (epsilon(chl) = alpha x PRInadir + beta). The satellite CchlPRI(nadir) linear relationship for the cornfield was implemented to develop an integrated daily GPP model [GPP = (alpha x PRInadir P) x fAPAR(chl) x PAR], which was evaluated with fAPAR(chl) and PRInadir retrieved from field measurements. Daily GPP estimated with this fAPAR(chl)-PRInadir integration model was strongly correlated with the observed tower in-situ daily GPP (R-2 = 0.93); with a root mean square error (RMSE) of 1.71 g C mot(-1) PPFD and coefficient of variation (CV) of 16.57%. Both seasonal epsilon(chl) and PRInadir were strongly correlated with fAPAR(chl) retrieved from field measurements, which indicates that chlorophyll content strongly affects seasonal Echi and PRInadir. We demonstrate the potential capacity to monitor GPP with space-based visible through shortwave infrared (VSWIR) imaging spectrometers such as NASA's soon to be decommissioned EO-1/Hyperion and the future Hyperspectral Infrared Imager (HyspIRl). (C) 2016 Elsevier Inc. All rights reserved.
C1 [Zhang, Qingyuan; Yao, Tian] Unversities Space Res Assoc, Columbia, MD 21044 USA.
[Zhang, Qingyuan; Middleton, Elizabeth M.; Cheng, Yen-Ben; Huemmrich, K. Fred; Cook, Bruce D.; Corp, Lawrence A.; Yao, Tian] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Code 618, Greenbelt, MD 20771 USA.
[Cheng, Yen-Ben] Sigma Space Corp, Lanham, MD 20706 USA.
[Huemmrich, K. Fred] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Corp, Lawrence A.] Syst Sci & Applicat Inc, Lanham, MD 20706 USA.
[Kustas, William P.; Russ, Andrew L.] USDA Agr Res Serv, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA.
[Prueger, John H.] USDA Agr Res Serv, Ames, IA 50011 USA.
RP Zhang, Q (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Code 618, Greenbelt, MD 20771 USA.
EM qyz72@yahoo.com
FU NASA; NASA Terrestrial Ecology Program [NNX12AJ51G]; Science of Terra
and Aqua Program [NNX14AK50G]
FX This study was partially supported by two NASA Headquarters sponsored
programs (PI: E. Middleton), the Earth Observing One (EO-1) Mission
Science Office (Sponsor, Dr. Garik Gutman) and the HyspIRI science
support project at the Goddard Space Flight Center (NASA/GSFC), through
Mr. William (Woody) Turner. This work was also partially funded by the
NASA Terrestrial Ecology Program (Grant # NNX12AJ51G, PI: Q. Zhang) and
the Science of Terra and Aqua Program (Grant # NNX14AK50G, PI: Q.
Zhang). USDA is an equal opportunity provider and employer.
NR 108
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Z9 0
U1 1
U2 1
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD DEC 1
PY 2016
VL 186
BP 311
EP 321
DI 10.1016/j.rse.2016.08.026
PG 11
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA EO0IW
UT WOS:000396382500024
ER
PT J
AU Meerdink, SK
Roberts, DA
King, JY
Roth, KL
Dennison, PE
Amaral, CH
Hook, SJ
AF Meerdink, Susan K.
Roberts, Dar A.
King, Jennifer Y.
Roth, Keely L.
Dennison, Philip E.
Amaral, Cibele H.
Hook, Simon J.
TI Linking seasonal foliar traits to VSWIR-TIR spectroscopy across
California ecosystems
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Leaf traits; Visible Shortwave Infrared (VSWIR); Thermal Infrared (TIR);
HyspIRl; AVIRIS; HyTES; Spectroscopy; Partial least squares regression
ID NEAR-INFRARED REFLECTANCE; IMAGING SPECTROSCOPY; SPECTRAL REFLECTANCE;
TROPICAL FORESTS; WATER-CONTENT; MU-M; NITROGEN CONCENTRATION;
HYPERSPECTRAL DATA; LEAF; PLANT
AB Vegetation traits provide critical information on ecosystem function that can be used to assess the effects of disturbance, land use, and climate change. Recent studies have demonstrated the use of spectroscopy to predict vegetation traits accurately and efficiently. To date, most spectroscopic studies have utilized data from the Visible Short Wave Infrared spectrum (VSWIR) or, occasionally, the Thermal Infrared spectrum (TIR), but not in combination. This study focuses on VSWIR and TIR synergy to evaluate the ability to predict leaf level cellulose, lignin, leaf mass per area (LMA), nitrogen, and water content across seasons. We used fresh leaves from sixteen common California shrub and tree species collected in the 2013 spring, summer, and fall seasons. The 284 samples exhibited a wide range of leaf traits as determined by standard analytical procedures: 4.2-27.3% for cellulose, 2.6-22.5% for lignin, 34.7-388.9 g/m(2) for LMA, 0.45-3.81% for nitrogen, and 20.2-76.9% for water content. For each leaf trait, partial least squares regression (PLSR) models were fit using different portions of the spectrum: VSWIR (0.35-2.5 mu m), TIR (2.5-15.4 mu m), and Full spectrum (0.35-15.4 mu m). We also fit PLSR models using spectra resampled to simulate three airborne sensors: the Airborne Visible/Infrared Imaging Spectrometer (AVIRIS; 0.4-2.5 mu m), the Hyperspectral Thermal Emission Spectrometer (HyTES; 7.5-12 mu m), and the Hyperspectral InfraRed Imager (HyspIRl; 0.4-12 mu m). The majority of best performing models used the Full spectrum, demonstrating the value of combining TIR and VSWIR spectra for leaf trait prediction. Sensor simulated PLSR models created with the entire data set yielded validation R-2 and root mean square error of prediction (RMSEP) values as follows: R-2 = 0.70 and RMSEP = 13.1% for cellulose, R-2 = 0.50 and RMSEP = 17.7% for lignin, R-2 = 0.56 and RMSEP = 18.3% for LMA, R-2 = 0.56 and RMSEP = 18.1% for nitrogen, and R-2 = 0.89 and RMSEP = 5.7% for water content. General models successfully captured the variability among all seasons and leaf forms for cellulose and water content, while the other leaf traits were better modeled with season or leaf form -specific models. This study successfully captured the large seasonal and geographical variation in leaf traits across California's diverse ecosystems, supporting the possibility of using HyspIRl's imagery for global mapping efforts of these traits. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Meerdink, Susan K.; Roberts, Dar A.; King, Jennifer Y.] Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA.
[Roth, Keely L.] Univ Calif Davis, Dept Land & Water Resources, Dept Air & Water Resources, Davis, CA 95616 USA.
[Dennison, Philip E.] Univ Utah, Dept Geog, Salt Lake City, UT 84112 USA.
[Amaral, Cibele H.] Univ Fed Vicosa, Dept Forest Engn, Avenida Purdue sn,Campus Univ, BR-36570900 Vicosa, MG, Brazil.
[Hook, Simon J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Meerdink, SK (reprint author), Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA.
EM susan.meerdink@gmail.com
FU NASA [NNX12AP08G]; Sao Paulo Research Foundation [10/51718-0]
FX We wish to thank Dr. Carla D'Antonio for the use of her laboratory and
equipment. This research was supported by NASA grant NNX12AP08G, HyspIRI
discrimination of plant species and functional types along a strong
environmental-temperature gradient. A portion of this work was carried
out at the Jet Propulsion Laboratory/California Institute of Technology,
Pasadena, California, under contract with the National Aeronautics and
Space Administration. Dr. Cibele Hummel do Amaral thanks the Sao Paulo
Research Foundation (# 10/51718-0) for supporting her stay in the United
States.
NR 59
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U1 2
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PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD DEC 1
PY 2016
VL 186
BP 322
EP 338
DI 10.1016/j.rse.2016.08.003
PG 17
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA EO0IW
UT WOS:000396382500025
ER
PT J
AU Ramsey, E
Rangoonwala, A
Jones, CE
AF Ramsey, Elijah, III
Rangoonwala, Amina
Jones, Cathleen E.
TI Marsh canopy structure changes and the Deepwater Horizon oil spill
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE NASA UAVSAR; Polarimetric synthetic aperture radar (PoISAR); Deepwater
Horizon oil spill; Leaf area index (LAI) and leaf angle distribution
(LAD); Marsh change maps
ID POLARIMETRIC RADAR; BARATARIA BAY; LOUISIANA; RECOVERY; IMPACTS;
DIEBACK; SAR
AB Marsh canopy structure was mapped yearly from 2009 to 2012 in the Barataria Bay, Louisiana coastal region that was impacted by the 2010 Deepwater Horizon (DWH) oil spill. Based on the previously demonstrated capability of NASA's UAVSAR polarimetric synthetic aperture radar (PoISAR) image data to map Spartina alterniflora marsh canopy structure, structure maps combining the leaf area index (LAI) and leaf angle distribution (IAD, orientation) were constructed for yearly intervals that were directly relatable to the 2010 LAI-LAD classification. The yearly LAI-LAD and LAI difference maps were used to investigate causes for the previously revealed dramatic change in marsh structure from prespill (2009) to postspill (2010, spill cessation), and the occurrence of structure features that exhibited abnormal spatial and temporal patterns. Water level and salinity records showed that freshwater releases used to keep the oil offshore did not cause the rapid growth from 2009 to 2010 in marsh surrounding the inner Bay. Photointerpretation of optical image data determined that interior marsh patches exhibiting rapid change were caused by burns and burn recovery, and that the pattern of 2010 to 2011 1AI decreases in backshore marsh and extending along some tidal channels into the interior marsh were not associated with burns. Instead, the majority of 2010 to 2011 shoreline features aligned with vectors displaying the severity of 2010 shoreline oiling from the DWH spill. Although the association is not conclusive of a causal oil impact, the coexistent pattern is a significant discovery. PoISAR marsh structure mapping provided a unique perspective of marsh biophysical status that enhanced detection of change and monitoring of trends important to management effectiveness. Published by Elsevier Inc.
C1 [Ramsey, Elijah, III; Rangoonwala, Amina] Wetland & Aquat Res Ctr, Us Geol Survey, 700 Cajundome Blvd, Lafayette, IA 70506 USA.
[Jones, Cathleen E.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Ramsey, E (reprint author), Wetland & Aquat Res Ctr, Us Geol Survey, 700 Cajundome Blvd, Lafayette, IA 70506 USA.
EM ramseye@usgs.gov
FU National Aeronautics Space Administration (NASA) [11-TE11-104]
FX We thank Francis Fields Jr. of the Apache Louisiana Minerals LLC, a
subsidiary of Apache Corporation, for access to their properties and
Jeff Deblieux IV of the Louisiana Land and Exploration Company, a
subsidiary of Conoco Phillips, for access to their properties. We are
indebted to late Clint Jeske of the U.S. Geological Survey for his
invaluable assistance in field reconnaissance. We thank William Jones of
the U.S. Geological Survey and Corey Hotard a U.S. Geological Survey
student intern for locating archived optical image data. Research was
supported in part by the National Aeronautics Space Administration
(NASA) grant #11-TE11-104 and was carried out in collaboration with the
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with NASA. UAVSAR data are provided courtesy of
NASA/JPL-Caltech. Any use of trade, firm, or product names is for
descriptive purposes only and does not imply endorsement by the U.S.
Government.
NR 24
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PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD DEC 1
PY 2016
VL 186
BP 350
EP 357
DI 10.1016/j.rse.2016.08.001
PG 8
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA EO0IW
UT WOS:000396382500027
ER
PT J
AU Eitel, JUH
Hofle, B
Vierling, LA
Abellan, A
Asner, GP
Deems, JS
Glennie, CL
Joerg, PC
LeWinter, AL
Magney, TS
Mandlburger, G
Morton, DC
Muller, J
Vierling, KT
AF Eitel, Jan U. H.
Hoefle, Bernhard
Vierling, Lee A.
Abellan, Antonio
Asner, Gregory P.
Deems, Jeffrey S.
Glennie, Craig L.
Joerg, Philip C.
LeWinter, Adam L.
Magney, Troy S.
Mandlburger, Gottfried
Morton, Douglas C.
Mueller, Joerg
Vierling, Kerri T.
TI Beyond 3-D: The new spectrum of lidar applications for earth and
ecological sciences
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Review
DE Multitemporal lidar; Hypertemporal lidar; Multispectral lidar;
Hyperspectral lidar; Laser return intensity; Data dimensions
ID TERRESTRIAL LASER SCANNER; WAVE-FORM LIDAR; GROUND-BASED LIDAR;
DISCRETE-RETURN LIDAR; LEAF-AREA INDEX; HYPERSPECTRAL DATA FUSION; WHEAT
NITROGEN STATUS; FOREST CARBON STOCKS; AIRBORNE LIDAR; CANOPY STRUCTURE
AB Capturing and quantifying the world in three dimensions (x,y,z) using light detection and ranging (lidar) technology drives fundamental advances in the Earth and Ecological Sciences (EES). However, additional lidar dimensions offer the possibility to transcend basic 3-D mapping capabilities, including i) the physical time (t) dimension from repeat lidar acquisition and ii) laser return intensity (LRIK) data dimension based on the brightness of single- or multi-wavelength (lambda) laser returns. The additional dimensions thus add to the x,y, and z dimensions to constitute the five dimensions of lidar (x.y,z, t, lambda n). This broader spectrum of lidar dimensionality has already revealed new insights across multiple EES topics, and will enable a wide range of new research and applications. Here, we review recent advances based on repeat lidar collections and analysis of LRI data to highlight novel applications of lidar remote sensing beyond 3-D. Our review outlines the potential and current challenges of time and LRI information from lidar sensors to expand the scope of research applications and insights across the full range of EES applications. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Eitel, Jan U. H.; Vierling, Lee A.] Univ Idaho, Geospatial Lab Environm Dynam, Moscow, ID 83844 USA.
[Hoefle, Bernhard; Abellan, Antonio] McCall Outdoor Sci Sch, Univ Idaho, McCall, ID 83638 USA.
[Hoefle, Bernhard] Heidelberg Univ, Inst Geog, GISci Res Grp, D-69120 Heidelberg, Germany.
[Abellan, Antonio] Univ Lausanne, Risk Anal Grp, CH-1015 Lausanne, Switzerland.
[Joerg, Philip C.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA.
[Deems, Jeffrey S.] Univ Colorado, Natl Snow & Ice Data Ctr, Boulder, CO 80309 USA.
[Glennie, Craig L.] Univ Houston, Dept Civil Environm Engn, Houston, TX USA.
[Joerg, Philip C.] Univ Zurich, Dept Geog, CH-8057 Zurich, Switzerland.
[LeWinter, Adam L.] S Army Corps Engn, Cold Regions Res & Engn Lab, Hanover, NH 03766 USA.
[Magney, Troy S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mandlburger, Gottfried] TU Wien, Dept Geodesy & Geoinformat, A-1040 Vienna, Austria.
[Morton, Douglas C.] NASA Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Mueller, Joerg] Bavarian Forest Natl Pk, D-94481 Grafenau, Germany.
[Mueller, Joerg] Univ Wilrzburg, Field Stn Fabrikschleichach Biocenter, D-96181 Rauhenebrach, Germany.
[Vierling, Kerri T.] Univ Idaho, Dept Fish & Wildlife, Moscow, ID 83844 USA.
RP Eitel, JUH (reprint author), Univ Idaho, Geospatial Lab Environm Dynam, Moscow, ID 83844 USA.
EM jeitel@uidaho.edu
RI Hofle, Bernhard/A-4702-2010
OI Hofle, Bernhard/0000-0001-5849-1461
FU USDA-NIFA [2011-67003-3034, 2011-68002-30191]; NASA Terrestrial Ecology
[NNX12AK83G, NNX15AT86A]; Ministry of Science, Research and Arts,
Baden-Wuerttemberg [7635.521/Hofle]; Austrian Research Promotion Agency
(FFG) project "Alpine Airborne Hydromapping - from research to
practice"; NASA
FX We thank Dr. Alan Strahler and two anonymous reviewers for their
thoughtful comments and edits that helped to greatly improve the
manuscript. We further thank Matt Daniels for his help with some of the
graphics shown in the manuscript. Jan Eitel and Lee Vierling were
supported by USDA-NIFA Award Nos. 2011-67003-3034 and 2011-68002-30191
and funding from NASA Terrestrial Ecology grants NNX12AK83G and
NNX15AT86A. Bernhard Hofle was supported by the Ministry of Science,
Research and Arts, Baden-Wuerttemberg (Grant no. 7635.521/Hofle), within
the project "4DEMON: 4D Near Real-Time Environmental Monitoring"
(http://www.uni-heidelberg.de/4demon). Gottfried Mandlburger was
supported by the Austrian Research Promotion Agency (FFG) project
"Alpine Airborne Hydromapping - from research to practice". Douglas
Morton was supported by NASA's Terrestrial Ecology and Carbon Monitoring
System Programs. Use of trade names does not constitute an official
endorsement by the authors.
NR 314
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U1 1
U2 1
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD DEC 1
PY 2016
VL 186
BP 372
EP 392
DI 10.1016/j.rse.2016.08.018
PG 21
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA EO0IW
UT WOS:000396382500029
ER
PT J
AU Ibrahim, A
Gilerson, A
Chowdhary, J
Ahmed, S
AF Ibrahim, Amir
Gilerson, Alexander
Chowdhary, Jacek
Ahmed, Samir
TI Retrieval of macro- and micro-physical properties of oceanic hydrosols
from polarimetric observations
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Remote sensing; Polarization; Hydrosol; Ocean color; Case-I waters; Case
II waters; Bio-optics; Chlorophyll a; CDOM; Plankton; Minerals;
Scattering; Vector radiative transfer modeling; Aerosol; Cloud; Ocean
ecosystem; PACE
ID INHERENT OPTICAL-PROPERTIES; WATER-LEAVING RADIANCES; COASTAL WATERS;
SIZE DISTRIBUTION; MARINE PARTICLES; LIGHT-SCATTERING; POLARIZED
REFLECTANCE; RADIATIVE-TRANSFER; REFRACTIVE-INDEX; BEAM ATTENUATION
AB Remote sensing has mainly relied on measurements of scalar radiance and its spectral and angular features to retrieve micro- and macro-physical properties of aerosols/hydrosols. However, it is recognized that measurements that include the polarimetric characteristics of light provide more intrinsic information about particulate scattering. To take advantage of this, we used vector radiative transfer (VRT) simulations and developed an analytical relationship to retrieve the macro and micro-physical properties of the oceanic hydrosols. Specifically, we investigated the relationship between the observed degree of linear polarization (DoLP) and the ratio of attenuation to-absorption coefficients (c/a) in water, from which the scattering coefficient can be readily computed (b = c - a), after retrieving a. This relationship was parameterized for various scattering geometries, including sensor zenith/azimuth angles relative to the Sun's principal plane, and for varying Sun zenith angles. An inversion method was also developed for the retrieval of the microphysical properties of hydrosols, such as the bulk refractive index and the particle size distribution. The DoLP vs c/a relationship was tested and validated against in-situ measurements of underwater light polarization obtained by a custom-built polarimeter and measurements of the coefficients a and c, obtained using an in-water WET Labs ac-s instrument package. These measurements confirmed the validity of the approach, with retrievals of attenuation coefficients showing a high coefficient of determination depending on the wavelength. We also performed a sensitivity analysis of the DoLP at the Top of Atmosphere (TOA) over coastal waters showing the possibility of polarimetric remote sensing application for ocean color. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Ibrahim, Amir; Gilerson, Alexander; Ahmed, Samir] CUNY City Coll, Dept Elect Engn, Opt Remote Sensing Lab, New York, NY 10031 USA.
[Ibrahim, Amir] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ibrahim, Amir] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Chowdhary, Jacek] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY 10025 USA.
[Chowdhary, Jacek] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Ibrahim, A (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM amir.ibrahim@nasa.gov
OI Ibrahim, Amir/0000-0002-3290-056X
FU Ocean Biology and Biochemistry Program of National Aeronautics and Space
Administration (NASA) [NNX13AF44G]; National Oceanic and Atmospheric
Administration (NOAA) [NA11SEC4810004]; Office of Naval Research (ONR)
[N00014-09-1-1054]
FX The Ocean Biology and Biochemistry Program of National Aeronautics and
Space Administration (NASA NNX13AF44G), National Oceanic and Atmospheric
Administration (NOAA NA11SEC4810004), and the Office of Naval Research
(ONR N00014-09-1-1054) funded this research. We acknowledge our thanks
to Dr. Samantha Weltz and Amy Houghton for editorial efforts to improve
the manuscript and the anonymous reviewers for their insightful remarks.
NR 68
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Z9 1
U1 1
U2 1
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD DEC 1
PY 2016
VL 186
BP 548
EP 566
DI 10.1016/j.rse.2016.09.004
PG 19
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA EO0IW
UT WOS:000396382500042
ER
PT J
AU Hall, FG
AF Hall, Forrest G.
TI Tribute to Thomas Hilker
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Biographical-Item
C1 [Hall, Forrest G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Hall, FG (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD DEC 1
PY 2016
VL 186
BP A1
EP A2
DI 10.1016/j.rse.2016.10.028
PG 2
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA EO0IW
UT WOS:000396382500034
ER
PT J
AU Correa, J
Marras, A
Wunderer, CB
Gottlicher, P
Lange, S
Reza, S
Shevyakov, I
Tennert, M
Niemann, M
Hirsemann, H
Smoljanin, S
Supra, J
Xia, Q
Zimmer, M
Allahgholi, A
Gloskovskii, A
Viefhaus, J
Scholz, F
Seltmann, J
Klumpp, S
Cautero, G
Giuressi, D
Khromova, A
Menk, R
Pinaroli, G
Stebel, L
Rinaldi, S
Zema, N
Catone, D
Pedersen, U
Tartoni, N
Guerrini, N
Marsh, B
Sedgwick, I
Nicholls, T
Turchetta, R
Hyun, HJ
Kim, KS
Rah, SY
Hoenk, ME
Jewell, AD
Jones, TJ
Nikzad, S
Graafsma, H
AF Correa, J.
Marras, A.
Wunderer, C. B.
Goettlicher, P.
Lange, S.
Reza, S.
Shevyakov, I.
Tennert, M.
Niemann, M.
Hirsemann, H.
Smoljanin, S.
Supra, J.
Xia, Q.
Zimmer, M.
Allahgholi, A.
Gloskovskii, A.
Viefhaus, J.
Scholz, F.
Seltmann, J.
Klumpp, S.
Cautero, G.
Giuressi, D.
Khromova, A.
Menk, R.
Pinaroli, G.
Stebel, L.
Rinaldi, S.
Zema, N.
Catone, D.
Pedersen, U.
Tartoni, N.
Guerrini, N.
Marsh, B.
Sedgwick, I.
Nicholls, T.
Turchetta, R.
Hyun, H. J.
Kim, K. S.
Rah, S. Y.
Hoenk, M. E.
Jewell, A. D.
Jones, T. J.
Nikzad, S.
Graafsma, H.
TI On the Charge Collection Efficiency of the PERCIVAL Detector
SO JOURNAL OF INSTRUMENTATION
LA English
DT Article
DE Instrumentation for FEL; Solid state detectors; X-ray detectors
ID PETRA III
AB The PERCIVAL soft X-ray imager is being developed by DESY, RAL, Elettra, DLS, and PAL to address the challenges at high brilliance Light Sources such as new-generation Synchrotrons and Free Electron Lasers. Typical requirements for detector systems at these sources are high frame rates, large dynamic range, single-photon counting capability with low probability of false positives, high quantum efficiency, and (multi)-mega-pixel arrangements. PERCIVAL is a monolithic active pixel sensor, based on CMOS technology. It is designed for the soft X-ray regime and, therefore, it is post-processed in order to achieve high quantum efficiency in its primary energy range (250 eV to 1 keV). This work will report on the latest experimental results on charge collection efficiency obtained for multiple back-side-illuminated test sensors during two campaigns, at the P04 beam-line at PETRA III, and the CiPo beam-line at Elettra, spanning most of the primary energy range as well as testing the performance for photon-energies below 250 eV. In addition, XPS surface analysis was used to cross-check the obtained results.
C1 [Correa, J.; Marras, A.; Wunderer, C. B.; Goettlicher, P.; Lange, S.; Reza, S.; Shevyakov, I.; Tennert, M.; Niemann, M.; Hirsemann, H.; Smoljanin, S.; Supra, J.; Xia, Q.; Zimmer, M.; Allahgholi, A.; Gloskovskii, A.; Viefhaus, J.; Scholz, F.; Seltmann, J.; Klumpp, S.; Graafsma, H.] DESY, Deutsch Elektronensynchrotron, Notkestr 85, D-22607 Hamburg, Germany.
[Correa, J.; Marras, A.; Wunderer, C. B.; Lange, S.; Tennert, M.; Niemann, M.; Hirsemann, H.; Smoljanin, S.; Allahgholi, A.] CFEL, Ctr Free Electron Laser Sci, Luruper Ch 149, D-22607 Hamburg, Germany.
[Cautero, G.; Giuressi, D.; Khromova, A.; Menk, R.; Pinaroli, G.; Stebel, L.; Rinaldi, S.] Elettra Sincrotrone Trieste, SS 14 Km 163-5, I-34149 Trieste, Italy.
[Pedersen, U.; Tartoni, N.] DLS, Diamond Light Source, Didcot OX11 ODE, Oxon, England.
[Guerrini, N.; Marsh, B.; Sedgwick, I.; Nicholls, T.; Turchetta, R.] RAL, STFC, Didcot OX11 0QX, Oxon, England.
[Hyun, H. J.; Kim, K. S.; Rah, S. Y.] PAL, Jigokro 127 Beongil, Pohang 790834, South Korea.
[Hoenk, M. E.; Jewell, A. D.; Jones, T. J.; Nikzad, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Reza, S.; Graafsma, H.] Mid Sweden Univ, Holmgatan 10, S-85170 Sundsvall, Sweden.
[Zema, N.; Catone, D.] CNR, Ist Struttura Mat, Via Fosso Cavaliere 100, I-00133 Rome, Italy.
[Khromova, A.] Univ Trieste, Piazzale Europa 1, I-34128 Trieste, Italy.
[Pinaroli, G.] Univ Udine, Via Sci 206, I-33100 Udine, Italy.
RP Correa, J (reprint author), DESY, Deutsch Elektronensynchrotron, Notkestr 85, D-22607 Hamburg, Germany.; Correa, J (reprint author), CFEL, Ctr Free Electron Laser Sci, Luruper Ch 149, D-22607 Hamburg, Germany.
EM Jonathan.Correa@desy.de
NR 10
TC 0
Z9 0
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-0221
J9 J INSTRUM
JI J. Instrum.
PD DEC
PY 2016
VL 11
AR C12032
DI 10.1088/1748-0221/11/12/C12032
PG 7
WC Instruments & Instrumentation
SC Instruments & Instrumentation
GA EN0WJ
UT WOS:000395731900032
ER
PT J
AU D'Ai, A
Evans, PA
Burrows, DN
Kuin, NPM
Kann, DA
Campana, S
Maselli, A
Romano, P
Cusumano, G
La Parola, V
Barthelmy, SD
Beardmore, AP
Cenko, SB
De Pasquale, M
Gehrels, N
Greiner, J
Kennea, JA
Klose, S
Melandri, A
Nousek, JA
Osborne, JP
Palmer, DM
Sbarufatti, B
Schady, P
Siegel, MH
Tagliaferri, G
Yates, R
Zane, S
AF D'Ai, A.
Evans, P. A.
Burrows, D. N.
Kuin, N. P. M.
Kann, D. A.
Campana, S.
Maselli, A.
Romano, P.
Cusumano, G.
La Parola, V.
Barthelmy, S. D.
Beardmore, A. P.
Cenko, S. B.
De Pasquale, M.
Gehrels, N.
Greiner, J.
Kennea, J. A.
Klose, S.
Melandri, A.
Nousek, J. A.
Osborne, J. P.
Palmer, D. M.
Sbarufatti, B.
Schady, P.
Siegel, M. H.
Tagliaferri, G.
Yates, R.
Zane, S.
TI Evidence for the magnetar nature of 1E 161348-5055 in RCW 103
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE X-rays: general; X-rays: individual: 1E 161348-5055
ID X-RAY SOURCE; SUPERNOVA REMNANT RCW-103; CENTRAL COMPACT OBJECTS;
NEUTRON-STARS; GALACTIC MAGNETAR; ANTI-MAGNETARS; SPIN-DOWN; OUTBURST;
PULSAR; TELESCOPE
AB We report on the detection of a bright, short, structured X-ray burst coming from the supernova remnant RCW 103 on 2016 June 22 caught by the Swift/Burst Alert Telescope (BAT) monitor, and on the follow-up campaign made with Swift/X-ray Telescope, Swift/UV/Optical Telescope, and the optical/near-infrared (NIR) Gamma-Ray burst Optical and Near-infrared Detector. The characteristics of this flash, such as duration and spectral shape, are consistent with typical short bursts observed from soft gamma repeaters. The BAT error circle at 68 per cent confidence range encloses the point-like X-ray source at the centre of the nebula, 1E 161348-5055. Its nature has been long debated due to a periodicity of 6.67 h in X-rays, which could indicate either an extremely slow pulsating neutron star, or the orbital period of a very compact X-ray binary system. We found that 20 min before the BAT trigger, the soft X-ray emission of 1E 161348-5055 was a factor of similar to 100 higher than measured 2 yr earlier, indicating that an outburst had already started. By comparing the spectral and timing characteristics of the source in the 2 yr before the outburst and after the BAT event, we find that, besides a change in luminosity and spectral shape, also the 6.67 h pulsed profile has significantly changed with a clear phase shift with respect to its low-flux profile. The UV/optical/NIR observations did not reveal any counterpart at the position of 1E 161348-5055. Based on these findings, we associate the BAT burst with 1E 161348-5055, we classify it as a magnetar, and pinpoint the 6.67 h periodicity as the magnetar spin period.
C1 [D'Ai, A.; Maselli, A.; Romano, P.; Cusumano, G.; La Parola, V.] INAF IASF Palermo, Via Ugo La Malfa 153, I-90146 Palermo, Italy.
[Evans, P. A.; Beardmore, A. P.; Osborne, J. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Burrows, D. N.; Kennea, J. A.; Nousek, J. A.; Sbarufatti, B.; Siegel, M. H.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
[Kuin, N. P. M.; De Pasquale, M.; Zane, S.] UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Kann, D. A.] Thuringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, Germany.
[Campana, S.; Melandri, A.; Sbarufatti, B.; Tagliaferri, G.] Osserv Astron Brera, INAF, Via E Bianchi 46, I-23807 Merate, Italy.
[Barthelmy, S. D.; Cenko, S. B.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Mail Code 661, Greenbelt, MD 20771 USA.
[Cenko, S. B.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Greiner, J.; Schady, P.; Yates, R.] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany.
[Palmer, D. M.] Los Alamos Natl Lab, B244, Los Alamos, NM 87545 USA.
RP D'Ai, A (reprint author), INAF IASF Palermo, Via Ugo La Malfa 153, I-90146 Palermo, Italy.
EM antonino.dai@ifc.inaf.it
OI Sbarufatti, Boris/0000-0001-6620-8347
FU UK Space Agency; Leibniz-Prize; DFG [HA 1850/28-1]; [ASI-INAF
I/004/11/0]
FX The authors are very grateful to Amy Y. Lien for her support in the data
reduction and analysis of the BAT data. PAE, APB, NPMK, and JPO
acknowledge Swift funding from the UK Space Agency. We acknowledge
contract ASI-INAF I/004/11/0.; Part of the funding for GROND (both
hardware as well as personnel) was generously granted from the
Leibniz-Prize to Professor G. Hasinger (DFG grant HA 1850/28-1). This
work made use of data supplied by the UK Swift Science Data Centre at
the University of Leicester. This research has made use of the XRT Data
Analysis Software (XRTDAS) developed under the responsibility of the ASI
Science Data Center (ASDC), Italy.
NR 59
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U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD DEC
PY 2016
VL 463
IS 3
BP 2394
EP 2404
DI 10.1093/mnras/stw2023
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EJ9SC
UT WOS:000393566000011
ER
PT J
AU Guillot, S
Kaspi, VM
Archibald, RF
Bachetti, M
Flynn, C
Jankowski, F
Bailes, M
Boggs, S
Christensen, FE
Craig, WW
Hailey, CA
Harrison, FA
Stern, D
Zhang, WW
AF Guillot, S.
Kaspi, V. M.
Archibald, R. F.
Bachetti, M.
Flynn, C.
Jankowski, F.
Bailes, M.
Boggs, S.
Christensen, F. E.
Craig, W. W.
Hailey, C. A.
Harrison, F. A.
Stern, D.
Zhang, W. W.
TI The NuSTAR view of the non-thermal emission from PSR J0437-4715
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: neutron; pulsars: individual: PSR 0437-4715
ID MILLISECOND PULSAR J0437-4715; HIGH-ENERGY EMISSION; EQUATION-OF-STATE;
XMM-NEWTON OBSERVATIONS; X-RAY OBSERVATIONS; NEUTRON-STAR; DENSE MATTER;
RADIUS CONSTRAINTS; GLOBULAR-CLUSTERS; IMPROVED MASS
AB We present a hard X-ray Nuclear Spectroscopic Telescope Array (NuSTAR) observation of PSR J0437-4715, the nearest millisecond pulsar. The known pulsations at the apparent pulse period similar to 5.76 ms are observed with a significance of 3.7 sigma, at energies up to 20 keV above which the NuSTAR background dominates. We measure a photon index Gamma = 1.50 +/- 0.25 (90 per cent confidence) for the power-law fit to the non-thermal emission. It had been shown that spectral models with two or three thermal components fit the XMM-Newton spectrum of PSR J0437-4715, depending on the slope of the power-law component, and the amount of absorption of soft X-rays. The new constraint on the high-energy emission provided by NuSTAR removes ambiguities regarding the thermal components of the emission below 3 keV. We performed a simultaneous spectral analysis of the XMM-Newton and NuSTAR data to confirm that three thermal components and a power law are required to fit the 0.3-20 keV emission of PSR J0437-4715. Adding a ROSAT-PSPC spectrum further confirmed this result and allowed us to better constrain the temperatures of the three thermal components. A phase-resolved analysis of the NuSTAR data revealed no significant change in the photon index of the high-energy emission. This NuSTAR observation provides further impetus for future observations with the NICER mission (Neutron Star Interior Composition Explorer) whose sensitivity will provide much stricter constraints on the equation of state of nuclear matter by combining model fits to the pulsar's phase-folded light curve with the pulsar's well-defined mass and distance from radio timing observations.
C1 [Guillot, S.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Av Vicuna Mackenna 4860, Santiago 7820436, Chile.
[Guillot, S.; Kaspi, V. M.; Archibald, R. F.] McGill Univ, Dept Phys, 3600 Rue Univ Montreal, Montreal, PQ H3A 2T8, Canada.
[Guillot, S.; Kaspi, V. M.; Archibald, R. F.] McGill Univ, McGill Space Inst, 3600 Rue Univ Montreal, Montreal, PQ H3A 2T8, Canada.
[Bachetti, M.] Osservatorio Astron Cagliari, Via Sci 5, I-09047 Selargius, Italy.
[Flynn, C.; Jankowski, F.; Bailes, M.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, POB 218, Hawthorn, Vic 3122, Australia.
[Flynn, C.; Jankowski, F.; Bailes, M.] Swinburne Univ Technol, ARC Ctr All Sky Astrophys CAASTRO, POB 218, Hawthorn, Vic 3122, Australia.
[Boggs, S.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Christensen, F. E.; Craig, W. W.] Tech Univ Denmark, Natl Space Inst, DTU Space, Elektrovej 327, DK-2800 Lyngby, Denmark.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Hailey, C. A.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Harrison, F. A.] CALTECH, Space Radiat Lab, 1200 E Calif Blvd,MC 249-17, Pasadena, CA 91125 USA.
[Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, W. W.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 661, Greenbelt, MD 20771 USA.
RP Guillot, S (reprint author), Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Av Vicuna Mackenna 4860, Santiago 7820436, Chile.; Guillot, S (reprint author), McGill Univ, Dept Phys, 3600 Rue Univ Montreal, Montreal, PQ H3A 2T8, Canada.; Guillot, S (reprint author), McGill Univ, McGill Space Inst, 3600 Rue Univ Montreal, Montreal, PQ H3A 2T8, Canada.
EM sguillot@astro.puc.cl
OI Jankowski, Fabian/0000-0002-6658-2811
FU National Aeronautics and Space Administration; NSERC; Centre de
Recherche en Astrophysique du Quebec; R. Howard Webster Foundation from
the Canadian Institute for Advanced Study; Canada Research Chairs
Program; Lorne Trottier Chair in Astrophysics and Cosmology; Australian
Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO)
[CE110001020]; [3150428]
FX The authors thank the referee, Slavko Bogdanov, for very useful
suggestions that significantly improved this paper. This work made use
of data from the NuSTAR mission, a project led by the California
Institute of Technology, managed by the Jet Propulsion Laboratory, and
funded by the National Aeronautics and Space Administration. The data
analysis was performed with the NuSTAR Data Analysis Software
(NUSTARDAS) jointly developed by the ASI Science Data Center (ASDC,
Italy) and the California Institute of Technology (USA). SG is a
FONDECYT post-doctoral fellow, funded by grant # 3150428. VMK receives
support from an NSERC Discovery Grant and Accelerator Supplement, from
the Centre de Recherche en Astrophysique du Quebec, an R. Howard Webster
Foundation Fellowship from the Canadian Institute for Advanced Study,
the Canada Research Chairs Program and the Lorne Trottier Chair in
Astrophysics and Cosmology. Parts of this research were conducted by the
Australian Research Council Centre of Excellence for All-sky
Astrophysics (CAASTRO), through project number CE110001020.
NR 52
TC 0
Z9 0
U1 2
U2 2
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD DEC
PY 2016
VL 463
IS 3
BP 2612
EP 2622
DI 10.1093/mnras/stw2194
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EJ9SC
UT WOS:000393566000026
ER
EF