FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Colliander, A
Mckague, D
AF Colliander, Andreas
Mckague, Darren
TI The Microwave Radiometer Working Group
SO IEEE GEOSCIENCE AND REMOTE SENSING MAGAZINE
LA English
DT Article
C1 [Colliander, Andreas] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Mckague, Darren] Univ Michigan, Ann Arbor, MI 48109 USA.
RP Colliander, A (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
NR 10
TC 0
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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 2168-6831
J9 IEEE GEOSC REM SEN M
JI IEEE Geosci. Remote Sens. Mag.
PD SEP
PY 2016
VL 4
IS 3
SI SI
BP 69
EP 72
DI 10.1109/MGRS.2016.2588442
PG 4
WC Geochemistry & Geophysics; Remote Sensing; Imaging Science &
Photographic Technology
SC Geochemistry & Geophysics; Remote Sensing; Imaging Science &
Photographic Technology
GA EF0HY
UT WOS:000390007700009
ER
PT J
AU Eingorn, M
Kiefer, C
Zhuk, A
AF Eingorn, Maxim
Kiefer, Claus
Zhuk, Alexander
TI Scalar and vector perturbations in a universe with discrete and
continuous matter sources
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE cosmological perturbation theory; dark energy theory; gravity
ID COSMOLOGICAL PERTURBATIONS; DARK-MATTER; NETWORKS; ENERGY
AB We study a universe filled with dust-like matter in the form of discrete inhomogeneities (e.g., galaxies and their groups and clusters) and two sets of perfect fluids with linear and nonlinear equations of state, respectively. The background spacetime geometry is defined by the FLRW metric. In the weak gravitational field limit, we develop the first-order scalar and vector cosmological perturbation theory. Our approach works at all cosmological scales (i.e. sub-horizon and super-horizon ones) and incorporates linear and nonlinear effects with respect to energy density fluctuations. We demonstrate that the scalar perturbation (i.e. the gravitational potential) as well as the vector perturbation can be split into individual contributions from each matter source. Each of these contributions satisfies its own equation. The velocity-independent parts of the individual gravitational potentials are characterized by a finite time-dependent Yukawa interaction range being the same for each individual contribution. We also obtain the exact form of the gravitational potential and vector perturbation related to the discrete matter sources. The self-consistency of our approach is thoroughly checked. The derived equations can form the theoretical basis for numerical simulations for a wide class of cosmological models.
C1 [Eingorn, Maxim] North Carolina Cent Univ, CREST, Fayetteville St 1801, Durham, NC 27707 USA.
[Eingorn, Maxim] NASA, Res Ctr, Fayetteville St 1801, Durham, NC 27707 USA.
[Eingorn, Maxim; Kiefer, Claus] Univ Cologne, Inst Theoret Phys, Zulpicher Str 77, D-50937 Cologne, Germany.
[Zhuk, Alexander] Odessa Natl Univ, Astron Observ, Dvoryanskaya St 2, UA-65082 Odessa, Ukraine.
RP Eingorn, M (reprint author), North Carolina Cent Univ, CREST, Fayetteville St 1801, Durham, NC 27707 USA.; Eingorn, M (reprint author), NASA, Res Ctr, Fayetteville St 1801, Durham, NC 27707 USA.; Eingorn, M (reprint author), Univ Cologne, Inst Theoret Phys, Zulpicher Str 77, D-50937 Cologne, Germany.
EM maxim.eingorn@gmail.com; kiefer@thp.uni-koeln.de; ai.zhuk2@gmail.com
FU Albert's Researcher Reunion Grant of the University of Cologne
FX The work of M. Eingorn was partially supported by an Albert's Researcher
Reunion Grant of the University of Cologne.
NR 39
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Z9 0
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1475-7516
J9 J COSMOL ASTROPART P
JI J. Cosmol. Astropart. Phys.
PD SEP
PY 2016
IS 9
AR 032
DI 10.1088/1475-7516/2016/09/032
PG 19
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA EE7CM
UT WOS:000389772300017
ER
PT J
AU Eliasson, B
Speirs, DC
Daldorff, LKS
AF Eliasson, B.
Speirs, D. C.
Daldorff, L. K. S.
TI Electrostatic electron cyclotron instabilities near the upper hybrid
layer due to electron ring distributions
SO PLASMA PHYSICS AND CONTROLLED FUSION
LA English
DT Article
DE electron cyclotron instability; electron Bernstein waves; ring
distribution
ID STIMULATED ELECTROMAGNETIC EMISSION; BROAD UPSHIFTED MAXIMUM;
MAGNETIC-FIELD; PLASMA-WAVES; BERNSTEIN MODES; SIMULATION; SPACE;
HARMONICS; RADIATION; DISCHARGE
AB A theoretical study is presented of the electrostatic electron cyclotron instability involving Bernstein modes in a magnetized plasma. The presence of a tenuous thermal ring distribution in a Maxwellian plasma decreases the frequency of the upper hybrid branch of the electron Bernstein mode until it merges with the nearest lower branch with a resulting instability. The instability occurs when the upper hybrid frequency is somewhat above the third, fourth, and higher electron cyclotron harmonics, and gives rise to a narrow spectrum of waves around the electron cyclotron harmonic nearest to the upper hybrid frequency. For a tenuous cold ring distribution together with a Maxwellian distribution an instability can take place also near the second electron cyclotron harmonic. Noise-free Vlasov simulations are used to assess the theoretical linear growth-rates and frequency spectra, and to study the nonlinear evolution of the instability. The relevance of the results to laboratory and ionospheric heating experiments is discussed.
C1 [Eliasson, B.; Speirs, D. C.] Univ Strathclyde, Dept Phys, SUPA, John Anderson Bldg, Glasgow G4 0NG, Lanark, Scotland.
[Daldorff, L. K. S.] Catholic Univ Amer, 620 Michigan Ave NE, Washington, DC 20064 USA.
[Daldorff, L. K. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Eliasson, B (reprint author), Univ Strathclyde, Dept Phys, SUPA, John Anderson Bldg, Glasgow G4 0NG, Lanark, Scotland.
EM bengt.eliasson@strath.ac.uk
FU Engineering and Physical Sciences Research Council (EPSRC), U.K.
[EP/M009386/1]
FX Discussions with Thomas Leyser at the Swedish Institute of Space Physics
are gratefully acknowledged. This work was supported by the Engineering
and Physical Sciences Research Council (EPSRC), U.K., Grant no.
EP/M009386/1. Simulation data supporting the figures are available at
http://dx.doi.org/10.15129/56448d9e-adb0-4d2b-afdb-029165a40f54.
NR 50
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U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0741-3335
EI 1361-6587
J9 PLASMA PHYS CONTR F
JI Plasma Phys. Control. Fusion
PD SEP
PY 2016
VL 58
IS 9
AR 095002
DI 10.1088/0741-3335/58/9/095002
PG 10
WC Physics, Fluids & Plasmas
SC Physics
GA EE2TI
UT WOS:000389437000002
ER
PT J
AU Bartholomaus, TC
Stearns, LA
Sutherland, DA
Shroyer, EL
Nash, JD
Walker, RT
Catania, G
Felikson, D
Carroll, D
Fried, MJ
Noel, BPY
Van Den Broeke, MR
AF Bartholomaus, Timothy C.
Stearns, Leigh A.
Sutherland, David A.
Shroyer, Emily L.
Nash, Jonathan D.
Walker, Ryan T.
Catania, Ginny
Felikson, Denis
Carroll, Dustin
Fried, Mason J.
Noel, Brice P. Y.
Van Den Broeke, Michiel R.
TI Contrasts in the response of adjacent fjords and glaciers to ice-sheet
surface melt in West Greenland
SO ANNALS OF GLACIOLOGY
LA English
DT Article
DE atmosphere/ice/ocean interactions; ice velocity; ice/ocean interactions;
iceberg calving; subglacial processes
ID SIGNIFICANT SUBMARINE MELT; JAKOBSHAVN ISBRAE; OUTLET GLACIERS; OCEAN
WATERS; SOUTHEAST GREENLAND; TIDEWATER GLACIER; HELHEIM GLACIER;
MASS-BALANCE; DYNAMICS; TERMINUS
AB Neighboring tidewater glaciers often exhibit asynchronous dynamic behavior, despite relatively uniform regional atmospheric and oceanic forcings. This variability may be controlled by a combination of local factors, including glacier and fjord geometry, fjord heat content and circulation, and glacier surface melt. In order to characterize and understand contrasts in adjacent tidewater glacier and fjord dynamics, we made coincident ice-ocean-atmosphere observations at high temporal resolution (minutes to weeks) within a 10 000 km(2) area near Uummannaq, Greenland. Water column velocity, temperature and salinity measurements reveal systematic differences in neighboring fjords that imply contrasting circulation patterns. The observed ocean velocity and hydrography, combined with numerical modeling, suggest that subglacial discharge plays a major role in setting fjord conditions. In addition, satellite remote sensing of seasonal ice flow speed and terminus position reveal both speedup and slow-down in response to melt, as well as differences in calving style among the neighboring glaciers. Glacier force budgets and modeling also point toward subglacial discharge as a key factor in glacier behavior. For the studied region, individual glacier and fjord geometry modulate subglacial discharge, which leads to contrasts in both fjord and glacier dynamics.
C1 [Bartholomaus, Timothy C.; Catania, Ginny; Felikson, Denis; Fried, Mason J.] Univ Texas Austin, Inst Geophys, Austin, TX 78712 USA.
[Stearns, Leigh A.] Univ Kansas, Lawrence, KS 66045 USA.
[Sutherland, David A.; Carroll, Dustin] Univ Oregon, Eugene, OR 97403 USA.
[Shroyer, Emily L.; Nash, Jonathan D.] Oregon State Univ, Corvallis, OR 97331 USA.
[Walker, Ryan T.] Univ Maryland, Greenbelt, MD USA.
[Walker, Ryan T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Noel, Brice P. Y.; Van Den Broeke, Michiel R.] Univ Utrecht, Inst Marine & Atmospher Res Utrecht IMAU, Utrecht, Netherlands.
RP Bartholomaus, TC (reprint author), Univ Texas Austin, Inst Geophys, Austin, TX 78712 USA.
EM tbartholomaus@ig.utexas.edu
RI Van den Broeke, Michiel/F-7867-2011; Catania, Ginny/B-9787-2008;
OI Van den Broeke, Michiel/0000-0003-4662-7565; Bartholomaus,
Timothy/0000-0002-1470-6720; Felikson, Denis/0000-0002-3785-5112
FU National Aeronautics and Space Administration [NNX12AP50G]; University
of Texas Institute for Geophysics; Polar Program of the Netherlands
Organization for Scientific Research (NOW/ALW)
FX This work was partially supported by the National Aeronautics and Space
Administration through grant NNX12AP50G. T.C.B. was supported by a
postdoctoral fellowship from the University of Texas Institute for
Geophysics. We acknowledge field support from CH2MHill Polar Services
and the captain and crew of the R/V Sanna. We thank Ian Joughin for
deriving glacier velocities from TerraSAR-X scenes within our area and
the Polar Geospatial Center for providing World View imagery. B.N. and
M.vdB. acknowledge support of the Polar Program of the Netherlands
Organization for Scientific Research (NOW/ALW). The constructive
critiques of two anonymous reviewers significantly improved the quality
and clarity of this publication.
NR 75
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U2 8
PU CAMBRIDGE UNIV PRESS
PI CAMBRIDGE
PA EDINBURGH BLDG, SHAFTESBURY RD, CB2 8RU CAMBRIDGE, ENGLAND
SN 0260-3055
EI 1727-5644
J9 ANN GLACIOL
JI Ann. Glaciol.
PD SEP
PY 2016
VL 57
IS 73
BP 25
EP 38
DI 10.1017/aog.2016.19
PG 14
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA ED6GJ
UT WOS:000388953800005
ER
PT J
AU Shuman, C
Scambos, T
Berthier, E
AF Shuman, Christopher
Scambos, Ted
Berthier, Etienne
TI Ice loss processes in the Seal Nunataks ice shelf region from satellite
altimetry and imagery
SO ANNALS OF GLACIOLOGY
LA English
DT Article
DE Antarctic glaciology; ice shelves; remote sensing
ID ANTARCTIC PENINSULA; MASS-BALANCE; LARSEN; SHEET; ELEVATION; GLACIERS;
DISINTEGRATION; RESOLUTION; DISCHARGE; TRIBUTARY
AB The Seal Nunataks ice shelf (SNIS, similar to 743 km(2) in 2013) is an unofficial name for a remnant area between the former Larsen A and Larsen B ice shelves off the northeastern Antarctic Peninsula. Analyses using Landsat 7 ETM+ and Terra ASTER images from 2001 to 13 and ICESat altimetry from 2003 to 09 show it has retreated and thinned following the Larsen A (1995) and Larsen B (2002) disintegrations. Despite some regional cooling and more fast ice since 2008, SNIS continues to lose ice along its margins and may be losing contact with some nunataks. Detailed analysis of data from four ICESat tracks indicates that ice shelf thinning rates range between 1.9 and 2.7 m a(-1), and generally increase from west to east. An ICESat repeat track crossing the adjacent Robertson Island shows a mean elevation loss of 1.8 m a(-1). Two tracks crossing the SNIS's remaining tributary, Rogosh Glacier, show sub-meter elevation losses. Comparing shelf remnant and grounded ice thinning rates implies that basal ocean melting augments SNIS thinning by similar to 1 m a(-1), a rate that is consistent with other estimates of ocean-driven shelf thinning in the region.
C1 [Shuman, Christopher] NASA, Goddard Space Flight Ctr, UMBC, JCET, Greenbelt, MD USA.
[Scambos, Ted] Univ Colorado Boulder, CIRES, NSIDC, Boulder, CO USA.
[Berthier, Etienne] Univ Toulouse, UPS, CNRS, CNES,IRD,LEGOS, Toulouse, France.
RP Shuman, C (reprint author), NASA, Goddard Space Flight Ctr, UMBC, JCET, Greenbelt, MD USA.
EM Christopher.A.Shuman@nasa.gov
RI Berthier, Etienne/B-8900-2009
OI Berthier, Etienne/0000-0001-5978-9155
FU NSF [NSF ANT-0732921]; NASA [NASA NNX10AR76G]; TOSCA program of the
French Space Agency (CNES); ISIS program of the French Space Agency
(CNES); NASA
FX The authors would like to acknowledge the support of H. Pritchard for
additional insights on a previously published analysis for the area
(Pritchard and others, 2012). The authors would also like to thank J.
Bohlander, K. Melocik, V. Suchdeo, and P. Vornberger for help with
aspects of the imagery analysis. This project also benefitted from the
help of M. Siegfried and L. Padman regarding the best available ocean
tide model for the ICESat data. The ICESat data for this paper are
available at the NASA Distributed Active Archive Center at the National
Snow and Ice Data Center (GLA12 - GLAS/ICESat L2 Antarctic and Greenland
Ice Sheet Altimetry Data). The Landsat data were acquired at no cost via
the Earth Explorer website from the US Geological Survey's Earth
Resource Observation and Science Center (EROS), home of the national
archive for Landsat imagery. The ASTER data were provided at no cost
through the Global Land Ice Measurements from Space (GLIMS) project.
This work was supported by NSF and NASA grants to T. Scambos (NSF
ANT-0732921; NASA NNX10AR76G), the TOSCA and ISIS programs of the French
Space Agency (CNES) to E. Berthier, and NASA Cryospheric Sciences
Program funds to C. Shuman. The final paper benefitted from the many
helpful comments provided by two anonymous reviewers.
NR 50
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PU CAMBRIDGE UNIV PRESS
PI CAMBRIDGE
PA EDINBURGH BLDG, SHAFTESBURY RD, CB2 8RU CAMBRIDGE, ENGLAND
SN 0260-3055
EI 1727-5644
J9 ANN GLACIOL
JI Ann. Glaciol.
PD SEP
PY 2016
VL 57
IS 73
BP 94
EP 104
DI 10.1017/aog.2016.29
PG 11
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA ED6GJ
UT WOS:000388953800012
ER
PT J
AU Geller, MA
Zhou, TH
Shindell, D
Ruedy, R
Aleinov, I
Nazarenko, L
Tausnev, NL
Kelley, M
Sun, S
Cheng, Y
Field, RD
Faluvegi, G
AF Geller, Marvin A.
Zhou, Tiehan
Shindell, D.
Ruedy, R.
Aleinov, I.
Nazarenko, L.
Tausnev, N. L.
Kelley, M.
Sun, S.
Cheng, Y.
Field, R. D.
Faluvegi, G.
TI Modeling the QBO-Improvements resulting from higher-model vertical
resolution
SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS
LA English
DT Article
DE modeling the QBO; fine vertical resolution; other model improvements
ID QUASI-BIENNIAL OSCILLATION; STRATOSPHERIC WATER-VAPOR; TROPICAL
TROPOPAUSE; GENERAL-CIRCULATION; ATMOSPHERE MODEL; GLOBAL CLIMATE;
GRAVITY-WAVES; TRANSPORT; SIMULATION; CHEMISTRY
AB Using the NASA Goddard Institute for Space Studies (GISS) climate model, it is shown that with proper choice of the gravity wave momentum flux entering the stratosphere and relatively fine vertical layering of at least 500 m in the upper troposphere-lower stratosphere (UTLS), a realistic stratospheric quasi-biennial oscillation (QBO) is modeled with the proper period, amplitude, and structure down to tropopause levels. It is furthermore shown that the specified gravity wave momentum flux controls the QBO period whereas the width of the gravity wave momentum flux phase speed spectrum controls the QBO amplitude. Fine vertical layering is required for the proper downward extension to tropopause levels as this permits wave-mean flow interactions in the UTLS region to be resolved in the model. When vertical resolution is increased from 1000 to 500 m, the modeled QBO modulation of the tropical tropopause temperatures increasingly approach that from observations, and the tape recorder of stratospheric water vapor also approaches the observed. The transport characteristics of our GISS models are assessed using age-of-air and N2O diagnostics, and it is shown that some of the deficiencies in model transport that have been noted in previous GISS models are greatly improved for all of our tested model vertical resolutions. More realistic tropical-extratropical transport isolation, commonly referred to as the tropical pipe, results from the finer vertical model layering required to generate a realistic QBO.
C1 [Geller, Marvin A.] SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA.
[Zhou, Tiehan; Ruedy, R.; Aleinov, I.; Nazarenko, L.; Tausnev, N. L.; Kelley, M.; Cheng, Y.; Field, R. D.; Faluvegi, G.] NASA Goddard Inst Space Studies, New York, NY USA.
[Zhou, Tiehan; Aleinov, I.; Nazarenko, L.; Cheng, Y.; Faluvegi, G.] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
[Shindell, D.] Duke Univ, Nicholas Sch Environm, Earth & Ocean Sci, Durham, NC 27708 USA.
[Ruedy, R.; Tausnev, N. L.; Kelley, M.] Trinnovim LLC, New York, NY USA.
[Sun, S.] NOAA Earth Syst Res Lab, Boulder, CO USA.
[Field, R. D.] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA.
RP Geller, MA (reprint author), SUNY Stony Brook, Sch Marine & Atmospher Sci, Stony Brook, NY 11794 USA.
EM marvin.geller@stonybrook.edu
FU NASA Modeling, Analysis and Prediction Program; NASA High-End Computing
(HEC) Program through NASA Center for Climate Simulation (NCCS) at
Goddard Space Flight Center
FX This work was supported by the NASA Modeling, Analysis and Prediction
Program and the NASA High-End Computing (HEC) Program through the NASA
Center for Climate Simulation (NCCS) at Goddard Space Flight Center.
Data from these runs are available from Tiehan Zhou
(tz2131@columbia.edu). We thank Jae N. Lee for kindly providing the AURA
MLS water vapor data. The authors acknowledge the two anonymous
reviewers for their helpful comments, which led to an improved paper.
NR 49
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1942-2466
J9 J ADV MODEL EARTH SY
JI J. Adv. Model. Earth Syst.
PD SEP
PY 2016
VL 8
IS 3
BP 1092
EP 1105
DI 10.1002/2016MS000699
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EC0LV
UT WOS:000387793500004
PM 27917258
ER
PT J
AU Pithan, F
Ackerman, A
Angevine, WM
Hartung, K
Ickes, L
Kelley, M
Medeiros, B
Sandu, I
Steeneveld, GJ
Sterk, HAM
Svensson, G
Vaillancourt, PA
Zadra, A
AF Pithan, Felix
Ackerman, Andrew
Angevine, Wayne M.
Hartung, Kerstin
Ickes, Luisa
Kelley, Maxwell
Medeiros, Brian
Sandu, Irina
Steeneveld, Gert-Jan
Sterk, H. A. M.
Svensson, Gunilla
Vaillancourt, Paul A.
Zadra, Ayrton
TI Select strengths and biases of models in representing the Arctic winter
boundary layer over sea ice: the Larcform 1 single column model
intercomparison
SO JOURNAL OF ADVANCES IN MODELING EARTH SYSTEMS
LA English
DT Article
DE Arctic; boundary-layer; mixed-phase clouds; models; intercomparison;
inversion
ID LARGE-EDDY SIMULATIONS; CLIMATE MODELS; CLOUDS; PARAMETERIZATION;
PRECIPITATION; INVERSIONS; RADIATION; SYSTEM; SHEBA
AB Weather and climate models struggle to represent lower tropospheric temperature and moisture profiles and surface fluxes in Arctic winter, partly because they lack or misrepresent physical processes that are specific to high latitudes. Observations have revealed two preferred states of the Arctic winter boundary layer. In the cloudy state, cloud liquid water limits surface radiative cooling, and temperature inversions are weak and elevated. In the radiatively clear state, strong surface radiative cooling leads to the build-up of surface-based temperature inversions. Many large-scale models lack the cloudy state, and some substantially underestimate inversion strength in the clear state. Here, the transformation from a moist to a cold dry air mass is modeled using an idealized Lagrangian perspective. The trajectory includes both boundary layer states, and the single-column experiment is the first Lagrangian Arctic air formation experiment (Larcform 1) organized within GEWEX GASS (Global atmospheric system studies). The intercomparison reproduces the typical biases of large-scale models: some models lack the cloudy state of the boundary layer due to the representation of mixed-phase microphysics or to the interaction between micro- and macrophysics. In some models, high emissivities of ice clouds or the lack of an insulating snow layer prevent the build-up of surface-based inversions in the radiatively clear state. Models substantially disagree on the amount of cloud liquid water in the cloudy state and on turbulent heat fluxes under clear skies. Observations of air mass transformations including both boundary layer states would allow for a tighter constraint of model behavior.
C1 [Pithan, Felix] Univ Reading, Dept Meteorol, Reading, Berks, England.
[Ackerman, Andrew; Kelley, Maxwell] NASA Goddard Inst Space Studies, New York, NY USA.
[Angevine, Wayne M.] Univ Colorado, CIRES, Boulder, CO 80309 USA.
[Angevine, Wayne M.] NOAA Earth Syst Res Lab, Boulder, CO USA.
[Hartung, Kerstin; Svensson, Gunilla] Stockholm Univ, Dept Meteorol, Stockholm, Sweden.
[Ickes, Luisa] ETHZ, Inst Atmosphere & Climate, Zurich, Switzerland.
[Medeiros, Brian] NCAR, Boulder, CO USA.
[Sandu, Irina] ECMWF, Reading, Berks, England.
[Steeneveld, Gert-Jan; Sterk, H. A. M.] Wageningen Univ, Meteorol & Air Qual Sect, Wageningen, Netherlands.
[Vaillancourt, Paul A.; Zadra, Ayrton] Environm Canada, Rech Previs Numer Atmospher, Dorval, PQ, Canada.
RP Pithan, F (reprint author), Univ Reading, Dept Meteorol, Reading, Berks, England.
EM felix.pithan@awi.de
RI Steeneveld, Gert-Jan/B-2816-2010; Manager, CSD Publications/B-2789-2015
OI Steeneveld, Gert-Jan/0000-0002-5922-8179;
FU GASS (Global atmospheric system studies) steering group; ERC under
Marie-Curie grant UACSURF [GAP-654492]; NASA MAP program; NWO
[863.10.010, 829.09.005]; Regional and Global Climate Modeling Program
of the U.S. Department of Energy's Office of Science
[DE-FC02-97ER62402]; National Science Foundation; Swedish e-Science
Research Centre SeRC
FX We gratefully acknowledge support from the GASS (Global atmospheric
system studies) steering group. We thank the researchers involved in the
collection of SHEBA and ARM data for making their data sets available,
and the modeling groups, the Program for Climate Model Diagnosis and
Intercomparison and the World Climate Research Program's Working Group
on Coupled Modeling for making available the CMIP5 multimodel data set.
F.P. was funded by the ERC under Marie-Curie grant UACSURF (GAP-654492)
for parts of this study. AA and MK were funded by the NASA MAP program.
GJS acknowledges funding from NWO contract 863.10.010. M.S. acknowledges
the support from NWO (The Dutch Science Foundation) with grant
829.09.005 ("Quantifying contributions of surface climate feedbacks to
the Arctic amplification of greenhouse warming'' in the Sustainable
Earth program). B.M. was supported by the Regional and Global Climate
Modeling Program of the U.S. Department of Energy's Office of Science,
Cooperative Agreement DE-FC02-97ER62402. NCAR is sponsored by the
National Science Foundation. K.H. was supported by the Swedish e-Science
Research Centre SeRC. Thanks to Bert Holtslag for comments on an earlier
version of this manuscript, and to Thorsten Mauritsen for advice and
support in the development of the case. We gratefully acknowledge the
input and advice of two anonymous reviewers. Model results are available
at https://doi.org/10.1594/PANGAEA.856770.
NR 50
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PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1942-2466
J9 J ADV MODEL EARTH SY
JI J. Adv. Model. Earth Syst.
PD SEP
PY 2016
VL 8
IS 3
BP 1345
EP 1357
DI 10.1002/2016MS000630
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA EC0LV
UT WOS:000387793500017
ER
PT J
AU Hudson, J
Spangelo, S
Hine, A
Kolosa, D
Lemmer, K
AF Hudson, Jennifer
Spangelo, Sara
Hine, Andrew
Kolosa, Daniel
Lemmer, Kristina
TI Mission Analysis for CubeSats with Micropropulsion
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID ORBIT TRANSFERS; PROPULSION; THRUSTER
AB The orbital maneuver capabilities of several CubeSat propulsion systems are analyzed using trajectory simulations. Properties of several types of developmental micropropulsion systems are reviewed, and Delta V capabilities are compared. Mission simulations are used to analyze the relationship between thrust arc length and orbit change capability in a low-thrust spiral trajectory. Constraints on power, fuel mass, and mission duration, as well as system-level constraints, are considered. Feasible CubeSat architectures and mission designs are developed for three electric propulsion systems. The most effective combinations of thruster operational modes and trajectory control strategies are discussed.
C1 [Hudson, Jennifer; Hine, Andrew; Kolosa, Daniel; Lemmer, Kristina] Western Michigan Univ, Dept Mech & Aerosp Engn, 1903 West Michigan Ave,Mail Stop 5343, Kalamazoo, MI 49008 USA.
[Spangelo, Sara] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Hudson, J (reprint author), Western Michigan Univ, Dept Mech & Aerosp Engn, 1903 West Michigan Ave,Mail Stop 5343, Kalamazoo, MI 49008 USA.
FU NASA [NNX13AR18A]
FX The authors acknowledge support from NASA cooperative agreement
NNX13AR18A.
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U1 2
U2 2
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 SEP
PY 2016
VL 53
IS 5
BP 836
EP 846
DI 10.2514/1.A33564
PG 11
WC Engineering, Aerospace
SC Engineering
GA ED1FY
UT WOS:000388591400006
ER
PT J
AU Blandino, JJ
Martinez-Baquero, N
Demetriou, MA
Gatsonis, NA
Paschalidis, N
AF Blandino, John J.
Martinez-Baquero, Nicolas
Demetriou, Michael A.
Gatsonis, Nikolaos A.
Paschalidis, Nicholas
TI Feasibility for Orbital Life Extension of a CubeSat in the Lower
Thermosphere
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article; Proceedings Paper
CT 54th AIAA Aerospace Sciences Meeting / AIAA Science and Technology Forum
and Exposition
CY JAN 04-08, 2016
CL San Diego, CA
SP AIAA
ID ATMOSPHERE; SATELLITE; THRUSTER; MISSION
AB Orbital flight of CubeSats at altitudes between 150 and 250 km has the potential to enable a new class of scientific, commercial, and defense-related missions. A study is presented to demonstrate the feasibility of extending the orbital lifetime of a CubeSat in a 210 km orbit. Propulsion consists of an electrospray thruster operating at a 2 W, 0.175 mN thrust, and an specific impulse (Isp) of 500 s. The mission consists of two phases. In phase 1, the CubeSat is deployed from a 414 km orbit and uses the thruster to deorbit to the target altitude of 210 km. In phase 2, the propulsion system is used to extend the mission lifetime until propellant is fully expended. A control algorithm based on maintaining a target orbital energy is presented that uses an extended Kalman filter to generate estimates of the orbital dynamic state, which are periodically updated by Global Positioning System measurements. For phase 1, the spacecraft requires 25.21 days to descend from 414 to 210 km, corresponding to a Delta V = 96.25 m/s and a propellant consumption of 77.8 g. Phase 2 lasts 57.83 days, corresponding to a Delta V = 119.15 m/s, during which the remaining 94.2 g of propellant are consumed.
C1 [Blandino, John J.; Martinez-Baquero, Nicolas; Demetriou, Michael A.; Gatsonis, Nikolaos A.] Worcester Polytech Inst, Aerosp Engn Program, 100 Inst Rd, Worcester, MA 01609 USA.
[Paschalidis, Nicholas] NASA, Goddard Space Flight Ctr, Technol, Greenbelt, MD 20771 USA.
RP Blandino, JJ (reprint author), Worcester Polytech Inst, Aerosp Engn Program, 100 Inst Rd, Worcester, MA 01609 USA.
NR 29
TC 0
Z9 0
U1 2
U2 2
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 SEP
PY 2016
VL 53
IS 5
BP 864
EP 875
DI 10.2514/1.A33462
PG 12
WC Engineering, Aerospace
SC Engineering
GA ED1FY
UT WOS:000388591400008
ER
PT J
AU Shapiro, AA
Borgonia, JP
Chen, QN
Dillon, RP
McEnerney, B
Polit-Casillas, R
Soloway, L
AF Shapiro, A. A.
Borgonia, J. P.
Chen, Q. N.
Dillon, R. P.
McEnerney, B.
Polit-Casillas, R.
Soloway, L.
TI Additive Manufacturing for Aerospace Flight Applications
SO JOURNAL OF SPACECRAFT AND ROCKETS
LA English
DT Article
ID INCONEL 718; LASER; STEEL; DEPOSITION; CERAMICS; PARTS; MICROSTRUCTURE;
OPTIMIZATION; ELECTRONICS; FABRICATION
AB Additive manufacturing can provide many advantages to the future of space flight. Although it has been in use for plastic prototyping applications, it is only more recently that additive technologies have been investigated to produce metal and ceramic flight parts. This review paper presents some of the specific issues that arise for space flight applications, including materials selection, processing and postprocessing parameters, and the qualification process. With these concerns in mind, there are seven main applications in which additive manufacturing can provide a benefit. These applications include innovative design strategies that use the unique parameters of additive manufacturing, as well as some specific uses such as mass reduction or in situ production in space.
C1 [Shapiro, A. A.] CALTECH, Jet Prop Lab, Space Technol Program Off, 4800 Oak Grove Dr,M-S 180-701, Pasadena, CA 91109 USA.
[Borgonia, J. P.; Dillon, R. P.] CALTECH, Jet Prop Lab, Mech Syst Engn Fabricat & Test, 4800 Oak Grove Dr,M-S 170-104, Pasadena, CA 91109 USA.
[Chen, Q. N.] CALTECH, Jet Prop Lab, Mech Syst Engn Fabricat & Test, 4800 Oak Grove Dr,M-S 158-103, Pasadena, CA 91109 USA.
[McEnerney, B.] CALTECH, Jet Prop Lab, Mech Syst Engn Fabricat & Test, 4800 Oak Grove Dr,M-S 125-109, Pasadena, CA 91109 USA.
[Polit-Casillas, R.] CALTECH, Jet Prop Lab, Mech Syst Engn Fabricat & Test, 4800 Oak Grove Dr,M-S 154-410, Pasadena, CA 91109 USA.
[Soloway, L.] CALTECH, Jet Prop Lab, Engn & Sci Directorate, 4800 Oak Grove Dr,M-S 180-502, Pasadena, CA 91109 USA.
RP Shapiro, AA (reprint author), CALTECH, Jet Prop Lab, Space Technol Program Off, 4800 Oak Grove Dr,M-S 180-701, Pasadena, CA 91109 USA.
NR 43
TC 0
Z9 0
U1 20
U2 20
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 SEP
PY 2016
VL 53
IS 5
BP 952
EP 959
DI 10.2514/1.A33544
PG 8
WC Engineering, Aerospace
SC Engineering
GA ED1FY
UT WOS:000388591400015
ER
PT J
AU Jacobson, AR
Holzworth, RH
Pfaff, R
Heelis, R
AF Jacobson, Abram R.
Holzworth, Robert H.
Pfaff, Robert
Heelis, Roderick
TI Automated identification of discrete, lightning-generated,
multiple-dispersed whistler waves in C/NOFS-VEFI very low frequency
observations
SO RADIO SCIENCE
LA English
DT Article
ID LOW-LATITUDE IONOSPHERE; RADIATION BELT; TEMPORAL SIGNATURES; TWEEK
ATMOSPHERICS; LOCATION NETWORK; PLASMASPHERE; PROPAGATION; ORIGIN; GUIDE
AB Automated wave feature detection is required to efficiently analyze large archives of very low frequency broadband recordings for discrete whistler identification and feature extraction. We describe a new method to do this, even in the presence of simultaneous, multiple whistler phase dispersions. Previous techniques of whistler identification were unable to deal with simultaneous, multiple phase dispersions. We demonstrate the new method with data from the Vector Electric Field Investigation (VEFI) payload on the Communication/Navigation Outage Forecast System (C/NOFS) satellite, from the mission years 2008-2014.
C1 [Jacobson, Abram R.; Holzworth, Robert H.] Univ Washington, Earth & Space Sci Dept, Seattle, WA 98195 USA.
[Pfaff, Robert] NASA, Goddard Spaceflight Ctr, Greenbelt, MD USA.
[Heelis, Roderick] Univ Texas Dallas, Ctr Space Sci, Richardson, TX 75083 USA.
RP Jacobson, AR (reprint author), Univ Washington, Earth & Space Sci Dept, Seattle, WA 98195 USA.
EM abramj@u.washington.edu
FU NSF [1443011]
FX This work was partially supported by NSF grant 1443011,
"Wave-vector-resolved Study of Lightning Whistler Propagation and
Energetics in the Low-latitude Plasmasphere." Readers wishing to examine
the original data are invited to contact the corresponding author.
NR 37
TC 0
Z9 0
U1 3
U2 3
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 SEP
PY 2016
VL 51
IS 9
BP 1547
EP 1569
DI 10.1002/2016RS005989
PG 23
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
GA ED6EI
UT WOS:000388947900009
ER
PT J
AU Wilson, SA
Howard, AD
Moore, JM
Grant, JA
AF Wilson, Sharon A.
Howard, Alan D.
Moore, Jeffrey M.
Grant, John A.
TI A cold-wet middle-latitude environment on Mars during the
Hesperian-Amazonian transition: Evidence from northern Arabia valleys
and paleolakes
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID GALE CRATER; TERRA-CIMMERIA; SURFACE RUNOFF; ALLUVIAL FANS; EVOLUTION;
ORIGIN; PRECIPITATION; NETWORKS; IMPACTS; SYSTEMS
AB The growing inventory of post-Noachian fluvial valleys may represent a late, widespread episode of aqueous activity on Mars, contrary to the paradigm that fluvial activity largely ceased around the Noachian-Hesperian boundary. Fresh shallow valleys (FSVs) are widespread from similar to 30 to 45 degrees in both hemispheres with a high concentration in northern Arabia Terra. Valleys in northern Arabia Terra characteristically start abruptly on steeper slopes and terminate in topographic depressions at elevations corresponding to model-predicted lake levels. Longer valley systems flowed into and out of chains of paleolakes. Minimum discharges based on the dimensions of the incised channel assuming medium to coarse sand-size grains ranges from tens to hundreds of m(3) s(-1), respectively, consistent with formation via snowmelt from surface or sub-ice flows. Hydrologic calculations indicate the valleys likely formed in hundreds of years or less, and crater statistics constrain the timing of fluvial activity to between the Hesperian and middle Amazonian. Several craters with channels extending radially outward supports evidence for overflow of interior crater lakes possibly fed by groundwater. Most FSVs occur away from young impact craters which make an association with impact processes improbable. The widespread occurrence of FSVs along with their similar morphology and shared modest state of degradation is consistent with most forming during a global interval of favorable climate, perhaps contemporaneous with alluvial fan formation in equatorial and midlatitudes. Evidence for a snowmelt-based hydrology and considerable depths of water on the landscape in Arabia supports a cold, wet, and possibly habitable environment late in Martian history.
C1 [Wilson, Sharon A.; Grant, John A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
[Wilson, Sharon A.; Howard, Alan D.] Univ Virginia, Dept Environm Sci, Clark Hall, Charlottesville, VA 22903 USA.
[Moore, Jeffrey M.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
RP Wilson, SA (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.; Wilson, SA (reprint author), Univ Virginia, Dept Environm Sci, Clark Hall, Charlottesville, VA 22903 USA.
EM wilsons@si.edu
FU NASA [12-MDAP12-0033]
FX Thanks to Cathy Quantin-Nataf and Nick Warner for their insightful
reviews and to Caleb Fassett for his Associate Editor evaluation. This
work was supported by a NASA grant 12-MDAP12-0033 from the Mars Data
Analysis Program. The data used are listed in the figures, tables,
supplemental material, and or repository at
http://airandspace.si.edu/CEPSData.
NR 82
TC 1
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U1 4
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD SEP
PY 2016
VL 121
IS 9
BP 1667
EP 1694
DI 10.1002/2016JE005052
PG 28
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EC0MO
UT WOS:000387795400006
ER
PT J
AU Miljkovic, K
Collins, GS
Wieczorek, MA
Johnson, BC
Soderblom, JM
Neumann, GA
Zuber, MT
AF Miljkovic, K.
Collins, G. S.
Wieczorek, M. A.
Johnson, B. C.
Soderblom, J. M.
Neumann, G. A.
Zuber, M. T.
TI Subsurface morphology and scaling of lunar impact basins
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID INNER SOLAR-SYSTEM; POLE-AITKEN BASIN; HEAVY BOMBARDMENT; MASCON BASINS;
MARE BASALTS; MOON; ORIGIN; GRAVITY; GRAIL; CRUST
AB Impact bombardment during the first billion years after the formation of the Moon produced at least several tens of basins. The Gravity Recovery and Interior Laboratory (GRAIL) mission mapped the gravity field of these impact structures at significantly higher spatial resolution than previous missions, allowing for detailed subsurface and morphological analyses to be made across the entire globe. GRAIL-derived crustal thickness maps were used to define the regions of crustal thinning observed in centers of lunar impact basins, which represents a less unambiguous measure of a basin size than those based on topographic features. The formation of lunar impact basins was modeled numerically by using the iSALE-2D hydrocode, with a large range of impact and target conditions typical for the first billion years of lunar evolution. In the investigated range of impactor and target conditions, the target temperature had the dominant effect on the basin subsurface morphology. Model results were also used to update current impact scaling relationships applicable to the lunar setting (based on assumed target temperature). Our new temperature-dependent impact-scaling relationships provide estimates of impact conditions and transient crater diameters for the majority of impact basins mapped by GRAIL. As the formation of lunar impact basins is associated with the first similar to 700 Myr of the solar system evolution when the impact flux was considerably larger than the present day, our revised impact scaling relationships can aid further analyses and understanding of the extent of impact bombardment on the Moon and terrestrial planets in the early solar system.
C1 [Miljkovic, K.; Johnson, B. C.; Soderblom, J. M.; Zuber, M. T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Miljkovic, K.] Curtin Univ, Dept Appl Geol, Perth, WA, Australia.
[Collins, G. S.] Imperial Coll London, Dept Earth Sci & Engn, London, England.
[Wieczorek, M. A.] Univ Paris Diderot, Sorbonne Paris Cite, Inst Phys Globe Paris, Paris, France.
[Johnson, B. C.] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA.
[Neumann, G. A.] NASA, Solar Syst Explorat Div, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Miljkovic, K (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.; Miljkovic, K (reprint author), Curtin Univ, Dept Appl Geol, Perth, WA, Australia.
EM katarina.miljkovic@curtin.edu.au
RI Neumann, Gregory/I-5591-2013;
OI Neumann, Gregory/0000-0003-0644-9944; Soderblom,
Jason/0000-0003-3715-6407; Collins, Gareth/0000-0002-6087-6149
FU NASA; French Space Agency (CNES); STFC [ST/N000803/1]
FX The GRAIL mission is supported by the Discovery Program of NASA and is
performed under contract to the Massachusetts Institute of Technology
and the Jet Propulsion Laboratory, California Institute of Technology.
Additional support for this work was provided by the French Space Agency
(CNES). We gratefully acknowledge the developers of iSALE-2D, including
Kai Wunnemann, Dirk Elbeshausen, Boris Ivanov, and Jay Melosh. G.S.C.
was funded by STFC grant ST/N000803/1. The data used in this study are
attached as supporting information and are also available upon request
from the main author (Katarina. Miljkovic@curtin.edu.au).
NR 64
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U1 2
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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 SEP
PY 2016
VL 121
IS 9
BP 1695
EP 1712
DI 10.1002/2016JE005038
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EC0MO
UT WOS:000387795400007
ER
PT J
AU Fraeman, AA
Ehlmann, BL
Arvidson, RE
Edwards, CS
Grotzinger, JP
Milliken, RE
Quinn, DP
Rice, MS
AF Fraeman, A. A.
Ehlmann, B. L.
Arvidson, R. E.
Edwards, C. S.
Grotzinger, J. P.
Milliken, R. E.
Quinn, D. P.
Rice, M. S.
TI The stratigraphy and evolution of lower Mount Sharp from spectral,
morphological, and thermophysical orbital data sets
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID THERMAL-CONDUCTIVITY MEASUREMENTS; GALE CRATER; REFLECTANCE
SPECTROSCOPY; LANDING SITE; PARTICULATE MATERIALS; SEDIMENTARY-ROCKS;
EARLY MARS; SULFATE; MINERALOGY; CONSTRAINTS
AB We have developed a refined geologic map and stratigraphy for lower Mount Sharp using coordinated analyses of new spectral, thermophysical, and morphologic orbital data products. The Mount Sharp group consists of seven relatively planar units delineated by differences in texture, mineralogy, and thermophysical properties. These units are (1-3) three spatially adjacent units in the Murray formation which contain a variety of secondary phases and are distinguishable by thermal inertia and albedo differences, (4) a phyllosilicate-bearing unit, (5) a hematite-capped ridge unit, (6) a unit associated with material having a strongly sloped spectral signature at visible near-infrared wavelengths, and (7) a layered sulfate unit. The Siccar Point group consists of the Stimson formation and two additional units that unconformably overlie the Mount Sharp group. All Siccar Point group units are distinguished by higher thermal inertia values and record a period of substantial deposition and exhumation that followed the deposition and exhumation of the Mount Sharp group. Several spatially extensive silica deposits associated with veins and fractures show that late-stage silica enrichment within lower Mount Sharp was pervasive. At least two laterally extensive hematitic deposits are present at different stratigraphic intervals, and both are geometrically conformable with lower Mount Sharp strata. The occurrence of hematite at multiple stratigraphic horizons suggests redox interfaces were widespread in space and/or in time, and future measurements by the Mars Science Laboratory Curiosity rover will provide further insights into the depositional settings of these and other mineral phases.
C1 [Fraeman, A. A.; Ehlmann, B. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Ehlmann, B. L.; Grotzinger, J. P.; Quinn, D. P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Arvidson, R. E.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
[Edwards, C. S.] US Geol Survey, Flagstaff, AZ 86001 USA.
[Edwards, C. S.] Northern Univ Arizona, Dept Phys & Astron, Flagstaff, AZ USA.
[Milliken, R. E.] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA.
[Rice, M. S.] Western Washington Univ, Dept Phys & Astron, Dept Geol, Bellingham, WA 98225 USA.
RP Fraeman, AA (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM abigail.a.fraeman@jpl.nasa.gov
FU W.M. Keck Institution for Space Studies; Caltech; National Aeronautics
and Space Administration; National Aeronautics and Space Administration
through the internal Research and Technology Development program; MSL
Participating Scientist Program grant
FX We thank two anonymous reviewers for their careful reading and insight
comments that improved the quality of this manuscript. Thanks to Lulu
Pan for providing helpful advice on CRISM parameter mapping techniques,
Ara Oshagan for assistance in generating the HiRISE color mosaic, Dawn
Sumner for nomenclature guidance, and Kathryn Stack Morgan for fruitful
discussions about orbital mapping interpretations and sharing her
general knowledge of the Gale Crater geologic context. A.A.F. was
partially supported by a W.M. Keck Institution for Space Studies
Postdoctoral Fellowship and Caltech Geological and Planetary Sciences
Texaco Postdoctoral Fellowship. A portion of this research was also
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration and funded through the internal Research and Technology
Development program. B.L.E. was partially supported by an MSL
Participating Scientist Program grant. All raw data products supporting
the conclusions of this work can be obtained from the NASA Planetary
Data System (PDS).
NR 66
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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 SEP
PY 2016
VL 121
IS 9
BP 1713
EP 1736
DI 10.1002/2016JE005095
PG 24
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EC0MO
UT WOS:000387795400008
PM 27867788
ER
PT J
AU Blewett, DT
Stadermann, AC
Susorney, HC
Ernst, CM
Xiao, ZY
Chabot, NL
Denevi, BW
Murchie, SL
McCubbin, FM
Kinczyk, MJ
Gillis-Davis, JJ
Solomon, SC
AF Blewett, David T.
Stadermann, Amanda C.
Susorney, Hannah C.
Ernst, Carolyn M.
Xiao, Zhiyong
Chabot, Nancy L.
Denevi, Brett W.
Murchie, Scott L.
McCubbin, Francis M.
Kinczyk, Mallory J.
Gillis-Davis, Jeffrey J.
Solomon, Sean C.
TI Analysis of MESSENGER high-resolution images of Mercury's hollows and
implications for hollow formation
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID LOW-REFLECTANCE MATERIAL; DUAL IMAGING-SYSTEM; IMPACT CRATERS; SURFACE
VOLATILES; RAY SPECTROMETER; SULFUR; CARBON; MOON; EROS; STRATIGRAPHY
AB High-resolution images from MESSENGER provide morphological information on the nature and origin of Mercury's hollows, small depressions that likely formed when a volatile constituent was lost from the surface. Because graphite may be a component of the low-reflectance material that hosts hollows, we suggest that loss of carbon by ion sputtering or conversion to methane by proton irradiation could contribute to hollows formation. Measurements of widespread hollows in 565 images with pixel scales <20m indicate that the average depth of hollows is 24 +/- 16m. We propose that hollows cease to increase in depth when a volatile-depleted lag deposit becomes sufficiently thick to protect the underlying surface. The difficulty of developing a lag on steep topography may account for the common occurrence of hollows on crater central peaks and walls. Disruption of the lag, e.g., by secondary cratering, could restart growth of hollows in a location that had been dormant. Images at extremely high resolution (similar to 3 m/pixel) show that the edges of hollows are straight, as expected if the margins formed by scarp retreat. These highest-resolution images reveal no superposed impact craters, implying that hollows are very young. The width of hollows within rayed crater Balanchine suggests that the maximum time for lateral growth by 1 cm is similar to 10,000 yr. A process other than entrainment of dust by gases evolved in a steady-state sublimation-like process is likely required to explain the high-reflectance haloes that surround many hollows.
C1 [Blewett, David T.; Ernst, Carolyn M.; Chabot, Nancy L.; Denevi, Brett W.; Murchie, Scott L.; Kinczyk, Mallory J.] Johns Hopkins Univ, Appl Phys Lab, Planetary Explorat Grp, Laurel, MD 20723 USA.
[Stadermann, Amanda C.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
[Susorney, Hannah C.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[Xiao, Zhiyong] China Univ Geosci, Wuhan, Peoples R China.
[Xiao, Zhiyong] Univ Oslo, Ctr Earth Evolut & Dynam, Oslo, Norway.
[McCubbin, Francis M.] NASA, Johnson Space Ctr, Houston, TX USA.
[Gillis-Davis, Jeffrey J.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
[Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DE USA.
RP Blewett, DT (reprint author), Johns Hopkins Univ, Appl Phys Lab, Planetary Explorat Grp, Laurel, MD 20723 USA.
EM david.blewett@jhuapl.edu
RI Murchie, Scott/E-8030-2015; Denevi, Brett/I-6502-2012
OI Murchie, Scott/0000-0002-1616-8751; Denevi, Brett/0000-0001-7837-6663
FU NASA [NAS5-97271, NASW-00002]; NASA MESSENGER Participating Scientist
grant [NNX08AN29G]; NASA/APL; NASA
FX We appreciate discussions on the physics of dust lofting with David
Jewitt (University of California, Los Angeles). Helpful reviews from
Rebecca Thomas (University of Colorado), an anonymous reviewer, and
Editor David Baratoux led us to make key improvements to this paper. The
MESSENGER project is supported by the NASA Discovery Program under
contracts NAS5-97271 to The Johns Hopkins University Applied Physics
Laboratory (APL) and NASW-00002 to the Carnegie Institution of
Washington. D.T.B. is supported by NASA MESSENGER Participating
Scientist grant NNX08AN29G. A.C.S. was supported by the NASA/APL
internship program. F.M.M. acknowledges support from the NASA Solar
System Workings Program. This work made use of the Integrated Software
for Imagers and Spectrometers (ISIS), which is a product maintained by
the U.S. Geological Survey Astrogeology Science Center. MESSENGER data
are available through the NASA Planetary Data System. Supporting
information "2016JE005070-ds01.txt" gives the file names of the 882
high-resolution images that contain hollows along with latitude,
longitude, and pixel scale. Supporting information
"2016JE005070-ds02.txt" contains information for the 2518 individual
depth measurements: file name, pixel scale, depth, latitude, and
longitude.
NR 64
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 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD SEP
PY 2016
VL 121
IS 9
BP 1798
EP 1813
DI 10.1002/2016JE005070
PG 16
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EC0MO
UT WOS:000387795400013
ER
PT J
AU Trammell, HJ
Li, LM
Jiang, X
Pan, YF
Smith, MA
Bering, EA
Horst, SM
Vasavada, AR
Ingersoll, AP
Janssen, MA
West, RA
Porco, CC
Li, C
Simon, AA
Baines, KH
AF Trammell, Harold Justin
Li, Liming
Jiang, Xun
Pan, Yefeng
Smith, Mark A.
Bering, Edgar A., III
Horst, Sarah M.
Vasavada, Ashwin R.
Ingersoll, Andrew P.
Janssen, Michael A.
West, Robert A.
Porco, Carolyn C.
Li, Cheng
Simon, Amy A.
Baines, Kevin H.
TI Vortices in Saturn's Northern Hemisphere (2008-2015) observed by Cassini
ISS
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID GROUND-BASED OBSERVATIONS; POLAR SPOT; THERMAL STRUCTURE; MOIST
CONVECTION; IMAGING SCIENCE; CLOUD STRUCTURE; VOYAGER IMAGES; JUPITER;
ATMOSPHERE; DYNAMICS
AB We use observations from the Imaging Science Subsystem on Cassini to create maps of Saturn's Northern Hemisphere (NH) from 2008 to 2015, a time period including a seasonal transition (i.e., spring equinox in 2009) and the 2010 giant storm. The processed maps are used to investigate vortices in the NH during the period of 2008-2015. All recorded vortices have diameters (east-west) smaller than 6000km except for the largest vortex that developed from the 2010 giant storm. The largest vortex decreased its diameter from similar to 11,000 km in 2011 to similar to 5000 km in 2015, and its average diameter is similar to 6500 km during the period of 2011-2015. The largest vortex lasts at least 4 years, which is much longer than the lifetimes of most vortices (less than 1 year). The largest vortex drifts to north, which can be explained by the beta drift effect. The number of vortices displays varying behaviors in the meridional direction, in which the 2010 giant storm significantly affects the generation and development of vortices in the middle latitudes (25-45 degrees N). In the higher latitudes (45-90 degrees N), the number of vortices also displays strong temporal variations. The solar flux and the internal heat do not directly contribute to the vortex activities, leaving the temporal variations of vortices in the higher latitudes (45-90 degrees N) unexplained.
C1 [Trammell, Harold Justin; Jiang, Xun] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX USA.
[Li, Liming; Pan, Yefeng; Bering, Edgar A., III] Univ Houston, Dept Phys, Houston, TX 77004 USA.
[Smith, Mark A.] Univ Houston, Dept Chem, Houston, TX USA.
[Horst, Sarah M.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[Vasavada, Ashwin R.; Janssen, Michael A.; West, Robert A.; Baines, Kevin H.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Ingersoll, Andrew P.; Li, Cheng] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Porco, Carolyn C.] Univ Wisconsin, Space Sci & Engn Ctr, Madison, WI USA.
[Simon, Amy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Li, LM (reprint author), Univ Houston, Dept Phys, Houston, TX 77004 USA.
EM lli7@central.uh.eduu
RI Simon, Amy/C-8020-2012; Horst, Sarah/A-9906-2010
OI Simon, Amy/0000-0003-4641-6186; Horst, Sarah/0000-0003-4596-0702
FU NASA ROSES Cassini Data Analysis and Participating Scientists program;
NASA ROSES Planetary Data Archiving, Restoration, and Tools program
FX We gratefully acknowledge the Cassini ISS team for recording the raw
data sets. We also acknowledge the support from the NASA ROSES Cassini
Data Analysis and Participating Scientists program and Planetary Data
Archiving, Restoration, and Tools program. Finally, we thank the two
anonymous reviewers for providing their constructive suggestions to
significantly improve the manuscript. We used the new Cassini data in
2015, which are not archived in the public Planetary Data System (PDS)
(https://pds.nasa.gov) yet. The 2015 Cassini ISS raw data will be
released by the Cassini ISS team and archived in the PDS in late 2016.
We cannot archive the processed 2015 data before the release of the ISS
raw data, so we plan to archive the data of the processed NH maps in the
atmospheres node of PDS (http://atmos.pds.nasa.gov) in the beginning of
2017 or so.
NR 48
TC 0
Z9 0
U1 5
U2 5
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 SEP
PY 2016
VL 121
IS 9
BP 1814
EP 1826
DI 10.1002/2016JE005122
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA EC0MO
UT WOS:000387795400014
ER
PT J
AU Travinsky, A
Vorobiev, D
Ninkov, Z
Raisanen, AD
Pellish, J
Robberto, M
Heap, S
AF Travinsky, Anton
Vorobiev, Dmitry
Ninkov, Zoran
Raisanen, Alan D.
Pellish, Jonny
Robberto, Massimo
Heap, Sara
TI Effects of heavy ion radiation on digital micromirror device performance
SO OPTICAL ENGINEERING
LA English
DT Article
DE digital micromirror device; digital micromirror device; digital
micromirror array; multiobject spectrometer; multiple-object
spectroscopy; heavy-ion radiation
ID MULTIOBJECT SPECTROGRAPH; SPECTROMETER; SPECTROSCOPY; TELESCOPE
AB There is a pressing need in the astronomical community for space-suitable multiobject spectrometers (MOSs). Several digital micromirror device (DMD)-based prototype MOSs have been developed for ground-based observatories; however, their main use will come with deployment on a space-based mission. Therefore, the performance of DMDs under exoatmospheric radiation needs to be evaluated. DMDs were rewindowed with 2-mu m thick pellicle and tested under accelerated heavy-ion radiation (control electronics shielded from radiation), with a focus on the detection of single-event effects (SEEs) including latch-up events. Testing showed that while DMDs are sensitive to nondestructive ion-induced state changes, all SEEs are cleared with a soft reset (i.e., sending a pattern to the device). The DMDs did not experience single-event induced permanent damage or functional changes that required a hard reset (power cycle), even at high ion fluences. This suggests that the SSE rate burden will be manageable for a DMD-based instrument when exposed to solar particle fluxes and cosmic rays in orbit. (C) 2016 Society of Photo-Optical Instrumentation Engineers (SPIE)
C1 [Travinsky, Anton; Vorobiev, Dmitry; Ninkov, Zoran] Rochester Inst Technol, Ctr Imaging Sci, 54 Lomb Mem Dr, Rochester, NY 14623 USA.
[Raisanen, Alan D.] Rochester Inst Technol, Dept Mfg & Mech Engn Technol, 78 Lomb Mem Dr, Rochester, NY 14623 USA.
[Pellish, Jonny; Heap, Sara] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Robberto, Massimo] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
RP Travinsky, A (reprint author), Rochester Inst Technol, Ctr Imaging Sci, 54 Lomb Mem Dr, Rochester, NY 14623 USA.
EM at4395@g.rit.edu
FU National Aeronautics and Space Administration (NASA) [NNX14AI62G S01]
FX This research was supported by the National Aeronautics and Space
Administration (NASA), Grant No. NNX14AI62G S01. We thank Dr. Vladimir
Horvat and Bruce Hyman from Texas A&M University Cyclotron Institute for
providing their prompt assistance during the testing and answering
practical questions about the facility. We thank Michael Douglas and
Benjamin Lee from Texas Instruments for productive discussions about DMD
performance under extreme conditions. We are also thankful to Mike
Buffalin and John "Sean" Greenslade from The Construct at RIT for
sharing their expertise in rapid manufacturing and help in producing
custom made parts for the test setup. Last but not least, we thank Emily
Berkson from Rochester Institute of Technology for her help with the
manuscript.
NR 34
TC 0
Z9 0
U1 1
U2 1
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 0091-3286
EI 1560-2303
J9 OPT ENG
JI Opt. Eng.
PD SEP
PY 2016
VL 55
IS 9
AR 094107
DI 10.1117/1.OE.55.9.094107
PG 8
WC Optics
SC Optics
GA EC6FV
UT WOS:000388232800037
ER
PT J
AU Ahnen, ML
Ansoldi, S
Antonelli, LA
Antoranz, P
Babic, A
Banerjee, B
Bangale, P
de Almeida, UB
Barrio, JA
Gonzalez, JB
Bednarek, W
Bernardini, E
Biasuzzi, B
Bilandl, A
Blanch, O
Bonnefoy, S
Bonnoli, G
Borracci, F
Bretz, T
Buson, S
Carosi, A
Chatterjee, A
Clavero, R
Colin, P
Colombo, E
Contreras, JL
Cortina, J
Covino, S
da Vela, P
Dazzi, F
De Angelis, A
De Lotto, B
Wilhelmi, ED
Di Pierro, F
Dominguez, A
Prester, DD
Dorner, D
Doro, M
Einecke, S
Glawion, DE
Elsaesser, D
Fernandez-Barra, A
Fidalgo, D
Fonseca, MV
Font, L
Frantzen, K
Fruck, C
Galindo, D
Lopez, RJG
Garczarczyk, M
Terrats, DG
Gaug, M
Giammaria, P
Godinovic, N
Munoz, AG
Gora, D
Guberman, D
Hadasch, D
Hahn, A
Hanabata, Y
Hayashida, M
Herrera, J
Hose, J
Hrupec, D
Hughes, G
Idec, W
Kodani, K
Konno, Y
Kubo, H
Kushida, J
La Barbera, A
Lelas, D
Lindfors, E
Lombardi, S
Longo, F
Lopez, M
Lopez-Coto, R
Majumdar, P
Makariev, M
Manganaro, M
Mannheim, K
Maraschi, L
Marcote, B
Mariotti, M
Martinez, M
Mazin, D
Menzel, U
Miranda, JM
Mirzoyan, R
Moralejo, A
Moretti, E
Nakajima, D
Neustroev, V
Niedzwieckil, A
Rosillo, MN
Nilsson, K
Nishijima, K
Noda, K
Nogues, L
Orito, R
Overkemping, A
Paiano, S
Palacio, J
Palatiello, M
Paneque, D
Paoletti, R
Paredes, JM
Paredes-Fortuny, X
Pedaletti, G
Perri, L
Persic, M
Poutanen, J
Moroni, PGP
Prandini, E
Puljak, I
Rhode, W
Ribo, M
Rico, J
Garcia, JR
Saito, T
Satalecka, K
Schultz, C
Schweizer, T
Shore, SN
Sillanpaa, A
Sitarek, J
Snidaric, I
Sobczynska, D
Stamerra, A
Steinbring, T
Strzys, M
Takalo, L
Takami, H
Tavecchio, F
Temnikov, P
Terzic, T
Tescaro, D
Teshima, M
Thaele, J
Torres, DF
Toyama, T
Treves, A
Verguilov, V
Vovk, I
Ward, JE
Will, M
Wu, MH
Zanin, R
Blinov, DA
Chen, WP
Efimova, NV
Forne, E
Grishina, TS
Hovatta, T
Jordan, B
Kimeridze, GN
Kopatskaya, EN
Koptelova, E
Kurtanidze, OM
Kurtanidze, SO
Lahteenmaki, A
Larionov, VM
Larionova, EG
Larionova, LV
Ligustri, R
Lin, HC
McBreen, B
Morozova, DA
Nikolashvili, MG
Raiteri, CM
Ros, JA
Sadun, AC
Sigua, LA
Tornikoski, M
Troitsky, IS
Villata, M
AF Ahnen, M. L.
Ansoldi, S.
Antonelli, L. A.
Antoranz, P.
Babic, A.
Banerjee, B.
Bangale, P.
de Almeida, U. Barres
Barrio, J. A.
Gonzalez, J. Becerra
Bednarek, W.
Bernardini, E.
Biasuzzi, B.
Bilandl, A.
Blanch, O.
Bonnefoy, S.
Bonnoli, G.
Borracci, F.
Bretz, T.
Buson, S.
Carosi, A.
Chatterjee, A.
Clavero, R.
Colin, P.
Colombo, E.
Contreras, J. L.
Cortina, J.
Covino, S.
da Vela, P.
Dazzi, F.
De Angelis, A.
De Lotto, B.
Wilhelmi, E. de Ona
Di Pierro, F.
Dominguez, A.
Prester, D. Dominis
Dorner, D.
Doro, M.
Einecke, S.
Glawion, D. Eisenacher
Elsaesser, D.
Fernandez-Barral, A.
Fidalgo, D.
Fonseca, M. V.
Font, L.
Frantzen, K.
Fruck, C.
Galindo, D.
Lopez, R. J. Garcia
Garczarczyk, M.
Terrats, D. Garrido
Gaug, M.
Giammaria, P.
Godinovic, N.
Munoz, A. Gonzalez
Gora, D.
Guberman, D.
Hadasch, D.
Hahn, A.
Hanabata, Y.
Hayashida, M.
Herrera, J.
Hose, J.
Hrupec, D.
Hughes, G.
Idec, W.
Kodani, K.
Konno, Y.
Kubo, H.
Kushida, J.
La Barbera, A.
Lelas, D.
Lindfors, E.
Lombardi, S.
Longo, F.
Lopez, M.
Lopez-Coto, R.
Majumdar, P.
Makariev, M.
Manganaro, M.
Mannheim, K.
Maraschi, L.
Marcote, B.
Mariotti, M.
Martinez, M.
Mazin, D.
Menzel, U.
Miranda, J. M.
Mirzoyan, R.
Moralejo, A.
Moretti, E.
Nakajima, D.
Neustroev, V.
Niedzwieckil, A.
Rosillo, M. Nievas
Nilsson, K.
Nishijima, K.
Noda, K.
Nogues, L.
Orito, R.
Overkemping, A.
Paiano, S.
Palacio, J.
Palatiello, M.
Paneque, D.
Paoletti, R.
Paredes, J. M.
Paredes-Fortuny, X.
Pedaletti, G.
Perri, L.
Persic, M.
Poutanen, J.
Moroni, P. G. Prada
Prandini, E.
Puljak, I.
Rhode, W.
Ribo, M.
Rico, J.
Garcia, J. Rodriguez
Saito, T.
Satalecka, K.
Schultz, C.
Schweizer, T.
Shore, S. N.
Sillanpaa, A.
Sitarek, J.
Snidaric, I.
Sobczynska, D.
Stamerra, A.
Steinbring, T.
Strzys, M.
Takalo, L.
Takami, H.
Tavecchio, F.
Temnikov, P.
Terzic, T.
Tescaro, D.
Teshima, M.
Thaele, J.
Torres, D. F.
Toyama, T.
Treves, A.
Verguilov, V.
Vovk, I.
Ward, J. E.
Will, M.
Wu, M. H.
Zanin, R.
Blinov, D. A.
Chen, W. P.
Efimova, N. V.
Forne, E.
Grishina, T. S.
Hovatta, T.
Jordan, B.
Kimeridze, G. N.
Kopatskaya, E. N.
Koptelova, E.
Kurtanidze, O. M.
Kurtanidze, S. O.
Lahteenmaki, A.
Larionov, V. M.
Larionova, E. G.
Larionova, L. V.
Ligustri, R.
Lin, H. C.
McBreen, B.
Morozova, D. A.
Nikolashvili, M. G.
Raiteri, C. M.
Ros, J. A.
Sadun, A. C.
Sigua, L. A.
Tornikoski, M.
Troitsky, I. S.
Villata, M.
CA Magic Collaboration
TI Long-term multi-wavelength variability and correlation study of
Markarian 421 from 2007 to 2009
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE astroparticle physics; BL Lacertae objects: individual: Markarian 421;
radiation mechanisms: non-thermal
ID X-RAY; MAGIC TELESCOPES; MAJOR UPGRADE; TEV PHOTONS; CRAB-NEBULA;
EMISSION; BLAZAR; RADIO; VIEW; PERFORMANCE
AB Aims. We study the multi-band variability and correlations of the TeV blazar Mrk 421 on year timescales, which can bring additional insight on the processes responsible for its broadband emission.
Methods. We observed Mrk 421 in the very high energy (VHE) gamma-ray range with the Cherenkov telescope MAGIC-I from March 2007 to June 2009 for a total of 96 h of effective time after quality cuts. The VHE flux variability is quantified using several methods, including the Bayesian Block algorithm, which is applied to data from Cherenkov telescopes here for the first time. The 2.3 yr long MAGIC light curve is complemented with data from the Swift/BAT and RXTE/ASM satellites and the KVA, GASP-WEBT, OVRO, and Metsahovi telescopes from February 2007 to July 2009, allowing for an excellent characterisation of the multi-band variability and correlations over year timescales.
Results. Mrk 421 was found in different gamma-ray emission states during the 2.3 yr long observation period: The flux above 400 GeV spans from the minimum nightly value of (1.3 +/- 0.4) x 10(-11) cm(-2) s(-1) to the maximum flux, that is about 24 times higher, at (3.1 +/- 0.1) x 10(-10) cm(-2) s(-1). Flares and different levels of variability in the gamma-ray light curve could be identified with the Bayesian Block algorithm. The same behaviour of a quiet and active emission was found in the X-ray light curves measured by Swift/BAT and the RXTE/ASM, with a direct correlation in time. The behaviour of the optical light curve of GASP-WEBT and the radio light curves by OVRO and Metsahovi are different as they show no coincident features with the higher energetic light curves and a less variable emission. Overall, the fractional variability increases with energy. The comparable variability in the X-ray and VHE bands and their direct correlation during both high-and low-activity periods spanning many months show that the electron populations radiating the X-ray and gamma-ray photons are either the same, as expected in the synchrotron-self-Compton mechanism, or at least strongly correlated, as expected in electromagnetic cascades.
C1 [Ahnen, M. L.; Bilandl, A.; Hughes, G.; Prandini, E.] Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland.
[Ansoldi, S.; Biasuzzi, B.; De Lotto, B.; Longo, F.; Palatiello, M.; Persic, M.; Treves, A.] Univ Udine, I-33100 Udine, Italy.
[Ansoldi, S.; Biasuzzi, B.; De Lotto, B.; Longo, F.; Palatiello, M.; Persic, M.; Treves, A.] INFN Trieste, I-33100 Udine, Italy.
[Antonelli, L. A.; Bonnoli, G.; Carosi, A.; Covino, S.; Di Pierro, F.; Giammaria, P.; La Barbera, A.; Lombardi, S.; Maraschi, L.; Perri, L.; Stamerra, A.; Tavecchio, F.] INAF Natl Inst Astrophys, I-00136 Rome, Italy.
[Antoranz, P.; da Vela, P.; Miranda, J. M.; Paoletti, R.] Univ Siena, I-53100 Siena, Italy.
[Antoranz, P.; da Vela, P.; Miranda, J. M.; Paoletti, R.] INFN Pisa, I-53100 Siena, Italy.
[Babic, A.; Prester, D. Dominis; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Terzic, T.] Univ Split, Univ Rijeka, Rudjer Boskov Inst, Croatian MAGIC Consortium, Split, Croatia.
[Babic, A.; Prester, D. Dominis; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Terzic, T.] Univ Zagreb, Zagreb 41000, 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. Rodriguez; 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.; Rosillo, M. Nievas] Univ Complutense, E-28040 Madrid, Spain.
[Gonzalez, J. Becerra; Clavero, R.; Colombo, E.; Lopez, R. J. Garcia; Herrera, J.; Manganaro, M.; Will, M.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain.
[Gonzalez, J. Becerra; Clavero, R.; Colombo, E.; Lopez, R. J. Garcia; Herrera, J.; Manganaro, M.; Will, M.] Univ La Laguna, Dept Astrofis, Tenerife 38206, Spain.
[Bednarek, W.; Idec, W.; Niedzwieckil, A.; Sitarek, J.; Sobczynska, D.] Univ Lodz, PL-90236 Lodz, Poland.
[Bernardini, E.; Garczarczyk, M.; Gora, D.; Pedaletti, G.; Satalecka, K.] Deutsch Elekt Synchrotron DESY, D-15738 Zeuthen, Germany.
[Blanch, O.; Cortina, J.; Fernandez-Barral, A.; Munoz, A. Gonzalez; Guberman, D.; Lopez-Coto, R.; Martinez, M.; Moralejo, A.; Nogues, L.; Palacio, J.; Rico, J.; Ward, J. E.] Campus UAB, Barcelona Inst Sci & Technol, Inst Fis Altes Energies IFAE, Bellaterra 08193, Barcelona, Spain.
[Bretz, T.; Dorner, D.; Glawion, D. Eisenacher; Mannheim, K.; Steinbring, T.] Univ Wurzburg, D-97074 Wurzburg, Germany.
[Buson, S.; De Angelis, A.; Doro, M.; Mariotti, M.; Paiano, S.; Schultz, C.; Tescaro, D.] Univ Padua, I-35131 Padua, Italy.
[Buson, S.; De Angelis, A.; Doro, M.; Mariotti, M.; Paiano, S.; Schultz, C.; Tescaro, D.] Ist Nazl Fis Nucl, I-35131 Padua, Italy.
[Wilhelmi, E. de Ona; Wu, M. H.] CSIC IEEC, Inst Space Sci, Barcelona 08193, Spain.
[Einecke, S.; Elsaesser, D.; Frantzen, K.; Overkemping, A.; Rhode, W.; Thaele, J.] Tech Univ Dortmund, D-44221 Dortmund, Germany.
[Font, L.; Terrats, D. Garrido; Gaug, M.] Univ Autonoma Barcelona, Dept Fis, Unitat Fis Radiat, Bellaterra 08193, Spain.
[Font, L.; Terrats, D. Garrido; Gaug, M.] Univ Autonoma Barcelona, CERES IEEC, Bellaterra 08193, Spain.
[Galindo, D.; Marcote, B.; Paredes, J. M.; Paredes-Fortuny, X.; Ribo, M.; Zanin, R.] Univ Barcelona, ICC, IEEC UB, E-08028 Barcelona, Spain.
[Hadasch, D.; Hanabata, Y.; Hayashida, M.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Nakajima, D.; Nishijima, K.; Orito, R.; Saito, T.; Takami, H.] Univ Tokyo, Dept Phys, ICRR, Japanese MAGIC Consortium, Tokyo 1138654, Japan.
[Hadasch, D.; Hanabata, Y.; Hayashida, M.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Nakajima, D.; Nishijima, K.; Orito, R.; Saito, T.; Takami, H.] Univ Tokushima, Tokai Univ, Kyoto Univ, Hakubi Ctr,KEK, Tokushima, Japan.
[Lindfors, E.; Neustroev, V.; Nilsson, K.; Poutanen, J.; Sillanpaa, A.; Takalo, L.] Univ Turku, Tuorla Observ, Finnish MAGIC Consortium, Oulu 90014, Finland.
[Lindfors, E.; Neustroev, V.; Nilsson, K.; Poutanen, J.; Sillanpaa, A.; Takalo, L.] Univ Oulu, Astron Div, Oulu 90014, Finland.
[Makariev, M.; Temnikov, P.; Verguilov, V.] Inst Nucl Energy Res, Sofia 1784, Bulgaria.
[Moroni, P. G. Prada; Shore, S. N.] Univ Pisa, I-56126 Pisa, Italy.
[Moroni, P. G. Prada; Shore, S. N.] Ist Nazl Fis Nucl, I-56126 Pisa, Italy.
[Torres, D. F.] ICREA, Barcelona 08193, Spain.
[Torres, D. F.] CSIC IEEC, Inst Space Sci, Barcelona 08193, Spain.
[de Almeida, U. Barres] CBPF MCTI, 150 Urca, BR-22290180 Rio De Janeiro, Brazil.
[Gonzalez, J. Becerra] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gonzalez, J. Becerra] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Gonzalez, J. Becerra] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Bernardini, E.] Humboldt Univ, Inst Phys Newtonstr 15, D-12489 Berlin, Germany.
[Bretz, T.] Ecole Polytech Fed Lausanne, Lausanne, Switzerland.
[Mazin, D.; Teshima, M.] Japanese MAGIC Consortium, Kyoto, Japan.
[Nilsson, K.] Finnish Ctr Astron ESO FINCA, Turku, Finland.
[Persic, M.] INAF Trieste, I-34143 Trieste, Italy.
[Prandini, E.] ISDC Sci Data Ctr Astrophys, CH-1290 Geneva, Switzerland.
[Blinov, D. A.; Grishina, T. S.; Kopatskaya, E. N.; Larionov, V. M.; Larionova, E. G.; Larionova, L. V.; Morozova, D. A.; Troitsky, I. S.] St Petersburg State Univ, Astron Inst, St Petersburg 198504, Russia.
[Blinov, D. A.] Univ Crete, Iraklion, Greece.
[Chen, W. P.; Koptelova, E.; Lin, H. C.] Natl Cent Univ, Grad Inst Astron, 300 Zhongda Rd, Taoyuan 32001, Taiwan.
[Efimova, N. V.; Larionov, V. M.] Pulkovo Observ, St Petersburg 196140, Russia.
[Forne, E.; Ros, J. A.] Agrupacio Astron Sabadell, Barcelona 08206, Spain.
[Hovatta, T.; Lahteenmaki, A.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, Metsahovintie 114, Kylmala 02540, Finland.
[Jordan, B.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland.
[Kimeridze, G. N.; Kurtanidze, O. M.; Kurtanidze, S. O.; Nikolashvili, M. G.; Sigua, L. A.] Abastumani Observ, GE-0301 Abastumani, Rep of Georgia.
[Kurtanidze, O. M.] Kazan Fed Univ, Engelhardt Astron Observ, Tatarstan, Russia.
[Lahteenmaki, A.] Aalto Univ, Dept Radio Sci & Engn, POB 3000, Aalto 00076, Finland.
[Ligustri, R.] Circolo Astrofili Talmassons, Via Cadorna,57, I-33030 Talmassons, Italy.
[McBreen, B.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Raiteri, C. M.; Villata, M.] INAF Osservatorio Astrofis Torino, I-10025 Pino Torinese, TO, Italy.
[Sadun, A. C.] Univ Colorado, Dept Phys, Denver, CO 80217 USA.
RP Overkemping, A (reprint author), Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain.; Overkemping, A (reprint author), Univ La Laguna, Dept Astrofis, Tenerife 38206, Spain.; Tescaro, D (reprint author), Univ Padua, I-35131 Padua, Italy.; Tescaro, D (reprint author), Ist Nazl Fis Nucl, I-35131 Padua, Italy.; Manganaro, M (reprint author), Tech Univ Dortmund, D-44221 Dortmund, Germany.
EM manganaro@iac.es; ann-kristin.overkemping@tu-dortmund.de;
diego.tescaro@gmail.com
RI Lahteenmaki, Anne/L-5987-2013; Manganaro, Marina/B-7657-2011; Miranda,
Jose Miguel/F-2913-2013; Barrio, Juan/L-3227-2014; GAug,
Markus/L-2340-2014; Cortina, Juan/C-2783-2017; Morozova,
Daria/H-1298-2013; Puljak, Ivica/D-8917-2017;
OI Larionov, Valeri/0000-0002-4640-4356; Moretti,
Elena/0000-0001-5477-9097; Poutanen, Juri/0000-0002-0983-0049; Torres,
Diego F./0000-0002-1522-9065; Prandini, Elisa/0000-0003-4502-9053;
Manganaro, Marina/0000-0003-1530-3031; Miranda, Jose
Miguel/0000-0002-1472-9690; Barrio, Juan/0000-0002-0965-0259; GAug,
Markus/0000-0001-8442-7877; Cortina, Juan/0000-0003-4576-0452; Morozova,
Daria/0000-0002-9407-7804; Blinov, Dmitry/0000-0003-0611-5784;
Larionova, Elena/0000-0002-2471-6500; Grishina,
Tatiana/0000-0002-3953-6676
FU German BMBF; German MPG; Italian INFN; Italian INAF; Swiss National Fund
SNF; ERDF under the Spanish MINECO [FPA2012-39502]; Japanese JSPS;
Japanese MEXT; Centro de Excelencia Severo Ochoa of Spanish
Consolider-Ingenio programme [SEV-2012-0234]; Academy of Finland
[268740, 212656, 210338, 121148]; Croatian Science Foundation (HrZZ)
Project [09/176]; University of Rijeka [13.12.1.3.02]; DFG [SFB823/C4,
SFB876/C3]; Polish MNiSzW grant [745/N-HESS-MAGIC/2010/0]; NASA
[NNX08AW31G, NNX11A043G]; NFS [AST-0808050, AST-1109911]; Russian RFBR
[15-02-00949]; St. Petersburg University [6.38.335.2015]; Shota
Rustaveli National Science Foundation [FR/577/6-320/13]; CPAN Spanish
Consolider-Ingenio programme [CSD2007-00042]; MultiDark project of the
Spanish Consolider-Ingenio programme [CSD2009-00064]
FX We 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 ERDF under
the Spanish MINECO (FPA2012-39502), and the Japanese JSPS and MEXT is
gratefully acknowledged. This work was also supported by the Centro de
Excelencia Severo Ochoa SEV-2012-0234, CPAN CSD2007-00042, and MultiDark
CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme,
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. The
public data archives of Swift/BAT and RXTE/ASM are acknowledged. We
thank the OVRO telescope for making its results available for the
public. The OVRO 40 m monitoring program is supported in part by NASA
grants NNX08AW31G and NNX11A043G, and NFS grants AST-0808050 and
AST-1109911. We also thank the KVA and Metsahovi telescopes for making
their light curves available. M. Villata organized the optical-to-radio
observations by GASP-WEBT as the president of the collaboration. The
Metsahovi team acknowledges the support from the Academy of Finland to
our observing projects (numbers 212656, 210338, 121148, and others). St.
Petersburg University team acknowledges support from Russian RFBR grant
15-02-00949 and St. Petersburg University research grant 6.38.335.2015.
The Abastumani Observatory team acknowledges financial support by the
Shota Rustaveli National Science Foundation under contract
FR/577/6-320/13.
NR 52
TC 0
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U1 5
U2 5
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 SEP
PY 2016
VL 593
AR A91
DI 10.1051/0004-6361/201628447
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4HU
UT WOS:000385820100071
ER
PT J
AU Asensio-Torres, R
Janson, M
Hashimoto, J
Thalmann, C
Currie, T
Buenzli, E
Kudo, T
Kuzuhara, M
Kusakabe, N
Abe, L
Akiyama, E
Brandner, W
Brandt, TD
Carson, J
Egner, S
Feldt, M
Goto, M
Grady, C
Guyon, O
Hayano, Y
Hayashi, M
Hayashi, S
Henning, T
Hodapp, K
Ishii, M
Iye, M
Kandori, R
Knapp, G
Kwon, J
Matsuo, T
McElwain, M
Mayama, S
Miyama, S
Morino, J
Moro-Martin, A
Nishimura, T
Pyo, T
Serabyn, E
Suenaga, T
Suto, H
Suzuki, R
Takahashi, Y
Takami, M
Takato, N
Terada, H
Turner, E
Watanabe, M
Wisniewski, J
Yamada, T
Takami, H
Usuda, T
Tamura, M
AF Asensio-Torres, R.
Janson, M.
Hashimoto, J.
Thalmann, C.
Currie, T.
Buenzli, E.
Kudo, T.
Kuzuhara, M.
Kusakabe, N.
Abe, L.
Akiyama, E.
Brandner, W.
Brandt, T. D.
Carson, J.
Egner, S.
Feldt, M.
Goto, M.
Grady, C.
Guyon, O.
Hayano, Y.
Hayashi, M.
Hayashi, S.
Henning, T.
Hodapp, K.
Ishii, M.
Iye, M.
Kandori, R.
Knapp, G.
Kwon, J.
Matsuo, T.
McElwain, M.
Mayama, S.
Miyama, S.
Morino, J.
Moro-Martin, A.
Nishimura, T.
Pyo, T.
Serabyn, E.
Suenaga, T.
Suto, H.
Suzuki, R.
Takahashi, Y.
Takami, M.
Takato, N.
Terada, H.
Turner, E.
Watanabe, M.
Wisniewski, J.
Yamada, T.
Takami, H.
Usuda, T.
Tamura, M.
TI Polarimetry and flux distribution in the debris disk around HD 32297
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE protoplanetary disks; techniques: high angular resolution; stars:
individual: HD 32297
ID CIRCUMSTELLAR DISK; IMAGING POLARIMETRY; PROTOPLANETARY DISK; HR 4796A;
HD-32297; DISCOVERY; IMAGES; DUST; SUBTRACTION; EXOPLANETS
AB We present high-contrast angular differential imaging (ADI) observations of the debris disk around HD32297 in H-band, as well as the first polarimetric images for this system in polarized differential imaging (PDI) mode with Subaru/HICIAO. In ADI, we detect the nearly edge-on disk at > 5 sigma levels from similar to 0.45 '' to similar to 1.7 '' (50-192AU) from the star and recover the spine deviation from the midplane already found in previous works. We also find for the first time imaging and surface brightness (SB) indications for the presence of a gapped structure on both sides of the disk at distances of similar to 0.75 '' (NE side) and similar to 0.65 '' (SW side). Global forward-modelling work delivers a best-fit model disk and well-fitting parameter intervals that essentially match previous results, with high-forward scattering grains and a ring located at 110AU. However, this single ring model cannot account for the gapped structure seen in our SB profiles. We create simple double ring models and achieve a satisfactory fit with two rings located at 60 and 95AU, respectively, low-forward scattering grains and very sharp inner slopes. In polarized light we retrieve the disk extending from similar to 0.25-1.6 '', although the central region is quite noisy and high S/N are only found in the range similar to 0.75-1.2 ''. The disk is polarized in the azimuthal direction, as expected, and the departure from the midplane is also clearly observed. Evidence for a gapped scenario is not found in the PDI data. We obtain a linear polarization degree of the grains that increases from similar to 10% at 0.55 '' to similar to 25% at 1.6 ''. The maximum is found at scattering angles of similar to 90 degrees, either from the main components of the disk or from dust grains blown out to larger radii.
C1 [Asensio-Torres, R.; Janson, M.] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, S-10691 Stockholm, Sweden.
[Hashimoto, J.; Kusakabe, N.] NINS, Astrobiol Ctr, Mitaka, Tokyo 1818588, Japan.
[Thalmann, C.; Buenzli, E.] ETH, Inst Astron, Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland.
[Currie, T.; Kudo, T.; Egner, S.; Guyon, O.; Hayano, Y.; Hayashi, S.; Nishimura, T.; Pyo, T.; Takato, N.] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Kuzuhara, M.] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan.
[Abe, L.] Univ Nice Sophia Antipolis, Lab Lagrange UMR 7293, CNRS, Observ Cote Azur, F-06108 Nice 2, France.
[Akiyama, E.; Hayashi, M.; Ishii, M.; Iye, M.; Kandori, R.; Morino, J.; Suto, H.; Suzuki, R.; Takahashi, Y.; Terada, H.; Takami, H.; Usuda, T.; Tamura, M.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Brandner, W.; Carson, J.; Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Brandt, T. D.; Feldt, M.] Inst Adv Study, Dept Astrophys, Princeton, NJ 08540 USA.
[Carson, J.] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
[Goto, M.] Ludwig Maximilians Univ Munchen, Univ Sternwarte Munchen, D-81679 Munich, Germany.
[Grady, C.] Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Grady, C.] Eureka Sci, Oakland, CA 96002 USA.
[Grady, C.] Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.
[Hodapp, K.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
[Knapp, G.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Kwon, J.; Tamura, M.] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
[Matsuo, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto, Kyoto 6068502, Japan.
[Mayama, S.] Grad Univ Adv Studies SOKENDAI, Ctr Promot Integrated Sci, Hayama, Kanagawa 2400193, 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.; Turner, E.] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778568, Japan.
[Suenaga, T.] Grad Univ Adv Studies SOKENDAI, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan.
[Takami, M.] Acad Sin, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Watanabe, M.] Hokkaido Univ, Dept Cosmosci, Kita Ku, Sapporo, Hokkaido 0600810, Japan.
[Wisniewski, J.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Yamada, T.] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan.
RP Asensio-Torres, R (reprint author), Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, S-10691 Stockholm, Sweden.
EM ruben.torres@astro.su.se; markus.janson@astro.su.se
RI MIYAMA, Shoken/A-3598-2015;
OI Feldt, Markus/0000-0002-4188-5242
FU Knut and Alice Wallenberg foundation; US National Science Foundation
[1009203]
FX We would like to thank J.C. Augereau for providing the GraTeR code used
to create our disk models. R. Asensio-Torres and M. Janson gratefully
acknowledge funding from the Knut and Alice Wallenberg foundation. J.
Carson acknowledges support via the US National Science Foundation under
Award No. 1009203.
NR 47
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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 SEP
PY 2016
VL 593
AR A73
DI 10.1051/0004-6361/201628543
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4HU
UT WOS:000385820100081
ER
PT J
AU Drouart, G
Rocca-Volmerange, B
De Breuck, C
Fioc, M
Lehnert, M
Seymour, N
Stern, D
Vernet, J
AF Drouart, G.
Rocca-Volmerange, B.
De Breuck, C.
Fioc, M.
Lehnert, M.
Seymour, N.
Stern, D.
Vernet, J.
TI Disentangling star formation and AGN activity in powerful infrared
luminous radio galaxies at 1 < z < 4
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; galaxies: evolution; galaxies: high-redshift;
galaxies: star formation; quasars: general; galaxies: starburst
ID SPECTRAL ENERGY-DISTRIBUTIONS; INITIAL MASS FUNCTION; BLACK-HOLE
ACCRETION; DEEP FIELD SOUTH; SIMILAR-TO 2; HIGH-REDSHIFT; GALACTIC
NUCLEI; ELLIPTIC GALAXIES; STELLAR POPULATIONS; STARBURST GALAXIES
AB High-redshift radio galaxies present signs of both star formation and AGN activity, making them ideal candidates to investigate the connection and coevolution of AGN and star formation in the progenitors of present-day massive galaxies. We make use of a sample of 11 powerful radio galaxies spanning 1 < z < 4 which have complete coverage of their spectral energy distribution (SED) from UV to FIR wavelengths. Using Herschel data, we disentangle the relative contribution of the AGN and star formation by combining the galaxy evolution code PEGASE.3 with an AGN torus model. We find that three components are necessary to reproduce the observed SEDs: an evolved and massive stellar component, a submm bright young starburst, and an AGN torus. We find that powerful radio galaxies form at very high-redshift, but experience episodic and important growth at 1 < z < 4 as the mass of the associated starburst varies from 5 to 50% of the total mass of the system. The properties of star formation differ from source to source, indicating no general trend of the star formation properties in the most infrared luminous high-redshift radio galaxies and no correlation with the AGN bolometric luminosity. Moreover, we find that AGN scattered light have a very limited impact on broad-band SED fitting on our sample. Finally, our analysis also suggests a wide range in origins for the observed star formation, which we partially constrain for some sources.
C1 [Drouart, G.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden.
[Drouart, G.; Seymour, N.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA, Australia.
[Drouart, G.; Rocca-Volmerange, B.; Fioc, M.; Lehnert, M.] Inst Astrophys Paris, 98bis Blvd Arago, F-75014 Paris, France.
[De Breuck, C.; Vernet, J.] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Stern, D.] CALTECH, Jet Prop Lab, Mail Stop 169-221, Pasadena, CA 91109 USA.
RP Drouart, G (reprint author), Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden.; Drouart, G (reprint author), Curtin Univ, Int Ctr Radio Astron Res, Perth, WA, Australia.; Drouart, G (reprint author), Inst Astrophys Paris, 98bis Blvd Arago, F-75014 Paris, France.
EM guillaume.drouart@curtin.edu.au
FU ARC; NASA; ESO scientific visitor programme
FX G.D. would like to warmly thank Alessandro Romeo, Kirsten Knudsen, and
Clive Tadhunter for the useful discussions that contributed to improve
this paper. The authors also thank the referee for detailed suggestions
and a thorough report that helped to clarify this paper. G.D. also
thanks Nina Hatch for providing HST fluxes for the Spiderweb galaxy and
A. Galametz for providing images for part of the sample. G.D. thanks
Philip Best for providing the 3C 368 and 3C 470 data. N.S. is the
recipient of an ARC Future Fellowship. The work of DS was carried out at
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with NASA. Based on observations made with the NASA/ESA Hubble
Space Telescope, and obtained from the Hubble Legacy Archive, which is a
collaboration between the Space Telescope Science Institute
(STScI/NASA), the Space Telescope European Coordinating Facility
(ST-ECF/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA). GD
acknowledges the support from the ESO scientific visitor programme.
NR 161
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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 SEP
PY 2016
VL 593
AR A109
DI 10.1051/0004-6361/201526880
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4HU
UT WOS:000385820100015
ER
PT J
AU El-Marry, MR
Thomas, N
Gracia-Berna, A
Pajola, M
Lee, JC
Massironi, M
Davidsson, B
Marchi, S
Keller, HU
Hviid, SF
Besse, S
Sierks, H
Barbieri, C
Lamy, PL
Koschny, D
Rickman, H
Rodrigo, R
A'Hearn, MF
Auger, AT
Barucci, MA
Bertaux, JL
Bertini, I
Bodewits, D
Gremonese, G
Deppo, V
Cecco, M
Dehei, S
Guttler, C
Fornasier, S
Fulle, M
Giacomini, L
Groussin, O
Gutierrez, PJ
Ip, WH
Jorda, L
Knollenberg, J
Kovacs, G
Kramm, JR
Kuhrt, E
Kuppers, M
Lara, LM
Lazzarin, M
Moreno, JJL
Marschall, R
Marzari, F
Naletto, G
Oklay, N
Pommerol, A
Preusker, F
Scholten, F
Tubiana, C
Vincent, JB
AF El-Marry, M. R.
Thomas, N.
Gracia-Berna, A.
Pajola, M.
Lee, J. -C.
Massironi, M.
Davidsson, B.
Marchi, S.
Keller, H. U.
Hviid, S. F.
Besse, S.
Sierks, H.
Barbieri, C.
Lamy, P. L.
Koschny, D.
Rickman, H.
Rodrigo, R.
A'Hearn, M. F.
Auger, A. -T.
Barucci, M. A.
Bertaux, J. -L.
Bertini, I.
Bodewits, D.
Gremonese, G.
Da Deppo, V.
De Cecco, M.
Dehei, S.
Guettler, C.
Fornasier, S.
Fulle, M.
Giacomini, L.
Groussin, O.
Gutierrez, P. J.
Ip, W. -H
Jorda, L.
Knollenberg, J.
Kovacs, G.
Kramm, J. -R.
Kuehrt, E.
Kueppers, M.
Lara, L. M.
Lazzarin, M.
Moreno, J. J. Lopez
Marschall, R.
Marzari, F.
Naletto, G.
Oklay, N.
Pommerol, A.
Preusker, F.
Scholten, F.
Tubiana, C.
Vincent, J. -B.
TI Regional surface morphology of comet 67P/Churyumov-Gerasimenko from
Rosetta/OSIRIS images: The southern hemisphere
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE comets: general; comets: individual: 67P/Churyumov-Gerasimenko; methods:
observational
ID NUCLEUS; OSIRIS; 67P
AB Aims. The OSIRIS camera on board the Rosetta spacecraft has been acquiring images of the comet 67P/Churyumov-Gerasimenko (67P)'s nucleus since August 2014. Starting in May 2015, the southern hemisphere gradually became illuminated and was imaged for the first time. Here we present the regional morphology of the southern hemisphere, which serves as a companion to an earlier paper that presented the regional morphology of the northern hemisphere.
Methods. We used OSIRIS images that were acquired at orbits similar to 45-125 km from the center of the comet (corresponding to spatial resolutions of similar to 0.8 to 2.3 m/pixel) coupled with the use of digital terrain models to define the different regions on the surface, and identify structural boundaries accurately.
Results. Seven regions have been defined in the southern hemisphere bringing the total number of defined regions on the surface of the nucleus to 26. These classifications are mainly based on morphological and/or topographic boundaries. The southern hemisphere shows a remarkable dichotomy with its northern counterpart mainly because of the absence of wide-scale smooth terrains, dust coatings and large unambiguous depressions. As a result, the southern hemisphere closely resembles previously identified consolidated regions. An assessment of the overall morphology of comet 67P suggests that the comet's two lobes show surface heterogeneities manifested in different physical/mechanical characteristics, possibly extending to local (i.e., within a single region) scales.
C1 [El-Marry, M. R.; Thomas, N.; Gracia-Berna, A.; Pommerol, A.] Univ Bern, Inst Phys, Sidlerstr 5, CH-3012 Bern, Switzerland.
[Pajola, M.] Univ Padua, Ctr Ateneo Studied Attivita Spaziali Giuseppe Col, I-35131 Padua, Italy.
[Lee, J. -C.] Natl Cent Univ, Dept Earth Sci, Chungli 32054, Taiwan.
[Massironi, M.] Univ Padua, Dipartimento Geosci, Via G Gradenigo 6, I-35131 Padua, Italy.
[Davidsson, B.] Jet Prop Lab, M S 183-301,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Marchi, S.] Southwest Res Inst, Solar Syst Explorat Res Virtual Inst, 1050 Walnut St,Suite 300, Boulder, CO 80302 USA.
[Keller, H. U.] TU Braunschweig, Inst Geophys & Extraterr Phys, D-38106 Braunschweig, Germany.
[Hviid, S. F.; Preusker, F.; Scholten, F.] Inst Planetenforsch, Deutsch Zentrum Luft & Raumfahrt DLR, Rutherfordstr 2, D-12489 Berlin, Germany.
[Besse, S.; Koschny, D.] European Space Agcy, Sci Support Off, NL-2201 Noordwijk, Netherlands.
[Sierks, H.; Guettler, C.; Kovacs, G.; Kramm, J. -R.; Oklay, N.; Tubiana, C.; Vincent, J. -B.] Max Planck Inst Sonnensystemforsch, Justus von Liebig Weg 3, D-37077 Gottingen, Germany.
[Barbieri, C.; Gremonese, G.; Lazzarin, M.; Marzari, F.] INAF Osservatorio Astrono, Vicolo Osservatorio 5, I-35122 Padua, Italy.
[Lamy, P. L.; Auger, A. -T.] Aix Marseille Univ, CNRS, LAM, UMR 7326, 38 Rue Frederic Joliot Curie, F-13388 Marseille, France.
[Rodrigo, R.] Int Space Sci Inst, Hallerstr 6, CH-3012 Bern, Switzerland.
[Rickman, H.; Rodrigo, R.] CSIC INTA, Ctr Astrobiol, Madrid 28850, Spain.
[Rickman, H.] Uppsala Univ, Dept Phys & Astron, Box 516, S-75120 Uppsala, Sweden.
PAS Space Res Ctr, Bartycka 18A, PL-00716 Warsaw, Poland.
[A'Hearn, M. F.; Bodewits, D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Barucci, M. A.] Univ Paris Diderot, Univ Paris 06, CNRS, Obs Paris,LESIA, 5 Pl J Janssen, F-92195 Meudon, France.
[Bertaux, J. -L.] CNRS UVSQ IPSL, LATMOS, 11 Blvd Alembert, F-78280 Guyancourt, France.
[Bertini, I.] Univ Padua, Ctr Ateneo Studied Attivita Spaziali Giuseppe Col, I-35131 Padua, Italy.
[Da Deppo, V.] CNR IFN UOS Padova LUXOR, Via Trasea 7, I-35131 Padua, Italy.
[De Cecco, M.] Univ Trento, UNITN, Via Mesiano 77, I-38100 Trento, Italy.
[Dehei, S.] Univ Padua, Dept Mech Engn, Via Venezia 1, I-35131 Padua, Italy.
[Fulle, M.] INAF Osservatorio Astron, Via Tiepolo 11, I-34014 Trieste, Italy.
[Gutierrez, P. J.; Lara, L. M.; Moreno, J. J. Lopez] CSIC, Inst Astrofis Andalucia, C Glorieta Astron S-N, E-18008 Granada, Spain.
[Ip, W. -H] Natl Cent Univ, Grad Inst Astron, 300 Chung Da Rd, Chungli 32054, Taiwan.
[Jorda, L.] Lab Astrophys Marseille, 38 Rue Frederic Joliot Curie, F-13388 Marseille 13, France.
[Kueppers, M.] European Space Astron Ctr ESA, Sci Support Off, POB 78, Madrid 28691, Spain.
[Naletto, G.] Univ Padua, Dept Informat Engn, Via Gradenigo 6-B, I-35131 Padua, Italy.
RP El-Marry, MR (reprint author), Univ Bern, Inst Phys, Sidlerstr 5, CH-3012 Bern, Switzerland.
EM mohammed.elmaarry@space.unibe.ch
RI Naletto, Giampiero/S-6329-2016; Gutierrez, Pedro/K-9637-2014;
OI Naletto, Giampiero/0000-0003-2007-3138; Gutierrez,
Pedro/0000-0002-7332-6269; fulle, marco/0000-0001-8435-5287; Massironi,
Matteo/0000-0002-7757-8818
FU Germany (DLR); France (CNES); Italy (ASI); Spain (MEC); Sweden (SNSB);
ESA Technical Directorate; Rosetta mission
FX OSIRIS was built by a consortium of the Max-Planck-Institut fur
Sonnensystemforschung, in Gottingen, Germany, CISAS-University of
Padova, Italy, the Laboratoire d'Astrophysique de Marseille, France, the
Instituto de Astrofisica de Andalucia, CSIC, Granada, Spain, the
Research and Scientific Support Department of the European Space Agency,
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
national funding agencies of Germany (DLR), France (CNES), Italy (ASI),
Spain (MEC), Sweden (SNSB), and the ESA Technical Directorate is
gratefully acknowledged. We thank the ESA teams at ESAC, ESOC and ESTEC
for their work in support of the Rosetta mission.
NR 26
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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 SEP
PY 2016
VL 593
AR A110
DI 10.1051/0004-6361/201628634
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4HU
UT WOS:000385820100095
ER
PT J
AU Luna, M
Diaz, AJ
Oliver, R
Terradas, J
Karpen, J
AF Luna, M.
Diaz, A. J.
Oliver, R.
Terradas, J.
Karpen, J.
TI The effects of magnetic-field geometry on longitudinal oscillations of
solar prominences: Cross-sectional area variation for thin tubes
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Sun: corona; Sun: filaments, prominences; Sun: oscillations; Sun:
magnetic fields
ID MAGNETOHYDRODYNAMIC WAVES; FILAMENT; MODEL
AB Context. Solar prominences are subject to both field-aligned (longitudinal) and transverse oscillatory motions, as evidenced by an increasing number of observations. Large-amplitude longitudinal motions provide valuable information on the geometry of the filament-channel magnetic structure that supports the cool prominence plasma against gravity. Our pendulum model, in which the restoring force is the gravity projected along the dipped field lines of the magnetic structure, best explains these oscillations. However, several factors can influence the longitudinal oscillations, potentially invalidating the pendulum model.
Aims. The aim of this work is to study the influence of large-scale variations in the magnetic field strength along the field lines, i.e., variations of the cross-sectional area along the flux tubes supporting prominence threads.
Methods. We studied the normal modes of several flux tube configurations, using linear perturbation analysis, to assess the influence of different geometrical parameters on the oscillation properties.
Results. We found that the influence of the symmetric and asymmetric expansion factors on longitudinal oscillations is small.
Conclusions. We conclude that the longitudinal oscillations are not significantly influenced by variations of the cross-section of the flux tubes, validating the pendulum model in this context.
C1 [Luna, M.] Inst Astrofis Canarias, Tenerife 38205, Spain.
[Luna, M.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Diaz, A. J.; Oliver, R.; Terradas, J.] Univ Illes Balears, Dept Fis, Palma de Mallorca 07122, Spain.
[Oliver, R.; Terradas, J.] Inst Appl Comp & Community Code IAC3, Palma de Mallorca 07122, Spain.
[Karpen, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Luna, M (reprint author), Inst Astrofis Canarias, Tenerife 38205, Spain.; Luna, M (reprint author), Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
EM mluna@iac.es
FU Spanish Ministry of Economy and Competitiveness [AYA2011-24808,
AYA2010-18029, AYA2014-55078-P]; FP7 European Research Council [277829];
Spanish "Ministerio de Educacion y Ciencia"; MINECO; FEDER
[AYA2014-54485-P]; International Space Science Institute (ISSI) [314]
FX M. Luna acknowledges the support by the Spanish Ministry of Economy and
Competitiveness through projects AYA2011-24808, AYA2010-18029, and
AYA2014-55078-P. This work contributes to the deliverables identified in
FP7 European Research Council grant agreement 277829, "Magnetic
Connectivity through the Solar Partially Ionized Atmosphere" (PI: E.
Khomenko). J.T. acknowledges support from the Spanish "Ministerio de
Educacion y Ciencia" through a Ramon y Cajal grant and support from
MINECO and FEDER funds through project AYA2014-54485-P. M.L., J.T., and
J.K. acknowledge support from the International Space Science Institute
(ISSI) to the Team 314 on "Large-Amplitude Oscillation in prominences"
led by M. Luna.
NR 18
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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 SEP
PY 2016
VL 593
AR A64
DI 10.1051/0004-6361/201628845
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4HU
UT WOS:000385820100124
ER
PT J
AU Montesinos, B
Eiroa, C
Krivov, AV
Marshall, JP
Pilbratt, GL
Liseau, R
Mora, A
Maldonado, J
Wolf, S
Ertel, S
Bayo, A
Augereau, JC
Heras, AM
Fridlund, M
Danchi, WC
Solano, E
Kirchschlager, F
del Burgo, C
Montes, D
AF Montesinos, B.
Eiroa, C.
Krivov, A. V.
Marshall, J. P.
Pilbratt, G. L.
Liseau, R.
Mora, A.
Maldonado, J.
Wolf, S.
Ertel, S.
Bayo, A.
Augereau, J. -C.
Heras, A. M.
Fridlund, M.
Danchi, W. C.
Solano, E.
Kirchschlager, F.
del Burgo, C.
Montes, D.
TI Incidence of debris discs around FGK stars in the solar neighbourhood
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: late-type; circumstellar matter; protoplanetary disks; infrared:
stars
ID MAIN-SEQUENCE STARS; CA-II H; ABSOLUTE FLUX CALIBRATION; SUN-LIKE STARS;
NEARBY STARS; BOLOMETRIC CORRECTIONS; PLANET-SEARCH; FIELD STARS; HOST
STARS; COOL STARS
AB Context. Debris discs are a consequence of the planet formation process and constitute the fingerprints of planetesimal systems. Their counterparts in the solar system are the asteroid and Edgeworth-Kuiper belts.
Aims. The aim of this paper is to provide robust numbers for the incidence of debris discs around FGK stars in the solar neighbourhood.
Methods. The full sample of 177 FGK stars with d <= 20 pc proposed for the DUst around NEarby Stars (DUNES) survey is presented. Herschel/PACS observations at 100 and 160 mu m were obtained, and were complemented in some cases with data at 70 mu m and at 250, 350, and 500 mu m SPIRE photometry. The 123 objects observed by the DUNES collaboration were presented in a previous paper. The remaining 54 stars, shared with the Disc Emission via a Bias-free Reconnaissance in IR and Sub-mm (DEBRIS) consortium and observed by them, and the combined full sample are studied in this paper. The incidence of debris discs per spectral type is analysed and put into context together with other parameters of the sample, like metallicity, rotation and activity, and age.
Results. The subsample of 105 stars with d <= 15 pc containing 23 F, 33 G, and 49 K stars is complete for F stars, almost complete for G stars, and contains a substantial number of K stars from which we draw solid conclusions on objects of this spectral type. The incidence rates of debris discs per spectral type are 0.26(-0.14)(+0.21) (6 objects with excesses out of 23 F stars), 0.21(-0.11)(+0.17) (7 out of 33 G stars), and 0.20(-0.09)(+0.14) (10 out of 49 K stars); the fraction for all three spectral types together is 0.22(-0.07)(+0.08) (23 out of 105 stars). The uncertainties correspond to a 95% confidence level. The medians of the upper limits of L-dust/L-* for each spectral type are 7.8 x 10(-7) (F), 1.4 x 10(-6) (G), and 2.2 x 10(-6) (K); the lowest values are around 4.0 x 10(-7). The incidence of debris discs is similar for active (young) and inactive (old) stars. The fractional luminosity tends to drop with increasing age, as expected from collisional erosion of the debris belts.
C1 [Montesinos, B.; Solano, E.] CSIC INTA, Ctr Astrobiol CAB, Dept Astrofis, ESAC Campus,Camino Bajo Castillo S-N, Madrid 28692, Spain.
[Eiroa, C.] Univ Autonoma Madrid, Fac Ciencias, Dept Fis Teor, Modulo 15,Campus Cantoblanco, E-28049 Madrid, Spain.
[Montesinos, B.; Eiroa, C.] UAM, Unidad Asociada CAB, Madrid, Spain.
[Krivov, A. V.] Univ Jena, Astrophys Inst & Univ, Schillergasschen 2-3, D-07745 Jena, Germany.
[Marshall, J. P.] UNSW Australia, Sch Phys, Sydney, NSW 2052, Australia.
[Marshall, J. P.] UNSW Australia, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia.
[Pilbratt, G. L.; Heras, A. M.] European Space Res & Technol Ctr ESTEC SCIS, Sci Support Off, Directorate Sci, ESA, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands.
[Liseau, R.; Fridlund, M.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden.
[Mora, A.] ESA ESAC Gaia SOC, POB 78, Madrid 28691, Spain.
INAF, Osservatorio Astron Palermo, Piazza Parlamento 1, I-90134 Palermo, Italy.
[Wolf, S.; Kirchschlager, F.] Univ Kiel, Inst Theoret Phys & Astrophys, Leibnizstr 15, D-24118 Kiel, Germany.
[Ertel, S.] Univ Arizona, Dept Astron, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.
[Bayo, A.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Av Gran Bretana 1111,5030 Casilla, Valparaiso, Chile.
[Bayo, A.] Univ Valparaiso, ICM Nucleus Protoplanetary Disks, Av Gran Bretana 1111, Valparaiso 2360102, Chile.
[Augereau, J. -C.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.
[Augereau, J. -C.] CNRS, IPAG, F-38000 Grenoble, France.
[Fridlund, M.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
[Danchi, W. C.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys, Code 667, Greenbelt, MD 20771 USA.
[Solano, E.] CSIC INTA, Ctr Astrobiol CAB, Spanish Virtual Observ, ESAC Campus,Camino Bajo Castillo S-N, Madrid 28692, Spain.
[del Burgo, C.] Inst Nacl Astrofis Opt & Electr, Luis Enrique Erro 1, Puebla, Mexico.
[Montes, D.] Univ Complutense Madrid, Fac Ciencias Fis, Dept Astrofis, E-28040 Madrid, Spain.
RP Montesinos, B (reprint author), CSIC INTA, Ctr Astrobiol CAB, Dept Astrofis, ESAC Campus,Camino Bajo Castillo S-N, Madrid 28692, Spain.; Montesinos, B (reprint author), UAM, Unidad Asociada CAB, Madrid, Spain.
EM benjamin.montesinos@cab.inta-csic.es
RI Solano, Enrique/C-2895-2017; Montesinos, Benjamin/C-3493-2017;
OI Montesinos, Benjamin/0000-0002-7982-2095; Montes,
David/0000-0002-7779-238X
FU Spanish grant [AYA2013-45347-P]; DFG [KR 2164/13-1, KR 2164/15-1, WO
857/151]; UNSW Vice-Chancellor's postdoctoral fellowship; Proyecto
Fondecyt de Iniciacion [11140572]; PNP; CNES; Mexican CONACyT
[CB-2012-183007]; [AYA2011-26202]
FX The authors are grateful to the referee for the careful revision of the
original manuscript, and for the comments and suggestions. We also thank
Francisco Galindo, Mauro Lopez del Fresno, and Pablo Riviere for their
valuable help. B. Montesinos and C. Eiroa are supported by Spanish grant
AYA2013-45347-P; they and J.P. Marshall and J. Maldonado were supported
by grant AYA2011-26202. A.V. Krivov acknowledges the DFG support under
contracts KR 2164/13-1 and KR 2164/15-1. J.P. Marshall is supported by a
UNSW Vice-Chancellor's postdoctoral fellowship. R. Liseau thanks the
Swedish National Space Board for its continued support. A. Bayo
acknowledges financial support from the Proyecto Fondecyt de Iniciacion
11140572 and scientific support from the Millenium Science Initiative,
Chilean Ministry of Economy, Nucleus RC130007. J.-C. Augereau
acknowledges support from PNP and CNES. F. Kirchschlager thanks the DFG
for finantial support under contract WO 857/151. C. del Burgo has been
supported by Mexican CONACyT research grant CB-2012-183007.
NR 95
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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 SEP
PY 2016
VL 593
AR A51
DI 10.1051/0004-6361/201628329
PG 31
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4HU
UT WOS:000385820100058
ER
PT J
AU Muller, C
Burd, PR
Schulz, R
Coppejans, R
Falcke, H
Intema, H
Kadler, M
Krauss, F
Ojha, R
AF Mueller, C.
Burd, P. R.
Schulz, R.
Coppejans, R.
Falcke, H.
Intema, H.
Kadler, M.
Krauss, F.
Ojha, R.
TI The MHz-peaked radio spectrum of the unusual gamma-ray source
PMNJ1603-4904
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Letter
DE galaxies: active; galaxies: jets; galaxies: individual: PMN J1603-4904
ID LARGE-AREA TELESCOPE; COMPACT STEEP-SPECTRUM; ACTIVE GALACTIC NUCLEI;
FREE-FREE ABSORPTION; SOURCE CATALOG; SYMMETRIC OBJECTS; EVOLUTION;
YOUNG; EMISSION; GALAXIES
AB Context. The majority of bright extragalactic gamma-ray sources are blazars. Only a few radio galaxies have been detected by Fermi/LAT. Recently, the GHz-peaked spectrum source PKS 1718-649 was confirmed to be gamma-ray bright, providing further evidence for the existence of a population of gamma-ray loud, compact radio galaxies. A spectral turnover in the radio spectrum in the MHz to GHz range is a characteristic feature of these objects, which are thought to be young due to their small linear sizes. The multiwavelength properties of the gamma-ray source PMNJ1603-4904 suggest that it is a member of this source class.
Aims. The known radio spectrum of PMNJ1603-4904 can be described by a power law above 1 GHz. Using observations from the Giant Metrewave Radio Telescope (GMRT) at 150, 325, and 610 MHz, we investigate the behavior of the spectrum at lower frequencies to search for a low-frequency turnover.
Methods. Data from the TIFR GMRT Sky Survey (TGSS ADR) catalog and archival GMRT observations were used to construct the first MHz to GHz spectrum of PMNJ1603-4904.
Results. We detect a low-frequency turnover of the spectrum and measure the peak position at about 490 MHz (rest-frame), which, using the known relation of peak frequency and linear size, translates into a maximum linear source size of similar to 1.4 kpc.
Conclusions. The detection of the MHz peak indicates that PMNJ1603-4904 is part of this population of radio galaxies with turnover frequencies in the MHz to GHz regime. Therefore it can be considered the second confirmed object of this kind detected in gamma-rays. Establishing this gamma-ray source class will help to investigate the gamma-ray production sites and to test broadband emission models.
C1 [Mueller, C.; Coppejans, R.; Falcke, H.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands.
[Burd, P. R.; Kadler, M.] Univ Wurzburg, Inst Theoret Phys & Astrophys, Hubland, D-97074 Wurzburg, Germany.
[Schulz, R.] ASTRON, Netherlands Inst Radio Astron, Postbus 2, NL-7990 AA Dwingeloo, Netherlands.
[Intema, H.] Leiden Univ, Leiden Observ, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands.
[Krauss, F.] Univ Amsterdam, GRAPPA, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.
[Krauss, F.] Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.
[Ojha, R.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 661, Greenbelt, MD 20771 USA.
[Ojha, R.] CRESST Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Ojha, R.] Catholic Univ Amer, Washington, DC 20064 USA.
RP Muller, C (reprint author), Radboud Univ Nijmegen, Dept Astrophys IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands.
EM cmueller@astro.ru.nl
NR 51
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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 SEP
PY 2016
VL 593
AR L19
DI 10.1051/0004-6361/201629547
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4HU
UT WOS:000385820100159
ER
PT J
AU Werner, K
Rauch, T
Kruk, JW
AF Werner, K.
Rauch, T.
Kruk, J. W.
TI The far-ultraviolet spectra of two hot PG1159 stars
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: abundances; stars: atmospheres; stars: evolution; stars: AGB and
post-AGB; white dwarfs
ID PRE-WHITE-DWARFS; TO-OXYGEN RATIO; POST-AGB STARS; PLANETARY-NEBULAE;
INTERSTELLAR-MEDIUM; ATOMIC DATABASE; IRON ABUNDANCE; LINES;
SPECTROSCOPY; MODEL
AB PG 115(stars are hot, hydrogen-deficient (pre-) white dwarfs with atmospheres mainly composed of helium, carbon, and oxygen. The unusual surface chemistry is the result of a late helium-shell flash. Observed element abundances enable us to test stellar evolution models quantitatively with respect to their nucleosynthesis products formed near the helium-burning shell of the progenitor asymptotic giant branch stars. Because of the high effective temperatures (T-eff), abundance determinations require ultraviolet spectroscopy and non-local thermodynamic equilibrium model atmosphere analyses. Up to now, we have presented results for the prototype of this spectral class and two cooler members (T-eff in the range 85 000-140 000 K). Here we report on the results for two even hotter stars (PG 1520 + 525 and PG 1144 + 005, both with T-eff = 150 000 K) which are the only two objects in this temperature-gravity region for which useful far-ultraviolet spectra are available, and revisit the prototype star. Previous results on the abundances of some species are confirmed, while results on others (Si, P, S) are revised. In particular, a solar abundance of sulphur is measured in contrast to earlier claims of a strong S deficiency that contradicted stellar evolution models. For the first time, we assess the abundances of Na, Al, and Cl with newly constructed non-LTE model atoms. Besides the main constituents (He, C, O), we determine the abundances (or upper limits) of N, F, Ne, Na, Al, Si, P, S, Cl, Ar, and Fe. Generally, good agreement with stellar models is found.
C1 [Werner, K.; Rauch, T.] Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany.
[Kruk, J. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Werner, K (reprint author), Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany.
EM werner@astro.uni-tuebingen.de
FU German Aerospace Center (DLR) [50 OR 1507]
FX We thank Amanda Karakas and Luke Shingles for reporting unpublished
results to us. T. Rauch is supported by the German Aerospace Center
(DLR) under grant 50 OR 1507. The TMAD service
(http://astro-uni-tuebingen.de/similar to TMAD) used to compile atomic
data for this paper was constructed as part of the activities of the
German Astrophysical Virtual Observatory. This research has made use of
the SIMBAD database, operated at CDS, Strasbourg, France, and of NASA's
Astrophysics Data System Bibliographic Services. Some of the data
presented in this paper were obtained from the Mikulski Archive for
Space Telescopes (MAST). This work had been done using the profile
fitting procedure OWENS, developed by M. Lemoine and the FUSE French
Team.
NR 48
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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 SEP
PY 2016
VL 593
AR A104
DI 10.1051/0004-6361/201628892
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4HU
UT WOS:000385820100130
ER
PT J
AU Hopkins, FM
Ehleringer, JR
Bush, SE
Duren, RM
Miller, CE
Lai, CT
Hsu, YK
Carranza, V
Randerson, JT
AF Hopkins, Francesca M.
Ehleringer, James R.
Bush, Susan E.
Duren, Riley M.
Miller, Charles E.
Lai, Chun-Ta
Hsu, Ying-Kuang
Carranza, Valerie
Randerson, James T.
TI Mitigation of methane emissions in cities: How new measurements and
partnerships can contribute to emissions reduction strategies
SO EARTHS FUTURE
LA English
DT Article
ID GREENHOUSE-GAS EMISSIONS; WASTE-WATER TREATMENT; MUNICIPAL SOLID-WASTE;
CLIMATE-CHANGE ACTION; NATURAL-GAS; CARBON-DIOXIDE; UNITED-STATES;
NITROUS-OXIDE; LOS-ANGELES; PIPELINE LEAKS
AB Cities generate 70% of anthropogenic greenhouse gas emissions, a fraction that is growing with global urbanization. While cities play an important role in climate change mitigation, there has been little focus on reducing urban methane (CH4) emissions. Here, we develop a conceptual framework for CH4 mitigation in cities by describing emission processes, the role of measurements, and a need for new institutional partnerships. Urban CH4 emissions are likely to grow with expanding use of natural gas and organic waste disposal systems in growing population centers; however, we currently lack the ability to quantify this increase. We also lack systematic knowledge of the relative contribution of these distinct source sectors on emissions. We present new observations from four North American cities to demonstrate that CH4 emissions vary in magnitude and sector from city to city and hence require different mitigation strategies. Detections of fugitive emissions from these systems suggest that current mitigation approaches are absent or ineffective. These findings illustrate that tackling urban CH4 emissions will require research efforts to identify mitigation targets, develop and implement new mitigation strategies, and monitor atmospheric CH4 levels to ensure the success of mitigation efforts. This research will require a variety of techniques to achieve these objectives and should be deployed in cities globally. We suggest that metropolitan scale partnerships may effectively coordinate systematic measurements and actions focused on emission reduction goals.
C1 [Hopkins, Francesca M.; Randerson, James T.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Hopkins, Francesca M.; Duren, Riley M.; Miller, Charles E.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
[Ehleringer, James R.; Bush, Susan E.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA.
[Ehleringer, James R.] Univ Utah, Global Change & Sustainabil Ctr, Salt Lake City, UT USA.
[Lai, Chun-Ta] San Diego State Univ, Dept Biol, San Diego, CA 92182 USA.
[Hsu, Ying-Kuang] Calif Air Resources Board, Monitoring & Lab Div, Sacramento, CA USA.
[Carranza, Valerie] Univ Calif Los Angeles, Environm Sci, Los Angeles, CA USA.
RP Hopkins, FM (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.; Hopkins, FM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM francesca.m.hopkins@jpl.nasa.gov
FU U.S. Department of Energy Office of Science (BER) [DE-SC0005266]; NASA
Postdoctoral Program fellowship; NASA
FX This study was supported by U.S. Department of Energy Office of Science
(BER), Grant No. DE-SC0005266. F.M.H. also acknowledges support from a
NASA Postdoctoral Program fellowship. We thank Liz Wiggins, Gergana
Mouteva, Massimo Lupascu, Clayton Elder, Nicky Cuozzo, Ashley Braunthal,
Joshua Miu, and Simon Fahrni for collecting Fairbanks data, Joshua Rambo
for collecting San Diego data, and Bill Johnson for thermal camera
images. Portions of this work were performed at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with
NASA. The data used are listed in the references, tables, figures, and
supplement. Raw data are available by contacting
francesca.m.hopkins@jpl.nasa.gov.
NR 123
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U1 11
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PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 2328-4277
J9 EARTHS FUTURE
JI Earth Future
PD SEP
PY 2016
VL 4
IS 9
BP 408
EP 425
DI 10.1002/2016EF000381
PG 18
WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric
Sciences
GA EC0BB
UT WOS:000387761400001
ER
PT J
AU Verma, M
Fisher, JB
Mallick, K
Ryu, Y
Kobayashi, H
Guillaume, A
Moore, G
Ramakrishnan, L
Hendrix, V
Wolf, S
Sikka, M
Kiely, G
Wohlfahrt, G
Gielen, B
Roupsard, O
Toscano, P
Arain, A
Cescatti, A
AF Verma, Manish
Fisher, Joshua B.
Mallick, Kaniska
Ryu, Youngryel
Kobayashi, Hideki
Guillaume, Alexandre
Moore, Gregory
Ramakrishnan, Lavanya
Hendrix, Valerie
Wolf, Sebastian
Sikka, Munish
Kiely, Gerard
Wohlfahrt, Georg
Gielen, Bert
Roupsard, Olivier
Toscano, Piero
Arain, Altaf
Cescatti, Alessandro
TI Global Surface Net-Radiation at 5 km from MODIS Terra
SO REMOTE SENSING
LA English
DT Article
DE surface net-radiation; MODIS; FLUXNET; SURFRAD; modeling; validation
ID DOWNWELLING LONGWAVE RADIATION; CLEAR-SKY DAYS; HETEROGENEOUS LANDSCAPE;
LAND; EVAPOTRANSPIRATION; VALIDATION; ATMOSPHERE; FLUX; ALGORITHMS;
PRODUCT
AB Reliable and fine resolution estimates of surface net-radiation are required for estimating latent and sensible heat fluxes between the land surface and the atmosphere. However, currently, fine resolution estimates of net-radiation are not available and consequently it is challenging to develop multi-year estimates of evapotranspiration at scales that can capture land surface heterogeneity and are relevant for policy and decision-making. We developed and evaluated a global net-radiation product at 5 km and 8-day resolution by combining mutually consistent atmosphere and land data from the Moderate Resolution Imaging Spectroradiometer (MODIS) on board Terra. Comparison with net-radiation measurements from 154 globally distributed sites (414 site-years) from the FLUXNET and Surface Radiation budget network (SURFRAD) showed that the net-radiation product agreed well with measurements across seasons and climate types in the extratropics (Wilmott's index ranged from 0.74 for boreal to 0.63 for Mediterranean sites). Mean absolute deviation between the MODIS and measured net-radiation ranged from 38.0 +/- 1.8 W.m(-2) in boreal to 72.0 +/- 4.1 W.m(-2) in the tropical climates. The mean bias was small and constituted only 11%, 0.7%, 8.4%, 4.2%, 13.3%, and 5.4% of the mean absolute error in daytime net-radiation in boreal, Mediterranean, temperate-continental, temperate, semi-arid, and tropical climate, respectively. To assess the accuracy of the broader spatiotemporal patterns, we upscaled error-quantified MODIS net-radiation and compared it with the net-radiation estimates from the coarse spatial (1 degrees x 1 degrees) but high temporal resolution gridded net-radiation product from the Clouds and Earth's Radiant Energy System (CERES). Our estimates agreed closely with the net-radiation estimates from the CERES. Difference between the two was less than 10 W center dot m(-2) in 94% of the total land area. MODIS net-radiation product will be a valuable resource for the science community studying turbulent fluxes and energy budget at the Earth's surface.
C1 [Verma, Manish; Fisher, Joshua B.; Guillaume, Alexandre; Moore, Gregory; Sikka, Munish] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Mallick, Kaniska] LIST, Dept Environm Res & Innovat ERIN, L-4422 Belvaux, Luxembourg.
[Ryu, Youngryel] Seoul Natl Univ, Dept Landscape Architecture & Rural Syst Engn, Seoul 151921, South Korea.
[Kobayashi, Hideki] Japan Agcy Marine Earth Sci & Technol, Yokohama, Kanagawa 2360001, Japan.
[Ramakrishnan, Lavanya; Hendrix, Valerie] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA.
[Wolf, Sebastian] Swiss Fed Inst Technol, Dept Environm Syst Sci, CH-8092 Zurich, Switzerland.
[Kiely, Gerard] Univ Coll, Environm Res Inst, Civil & Environm Engn Dept, Cork T12P2FY, Ireland.
[Wohlfahrt, Georg] Univ Innsbruck, Inst Ecol, Sternwartestr 15, A-6020 Innsbruck, Austria.
[Gielen, Bert] Univ Antwerp, Dept Biol, Res Grp Plant & Vegetat Ecol, B-2610 Antwerp, Belgium.
[Roupsard, Olivier] CIRAD, UMR Eco & Sols Ecol Fonct Biogeochim Sols & Agroe, F-34000 Montpellier, France.
[Roupsard, Olivier] CATIE Trop Agr Ctr Res & Higher Educ, Turrialba 937170, Costa Rica.
[Toscano, Piero] CNR, Inst Biometeorol IBIMET, Via G Caproni 8, I-50145 Florence, Italy.
[Arain, Altaf] McMaster Univ, McMaster Ctr Climate Change, Sch Geog & Earth Sci, 1280 Main St West, Hamilton, ON L8S 4K1, Canada.
[Cescatti, Alessandro] European Commiss, Joint Res Ctr, Directorate Sustainable Resources, I-21027 Ispra, Italy.
RP Verma, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM manishve@umich.edu; Joshua.B.Fisher@jpl.nasa.gov;
kaniska.mallick@gmail.com; ryuyr77@gmail.com; hkoba@jamstec.go.jp;
alexandre.guillaume@jpl.nasa.gov; Gregory.J.Moore@jpl.nasa.gov;
LRamakrishnan@lbl.gov; vchendrix@lbl.gov; sewolf@ethz.ch;
Munish.Sikka@jpl.nasa.gov; g.kiely@ucc.ie; Georg.Wohlfahrt@uibk.ac.at;
bert.gielen@uantwerpen.be; olivier.roupsard@cirad.fr;
p.toscano@ibimet.cnr.it; arainm@mcmaster.ca;
alessandro.cescatti@jrc.ec.europa.eu
RI Wohlfahrt, Georg/D-2409-2009; Wolf, Sebastian/B-4580-2010;
OI Wohlfahrt, Georg/0000-0003-3080-6702; Wolf,
Sebastian/0000-0001-7717-6993; Toscano, Piero/0000-0001-9184-0707;
Mallick, Kaniska/0000-0002-2735-930X; Fisher, Joshua/0000-0003-4734-9085
FU NASA Terrestrial Hydrology Program; Jet Propulsion Laboratory Strategic
Research & Technology Development Climate Initiative; U.S. Department of
Energy, Biological and Environmental Research, Terrestrial Carbon
Program [DE-FG02-04ER63917, DE-FG02-04ER63911]; AfriFlux; AsiaFlux;
CarboAfrica; CarboEuropeIP; CarboItaly; CarboMont; ChinaFlux;
Fluxnet-Canada; CFCAS; NSERC; BIOCAP; Environment Canada; NRCan;
GreenGrass; KoFlux; LBA; NECC; OzFlux; TCOS-Siberia; USCCC; Australian
Research Council [DP0451247, DP0344744, DP0772981, DP130101566];
European Commission [300083]
FX Support for this study was provided by the NASA Terrestrial Hydrology
Program and Jet Propulsion Laboratory Strategic Research & Technology
Development Climate Initiative. The research was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
Copyright 2015 California Institute of Technology. Government
sponsorship acknowledged. This work used net-radiation 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)), AfriFlux, AsiaFlux, CarboAfrica, CarboEuropeIP,
CarboItaly, CarboMont, ChinaFlux, Fluxnet-Canada (supported by CFCAS,
NSERC, BIOCAP, Environment Canada, and NRCan), GreenGrass, KoFlux, LBA,
NECC, OzFlux, TCOS-Siberia, USCCC. The authors gratefully acknowledge
the efforts of the FLUXNET community to compile and make available the
La Thuile data set. Data from AU-Fog-Fogg Dam, AU-How-Howard Springs,
AU-Wac-Wallaby Creek was funded by the Australian Research Council
(DP0451247, DP0344744, DP0772981 and DP130101566). Support for
collection and archiving was provided through the Australia Terrestrial
Ecosystem Research Network (TERN) (http://www.tern.org.au). SW was
supported by the European Commission with a Marie Curie International
Outgoing Fellowship (grant 300083).
NR 61
TC 0
Z9 0
U1 7
U2 7
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 SEP
PY 2016
VL 8
IS 9
AR UNSP 739
DI 10.3390/rs8090739
PG 20
WC Remote Sensing
SC Remote Sensing
GA DY9XB
UT WOS:000385488000049
ER
PT J
AU Wang, XJ
Key, J
Kwok, R
Zhang, JL
AF Wang, Xuanji
Key, Jeffrey
Kwok, Ron
Zhang, Jinlun
TI Comparison of Arctic Sea Ice Thickness from Satellites, Aircraft, and
PIOMAS Data
SO REMOTE SENSING
LA English
DT Article
DE sea ice thickness; Arctic; remote sensing; satellite; ICESat; CryoSat-2;
SMOS; IceBridge; PIOMAS; APP-x
ID SNOW DEPTH; OPERATION ICEBRIDGE; MODEL; RETRIEVAL; FREEBOARD; ALGORITHM;
CLOUD
AB In this study, six Arctic sea ice thickness products are compared: the AVHRR Polar Pathfinder-extended (APP-x), ICESat, CryoSat-2, SMOS, NASA IceBridge aircraft flights, and the Pan-Arctic Ice Ocean Modeling and Assimilation System (PIOMAS). The satellite products are based on three different retrieval methods: an energy budget approach, measurements of ice freeboard, and the relationship between passive microwave brightness temperatures and thin ice thickness. Inter-comparisons are done for the periods of overlap from 2003 to 2013. Results show that ICESat sea ice is thicker than APP-x and PIOMAS overall, particularly along the north coast of Greenland and Canadian Archipelago. The relative differences of APP-x and PIOMAS with ICESat are -0.48 m and -0.31 m, respectively. APP-x underestimates thickness relative to CryoSat-2, with a mean difference of -0.19 m. The biases for APP-x, PIOMAS, and CryoSat-2 relative to IceBridge thicknesses are 0.18 m, 0.18 m, and 0.29 m. The mean difference between SMOS and CryoSat-2 for 0 similar to 1 m thick ice is 0.13 m in March and -0.24 m in October. All satellite-retrieved ice thickness products and PIOMAS overestimate the thickness of thin ice (1 m or less) compared to IceBridge for which SMOS has the smallest bias (0.26 m). The spatial correlation between the datasets indicates that APP-x and PIOMAS are the most similar, followed by APP-x and CryoSat-2.
C1 [Wang, Xuanji] UW Madison, CIMSS, SSEC, Madison, WI 53706 USA.
[Key, Jeffrey] NOAA NESDIS, Ctr Satellite Applicat & Res, Madison, WI 53706 USA.
[Kwok, Ron] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Zhang, Jinlun] Univ Washington, Appl Phys Lab, Polar Sci Ctr, 1013 NE 40th St, Seattle, WA 98105 USA.
RP Wang, XJ (reprint author), UW Madison, CIMSS, SSEC, Madison, WI 53706 USA.
EM xuanjiw@ssec.wisc.edu; jeff.key@noaa.gov; ronald.kwok@jpl.nasa.gov;
zhang@apl.washington.edu
OI Wang, Xuanji/0000-0002-5893-758X; Key, Jeffrey/0000-0001-6109-3050
FU JPSS Program Office; GOES-R Program Office; National Science Foundation
[ARC-1023371]; NASA Cryosphere Program [NNX15AG68G]
FX This work was supported by the JPSS Program Office, the GOES-R Program
Office, the National Science Foundation (ARC-1023371), and the NASA
Cryosphere Program (NNX15AG68G). We thank the Alfred Wegener
Institute/Helmholtz Centre for Polar and Marine Research and the
European Space Agency for making the Cryosat-2 ice thickness product
available to the scientific community, the University of Hamburg for the
SMOS ice thicknesses, and the National Snow and Ice Data Center and NASA
for the IceBridge data. The views, opinions, and findings contained in
this report are those of the author(s) and should not be construed as an
official National Oceanic and Atmospheric Administration or U.S.
Government position, policy, or decision.
NR 31
TC 2
Z9 2
U1 6
U2 6
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 SEP
PY 2016
VL 8
IS 9
AR 713
DI 10.3390/rs8090713
PG 17
WC Remote Sensing
SC Remote Sensing
GA DY9XB
UT WOS:000385488000023
ER
PT J
AU Meier, MM
Matthia, D
Forkert, T
Wirtz, M
Scheibinger, M
Hubel, R
Mertens, CJ
AF Meier, Matthias M.
Matthiae, Daniel
Forkert, Tomas
Wirtz, Michael
Scheibinger, Markus
Huebel, Robert
Mertens, Christopher J.
TI RaD-X: Complementary measurements of dose rates at aviation altitudes
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID GALACTIC COSMIC-RAYS; CALIBRATION; MODEL; DOSIMETERS
AB The RaD-X stratospheric balloon flight organized by the National Aeronautics and Space Administration was launched from Fort Sumner on 25 September 2015 and carried several instruments to measure the radiation field in the upper atmosphere at the average vertical cutoff rigidity R-c of 4.1 GV. The German Aerospace Center (Deutsches Zentrum fur Luft-und Raumfahrt) in cooperation with Lufthansa German Airlines supported this campaign with an independent measuring flight at the altitudes of civil aviation on a round trip from Germany to Japan. The goal was to measure dose rates under similar space weather conditions over an area on the Northern Hemisphere opposite to the RaD-X flight. Dose rates were measured in the target areas, i.e., around vertical cutoff rigidity Rc of 4.1 GV, at two flight altitudes for about 1 h at each position with acceptable counting statistics. The analysis of the space weather situation during the flights shows that measuring data were acquired under stable and moderate space weather conditions with a virtually undisturbed magnetosphere. The measured rates of absorbed dose in silicon and ambient dose equivalent complement the data recorded during the balloon flight. The combined measurements provide a set of experimental data suitable for validating and improving numerical models for the calculation of radiation exposure at aviation altitudes.
C1 [Meier, Matthias M.; Matthiae, Daniel; Forkert, Tomas; Wirtz, Michael] Inst Aerosp Med, German Aerosp Ctr, Cologne, Germany.
[Scheibinger, Markus; Huebel, Robert] Lufthansa German Airlines, Lufthansa Basis, Frankfurt, Germany.
[Mertens, Christopher J.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Meier, MM (reprint author), Inst Aerosp Med, German Aerosp Ctr, Cologne, Germany.
EM Matthias.Meier@dlr.de
OI Matthia, Daniel/0000-0003-1507-0143
FU Lufthansa German Airlines
FX We would like to especially express our gratitude to Lufthansa German
Airlines for their support during the preparation and performance of the
measuring flights. Furthermore, we would like to thank the Sodankyla
Geophysical Observatory and the website team (http://cosmicrays.oulu.fi)
for providing the Oulu neutron monitor data. The flight data are
available from the German Aerospace Center upon request.
NR 19
TC 3
Z9 3
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 SEP
PY 2016
VL 14
IS 9
BP 689
EP 694
DI 10.1002/2016SW001418
PG 6
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA EC0PE
UT WOS:000387802300006
ER
PT J
AU Kannawadi, A
Shapiro, CA
Mandelbaum, R
Hirata, CM
Kruk, JW
Rhodes, JD
AF Kannawadi, Arun
Shapiro, Charles A.
Mandelbaum, Rachel
Hirata, Christopher M.
Kruk, Jeffrey W.
Rhodes, Jason D.
TI The Impact of Interpixel Capacitance in CMOS Detectors on PSF Shapes and
Implications for WFIRST
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
DE instrumentation: detectors; instrumentation: high angular resolution
ID DARK-MATTER HALOES; COSMOLOGICAL PARAMETER CONSTRAINTS; IMAGE
COMBINATION; LARGE SCALES; SDSS DR7; WEAK; CFHTLENS; CONNECTION;
EVOLUTION; GALAXIES
AB Unlike optical CCDs, near-infrared detectors, which are based on CMOS hybrid readout technology, typically suffer from electrical crosstalk between the pixels. The interpixel capacitance (IPC) responsible for the crosstalk affects the point-spread function (PSF) of the telescope, increasing the size and modifying the shape of all objects in the images while correlating the Poisson noise. Upcoming weak lensing surveys that use these detectors, such as WFIRST, place stringent requirements on the PSF size and shape (and the level at which these are known), which in turn must be translated into requirements on IPC. To facilitate this process, we present a first study of the effect of IPC on WFIRST PSF sizes and shapes. Realistic PSFs are forward-simulated from physical principles for each WFIRST bandpass. We explore how the PSF size and shape depends on the range of IPC coupling with pixels that are connected along an edge or corner; for the expected level of IPC in WFIRST, IPC increases the PSF sizes by similar to 5%. We present a linear fitting formula that describes the uncertainty in the PSF size or shape due to uncertainty in the IPC, which could arise for example due to unknown time evolution of IPC as the detectors age or due to spatial variation of IPC across the detector. We also study of the effect of a small anisotropy in the IPC, which further modifies the PSF shapes. Our results are a first, critical step in determining the hardware and characterization requirements for the detectors used in the WFIRST survey.
C1 [Kannawadi, Arun; Mandelbaum, Rachel] Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA.
[Shapiro, Charles A.; Rhodes, Jason D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Hirata, Christopher M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, 191 West Woodruff Lane, Columbus, OH 43210 USA.
[Kruk, Jeffrey W.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Rhodes, Jason D.] CALTECH, Pasadena, CA 91125 USA.
RP Kannawadi, A (reprint author), Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA.
EM arunkannawadi@cmu.edu
RI Mandelbaum, Rachel/N-8955-2014
OI Mandelbaum, Rachel/0000-0003-2271-1527
FU WFIRST study office; US Department of Energy; Packard Foundation; Simons
Foundation
FX The authors thank Roger Smith, Bernard Rauscher, and Andres Plazas
Malagon for many useful discussions and Mike Jarvis and Joshua Meyers
for their inputs in developing the GalSim WFIRST module. We thank Edward
Cheng of Conceptual Analytics for his comments in improving the
manuscript and the referee, David Spergel, for correcting a few minor
errors in the original version of the manuscript. This work was carried
out in part at the Jet Propulsion Laboratory (JPL), a NASA center run by
California Institute of Technology. The authors acknowledge funding from
WFIRST study office. CMH is supported by the US Department of Energy,
the Packard Foundation, and the Simons Foundation.
NR 49
TC 1
Z9 1
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6280
EI 1538-3873
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD SEP
PY 2016
VL 128
IS 967
AR 095001
DI 10.1088/1538-3873/128/967/095001
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EB1LK
UT WOS:000387113200007
ER
PT J
AU Nguyen, HT
Zemcov, M
Battle, J
Bock, JJ
Hristov, V
Korngut, P
Meek, A
AF Nguyen, Hien T.
Zemcov, Michael
Battle, John
Bock, James J.
Hristov, Viktor
Korngut, Phillip
Meek, Andrew
TI Spatial and Temporal Stability of Airglow Measured in the Meinel Band
Window at 1191.3 nm
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
DE atmospheric effects; site testing; techniques: imaging spectroscopy
ID BACKGROUND-EXPERIMENT CIBER; SKY BRIGHTNESS; EMISSION; FLUCTUATIONS;
SUPPRESSION; ATMOSPHERE; MODEL; LINES
AB We report on the temporal and spatial fluctuations in the atmospheric brightness in the narrow band between Meinel emission lines at 1191.3 nm using a lambda/Delta lambda = 320 near-infrared instrument. We present the instrument design and implementation, followed by a detailed analysis of data taken over the course of a night from Table Mountain Observatory. At low airmasses, the absolute sky brightness at this wavelength is found to be 5330 +/- 30 nW m(-2) sr(-1), consistent with previous measurements of the inter-band airglow at these wavelengths. This amplitude is larger than simple models of the continuum component of the airglow emission at these wavelengths, confirming that an extra emissive or scattering component is required to explain the observations. We perform a detailed investigation of the noise properties of the data and find no evidence for a noise component associated with temporal instability in the inter-line continuum. This result demonstrates that in several hours of similar to 100 s integrations the noise performance of the instrument does not appear to significantly degrade from expectations, giving a proof of concept that near-infrared line intensity mapping may be feasible from ground-based sites.
C1 [Nguyen, Hien T.; Zemcov, Michael; Bock, James J.; Korngut, Phillip] NASA, JPL, Pasadena, CA 91109 USA.
[Nguyen, Hien T.; Zemcov, Michael; Battle, John; Bock, James J.; Hristov, Viktor; Korngut, Phillip; Meek, Andrew] CALTECH, Dept Phys Math & Astron, Pasadena, CA 91125 USA.
RP Nguyen, HT (reprint author), NASA, JPL, Pasadena, CA 91109 USA.; Nguyen, HT (reprint author), CALTECH, Dept Phys Math & Astron, Pasadena, CA 91125 USA.
EM htnguyen@jpl.nasa.gov
FU JPL Research and Technology Development Fund; National Aeronautics and
Space Administration; National Science Foundation
FX The authors wish to thank Jaime Luna for his help designing the LAMP
mechanical assembly, Heath Rhoades at JPL's Table Mountain Observatory
for his assistance setting up the instrument and guidance using the 24
'' telescope, and the Gemini Observatory for making their sky model
tables public. The development of LAMP was supported by the JPL Research
and Technology Development Fund. 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.
NR 26
TC 0
Z9 0
U1 1
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6280
EI 1538-3873
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD SEP
PY 2016
VL 128
IS 967
AR 094504
DI 10.1088/1538-3873/128/967/094504
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EB1LK
UT WOS:000387113200006
ER
PT J
AU Stevenson, KB
Lewis, NK
Bean, JL
Beichman, C
Fraine, J
Kilpatrick, BM
Krick, JE
Lothringer, JD
Mandell, AM
Valenti, JA
Agol, E
Angerhausen, D
Barstow, JK
Birkmann, SM
Burrows, A
Charbonneau, D
Cowan, NB
Crouzet, N
Cubillos, PE
Curry, SM
Dalba, PA
de Wit, J
Deming, D
Desert, JM
Doyon, R
Dragomir, D
Ehrenreich, D
Fortney, JJ
Munoz, AG
Gibson, NP
Gizis, JE
Greene, TP
Harrington, J
Heng, K
Kataria, T
Kempton, EMR
Knutson, H
Kreidberg, L
Lafreniere, D
Lagage, PO
Line, MR
Lopez-Morales, M
Madhusudhan, N
Morley, CV
Rocchetto, M
Schlawin, E
Shkolnik, EL
Shporer, A
Sing, DK
Todorov, KO
Tucker, GS
Wakeford, HR
AF Stevenson, Kevin B.
Lewis, Nikole K.
Bean, Jacob L.
Beichman, Charles
Fraine, Jonathan
Kilpatrick, Brian M.
Krick, J. E.
Lothringer, Joshua D.
Mandell, Avi M.
Valenti, Jeff A.
Agol, Eric
Angerhausen, Daniel
Barstow, Joanna K.
Birkmann, Stephan M.
Burrows, Adam
Charbonneau, David
Cowan, Nicolas B.
Crouzet, Nicolas
Cubillos, Patricio E.
Curry, S. M.
Dalba, Paul A.
de Wit, Julien
Deming, Drake
Desert, Jean-Michel
Doyon, Rene
Dragomir, Diana
Ehrenreich, David
Fortney, Jonathan J.
Munoz, Antonio Garcia
Gibson, Neale P.
Gizis, John E.
Greene, Thomas P.
Harrington, Joseph
Heng, Kevin
Kataria, Tiffany
Kempton, Eliza M. -R.
Knutson, Heather
Kreidberg, Laura
Lafreniere, David
Lagage, Pierre-Olivier
Line, Michael R.
Lopez-Morales, Mercedes
Madhusudhan, Nikku
Morley, Caroline V.
Rocchetto, Marco
Schlawin, Everett
Shkolnik, Evgenya L.
Shporer, Avi
Sing, David K.
Todorov, Kamen O.
Tucker, Gregory S.
Wakeford, Hannah R.
TI Transiting Exoplanet Studies and Community Targets for JWST's Early
Release Science Program
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
DE planets and satellites: atmospheres; planets and satellites: individual;
telescopes
ID WEBB-SPACE-TELESCOPE; FIELD CAMERA 3; HOT JUPITERS; MIDINFRARED
INSTRUMENT; RESOLUTION SPECTROMETER; TRANSMISSION SPECTRUM; GIANT
PLANET; KEPLER FIELD; HD 149026B; WASP-SOUTH
AB The James Webb Space Telescope (JWST) will likely revolutionize transiting exoplanet atmospheric science, due to a combination of its capability for continuous, long duration observations and its larger collecting area, spectral coverage, and spectral resolution compared to existing space-based facilities. However, it is unclear precisely how well JWST will perform and which of its myriad instruments and observing modes will be best suited for transiting exoplanet studies. In this article, we describe a prefatory JWST Early Release Science (ERS) Cycle. 1 program that focuses on testing specific observing modes to quickly give the community the data and experience it needs to plan more efficient and successful transiting exoplanet characterization programs in later cycles. We propose a multi-pronged approach wherein one aspect of the program focuses on observing transits of a single target with all of the recommended observing modes to identify and understand potential systematics, compare transmission spectra at overlapping and neighboring wavelength regions, confirm throughputs, and determine overall performances. In our search for transiting exoplanets that are well suited to achieving these goals, we identify 12 objects (dubbed "community targets") that meet our defined criteria. Currently, the most favorable target is WASP-62b because of its large predicted signal size, relatively bright host star, and location in JWST's continuous viewing zone. Since most of the community targets do not have well-characterized atmospheres, we recommend initiating preparatory observing programs to determine the presence of obscuring clouds/hazes within their atmospheres. Measurable spectroscopic features are needed to establish the optimal resolution and wavelength regions for exoplanet characterization. Other initiatives from our proposed ERS program include testing the instrument brightness limits and performing phase-curve observations. The latter are a unique challenge compared to transit observations because of their significantly longer durations. Using only a single mode, we propose to observe a full-orbit phase curve of one of the previously characterized, short-orbital-period planets to evaluate the facility-level aspects of long, uninterrupted time-series observations.
C1 [Stevenson, Kevin B.; Bean, Jacob L.; Dragomir, Diana; Kreidberg, Laura] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
[Lewis, Nikole K.; Valenti, Jeff A.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Beichman, Charles] CALTECH, Jet Prop Lab, NASA Exoplanet Sci Inst, Pasadena, CA USA.
[Fraine, Jonathan; Schlawin, Everett] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Kilpatrick, Brian M.; Tucker, Gregory S.] Brown Univ, Dept Phys, Providence, RI 02912 USA.
[Krick, J. E.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91106 USA.
[Lothringer, Joshua D.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Mandell, Avi M.] NASA Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Agol, Eric] Univ Washington, Box 351580, Seattle, WA 98195 USA.
[Angerhausen, Daniel; Wakeford, Hannah R.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Barstow, Joanna K.] Univ Oxford, Dept Phys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England.
[Birkmann, Stephan M.] European Space Agcy, Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA.
[Charbonneau, David; Lopez-Morales, Mercedes] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Cowan, Nicolas B.] McGill Space Inst, 3550 Rue Univ, Montreal, PQ H3A 1A1, Canada.
[Crouzet, Nicolas] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON, Canada.
[Cubillos, Patricio E.] Austrian Acad Sci, Space Res Inst, Schmiedlstr 6, A-8042 Graz, Austria.
[Curry, S. M.] Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
[Dalba, Paul A.] Boston Univ, Dept Astron, Boston, MA 02215 USA.
[de Wit, Julien] MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Desert, Jean-Michel] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands.
[Doyon, Rene; Lafreniere, David] Univ Montreal, Dept Phys, Inst Rech Exoplanetes, CP 6128,Succ Ctr Vile, Montreal, PQ H3C 3J7, Canada.
[Ehrenreich, David] Observ Univ Geneve, 51 Chemin Maillettes, CH-1290 Versoix, Switzerland.
[Fortney, Jonathan J.; Morley, Caroline V.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Munoz, Antonio Garcia] Tech Univ Berlin, Zentrum Astron & Astrophys, D-10623 Berlin, Germany.
[Gibson, Neale P.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Gizis, John E.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Greene, Thomas P.; Line, Michael R.] NASA Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA.
[Harrington, Joseph] Univ Cent Florida, Dept Phys, Planetary Sci Grp, Orlando, FL 32816 USA.
[Heng, Kevin] Univ Bern, Ctr Space & Habitabil, Sidlerstr 5, CH-3012 Bern, Switzerland.
[Kataria, Tiffany; Sing, David K.] Univ Exeter, Sch Phys, Astrophys Grp, Stocker Rd, Exeter EX4 4QL, Devon, England.
[Kempton, Eliza M. -R.] Grinnell Coll, Dept Phys, Noyce Sci Bldg, Grinnell, IA 50112 USA.
[Knutson, Heather] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Lagage, Pierre-Olivier] Paris Saclay Univ, Irfu AIM, CEA Saclay, F-91191 Gif Sur Yvette, France.
[Madhusudhan, Nikku] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Rocchetto, Marco] UCL, Dept Phys & Astron, London NW1 2PS, England.
[Shkolnik, Evgenya L.] Arizona State Univ, Sch Earth & Space Explorat, 781 S Terrace Rd, Tempe, AZ 85281 USA.
[Shporer, Avi] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Todorov, Kamen O.] ETH, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.
RP Stevenson, KB (reprint author), Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
EM kbs@uchicago.edu
RI Harrington, Joseph/E-6250-2011;
OI Gibson, Neale/0000-0002-9308-2353
FU Sagan Fellowship Program - NASA
FX K.B.S. recognizes support from the Sagan Fellowship Program, supported
by NASA and administered by the NASA Exoplanet Science Institute
(NExScI).
NR 50
TC 4
Z9 4
U1 1
U2 1
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 SEP
PY 2016
VL 128
IS 967
AR 094401
DI 10.1088/1538-3873/128/967/094401
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EB1LK
UT WOS:000387113200002
ER
PT J
AU Brown, PJ
Yang, Y
Cooke, J
Olaes, M
Quimby, RM
Baade, D
Gehrels, N
Hoeflich, P
Maund, J
Mould, J
Wang, LF
Wheeler, JC
AF Brown, Peter J.
Yang, Yi
Cooke, Jeff
Olaes, Melanie
Quimby, Robert M.
Baade, Dietrich
Gehrels, Neil
Hoeflich, Peter
Maund, Justyn
Mould, Jeremy
Wang, Lifan
Wheeler, J. Craig
TI ASASSN-15LH: A SUPERLUMINOUS ULTRAVIOLET REBRIGHTENING OBSERVED BY SWIFT
AND HUBBLE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE polarization; supernovae: individual (ASASSN-15lh, SN2015L);
ultraviolet: general; X-rays: general
ID X-RAY OBSERVATIONS; PAIR-INSTABILITY SUPERNOVAE; MASSIVE BLACK-HOLE;
CORE-COLLAPSE SUPERNOVAE; TIDAL DISRUPTION; SPACE-TELESCOPE; IIN
SUPERNOVA; LUMINOUS SUPERNOVAE; LINEAR-POLARIZATION; MAGNETAR BIRTH
AB We present and discuss ultraviolet and optical photometry from the Ultraviolet/Optical Telescope, X-ray limits from the X-Ray Telescope on Swift, and imaging polarimetry and ultraviolet/optical spectroscopy with the Hubble Space Telescope, all from observations of ASASSN-15lh. It has been classified as a hydrogen-poor superluminous supernova (SLSN I), making it more luminous than any other supernova observed. ASASSN-15lh is not detected in the X-rays in individual or co-added observations. From the polarimetry we determine that the explosion was only mildly asymmetric. We find the flux of ASASSN-15lh to increase strongly into the ultraviolet, with an ultraviolet luminosity 100 times greater than the hydrogen-rich, ultraviolet-bright SLSN II SN 2008es. We find that objects as bright as ASASSN-15lh are easily detectable beyond redshifts of similar to 4 with the single-visit depths planned for the Large Synoptic Survey Telescope. Deep near-infrared surveys could detect such objects past a redshift of similar to 20, enabling a probe of the earliest star formation. A late rebrightening-most prominent at shorter wavelengths -is seen about two months after the peak brightness, which is itself as bright as an SLSN. The ultraviolet spectra during the rebrightening are dominated by the continuum without the broad absorption or emission lines seen in SLSNe or tidal disruption events (TDEs) and the early optical spectra of ASASSN-15lh. Our spectra show no strong hydrogen emission, showing only Lya absorption near the redshift previously found by optical absorption lines of the presumed host. The properties of ASASSN-15lh are extreme when compared to either SLSNe or TDEs.
C1 [Brown, Peter J.; Yang, Yi; Wang, Lifan] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, Dept Phys & Astron, 4242 TAMU, College Stn, TX 77843 USA.
[Cooke, Jeff; Mould, Jeremy] Swinburne Univ, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Olaes, Melanie; 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.
[Baade, Dietrich] Southern Hemisphere ESO, European Org Astron Res, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
[Gehrels, Neil] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hoeflich, Peter] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA.
[Maund, Justyn] Dept Phys & Astron, F39 Hicks Bldg,Hounsfield Rd, Sheffield S3 7RH, S Yorkshire, England.
[Wheeler, J. Craig] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
RP Brown, PJ (reprint author), Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, Dept Phys & Astron, 4242 TAMU, College Stn, TX 77843 USA.
OI Maund, Justyn/0000-0003-0733-7215
FU NASA from Space Telescope Science Institute [NASA 5-26555,
HST-GO-14450.001-A]; NASA [NAS5-26555]; STSCi by STScI
[HST-AR-13276.02-A]; Swift GI program [NNX15AR41G]; NASA's Astrophysics
Data Analysis Program [NNX13AF35G]; [14348]; [14450]
FX We thank the HST director for approving the DDT requests. We thank Matt
McMaster and Dean Hines for helping with the calibration of the ACS/WFC
polarizers. This work is based on observations made with the NASA/ESA
Hubble Space Telescope, obtained from the data archive at the Space
Telescope Science Institute. STScI is operated by the Association of
Universities for Research in Astronomy, Inc. under NASA contract NASA
5-26555. These observations are associated with programs #14348 and
#14450. Support for this work was provided by NASA through grant number
HST-GO-14450.001-A from the Space Telescope Science Institute, which is
operated by AURA, Inc., under NASA contract NAS5-26555. J.C.W. was
supported by STSCi by STScI grant HST-AR-13276.02-A. This work is
supported by the Swift GI program through grant NNX15AR41G. The Swift
Optical/ Ultraviolet Supernova Archive (SOUSA) is supported by NASA's
Astrophysics Data Analysis Program through grant NNX13AF35G. This work
made use of public data in the Swift data archive from observations
requested by several others (PIs: Dong, Godoy, Holoien, Leloudas,
Jonker). This research has made use of NASA's Astrophysics Data System
Bibliographic Services.
NR 101
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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 SEP 1
PY 2016
VL 828
IS 1
AR 3
DI 10.3847/0004-637X/828/1/3
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EA8OE
UT WOS:000386894900003
ER
PT J
AU Cordiner, MA
Boogert, ACA
Charnley, SB
Justtanont, K
Cox, NLJ
Smith, RG
Tielens, AGGM
Wirstrom, ES
Milam, SN
Keane, JV
AF Cordiner, M. A.
Boogert, A. C. A.
Charnley, S. B.
Justtanont, K.
Cox, N. L. J.
Smith, R. G.
Tielens, A. G. G. M.
Wirstrom, E. S.
Milam, S. N.
Keane, J. V.
TI ON THE NATURE OF THE ENIGMATIC OBJECT IRAS 19312+1950: A RARE PHASE OF
MASSIVE STAR FORMATION?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: molecules; masers; stars: AGB and post-AGB; stars: formation;
stars: protostars; stars: winds, outflows
ID YOUNG STELLAR OBJECTS; POSTASYMPTOTIC GIANT BRANCH; WIDE-FIELD CAMERA;
HI-GAL SURVEY; FORMING REGIONS; HERSCHEL OBSERVATIONS; MOLECULAR CLOUDS;
MASER SURVEY; H2O MASERS; CLASS-I
AB IRAS 19312+1950 is a peculiar object that has eluded firm characterization since its discovery, with combined maser properties similar to an evolved star and a young stellar object (YSO). To help determine its true nature, we obtained infrared spectra of IRAS 19312+1950 in the range 5-550 mu m using the Herschel and Spitzer space observatories. The Herschel PACS maps exhibit a compact, slightly asymmetric continuum source at 170 mu m, indicative of a large, dusty circumstellar envelope. The far-IR CO emission line spectrum reveals two gas temperature components: approximate to 0.22 Me of material at 280 +/- 18 K, and approximate to 1.6 M-circle dot of material at 157 +/- 3 K. The O I 63 mu m line is detected on-source but no significant emission from atomic ions was found. The HIFI observations display shocked, high-velocity gas with outflow speeds up to 90 km s(-1) along the line of sight. From Spitzer spectroscopy, we identify ice absorption bands due to H2O at 5.8 mu m and CO2 at 15 mu m. The spectral energy distribution is consistent with a massive, luminous (similar to 2 x 10(4) Le) central source surrounded by a dense, warm circumstellar disk and envelope of total mass similar to 500-700 Me, with large bipolar outflow cavities. The combination of distinctive far-IR spectral features suggest that IRAS 19312+1950 should be classified as an accreting, highmass YSO rather than an evolved star. In light of this reclassification, IRAS 19312+1950 becomes only the fifth high-mass protostar known to exhibit SiO maser activity, and demonstrates that 18 cm OH maser line ratios may not be reliable observational discriminators between evolved stars and YSOs.
C1 [Cordiner, M. A.; Charnley, S. B.; Milam, S. N.] NASA, Astrochem Lab, Goddard Space Flight Ctr, Code 691,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Cordiner, M. A.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Boogert, A. C. A.] Univ Space Res Assoc, Stratospher Observ Infrared Astron, NASA, Ames Res Ctr, MS 232-11, Moffett Field, CA 94035 USA.
[Justtanont, K.; Wirstrom, E. S.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden.
[Cox, N. L. J.] Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D,Bus 2401, B-3001 Leuven, Belgium.
[Cox, N. L. J.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse, France.
[Smith, R. G.] Univ New South Wales, Australian Def Force Acad, Sch Phys Environm & Math Sci, Canberra, ACT 2600, Australia.
[Tielens, A. G. G. M.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
[Keane, J. V.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
RP Cordiner, MA (reprint author), NASA, Astrochem Lab, Goddard Space Flight Ctr, Code 691,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.; Cordiner, MA (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
EM martin.cordiner@nasa.gov
OI Wirstrom, Eva/0000-0002-0656-876X; /0000-0003-1689-9201
FU NASA through JPL/Caltech; NASA through NASA's Origins of Solar Systems
program
FX Support for this work was provided by NASA through an award issued by
JPL/Caltech and through NASA's Origins of Solar Systems program. We
gratefully acknowledge the work of Thomas Robitaille for providing and
supporting the Hyperion radiative transfer code.
NR 95
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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 SEP 1
PY 2016
VL 828
IS 1
AR 51
DI 10.3847/0004-637X/828/1/51
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EA8OE
UT WOS:000386894900051
ER
PT J
AU D'Angelo, G
Bodenheimer, P
AF D'Angelo, Gennaro
Bodenheimer, Peter
TI IN SITU AND EX SITU FORMATION MODELS OF KEPLER 11 PLANETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planet-disk interactions; planetary systems; planets and satellites:
formation; planets and satellites: individual (Kepler 11); planets and
satellites: interiors; protoplanetary disks
ID MEAN-MOTION RESONANCES; EQUATION-OF-STATE; X-RAY-DIFFRACTION;
DISK-SATELLITE INTERACTION; ISOTHERMAL GASEOUS DISK; TERRESTRIAL MAGMA
OCEAN; EARTHS CORE CONDITIONS; LOW-MASS STARS; SUPER-EARTHS; GIANT
PLANETS
AB We present formation simulations of the six Kepler 11 planets. Models assume either in situ or ex situ assembly, the latter with migration, and are evolved to the estimated age of the system, approximate to 8 Gyr. Models combine detailed calculations of both the gaseous envelope and the condensed core structures, including accretion of gas and solids, of the disk's viscous and thermal evolution, including photo-evaporation and disk-planet interactions, and of the planet's evaporative mass loss after disk dispersal. Planet-planet interactions are neglected. Both sets of simulations successfully reproduce measured radii, masses, and orbital distances of the planets, except for the radius of Kepler 11b, which loses its entire gaseous envelope shortly after formation. Gaseous (H+ He) envelopes account for less than or similar to 18% of the planet masses, and between approximate to 35 and approximate to 60% of the planet radii. In situ models predict a very massive inner disk, whose solid surface density (sigma(Z)) varies from over 10(4) to approximate to 10(3) g cm(-2) at stellocentric distances 0.1 less than or similar to r less than or similar to 0.5 au. Initial gas densities would be in excess of 10(5) g cm(-2) if solids formed locally. Given the high disk temperatures (greater than or similar to 1000 K), planetary interiors can only be composed of metals and highly refractory materials. Sequestration of hydrogen by the core and subsequent outgassing is required to account for the observed radius of Kepler 11b. Ex situ models predict a relatively low-mass disk, whose initial sigma(Z) varies from approximate to 10 to approximate to 5 g cm(-2) at 0.5 less than or similar to r less than or similar to 7 au and whose initial gas density ranges from approximate to 10(3) to approximate to 100 g cm(-2). All planetary interiors are expected to be rich in H2O, as core assembly mostly occurs exterior to the ice condensation front. Kepler 11b is expected to have a steam atmosphere, and H2O is likely mixed with H+He in the envelopes of the other planets. Results indicate that Kepler. 11g may not be more massive than Kepler. 11e.
C1 [D'Angelo, Gennaro] NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA.
[D'Angelo, Gennaro] SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA.
[Bodenheimer, Peter] Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA.
RP D'Angelo, G (reprint author), NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA.; D'Angelo, G (reprint author), SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA.
EM gennaro.dangelo@nasa.gov; peter@ucolick.org
OI D'Angelo, Gennaro/0000-0002-2064-0801; Bodenheimer,
Peter/0000-0001-6093-3097
FU NASA Outer Planets Research Program [202844.02.02.01.75]; NASA Origins
of Solar Systems Program [NNX14AG92G]; NASA High-End Computing (HEC)
Program through the NASA Advanced Supercomputing (NAS) Division at Ames
Research Center
FX We thank Uma Gorti for numerous helpful discussions and for her precious
guidance during the implementation of the disk photo-evaporation module.
We are grateful to an anonymous referee, whose insightful comments
helped improve several parts of this paper. G.D. thanks the Los Alamos
National Laboratory for its hospitality. G.D. acknowledges support from
NASA Outer Planets Research Program grant 202844.02.02.01.75 and from
NASA Origins of Solar Systems Program grant NNX14AG92G. Resources
supporting this work were provided by the NASA High-End Computing (HEC)
Program through the NASA Advanced Supercomputing (NAS) Division at Ames
Research Center.
NR 186
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U1 3
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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 SEP 1
PY 2016
VL 828
IS 1
AR 33
DI 10.3847/0004-637X/828/1/33
PG 32
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EA8OE
UT WOS:000386894900033
ER
PT J
AU Deller, AT
Vigeland, SJ
Kaplan, DL
Goss, WM
Brisken, WF
Chatterjee, S
Cordes, JM
Janssen, GH
Lazio, TJW
Petrov, L
Stappers, BW
Lyne, A
AF Deller, A. T.
Vigeland, S. J.
Kaplan, D. L.
Goss, W. M.
Brisken, W. F.
Chatterjee, S.
Cordes, J. M.
Janssen, G. H.
Lazio, T. J. W.
Petrov, L.
Stappers, B. W.
Lyne, A.
TI MICROARCSECOND VLBI PULSAR ASTROMETRY WITH PSR pi. I. TWO BINARY
MILLISECOND PULSARS WITH WHITE DWARF COMPANIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrometry; pulsars: individual (PSR J1022+1001, J2145-0750); stars:
neutron; techniques: high angular resolution; white dwarfs
ID BASE-LINE ARRAY; DATA RELEASE; SPECTROSCOPIC ANALYSIS; SOFTWARE
CORRELATOR; PROPER MOTION; PARALLAXES; SKY; DISTANCE; MASS;
INTERFEROMETRY
AB Model-independent distance constraints to binary millisecond pulsars (MSPs) are of great value to both the timing observations of the radio pulsars and multiwavelength observations of their companion stars. Astrometry using very long baseline interferometry (VLBI) can be employed to provide these model-independent distances with very high precision via the detection of annual geometric parallax. Using the Very Long Baseline Array, we have observed two binary MSPs, PSR J1022+1001 and J2145-0750, over a two-year period and measured their distances to be 700(10)(+14) pc and 613(-14)(+16) pc respectively. We use the well-calibrated distance in conjunction with revised analysis of optical photometry to tightly constrain the nature of their massive (M similar to 0.85 M-circle dot) white dwarf companions. Finally, we show that several measurements of the parallax and proper motion of PSR J1022 + 1001 and PSR J2145-0750 obtained by pulsar timing array projects are incorrect, differing from the more precise VLBI values by up to 5 sigma. We investigate possible causes for the discrepancy, and find that imperfect modeling of the solar wind is a likely candidate for the errors in the timing model given the low ecliptic latitude of these two pulsars.
C1 [Deller, A. T.; Janssen, G. H.] Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands.
[Vigeland, S. J.; Kaplan, D. L.] Univ Wisconsin Milwaukee, POB 413, Milwaukee, WI 53201 USA.
[Goss, W. M.; Brisken, W. F.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Chatterjee, S.; Cordes, J. M.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Lazio, T. J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Petrov, L.] Astrogeo Ctr, Falls Church, VA 22043 USA.
[Stappers, B. W.; Lyne, A.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
RP Deller, AT (reprint author), Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands.
OI Deller, Adam/0000-0001-9434-3837
FU NWO Veni Fellowship; NANOGrav project through National Science
Foundation (NSF) PIRE program [0968296]; NSF Physics Frontiers Center
[1430284]; National Aeronautics and Space Administration; Alfred P.
Sloan Foundation; National Science Foundation; U.S. Department of Energy
Office of Science
FX A.T.D. was supported by an NWO Veni Fellowship. D.L.K. an d S.J.V.
receive support from the NANOGrav project through National Science
Foundation (NSF) PIRE program award number 0968296 and NSF Physics
Frontiers Center award number 1430284. 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. The authors thank David Nice and Pierre Bergeron for
useful discussions. The National Radio Astronomy Observatory is a
facility of the National Science Foundation operated under cooperative
agreement by Associated Universities, Inc. Pulsar research at the
Jodrell Bank Centre for Astrophysics and the observations using the
Lovell Telescope are supported by a consolidated grant from the STFC in
the UK. 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/.
NR 55
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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 SEP 1
PY 2016
VL 828
IS 1
AR 8
DI 10.3847/0004-637X/828/1/8
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EA8OE
UT WOS:000386894900008
ER
PT J
AU Furst, F
Grinberg, V
Tomsick, JA
Bachetti, M
Boggs, SE
Brightman, M
Christensen, FE
Craig, WW
Gandhi, P
Grefenstette, B
Hailey, CJ
Harrison, FA
Madsen, KK
Parker, ML
Pottschmidt, K
Stern, D
Walton, DJ
Wilms, J
Zhang, WW
AF Furst, F.
Grinberg, V.
Tomsick, J. A.
Bachetti, M.
Boggs, S. E.
Brightman, M.
Christensen, F. E.
Craig, W. W.
Gandhi, P.
Grefenstette, B.
Hailey, C. J.
Harrison, F. A.
Madsen, K. K.
Parker, M. L.
Pottschmidt, K.
Stern, D.
Walton, D. J.
Wilms, J.
Zhang, W. W.
TI SPECTRO-TIMING STUDY OF GX 339-4 IN A HARD INTERMEDIATE STATE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; stars: black holes; X-rays: binaries;
X-rays: individual (GX 339-4)
ID QUASI-PERIODIC OSCILLATIONS; X-RAY BINARIES; BLACK-HOLE CANDIDATES;
ADVECTION-DOMINATED ACCRETION; RELATIVISTIC PRECESSION MODEL;
LENS-THIRRING PRECESSION; NOVA XTE J1550-564; LOW/HARD STATE; CYGNUS
X-1; FREQUENCY CORRELATION
AB We present an analysis of Nuclear Spectroscopic Telescope Array. observations of a hard intermediate state of the transient. black hole GX 339-4 taken in 2015 January. With. the source softening significantly over the course of the 1.3 day long observation we split the data into 21 sub-sets and find that the spectrum of all of them can be well described by a power-law continuum with an additional relativistically blurred reflection component. The photon index increases from similar to 1.69 to similar to 1.77 over the course of the observation. The accretion disk is truncated at around nine gravitational radii in all spectra. We also perform timing analysis on the same 21 individual data sets, and find a strong type-C quasi-periodic oscillation (QPO), which increases. in frequency from similar to 0.68 to similar to 1.05 Hz with time. The frequency change is well correlated with the softening of the spectrum. We discuss possible scenarios for the production of the QPO and calculate predicted inner radii in the relativistic precession model as well as the global disk mode oscillations model. We find discrepancies with respect to the observed values in both models unless we allow for a black hole mass of similar to 100 M-circle dot, which is highly unlikely. We discuss possible systematic uncertainties, in particular with the measurement of the inner accretion disk radius in the relativistic reflection model. We conclude that the combination of observed QPO frequencies and inner accretion disk radii, as obtained from spectral fitting,. is difficult to reconcile with current models.
C1 [Furst, F.; Brightman, M.; Grefenstette, B.; Harrison, F. A.; Madsen, K. K.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Grinberg, V.] MIT, Kavli Inst Astrophys, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Tomsick, J. A.; Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Bachetti, M.] INAF, Osservatorio Astron Cagliari, I-09047 Selargius, CA, Italy.
[Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark.
[Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
[Gandhi, P.] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Parker, M. L.] Inst Astron, Cambridge CB3 0HA, England.
[Pottschmidt, K.] UMBC, CRESST, Dept Phys, Baltimore, MD 21250 USA.
[Pottschmidt, K.] UMBC, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Pottschmidt, K.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Stern, D.; Walton, D. J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Wilms, J.] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & ECAP, D-96049 Bamberg, Germany.
RP Furst, F (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
RI Wilms, Joern/C-8116-2013
OI Wilms, Joern/0000-0003-2065-5410
FU NASA [NNG08FD60C, NAS8-03060]; National Aeronautics and Space
Administration; NASA through Smithsonian Astrophysical Observatory (SAO)
[SV3-73016]
FX We thank the anonymous referee for the constructive and helpful
comments. We thank the NuSTAR schedulers and SOC, in particular Karl
Forster, for making this observation possible. We thank Javier Garcia
and Thomas Dauser for helpful discussions about the reflection models.
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. Support for
this work was provided by NASA through the Smithsonian Astrophysical
Observatory (SAO) contract SV3-73016 to MIT for Support of the Chandra
X-ray Center (CXC) and Science Instruments; CXC is operated by SAO for
and on behalf of NASA under contract NAS8-03060. 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 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. This research has made use of MAXI data provided
by RIKEN, JAXA and the MAXI team.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
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JI Astrophys. J.
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SC Astronomy & Astrophysics
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UT WOS:000386894900034
ER
PT J
AU Hamren, K
Beaton, RL
Guhathakurta, P
Gilbert, KM
Tollerud, EJ
Boyer, ML
Rockosi, CM
Smith, GH
Majewski, SR
Howley, K
AF Hamren, Katherine
Beaton, Rachael L.
Guhathakurta, Puragra
Gilbert, Karoline M.
Tollerud, Erik J.
Boyer, Martha L.
Rockosi, Constance M.
Smith, Graeme H.
Majewski, Steven R.
Howley, Kirsten
TI CARBON STARS IN THE SATELLITES AND HALO OF M31
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (M31); stars: AGB and post-AGB; stars: carbon
ID ASYMPTOTIC GIANT BRANCH; DIGITAL-SKY-SURVEY; LOCAL GROUP GALAXIES; DWARF
SPHEROIDAL GALAXIES; SPITZER-SPACE-TELESCOPE; SURVEY STELLAR SPECTRA;
LARGE-MAGELLANIC-CLOUD; AGB STARS; SPLASH SURVEY; METAL-POOR
AB We spectroscopically identify a sample of carbon stars in the satellites and halo of M31 using moderate-resolution optical spectroscopy from the Spectroscopic and Photometric Landscape of Andromeda's Stellar Halo survey. We present the photometric properties of our sample of 41 stars, including their brightness with respect to the tip of the red giant branch (TRGB) and their distributions in various color-color spaces. This analysis reveals a bluer population of carbon stars fainter than the TRGB and a redder population of carbon stars brighter than the TRGB. We then apply principal component analysis to determine the sample's eigenspectra and eigencoefficients. Correlating the eigencoefficients with various observable properties reveals the spectral features that trace effective temperature and metallicity. Putting the spectroscopic and photometric information together, we find the carbon stars in the satellites and halo of M31 to be minimally impacted by dust and internal dynamics. We also find that while there is evidence to suggest that the sub-TRGB stars are extrinsic in origin, it is also possible that they are are particularly faint members of the asymptotic giant branch.
C1 [Hamren, Katherine; Guhathakurta, Puragra; Rockosi, Constance M.; Smith, Graeme H.] Univ Calif Santa Cruz, Dept Astron & Astrophys, 1156 High St, Santa Cruz, CA 95064 USA.
[Beaton, Rachael L.] Observ Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA.
[Gilbert, Karoline M.; Tollerud, Erik J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Gilbert, Karoline M.] Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA.
[Boyer, Martha L.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA.
[Majewski, Steven R.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Howley, Kirsten] Lawrence Livermore Natl Lab, POB 808, Livermore, CA 94551 USA.
RP Hamren, K (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, 1156 High St, Santa Cruz, CA 95064 USA.
EM khamren@ucolick.org
OI Guhathakurta, Puragra/0000-0001-8867-4234
FU NSF [AST-1010039, AST-1412648, AST-1413269]; NASA [HST-GO-12055]; NSF
Graduate Research Fellowship; Giacconi Fellowship
FX The authors would like to thank Bernhard Aringer and Leo Girardi for
helpful conversations and an early look at the 2016 cool star models. We
would also like to thank Marla Geha, James Bullock, and Jason Kalirai
for their work on the SPLASH survey over the years. and their
willingness to provide data for this paper. P.G. and K.H. acknowledge
NSF grants AST-1010039 and AST-1412648 and NASA grant HST-GO-12055.
R.L.B. and S.R.M. thank NSF grant AST-1413269. K. H. was supported by an
NSF Graduate Research Fellowship, and E.J.T. was supported by a Giacconi
Fellowship. We appreciate the very significant cultural role and
reverence that the summit of Mauna Kea has always held within the
indigenous Hawaiian community. We are most grateful to have had the
opportunity to conduct observations from this mountain.
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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.
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SC Astronomy & Astrophysics
GA EA8OE
UT WOS:000386894900015
ER
PT J
AU Han, C
Udalski, A
Gould, A
Zhu, W
Street, RA
Yee, JC
Beichman, C
Bryden, C
Novati, SC
Carey, S
Fausnaugh, M
Gaudi, BS
Henderson, CB
Shvartzvald, Y
Wibking, B
Szymanski, MK
Soszynski, I
Skowron, J
Mroz, P
Poleski, R
Pietrukowicz, P
Kozlowski, S
Ulaczyk, K
Wyrzykowski, L
Pawlak, M
Tsapras, Y
Hundertmark, M
Bachelet, E
Dominik, M
Bramich, DM
Cassan, A
Jaimes, RF
Horne, K
Ranc, C
Schmidt, R
Snodgrass, C
Wambsganss, J
Steele, IA
Menzies, J
Mao, S
Bozza, V
Jorgensen, UG
Alsubai, KA
Ciceri, S
D'Ago, G
Haugbolle, T
Hessman, FV
Hinse, TC
Juncher, D
Korhonen, H
Mancini, L
Popovas, A
Rabus, M
Rahvar, S
Scarpetta, G
Skottfelt, J
Southworth, J
Starkey, D
Surdej, J
Wertz, O
Zarucki, M
Pogge, RW
DePpoy, DL
AF Han, C.
Udalski, A.
Gould, A.
Zhu, Wei
Street, R. A.
Yee, J. C.
Beichman, C.
Bryden, C.
Novati, S. Calchi
Carey, S.
Fausnaugh, M.
Gaudi, B. S.
Henderson, Calen B.
Shvartzvald, Y.
Wibking, B.
Szymanski, M. K.
Soszynski, I.
Skowron, J.
Mroz, P.
Poleski, R.
Pietrukowicz, P.
Kozlowski, S.
Ulaczyk, K.
Wyrzykowski, L.
Pawlak, M.
Tsapras, Y.
Hundertmark, M.
Bachelet, E.
Dominik, M.
Bramich, D. M.
Cassan, A.
Jaimes, R. Figuera
Horne, K.
Ranc, C.
Schmidt, R.
Snodgrass, C.
Wambsganss, J.
Steele, I. A.
Menzies, J.
Mao, S.
Bozza, V.
Jorgensen, U. G.
Alsubai, K. A.
Ciceri, S.
D'Ago, G.
Haugbolle, T.
Hessman, F. V.
Hinse, T. C.
Juncher, D.
Korhonen, H.
Mancini, L.
Popovas, A.
Rabus, M.
Rahvar, S.
Scarpetta, G.
Skottfelt, J.
Southworth, J.
Starkey, D.
Surdej, J.
Wertz, O.
Zarucki, M.
Pogge, R. W.
DePpoy, D. L.
CA Spitzer Microlensing Team
OGLE Collaboration
RoboNet Collaboration
MINDSTEp Consortium
Fun Collaboration
TI OGLE-2015-BLG-0479LA,B: BINARY GRAVITATIONAL MICROLENS CHARACTERIZED BY
SIMULTANEOUS GROUND-BASED AND SPACE-BASED OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; gravitational lensing: micro
ID DIFFERENCE IMAGE-ANALYSIS; PARALLAX SATELLITE MASS; LENSING EXPERIMENT;
PLANET PHOTOMETRY; GALACTIC BULGE; OGLE-III; SPITZER; EVENTS; STARS;
DISTANCES
AB We present a combined analysis of the observations of the gravitational microlensing event OGLE-2015-BLG-0479 taken both from the ground and by the Spitzer Space Telescope. The light curves seen from the ground and from space exhibit a time offset of similar to 13 days between the caustic spikes, indicating that the relative lens-source positions seen from the two places are displaced by parallax effects. From modeling the light curves, we measure the space-based microlens parallax. Combined with the angular Einstein radius measured by analyzing the caustic crossings, we determine the mass and distance of the lens. We find that the lens is a binary composed of two G-type stars with masses of similar to 1.0 M-circle dot and similar to 0.9 M-circle dot located at a distance. of similar to 3 kpc. In addition, we are able to constrain the complete orbital parameters of the lens thanks to the precise measurement of the microlens parallax derived from the joint analysis. In contrast to the binary event OGLE-2014-BLG-1050, which was also observed by Spitzer, we find that the interpretation of OGLE-2015-BLG-0479 does not suffer from the degeneracy between (+/-, +/-) and (+/-, -/+) solutions, confirming that the four-fold parallax degeneracy in single-lens events collapses into the two-fold degeneracy for the general case of binary-lens events. The location of the blend in the color-magnitude diagram is consistent with the lens properties, suggesting that the blend is the lens itself. The blend is bright enough for spectroscopy and thus this possibility can be checked from future follow-up observations.
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.; Wyrzykowski, L.; Pawlak, M.] Univ Warsaw Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland.
[Gould, A.; Zhu, Wei; Gaudi, B. S.; Wibking, B.] Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA.
[Gould, A.; Ciceri, S.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Street, R. A.] Queen Mary Univ London, Sch Phys & Astron, Mile End Rd, London E1 4NS, England.
[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.
[Bryden, C.; Henderson, Calen B.; Shvartzvald, Y.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Novati, S. Calchi] Univ Salerno, Dipartimento Fis ER Caianiello, Via Giovanni Paolo II, I-84084 Fisciano, SA, Italy.
[Novati, S. Calchi] IIASS, Via G Pellegrino 19, I-84019 Vietri Sul Mare, SA, Italy.
[Carey, S.] CALTECH, Spitzer Sci Ctr, MS 220-6, Pasadena, CA 91125 USA.
[Tsapras, Y.; Jaimes, R. Figuera; Schmidt, R.; Wambsganss, J.] Univ Heidelberg ZAH, Zentrum Astron, Astronom Rechen Inst, D-69120 Heidelberg, Germany.
[Hundertmark, M.] Univ Copenhagen, Niels Bohr Inst, Oster Voldgade 5, DK-1350 Copenhagen K, Denmark.
[Hundertmark, M.] Univ Copenhagen, Ctr Star & Planet Format, Oster Voldgade 5, DK-1350 Copenhagen K, Denmark.
[Bachelet, E.] Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA.
[Bachelet, E.; Bramich, D. M.; Alsubai, K. A.] Qatar Fdn, HBKU, QEERI, Doha, Qatar.
[Dominik, M.; Jaimes, R. Figuera; Horne, K.; Starkey, D.] Univ St Andrews, Sch Phys Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Ranc, C.] UPMC Univ Paris 6, Sorbonne Univ, CNRS, Inst Astrophys Paris,UMR 7095, 98 Bis Bd Arago, F-75014 Paris, France.
[Snodgrass, C.] Open Univ, Dept Phys Sci, Planetary & Space Sci, Milton Keynes MK7 6AA, Bucks, England.
[Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool CH41 1LD, Merseyside, England.
[Menzies, J.] South African Astron Observ, POB 9, ZA-7935 Observatory, South Africa.
[Mao, S.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
[Jorgensen, U. G.; Haugbolle, T.; Juncher, D.; Korhonen, H.; Popovas, A.; Skottfelt, J.] Univ Copenhagen, Niels Bohr Inst, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark.
[Hessman, F. V.] Georg August Univ Gottingen, Inst Astrophys, Friedrich Hund Pl 1, D-37077 Gottingen, Germany.
[Hinse, T. C.] Korea Astron & Space Sci Inst, 776 Daedeokdae Ro, Daejeon 305348, South Korea.
[Korhonen, H.] Univ Turku, Finnish Ctr Astron ESO FINCA, Vaisalantie 20, FI-21500 Piikkio, Finland.
[Rabus, M.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Av Vicuna Mackenna 4860, Santiago 7820436, Chile.
[Rahvar, S.] Sharif Univ Technol, Dept Phys, POB 11155-9161, Tehran, Iran.
[Southworth, J.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Surdej, J.; Wertz, O.] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[DePpoy, D. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
RP Han, C (reprint author), Chungbuk Natl Univ, Dept Phys, Cheongju 361763, South Korea.
RI Korhonen, Heidi/E-3065-2016; D'Ago, Giuseppe/N-8318-2016
OI Korhonen, Heidi/0000-0003-0529-1161; D'Ago, Giuseppe/0000-0001-9697-7331
FU Creative Research Initiative Program of National Research Foundation of
Korea [2009-0081561]; National Science Centre, Poland [MAESTRO
2014/14/A/ST9/00121]; JPL grant [1500811]; NASA through the 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 and G.. Pietrzynski, 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. 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 Universities Space Research Association
through a contract with NASA. The Spitzer Team thanks Christopher S.
Kochanek for graciously trading us his allocated observing time on the
CTIO 1.3m during the Spitzer campaign. We acknowledge the high-speed
internet service (KREONET) provided by Korea Institute of Science and
Technology Information (KISTI).
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
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JI Astrophys. J.
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SC Astronomy & Astrophysics
GA EA8OE
UT WOS:000386894900053
ER
PT J
AU Lieman-Sifry, J
Hughes, AM
Carpenter, JM
Gorti, U
Hales, A
Flaherty, KM
AF Lieman-Sifry, Jesse
Hughes, A. Meredith
Carpenter, John M.
Gorti, Uma
Hales, Antonio
Flaherty, Kevin M.
TI DEBRIS DISKS IN THE SCORPIUS-CENTAURUS OB ASSOCIATION RESOLVED BY ALMA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; planetary systems; planets and satellites:
formation; protoplanetary disks; submillimeter: planetary systems
ID TERRESTRIAL PLANET FORMATION; CIRCLE-DOT STARS; ANALOG HD 107146; A-TYPE
STARS; BETA-PICTORIS; DUSTY DEBRIS; MOLECULAR GAS; MILLIMETER EMISSION;
CIRCUMSTELLAR DISK; SCATTERED-LIGHT
AB We present a CO(2-1) and 1240 mu m continuum survey of 23 debris disks with spectral types B9-G1, observed at an angular resolution of 0.5 ''-1 '' with the Atacama Large Millimeter/Submillimeter Array (ALMA). The sample was selected for large infrared excess and age similar to 10 Myr, to characterize the prevalence of molecular gas emission in young debris disks. We identify three CO-rich debris disks, plus two additional tentative (3 sigma) CO detections. Twenty disks were detected in the continuum at the >3 sigma level. For the 12 disks in the sample that are spatially resolved by our observations, we perform an independent analysis of the interferometric continuum visibilities to constrain the basic dust disk geometry, as well as a simultaneous analysis of the visibilities and broadband spectral energy distribution to constrain the characteristic grain size and disk mass. The gas-rich debris disks exhibit preferentially larger outer radii in their dust disks, and a higher prevalence of characteristic grain sizes smaller than the blowout size. The gas-rich disks do not exhibit preferentially larger dust masses, contrary to expectations for a scenario in which a higher cometary destruction rate would be expected to result in a larger mass of both CO and dust. The three debris disks in our sample with strong CO detections are all around A stars: the conditions in disks around intermediate-mass stars appear to be the most conducive to the survival or formation of CO.
C1 [Lieman-Sifry, Jesse; Hughes, A. Meredith; Flaherty, Kevin M.] Wesleyan Univ, Van Vleck Observ, Dept Astron, 96 Foss Hill Dr, Middletown, CT 06459 USA.
[Carpenter, John M.] CALTECH, Dept Astron, MC 249-17, Pasadena, CA 91125 USA.
[Carpenter, John M.; Hales, Antonio] Joint ALMA Observ, Atacama Large Millimeter Submillimeter Array, Alonso Cordova 3107, Santiago 7630355, Chile.
[Gorti, Uma] SETI Inst, Mountain View, CA USA.
[Gorti, Uma] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Hales, Antonio] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA.
RP Lieman-Sifry, J (reprint author), Wesleyan Univ, Van Vleck Observ, Dept Astron, 96 Foss Hill Dr, Middletown, CT 06459 USA.
FU NSF [AST-1412647, CNS-0619508]; NASA CT Space Grant Directed Campus
Scholarship
FX The authors thank Angelo Ricarte for his contributions to the code base
and helpful comments, and the anonymous referee for a careful commentary
that improved the paper. J.L.S. and A.M.H. gratefully acknowledge
support from NSF grant AST-1412647. J.L.S. was also supported in part by
a NASA CT Space Grant Directed Campus Scholarship. We acknowledge
Wesleyan University for time on its high-performance computing cluster,
supported by the NSF under grant number CNS-0619508. This work makes use
of the following ALMA data: ADS/JAO. ALMA#2012.1.00688. S. ALMA is a
partnership of ESO (representing its member states), NSF (USA), and NINS
(Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in
cooperation with the Republic of Chile. The Joint ALMA Observatory is
operated by ESO, AUI/ NRAO, and NAOJ. 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 NASA's Astrophysics Data System Bibliographic
Services, as well as Astropy, a community-developed core Python package
for Astronomy (Astropy Collaboration et al. 2013).
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
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J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
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PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EA8OE
UT WOS:000386894900025
ER
PT J
AU Lomax, JR
Wisniewski, JP
Grady, CA
McElwain, MW
Hashimoto, J
Kudo, T
Kusakabe, N
Okamoto, YK
Fukagawa, M
Abe, L
Brandner, W
Brandt, TD
Carson, JC
Currie, TM
Egner, S
Feldt, M
Goto, M
Guyon, O
Hayano, Y
Hayashi, M
Hayashi, SS
Henning, T
Hodapp, KW
Inoue, A
Ishii, M
Iye, M
Janson, M
Kandori, R
Knapp, GR
Kuzuhara, M
Kwon, J
Matsuo, T
Mayama, S
Miyama, S
Momose, M
Morino, JI
Moro-Martin, A
Nishimura, T
Pyo, TS
Schneider, GH
Serabyn, E
Sitko, ML
Suenaga, T
Suto, H
Suzuki, R
Takahashi, YH
Takami, M
Takato, N
Terada, H
Thalmann, C
Tomono, D
Turner, EL
Watanabe, M
Yamada, T
Takami, H
Usuda, T
Tamura, M
AF Lomax, Jamie R.
Wisniewski, John P.
Grady, Carol A.
McElwain, Michael W.
Hashimoto, Jun
Kudo, Tomoyuki
Kusakabe, Nobuhiko
Okamoto, Yoshiko K.
Fukagawa, Misato
Abe, Lyu
Brandner, Wolfgang
Brandt, Timothy D.
Carson, Joseph C.
Currie, Thayne M.
Egner, Sebastian
Feldt, Markus
Goto, Miwa
Guyon, Olivier
Hayano, Yutaka
Hayashi, Masahiko
Hayashi, Saeko S.
Henning, Thomas
Hodapp, Klaus W.
Inoue, Akio
Ishii, Miki
Iye, Masanori
Janson, Markus
Kandori, Ryo
Knapp, Gillian R.
Kuzuhara, Masayuki
Kwon, Jungmi
Matsuo, Taro
Mayama, Satoshi
Miyama, Shoken
Momose, Munetake
Morino, Jun-Ichi
Moro-Martin, Amaya
Nishimura, Tetsuo
Pyo, Tae-Soo
Schneider, Glenn H.
Serabyn, Eugene
Sitko, Michael L.
Suenaga, Takuya
Suto, Hiroshi
Suzuki, Ryuji
Takahashi, Yasuhiro H.
Takami, Michihiro
Takato, Naruhisa
Terada, Hiroshi
Thalmann, Christian
Tomono, Daigo
Turner, Edwin L.
Watanabe, Makoto
Yamada, Toru
Takami, Hideki
Usuda, Tomonori
Tamura, Motohide
TI CONSTRAINING THE MOVEMENT OF THE SPIRAL FEATURES AND THE LOCATIONS OF
PLANETARY BODIES WITHIN THE AB AUR SYSTEM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planet-disk interactions; planetary systems; protoplanetary disks;
radiative transfer; stars: individual (AB Aur); stars: pre-main sequence
ID YOUNG STELLAR OBJECTS; HERBIG AE STARS; SPECTRAL ENERGY-DISTRIBUTIONS;
CIRCUMSTELLAR DUST; PROTOPLANETARY DISK; RADIATION TRANSFER;
INTERSTELLAR DUST; SIZE DISTRIBUTION; HIGH-RESOLUTION; TAURUS-AURIGA
AB We present a new analysis of multi-epoch, H-band, scattered light images of the AB Aur system. We use a Monte Carlo radiative transfer code to simultaneously model the system's spectral energy distribution (SED) and H-band polarized intensity (PI) imagery. We find that a disk-dominated model, as opposed to one that is envelope-dominated, can plausibly reproduce AB Aur's SED and near-IR imagery. This is consistent with previous modeling attempts presented in the literature and supports the idea that at least a subset of AB Aur's spirals originate within the disk. In light of this, we also analyzed the movement of spiral structures in multi-epoch H-band total light and PI imagery of the disk. We detect no significant rotation or change in spatial location of the spiral structures in these data, which span a 5.8-year baseline. If such structures are caused by disk-planet interactions, the lack of observed rotation constrains the location of the orbit of planetary perturbers to be >47 au.
C1 [Lomax, Jamie R.; Wisniewski, John P.; Hashimoto, Jun] Univ Oklahoma, Homer L Dodge Dept Phys, Norman, OK 73071 USA.
[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, Pasadena, CA USA.
[McElwain, Michael W.] NASA, Goddard Space Flight Ctr, Code 6681, Greenbelt, MD 20771 USA.
[Kudo, Tomoyuki; Currie, Thayne M.; Egner, Sebastian; Guyon, Olivier; Hayano, Yutaka; Hayashi, Saeko S.; Nishimura, Tetsuo; Pyo, Tae-Soo; Takato, Naruhisa; Terada, Hiroshi; Tomono, Daigo] Natl Astron Observ Japan, Subaru Telescope, 650 N Aohoku Pl, Hilo, HI 96720 USA.
[Kusakabe, Nobuhiko; Hayashi, Masahiko; Ishii, Miki; Iye, Masanori; Kandori, Ryo; Morino, Jun-Ichi; Suenaga, Takuya; Suto, Hiroshi; Suzuki, Ryuji; Takahashi, Yasuhiro H.; Takami, Hideki; Tamura, Motohide] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Okamoto, Yoshiko K.] Ibaraki Univ, Fac Sci, Inst Astrophys & Planetary Sci, 2-1-1 Bunkyo, Mito, Ibaraki 3108512, Japan.
[Fukagawa, Misato] Osaka Univ, Grad Sch Sci, 1-1 Machikaneyama, Toyonaka, Osaka 5600043, Japan.
[Abe, Lyu] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange UMR 7293, 28 Ave Valrose, F-06108 Nice 2, France.
[Brandner, Wolfgang] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Brandt, Timothy D.; Turner, Edwin L.] Inst Adv Study, Dept Astrophys, Princeton, NJ 08540 USA.
[Carson, Joseph C.] Coll Charleston, Dept Phys & Astron, 58 Coming St, Charleston, SC 29424 USA.
[Goto, Miwa] Univ Munich, Univ Sternwarte Munchen, Scheinerstr 1, D-81679 Munich, Germany.
[Hodapp, Klaus W.] Univ Hawaii, Inst Astron, 640 N Aohoku Pl, Hilo, HI 96720 USA.
[Janson, Markus] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, SE-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; Usuda, Tomonori; Tamura, Motohide] Univ Tokyo, Dept Astron, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan.
[Matsuo, Taro] Kyoto Univ, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan.
[Mayama, Satoshi] Grad Univ Adv Studies SOKENDAI, Ctr Promot Integrated Sci, Hayama Cho, Hayama, Kanagawa 2400193, Japan.
[Miyama, Shoken] Hiroshima Univ, 1-3-2 Kagamiyama, Higashihiroshima 7398511, Japan.
[Momose, Munetake] Ibaraki Univ, Coll Sci, Bunkyo 2-1-1, Mito, Ibaraki 3108512, Japan.
[Moro-Martin, Amaya] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Moro-Martin, Amaya] Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA.
[Schneider, Glenn H.] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA.
[Serabyn, Eugene] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Sitko, Michael L.] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA.
[Sitko, Michael L.] Space Sci Inst, 475 Walnut St,Suite 205, Boulder, CO 80301 USA.
[Suenaga, Takuya] Grad Univ Adv Studies, Dept Astron Sci, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Takami, Michihiro] Acad Sinica, Inst Astron & Astrophys, POB 23141, Taipei 10617, Taiwan.
[Thalmann, Christian] Swiss Fed Inst Technol, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.
[Watanabe, Makoto] Hokkaido Univ, Dept Cosmosci, Kita Ku, Sapporo, Hokkaido 0600810, Japan.
[Yamada, Toru] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan.
RP Lomax, JR (reprint author), Univ Oklahoma, Homer L Dodge Dept Phys, Norman, OK 73071 USA.
EM Jamie.R.Lomax@ou.edu; wisniewski@ou.edu; carol.a.grady@nasa.gov
RI MIYAMA, Shoken/A-3598-2015
FU NASA Origins of Solar System program [NNX13AK17G, RTOP 12-OSS12-0045,
NNG13PB64P]; MEXT Japan; Mitsubishi Foundation; [NSF-AST 1009203];
[1008440]; [1009314]
FX We acknowledge support from NSF-AST 1009203 (J.C.), 1008440 (C.G.), and
1009314 (E.R., J.W., J.H.) and the NASA Origins of Solar System program
under NNX13AK17G (J.W.), RTOP 12-OSS12-0045 (M.M.), and NNG13PB64P
(C.G.). This work is partly supported by a Grant-in-Aid for Science
Research in a Priority Area from MEXT Japan and by the Mitsubishi
Foundation. The authors recognize and acknowledge the 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. We wish to
extend special thanks to those of Hawaiian ancestry on whose sacred
mountain we are privileged to be guests. This work is based in part on
data collected at the Subaru Telescope, which is operated by the
National Astronomical Observatory of Japan. We also thank Barbara
Whitney for providing us with helpful feedback that improved our paper
and for clarifying aspects of her HOCHUNK3D code, and Anthony Paat for
helping run models. Additionally, we would like to thank the anonymous
reviewer for providing comments that led to an improved paper.
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J9 ASTROPHYS J
JI Astrophys. J.
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SC Astronomy & Astrophysics
GA EA8OE
UT WOS:000386894900002
ER
PT J
AU Nelson, EJ
van Dokkum, PG
Schreiber, NMF
Franx, M
Brammer, GB
Momcheva, IG
Wuyts, S
Whitaker, KE
Skelton, RE
Fumagalli, M
Hayward, CC
Kriek, M
Labbe, I
Leja, J
Rix, HW
Tacconi, LJ
van der Wel, A
van den Bosch, FC
Oesch, PA
Dickey, C
Lange, JU
AF Nelson, Erica June
van Dokkum, Pieter G.
Schreiber, Natascha M. Foerster
Franx, Marijn
Brammer, Gabriel B.
Momcheva, Ivelina G.
Wuyts, Stijn
Whitaker, Katherine E.
Skelton, Rosalind E.
Fumagalli, Mattia
Hayward, Christopher C.
Kriek, Mariska
Labbe, Ivo
Leja, Joel
Rix, Hans-Walter
Tacconi, Linda J.
van der Wel, Arjen
van den Bosch, Frank C.
Oesch, Pascal A.
Dickey, Claire
Lange, Johannes Ulf
TI WHERE STARS FORM: INSIDE-OUT GROWTH AND COHERENT STAR FORMATION FROM HST
H alpha MAPS OF 3200 GALAXIES ACROSS THE MAIN SEQUENCE AT 0.7 < z < 1.5
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: formation; galaxies: high-redshift;
galaxies: star formation; galaxies: structure
ID SIMILAR-TO 2; HUBBLE-SPACE-TELESCOPE; SINS/ZC-SINF SURVEY; INTEGRAL
FIELD SPECTROSCOPY; LYMAN BREAK GALAXIES; ULTRA-DEEP FIELD;
EXTRAGALACTIC LEGACY SURVEY; COMPACT QUIESCENT GALAXIES;
MASS-METALLICITY RELATION; KILOPARSEC-SCALE CLUMPS
AB We present H alpha maps at 1 kpc spatial resolution for star-forming galaxies at z similar to 1, made possible by the Wide Field Camera 3 grism on Hubble Space Telescope (HST). Employing this capability over all five 3D-HST/CANDELS fields provides a sample of 3200 galaxies enabling a division into subsamples based on stellar mass and star formation rate (SFR). By creating deep stacked H alpha images, we reach surface brightness limits of 1 x 10(-18) erg s(-1) cm(-2) arc sec(-2), allowing us to map the distribution of ionized gas to similar to 10 kpc for typical L* galaxies at this epoch. We find that the spatial extent of the H alpha distribution increases with stellar mass as r(H alpha) = 1.5(M-*/10(10) M-circle dot)(0.23) kpc. The H alpha emission is more extended than the stellar continuum emission, consistent with inside-out assembly of galactic disks. This effect grows stronger with mass as r(H alpha)/r(*) = 1.1(M-*/10(10) M-circle dot)(0.054). We map the H alpha distribution as a function of SFR(IR+UV) and find evidence for "coherent star formation" across the SFR-M-* plane: above the main sequence (MS), H alpha is enhanced at all radii; below the MS, H alpha is depressed at all radii. This suggests that at all masses the physical processes driving the enhancement or suppression of star formation act throughout the disks of galaxies. At high masses (10(10.5) < M-*/M-circle dot < 10(11)), above the MS, H alpha is particularly enhanced in the center, potentially building bulges and/or supermassive black holes. Below the MS, a strong central dip in the EW(H alpha), as well as. the inferred specific SFR, appears. Importantly, though, across the entirety of the SFR-M-* plane, the absolute SFR as traced by H alpha is always centrally peaked, even in galaxies below the MS.
C1 [Nelson, Erica June; van Dokkum, Pieter G.; Momcheva, Ivelina G.; Leja, Joel; van den Bosch, Frank C.; Oesch, Pascal A.; Dickey, Claire; Lange, Johannes Ulf] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Schreiber, Natascha M. Foerster; Wuyts, Stijn; Tacconi, Linda J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Franx, Marijn; Fumagalli, Mattia; Labbe, Ivo] Leiden Univ, Leiden Observ, Leiden, Netherlands.
[Brammer, Gabriel B.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Wuyts, Stijn] Univ Bath, Dept Phys, Bath BA2 7AY, Avon, England.
[Whitaker, Katherine E.] Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Skelton, Rosalind E.] South African Astron Observ, POB 9, ZA-7935 Observatory, South Africa.
[Hayward, Christopher C.] CALTECH, TAPIR, Pasadena, CA 91125 USA.
[Hayward, Christopher C.] Harvard Smithsonian CfA, Cambridge, MA 02138 USA.
[Kriek, Mariska] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Rix, Hans-Walter; van der Wel, Arjen] MPIA, Konigstuhl 17, Heidelberg, Germany.
RP Nelson, EJ (reprint author), Yale Univ, Dept Astron, New Haven, CT 06511 USA.
RI Skelton, Rosalind/S-1845-2016
OI Skelton, Rosalind/0000-0001-7393-3336
FU 3D-HST Treasury Program [GO 12177, 12328]; NASA [NAS5-26555]; National
Science Foundation Graduate Research Fellowship
FX We thank the referee for their thoughtful report,. which improved the
paper. This work is based on observations taken by the 3D-HST Treasury
Program (GO 12177 and 12328) with the NASA/ESA HST, which is operated by
the Associations of Universities for Research in Astronomy, Inc., under
NASA contract NAS5-26555. E.J.N. gratefully acknowledges support from
the National Science Foundation Graduate Research Fellowship.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
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JI Astrophys. J.
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PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EA8OE
UT WOS:000386894900027
ER
PT J
AU Odegard, N
Kogut, A
Chuss, DT
Miller, NJ
AF Odegard, N.
Kogut, A.
Chuss, D. T.
Miller, N. J.
TI ASSESSMENT OF MODELS OF GALACTIC THERMAL DUST EMISSION USING COBE/FIRAS
AND COBE/DIRBE OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; infrared: ISM; submillimeter: ISM
ID BACKGROUND EXPERIMENT SEARCH; TEMPERATURE-DEPENDENCE; AMORPHOUS SOLIDS;
COBE FIRAS; ABSORPTION-COEFFICIENT; SPECTRAL OBSERVATIONS;
INFRARED-EMISSION; GAL OBSERVATIONS; COLD CLUMPS; PLANCK
AB Accurate modeling of the spectrum of thermal dust emission at millimeter wavelengths is important for improving the accuracy of foreground subtraction for cosmic microwave background (CMB) measurements, for improving the accuracy with which the contributions of different foreground emission components can be determined, and for improving our understanding of dust composition and dust physics. We fit four models of dust emission to high Galactic latitude COBE/FIRAS and COBE/DIRBE observations from 3 mm to 100 mu m and compare the quality of the fits. We consider the two-level systems (TLS) model because it provides a physically motivated explanation for the observed long wavelength flattening of the dust spectrum and the anti-correlation between emissivity index and dust temperature. We consider the model of Finkbeiner et al. because it has been widely used for CMB studies, and the generalized version of this model that was recently applied to Planck data by Meisner and Finkbeiner. For comparison we have also fit a phenomenological model consisting of the sum of two graybody components. We find that the two-graybody model gives the best fit and the FDS model gives a significantly poorer fit than the other models. The Meisner and Finkbeiner model and the TLS model remain viable for use in Galactic foreground subtraction, but the FIRAS data do not have a sufficient signal-to-noise ratio to provide a strong test of the predicted spectrum at millimeter wavelengths.
C1 [Odegard, N.] NASA, Goddard Space Flight Ctr, ADNET Syst Inc, Code 665, Greenbelt, MD 20771 USA.
[Kogut, A.; Miller, N. J.] NASA, Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA.
[Chuss, D. T.] Villanova Univ, Dept Phys, 800 E Lancaster Ave, Villanova, PA 19085 USA.
[Miller, N. J.] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.
RP Odegard, N (reprint author), NASA, Goddard Space Flight Ctr, ADNET Syst Inc, Code 665, Greenbelt, MD 20771 USA.
EM Nils.Odegard@nasa.gov
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J9 ASTROPHYS J
JI Astrophys. J.
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SC Astronomy & Astrophysics
GA EA8OE
UT WOS:000386894900016
ER
PT J
AU Parmentier, V
Fortney, JJ
Showman, AP
Morley, C
Marley, MS
AF Parmentier, Vivien
Fortney, Jonathan J.
Showman, Adam P.
Morley, Caroline
Marley, Mark S.
TI TRANSITIONS IN THE CLOUD COMPOSITION OF HOT JUPITERS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: atmospheres; planets and satellites: gaseous
planets; radiative transfer; scattering
ID 3-DIMENSIONAL ATMOSPHERIC CIRCULATION; EXTRASOLAR GIANT PLANETS; GREY
ANALYTICAL-MODEL; EXOPLANET HD 189733B; OPTICAL-PHASE CURVES; MASS DWARF
STARS; BROWN DWARFS; IRRADIATED ATMOSPHERES; THERMAL STRUCTURE;
TRANSMISSION SPECTRUM
AB Over a large range of equilibrium temperatures, clouds shape the transmission spectrum of hot Jupiter atmospheres, yet their composition remains unknown. Recent observations show that the Kepler light. curves of some hot Jupiters are asymmetric: for the hottest planets, the light. curve peaks before secondary eclipse, whereas for planets cooler than similar to 1900 K, it peaks after secondary eclipse. We use the thermal structure from 3D global circulation models to determine the expected cloud distribution and Kepler light. curves of hot Jupiters. We demonstrate that the change from an optical light. curve dominated by thermal emission to one dominated by scattering (reflection) naturally explains the observed trend from negative to positive offset. For the cool planets the presence of an asymmetry in the Kepler light curve is a telltale sign of the cloud composition, because each cloud species can produce an offset only over a narrow range of effective temperatures. By comparing our models and the observations, we show that the cloud composition of hot Jupiters likely varies with equilibrium temperature. We suggest that a transition occurs between silicate and manganese sulfide clouds at a temperature near 1600 K, analogous to the L/T transition on brown dwarfs. The cold trapping of cloud species below the photosphere naturally produces such a transition and predicts similar transitions for other condensates, including TiO. We predict that most hot Jupiters should have cloudy nightsides, that partial cloudiness should be common at the limb, and that the dayside hot spot should often be cloud-free.
C1 [Parmentier, Vivien; Fortney, Jonathan J.; Morley, Caroline] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Parmentier, Vivien; Showman, Adam P.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Parmentier, Vivien; Showman, Adam P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Marley, Mark S.] NASA, Ames Res Ctr, MS-245-3, Moffett Field, CA 94035 USA.
RP Parmentier, V (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.; Parmentier, V (reprint author), Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.; Parmentier, V (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
OI Marley, Mark/0000-0002-5251-2943
FU Sagan Postdoctoral Fellowship through NASA Exoplanet Science Institute;
Origins grant [NNX12AI196]
FX We thank Mike Line for reading the manuscript and providing useful
comments and Kevin Stevenson for useful discussions. V. P. acknowledges
support from the Sagan Postdoctoral Fellowship through the NASA
Exoplanet Science Institute. A.P.S. was supported by Origins grant
NNX12AI196.
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JI Astrophys. J.
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SC Astronomy & Astrophysics
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UT WOS:000386894900022
ER
PT J
AU Sadykov, VM
Kosovichev, AG
Sharykin, IN
Zimovets, IV
Dominguez, SV
AF Sadykov, Viacheslav M.
Kosovichev, Alexander G.
Sharykin, Ivan N.
Zimovets, Ivan V.
Vargas Dominguez, Santiago
TI RELATIONSHIP BETWEEN CHROMOSPHERIC EVAPORATION AND MAGNETIC FIELD
TOPOLOGY IN AN M-CLASS SOLAR FLARE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: activity; Sun: chromosphere; Sun: flares; Sun: magnetic fields;
Sun: UV radiation; techniques: spectroscopic
ID LOOP RADIATIVE HYDRODYNAMICS; QUASI-SEPARATRIX LAYERS;
REGION-IMAGING-SPECTROGRAPH; SLIP-RUNNING RECONNECTION; THICK-TARGET;
RESOLUTION OBSERVATIONS; MODEL; IRIS; DYNAMICS; PLASMA
AB Chromospheric evaporation is observed as Doppler blueshift during solar flares. It plays a key role in the dynamics and energetics of solar flares; however, its mechanism is still unknown. In this paper,. we present a detailed analysis of spatially resolved multi-wavelength observations of chromospheric evaporation during an M 1.0-class solar flare (SOL2014-06-12T21:12) using data from NASA's Interface Region Imaging Spectrograph and HMI/SDO (the. Helioseismic and Magnetic Imager on. board. the. Solar Dynamics Observatory), and high-resolution observations from VIS/NST (the. Visible Imaging Spectrometer at the. New Solar Telescope). The results show that the averaged over the flare region Fe XXI blueshift of the hot (10(7) K) evaporating plasma is delayed relative to the C II redshift of the relatively cold (10(4) K) chromospheric plasma by about one minute. The spatial distribution of the delays is not uniform across the region and can be as long as two minutes in several zones. Using vector magnetograms from HMI, we reconstruct the magnetic field topology and the quasi-separatrix layer, and find that the blueshift delay regions as well as the Ha flare ribbons are connected to the region of the. magnetic polarity inversion line (PIL) and an expanding flux rope via a system of low-lying loop arcades with a. height of less than or similar to 4.5 Mm. As a result, the chromospheric evaporation may be driven by the energy release in the vicinity of PIL, and has the observed properties due to a local magnetic field topology.
C1 [Sadykov, Viacheslav M.; Kosovichev, Alexander G.] New Jersey Inst Technol, Dept Phys, Newark, NJ 07102 USA.
[Kosovichev, Alexander G.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kosovichev, Alexander G.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Sharykin, Ivan N.; Zimovets, Ivan V.] Russian Acad Sci, Space Res Inst IKI, Moscow 117997, Russia.
[Vargas Dominguez, Santiago] Univ Nacl Colombia, Observ Astron, Sede Bogota, Carrera 45 26-85, Bogota, Colombia.
RP Sadykov, VM (reprint author), New Jersey Inst Technol, Dept Phys, Newark, NJ 07102 USA.
RI Zimovets, Ivan/E-4431-2017
OI Zimovets, Ivan/0000-0001-6995-3684
FU NJIT; US NSF [AGS-1250818]; NASA [NNX13AG14G, NNX14AB68G, NNX14AB70G,
NNX11AO736]; Korea Astronomy and Space Science Institute; Seoul National
University; strategic priority research program of CAS [XDB09000000];
ESA; Norwegian Space Centre; NSF [AGS-1250818]; RFBR [15-32-21078,
16-32-00462]
FX The authors acknowledge the BBSO, IRIS, and SDO mission teams for their
contribution and support. The BBSO operation is supported by NJIT, US
NSF AGS-1250818, and NASA NNX13AG14G grants, and the NST operation is
partly supported by the Korea Astronomy and Space Science Institute and
Seoul National University and by the strategic priority research program
of CAS with grant No. XDB09000000. IRIS is a NASA small explorer mission
developed and operated by LMSAL with mission operations executed at the
NASA Ames Research Center and major contributions to downlink
communications funded by ESA and the Norwegian Space Centre. The authors
thank NASA's SDO HMI team for the availability of the high-quality
scientific data. The authors also thank the. anonymous referee for
valuable comments. The work was partially supported by NASA grants
NNX14AB68G, NNX14AB70G, and NNX11AO736; NSF grant AGS-1250818; RFBR
grants 15-32-21078 and 16-32-00462; and an NJIT grant.
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JI Astrophys. J.
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PG 9
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SC Astronomy & Astrophysics
GA EA8OE
UT WOS:000386894900004
ER
PT J
AU Watson, DM
Calvet, NP
Fischer, WJ
Forrest, WJ
Manoj, P
Megeath, ST
Melnick, GJ
Najita, J
Neufeld, DA
Sheehan, PD
Stutz, AM
Tobin, JJ
AF Watson, Dan M.
Calvet, Nuria P.
Fischer, William J.
Forrest, W. J.
Manoj, P.
Megeath, S. Thomas
Melnick, Gary J.
Najita, Joan
Neufeld, David A.
Sheehan, Patrick D.
Stutz, Amelia M.
Tobin, John J.
TI EVOLUTION OF MASS OUTFLOW IN PROTOSTARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Herbig-Haro objects; ISM: jets and outflows; shock waves; stars: jets;
stars: pre-main sequence stars: protostars
ID SPITZER-SPACE-TELESCOPE; YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS;
T-TAURI STARS; MAGNETOCENTRIFUGALLY DRIVEN FLOWS; PROTOSTELLAR ACCRETION
DISCS; FAST INTERSTELLAR SHOCKS; O I LINE; 63 MU-M; C-II
AB We have surveyed 84 Class 0, Class I, and flat-spectrum protostars in mid-infrared [Si II], [Fe II], and [S I] line emission, and 11 of these in far-infrared [O I] emission. We use the results to derive their mass. outflow rates, (M) over dot(w). Thereby we observe a strong correlation of (M) over dot(w) with bolometric luminosity, and with the inferred mass accretion rates of the central objects, (M) over dot(a), which continues through the Class 0 range the trend observed in Class II young stellar objects. Along this trend from large to small mass. flow rates, the different classes of young stellar objects lie in the sequence Class 0-Class I/flat-spectrum-Class II, indicating that the trend is an evolutionary sequence in which (M) over dot(a) and (M) over dot(w) decrease together with increasing age, while maintaining rough proportionality. The survey results include two that. are key tests of magnetocentrifugal outflow-acceleration mechanisms: the distribution of the outflow/accretion branching ratio b = (M) over dot(w)/(M) over dot(a), and limits on the distribution of outflow speeds. Neither rules out any of the three leading outflow-acceleration, angular-momentum-ejection mechanisms, but they provide some evidence that disk winds and accretion-powered stellar winds (APSWs) operate in many protostars. An upper edge observed in the branching-ratio distribution is consistent with the upper bound of b = 0.6 found in models of APSWs, and a large fraction (31%) of the sample have a. branching ratio sufficiently small that only disk winds, launched on scales as large as several au, have been demonstrated to account for them.
C1 [Watson, Dan M.; Forrest, W. J.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
[Calvet, Nuria P.] Univ Michigan, Dept Astron, 825 Dennison Bldg,500 Church St, Ann Arbor, MI 48109 USA.
[Fischer, William J.; Megeath, S. Thomas] Univ Toledo, Dept Phys & Astron, 2801 W Bancroft St, Toledo, OH 43606 USA.
[Fischer, William J.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Manoj, P.] Tata Inst Fundamental Res, Homi Bhabha Rd, Bombay 400005, Maharashtra, India.
[Melnick, Gary J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Najita, Joan] Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85719 USA.
[Neufeld, David A.] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.
[Sheehan, Patrick D.] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA.
[Stutz, Amelia M.] Max Planck Inst Astron, Koenigstuhl 17, D-69117 Heidelberg, Germany.
[Tobin, John J.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
RP Watson, DM (reprint author), Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
EM dmw@pas.rochester.edu
FU NASA [NNX14AF79G]
FX We are grateful to Ingrid Koch for her help with the IRS data reduction.
This work was supported in part by NASA grant NNX14AF79G.
NR 77
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 SEP 1
PY 2016
VL 828
IS 1
AR 52
DI 10.3847/0004-637X/828/1/52
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA EA8OE
UT WOS:000386894900052
ER
PT J
AU Koster, RD
Brocca, L
Crow, WT
Burgin, MS
De Lannoy, GJM
AF Koster, Randal D.
Brocca, Luca
Crow, Wade T.
Burgin, Mariko S.
De Lannoy, Gabrielle J. M.
TI Precipitation estimation using L-band and C-band soil moisture
retrievals
SO WATER RESOURCES RESEARCH
LA English
DT Article
DE precipitation; soil moisture; remote sensing
ID TIME SATELLITE PRECIPITATION; DATA SETS; RAINFALL
AB An established methodology for estimating precipitation amounts from satellite-based soil moisture retrievals is applied to L-band products from the Soil Moisture Active Passive (SMAP) and Soil Moisture and Ocean Salinity (SMOS) satellite missions and to a C-band product from the Advanced Scatterometer (ASCAT) mission. The precipitation estimates so obtained are evaluated against in situ (gauge-based) precipitation observations from across the globe. The precipitation estimation skill achieved using the L-band SMAP and SMOS data sets is higher than that obtained with the C-band product, as might be expected given that L-band is sensitive to a thicker layer of soil and thereby provides more information on the response of soil moisture to precipitation. The square of the correlation coefficient between the SMAP-based precipitation estimates and the observations (for aggregations to approximate to 100 km and 5 days) is on average about 0.6 in areas of high rain gauge density. Satellite missions specifically designed to monitor soil moisture thus do provide significant information on precipitation variability, information that could contribute to efforts in global precipitation estimation.
C1 [Koster, Randal D.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Brocca, Luca] CNR, Res Inst Geohydrol Protect, Perugia, Italy.
[Crow, Wade T.] USDA, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA.
[Burgin, Mariko S.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[De Lannoy, Gabrielle J. M.] Katholieke Univ Leuven, Dept Earth & Environm Sci, Heverlee, Belgium.
RP Koster, RD (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
EM randal.d.koster@nasa.gov
RI Brocca, Luca/F-2854-2010; Koster, Randal/F-5881-2012
OI Brocca, Luca/0000-0002-9080-260X; Koster, Randal/0000-0001-6418-6383
FU NASA SMAP mission; SMAP Science Team; Italian Department of Civil
Protection
FX 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 (NASA). This work (mainly carried
out at the NASA Goddard Space Flight Center) was supported by the NASA
SMAP mission and the SMAP Science Team. Author Brocca appreciates
support from the Italian Department of Civil Protection. Qing Liu and
Clara Draper assisted with the processing of the data. SMAP data are
available from https://nsidc.org/data/smap, SMOS data from
https://smos-ds-02.eo.esa.int/oads/access/, and ASCAT data from
http://www.eumetsat.int/website/home/index.htm. Precipitation data are
available from
ftp://ftp.cpc.ncep.noaa.gov/precip/CPC_UNI_PRCP/GAUGE_GLB.
NR 28
TC 4
Z9 4
U1 8
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0043-1397
EI 1944-7973
J9 WATER RESOUR RES
JI Water Resour. Res.
PD SEP
PY 2016
VL 52
IS 9
BP 7213
EP 7225
DI 10.1002/2016WR019024
PG 13
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA EA9QC
UT WOS:000386977900029
ER
PT J
AU Wiese, DN
Landerer, FW
Watkins, MM
AF Wiese, David N.
Landerer, Felix W.
Watkins, Michael M.
TI Quantifying and reducing leakage errors in the JPL RL05M GRACE mascon
solution
SO WATER RESOURCES RESEARCH
LA English
DT Article
DE GRACE; postprocessing; mascon; leakage errors; gain factors
ID SEA-LEVEL; MASS; DECADE; OCEAN; SYSTEM
AB Recent advances in processing data from the Gravity Recovery and Climate Experiment (GRACE) have led to a new generation of gravity solutions constrained within a Bayesian framework to remove correlated errors rather than relying on empirical filters. The JPL RL05M mascon solution is one such solution, solving for mass variations using spherical cap mass concentration elements (mascons), while relying on external information provided by near-global geophysical models to constrain the solution. This new gravity solution is fundamentally different than the traditional spherical harmonic gravity solution, and as such, requires different care when postprocessing. Here we discuss two classes of postprocessing considerations for the JPL RL05M GRACE mascon solution: (1) reducing leakage errors across land/ocean boundaries, and (2) scaling the solutions to account for leakage errors introduced through parameterizing the gravity solution in terms of mascons. A Coastline Resolution Improvement (CRI) filter is developed to reduce leakage errors across coastlines. Synthetic simulations reveal a reduction in leakage errors of approximate to 50%, such that residual leakage errors are approximate to 1 cm equivalent water height (EWH) averaged globally. A set of gain factors is derived to reduce leakage errors for continental hydrology applications. The combined effect of the CRI filter coupled with application of the gain factors, is shown to reduce leakage errors when determining the mass balance of large (>160,000 km(2)) hydrological basins from 11% to 30% (0.6-1.5 mm EWH) averaged globally, with local improvements up to 38%-81% (9-19 mm EWH).
C1 [Wiese, David N.; Landerer, Felix W.; Watkins, Michael M.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Wiese, DN (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM david.n.wiese@jpl.nasa.gov
NR 31
TC 2
Z9 2
U1 2
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0043-1397
EI 1944-7973
J9 WATER RESOUR RES
JI Water Resour. Res.
PD SEP
PY 2016
VL 52
IS 9
BP 7490
EP 7502
DI 10.1002/2016WR019344
PG 13
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA EA9QC
UT WOS:000386977900044
ER
PT J
AU Molotch, NP
Barnard, DM
Burns, SP
Painter, TH
AF Molotch, Noah P.
Barnard, David M.
Burns, Sean P.
Painter, Thomas H.
TI Measuring spatiotemporal variation in snow optical grain size under a
subalpine forest canopy using contact spectroscopy
SO WATER RESOURCES RESEARCH
LA English
DT Article
DE snow; forests; snow grain size; spectroscopy; snow temperature;
snow-forest interactions
ID INFRARED REFLECTANCE; SURFACE-AREA; WATER EQUIVALENT; NUMERICAL-MODEL;
COVERED AREA; STRATIGRAPHY; ACCUMULATION; COVARIANCE; ABLATION; DENSITY
AB The distribution of forest cover exerts strong controls on the spatiotemporal distribution of snow accumulation and snowmelt. The physical processes that govern these controls are poorly understood given a lack of detailed measurements of snow states. In this study, we address one of many measurement gaps by using contact spectroscopy to measure snow optical grain size at high spatial resolution in trenches dug between tree boles in a subalpine forest. Trenches were collocated with continuous measurements of snow depth and vertical profiles of snow temperature and supplemented with manual measurements of snow temperature, geometric grain size, grain type, and density from trench walls. There was a distinct difference in snow optical grain size between winter and spring periods. In winter and early spring, when facetted snow crystal types were dominant, snow optical grain size was 6% larger in canopy gaps versus under canopy positions; a difference that was smaller than the measurement uncertainty. By midspring, the magnitude of snow optical grain size differences increased dramatically and patterns of snow optical grain size became highly directional with 34% larger snow grains in areas south versus north of trees. In winter, snow temperature gradients were up to 5-15 degrees C m(-1) greater under the canopy due to shallower snow accumulation. However, in canopy gaps, snow depths were greater in fall and early winter and therefore more significant kinetic growth metamorphism occurred relative to under canopy positions, resulting in larger snow grains in canopy gaps. Our findings illustrate the novelty of our method of measuring snow optical grain size, allowing for future studies to advance the understanding of how forest and meteorological conditions interact to impact snowpack evolution.
C1 [Molotch, Noah P.; Barnard, David M.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA.
[Molotch, Noah P.; Burns, Sean P.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA.
[Molotch, Noah P.; Painter, Thomas H.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Burns, Sean P.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
RP Molotch, NP (reprint author), Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA.; Molotch, NP (reprint author), Univ Colorado, Dept Geog, Boulder, CO 80309 USA.; Molotch, NP (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM noah.molotch@colorado.edu
RI Molotch, Noah/C-8576-2009; Painter, Thomas/B-7806-2016
FU U.S. National Aeronautics and Space Administration [NNXIIAK35A]; U.S.
National Science Foundation (NSF) [EAR 1141764]; U.S. Department of
Agriculture [2012-67003-19802]; NSF Niwot Ridge Long Term Ecological
Research program; Department of Energy Ameriflux program
FX This work was supported by the U.S. National Aeronautics and Space
Administration under grant NNXIIAK35A, by the U.S. National Science
Foundation (NSF) under grant EAR 1141764, and by the U.S. Department of
Agriculture under grant 2012-67003-19802. Additional support was
provided by the NSF Niwot Ridge Long Term Ecological Research program
and by the Department of Energy Ameriflux program. Part of this work was
conducted at the Jet Propulsion Laboratory, California Institute of
Technology under contract from NASA. Snow grain size data sets can be
downloaded from
ftp://snowserver.colorado.edu/pub/NWT_snow_grain_size_trenches2006/grain
-Size.zip. All meteorological data can be obtained from
http://fluxnet.ornl.gov/site/997.
NR 40
TC 0
Z9 0
U1 1
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0043-1397
EI 1944-7973
J9 WATER RESOUR RES
JI Water Resour. Res.
PD SEP
PY 2016
VL 52
IS 9
BP 7513
EP 7522
DI 10.1002/2016WR018954
PG 10
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA EA9QC
UT WOS:000386977900046
PM 27917006
ER
PT J
AU Jung-Kubiak, C
Reck, TJ
Siles, JV
Lin, R
Lee, C
Gill, J
Cooper, K
Mehdi, I
Chattopadhyay, G
AF Jung-Kubiak, Cecile
Reck, Theodore J.
Siles, Jose V.
Lin, Robert
Lee, Choonsup
Gill, John
Cooper, Ken
Mehdi, Imran
Chattopadhyay, Goutam
TI A Multistep DRIE Process for Complex Terahertz Waveguide Components
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Deep reactive-ion etching (DRIE); orthomode transducer (OMT); silicon
dioxide (SiO2); silicon micromachining; submillimeter waves; terahertz
(THz)
ID SATELLITE; GHZ
AB Asilicon deep reactive-ion etching (DRIE) process has been developed, using multiple SiO2 masks to enable multidepth waveguide features with +/- 2% tolerance. The unique capability of this process is demonstrated by designing, fabricating, and testing an orthomode transducer working in the 500-600 GHz frequency range. Straight waveguide measurements are also performed to characterize the losses associated with the multistep DRIE process, giving results slightly better than expected for metal-machined waveguides. This process enables the integration of multiple terahertz waveguide components such as mixers, multipliers, quadrature hybrids, and polarization twists onto a single silicon package.
C1 [Jung-Kubiak, Cecile; Reck, Theodore J.; Siles, Jose V.; Lin, Robert; Lee, Choonsup; Gill, John; Cooper, Ken; Mehdi, Imran; Chattopadhyay, Goutam] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA.
RP Jung-Kubiak, C (reprint author), CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA.
EM Cecile.D.Jung@jpl.nasa.gov; theodore.reck@jpl.nasa.gov;
Jose.V.Siles@jpl.nasa.gov; Robert.H.Lin@jpl.nasa.gov;
Choonsup.Lee@jpl.nasa.gov; John.J.Gill@jpl.nasa.gov;
Ken.B.Cooper@jpl.nasa.gov; imran.mehdi@jpl.nasa.gov;
goutam.chattopadhyay@jpl.nasa.gov
FU National Aeronautical and Space Administration
FX This work was carried out at the Jet Propulsion Laboratory, California
Institute of Technology supported under a contract with the National
Aeronautical and Space Administration.
NR 19
TC 1
Z9 1
U1 3
U2 3
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 SEP
PY 2016
VL 6
IS 5
BP 690
EP 695
DI 10.1109/TTHZ.2016.2593793
PG 6
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA DZ7QF
UT WOS:000386060200007
ER
PT J
AU Shah, U
Decrossas, E
Jung-Kubiak, C
Reck, T
Chattopadhyay, G
Mehdi, I
Oberhammer, J
AF Shah, Umer
Decrossas, Emmanuel
Jung-Kubiak, Cecile
Reck, Theodore
Chattopadhyay, Goutam
Mehdi, Imran
Oberhammer, Joachim
TI Submillimeter-Wave 3.3-bit RF MEMS Phase Shifter Integrated in
Micromachined Waveguide
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Micromachined waveguide; phase shifter; radio-frequency (RF)
microelectromechanical system (MEMS); rectangular waveguide;
submillimeter-wave; terahertz (THz)
ID E-PLANE; BAND; TECHNOLOGY; COMPONENTS; FILTERS
AB This paper presents a submillimeter-wave 500-550-GHz MEMS-reconfigurable phase shifter, which is based on loading a micromachined rectangular waveguide with 9 E-plane stubs. The phase shifter uses MEMS-reconfigurable surfaces to individually block/unblock the E-plane stubs from the micromachined waveguide. Each MEMS-reconfigurable surface is designed so that in the nonblocking state, it allows the electromagnetic wave to pass freely through it into the stub, while in the blocking state, it serves as the roof of the main waveguide and blocks the wave propagation into the stub. The phase-shifter design comprises three micromachined chips that are mounted in the H-plane cuts of the rectangular waveguide. Experimental results of the first device prototypes show that the microelectromechanical system (MEMS)- reconfigurable phase shifter has a linear phase shift of 20 degrees in ten discrete steps (3.3 bits). The measured insertion loss is better than 3 dB, of which only 0.5-1.5 dB is attributed to the MEMS surfaces and switched stubs, and the measured return loss is better than 15 dB in the design frequency band of 500-550 GHz. It is also shown that the major part of the insertion loss is attributed to misalignment and assembly uncertainties of the micromachined chips and the waveguide flanges, shown by simulations and reproducibility measurements. The MEMS-reconfigurable phase shifter is also operated in an analog tuning mode for high phase resolution. Furthermore, a detailed study has been carried out identifying the reason for the discrepancy between the simulated (90 degrees) and the measured (20 degrees) phase shift. Comb-drive actuators with spring constant variations between 2.13 and 8.71 N/m are used in the phase shifter design. An actuation voltage of 21.94 V with a reproducibility better than sigma = 0.0503 V is measured for the actuator design with a spring constant of 2.13 N/m. Reliability measurement on this actuator was performed in an uncontrolled laboratory environment and showed no deterioration in the functioning of the actuator observed over one hundred million cycles.
C1 [Shah, Umer; Oberhammer, Joachim] KTH Royal Inst Technol, Sch Elect Engn, Micro & Nanosyst, SE-10044 Stockholm, Sweden.
[Decrossas, Emmanuel; Jung-Kubiak, Cecile; Reck, Theodore; Chattopadhyay, Goutam; Mehdi, Imran] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Shah, U (reprint author), KTH Royal Inst Technol, Sch Elect Engn, Micro & Nanosyst, SE-10044 Stockholm, Sweden.
EM umers@kth.se; Emmanuel.Decrossas@jpl.nasa.gov;
Cecile.D.Jung@jpl.nasa.gov; theodore.reck@jpl.nasa.gov;
goutam.chattopadhyay@jpl.nasa.gov; imran.mehdi@jpl.nasa.gov;
joachim.oberhammer@ee.kth.se
OI Oberhammer, Joachim/0000-0003-3339-9137
FU European Research Council Consolidator Grant [616846]; Swedish
Foundation for Strategic Research Synergy Grant Electronics [SE13-007];
Nils and Hans Backmark scholarship
FX The contribution by KTH to this work was supported under the European
Research Council Consolidator Grant 616846, under the Swedish Foundation
for Strategic Research Synergy Grant Electronics SE13-007, and under a
Nils and Hans Backmark scholarship.
NR 19
TC 0
Z9 0
U1 7
U2 7
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 SEP
PY 2016
VL 6
IS 5
BP 706
EP 715
DI 10.1109/TTHZ.2016.2584924
PG 10
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA DZ7QF
UT WOS:000386060200009
ER
PT J
AU Kempes, CP
Wang, L
Amend, JP
Doyle, J
Hoehler, T
AF Kempes, Christopher P.
Wang, Lawrence
Amend, Jan P.
Doyle, John
Hoehler, Tori
TI Evolutionary tradeoffs in cellular composition across diverse bacteria
SO ISME JOURNAL
LA English
DT Article
ID ESCHERICHIA-COLI; AEROBACTER-AEROGENES; UNIFYING THEORY; SIZE CONTROL;
GROWTH; PROTEIN; CELLS; RATES; RNA; EUKARYOTES
AB One of the most important classic and contemporary interests in biology is the connection between cellular composition and physiological function. Decades of research have allowed us to understand the detailed relationship between various cellular components and processes for individual species, and have uncovered common functionality across diverse species. However, there still remains the need for frameworks that can mechanistically predict the tradeoffs between cellular functions and elucidate and interpret average trends across species. Here we provide a comprehensive analysis of how cellular composition changes across the diversity of bacteria as connected with physiological function and metabolism, spanning five orders of magnitude in body size. We present an analysis of the trends with cell volume that covers shifts in genomic, protein, cellular envelope, RNA and ribosomal content. We show that trends in protein content are more complex than a simple proportionality with the overall genome size, and that the number of ribosomes is simply explained by cross-species shifts in biosynthesis requirements. Furthermore, we show that the largest and smallest bacteria are limited by physical space requirements. At the lower end of size, cell volume is dominated by DNA and protein content-the requirement for which predicts a lower limit on cell size that is in good agreement with the smallest observed bacteria. At the upper end of bacterial size, we have identified a point at which the number of ribosomes required for biosynthesis exceeds available cell volume. Between these limits we are able to discuss systematic and dramatic shifts in cellular composition. Much of our analysis is connected with the basic energetics of cells where we show that the scaling of metabolic rate is surprisingly superlinear with all cellular components.
C1 [Kempes, Christopher P.] Santa Fe Inst, 1399 Hyde Pk Rd, Santa Fe, NM 87501 USA.
[Kempes, Christopher P.; Wang, Lawrence; Doyle, John] CALTECH, Control & Dynam Syst, Pasadena, CA 91125 USA.
[Kempes, Christopher P.; Hoehler, Tori] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Amend, Jan P.] Univ Southern Calif, Dept Earth Sci, Los Angeles, CA USA.
[Amend, Jan P.] Univ Southern Calif, Dept Biol Sci, Los Angeles, CA USA.
RP Kempes, CP (reprint author), Santa Fe Inst, 1399 Hyde Pk Rd, Santa Fe, NM 87501 USA.
EM ckempes@gmail.com
FU 'Life Underground' NASA Astrobiology Institute [NNA13AA92A]; Gordon and
Betty Moore Foundation
FX CPK acknowledges the support of the 'Life Underground' NASA Astrobiology
Institute (NNA13AA92A) and the Gordon and Betty Moore Foundation.
NR 41
TC 4
Z9 4
U1 13
U2 13
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1751-7362
EI 1751-7370
J9 ISME J
JI ISME J.
PD SEP
PY 2016
VL 10
IS 9
BP 2145
EP 2157
DI 10.1038/ismej.2016.21
PG 13
WC Ecology; Microbiology
SC Environmental Sciences & Ecology; Microbiology
GA EA5MK
UT WOS:000386664600007
PM 27046336
ER
PT J
AU Saghaian, SM
Karaca, HE
Tobe, H
Pons, J
Santamarta, R
Chumlyakov, YI
Noebe, RD
AF Saghaian, S. M.
Karaca, H. E.
Tobe, H.
Pons, J.
Santamarta, R.
Chumlyakov, Y. I.
Noebe, R. D.
TI Effects of Ni content on the shape memory properties and microstructure
of Ni-rich NiTi-20Hf alloys
SO SMART MATERIALS AND STRUCTURES
LA English
DT Article
DE Ni-rich NiTiHf; high temperature shape memory alloys; martensite
morphology; high strength
ID NITIHFPD SINGLE-CRYSTALS; MARTENSITIC-TRANSFORMATION; COMPRESSIVE
RESPONSE; BEHAVIOR; PHASE; TEMPERATURES; STRENGTH
AB Shape memory properties and microstructure of four Ni-rich NiTiHf alloys (Ni50.3Ti29.7Hf20, Ni50.7Ti29.3Hf20, Ni51.2Ti28.8Hf20, and Ni52Ti28Hf20 (at.%)) were systematically characterized in the furnace cooled condition. H-phase precipitates were formed during furnace cooling in compositions with greater than 50.3Ni and the driving force for nucleation increased with Ni content. Alloy strength increased while recoverable strain decreased with increasing Ni content due to changes in precipitate characteristics. When the precipitates were small (similar to 5-15 nm), they were readily absorbed by martensite plates, which resulted in maximum recoverable strain of 2% in Ni50.7Ti29.3Hf20. With increasing Ni content, the size (>100 nm) and volume fraction of precipitates increased and the growth of martensite plates was constrained between the precipitates when the Ni concentration was greater than 50.7 at.%. Near perfect dimensional stability with negligible irrecoverable strain was observed at stress levels as high as 2 GPa in the Ni52Ti28Hf20 alloy, though the recoverable strain was rather small. In general, strong local stress fields were created at precipitate/matrix interphases, which lead to high stored elastic energy during the martensitic transformation.
C1 [Saghaian, S. M.; Karaca, H. E.; Tobe, H.] Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA.
[Pons, J.; Santamarta, R.] Univ Illes Balears, Dept Fis, E-07122 Palma De Mallorca, Spain.
[Chumlyakov, Y. I.] Tomsk State Univ, Siberian Phys Tech Inst, Tomsk 634050, Russia.
[Noebe, R. D.] NASA, Glenn Res Ctr, Mat & Struct Div, Cleveland, OH USA.
RP Karaca, HE (reprint author), Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA.
EM karacahaluk@uky.edu
RI Chumlyakov, Yuriy/R-6496-2016
FU NASA Transformative Aeronautics Concepts Program (TACP),
Transformational Tools and Technologies Project; NASA EPSCOR program
[NNX11AQ31A]; RFBR [10-03-0154-a]; RSF program [14-29-00012]; Spanish
MINECO [MAT2011-28217-C02-01]; MECOMP-DGICT [MAT2014-56116-C4-1-R];
FEDER
FX This work was supported in part by the NASA Transformative Aeronautics
Concepts Program (TACP), Transformational Tools and Technologies Project
and the NASA EPSCOR program under grant No: NNX11AQ31A and RFBR project
with grant No: 10-03-0154-a and RSF program under grant No: 14-29-00012.
J Pons and R Santamarta also acknowledge the financial support from the
Spanish MINECO (ref. MAT2011-28217-C02-01), MECOMP-DGICT (ref.
MAT2014-56116-C4-1-R) and FEDER.
NR 42
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Z9 0
U1 12
U2 12
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0964-1726
EI 1361-665X
J9 SMART MATER STRUCT
JI Smart Mater. Struct.
PD SEP
PY 2016
VL 25
IS 9
AR 095029
DI 10.1088/0964-1726/25/9/095029
PG 11
WC Instruments & Instrumentation; Materials Science, Multidisciplinary
SC Instruments & Instrumentation; Materials Science
GA DZ6UJ
UT WOS:000385997500029
ER
PT J
AU Meskhidze, N
Johnson, MS
Hurley, D
Dawson, K
AF Meskhidze, Nicholas
Johnson, Matthew S.
Hurley, David
Dawson, Kyle
TI Influence of measurement uncertainties on fractional solubility of iron
in mineral aerosols over the oceans
SO AEOLIAN RESEARCH
LA English
DT Article
DE Soluble iron; Mineral dust; Measurement techniques; 3-D chemical
transport model
ID DRY DEPOSITION; SIZE DISTRIBUTION; SAHARAN DUST; DISSOLUTION; MODEL;
DISTRIBUTIONS; TRANSPORT; PACIFIC; CYCLE; FE
AB The atmospheric supply of mineral dust iron (Fe) plays a crucial role in the Earth's biogeochemical cycle and is of specific importance as a micronutrient in the marine environment. Observations show several orders of magnitude variability in the fractional solubility of Fe in mineral dust aerosols, making it hard to assess the role of mineral dust in the global ocean biogeochemical Fe cycle. In this study we compare the operational solubility of mineral dust aerosol Fe associated with the flow-through leaching protocol to the results of the global 3-D chemical transport model GEOS-Chem. According to the protocol, aerosol Fe is defined as soluble by first deionized water leaching of mineral dust through a 0.45 mu m pore size membrane followed by acidification and storage of the leachate over a long period of time prior to analysis. To estimate the uncertainty in soluble Fe results introduced by the flow-through leaching protocol, we prescribe an average 50% (range of 30-70%) fractional solubility to sub-0.45 mu m sized mineral dust particles that may inadvertently pass the filter and end up in the acidified (at pH similar to 1.7) leachate for a couple of month period. In the model, the fractional solubility of Fe is either explicitly calculated using a complex mineral aerosol Fe dissolution equations; or prescribed to be 1% and 4% often used by global ocean biogeochemical Fe cycle models to reproduce the broad characteristics of the presently observed ocean dissolved iron distribution. Calculations show that the fractional solubility of Fe derived through the flow-through leaching is higher compared to the model results. The largest differences (similar to 40%) are predicted to occur farther away from the dust source regions, over the areas where sub-0.45 mu m sized mineral dust particles contribute a larger fraction of the total mineral dust mass. This study suggests that different methods used in soluble Fe measurements and inconsistences in the operational definition of filterable Fe in marine environment and soluble Fe in atmospheric aerosols are likely to contribute to the wide range of fractional solubility of aerosol Fe reported in the literature. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Meskhidze, Nicholas; Hurley, David; Dawson, Kyle] North Carolina State Univ, Marine Earth & Atmospher Sci, Raleigh, NC 27695 USA.
[Johnson, Matthew S.] NASA, Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA.
RP Meskhidze, N (reprint author), North Carolina State Univ, Marine Earth & Atmospher Sci, Raleigh, NC 27695 USA.
EM nmeskhidze@ncsu.edu
RI Chem, GEOS/C-5595-2014;
OI Dawson, Kyle/0000-0003-3175-0456
FU NCSU Faculty Research & Professional Development Fund; Office of
Undergraduate Research at North Carolina State University; NASA High-End
Computing (HEC) Program through the NASA Advanced Supercomputing (NAS)
Division at NASA Ames Research Center
FX This research was supported by NCSU Faculty Research & Professional
Development Fund and the grant from the Office of Undergraduate Research
at North Carolina State University. The authors would like to thank
Daniel Jacob and the Harvard University Atmospheric Chemistry Modeling
Group for providing the base GEOS-Chem model used during our research.
Resources supporting this work were provided by the NASA High-End
Computing (HEC) Program through the NASA Advanced Supercomputing (NAS)
Division at NASA Ames Research Center. We also thank Dr. Akinori Ito
from the Japan Agency for Marine-Earth Science and Technology (JAMSTEC)
for providing the dust-Fe dissolution code used in Ito and Xu (2014).
NR 79
TC 1
Z9 1
U1 6
U2 6
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 1875-9637
EI 2212-1684
J9 AEOLIAN RES
JI Aeolian Res.
PD SEP
PY 2016
VL 22
BP 85
EP 92
DI 10.1016/j.aeolia.2016.07.002
PG 8
WC Geography, Physical
SC Physical Geography
GA DZ1NP
UT WOS:000385605400008
ER
PT J
AU Nicolas, MJ
Sullivan, RW
Richards, WL
AF Nicolas, Matthew J.
Sullivan, Rani W.
Richards, W. Lance
TI Large Scale Applications Using FBG Sensors: Determination of In-Flight
Loads and Shape of a Composite Aircraft Wing
SO AEROSPACE
LA English
DT Article
DE fiber Bragg grating; FBG; carbon composite wing; optical fiber strain
measurement; flight loads; wing deflection; wing shape; structural
health monitoring
ID FIBER-OPTIC SENSORS; BRAGG GRATING SENSORS; STRAIN
AB Technological advances have enabled the development of a number of optical fiber sensing methods over the last few years. The most prevalent optical technique involves the use of fiber Bragg grating (FBG) sensors. These small, lightweight sensors have many attributes that enable their use for a number of measurement applications. Although much literature is available regarding the use of FBGs for laboratory level testing, few publications in the public domain exist of their use at the operational level. Therefore, this paper gives an overview of the implementation of FBG sensors for large scale structures and applications. For demonstration, a case study is presented in which FBGs were used to determine the deflected wing shape and the out-of-plane loads of a 5.5-m carbon-composite wing of an ultralight aerial vehicle. The in-plane strains from the 780 FBG sensors were used to obtain the out-of-plane loads as well as the wing shape at various load levels. The calculated out-of-plane displacements and loads were within 4.2% of the measured data. This study demonstrates a practical method in which direct measurements are used to obtain critical parameters from the high distribution of FBG sensors. This procedure can be used to obtain information for structural health monitoring applications to quantify healthy vs. unhealthy structures.
C1 [Nicolas, Matthew J.] PACCAR Engine Co, Dept Mfg Engn, Columbus, MS 39701 USA.
[Sullivan, Rani W.] Mississippi State Univ, Dept Aerosp Engn, Mississippi State, MS 39762 USA.
[Richards, W. Lance] NASA Langley Res Ctr, NASA Engn & Safety Ctr, Hampton, VA 23681 USA.
RP Sullivan, RW (reprint author), Mississippi State Univ, Dept Aerosp Engn, Mississippi State, MS 39762 USA.
EM matthewnicolas52@gmail.com; sullivan@ae.msstate.edu;
lance.richards-1@nasa.gov
OI Nicolas, Matthew/0000-0001-9807-5817
FU NASA Armstrong Flight Research Center [AERO532 11020161]; Raspet Flight
Research Laboratory; NASA/Mississippi Space Grant Consortium [12040456
12070825]
FX The support provided for this study by the NASA Armstrong Flight
Research Center (Award No. AERO532 11020161), Raspet Flight Research
Laboratory, and the NASA/Mississippi Space Grant Consortium (Award No.
12040456 12070825) is gratefully acknowledged.
NR 38
TC 0
Z9 0
U1 5
U2 5
PU MDPI AG
PI BASEL
PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND
SN 2226-4310
J9 AEROSPACE
JI Aerospace
PD SEP
PY 2016
VL 3
IS 3
AR 18
DI 10.3390/aerospace3030018
PG 15
WC Engineering, Aerospace
SC Engineering
GA DZ0LQ
UT WOS:000385531300001
ER
PT J
AU Sree, D
Stephens, DB
AF Sree, Dave
Stephens, David B.
TI Improved Separation of Tone and Broadband Noise Components from Open
Rotor Acoustic Data
SO AEROSPACE
LA English
DT Article
DE acoustic; broadband; open rotor; phase-shift; segment-pair; separation;
spectrum; spike; tone
AB The term open rotor refers to unducted counter-rotating dual rotors or propellers used for propulsion. The noise generated by an open rotor is very complicated and requires special techniques for its analysis. The determination of its tone and broadband components is vital for properly assessing the noise control parameters and also for validating open rotor noise prediction codes. The data analysis technique developed by Sree for processing raw acoustic data of open rotors has been modified to yield much better results of tone and broadband separation particularly for the case when the two rotor speeds are approximately the same. The modified algorithm is found to eliminate most or all of the spikes previously observed in the broadband spectra computed from the original algorithm. A full description of the modified algorithm and examples of improved results from its application are presented in this paper.
C1 [Sree, Dave] Tuskegee Univ, Dept Mech Engn, Tuskegee, AL 36088 USA.
[Stephens, David B.] NASA, Acoust Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Sree, D (reprint author), Tuskegee Univ, Dept Mech Engn, Tuskegee, AL 36088 USA.
EM dave.sree@gmail.com; david.stephens@nasa.gov
FU NASA Environmentally Responsible Aviation project; GE Aviation,
Evendale, OH, USA; NASA Advanced Air Transportation Technology project
FX Sincere thanks and appreciation are expressed to Acoustics Branch at
NASA GRC for providing the non-proprietary open rotor acoustic data used
in this work, in particular to Daniel L. Sutliff regarding the mini-open
rotor data. The open rotor wind tunnel test campaign was funded by the
NASA Environmentally Responsible Aviation project, in collaboration with
GE Aviation, Evendale, OH, USA. The NASA Advanced Air Transportation
Technology project funded David B. Stephens during the preparation of
this report.
NR 14
TC 0
Z9 0
U1 0
U2 0
PU MDPI AG
PI BASEL
PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND
SN 2226-4310
J9 AEROSPACE
JI Aerospace
PD SEP
PY 2016
VL 3
IS 3
AR 29
DI 10.3390/aerospace3030029
PG 15
WC Engineering, Aerospace
SC Engineering
GA DZ0LQ
UT WOS:000385531300012
ER
PT J
AU Righter, K
Sutton, SR
Danielson, L
Pando, K
Newville, M
AF Righter, Kevin
Sutton, Steve R.
Danielson, Lisa
Pando, Kellye
Newville, Matt
TI Redox variations in the inner solar system with new constraints from
vanadium XANES in spinels
SO AMERICAN MINERALOGIST
LA English
DT Review
DE Oxygen fugacity; meteorites; solar nebula; spinel; chromite; vanadium;
Invited Centennial article
ID INTERPLANETARY DUST PARTICLES; COMET 81P/WILD 2; OXYGEN FUGACITY;
OXIDATION-STATE; CARBONACEOUS CHONDRITES; ENSTATITE CHONDRITES; MARTIAN
BASALTS; ELECTROCHEMICAL MEASUREMENTS; THERMODYNAMIC CONSTRAINTS;
LAYERED INTRUSION
AB Many igneous rocks contain mineral assemblages that are not appropriate for application of common mineral equilibria or oxybarometers to estimate oxygen fugacity. Spinel-structured oxides, common minerals in 1916 z A 2016 many igneous rocks, typically contain sufficient V for XANES measurements, allowing use of the correlation between oxygen fugacity and V K pre-edge peak intensity. Here we report V pre-edge peak intensities for a wide range of spinels from source rocks ranging from terrestrial basalt to achondrites to oxidized chondrites. The XANES measurements are used to calculate oxygen fugacity from experimentally produced spinels of known f(o2). We obtain values, in order of increasing f(o2), from IW-3 for lodranites and acapulcoites, to diogenites, brachinites (near IW), ALH 84001, terrestrial basalt, hornblende-bearing R chondrite LAP 04840 (IW+1.6), and finally ranging up to IW+3.1 for CK chondrites (where the Delta IW notation = logf(o2), of a sample relative to the logf(o2), of the IW buffer at specific 7). To place the significance of these new measurements into context we then review the range of oxygen fugacities recorded in major achondrite groups, chondritic and primitive materials, and planetary materials. This range extends from IW-8 to IW+2. Several chondrite groups associated with aqueous alteration exhibit values that are slightly higher than this range, suggesting that water and oxidation may be linked. The range in planetary materials is even wider than that defined by meteorite groups. Earth and Mars exhibit values higher than IW+2, due to a critical role played by pressure. Pressure allows dissolution of volatiles into magmas, which can later cause oxidation or reduction during fractionation, cooling, and degassing. Fluid mobility, either in the sub-arc mantle and crust, or in regions of metasomatism, can generate values >IW+2, again suggesting an important link between water and oxidation. At the very least, Earth exhibits a higher range of oxidation than other planets and astromaterials due to the presence of an O-rich atmosphere, liquid water, and hydrated interior. New analytical techniques and sample suites will revolutionize our understanding of oxygen fugacity variation in the inner solar system, and the origin of our solar system in general.
C1 [Righter, Kevin] NASA, JSC, NASA Pkwy, Houston, TX 77058 USA.
[Sutton, Steve R.; Newville, Matt] Univ Chicago, GSECARS, 9700 South Cass Ave,Bldg 434A, Argonne, IL 60439 USA.
[Danielson, Lisa; Pando, Kellye] Jacobs Engn, ESCG, Houston, TX 77058 USA.
RP Righter, K (reprint author), NASA, JSC, NASA Pkwy, Houston, TX 77058 USA.
EM kevin.righter-1@nasa.gov
FU RTOP from the NASA Cosmochemistry/Emerging Worlds programs; National
Science Foundation, Earth Sciences [EAR-1128799]; Department of
Energy-GeoSciences [DE-FG02-94ER14466]; DOE Office of Science
[DE-AC02-06CH11357]
FX This work was supported by an RTOP from the NASA Cosmochemistry/Emerging
Worlds programs. Portions of this work were performed at
GeoSoilEnviroCARS (Sector 13), Advanced Photon Source (APS), Argonne
National Laboratory. GeoSoilEnviroCARS is supported by the National
Science Foundation, Earth Sciences (EAR-1128799) and Department of
Energy-GeoSciences (DE-FG02-94ER14466). This research used resources of
the Advanced Photon Source, a U.S. Department of Energy (DOE) Office of
Science User Facility operated for the DOE Office of Science by Argonne
National Laboratory under Contract No. DE-AC02-06CH11357. All meteorite
samples were provided by the Meteorite Working Group except for the
acapulcoites/lodranites (J. Herrin), GRA 06128 (A. Treiman), and ALH
84001 (M. Righter). The manuscript benefitted from the careful reviews
and constructive comments of P. Burger, S. Paque, and AE S. Simon. We
thank K. Putirka for the invitation to contribute a paper in celebration
of the American Mineralogist centennial, and K.R. acknowledges the
enormous and continuing influence the Mineralogical Society of America
has had on his science and understanding of the natural world.
NR 140
TC 1
Z9 1
U1 8
U2 8
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 SEP-OCT
PY 2016
VL 101
IS 9-10
BP 1928
EP 1942
DI 10.2138/am-2016-5638
PG 15
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA DZ1NM
UT WOS:000385605100003
ER
PT J
AU Lee, S
Shen, ZZ
Xu, HF
AF Lee, Seungyeol
Shen, Zhizhang
Xu, Huifang
TI Study on nanophase iron oxyhydroxides in freshwater ferromanganese
nodules from Green Bay, Lake Michigan, with implications for the
adsorption of As and heavy metals
SO AMERICAN MINERALOGIST
LA English
DT Article
DE XRD; HRTEM; Z-contrast imaging; ab initio; two-line ferrihydrite;
proto-goethite; nanophase goethite; feroxyhyte; ferromanganese nodule;
arsenic
ID AB-INITIO; POWDER DIFFRACTION; STRUCTURAL MODEL; AKDALAITE MODEL;
FERRIHYDRITE; SPECIATION; SEDIMENTS; MANGANESE; FEOOH; MN
AB Nanophase Fe-oxyhydroxides in freshwater ferromanganese nodules (FFN) from Green Bay, Lake Michigan, and adsorbed arsenate have been investigated by X-ray powder diffraction (XRD), high-resolution transmission electron microscopy (HRTEM), Z-contrast imaging, and ab initio calculations using the density functional theory (DFT). The samples from northern Green Bay can be divided into two types: Fe-Mn nodules and Fe-rich nodules. The manganese-bearing phases are todorokite, birnessite, and buserite. The iron-bearing phases are feroxyhyte, nanophase goethite, two-line ferrihydrite, and nanophase FeOOH with guyanaite structure. Z-contrast images of the Fe-oxyhydroxides show ordered FeOOH nano-domains with guyanaite structure intergrown with nanophase goethite. The FeOOH nanophase is a precursor to the goethite. Henceforth, we will refer to it as "proto-goethite." DFT calculations indicate that goethite is more stable than proto-goethite. Our results suggest that ordering between Fe and vacancies in octahedral sites result in the transformation from feroxyhyte to goethite through a proto-goethite intermediate phase. Combining Z-contrast images and TEM-EDS reveals that arsenate (AsO43-) tetrahedra are preferentially adsorbed on the proto-goethite (001) surface via tridentate adsorption. Our study directly shows the atomic positions of Fe-oxyhydroxides with associated trace elements. The methods can be applied for identifying structures of nano-phases and adsorbed trace elements and heavy metals.
C1 [Lee, Seungyeol; Shen, Zhizhang; 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 NASA Astrobiology Institute [N07-5489]
FX The authors acknowledge the financial support from NASA Astrobiology
Institute (N07-5489). The authors thank Carl Bowser for providing the
samples and their locations, Hiromi Konishi for assistance in acquiring
Z-contrast images, Izabela Szlufarska for allowing us to access
computing facility, Gabor J. Kemeny of Middleton Spectral Vision and
Michael Beauchaine of Bruker AXS for XRF mapping. The authors also thank
Philip E. Brown, John W. Valley, Clark M. Johnson, Eric E. Roden, and
Franklin Hobbs for their helpful suggestions.
NR 53
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U1 8
U2 8
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 SEP-OCT
PY 2016
VL 101
IS 9-10
BP 1986
EP 1995
DI 10.2138/am-2016-5729
PG 10
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA DZ1NM
UT WOS:000385605100007
ER
PT J
AU Chan, QHS
Zolensky, ME
Martinez, JE
Tsuchiyama, A
Miyake, A
AF Chan, Queenie H. S.
Zolensky, Michael E.
Martinez, James E.
Tsuchiyama, Akira
Miyake, Akira
TI Magnetite plaquettes are naturally asymmetric materials in meteorites
SO AMERICAN MINERALOGIST
LA English
DT Article
DE Magnetite; plaquettes; carbonaceous chondrites; symmetry-breaking;
scanning electron microscopy; SEM; electron backscatter diffraction;
EBSD; synchrotron X-ray computed microtomography; SXRCT; aqueous
alteration; crystal structure
ID EXTRATERRESTRIAL AMINO-ACIDS; CARBONACEOUS CHONDRITE; TAGISH LAKE;
ADSORPTION; HOMOCHIRALITY; MINERALOGY; EVOLUTION; CRYSTALS; PARTICLES;
CHEMISTRY
AB Life on Earth shows preference toward the set of organics with particular spatial configurations. Enantiomeric excesses have been observed for a-methyl amino acids in meteorites, which suggests that chiral asymmetry might have an abiotic origin. A possible abiotic mechanism that could produce chiral asymmetry in meteoritic amino acids is their formation under the influence of asymmetric catalysts, as mineral crystallization can produce spatially asymmetric structures. Although magnetite plaquettes have been proposed to be a possible candidate for an asymmetric catalyst, based on the suggestion that they have a spiral structure, a comprehensive description of their morphology and interpretation of the mechanism associated with symmetry-breaking in biomolecules remain elusive. Here we report observations of magnetite plaquettes in carbonaceous chondrites (CC) that were made with scanning electron microscopy and synchrotron X-ray computed microtomography (SXRCT). We obtained the crystal orientation of the plaquettes using electron backscatter diffraction (EBSD) analysis. SXRCT permits visualization of the internal features of the plaquettes. It provides an unambiguous conclusion that the plaquettes are devoid of a spiral feature and, rather that they are stacks of individual magnetite disks that do not join to form a continuous spiral. Despite the lack of spiral features, our EBSD data show significant changes in crystal orientation between adjacent magnetite disks. The magnetite disks are displaced in a consistent relative direction that lead to an overall crystallographic rotational mechanism. This work offers an explicit understanding of the structures of magnetite plaquettes in CC, which provides a fundamental basis for future interpretation of the proposed symmetry-breaking mechanism.
C1 [Chan, Queenie H. S.; Zolensky, Michael E.] NASA, ARES, Johnson Space Ctr, Houston, TX 77058 USA.
[Martinez, James E.] Jacobs Engn, Houston, TX 77058 USA.
[Tsuchiyama, Akira; Miyake, Akira] Kyoto Univ, Grad Sch Sci, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan.
RP Chan, QHS (reprint author), NASA, ARES, Johnson Space Ctr, Houston, TX 77058 USA.
EM hschan@nasa.gov
FU NASA Cosmochemistry Program; NASA Postdoctoral Program at the Johnson
Space Center; Japan Ministry of Education, Culture, Sports, Science and
Technology [15H05695]
FX We acknowledge CAPTEM for loan of the Bench Crater sample, which is an
Apollo lunar sample. We thank Field Museum for Orgueil, Murchison,
Mighei, Renazzo, National Museum of Natural History for the Alais
meteorite sample, and American Museum of Natural History for the Ivuna
sample. This study was supported by the NASA Cosmochemistry Program
(M.E.Z. is the PI). Q.H.S.C. acknowledges support from the NASA
Postdoctoral Program at the Johnson Space Center, administered by the
Universities Space Research Association. A.T. was supported by a
Grant-in-aid of the Japan Ministry of Education, Culture, Sports,
Science and Technology (15H05695). We thank Tomoki Nakamura, John
Bradley, and Rhian Jones for careful reviews of the manuscript, and
Sandra Pizzarello, Jose Aponte, and Aaron Burton for the helpful
comments and insightful discussions. The microtomography experiment was
made by the project at SPring-8 (proposal no. 2015A1413) with help of
Kentaro Uesugi and Tsukasa Nakano.
NR 58
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U1 4
U2 4
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 SEP-OCT
PY 2016
VL 101
IS 9-10
BP 2041
EP 2050
DI 10.2138/am-2016-5604
PG 10
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA DZ1NM
UT WOS:000385605100012
ER
PT J
AU Gullikson, AL
Hagerty, JJ
Reid, MR
Rapp, JF
Draper, DS
AF Gullikson, Amber L.
Hagerty, Justin J.
Reid, Mary R.
Rapp, Jennifer F.
Draper, David S.
TI Silicic lunar volcanism: Testing the crustal melting model
SO AMERICAN MINERALOGIST
LA English
DT Article
DE Moon; silicic volcanism; crustal melting; partial melting experiments;
silicate liquid immiscibility
ID LIQUID IMMISCIBILITY; QUARTZ MONZODIORITE; MAIRAN DOMES; MOON; GRANITE;
PETROLOGY; GEOCHEMISTRY; GRUITHUISEN; CHEMISTRY; ROCKS
AB Lunar silicic rocks were first identified by granitic fragments found in samples brought to Earth by the Apollo missions, followed by the discovery of silicic domes on the lunar surface through remote sensing. Although these silicic lithologies are thought to make up a small portion of the lunar crust, their presence indicates that lunar crustal evolution is more complex than originally thought. Models currently used to describe the formation of silicic lithologies on the Moon include in situ differentiation of a magma, magma differentiation with silicate liquid immiscibility, and partial melting of the crust. This study focuses on testing a crustal melting model through partial melting experiments on compositions representing lithologies spatially associated with the silicic domes. The experiments were guided by the results of modeling melting temperatures and residual melt compositions of possible protoliths for lunar silicic rocks using the thermodynamic modeling software, rhyolite-MELTS.
Rhyolite-MELTS simulations predict liquidus temperatures of 950-1040 degrees C for lunar granites under anhydrous conditions, which guided the temperature range for the experiments. Monzogabbro, alkali gabbronorite, and KREEP basalt were identified as potential protoliths due to their ages, locations on the Moon (i.e., located near observed silicic domes), chemically evolved compositions, and the results from rhyolite-MELTS modeling. Partial melting experiments, using mixtures of reagent grade oxide powders representing bulk rock compositions of these rock types, were carried out at atmospheric pressure over the temperature range of 900-1100 degrees C. Because all lunar granite samples and remotely sensed domes have an elevated abundance of Th, some of the mixtures were doped with Th to observe its partitioning behavior.
Run products show that at temperatures of 1050 and 1100 degrees C, melts of the three protoliths are not silicic in nature (i.e., they have <63 wt% SiO2). By 1000 degrees C, melts of both monzogabbro and alkali gabbronorite approach the composition of granite, but are also characterized by immiscible Si-rich and Fe-rich liquids. Furthermore, Th strongly partitions into the Fe-rich, and not the Si-rich glass in all experimental runs.
Our work provides important constraints on the mechanism of silicic melt formation on the Moon. The observed high-Th content of lunar granite is difficult to explain by silicate liquid immiscibility, because through this process, Th is not fractionated into the Si-rich phase. Results of our experiments and modeling suggests that silicic lunar rocks could be produced from monzogabbro and alkali gabbronorite protoliths by partial melting at T < 1000 degrees C. Additionally, we speculate that at higher pressures (P >= 0.005 GPa), the observed immiscibility in the partial melting experiments would be suppressed.
C1 [Gullikson, Amber L.; Reid, Mary R.] Northern Univ Arizona, Flagstaff, AZ 86011 USA.
[Hagerty, Justin J.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Rapp, Jennifer F.] NASA, Johnson Space Ctr, Jacobs, Mail Code JE20, Houston, TX 77058 USA.
[Draper, David S.] NASA, Astromat Res Off, ARES Directorate, Johnson Space Ctr, Houston, TX USA.
RP Gullikson, AL (reprint author), Northern Univ Arizona, Flagstaff, AZ 86011 USA.
EM agullikson@usgs.gov
FU Geological Society of America; Sigma Xi; NAU Support for Graduate
Students program; Tom and Rose Bedwell Earth Physics Scholarship
FX We thank Brad Jolliff and Malcolm Rutherford for their insightful
comments, which greatly improved this paper. Funding for this work was
provided by the Geological Society of America research grant, Sigma Xi
Grants-in-Aid Research, the NAU Support for Graduate Students program,
and the Tom and Rose Bedwell Earth Physics Scholarship.
NR 68
TC 0
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U1 6
U2 6
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 SEP-OCT
PY 2016
VL 101
IS 9-10
BP 2312
EP 2321
DI 10.2138/am-2016-5619
PG 10
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA DZ1NM
UT WOS:000385605100034
ER
PT J
AU Singer, LP
Chen, HY
Holz, DE
Farr, WM
Price, LR
Raymond, V
Cenko, SB
Gehrels, N
Cannizzo, J
Kasliwal, MM
Nissanke, S
Coughlin, M
Farr, B
Urban, AL
Vitale, S
Veitch, J
Graff, P
Berry, CPL
Mohapatra, S
Mandel, I
AF Singer, Leo P.
Chen, Hsin-Yu
Holz, Daniel E.
Farr, Will M.
Price, Larry R.
Raymond, Vivien
Cenko, S. Bradley
Gehrels, Neil
Cannizzo, John
Kasliwal, Mansi M.
Nissanke, Samaya
Coughlin, Michael
Farr, Ben
Urban, Alex L.
Vitale, Salvatore
Veitch, John
Graff, Philip
Berry, Christopher P. L.
Mohapatra, Satya
Mandel, Ilya
TI SUPPLEMENT: "GOING THE DISTANCE: MAPPING HOST GALAXIES OF LIGO AND VIRGO
SOURCES IN THREE DIMENSIONS USING LOCAL COSMOGRAPHY AND TARGETED
FOLLOW-UP" (2016, ApJL, 829, L15)
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE catalogs; galaxies: distances and redshifts; gravitational waves;
surveys
AB This is a supplement to the Letter of Singer et al., in which we demonstrated a rapid algorithm for obtaining joint 3D estimates of sky location and luminosity distance from observations of binary neutron star mergers with Advanced LIGO and Virgo. We argued that combining the reconstructed volumes with positions and redshifts of possible host galaxies can provide large-aperture but small field of view instruments with a manageable list of targets to search for optical or infrared emission. In this Supplement, we document the new HEALPix-based file format for 3D localizations of gravitational-wave transients. We include Python sample code to show the reader how to perform simple manipulations of the 3D sky maps and extract ranked lists of likely host galaxies. Finally, we include mathematical details of the rapid volume reconstruction algorithm.
C1 [Singer, Leo P.; Cenko, S. Bradley; Gehrels, Neil; Cannizzo, John] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Mail Code 661, Greenbelt, MD 20771 USA.
[Chen, Hsin-Yu; Holz, Daniel E.; Farr, Ben] Univ Chicago, Enrico Fermi Inst, Dept Phys, Chicago, IL 60637 USA.
[Chen, Hsin-Yu; Holz, Daniel E.; Farr, Ben] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Farr, Will M.; Veitch, John; Berry, Christopher P. L.; Mandel, Ilya] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Price, Larry R.; Raymond, Vivien] CALTECH, LIGO Lab, Pasadena, CA 91125 USA.
[Raymond, Vivien] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Potsdam, Germany.
[Cenko, S. Bradley] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Kasliwal, Mansi M.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Nissanke, Samaya] Radboud Univ Nijmegen, Inst Math Astrophys & Particle Phys, Heyendaalseweg 135, NL-6525 AJ Nijmegen, Netherlands.
[Coughlin, Michael] Harvard Univ, Dept Phys & Astron, Cambridge, MA 02138 USA.
[Urban, Alex L.] Univ Wisconsin, Leonard E Parker Ctr Gravitat Cosmol & Astrophys, Milwaukee, WI 53201 USA.
[Vitale, Salvatore; Mohapatra, Satya] MIT, LIGO Lab, 185 Albany St, Cambridge, MA 02139 USA.
[Graff, Philip] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
RP Singer, LP (reprint author), NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Mail Code 661, Greenbelt, MD 20771 USA.
OI Singer, Leo/0000-0001-9898-5597; Chen, Hsin-Yu/0000-0001-5403-3762
FU NSF [1066293]
FX We thank the Aspen Center for Physics and NSF grant #1066293 for
hospitality during the conception, writing, and editing of this paper.
We thank P. Shawhan and F. Tombesi for detailed feedback on the
manuscript. The online data release is available at
https://dcc.ligo.org/P1500071/public/html. This is LIGO document
P1500071-v7.
NR 16
TC 1
Z9 1
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 SEP
PY 2016
VL 226
IS 1
AR 10
DI 10.3847/0067-0049/226/1/10
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DY8SH
UT WOS:000385400500001
ER
PT J
AU Jensen, MP
Petersen, WA
Bansemer, A
Bharadwaj, N
Carey, LD
Cecil, DJ
Collis, SM
Del Genio, AD
Dolan, B
Gerlach, J
Giangrande, SE
Heymsfield, A
Heymsfield, G
Kollias, P
Lang, TJ
Nesbitt, SW
Neumann, A
Poellot, M
Rutledge, SA
Schwaller, M
Tokay, A
Williams, CR
Wolff, DB
Xie, S
Zipser, EJ
AF Jensen, M. P.
Petersen, W. A.
Bansemer, A.
Bharadwaj, N.
Carey, L. D.
Cecil, D. J.
Collis, S. M.
Del Genio, A. D.
Dolan, B.
Gerlach, J.
Giangrande, S. E.
Heymsfield, A.
Heymsfield, G.
Kollias, P.
Lang, T. J.
Nesbitt, S. W.
Neumann, A.
Poellot, M.
Rutledge, S. A.
Schwaller, M.
Tokay, A.
Williams, C. R.
Wolff, D. B.
Xie, S.
Zipser, E. J.
TI THE MIDLATITUDE CONTINENTAL CONVECTIVE CLOUDS EXPERIMENT (MC3E)
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID RADIATION MEASUREMENT PROGRAM; ATMOSPHERIC RADIATION; POLARIMETRIC
RADAR; WIND PROFILERS; PRECIPITATION; RADIOMETER; RESOLUTION; MESOSCALE;
SYSTEMS; GHZ
AB The Midlatitude Continental Convective Clouds Experiment (MC3E), a field program jointly led by the U.S. Department of Energy's Atmospheric Radiation Measurement (ARM) Program and the National Aeronautics and Space Administration's (NASA) Global Precipitation Measurement (GPM) mission, was conducted in south-central Oklahoma during April-May 2011. MC3E science objectives were motivated by the need to improve our understanding of midlatitude continental convective cloud system life cycles, microphysics, and GPM precipitation retrieval algorithms. To achieve these objectives, a multi scale surface- and aircraft-based in situ and remote sensing observing strategy was employed. A variety of cloud and precipitation events were sampled during MC3E, of which results from three deep convective events are highlighted. Vertical structure, air motions, precipitation drop size distributions, and ice properties were retrieved from multiwavelength radar, profiler, and aircraft observations for a mesoscale convective system (MCS) on 11 May. Aircraft observations for another MCS observed on 20 May were used to test agreement between observed radar reflectivities and those calculated with forward-modeled reflectivity and microwave brightness temperatures using in situ particle size distributions and ice water content. Multiplatform observations of a supercell that occurred on 23 May allowed for an integrated analysis of kinematic and microphysical interactions. A core updraft of 25 m supported growth of hail and large raindrops. Data collected during the MC3E campaign are being used in a number of current and ongoing research projects and are available through the ARM and NASA data archives.
C1 [Jensen, M. P.; Giangrande, S. E.] Brookhaven Natl Lab, POB 5000,MS 490D, Upton, NY 11973 USA.
[Petersen, W. A.; Gerlach, J.; Heymsfield, G.; Schwaller, M.; Tokay, A.; Wolff, D. B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Petersen, W. A.; Gerlach, J.; Wolff, D. B.] NASA, Wallops Flight Facil, Wallops Isl, VA USA.
[Bansemer, A.; Heymsfield, A.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
[Bharadwaj, N.] Pacific Northwest Natl Lab, Richland, WA USA.
[Carey, L. D.] Univ Alabama, Huntsville, AL 35899 USA.
[Cecil, D. J.; Lang, T. J.] NASA, Marshall Space Flight Ctr, Huntsville, AL USA.
[Collis, S. M.] Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA.
[Del Genio, A. D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Dolan, B.; Rutledge, S. A.] Colorado State Univ, Ft Collins, CO 80523 USA.
[Kollias, P.] McGill Univ, Montreal, PQ, Canada.
[Nesbitt, S. W.] Univ Illinois, Urbana, IL USA.
[Neumann, A.; Poellot, M.] Univ North Dakota, Grand Forks, ND USA.
[Tokay, A.] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA.
[Williams, C. R.] Univ Colorado, Boulder, CO 80309 USA.
[Xie, S.] Lawrence Livermore Natl Lab, Livermore, CA USA.
[Zipser, E. J.] Univ Utah, Salt Lake City, UT USA.
RP Jensen, MP (reprint author), Brookhaven Natl Lab, POB 5000,MS 490D, Upton, NY 11973 USA.
EM mjensen@bnl.gov
RI Xie, Shaocheng/D-2207-2013
OI Xie, Shaocheng/0000-0001-8931-5145
FU U.S. Department of Energy's ARM Program; NASA's Global Precipitation
Measurement mission's Ground Validation Program; NASA [NNX10AN38G,
NNX10AH67G, NNX14AH06G]; U.S. Department of Energy, Office of Science,
Office of Biological and Environmental Research (BER), as part of the
Atmospheric System Research (ASR) program; U.S. Department of Energy,
Office of Science, Office of Biological and Environmental Research
(BER), as part of the ARM program; DOE [DE-SC0007016]; U.S. Department
of Energy [DE-AC02-98CH10886]
FX The MC3E field campaign was jointly funded by the U.S. Department of
Energy's ARM Program and NASA's Global Precipitation Measurement
mission's Ground Validation Program. We acknowledge the important
contributions of the ARM SGP site operations staff members for their
contributions to the siting, deployment, and maintenance of NASA MC3E
and SGP ARM Climate Facility instrumentation. We also acknowledge the
UND Citation flight and support crews for their excellent conduct of
airborne microphysical sampling, and Offutt AFB and Ponca City Regional
Airport for their hosting and field support of the NASA ER-2 and UND
Citation, respectively. Operations of the UND Citation aircraft were
funded under NASA Grant NNX10AN38G. MJ and SG were funded by the U.S.
Department of Energy, Office of Science, Office of Biological and
Environmental Research (BER), as part of the Atmospheric System Research
(ASR) and ARM programs. AH and AB were funded by NASA Grant NNX10AH67G.
SR and BD were funded by DOE Grant DE-SC0007016 and NASA Grant
NNX14AH06G. This paper has been coauthored by employees of Brookhaven
Science Associates, LLC, under Contract DE-AC02-98CH10886 with the U.S.
Department of Energy.
NR 56
TC 10
Z9 10
U1 6
U2 6
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 SEP
PY 2016
VL 97
IS 9
BP 1667
EP +
DI 10.1175/BAMS-D-14-00228.1
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DZ5PG
UT WOS:000385913400016
ER
PT J
AU Wood, R
Jensen, MP
Wang, J
Bretherton, CS
Burrows, SM
Del Genio, AD
Fridlind, AM
Ghan, SJ
Ghate, VP
Kollias, P
Krueger, SK
McGraw, RL
Miller, MA
Painemal, D
Russell, LM
Yuter, SE
Zuidema, P
AF Wood, Robert
Jensen, Michael P.
Wang, Jian
Bretherton, Christopher S.
Burrows, Susannah M.
Del Genio, Anthony D.
Fridlind, Ann M.
Ghan, Steven J.
Ghate, Virendra P.
Kollias, Pavlos
Krueger, Steven K.
McGraw, Robert L.
Miller, Mark A.
Painemal, David
Russell, Lynn M.
Yuter, Sandra E.
Zuidema, Paquita
TI PLANNING THE NEXT DECADE OF COORDINATED RESEARCH TO BETTER UNDERSTAND
AND SIMULATE MARINE LOW CLOUDS
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Editorial Material
ID STRATOCUMULUS
C1 [Wood, Robert; Bretherton, Christopher S.] Univ Washington, Seattle, WA 98195 USA.
[Jensen, Michael P.; Wang, Jian; McGraw, Robert L.] Brookhaven Natl Lab, Upton, NY 11973 USA.
[Burrows, Susannah M.; Ghan, Steven J.] Pacific Northwest Natl Lab, Richland, WA USA.
[Del Genio, Anthony D.; Fridlind, Ann M.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Ghate, Virendra P.] Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA.
[Kollias, Pavlos] SUNY Stony Brook, Stony Brook, NY 11794 USA.
[Krueger, Steven K.] Univ Utah, Salt Lake City, UT USA.
[Miller, Mark A.] Rutgers State Univ, New Brunswick, NJ USA.
[Painemal, David] NASA, Langley Res Ctr, Sci Syst & Applicat Inc, Hampton, VA 23665 USA.
[Russell, Lynn M.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
[Yuter, Sandra E.] North Carolina State Univ, Raleigh, NC USA.
[Zuidema, Paquita] Univ Miami, Miami, FL USA.
RP Wood, R (reprint author), Univ Washington, Dept Atmospher Sci, Box 351640, Seattle, WA 98195 USA.
EM robwood2@uw.edu
RI Ghan, Steven/H-4301-2011; Zuidema, Paquita/C-9659-2013; Wang,
Jian/G-9344-2011; Burrows, Susannah/A-7429-2011; Wood,
Robert/A-2989-2008
OI Ghan, Steven/0000-0001-8355-8699; Zuidema, Paquita/0000-0003-4719-372X;
Burrows, Susannah/0000-0002-0745-7252; Wood, Robert/0000-0002-1401-3828
NR 12
TC 0
Z9 0
U1 5
U2 5
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 SEP
PY 2016
VL 97
IS 9
BP 1699
EP 1702
DI 10.1175/BAMS-D-16-0160.1
PG 4
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DZ5PG
UT WOS:000385913400018
ER
PT J
AU Ichoku, C
Ellison, LT
Willmot, KE
Matsui, T
Dezfuli, AK
Gatebe, CK
Wang, J
Wilcox, EM
Lee, J
Adegoke, J
Okonkwo, C
Bolten, J
Policelli, FS
Habib, S
AF Ichoku, Charles
Ellison, Luke T.
Willmot, K. Elena
Matsui, Toshihisa
Dezfuli, Amin K.
Gatebe, Charles K.
Wang, Jun
Wilcox, Eric M.
Lee, Jejung
Adegoke, Jimmy
Okonkwo, Churchill
Bolten, John
Policelli, Frederick S.
Habib, Shahid
TI Biomass burning, land-cover change, and the hydrological cycle in
Northern sub-Saharan Africa
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE sub-Saharan Africa; biomass burning; water cycle; land cover change;
precipitation; fire
ID WESTERN EQUATORIAL AFRICA; FIRE DETECTION; CLIMATE-CHANGE; RAINFALL
VARIABILITY; TROPICAL OCEANS; SAHEL RAINFALL; SOIL-MOISTURE; LAKE CHAD;
PART I; SURFACE
AB The Northern Sub-Saharan African (NSSA) region, which accounts for 20%-25% of the global carbon emissions from biomass burning, also suffers from frequent drought episodes and other disruptions to the hydrological cycle whose adverse societal impacts have been widely reported during the last several decades. This paper presents a conceptual framework of the NSSA regional climate system components that may be linked to biomass burning, as well as detailed analyses of a variety of satellite data for 2001-2014 in conjunction with relevant model-assimilated variables. Satellite fire detections in NSSA show that the vast majority (>75%) occurs in the savanna and woody savanna land-cover types. Starting in the 2006-2007 burning season through the end of the analyzed data in 2014, peak burning activity showed a net decrease of 2-7%/yr in different parts of NSSA, especially in the savanna regions. However, fire distribution shows appreciable coincidence with land-cover change. Although there is variable mutual exchange of different land cover types, during 2003-2013, cropland increased at an estimated rate of 0.28%/yr of the total NSSA land area, with most of it (0.18%/yr) coming from savanna. During the last decade, conversion to croplands increased in some areas classified as forests and wetlands, posing a threat to these vital and vulnerable ecosystems. Seasonal peak burning is anti-correlated with annual water-cycle indicators such as precipitation, soil moisture, vegetation greenness, and evapotranspiration, except in humid West Africa (5 degrees-10 degrees latitude), where this anti-correlation occurs exclusively in the dry season and burning virtually stops when monthly mean precipitation reaches 4 mm d(-1). These results provide observational evidence of changes in land-cover and hydrological variables that are consistent with feedbacks from biomass burning in NSSA, and encourage more synergistic modeling and observational studies that can elaborate this feedback mechanism.
C1 [Ichoku, Charles; Ellison, Luke T.; Matsui, Toshihisa; Dezfuli, Amin K.; Gatebe, Charles K.; Bolten, John; Policelli, Frederick S.; Habib, Shahid] NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD 20771 USA.
[Ellison, Luke T.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Willmot, K. Elena] Vanderbilt Univ, Nashville, TN 37235 USA.
[Matsui, Toshihisa] Univ Maryland, ESSIC, College Pk, MD 20742 USA.
[Dezfuli, Amin K.; Gatebe, Charles K.] USRA, Columbia, MD USA.
[Wang, Jun] Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE USA.
[Wang, Jun] Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA 52242 USA.
[Wang, Jun] Univ Iowa, Dept Chem & Biochem Engn, Iowa City, IA 52242 USA.
[Wilcox, Eric M.] Desert Res Inst, Reno, NV USA.
[Lee, Jejung; Adegoke, Jimmy] Univ Missouri, Kansas City, MO 64110 USA.
[Okonkwo, Churchill] Howard Univ, Beltsville Ctr Climate Syst Observat, Washington, DC 20059 USA.
RP Ichoku, C (reprint author), NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD 20771 USA.
EM Charles.Ichoku@nasa.gov
RI Wang, Jun/A-2977-2008
OI Wang, Jun/0000-0002-7334-0490
FU NASA under its Research Opportunities in Space and Earth Sciences
(ROSES) through the Radiation Sciences Program; NASA under its
Interdisciplinary Studies (IDS) Program through the Radiation Sciences
Program
FX This research was fully funded by NASA under its Research Opportunities
in Space and Earth Sciences (ROSES)-2009 and 2013 Interdisciplinary
Studies (IDS) Program (Dr Jack Kaye, Earth Science Research Director)
through the Radiation Sciences Program managed by Dr Hal Maring. We also
appreciate the efforts of providers of the large diversity of data
products used for this study from various satellite sensors and global
models.
NR 72
TC 1
Z9 1
U1 15
U2 15
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 SEP
PY 2016
VL 11
IS 9
AR 095005
DI 10.1088/1748-9326/11/9/095005
PG 13
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DY8PW
UT WOS:000385393300001
ER
PT J
AU Marchand, P
Carr, JA
Dell'Angelo, J
Fader, M
Gephart, JA
Kummu, M
Magliocca, NR
Porkka, M
Puma, MJ
Ratajczak, Z
Rulli, MC
Seekell, DA
Suweis, S
Tavoni, A
D'Odorico, P
AF Marchand, Philippe
Carr, Joel A.
Dell'Angelo, Jampel
Fader, Marianela
Gephart, Jessica A.
Kummu, Matti
Magliocca, Nicholas R.
Porkka, Miina
Puma, Michael J.
Ratajczak, Zak
Rulli, Maria Cristina
Seekell, David A.
Suweis, Samir
Tavoni, Alessandro
D'Odorico, Paolo
TI Reserves and trade jointly determine exposure to food supply shocks
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Letter
DE food systems; resilience; food crises
ID LAND-USE; INTERNATIONAL-TRADE; AGRICULTURAL TRADE; GLOBALIZATION;
DISPLACEMENT; SECURITY; NATIONS; WATER
AB While a growing proportion of global food consumption is obtained through international trade, there is an ongoing debate on whether this increased reliance on trade benefits or hinders food security, and specifically, the ability of global food systems to absorb shocks due to local or regional losses of production. This paper introduces a model that simulates the short-term response to a food supply shock originating in a single country, which is partly absorbed through decreases in domestic reserves and consumption, and partly transmitted through the adjustment of trade flows. By applying the model to publicly-available data for the cereals commodity group over a 17 year period, we find that differential outcomes of supply shocks simulated through this time period are driven not only by the intensification of trade, but as importantly by changes in the distribution of reserves. Our analysis also identifies countries where trade dependency may accentuate the risk of food shortages from foreign production shocks; such risk could be reduced by increasing domestic reserves or importing food from a diversity of suppliers that possess their own reserves. This simulation-based model provides a framework to study the short-term, nonlinear and out-of-equilibrium response of trade networks to supply shocks, and could be applied to specific scenarios of environmental or economic perturbations.
C1 [Marchand, Philippe; Dell'Angelo, Jampel; Magliocca, Nicholas R.; D'Odorico, Paolo] Natl Socioenvironm Synth Ctr SESYNC, Annapolis, MD 21401 USA.
[Carr, Joel A.; Gephart, Jessica A.; Ratajczak, Zak; D'Odorico, Paolo] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA.
[Fader, Marianela] German Fed Inst Hydrol, Int Ctr Water Resources & Global Change UNESCO, POB 200253, D-56002 Koblenz, Germany.
[Kummu, Matti; Porkka, Miina] Aalto Univ, WDRG, FI-00076 Aalto, Finland.
[Puma, Michael J.] Columbia Univ, Ctr Climate Syst Res, NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Rulli, Maria Cristina] Politecn Milan, Dept Hydraul Roadways Environm & Surveying Engn, I-20133 Milan, Italy.
[Seekell, David A.] Umea Univ, Dept Ecol & Environm Sci, SE-90187 Ume, Sweden.
[Suweis, Samir] Univ Padua, Dept Phys & Astron, I-35131 Padua, Italy.
[Tavoni, Alessandro] London Sch Econ, Grantham Res Inst Climate Change & Environm, London WC2A 2AE, England.
RP Marchand, P (reprint author), Natl Socioenvironm Synth Ctr SESYNC, Annapolis, MD 21401 USA.
NR 44
TC 0
Z9 0
U1 3
U2 3
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 SEP
PY 2016
VL 11
IS 9
AR 095009
DI 10.1088/1748-9326/11/9/095009
PG 11
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DZ2XT
UT WOS:000385707100001
ER
PT J
AU Marchand, P
Carr, JA
Dell'Angelo, J
Fader, M
Gephart, JA
Kummu, M
Magliocca, NR
Porkka, M
Puma, MJ
Ratajczak, Z
Rulli, MC
Seekell, DA
Suweis, S
Tavoni, A
D'Odorico, P
AF Marchand, Philippe
Carr, Joel A.
Dell'Angelo, Jampel
Fader, Marianela
Gephart, Jessica A.
Kummu, Matti
Magliocca, Nicholas R.
Porkka, Miina
Puma, Michael J.
Ratajczak, Zak
Rulli, Maria Cristina
Seekell, David A.
Suweis, Samir
Tavoni, Alessandro
D'Odorico, Paolo
TI Reserves and trade jointly determine exposure to food supply shocks
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE food systems; resilience; food crises
ID LAND-USE; INTERNATIONAL-TRADE; AGRICULTURAL TRADE; GLOBALIZATION;
DISPLACEMENT; SECURITY; NATIONS; WATER
AB While a growing proportion of global food consumption is obtained through international trade, there is an ongoing debate on whether this increased reliance on trade benefits or hinders food security, and specifically, the ability of global food systems to absorb shocks due to local or regional losses of production. This paper introduces a model that simulates the short-term response to a food supply shock originating in a single country, which is partly absorbed through decreases in domestic reserves and consumption, and partly transmitted through the adjustment of trade flows. By applying the model to publicly-available data for the cereals commodity group over a 17 year period, we find that differential outcomes of supply shocks simulated through this time period are driven not only by the intensification of trade, but as importantly by changes in the distribution of reserves. Our analysis also identifies countries where trade dependency may accentuate the risk of food shortages from foreign production shocks; such risk could be reduced by increasing domestic reserves or importing food from a diversity of suppliers that possess their own reserves. This simulation-based model provides a framework to study the short-term, nonlinear and out-of-equilibrium response of trade networks to supply shocks, and could be applied to specific scenarios of environmental or economic perturbations.
C1 [Marchand, Philippe; Dell'Angelo, Jampel; Magliocca, Nicholas R.; D'Odorico, Paolo] Natl Socioenvironm Synth Ctr SESYNC, Annapolis, MD 21401 USA.
[Carr, Joel A.; Gephart, Jessica A.; Ratajczak, Zak; D'Odorico, Paolo] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA.
[Fader, Marianela] German Fed Inst Hydrol, Int Ctr Water Resources & Global Change UNESCO, POB 200253, D-56002 Koblenz, Germany.
[Kummu, Matti; Porkka, Miina] Aalto Univ, WDRG, FI-00076 Aalto, Finland.
[Puma, Michael J.] Columbia Univ, Ctr Climate Syst Res, NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Rulli, Maria Cristina] Politecn Milan, Dept Hydraul Roadways Environm & Surveying Engn, I-20133 Milan, Italy.
[Seekell, David A.] Umea Univ, Dept Ecol & Environm Sci, SE-90187 Umea, Sweden.
[Suweis, Samir] Univ Padua, Dept Phys & Astron, I-35131 Padua, Italy.
[Tavoni, Alessandro] London Sch Econ, Grantham Res Inst Climate Change & Environm, London WC2A 2AE, England.
RP Marchand, P (reprint author), Natl Socioenvironm Synth Ctr SESYNC, Annapolis, MD 21401 USA.
RI Kummu, Matti/C-4797-2011
OI Kummu, Matti/0000-0001-5096-0163
FU National Socio-Environmental Synthesis Center (SESYNC) under National
Science Foundation (NSF) [DBI-1052875]; Academy of Finland SRC project
Winland; Academy of Finland project SCART; Columbia University Center
for Climate and Life; Interdisciplinary Global Change Research under
NASA [NNX08AJ75A]; Carl Trygger Foundation for Scientific Research; NSF
[DBI-1402033]; Centre for Climate Change Economics and Policy - ESRC;
Grantham Foundation for the Protection of the Environment
FX We thank Roberto Patricio Korzeniewicz and Christina Prell for their
participation in early discussions on this project. This work was
supported by the National Socio-Environmental Synthesis Center (SESYNC)
under funding received from the National Science Foundation (NSF) grant
DBI-1052875. M Kummu received support from Academy of Finland SRC
project Winland and Academy of Finland project SCART. M J Puma is
supported by a fellowship from the Columbia University Center for
Climate and Life and the Interdisciplinary Global Change Research under
NASA cooperative agreement NNX08AJ75A. D A Seekell was supported by the
Carl Trygger Foundation for Scientific Research. Z Ratajczak received
support from NSF grant DBI-1402033. A Tavoni is supported by the Centre
for Climate Change Economics and Policy, funded by the ESRC, and the
Grantham Foundation for the Protection of the Environment.
NR 44
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 SEP
PY 2016
VL 11
IS 9
AR 095009
DI 10.1088/1748-9326/11/9/095009
PG 11
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DY8PW
UT WOS:000385393300005
ER
PT J
AU Sedano, F
Silva, JA
Machoco, R
Meque, CH
Sitoe, A
Ribeiro, N
Anderson, K
Ombe, ZA
Baule, SH
Tucker, CJ
AF Sedano, F.
Silva, J. A.
Machoco, R.
Meque, C. H.
Sitoe, A.
Ribeiro, N.
Anderson, K.
Ombe, Z. A.
Baule, S. H.
Tucker, C. J.
TI The impact of charcoal production on forest degradation: a case study in
Tete, Mozambique
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE forest degradation; charcoal; carbon emissions; remote sensing; very
high-resolution; Africa
ID DEVELOPING-COUNTRIES; DEVELOPING-WORLD; DEFORESTATION; IMAGERY; POLICY;
LIVELIHOODS; EMISSIONS; AFRICA; MAPS
AB Charcoal production for urban energy consumption is a main driver of forest degradation in sub Saharan Africa. Urban growth projections for the continent suggest that the relevance of this process will increase in the coming decades. Forest degradation associated to charcoal production is difficult to monitor and commonly overlooked and underrepresented in forest cover change and carbon emission estimates. We use a multitemporal dataset of very high-resolution remote sensing images to map kiln locations in a representative study area of tropical woodlands in central Mozambique. The resulting maps provided a characterization of the spatial extent and temporal dynamics of charcoal production. Using an indirect approach we combine kiln maps and field information on charcoal making to describe the magnitude and intensity of forest degradation linked to charcoal production, including aboveground biomass and carbon emissions. Our findings reveal that forest degradation associated to charcoal production in the study area is largely independent from deforestation driven by agricultural expansion and that its impact on forest cover change is in the same order of magnitude as deforestation. Our work illustrates the feasibility of using estimates of urban charcoal consumption to establish a link between urban energy demands and forest degradation. This kind of approach has potential to reduce uncertainties in forest cover change and carbon emission assessments in sub-Saharan Africa.
C1 [Sedano, F.; Silva, J. A.; Anderson, K.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Machoco, R.; Sitoe, A.; Ribeiro, N.] UEM, Fac Agron & Forest Engn, Dept Forest Engn, Maputo, Mozambique.
[Meque, C. H.] Mozambican Minist Sci & Technol, Zambezia, Mozambique.
[Ombe, Z. A.] Univ Pedagog, Fac Earth Sci & Environm, Maputo, Mozambique.
[Baule, S. H.] Univ Pedagog, Dept Language Commun & Arts, Beira, Mozambique.
[Tucker, C. J.] NASA, Goddard Space Flight Ctr, Washington, DC 20546 USA.
RP Sedano, F (reprint author), Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
EM fsedano@umd.edu
FU National Science Foundation-Dynamics of Coupled Natural and Human
Systems program [1413999]
FX This research is part of the 'CNH-Ex: Investigating the Dynamic
Intersections Among Economic Development, Urbanization, and Forest
Degradation' project, funded under the National Science
Foundation-Dynamics of Coupled Natural and Human Systems program (Award
number 1413999). The authors express their gratitude to students and
representatives of the Universidade Eduardo Mondlane, Universidade
Pegagogica-Tete branch and the personnel of the provincial Forest
Services of Tete whose contribution and support made possible field data
collection.
NR 39
TC 0
Z9 0
U1 10
U2 10
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 SEP
PY 2016
VL 11
IS 9
AR 094020
DI 10.1088/1748-9326/11/9/094020
PG 12
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DY8PU
UT WOS:000385393100008
ER
PT J
AU Rani, B
Krichbaum, T
Hodgson, JA
Koyama, S
Zensus, AJ
Fuhramnn, L
Marscher, A
Jorstad, S
AF Rani, Bindu
Krichbaum, Thomas
Hodgson, Jeff A.
Koyama, Shoko
Zensus, Anton J.
Fuhramnn, Lars
Marscher, Alan
Jorstad, Svetlana
TI Exploring the Magnetic Field Configuration in BL Lac Using GMVA
SO GALAXIES
LA English
DT Article
DE active galaxies; BL Lacertae object: BL Lac; jets; GMVA; high-resolution
VLBI; magnetic field; polarization
ID JET
AB The high radio frequency polarization imaging of non-thermal emission from active galactic nuclei (AGN) is a direct way to probe the magnetic field strength and structure in the immediate vicinity of supermassive black holes (SMBHs) and is crucial in testing the jet-launching scenario. To explore the the magnetic field configuration at the base of jets in blazars, we took advantage of the full polarization capabilities of the Global Millimeter VLBI Array (GMVA). With an angular resolution of similar to 50 micro-arcseconds (m as) at 86 GHz, one could resolve scales up to similar to 450 gravitational radii (for a 10(9) solar mass black hole at a redshift of 0.1). We present here the preliminary results of our study on the blazar BL Lac. Our results suggest that on sub-mas scales the core and the central jet of BL Lac are significantly polarized with two distinct regions of polarized intensity. We also noted a great morphological similarity between the 7 mm/3 mm VLBI images at very similar angular resolution.
C1 [Rani, Bindu] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Rani, Bindu; Krichbaum, Thomas; Koyama, Shoko; Zensus, Anton J.; Fuhramnn, Lars] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
[Hodgson, Jeff A.] Korea Astron & Space Inst, 776 Daedeokdae Ro, Daejeon 34055, South Korea.
[Marscher, Alan; Jorstad, Svetlana] Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02215 USA.
RP Rani, B (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Rani, B (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
EM bindu.rani@nasa.gov; tkrichbaum@mpifr-bonn.mpg.de; jhodgo@gmail.com;
skoyama@mpifr-bonn.mpg.de; azensus@mpifr-bonn.mpg.de;
fuhrmann.lars@googlemail.com; marscher@bu.edu; jorstad@bu.edu
OI Jorstad, Svetlana/0000-0001-6158-1708
NR 18
TC 0
Z9 0
U1 0
U2 0
PU MDPI AG
PI BASEL
PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND
SN 2075-4434
J9 GALAXIES
JI Galaxies
PD SEP
PY 2016
VL 4
IS 3
AR 32
DI 10.3390/galaxies4030032
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DY9UM
UT WOS:000385480600024
ER
PT J
AU Wilder, FD
Ergun, RE
Schwartz, SJ
Newman, DL
Eriksson, S
Stawarz, JE
Goldman, MV
Goodrich, KA
Gershman, DJ
Malaspina, DM
Holmes, JC
Sturner, AP
Burch, JL
Torbert, RB
Lindqvist, PA
Marklund, GT
Khotyaintsev, Y
Strangeway, RJ
Russell, CT
Pollock, CJ
Giles, BL
Dorrelli, JC
Avanov, LA
Patterson, WR
Plaschke, F
Magnes, W
AF Wilder, F. D.
Ergun, R. E.
Schwartz, S. J.
Newman, D. L.
Eriksson, S.
Stawarz, J. E.
Goldman, M. V.
Goodrich, K. A.
Gershman, D. J.
Malaspina, D. M.
Holmes, J. C.
Sturner, A. P.
Burch, J. L.
Torbert, R. B.
Lindqvist, P. -A.
Marklund, G. T.
Khotyaintsev, Y.
Strangeway, R. J.
Russell, C. T.
Pollock, C. J.
Giles, B. L.
Dorrelli, J. C.
Avanov, L. A.
Patterson, W. R.
Plaschke, F.
Magnes, W.
TI Observations of large-amplitude, parallel, electrostatic waves
associated with the Kelvin-Helmholtz instability by the magnetospheric
multiscale mission
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Kelvin-Helmholtz; electrostatic waves; boundary layer; turbulence
ID LATITUDE BOUNDARY-LAYER; MAGNETIC RECONNECTION; PLASMA TRANSPORT
AB On 8 September 2015, the four Magnetospheric Multiscale spacecraft encountered a Kelvin-Helmholtz unstable magnetopause near the dusk flank. The spacecraft observed periodic compressed current sheets, between which the plasma was turbulent. We present observations of large-amplitude (up to 100mV/m) oscillations in the electric field. Because these oscillations are purely parallel to the background magnetic field, electrostatic, and below the ion plasma frequency, they are likely to be ion acoustic-like waves. These waves are observed in a turbulent plasma where multiple particle populations are intermittently mixed, including cold electrons with energies less than 10eV. Stability analysis suggests a cold electron component is necessary for wave growth.
C1 [Wilder, F. D.; Ergun, R. E.; Schwartz, S. J.; Eriksson, S.; Stawarz, J. E.; Goodrich, K. A.; Malaspina, D. M.; Holmes, J. C.; Sturner, A. P.] Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
[Ergun, R. E.; Stawarz, J. E.; Goodrich, K. A.; Holmes, J. C.; Sturner, A. P.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Schwartz, S. J.] Imperial Coll London, Dept Phys, London, England.
[Newman, D. L.; Goldman, M. V.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Gershman, D. J.; Pollock, C. J.; Giles, B. L.; Dorrelli, J. C.; Avanov, L. A.; Patterson, W. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Burch, J. L.] Southwest Res Inst, San Antonio, TX USA.
[Torbert, R. B.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA.
[Lindqvist, P. -A.; Marklund, G. T.] Royal Inst Technol, Stockholm, Sweden.
[Khotyaintsev, Y.] Swedish Inst Space Phys, Uppsala, Sweden.
[Strangeway, R. J.; Russell, C. T.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA.
[Plaschke, F.; Magnes, W.] Austrian Acad Sci, Space Res Inst, Graz, Austria.
RP Wilder, FD (reprint author), Univ Colorado, Atmospher & Space Phys Lab, Campus Box 392, Boulder, CO 80309 USA.
EM frederick.wilder@lasp.colorado.edu
RI Stawarz, Julia/L-7387-2016; NASA MMS, Science Team/J-5393-2013;
OI Stawarz, Julia/0000-0002-5702-5802; NASA MMS, Science
Team/0000-0002-9504-5214; Eriksson, Stefan/0000-0002-5619-1577
FU NASA MMS project; Leverhulme Trust
FX This work was funded by the NASA MMS project. S.J.S. thanks the
Leverhulme Trust for the award of a research fellowship. We thank the
MMS search coil magnetometer team for providing burst data and comments
on our analyses. Level 2 spacecraft data are available via the MMS
Science Data Center (https://lasp.colorado.edu/mms/sdc/public/).
NR 22
TC 0
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 SEP
PY 2016
VL 43
IS 17
BP 8859
EP 8866
DI 10.1002/2016GL070404
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA DY8CX
UT WOS:000385357200005
ER
PT J
AU Xu, SS
Mitchell, D
Liemohn, M
Dong, CF
Bougher, S
Fillingim, M
Lillis, R
McFadden, J
Mazelle, C
Connerney, J
Jakosky, B
AF Xu, Shaosui
Mitchell, David
Liemohn, Michael
Dong, Chuanfei
Bougher, Stephen
Fillingim, Matthew
Lillis, Robert
McFadden, James
Mazelle, Christian
Connerney, Jack
Jakosky, Bruce
TI Deep nightside photoelectron observations by MAVEN SWEA: Implications
for Martian northern hemispheric magnetic topology and nightside
ionosphere source
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Mars; photoelectrons; nightside ionosphere; magnetic topology; weak
crustal fields; MAVEN
ID SOLAR-WIND INTERACTION; ELECTRON REFLECTOMETRY; MARS; FIELD; ATMOSPHERE;
MODEL; INSTRUMENT; MISSION; FLUXES; ATOMS
AB The Mars Atmosphere and Volatile EvolutioN (MAVEN) mission samples the Mars ionosphere down to altitudes of approximate to 150km over a wide range of local times and solar zenith angles. On 5 January 2015 (Orbit 520) when the spacecraft was in darkness at high northern latitudes (solar zenith angle, SZA>120 degrees; latitude>60 degrees), the Solar Wind Electron Analyzer (SWEA) instrument observed photoelectrons at altitudes below 200km. Such observations imply the presence of closed crustal magnetic field loops that cross the terminator and extend thousands of kilometers to the deep nightside. This occurs over the weak northern crustal magnetic source regions, where the magnetic field has been thought to be dominated by draped interplanetary magnetic fields (IMF). Such a day-night magnetic connectivity also provides a source of plasma and energy to the deep nightside. Simulations with the SuperThermal Electron Transport (STET) model show that photoelectron fluxes measured by SWEA precipitating onto the nightside atmosphere provide a source of ionization that can account for the O(2)(+)density measured by the Suprathermal and Thermal Ion Composition (STATIC) instrument below 200km. This finding indicates another channel for Martian energy redistribution to the deep nightside and consequently localized ionosphere patches and potentially aurora.
C1 [Xu, Shaosui; Mitchell, David; Fillingim, Matthew; Lillis, Robert; McFadden, James] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Xu, Shaosui; Liemohn, Michael; Dong, Chuanfei; Bougher, Stephen] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
[Dong, Chuanfei] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Dong, Chuanfei] Princeton Univ, Princeton Plasma Phys Lab, POB 451, Princeton, NJ 08543 USA.
[Mazelle, Christian] CNRS, IRAP, Toulouse, France.
[Mazelle, Christian] Univ Toulouse 3, Toulouse, France.
[Connerney, Jack] GSFC, Greenbelt, MD USA.
[Jakosky, Bruce] Univ Colorado, LASP, Boulder, CO 80309 USA.
RP Xu, SS (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.; Xu, SS (reprint author), Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
EM shaosui.xu@ssl.berkeley.edu
RI Dong, Chuanfei/E-6485-2010;
OI Dong, Chuanfei/0000-0002-8990-094X; Xu, Shaosui/0000-0002-5121-600X;
connerney, jack/0000-0001-7478-6462
FU NASA; NSF [NNX13AG26G, AST-0908311]; NASA Mars Scout Program; Rackham
graduate school of University of Michigan; NASA Living With a Star Jack
Eddy Postdoctoral Fellowship Program
FX The authors would like to thank NASA and NSF for their support of this
project under grants NNX13AG26G and AST-0908311. This work was also
supported by the NASA Mars Scout Program. The authors thank the Rackham
graduate school of University of Michigan for the research grant that
supports S. Xu's visit at SSL, University of California, Berkeley, which
makes this study possible. C.F. Dong is supported by the NASA Living
With a Star Jack Eddy Postdoctoral Fellowship Program, administered by
the University Corporation for Atmospheric Research. The MAVEN data used
in this study are available through Planetary Data System. The BATS-R-US
code is publicly available from http://csem.engin.umich.edu/tools/swmf.
For distribution of the model results used in this study, please contact
C. Dong (dcfy@pppl.gov).
NR 53
TC 1
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U1 8
U2 8
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 SEP
PY 2016
VL 43
IS 17
BP 8876
EP 8884
DI 10.1002/2016GL070527
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DY8CX
UT WOS:000385357200007
ER
PT J
AU Edwards, CS
Piqueux, S
AF Edwards, Christopher S.
Piqueux, Sylvain
TI The water content of recurring slope lineae on Mars
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Mars; recurring slope lineae; water budget; THEMIS; thermophysics
ID THERMAL-CONDUCTIVITY MEASUREMENTS; EMISSION SPECTROMETER; PARTICULATE
MATERIALS; REFLECTANCE; STABILITY; SURFACE; THEMIS; ICE
AB Observations of recurring slope lineae (RSL) from the High-Resolution Imaging Science Experiment have been interpreted as present-day, seasonally variable liquid water flows; however, orbital spectroscopy has not confirmed the presence of liquid H2O, only hydrated salts. Thermal Emission Imaging System (THEMIS) temperature data and a numerical heat transfer model definitively constrain the amount of water associated with RSL. Surface temperature differences between RSL-bearing and dry RSL-free terrains are consistent with no water associated with RSL and, based on measurement uncertainties, limit the water content of RSL to at most 0.5-3wt %. In addition, distinct high thermal inertia regolith signatures expected with crust-forming evaporitic salt deposits from cyclical briny water flows are not observed, indicating low water salinity (if any) and/or low enough volumes to prevent their formation. Alternatively, observed salts may be preexisting in soils at low abundances (i.e., near or below detection limits) and largely immobile. These RSL-rich surfaces experience similar to 100K diurnal temperature oscillations, possible freeze/thaw cycles and/or complete evaporation on time scales that challenge their habitability potential. The unique surface temperature measurements provided by THEMIS are consistent with a dry RSL hypothesis or at least significantly limit the water content of Martian RSL.
C1 [Edwards, Christopher S.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Edwards, Christopher S.] Northern Univ Arizona, Dept Phys & Astron, Flagstaff, AZ 86011 USA.
[Piqueux, Sylvain] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Edwards, CS (reprint author), US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.; Edwards, CS (reprint author), Northern Univ Arizona, Dept Phys & Astron, Flagstaff, AZ 86011 USA.
EM Christopher.Edwards@nau.edu
FU National Aeronautics and Space Administration
FX The authors thank the 2001 Mars Odyssey THEMIS team, who aided in the
collection of needed seasonal data. We thank Joshua Bandfield, Shane
Byrne, and two anonymous reviewers that greatly improved the manuscript.
All THEMIS, CTX, and HiRISE data presented in this work are available on
the Planetary Data System (http://pds-geosciences.wustl.edu), data
processing software was completed using davinci (http://davinci.asu.edu)
and the Integrated Software for Imaging Spectrometers
(http://isis.astrogeology.usgs.gov), and modeling was conducted using
the KRC thermal model (http://krc.mars.asu.edu). Work at the Jet
Propulsion Laboratory, California Institute of Technology was performed
under a contract with the National Aeronautics and Space Administration.
NR 59
TC 2
Z9 2
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 SEP
PY 2016
VL 43
IS 17
BP 8912
EP 8919
DI 10.1002/2016GL070179
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA DY8CX
UT WOS:000385357200011
ER
PT J
AU Coats, S
Mankin, JS
AF Coats, Sloan
Mankin, Justin S.
TI The challenge of accurately quantifying future megadrought risk in the
American Southwest
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE hydroclimate; drought; North America; climate; megadrought; projections
ID LAST MILLENNIUM; NORTH-AMERICA; DROUGHT; RECONSTRUCTIONS; VARIABILITY;
FREQUENCY; EVENTS; WATER
AB American Southwest (ASW) megadroughts represent decadal-scale periods of dry conditions the near-term risks of which arise from natural low-frequency hydroclimate variability and anthropogenic forcing. A large single-climate-model ensemble indicates that anthropogenic forcing increases near-term ASW megadrought risk by a factor of 100; however, accurate risk assessment remains a challenge. At the global-scale we find that anthropogenic forcing may alter the variability driving megadroughts over 55% of land areas, undermining accurate assessments of their risk. For the remaining areas, current ensembles are too small to characterize megadroughts' driving variability. For example, constraining uncertainty in near-term ASW megadrought risk to 5 percentage points with high confidence requires 287 simulations. Such ensemble sizes are beyond current computational and storage resources, and these limitations suggest that constraining errors in near-term megadrought risk projections with high confidenceeven in places where underlying variability is stationaryis not currently possible.
C1 [Coats, Sloan] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Mankin, Justin S.] Columbia Univ, Ocean & Climate Phys, Lamont Doherty Earth Observ, Palisades, NY USA.
[Mankin, Justin S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Coats, S (reprint author), Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
EM sloan.coats@colorado.edu
FU Center for International Security and Cooperation at Stanford
University; Earth Institute Fellowship at Columbia University;
Cooperative Institute for Research in Environmental Sciences at the
University of Colorado, Boulder
FX The authors would like to thank the National Center for Atmospheric
Research's CESM1 (CAM5) Large Ensemble Community Project (LENS) and
supercomputing resources provided by Stanford Center for Computational
Earth and Environmental Science in the School of Earth, Energy, and
Environmental Sciences at Stanford University. The model output employed
from the LENS can be accessed at
https://www2.cesm.ucar.edu/models/experiments/LENS. Our work was
supported by the Center for International Security and Cooperation at
Stanford University and the Earth Institute Fellowship at Columbia
University to J.S.M. and the Cooperative Institute for Research in
Environmental Sciences at the University of Colorado, Boulder, and
Kristopher B. Karnauskas to S.C. LDEO publication 8051.
NR 31
TC 0
Z9 0
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 SEP
PY 2016
VL 43
IS 17
BP 9225
EP 9233
DI 10.1002/2016GL070445
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DY8CX
UT WOS:000385357200049
ER
PT J
AU Tong, D
Pan, L
Chen, WW
Lamsal, L
Lee, P
Tang, YH
Kim, H
Kondragunta, S
Stajner, I
AF Tong, Daniel
Pan, Li
Chen, Weiwei
Lamsal, Lok
Lee, Pius
Tang, Youhua
Kim, Hyuncheol
Kondragunta, Shobha
Stajner, Ivanka
TI Impact of the 2008 Global Recession on air quality over the United
States: Implications for surface ozone levels from changes in NOx
emissions
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE ozone; recession; NO2; air quality
ID NITROGEN-OXIDES; NORTH-AMERICA; SATELLITE; POLLUTION; MODEL; CAPABILITY;
SYSTEM; TRENDS; CITIES; SPACE
AB Satellite and ground observations detected large variability in nitrogen oxides (NOx) during the 2008 economic recession, but the impact of the recession on air quality has not been quantified. This study combines observed NOx trends and a regional chemical transport model to quantify the impact of the recession on surface ozone (O-3) levels over the continental United States. The impact is quantified by simulating O-3 concentrations under two emission scenarios: business-as-usual (BAU) and recession. In the BAU case, the emission projection from the Cross-State Air Pollution Rule is used to estimate the would-be NOx emission level in 2011. In the recession case, the actual NO2 trends observed from Air Quality System ground monitors and the Ozone Monitoring Instrument on the Aura satellite are used to obtain realistic changes in NOx emissions. The model prediction with the recession effect agrees better with ground O-3 observations over time and space than the prediction with the BAU emission. The results show that the recession caused a 1-2ppbv decrease in surface O-3 concentration over the eastern United States, a slight increase (0.5-1ppbv) over the Rocky Mountain region, and mixed changes in the Pacific West. The gain in air quality benefits during the recession, however, could be quickly offset by the much slower emission reduction rate during the post-recession period.
C1 [Tong, Daniel] Univ Maryland, Cooperat Inst Climate & Satellites, College Pk, MD 20742 USA.
[Tong, Daniel; Pan, Li; Tang, Youhua; Kim, Hyuncheol] George Mason Univ, Ctr Spatial Informat Sci & Syst, Fairfax, VA 22030 USA.
[Tong, Daniel; Pan, Li; Chen, Weiwei; Lee, Pius; Tang, Youhua; Kim, Hyuncheol] NOAA, Air Resources Lab, College Pk, MD 20740 USA.
[Lamsal, Lok] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Lamsal, Lok] Univ Space Res Assoc, Greenbelt, MD USA.
[Kondragunta, Shobha] NOAA, Satellite & Informat Serv, Ctr Satellite Res & Applicat, College Pk, MD USA.
[Stajner, Ivanka] NOAA, Natl Weather Serv, Off Sci & Technol Integrat, Silver Spring, MD 20910 USA.
RP Tong, D (reprint author), Univ Maryland, Cooperat Inst Climate & Satellites, College Pk, MD 20742 USA.; Tong, D (reprint author), George Mason Univ, Ctr Spatial Informat Sci & Syst, Fairfax, VA 22030 USA.; Tong, D (reprint author), NOAA, Air Resources Lab, College Pk, MD 20740 USA.
EM daniel.tong@noaa.gov
RI Kondragunta, Shobha/F-5601-2010; Tong, Daniel/A-8255-2008; Kim,
Hyun/G-1315-2012
OI Kondragunta, Shobha/0000-0001-8593-8046; Tong,
Daniel/0000-0002-4255-4568; Kim, Hyun/0000-0003-3968-6145
FU NOAA's US Weather Research Program (USWRP); Joint Polar Satellite System
(JPSS) Proving Ground and Risk Reduction Programs
FX This work has been financially supported by grants from the NOAA's US
Weather Research Program (USWRP) and Joint Polar Satellite System (JPSS)
Proving Ground and Risk Reduction Programs. Modeling system development
was supported by the NOAA's National Air Quality Forecast Capability
program. The authors are grateful to Nina Randazzo for data analysis and
two anonymous reviewers for their constructive comments. The scientific
results and conclusions, as well as any views or opinions expressed
herein, are those of the authors and do not necessarily reflect the view
of NOAA or the Department of Commerce.
NR 34
TC 0
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U1 6
U2 6
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 SEP
PY 2016
VL 43
IS 17
BP 9280
EP 9288
DI 10.1002/2016GL069885
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DY8CX
UT WOS:000385357200055
ER
PT J
AU Schobesberger, S
Lopez-Hilfiker, FD
Taipale, D
Millet, DB
D'Ambro, EL
Rantala, P
Mammarella, I
Zhou, PT
Wolfe, GM
Lee, BH
Boy, M
Thornton, JA
AF Schobesberger, Siegfried
Lopez-Hilfiker, Felipe D.
Taipale, Ditte
Millet, Dylan B.
D'Ambro, Emma L.
Rantala, Pekka
Mammarella, Ivan
Zhou, Putian
Wolfe, Glenn M.
Lee, Ben H.
Boy, Michael
Thornton, Joel A.
TI High upward fluxes of formic acid from a boreal forest canopy
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE formic acid; eddy covariance fluxes; chemical ionization mass
spectrometry; boreal forest; biogenic emissions
ID ORGANIC-COMPOUND EMISSIONS; GASEOUS DRY DEPOSITION; ACETIC-ACIDS; SCOTS
PINE; MASS-SPECTROMETER; EDDY COVARIANCE; PEROXY NITRATES;
SULFURIC-ACID; NEW-MODEL; GAS
AB Eddy covariance fluxes of formic acid, HCOOH, were measured over a boreal forest canopy in spring/summer 2014. The HCOOH fluxes were bidirectional but mostly upward during daytime, in contrast to studies elsewhere that reported mostly downward fluxes. Downward flux episodes were explained well by modeled dry deposition rates. The sum of net observed flux and modeled dry deposition yields an upward gross flux of HCOOH, which could not be quantitatively explained by literature estimates of direct vegetative/soil emissions nor by efficient chemical production from other volatile organic compounds, suggesting missing or greatly underestimated HCOOH sources in the boreal ecosystem. We implemented a vegetative HCOOH source into the GEOS-Chem chemical transport model to match our derived gross flux and evaluated the updated model against airborne and spaceborne observations. Model biases in the boundary layer were substantially reduced based on this revised treatment, but biases in the free troposphere remain unexplained.
C1 [Schobesberger, Siegfried; Lopez-Hilfiker, Felipe D.; Lee, Ben H.; Thornton, Joel A.] Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.
[Schobesberger, Siegfried; Rantala, Pekka; Mammarella, Ivan; Zhou, Putian; Boy, Michael] Univ Helsinki, Dept Phys, Helsinki, Finland.
[Taipale, Ditte] Estonian Univ Life Sci, Dept Plant Physiol, Tartu, Estonia.
[Taipale, Ditte] Univ Helsinki, Dept Forest Sci, Helsinki, Finland.
[Millet, Dylan B.] Univ Minnesota, Dept Soil Water & Climate, Minneapolis, MN USA.
[D'Ambro, Emma L.] Univ Washington, Dept Chem, Seattle, WA 98195 USA.
[Wolfe, Glenn M.] NASA, Atmospher Chem & Dynam Lab, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Wolfe, Glenn M.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
RP Schobesberger, S (reprint author), Univ Washington, Dept Atmospher Sci, Seattle, WA 98195 USA.; Schobesberger, S (reprint author), Univ Helsinki, Dept Phys, Helsinki, Finland.
EM sschobes@uw.edu
RI Millet, Dylan/G-5832-2012; Chem, GEOS/C-5595-2014; Thornton,
Joel/C-1142-2009; Wolfe, Glenn/D-5289-2011;
OI Thornton, Joel/0000-0002-5098-4867; Taipale, Ditte/0000-0002-2023-2461;
Boy, Michael/0000-0002-8107-4524; Mammarella, Ivan/0000-0002-8516-3356;
Zhou, Putian/0000-0003-0803-7337
FU U.S. Department of Energy [DE-SC0006867]; European Commission (OXFLUX)
[701958]; European Regional Development Fund (Centre of Excellence
EcolChange); NSF CAREER [1148951]; Minnesota Supercomputing Institute
FX We thank T. Vesala, P. Kolari, P. Keronen, E. Siivola, M. Kajos, and A.
Manninen at U. Helsinki for helpful discussions and model and
measurement data related to SMEAR II. We also thank J. de Gouw (NOAA
ESRL), and the SENEX and TES science teams for providing observations,
and P. Punttila (Ymparisto) and D.M. Sorger (NC State) for entomological
insights. The University of Washington participated in the BAECC
campaign with funds from the U.S. Department of Energy (DE-SC0006867).
S. Schobesberger acknowledges support from the European Commission
(OXFLUX, project 701958), D. Taipale from the European Regional
Development Fund (Centre of Excellence EcolChange), and D. B. M. from
NSF CAREER (1148951) and the Minnesota Supercomputing Institute. We
thank K. Cady-Pereira (AER), M. Shephard (Environment Canada), and M.
Luo (JPL) for developing TES HCOOH measurements, publicly available at
http://tes.jpl.nasa.gov/data/. GEOS-Chem model code is available at
www.geos-chem.org. SOSAA model output, the high-frequency HCOOH mixing
ratio measurements by CIMS, and anemometer wind measurements are
available at http://hdl.handle.net/1773/36867.
NR 68
TC 0
Z9 0
U1 11
U2 11
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 SEP
PY 2016
VL 43
IS 17
BP 9342
EP 9351
DI 10.1002/2016GL069599
PG 10
WC Geosciences, Multidisciplinary
SC Geology
GA DY8CX
UT WOS:000385357200062
ER
PT J
AU Zhou, DK
Liu, X
Larar, AM
Tian, JL
Smith, WL
Kizer, SH
Wu, W
Liu, QH
Goldberg, MD
AF Zhou, Daniel K.
Liu, Xu
Larar, Allen M.
Tian, Jialin
Smith, William L.
Kizer, Susan H.
Wu, Wan
Liu, Quanhua
Goldberg, Mitch D.
TI First Suomi NPP Cal/Val Campaign: Intercomparison of Satellite and
Aircraft Sounding Retrievals
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Atmospheric measurements; geophysical inverse problems; infrared
measurements; remote sensing
ID VALIDATION; EAQUATE; CLOUD
AB Satellite ultraspectral infrared sensors provide key data records essential for weather forecasting and climate change science. The Suomi National Polar-orbiting Partnership (NPP) satellite environmental data records (EDRs) are retrieved from calibrated ultraspectral radiance or sensor data records (SDRs). Understanding the accuracy of retrieved EDRs is critical. The first Suomi NPP Calibration/Validation Campaign was conducted during May 2013. The NASA high-altitude ER-2 aircraft carrying ultraspectral interferometer sounders such as the National Airborne Sounder Testbed-Interferometer (NAST-I) flew under the Suomi NPP satellite that carries the cross-track infrared sounder (CrIS) and the advanced technology microwave sounder (ATMS). Here, we intercompare the EDRs produced with different retrieval algorithms from SDRs measured from satellite and aircraft. The available dropsonde and radiosonde measurements together with the European Centre for Medium-Range Weather Forecasts (ECMWF) analysis are used to assess the results of this experiment. This study indicates that the CrIS/ATMS retrieval accuracy meets the Suomi NPP EDR requirement, except in the planetary boundary layer (PBL) where we have less confidence in meeting the requirement due to retrieval null-space error.
C1 [Zhou, Daniel K.; Liu, Xu; Larar, Allen M.; Tian, Jialin] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Smith, William L.; Kizer, Susan H.; Wu, Wan] Sci Syst & Applicat Inc, Hampton, VA 23681 USA.
[Liu, Quanhua; Goldberg, Mitch D.] NOAA, NESDIS, College Pk, MD 20740 USA.
RP Zhou, DK (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM daniel.k.zhou@nasa.gov
FU NASA Headquarters; NASA Langley Research Center; NOAA NESDIS/JPSS
Program Office; NAST-I program
FX The authors greatly appreciate the contributions of NASA's Langley
Research Center and the U.K. Met Office. The authors would like to thank
NASA ER-2 aircraft pilots and crewmembers based at NASA's Armstrong
Flight Research Center for their dedication. The NAST-I program is
supported by NASA Headquarters, NASA Langley Research Center, and NOAA
NESDIS/JPSS Program Office. The authors would also like to thank Dr. A.
Gambacorta of NOAA NESDIS for useful discussion; and Dr. J. Kaye of
NASA's Science Mission Directorate for his continued, enabling support
of the NAST-I program.
NR 21
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U1 2
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
EI 2151-1535
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD SEP
PY 2016
VL 9
IS 9
BP 4037
EP 4046
DI 10.1109/JSTARS.2016.2516765
PG 10
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA DY6NW
UT WOS:000385245000005
ER
PT J
AU Selvakumaran, R
Veenadhari, B
Akiyama, S
Pandya, M
Gopalswamy, N
Yashiro, S
Kumar, S
Makela, P
Xie, H
AF Selvakumaran, R.
Veenadhari, B.
Akiyama, S.
Pandya, Megha
Gopalswamy, N.
Yashiro, S.
Kumar, Sandeep
Maekelae, P.
Xie, H.
TI On the reduced geoeffectiveness of solar cycle 24: A moderate storm
perspective
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE moderate storms; solar source identification; reduced geoeffectiveness
ID CORONAL MASS EJECTIONS; INTENSE GEOMAGNETIC STORMS; DST
LESS-THAN-OR-EQUAL-TO-50 NT; MAGNETIC STORMS; RING CURRENT;
INTERPLANETARY ORIGIN; INTERACTION REGIONS; SPACE WEATHER; TAIL CURRENT;
MAIN PHASE
AB The moderate and intense geomagnetic storms are identified for the first 77months of solar cycles 23 and 24. The solar sources responsible for the moderate geomagnetic storms are indentified during the same epoch for both the cycles. Solar cycle 24 has shown nearly 80% reduction in the occurrence of intense storms whereas it is only 40% in case of moderate storms when compared to previous cycle. The solar and interplanetary characteristics of the moderate storms driven by coronal mass ejection (CME) are compared for solar cycles 23 and 24 in order to see reduction in geoeffectiveness has anything to do with the occurrence of moderate storm. Though there is reduction in the occurrence of moderate storms, the Dst distribution does not show much difference. Similarly, the solar source parameters like CME speed, mass, and width did not show any significant variation in the average values as well as the distribution. The correlation between VBz and Dst is determined, and it is found to be moderate with value of 0.68 for cycle 23 and 0.61 for cycle 24. The magnetospheric energy flux parameter epsilon (epsilon) is estimated during the main phase of all moderate storms during solar cycles 23 and 24. The energy transfer decreased in solar cycle 24 when compared to cycle 23. These results are significantly different when all geomagnetic storms are taken into consideration for both the solar cycles.
C1 [Selvakumaran, R.; Veenadhari, B.; Pandya, Megha; Kumar, Sandeep] Indian Inst Geomagnetism, New Panvel, India.
[Akiyama, S.; Gopalswamy, N.; Yashiro, S.; Maekelae, P.; Xie, H.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD USA.
[Akiyama, S.; Yashiro, S.; Maekelae, P.; Xie, H.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Selvakumaran, R (reprint author), Indian Inst Geomagnetism, New Panvel, India.
EM selva2986@gmail.com
FU NASA's LWS TRT program
FX R. Selvakumaran benefited from the SCOSTEP Visiting Scholar Program,
under which he visited NASA Goddard Space Flight Center, where this
research was performed. Authors from Indian Institute of Geomagnetism
(IIG) are grateful to Director, IIG, for support and encouragement to
carry out the work. We thank the ACE, Wind, and OMNIWeb teams for
providing the solar wind data. We acknowledge the use of solar imagery
from SDO, SOHO, and STEREO missions. This work greatly benefited from
the open data policy of NASA. The work of N.G., S.A., S.Y., P.M., and
H.X. was supported by NASA's LWS TR&T program.
NR 76
TC 0
Z9 0
U1 3
U2 3
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.
PD SEP
PY 2016
VL 121
IS 9
BP 8188
EP 8202
DI 10.1002/2016JA022885
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4QM
UT WOS:000385844000003
ER
PT J
AU Neugebauer, M
Reisenfeld, D
Richardson, IG
AF Neugebauer, Marcia
Reisenfeld, Daniel
Richardson, Ian G.
TI Comparison of algorithms for determination of solar wind regimes
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE solar wind
ID CORONAL MASS EJECTIONS; COROTATING INTERACTION REGIONS; STREAM
INTERFACES; QUASI-STATIONARY; EARTH; SPACECRAFT; MISSION; CLOUDS; MATTER
AB This study compares the designation of different solar wind flow regimes (transient, coronal hole, and streamer belt) according to two algorithms derived from observations by the Solar Wind Ion Composition Spectrometer, the Solar Wind Electron Proton Alpha Monitor, and the Magnetometer on the ACE spacecraft, with a similar regime determination performed on board the Genesis spacecraft. The comparison is made for the interval from late 2001 to early 2004 when Genesis was collecting solar wind ions for return to Earth. The agreement between hourly regime assignments from any pair of algorithms was less than two thirds, while the simultaneous agreement between all three algorithms was only 49%. When the results of the algorithms were compared to a catalog of interplanetary coronal mass ejection events, it was found that almost all the events in the catalog were confirmed by the spacecraft algorithms. On the other hand, many short transient events, lasting 1 to 13h, that were unanimously selected as transient like by the algorithms, were not included in the catalog.
C1 [Neugebauer, Marcia] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Reisenfeld, Daniel] Univ Montana, Dept Phys & Astron, Missoula, MT 59812 USA.
[Richardson, Ian G.] Univ Maryland, CRESST, College Pk, MD 20742 USA.
[Richardson, Ian G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Richardson, Ian G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Neugebauer, M (reprint author), Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
EM mneugeb@lpl.arizona.edu
FU ACE mission; NSF; NASA Laboratory Analysis of Returned Samples (LARS)
program [NNX15AG19G]
FX The Genesis, SWICS, SWEPAM, and MAG parameters are all available at
http://cdaweb.gsfc.nasa.gov and other sites listed in the text. The
times of Genesis collector (regime) changes are available in the
supporting information of the paper by Reisenfeld et al. [2013]. I.G.R.
acknowledges support from the ACE mission. The Thule neutron monitor of
the Bartol Research Institute is supported by NSF. D.B.R. acknowledges
support from the NASA Laboratory Analysis of Returned Samples (LARS)
program, grant NNX15AG19G.
NR 35
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.
PD SEP
PY 2016
VL 121
IS 9
BP 8215
EP 8227
DI 10.1002/2016JA023142
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4QM
UT WOS:000385844000005
ER
PT J
AU Chamberlin, PC
Gong, Q
AF Chamberlin, Phillip C.
Gong, Qian
TI An integral field spectrograph utilizing mirrorlet arrays
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE Heliophysics; instrumentation; EUV; solar; photons; solar eruptive
events
ID IMAGING SPECTROMETER; SOLAR; REGION; 3D
AB An integral field spectrograph (IFS) has been developed that utilizes a new and novel optical design to observe two spatial dimensions simultaneously with one spectral dimension. This design employs an optical 2-D array of reflecting and focusing mirrorlets. This mirrorlet array is placed at the imaging plane of the front-end telescope to generate a 2-D array of tiny spots replacing what would be the slit in a traditional slit spectrometer design. After the mirrorlet in the optical path, a grating on a concave mirror surface will image the spot array and provide high-resolution spectrum for each spatial element at the same time; therefore, the IFS simultaneously obtains the 3-D data cube of two spatial and one spectral dimensions. The new mirrorlet technology is currently in-house and undergoing laboratory testing at NASA Goddard Space Flight Center. Section 1 describes traditional classes of instruments that are used in Heliophysics missions and a quick introduction to the new IFS design. Section 2 discusses the details of the most generic mirrorlet IFS, while section 3 presents test results of a lab-based instrument. An example application to a Heliophysics mission to study solar eruptive events in extreme ultraviolet wavelengths is presented in section 4 that has high spatial resolution (0.5arcsecpixels) in the two spatial dimensions and high spectral resolution (66m angstrom) across a 15 angstrom spectral window. Section 4 also concludes with some other optical variations that could be employed on the more basic IFS for further capabilities of this type of instrument.
C1 [Chamberlin, Phillip C.] NASA, Goddard Space Flight Ctr, Heliophys Div, Solar Phys Lab, Greenbelt, MD 20771 USA.
[Gong, Qian] NASA, Goddard Space Flight Ctr, Instrument Syst & Technol Div, Greenbelt, MD USA.
RP Chamberlin, PC (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Div, Solar Phys Lab, Greenbelt, MD 20771 USA.
EM Phillip.C.Chamberlin@NASA.gov
RI Chamberlin, Phillip/C-9531-2012
OI Chamberlin, Phillip/0000-0003-4372-7405
FU NASA Goddard Space Flight Center's Internal Research and Development
(IRAD) program
FX This work was support under NASA Goddard Space Flight Center's Internal
Research and Development (IRAD) program. The authors would like to thank
RPC Photonics for producing the mirrorlet array. No data were used in
producing this manuscript.
NR 25
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.
PD SEP
PY 2016
VL 121
IS 9
BP 8250
EP 8259
DI 10.1002/2016JA022487
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4QM
UT WOS:000385844000008
ER
PT J
AU Poh, G
Slavin, JA
Jia, XZ
DiBraccio, GA
Raines, JM
Imber, SM
Gershman, DJ
Sun, WJ
Anderson, BJ
Korth, H
Zurbuchen, TH
McNutt, RL
Solomon, SC
AF Poh, Gangkai
Slavin, James A.
Jia, Xianzhe
DiBraccio, Gina A.
Raines, Jim M.
Imber, Suzanne M.
Gershman, Daniel J.
Sun, Wei-Jie
Anderson, Brian J.
Korth, Haje
Zurbuchen, Thomas H.
McNutt, Ralph L., Jr.
Solomon, Sean C.
TI MESSENGER observations of cusp plasma filaments at Mercury
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE cusp filaments; Mercury; reconnection
ID FLUX-TRANSFER EVENTS; MAGNETIC-FIELD; SOLAR-WIND; MAGNETOPAUSE
RECONNECTION; DAYSIDE MAGNETOPAUSE; MAGNETOSPHERE; INSTRUMENT; MODEL;
HOLES; SHEAR
AB The MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft while in orbit about Mercury observed highly localized, similar to 3-s-long reductions in the dayside magnetospheric magnetic field, with amplitudes up to 90% of the ambient intensity. These magnetic field depressions are termed cusp filaments because they were observed from just poleward of the magnetospheric cusp to midlatitudes, i.e., similar to 55 degrees to 85 degrees N. We analyzed 345 high- and low-altitude cusp filaments identified from MESSENGER magnetic field data to determine their physical properties. Minimum variance analysis indicates that most filaments resemble cylindrical flux tubes within which the magnetic field intensity decreases toward its central axis. If the filaments move over the spacecraft at an estimated magnetospheric convection speed of similar to 35km/s, then they have a typical diameter of similar to 105km or similar to 7gyroradii for 1keVH(+) ions in a 300nT magnetic field. During these events, MESSENGER's Fast Imaging Plasma Spectrometer observed H+ ions with magnetosheath-like energies. MESSENGER observations during the spacecraft's final low-altitude campaign revealed that these cusp filaments likely extend down to Mercury's surface. We calculated an occurrence-rate-normalized integrated particle precipitation rate onto the surface from all filaments of (2.700.09)x10(25)s(-1). This precipitation rate is comparable to published estimates of the total precipitation rate in the larger-scale cusp. Overall, the MESSENGER observations analyzed here suggest that cusp filaments are the magnetospheric extensions of the flux transfer events that form at the magnetopause as a result of localized magnetic reconnection.
C1 [Poh, Gangkai; Slavin, James A.; Jia, Xianzhe; Raines, Jim M.; Imber, Suzanne M.; Gershman, Daniel J.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[DiBraccio, Gina A.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD USA.
[Imber, Suzanne M.] Univ Leicester, Dept Phys & Astron, Leicester, Leics, England.
[Gershman, Daniel J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Sun, Wei-Jie] Peking Univ, Sch Earth & Space Sci, Beijing, Peoples R China.
[Anderson, Brian J.; Korth, Haje; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
[Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA.
RP Poh, G (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
EM gangkai@umich.edu
RI Jia, Xianzhe/C-5171-2012; Slavin, James/H-3170-2012
OI Jia, Xianzhe/0000-0002-8685-1484; Slavin, James/0000-0002-9206-724X
FU NASA [NASW-00002, NAS5-97271, NNX15K88G, NNX15AL01G]; Living With a Star
Program [NNX16AJ67G]; Solar System Workings Program [NNX15AH28G]
FX Conversations with J. C. Kasper on the identification method used here
are appreciated. We also thank two anonymous reviewers for constructive
comments on an earlier draft. The MESSENGER project is supported by the
NASA Discovery Program under contracts NASW-00002 to the Carnegie
Institution of Washington and NAS5-97271 to The Johns Hopkins University
Applied Physics Laboratory. All data analyzed in this paper are archived
with the NASA Planetary Data System. Further support was provided by
NASA Discovery Data Analysis Program grants NNX15K88G and NNX15AL01G,
Living With a Star Program grant NNX16AJ67G, and Solar System Workings
Program grant NNX15AH28G to the University of Michigan.
NR 58
TC 0
Z9 0
U1 2
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD SEP
PY 2016
VL 121
IS 9
BP 8260
EP 8285
DI 10.1002/2016JA022552
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4QM
UT WOS:000385844000009
ER
PT J
AU Fennell, JF
Blake, JB
Claudepierre, S
Mazur, J
Kanekal, S
O'Brien, P
Baker, D
Crain, W
Mabry, D
Clemmons, J
AF Fennell, J. F.
Blake, J. B.
Claudepierre, S.
Mazur, J.
Kanekal, S.
O'Brien, P.
Baker, D.
Crain, W.
Mabry, D.
Clemmons, J.
TI Current energetic particle sensors
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE energetic particles; sensors
ID ALLEN PROBES OBSERVATIONS; RELATIVISTIC ELECTRONS; IMPENETRABLE BARRIER;
MAGNETOSONIC WAVES; RADIATION BELTS; STORM; PRECIPITATION; ACCELERATION;
PLASMASPHERE; ZONE
AB Several energetic particle sensors designed to make measurements in the current decade are described and their technology and capabilities discussed and demonstrated. Most of these instruments are already on orbit or approaching launch. These include the Magnetic Electron Ion Spectrometers (MagEIS) and the Relativistic Electron Proton Telescope (REPT) that are flying on the Van Allen Probes, the Fly's Eye Electron Proton Spectrometers (FEEPS) flying on the Magnetospheric Multiscale (MMS) mission, and Dosimeters flying on the AC6 Cubesat mission. We focus mostly on the electron measurement capability of these sensors while providing summary comments of their ion measurement capabilities if they have any.
C1 [Fennell, J. F.; Blake, J. B.; Claudepierre, S.; Mazur, J.; O'Brien, P.; Crain, W.; Mabry, D.; Clemmons, J.] Aerosp Corp, El Segundo, CA 90245 USA.
[Kanekal, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Baker, D.] Univ Colorado, LASP, Boulder, CO 80309 USA.
RP Fennell, JF (reprint author), Aerosp Corp, El Segundo, CA 90245 USA.
EM joseph.fennell@aero.org
OI Claudepierre, Seth/0000-0001-5513-5947; Clemmons,
James/0000-0002-5298-5222
FU Van Allen Probes ECT - JHU/APL [967399]; Southwest Research Institute
[792084N/E99017JD]; JHU/APL under NASA's prime [967399, NAS5-01072];
Research Opportunities in Space and Earth Science (ROSES)
[NNH12ZDA001N-GEO]; US Air Force SMC/AD (Space and Missile Systems
Center Advanced Systems and Development Directorate)
FX The development of the MagEIS and FEEPS sensors and the analysis of
their data were supported in part by Van Allen Probes ECT funding
provided by JHU/APL contract 967399 and by Southwest Research Institute
contract 792084N/E99017JD, respectively. The REPT sensor development at
LASP, University of Colorado, was supported by JHU/APL contract 967399
under NASA's prime contract NAS5-01072. CeREs is funded under the
NNH12ZDA001N-GEO for Research Opportunities in Space and Earth
Science-2012 (ROSES-2012). The AC6 bus was developed under the Aerospace
Corporation Multi-Program Acquisition Capability Enhancement Program,
and the AC6 dosimeter payload was funded by US Air Force SMC/AD (Space
and Missile Systems Center Advanced Systems and Development
Directorate). The Van Allen Probes ECT data are available at
http://www.rbsp-ect.lanl.gov/science/DataDirectories.php or from the
authors. The MMS/FEEPS data are available at
https://lasp.colorado.edu/mms/sdc/about/browse-wrapper/ or from the
authors.
NR 45
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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.
PD SEP
PY 2016
VL 121
IS 9
BP 8840
EP 8858
DI 10.1002/2016JA022588
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4QM
UT WOS:000385844000044
ER
PT J
AU Peterson, WK
Thiemann, EMB
Eparvier, FG
Andersson, L
Fowler, CM
Larson, D
Mitchell, D
Mazelle, C
Fontenla, J
Evans, JS
Xu, SS
Liemohn, M
Bougher, S
Sakai, S
Cravens, TE
Elrod, MK
Benna, M
Mahaffy, P
Jakosky, B
AF Peterson, W. K.
Thiemann, E. M. B.
Eparvier, Francis G.
Andersson, Laila
Fowler, C. M.
Larson, Davin
Mitchell, Dave
Mazelle, Christian
Fontenla, Juan
Evans, J. Scott
Xu, Shaosui
Liemohn, Mike
Bougher, Stephen
Sakai, Shotaro
Cravens, T. E.
Elrod, M. K.
Benna, M.
Mahaffy, P.
Jakosky, Bruce
TI Photoelectrons and solar ionizing radiation at Mars: Predictions versus
MAVEN observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE photoelectron; observation; model; Mars; thermosphere
ID ELECTRON; IRRADIANCE; MODEL; CODE; EUV
AB Understanding the evolution of the Martian atmosphere requires knowledge of processes transforming solar irradiance into thermal energy well enough to model them accurately. Here we compare Martian photoelectron energy spectra measured at periapsis by Mars Atmosphere and Volatile Evolution MissioN (MAVEN) with calculations made using three photoelectron production codes and three solar irradiance models as well as modeled and measured CO2 densities. We restricted our comparisons to regions where the contribution from solar wind electrons and ions were negligible. The two intervals examined on 19 October 2014 have different observed incident solar irradiance spectra. In spite of the differences in photoionization cross sections and irradiance spectra used, we find the agreement between models to be within the combined uncertainties associated with the observations from the MAVEN neutral density, electron flux, and solar irradiance instruments.
C1 [Peterson, W. K.; Thiemann, E. M. B.; Eparvier, Francis G.; Andersson, Laila; Fowler, C. M.; Jakosky, Bruce] Univ Colorado, LASP, Boulder, CO 80309 USA.
[Larson, Davin; Mitchell, Dave; Xu, Shaosui] Univ Calif Berkeley, SSL, Berkeley, CA 94720 USA.
[Mazelle, Christian] Univ Toulouse, IRAP, UPS OMP, Toulouse, France.
[Mazelle, Christian] CNRS, IRAP, Toulouse, France.
[Fontenla, Juan] Northwest Res Associates, Boulder, CO USA.
[Evans, J. Scott] Computat Phys Inc, Springfield, VA USA.
[Xu, Shaosui; Liemohn, Mike; Bougher, Stephen] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
[Sakai, Shotaro; Cravens, T. E.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Elrod, M. K.; Benna, M.; Mahaffy, P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Elrod, M. K.] Univ Maryland, CRESST, College Pk, MD 20742 USA.
RP Peterson, WK (reprint author), Univ Colorado, LASP, Boulder, CO 80309 USA.
EM bill.peterson@lasp.colorado.edu
RI Peterson, WK/A-8706-2009;
OI Peterson, WK/0000-0002-1513-6096; EPARVIER, FRANCIS/0000-0001-7143-2730;
Sakai, Shotaro/0000-0001-9135-2076
FU CNES; NASA's Planetary Science Division
FX We thank the MAVEN team for providing spacecraft instruments capable of
returning the exceptionally good data used in this report. Input values
used for the models are available on request from the lead author. Work
related to observations with the SWEA instrument was partially supported
by CNES. This research was supported by NASA's Planetary Science
Division.
NR 30
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U2 4
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.
PD SEP
PY 2016
VL 121
IS 9
BP 8859
EP 8870
DI 10.1002/2016JA022677
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4QM
UT WOS:000385844000045
ER
PT J
AU Verkhoglyadova, OP
Tsurutani, BT
Mannucci, AJ
Mlynczak, MG
Hunt, LA
Paxton, LJ
Komjathy, A
AF Verkhoglyadova, O. P.
Tsurutani, B. T.
Mannucci, A. J.
Mlynczak, M. G.
Hunt, L. A.
Paxton, L. J.
Komjathy, A.
TI Solar wind driving of ionosphere-thermosphere responses in three storms
near St. Patrick's Day in 2012, 2013, and 2015
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE ionosphere; thermosphere; coupling; solar wind; ICME; geomagnetic storm
ID ULTRAVIOLET IMAGER GUVI; GEOMAGNETIC STORMS; MAGNETIC STORMS; MASS
EJECTIONS; LOW-LATITUDE; CAWSES II; SUBSTORMS; SHOCKS; ELECTRODYNAMICS;
PROMINENCE
AB We identify interplanetary plasma regions associated with three intense interplanetary coronal mass ejections (ICMEs)-driven geomagnetic storm intervals which occurred around the same time of the year: day of year 74-79 (March) of 2012, 2013, and 2015. We show that differences in solar wind drivers lead to different dynamical ionosphere-thermosphere (IT) responses and to different preconditioning of the IT system. We introduce a new hourly based global metric for average low-latitude and northern middle-latitude vertical total electron content responses in the morning, afternoon, and evening local time ranges, derived from measurements from globally distributed Global Navigation Satellite System ground stations. Our novel technique of estimating nitric oxide (NO) cooling radiation in 11 degrees latitudinal zones is based on Thermosphere-Ionosphere-Mesosphere Energetics and Dynamics (TIMED)/Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) measurements. The thermospheric cooling throughout the storm phases is studied with this high latitudinal resolution for the first time. Additionally, TIMED/Global Ultraviolet Imager (GUVI) observations of the dynamical response of the thermospheric composition (O/N-2 ratio) are utilized to study negative ionospheric storm effects. Based on these data sets, we describe and quantify distinct IT responses to driving by ICME sheaths, magnetic clouds, coronal loop remnants, plasma discontinuities, and high-speed streams following ICMEs. Our analysis of coupling functions indicates strong connection between coupling with the solar wind and IT system response in ICME-type storms and also some differences. Knowledge of interplanetary features is crucial for understanding IT storm dynamics.
C1 [Verkhoglyadova, O. P.; Tsurutani, B. T.; Mannucci, A. J.; Komjathy, A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Mlynczak, M. G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Hunt, L. A.] Sci Syst & Applicat Inc, Hampton, VA USA.
[Paxton, L. J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
RP Verkhoglyadova, OP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Olga.Verkhoglyadova@jpl.nasa.gov
RI Paxton, Larry/D-1934-2015;
OI Paxton, Larry/0000-0002-2597-347X; Hunt, Linda/0000-0002-5330-541X
FU NASA TIMED project office
FX Portions of this work were done at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with NASA. M.
Mlynczak and L. Paxton would like to acknowledge support from the NASA
TIMED project office. O. Verkhoglyadova would like to thank M. Butala
(now at University of Illinois at Urbana-Champaign) for help with TEC
data processing and E. Astafyeva for stimulating discussions. SABER data
are available at http://saber.gats-inc.com/. GUVI data are available at
http://timedguvi.jhuapl.edu. Solar wind parameters and activity indices
are taken from the OMNI database
(http://omniweb.gsfc.nasa.gov/form/omni_min.html). We acknowledge IGS
data service, Geoscience Australia
(ftp://ftp.ga.gov.au/geodesy-outgoing/gnss/pub/maps/argn_map.pdf) and
the Geospatial Information Authority of Japan for providing GEONET data
(http://www.gsi.go.jp/ENGLISH/page_e30233.html). ACE magnetometer data
were provided by the ACE Science Center through
http://www.srl.caltech.edu/ACE/ASC/level2/index.html.
NR 75
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U1 3
U2 3
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.
PD SEP
PY 2016
VL 121
IS 9
BP 8900
EP 8923
DI 10.1002/2016JA022883
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4QM
UT WOS:000385844000048
ER
PT J
AU Zhou, YL
Luhr, H
Xiong, C
Pfaff, RF
AF Zhou, Yun-Liang
Luehr, Hermann
Xiong, Chao
Pfaff, Robert F.
TI Ionospheric storm effects and equatorial plasma irregularities during
the 17-18 March 2015 event
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE ionospheric storms; equatorial plasma irregularities; prompt penetration
electric field; disturbance dynamo electric field
ID PATRICKS DAY STORM; GEOMAGNETIC STORMS; ELECTRIC-FIELDS; F-REGION;
THERMOSPHERIC DYNAMICS; TOPSIDE IONOSPHERE; CHAMP OBSERVATIONS; BUBBLE
OCCURRENCE; MAGNETIC STORM; LOW LATITUDES
AB The intense magnetic storm on 17-18 March 2015 caused large disturbances of the ionosphere. Based on the plasma density (Ni) observations performed by the Swarm fleet of satellites, the Gravity Recovery and Climate Experiment mission, and the Communications/Navigation Outage Forecasting System satellite, we characterize the storm-related perturbations at low latitudes. All these satellites sampled the ionosphere in morning and evening time sectors where large modifications occurred. Modifications of plasma density are closely related to changes of the solar wind merging electric field (E-m). We consider two mechanisms, prompt penetration electric field (PPEF) and disturbance dynamo electric field (DDEF), as the main cause for the Ni redistribution, but effects of meridional wind are also taken into account. At the start of the storm main phase, the PPEF is enhancing plasma density on the dayside and reducing it on the nightside. Later, DDEF takes over and causes the opposite reaction. Unexpectedly, there appears during the recovery phase a strong density enhancement in the morning/prenoon sector and a severe Ni reduction in the afternoon/evening sector, and we suggest a combined effect of vertical plasma drift, and meridional wind is responsible for these ionospheric storm effects. Different from earlier studies about this storm, we also investigate the influence of storm dynamics on the initiation of equatorial plasma irregularities (EPIs). Shortly after the start of the storm main phase, EPIs appear in the postsunset sector. As a response to a short-lived decline of E-m, EPI activity appears in the early morning sector. Following the second start of the main phase, EPIs are generated for a few hours in the late evening sector. However, for the rest of the storm main phase, no more EPIs are initiated for more than 12h. Only after the onset of recovery phase does EPI activity start again in the postmidnight sector, lasting more than 7h. This comprehensive view of ionospheric storm effects and plasma irregularities adds to our understanding of conditions that lead to ionospheric instabilities.
C1 [Zhou, Yun-Liang] Wuhan Univ, Sch Elect Informat, Dept Space Phys, Wuhan, Peoples R China.
[Zhou, Yun-Liang; Luehr, Hermann; Xiong, Chao] GFZ German Res Ctr Geosci, Potsdam, Germany.
[Pfaff, Robert F.] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD USA.
RP Luhr, H (reprint author), GFZ German Res Ctr Geosci, Potsdam, Germany.
EM hluehr@gfz-potsdam.de
RI Barbosa, Flavio/G-3630-2013
FU Space Agency of the German Aerospace Center (DLR) through funds of the
Federal Ministry of Economics and Technology; National Nature Science
Foundation of China [41274194, 41431073]; China Scholarship Council
[201506275011]
FX The European Space Agency (ESA) is acknowledged for providing the Swarm
data. The electron density is obtained from http://earth.esa.int/swarm.
The GRACE mission is sponsored by the Space Agency of the German
Aerospace Center (DLR) through funds of the Federal Ministry of
Economics and Technology. The GRACE data are available at the
Information System and Data Center (ISDC) of GFZ German Research Centre
for Geosciences. Data set names are as follows: GA-OG-1B-NAVSOL,
GB-OG-1B-NAVSOL, and GX-OG-1B-KBRDAT. The solar wind and interplanetary
magnetic field data are derived from NASA's ACE mission, and they can be
found at http://www.srl.caltech.edu/ACE/ASC/level2/. The SYMH data are
provided by the World Data Center for Geomagnetism, Kyoto, and
downloaded from http://wdc.kugi.kyoto-u.ac.jp/aeasy/index.html. The
global ionospheric maps (GIM) are available from
ftp://cddis.gsfc.nasa.gov/gps/products/ionex/. The work of YunLiang Zhou
is supported by the National Nature Science Foundation of China
(41274194 and 41431073) and China Scholarship Council (201506275011).
NR 58
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U1 6
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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.
PD SEP
PY 2016
VL 121
IS 9
BP 9146
EP 9163
DI 10.1002/2016JA023122
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DZ4QM
UT WOS:000385844000065
ER
PT J
AU Qiu, JX
Crow, WT
Nearing, GS
AF Qiu, Jianxiu
Crow, Wade T.
Nearing, Grey S.
TI The Impact of Vertical Measurement Depth on the Information Content of
Soil Moisture for Latent Heat Flux Estimation
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID NEAR-SURFACE; ERS SCATTEROMETER; ASSIMILATION; VALIDATION; VEGETATION;
PRODUCTS; QUALITY
AB This study aims to identify the impact of vertical support on the information content of soil moisture (SM) for latent heat flux estimation. This objective is achieved via calculation of the mutual information (MI) content between multiple soil moisture variables (with different vertical supports) and current/future evaporative fraction (EF) using ground-based soil moisture and latent/sensible heat flux observations acquired from the AmeriFlux network within the contiguous United States. Through the intercomparison of MI results from different SM-EF pairs, the general value (for latent heat flux estimation) of superficial soil moisture observations theta(S), vertically integrated soil moisture observations theta(V), and vertically extrapolated soil moisture time series [soil wetness index (SWI) from a simple low-pass transformation of theta(S)] are examined. Results suggest that, contrary to expectations, 2-day averages of theta(S) and theta(V) have comparable mutual information with regards to EF. That is, there is no clear evidence that the information content for flux estimation is enhanced via deepening the vertical support of superficial soil moisture observations. In addition, the utility of SWI in monitoring and forecasting EF is partially dependent on the adopted parameterization of time-scale parameter T in the exponential filter. Similar results are obtained when analyses are conducted at the monthly time scale, only with larger error bars. The contrast between the results of this paper and past work focusing on utilizing soil moisture to predict vegetation condition demonstrates that the particular application should be considered when characterizing the information content of soil moisture time series measurements.
C1 [Qiu, Jianxiu] Sun Yat Sen Univ, Sch Geog & Planning, Guangdong Prov Key Lab Urbanizat & Geosimulat, 135 Xingang Xi Rd, Guangzhou 510275, Guangdong, Peoples R China.
[Crow, Wade T.] ARS, Hydrol & Remote Sensing Lab, USDA, Beltsville, MD USA.
[Nearing, Grey S.] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD USA.
RP Qiu, JX (reprint author), Sun Yat Sen Univ, Sch Geog & Planning, Guangdong Prov Key Lab Urbanizat & Geosimulat, 135 Xingang Xi Rd, Guangzhou 510275, Guangdong, Peoples R China.
EM qiujianxiu@mail.sysu.edu.cn
FU National Natural Science Foundation of China [41501450]; Natural Science
Foundation of Guangdong Province, China [2016A030310154]; Fundamental
Research Funds for the Central Universities [16lgpy06]
FX This work was supported by National Natural Science Foundation of China
(Grant 41501450), Natural Science Foundation of Guangdong Province,
China (Grant 2016A030310154), and the Fundamental Research Funds for the
Central Universities (16lgpy06). We thank the anonymous reviewers for
their helpful comments.
NR 31
TC 1
Z9 1
U1 3
U2 3
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
EI 1525-7541
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD SEP
PY 2016
VL 17
IS 9
BP 2419
EP 2430
DI 10.1175/JHM-D-16-0044.1
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DY8YZ
UT WOS:000385419800005
ER
PT J
AU Tan, J
Petersen, WA
Tokay, A
AF Tan, Jackson
Petersen, Walter A.
Tokay, Ali
TI A Novel Approach to Identify Sources of Errors in IMERG for GPM Ground
Validation
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID MULTISATELLITE PRECIPITATION ANALYSIS; UNCERTAINTY QUANTIFICATION;
PASSIVE MICROWAVE; UNITED-STATES; ANALYSIS TMPA; DAY-1 IMERG; REAL-TIME;
PRODUCTS; RESOLUTION; RAINFALL
AB The comparison of satellite and high-quality, ground-based estimates of precipitation is an important means to assess the confidence in satellite-based algorithms and to provide a benchmark for their continued development and future improvement. To these ends, it is beneficial to identify sources of estimation uncertainty, thereby facilitating a precise understanding of the origins of the problem. This is especially true for new datasets such as the Integrated Multisatellite Retrievals for GPM(IMERG) product, which provides global precipitation gridded at a high resolution using measurements from different sources and techniques. Here, IMERG is evaluated against a dense network of gauges in the mid-Atlantic region of the United States. A novel approach is presented, leveraging ancillary variables in IMERG to attribute the errors to the individual instruments or techniques within the algorithm. As a whole, IMERG exhibits some misses and false alarms for rain detection, while its rain-rate estimates tend to overestimate drizzle and underestimate heavy rain with considerable random error. Tracing the errors to their sources, the most reliable IMERG estimates come from passive microwave satellites, which in turn exhibit a hierarchy of performance. The morphing technique has comparable proficiency with the less skillful satellites, but infrared estimations perform poorly. The approach here demonstrated that, underlying the overall reasonable performance of IMERG, different sources have different reliability, thus enabling both IMERG users and developers to better recognize the uncertainty in the estimate. Future validation efforts are urged to adopt such a categorization to bridge between gridded rainfall and instantaneous satellite estimates.
C1 [Tan, Jackson] Univ Space Res Assoc, Greenbelt, MD USA.
[Tan, Jackson; Tokay, Ali] NASA, Goddard Space Flight Ctr, Code 613,Bldg 33,Room C327,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Petersen, Walter A.] NASA, Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL USA.
[Tokay, Ali] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA.
RP Tan, J (reprint author), NASA, Goddard Space Flight Ctr, Code 613,Bldg 33,Room C327,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM jackson.tan@nasa.gov
RI Measurement, Global/C-4698-2015;
OI Tan, Jackson/0000-0001-7085-3074
FU GPM Mission; PMM Science Team
FX We thank George Huffman and David Bolvin for informative discussions on
IMERG and Yudong Tian for instructive consultation on the multiplicative
error model. The gauge data are maintained by the NASA Wallops GPM GV
Team, and we acknowledge David Wolff for his assistance with the data.
The MRMS data were processed for the GPM GV Program by Pierre-Emmanuel
Kirstetter, and we appreciate the further assistance provided by Jianxin
Wang. We also thank two anonymous reviewers for their comments and
suggestions. J.T. is supported by an appointment to the NASA
Postdoctoral Program at Goddard Space Flight Center, administered by
Universities Space Research Association through a contract with NASA.
W.A.P. and A.T. acknowledge support from the GPM Mission (Project
Scientist, Gail S. Jackson, and GV Systems Manager, Mathew Schwaller)
and also PMM Science Team funding provided by Dr. Ramesh Kakar. The
IMERG data were provided by the NASA Goddard Space Flight Center's PMM
and PPS teams, which develop and compute the IMERG as a contribution to
GPM, and archived at the NASA GES DISC. All codes used in this analysis
are freely available at
https://github.com/JacksonTanBS/2016_Tan-et-al._JHM.
NR 52
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U1 10
U2 10
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
EI 1525-7541
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD SEP
PY 2016
VL 17
IS 9
BP 2477
EP 2491
DI 10.1175/JHM-D-16-0079.1
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DY8YZ
UT WOS:000385419800008
ER
PT J
AU Righter, K
Cosca, MA
Morgan, LE
AF Righter, K.
Cosca, M. A.
Morgan, L. E.
TI Preservation of ancient impact ages on the R chondrite parent body:
Ar-40/Ar-39 age of hornblende-bearing R chondrite LAP 04840
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID INNER SOLAR-SYSTEM; RUMURUTI CHONDRITE; EXPOSURE AGES; HISTORY;
MINERALOGY; METEORITE; AMPHIBOLE; SHOCK; ABUNDANCES; CHRONOLOGY
AB The hornblende- and biotite-bearing R chondrite LAP 04840 is a rare kind of meteorite possibly containing outer solar system water stored during metamorphism or postshock annealing deep within an asteroid. Because little is known regarding its age and origin, we determined Ar-40/Ar-39 ages on hornblende-rich separates of the meteorite, and obtained plateau ages of 4340(+/- 40) to 4380(+/- 30) Ma. These well-defined plateau ages, coupled with evidence for postshock annealing, indicate this meteorite records an ancient shock event and subsequent annealing. The age of 4340-4380Ma (or 4.34-4.38Ga) for this and other previously dated R chondrites is much older than most impact events recorded by ordinary chondrites and points to an ancient event or events that predated the late heavy bombardment that is recorded in so many meteorites and lunar samples.
C1 [Righter, K.] NASA, Johnson Space Ctr, Mailcode XI2,2101 NASA Pkwy, Houston, TX 77058 USA.
[Cosca, M. A.; Morgan, L. E.] US Geol Survey, Denver Fed Ctr, MS 963, Denver, CO 80225 USA.
RP Righter, K (reprint author), NASA, Johnson Space Ctr, Mailcode XI2,2101 NASA Pkwy, Houston, TX 77058 USA.
EM kevin.righter-1@nasa.gov
FU RTOP from NASA Cosmochemistry program; NSF; NASA
FX Funding for this study was provided by an RTOP to KR from the NASA
Cosmochemistry program. U.S. Antarctic meteorite samples are recovered
by the Antarctic Search for Meteorites (ANSMET) program which has been
funded by NSF and NASA, and characterized and curated by the Department
of Mineral Sciences of the Smithsonian Institution and Astromaterials
Curation Office at NASA Johnson Space Center. Any use of trade, product,
or firm names is for descriptive purposes only and does not imply
endorsement by the U.S. government. Reviews by J. Park, M. McCanta, and
comments of AE Yamaguchi helped to improve presentation of our results.
NR 47
TC 0
Z9 0
U1 2
U2 2
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 SEP
PY 2016
VL 51
IS 9
BP 1678
EP 1684
DI 10.1111/maps.12692
PG 7
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DW4QX
UT WOS:000383629200008
ER
PT J
AU Pugh, TAM
Muller, C
Elliott, J
Deryng, D
Folberth, C
Olin, S
Schmid, E
Arneth, A
AF Pugh, T. A. M.
Mueller, C.
Elliott, J.
Deryng, D.
Folberth, C.
Olin, S.
Schmid, E.
Arneth, A.
TI Climate analogues suggest limited potential for intensification of
production on current croplands under climate change
SO NATURE COMMUNICATIONS
LA English
DT Article
ID RISING CO2 CONCENTRATIONS; CROP YIELD; IMPACTS; FOOD; AGRICULTURE;
MANAGEMENT; MODEL
AB Climate change could pose a major challenge to efforts towards strongly increase food production over the coming decades. However, model simulations of future climate-impacts on crop yields differ substantially in the magnitude and even direction of the projected change. Combining observations of current maximum-attainable yield with climate analogues, we provide a complementary method of assessing the effect of climate change on crop yields. Strong reductions in attainable yields of major cereal crops are found across a large fraction of current cropland by 2050. These areas are vulnerable to climate change and have greatly reduced opportunity for agricultural intensification. However, the total land area, including regions not currently used for crops, climatically suitable for high attainable yields of maize, wheat and rice is similar by 2050 to the present-day. Large shifts in land-use patterns and crop choice will likely be necessary to sustain production growth rates and keep pace with demand.
C1 [Pugh, T. A. M.; Arneth, A.] Karlsruhe Inst Technol, Inst Meteorol & Climate Res Atmospher Environm Re, Kreuzeckbahnstr 19, D-82467 Garmisch Partenkirchen, Germany.
[Pugh, T. A. M.] Univ Birmingham, Sch Geog Earth & Environm Sci, Birmingham B15 2TT, W Midlands, England.
[Pugh, T. A. M.] Univ Birmingham, Birmingham Inst Forest Res, Birmingham B15 2TT, W Midlands, England.
[Mueller, C.] Potsdam Inst Climate Impact Res, POB 60 12 03, D-14412 Potsdam, Germany.
[Elliott, J.; Deryng, D.] Univ Chicago, Chicago, IL 60637 USA.
[Elliott, J.; Deryng, D.] Argonne Natl Lab, Computat Inst, Chicago, IL 60637 USA.
[Deryng, D.] Columbia Univ, Ctr Climate Syst Res, New York, NY 10025 USA.
[Deryng, D.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Folberth, C.] Int Inst Appl Syst Anal, Ecosyst Serv & Management Program, A-2361 Laxenburg, Austria.
[Folberth, C.] Univ Munich, Dept Geog, D-80333 Munich, Germany.
[Olin, S.] Lund Univ, Dept Phys Geog & Ecosyst Sci, Solvegatan 12, S-22362 Lund, Sweden.
[Schmid, E.] Univ Nat Resources & Life Sci, Dept Econ & Social Sci, Feistmantelstr 4, A-1180 Vienna, Austria.
RP Pugh, TAM (reprint author), Karlsruhe Inst Technol, Inst Meteorol & Climate Res Atmospher Environm Re, Kreuzeckbahnstr 19, D-82467 Garmisch Partenkirchen, Germany.
EM t.a.m.pugh@bham.ac.uk
RI Deryng, Delphine/F-7417-2010; Pugh, Thomas/A-3790-2010;
OI Deryng, Delphine/0000-0001-6214-7241; Pugh, Thomas/0000-0002-6242-7371;
Schmid, Erwin/0000-0003-4783-9666; Muller, Christoph/0000-0002-9491-3550
FU European Commission [603542 (LUC4C)]; German Federal Ministry of
Education and Research (BMBF), through the Helmholtz Association; MACMIT
project - BMBF [01LN1317A]; Research Fellowship of Ludwig Maximilian
University Munich; Global Gridded Crop Model Intercomparison project
(GGCMI) of the Agricultural Model Intercomparison and Improvement
Project (AgMIP)
FX T.A.M.P. and A.A. were funded by the European Commission's 7th Framework
Programme, under Grant Agreement number 603542 (LUC4C). This work was
supported, in part, by the German Federal Ministry of Education and
Research (BMBF), through the Helmholtz Association and its research
program ATMO. C.M. acknowledges financial support from the MACMIT
project (01LN1317A) funded through the BMBF. C.F. was supported by a
Research Fellowship of Ludwig Maximilian University Munich. We
acknowledge the World Climate Research Programme's Working Group on
Coupled Modelling, which is responsible for CMIP, and we thank the
climate modelling groups for producing and making available their model
output. The Global Gridded Crop Model Intercomparison project (GGCMI) of
the Agricultural Model Intercomparison and Improvement Project (AgMIP)
is thanked for funding travel to workshops where the ideas in this
manuscript were developed. This is paper number 17 of the Birmingham
Institute of Forest Research.
NR 34
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U2 9
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 SEP
PY 2016
VL 7
AR 12608
DI 10.1038/ncomms12608
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DY7BH
UT WOS:000385283700001
PM 27646707
ER
PT J
AU Wang, ZC
Monteiro, CD
Jagodnik, KM
Fernandez, NF
Gundersen, GW
Rouillard, AD
Jenkins, SL
Feldmann, AS
Hu, KS
McDermott, MG
Duan, QN
Clark, NR
Jones, MR
Kou, Y
Goff, T
Woodland, H
Amaral, FMR
Szeto, GL
Fuchs, O
Rose, SMSF
Sharma, S
Schwartz, U
Bausela, XB
Szymkiewicz, M
Maroulis, V
Salykin, A
Barra, CM
Kruth, CD
Bongio, NJ
Mathur, V
Todoric, RD
Rubin, UE
Malatras, A
Fulp, CT
Galindo, JA
Motiejunaite, R
Juschke, C
Dishuck, PC
Lahl, K
Jafari, M
Aibar, S
Zaravinos, A
Steenhuizen, LH
Allison, LR
Gamallo, P
Segura, FD
Devlin, TD
Perez-Garcia, V
Ma'ayan, A
AF Wang, Zichen
Monteiro, Caroline D.
Jagodnik, Kathleen M.
Fernandez, Nicolas F.
Gundersen, Gregory W.
Rouillard, Andrew D.
Jenkins, Sherry L.
Feldmann, Axel S.
Hu, Kevin S.
McDermott, Michael G.
Duan, Qiaonan
Clark, Neil R.
Jones, Matthew R.
Kou, Yan
Goff, Troy
Woodland, Holly
Amaral, Fabio M. R.
Szeto, Gregory L.
Fuchs, Oliver
Rose, Sophia M. Schussler-Fiorenza
Sharma, Shvetank
Schwartz, Uwe
Bengoetxea Bausela, Xabier
Szymkiewicz, Maciej
Maroulis, Vasileios
Salykin, Anton
Barra, Carolina M.
Kruth, Candice D.
Bongio, Nicholas J.
Mathur, Vaibhav
Todoric, Radmila D.
Rubin, Udi E.
Malatras, Apostolos
Fulp, Carl T.
Galindo, John A.
Motiejunaite, Ruta
Jueschke, Christoph
Dishuck, Philip C.
Lahl, Katharina
Jafari, Mohieddin
Aibar, Sara
Zaravinos, Apostolos
Steenhuizen, Linda H.
Allison, Lindsey R.
Gamallo, Pablo
de Andres Segura, Fernando
Devlin, Tyler Dae
Perez-Garcia, Vicente
Ma'ayan, Avi
TI Extraction and analysis of signatures from the Gene Expression Omnibus
by the crowd
SO NATURE COMMUNICATIONS
LA English
DT Article
ID FACIOSCAPULOHUMERAL MUSCULAR-DYSTROPHY; ENDOMETRIAL CANCER-RISK;
ESTROGEN-RECEPTOR; HEPATOCELLULAR-CARCINOMA; DIFFERENTIAL EXPRESSION;
DATABASE; DISEASE; DISCOVERY; INSULIN; GROWTH
AB Gene expression data are accumulating exponentially in public repositories. Reanalysis and integration of themed collections from these studies may provide new insights, but requires further human curation. Here we report a crowdsourcing project to annotate and reanalyse a large number of gene expression profiles from Gene Expression Omnibus (GEO). Through a massive open online course on Coursera, over 70 participants from over 25 countries identify and annotate 2,460 single-gene perturbation signatures, 839 disease versus normal signatures, and 906 drug perturbation signatures. All these signatures are unique and are manually validated for quality. Global analysis of these signatures confirms known associations and identifies novel associations between genes, diseases and drugs. The manually curated signatures are used as a training set to develop classifiers for extracting similar signatures from the entire GEO repository. We develop a web portal to serve these signatures for query, download and visualization.
C1 [Wang, Zichen; Monteiro, Caroline D.; Jagodnik, Kathleen M.; Fernandez, Nicolas F.; Gundersen, Gregory W.; Rouillard, Andrew D.; Jenkins, Sherry L.; Feldmann, Axel S.; Hu, Kevin S.; McDermott, Michael G.; Duan, Qiaonan; Clark, Neil R.; Jones, Matthew R.; Kou, Yan; Goff, Troy; Ma'ayan, Avi] Icahn Sch Med Mt Sinai, Dept Pharmacol Sci, LINCS Data Coordinat & Integrat Ctr BD2K, Illuminating Druggable Genome Knowledge Managemen, One Gustave L Levy Pl Box 1215, New York, NY 10029 USA.
[Jagodnik, Kathleen M.] NASA, Fluid Phys & Transport Processes Branch, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
[Jagodnik, Kathleen M.] Baylor Coll Med, Ctr Space Med, 1 Baylor Plaza, Houston, TX 77030 USA.
[Woodland, Holly] Daylesford, Weybridge KT13 0RZ, Surrey, England.
[Amaral, Fabio M. R.] Univ Nottingham, Sch Biosci, Sutton Bonington Campus, Loughborough LE12 5RD, Leics, England.
[Szeto, Gregory L.] MIT, Dept Biol Engn, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Szeto, Gregory L.] MIT, David H Koch Inst Integrat Canc Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Szeto, Gregory L.] MIT, Dept Mat Sci & Engn, Cambridge, MA 02139 USA.
[Szeto, Gregory L.] MIT, Ragon Inst MGH, 400 Technol Sq, Cambridge, MA 02139 USA.
[Szeto, Gregory L.] Harvard, 400 Technol Sq, Cambridge, MA 02139 USA.
[Fuchs, Oliver] Univ Munich, German Ctr Lung Res DZL, Dr von Hauner Univ Childrens Hosp, Paediat Allergol & Pulmonol, Lindwurmstr 4, D-80337 Munich, Germany.
[Rose, Sophia M. Schussler-Fiorenza] Veteran Affairs Palo Alto Hlth Care Syst, Spinal Cord Injury Serv, Palo Alto, CA 94304 USA.
[Rose, Sophia M. Schussler-Fiorenza] Stanford Sch Med, Dept Neurosurg, Stanford, CA 94304 USA.
[Sharma, Shvetank] Inst Liver & Biliary Sci, Dept Res, D1 Vasant Kunj, New Delhi 110070, India.
[Schwartz, Uwe] Univ Regensburg, Dept Biochem 3, Univ Str 31, D-93053 Regensburg, Germany.
[Bengoetxea Bausela, Xabier] Univ Navarra, Dept Pharmacol & Toxicol, Irunlarrea 1, E-31008 Pamplona, Spain.
[Szymkiewicz, Maciej] Polish Acad Sci, Warsaw Sch Informat Technol Auspices, 6 Newelska St, PL-01447 Warsaw, Poland.
[Maroulis, Vasileios] Plomariou 1 St, Athens 15126, Greece.
[Salykin, Anton] Masaryk Univ, Fac Med, Dept Biol, Brno 62500, Czech Republic.
[Barra, Carolina M.] Hosp del Mar, IMIM, PRBB Barcelona, Dr Aiguader 88, Barcelona 08003, Spain.
[Kruth, Candice D.] 85 Hailey Ln,Apt C-11, Strasburg, VA 22657 USA.
[Bongio, Nicholas J.] Shenandoah Univ, Dept Biol, 1460 Univ Dr Winchester, Winchester, VA 22601 USA.
[Mathur, Vaibhav] IBM India Pvt Ltd, Bengaluru 560045, India.
[Todoric, Radmila D.] Dr Aleksandra Sijacica 20, Backa Topola 24300, Serbia.
[Rubin, Udi E.] Columbia Univ, Dept Biol Sci, 600 Fairchild Ctr,Mail Code 2402, New York, NY 10032 USA.
[Malatras, Apostolos] Univ Paris 04, Univ Paris 06, INSERM UMRS975, Ctr Res Myol,CNRS FRE3617, 47 Blvd Hop, F-75013 Paris, France.
[Fulp, Carl T.] 13-1,Higashi 4 Chome Shibuya Ku, Tokyo 1500011, Japan.
[Galindo, John A.] Univ Nacl Colombia, Dept Biol, Cr 30 45-08, Bogota, Colombia.
[Galindo, John A.] Univ Nacl Colombia, Inst Genet, Cr 30 45-08, Bogota, Colombia.
[Motiejunaite, Ruta] Brigham & Womens Hosp, Ctr Interdisciplinary Cardiovasc Sci, 3 Blackfan Circle, Boston, MA 02115 USA.
[Jueschke, Christoph] Carl von Ossietzky Univ Oldenburg, Fac Med & Hlth Sci, Dept Human Genet, Ammerlander Heerstr 114-118, D-26129 Oldenburg, Germany.
[Dishuck, Philip C.] 2312 40th ST NW 2, Washington, DC 20007 USA.
[Lahl, Katharina] Tech Univ Denmark, Natl Vet Inst, Bulowsvej 27 Bldg 2-3, DK-1870 Frederiksberg, Denmark.
[Jafari, Mohieddin] Pasteur Inst Iran, Biotechnol Res Ctr, Prot Chem & Prote Unit, 358,12th Farwardin Ave,Jomhhoori St, Tehran 13164, Iran.
[Jafari, Mohieddin] Inst Res Fundamental Sci, Sch Biol Sci, Niavaran Sq,POB, Tehran 193955746, Iran.
[Aibar, Sara] Univ Salamanca, Madrid 37008, Spain.
[Zaravinos, Apostolos] Karolinska Inst, Dept Lab Med, Div Clin Immunol, Alfred Nobels Alle 8,Level 7, SE-14186 Stockholm, Sweden.
[Zaravinos, Apostolos] European Univ Cyprus, Sch Sci, Dept Life Sci, 6 Diogenes Str Engomi,POB 22006, CY-1516 Nicosia, Cyprus.
[Steenhuizen, Linda H.] Anna Blamansingel 216, NL-102 SW Amsterdam, Netherlands.
[Allison, Lindsey R.] 7300 Brompton 6024, Houston, TX 77025 USA.
[Gamallo, Pablo] Aligustre 30 1-C, Madrid 28039, Spain.
[de Andres Segura, Fernando] Extremadura Univ Hosp, Clin Res Ctr, CICAB, Elvas Av,S-N 06006, Badajoz 06006, Spain.
[Devlin, Tyler Dae] 69 Brown St,Box 8278, Providence, RI 02912 USA.
[Perez-Garcia, Vicente] CSIC, Ctr Nacl Biotecnol, Dept Immunol & Oncol, C-Darwin 3, E-28049 Madrid, Spain.
RP Ma'ayan, A (reprint author), Icahn Sch Med Mt Sinai, Dept Pharmacol Sci, LINCS Data Coordinat & Integrat Ctr BD2K, Illuminating Druggable Genome Knowledge Managemen, One Gustave L Levy Pl Box 1215, New York, NY 10029 USA.
EM avi.maayan@mssm.edu
OI Wang, Zichen/0000-0002-1415-1286; Szymkiewicz,
Maciej/0000-0003-1469-9396; Schussler-Fiorenza Rose, Sophia
Miryam/0000-0002-6311-6671; De Andres, Fernando/0000-0003-1076-0743
FU NIH [R01GM098316, U54HL127624, U54CA189201]
FX This work is supported by NIH grants: R01GM098316, U54HL127624 and
U54CA189201 to A.M.
NR 78
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U1 5
U2 5
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 SEP
PY 2016
VL 7
AR 12846
DI 10.1038/ncomms12846
PG 11
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DY8FA
UT WOS:000385363000014
PM 27667448
ER
PT J
AU Kassemi, M
Thompson, D
AF Kassemi, Mohammad
Thompson, David
TI Prediction of renal crystalline size distributions in space using a PBE
analytic model. 1. Effect of microgravity-induced biochemical
alterations
SO AMERICAN JOURNAL OF PHYSIOLOGY-RENAL PHYSIOLOGY
LA English
DT Article
DE nephrolithiasis; gravity; weightlessness; crystal nucleation; crystal
growth; agglomeration
ID URINARY STONE FORMATION; CALCIUM-OXALATE; RISK-FACTORS; GROWTH; DISEASE;
AGGLOMERATION; INHIBITION; ASTRONAUTS; KINETICS; KIDNEY
AB An analytical Population Balance Equation model is developed and used to assess the risk of critical renal stone formation for astronauts during future space missions. The model uses the renal biochemical profile of the subject as input and predicts the steady-state size distribution of the nucleating, growing, and agglomerating calcium oxalate crystals during their transit through the kidney. The model is verified through comparison with published results of several crystallization experiments. Numerical results indicate that the model is successful in clearly distinguishing between 1-G normal and 1-G recurrent stone-former subjects based solely on their published 24-h urine biochemical profiles. Numerical case studies further show that the predicted renal calculi size distribution for a microgravity astronaut is closer to that of a recurrent stone former on Earth rather than to a normal subject in 1 G. This interestingly implies that the increase in renal stone risk level in microgravity is relatively more significant for a normal person than a stone former. However, numerical predictions still underscore that the stone-former subject carries by far the highest absolute risk of critical stone formation during space travel.
C1 [Kassemi, Mohammad; Thompson, David] NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, 21000 Brookpark Rd,MS 110-3, Cleveland, OH 44135 USA.
RP Kassemi, M (reprint author), NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, 21000 Brookpark Rd,MS 110-3, Cleveland, OH 44135 USA.
EM Mohammad.Kassemi@nasa.gov
FU Exploration Medical Capabilities Element of NASA's Human Research
FX We gratefully acknowledge funding support from the Exploration Medical
Capabilities Element of NASA's Human Research.
NR 41
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U1 2
U2 2
PU AMER PHYSIOLOGICAL SOC
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA
SN 1931-857X
EI 1522-1466
J9 AM J PHYSIOL-RENAL
JI Am. J. Physiol.-Renal Physiol.
PD SEP 1
PY 2016
VL 311
IS 3
BP F520
EP F530
DI 10.1152/ajprenal.00401.2015
PG 11
WC Physiology; Urology & Nephrology
SC Physiology; Urology & Nephrology
GA DY3FZ
UT WOS:000384977500004
PM 27279490
ER
PT J
AU Kassemi, M
Thompson, D
AF Kassemi, Mohammad
Thompson, David
TI Prediction of renal crystalline size distributions in space using a PBE
analytic model. 2. Effect of dietary countermeasures
SO AMERICAN JOURNAL OF PHYSIOLOGY-RENAL PHYSIOLOGY
LA English
DT Article
DE nephrolithiasis; gravity; weightlessness; crystal nucleation; crystal
growth; agglomeration; inhibition; dietary countermeasures
ID OXALATE MONOHYDRATE CRYSTALLIZATION; POTASSIUM-MAGNESIUM CITRATE;
CALCIUM-OXALATE; STONE FORMATION; DIHYDRATE CRYSTALLIZATION; BED REST;
INHIBITION; GROWTH; URINE; FLIGHT
AB An analytic Population Balance Equation model is used to assess the efficacy of citrate, pyrophosphate, and augmented fluid intake as dietary countermeasures aimed at reducing the risk of renal stone formation for astronauts. The model uses the measured biochemical profile of the astronauts as input and predicts the steady-state size distribution of the nucleating, growing, and agglomerating renal calculi subject to biochemical changes brought about by administration of these dietary countermeasures. Numerical predictions indicate that an increase in citrate levels beyond its average normal ground-based urinary values is beneficial but only to a limited extent. Unfortunately, results also indicate that any decline in the citrate levels during space travel below its normal urinary values on Earth can easily move the astronaut into the stone-forming risk category. Pyrophosphate is found to be an effective inhibitor since numerical predictions indicate that even at quite small urinary concentrations, it has the potential of shifting the maximum crystal aggregate size to a much smaller and plausibly safer range. Finally, our numerical results predict a decline in urinary volume below 1.5 liters/day can act as a dangerous promoter of renal stone development in microgravity while urinary volume levels of 2.5-3 liters/day can serve as effective space countermeasures.
C1 [Kassemi, Mohammad; Thompson, David] NASA, Natl Ctr Space Explorat Res, Glenn Res Ctr, 21000 Brookpk Rd,MS 110-3, Cleveland, OH 44135 USA.
RP Kassemi, M (reprint author), NASA, Natl Ctr Space Explorat Res, Glenn Res Ctr, 21000 Brookpk Rd,MS 110-3, Cleveland, OH 44135 USA.
EM Mohammad.Kassemi@nasa.gov
FU Exploration Medical Capabilities Element of NASA's Human Research
Project
FX We gratefully acknowledge funding support from the Exploration Medical
Capabilities Element of NASA's Human Research Project.
NR 44
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U1 3
U2 3
PU AMER PHYSIOLOGICAL SOC
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA
SN 1931-857X
EI 1522-1466
J9 AM J PHYSIOL-RENAL
JI Am. J. Physiol.-Renal Physiol.
PD SEP 1
PY 2016
VL 311
IS 3
BP F531
EP F538
DI 10.1152/ajprenal.00402.2015
PG 8
WC Physiology; Urology & Nephrology
SC Physiology; Urology & Nephrology
GA DY3FZ
UT WOS:000384977500005
PM 27279491
ER
PT J
AU Mukai, K
Luna, GJM
Cusumano, G
Segreto, A
Munari, U
Sokoloski, JL
Lucy, AB
Nelson, T
Nunez, NE
AF Mukai, K.
Luna, G. J. M.
Cusumano, G.
Segreto, A.
Munari, U.
Sokoloski, J. L.
Lucy, A. B.
Nelson, T.
Nunez, N. E.
TI SU Lyncis, a hard X-ray bright M giant: clues point to a large hidden
population of symbiotic stars
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE binaries: symbiotic; stars: individual: SU Lyn; X-rays: binaries
ID SWIFT-BAT; T CRB; HIPPARCOS; EVOLUTION; OUTBURST; CATALOG; BINARY; NOVAE
AB Symbiotic star surveys have traditionally relied almost exclusively on low resolution optical spectroscopy. However, we can obtain a more reliable estimate of their total Galactic population by using all available signatures of the symbiotic phenomenon. Here we report the discovery of a hard X-ray source, 4PBC J0642.9+5528, in the Swift hard X-ray all-sky survey, and identify it with a poorly studied red giant, SU Lyn, using pointed Swift observations and ground-based optical spectroscopy. The X-ray spectrum, the optical to UV spectrum, and the rapid UV variability of SU Lyn are all consistent with our interpretation that it is a symbiotic star containing an accreting white dwarf. The symbiotic nature of SU Lyn went unnoticed until now, because it does not exhibit emission lines strong enough to be obvious in low resolution spectra. We argue that symbiotic stars without shell-burning have weak emission lines, and that the current lists of symbiotic stars are biased in favour of shell-burning systems. We conclude that the true population of symbiotic stars has been underestimated, potentially by a large factor.
C1 [Mukai, K.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Mukai, K.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Mukai, K.] Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
[Luna, G. J. M.] UBA, CONICET, IAFE, Ave Inte Guiraldes 2620,C1428ZAA, Buenos Aires, DF, Argentina.
[Cusumano, G.; Segreto, A.] INAF Ist Astrofis Spaziale & Fis Cosm, Via U La Malfa 153, I-90146 Palermo, Italy.
[Munari, U.] INAF Astron Observ Padova, I-36012 Asiago, VI, Italy.
[Sokoloski, J. L.; Lucy, A. B.] Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA.
[Nelson, T.] Univ Pittsburgh, Dept Phys & Astron, 3941 OHara St, Pittsburgh, PA 15260 USA.
[Nunez, N. E.] UNSJ, ICATE, CONICET, Ave Espana S E-1512,J5402 DSP, San Juan, Argentina.
RP Mukai, K (reprint author), NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.; Mukai, K (reprint author), NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.; Mukai, K (reprint author), Univ Maryland Baltimore Cty, Dept Phys, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
EM Koji.Mukai@nasa.gov
FU NASA ADAP grant [NNX15AF19G]; [ANPCYT-PICT 0478/14]
FX We thank Neil Gehrels, the PI of the Swift mission, for a generous
allocation of TOO time. GJML and NEN are members of the 'Carrera del
Investigador Cientifico (CIC)' of CONICET and acknowledge support from
Argentina under grant ANPCYT-PICT 0478/14. JLS and ABL acknowledge
support from NASA ADAP grant NNX15AF19G. JLS thanks Scott Kenyon for
conversations (a decade ago) about shell burning and selection bias.
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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 SEP 1
PY 2016
VL 461
IS 1
BP L1
EP L5
DI 10.1093/mnrasl/slw087
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DV9OE
UT WOS:000383269900001
ER
PT J
AU Fierce, L
Bond, TC
Bauer, SE
Mena, F
Riemer, N
AF Fierce, Laura
Bond, Tami C.
Bauer, Susanne E.
Mena, Francisco
Riemer, Nicole
TI Black carbon absorption at the global scale is affected by
particle-scale diversity in composition
SO NATURE COMMUNICATIONS
LA English
DT Article
ID MIXING STATE; SIZE DISTRIBUTIONS; OPTICAL-PROPERTIES; LIGHT-ABSORPTION;
BROWN CARBON; AEROSOL; SOOT; MODEL; CLIMATE; AMPLIFICATION
AB Atmospheric black carbon (BC) exerts a strong, but uncertain, warming effect on the climate. BC that is coated with non-absorbing material absorbs more strongly than the same amount of BC in an uncoated particle, but the magnitude of this absorption enhancement (E-abs) is not well constrained. Modelling studies and laboratory measurements have found stronger absorption enhancement than has been observed in the atmosphere. Here, using a particle-resolved aerosol model to simulate diverse BC populations, we show that absorption is overestimated by as much as a factor of two if diversity is neglected and population-averaged composition is assumed across all BC-containing particles. If, instead, composition diversity is resolved, we find E-abs=1-1.5 at low relative humidity, consistent with ambient observations. This study offers not only an explanation for the discrepancy between modelled and observed absorption enhancement, but also demonstrates how particle-scale simulations can be used to develop relationships for global-scale models.
C1 [Fierce, Laura] Brookhaven Natl Lab, Dept Environm & Climate Sci, Upton, NY 11973 USA.
[Fierce, Laura] Univ Corp Atmospheric Res, Visiting Scientists Program, Boulder, CO 80307 USA.
[Bond, Tami C.; Mena, Francisco] Univ Illinois, Dept Civil & Environm Engn, Urbana, IL 61801 USA.
[Bauer, Susanne E.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Bauer, Susanne E.] Columbia Univ, Earth Inst, New York, NY 10025 USA.
[Riemer, Nicole] Univ Illinois, Dept Atmospher Sci, Urbana, IL 61801 USA.
RP Fierce, L (reprint author), Brookhaven Natl Lab, Dept Environm & Climate Sci, Upton, NY 11973 USA.; Fierce, L (reprint author), Univ Corp Atmospheric Res, Visiting Scientists Program, Boulder, CO 80307 USA.
EM lfierce@bnl.gov
FU US Environmental Protection Agency [R83504201]; NASA [NNX09AK66G];
Department of Energy [DE-FG02-08ER64533]; Fulbright-Chile CONICYT
fellowship; NOAA Climate & Global Change Postdoctoral Fellowship through
the University Corporation for Atmospheric Research Visiting Scientists
Program
FX This work was supported by the US Environmental Protection Agency
(R83504201) and by NASA (NNX09AK66G). F. Mena was funded by the
Department of Energy under DE-FG02-08ER64533 and by a Fulbright-Chile
CONICYT fellowship. L. Fierce is funded by a NOAA Climate & Global
Change Postdoctoral Fellowship through the University Corporation for
Atmospheric Research Visiting Scientists Program.
NR 49
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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 SEP
PY 2016
VL 7
AR 12361
DI 10.1038/ncomms12361
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DY3CG
UT WOS:000384967800001
PM 27580627
ER
PT J
AU Thiery, W
Davin, EL
Seneviratne, SI
Bedka, K
Lhermitte, S
van Lipzig, NPM
AF Thiery, Wim
Davin, Edouard L.
Seneviratne, Sonia I.
Bedka, Kristopher
Lhermitte, Stef
van Lipzig, Nicole P. M.
TI Hazardous thunderstorm intensification over Lake Victoria
SO NATURE COMMUNICATIONS
LA English
DT Article
ID REGIONAL CLIMATE MODEL; AFRICAN GREAT-LAKES; EAST-AFRICA; PRECIPITATION
EXTREMES; RESOLUTION MODEL; TEMPERATURE; IMPACT; BASIN;
PARAMETERIZATION; SIMULATIONS
AB Weather extremes have harmful impacts on communities around Lake Victoria, where thousands of fishermen die every year because of intense night-time thunderstorms. Yet how these thunderstorms will evolve in a future warmer climate is still unknown. Here we show that Lake Victoria is projected to be a hotspot of future extreme precipitation intensification by using new satellite-based observations, a high-resolution climate projection for the African Great Lakes and coarser-scale ensemble projections. Land precipitation on the previous day exerts a control on night-time occurrence of extremes on the lake by enhancing atmospheric convergence (74%) and moisture availability (26%). The future increase in extremes over Lake Victoria is about twice as large relative to surrounding land under a high-emission scenario, as only over-lake moisture advection is high enough to sustain Clausius-Clapeyron scaling. Our results highlight a major hazard associated with climate change over East Africa and underline the need for high-resolution projections to assess local climate change.
C1 [Thiery, Wim; Lhermitte, Stef; van Lipzig, Nicole P. M.] Katholieke Univ Leuven, Dept Earth & Environm Sci, Celestijnenlaan 200E, B-3001 Leuven, Belgium.
[Thiery, Wim; Davin, Edouard L.; Seneviratne, Sonia I.] ETH, Inst Atmospher & Climate Sci, Univ Str 16, CH-8092 Zurich, Switzerland.
[Bedka, Kristopher] NASA, Langley Res Ctr, Sci Directorate, 21 Langley Blvd, Hampton, VA 23681 USA.
[Lhermitte, Stef] Delft Univ Technol, Dept Geosci & Remote Sensing, Stevinweg 1, NL-2600 GA Delft, Netherlands.
RP Thiery, W (reprint author), Katholieke Univ Leuven, Dept Earth & Environm Sci, Celestijnenlaan 200E, B-3001 Leuven, Belgium.; Thiery, W (reprint author), ETH, Inst Atmospher & Climate Sci, Univ Str 16, CH-8092 Zurich, Switzerland.
EM wim.thiery@env.ethz.ch
RI Davin, Edouard/L-7033-2016
OI Davin, Edouard/0000-0003-3322-9330
FU Research Foundation Flanders (FWO); ETH Zurich [Fel-45 15-1]; FWO;
Belgian Science Policy Office (BELSPO) [CD/AR/02A]; Hercules Foundation;
Flemish Government-department EWI
FX We acknowledge the CLM community (http://www.clm-community.eu) for
developing COSMO-CLM2 and making the model code available,
and Hans-Jurgen Panitz for providing the lateral boundary conditions. In
addition, we are grateful to the World Climate Research Programme (WRCP)
for initiating and coordinating the CORDEX-Africa initiative, to the
modelling centres for making their downscaling results publicly
available through ESGF, to ECMWF for providing access to ERA-Interim,
and to NASA and JAXA for developing the TRMM-3B42 data set. We
particularly thank Fabien Chatterjee, Matthias Demuzere, David Docquier,
Niels Souverijns and Kristof Van Tricht for their useful suggestions.
W.T. was supported by a PhD fellowship from the Research Foundation
Flanders (FWO) and an ETH Zurich postdoctoral fellowship (Fel-45 15-1).
S.L. was supported by an FWO postdoctoral fellowship. The Belgian
Science Policy Office (BELSPO) is acknowledged for the support through
the research project EAGLES (CD/AR/02A). Computational resources and
services used for the COSMO-CLM2 simulation were provided by
the VSC (Flemish Supercomputer Center), funded by the Hercules
Foundation and the Flemish Government-department EWI.
NR 52
TC 4
Z9 4
U1 8
U2 8
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 SEP
PY 2016
VL 7
AR 12786
DI 10.1038/ncomms12786
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DY6RU
UT WOS:000385256500016
PM 27658848
ER
PT J
AU Donnelly, M
AF Donnelly, Michael
TI You can't sit in an office and issue edicts via email. You need to go
where the work is being performed
SO AEROSPACE AMERICA
LA English
DT Editorial Material
C1 [Donnelly, Michael] NASA, OSIRIS REx, Washington, DC 20546 USA.
RP Donnelly, M (reprint author), NASA, OSIRIS REx, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 1
U2 1
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0740-722X
J9 AEROSPACE AM
JI Aerosp. Am.
PD SEP
PY 2016
VL 54
IS 8
BP 64
EP 64
PG 1
WC Engineering, Aerospace
SC Engineering
GA DX9TN
UT WOS:000384738200015
ER
PT J
AU Han, JW
Wong, HY
Moon, DI
Braga, N
Meyyappan, M
AF Han, Jin-Woo
Wong, Hiu Yung
Moon, Dong-Il
Braga, Nelson
Meyyappan, M.
TI Stringer Gate FinFET on Bulk Substrate
SO IEEE TRANSACTIONS ON ELECTRON DEVICES
LA English
DT Article
DE FinFET; low standby power; steep retrograde well; stringer gate; sub-fin
leakage
ID SUBTHRESHOLD LOGIC; DEVICE DESIGN; SOI MOSFETS; OPTIMIZATION;
TRANSISTORS; OPERATION; MOBILITY
AB A gate stringer normally considered parasitic is used as a subthreshold leakage suppressor in a bulk FinFET. The gate stringer remaining along the source/drain extension suppresses the formation of a sub-fin leakage path and improves the subthreshold slope. The stringer gate structure is implemented by simple process modification in the gate etch step while the other process steps are unchanged. The fabricated stringer gate FinFET shows 35% reduction in the OFF-state leakage current compared with a conventional FinFET without a retrograde well process at the expense of only 5% increase in parasitic capacitance. The power-delay product enhancement at reduced drive voltage characteristics exhibits that the stringer gate FinFET can be an attractive candidate for low standby power and subthreshold logic applications.
C1 [Han, Jin-Woo; Moon, Dong-Il; Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Wong, Hiu Yung; Braga, Nelson] Synopsys Inc, Mountain View, CA 94043 USA.
RP Han, JW (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM jin-woo.han@nasa.gov; hywong@synopsys.com; dong-il.moon@nasa.gov;
nelson.braga@synopsys.com; m.meyyappan@nasa.gov
NR 27
TC 0
Z9 0
U1 3
U2 3
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9383
EI 1557-9646
J9 IEEE T ELECTRON DEV
JI IEEE Trans. Electron Devices
PD SEP
PY 2016
VL 63
IS 9
BP 3432
EP 3438
DI 10.1109/TED.2016.2586607
PG 7
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA DX7NK
UT WOS:000384574400009
ER
PT J
AU Singh, D
Swain, DL
Mankin, JS
Horton, DE
Thomas, LN
Rajaratnam, B
Diffenbaugh, NS
AF Singh, Deepti
Swain, Daniel L.
Mankin, Justin S.
Horton, Daniel E.
Thomas, Leif N.
Rajaratnam, Bala
Diffenbaugh, Noah S.
TI Recent amplification of the North American winter temperature dipole
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE climate change detection; climate change impacts; extreme event
attribution; atmospheric dynamics
ID ARCTIC SEA-ICE; ATMOSPHERIC CIRCULATION; INTERNAL VARIABILITY;
CALIFORNIA DROUGHT; CLIMATE; TRENDS; SNOW; PATTERNS; EXTREMES; WEATHER
AB During the winters of 2013-2014 and 2014-2015, anomalously warm temperatures in western North America and anomalously cool temperatures in eastern North America resulted in substantial human and environmental impacts. Motivated by the impacts of these concurrent temperature extremes and the intrinsic atmospheric linkage between weather conditions in the western and eastern United States, we investigate the occurrence of concurrent warm-West/cool-East surface temperature anomalies, which we call the North American winter temperature dipole. We find that, historically, warm-West/cool-East dipole conditions have been associated with anomalous mid-tropospheric ridging over western North America and downstream troughing over eastern North America. We also find that the occurrence and severity of warm-West/cool-East events have increased significantly between 1980 and 2015, driven largely by an increase in the frequency with which high-amplitude ridge-trough wave patterns result in simultaneous severe temperature conditions in both the West and East. Using a large single-model ensemble of climate simulations, we show that the observed positive trend in the warm-West/cool-East events is attributable to historical anthropogenic emissions including greenhouse gases, but that the co-occurrence of extreme western warmth and eastern cold will likely decrease in the future as winter temperatures warm dramatically across the continent, thereby reducing the occurrence of severely cold conditions in the East. Although our analysis is focused on one particular region, our analysis framework is generally transferable to the physical conditions shaping different types of extreme events around the globe.
C1 [Singh, Deepti; Swain, Daniel L.; Horton, Daniel E.; Thomas, Leif N.; Rajaratnam, Bala; Diffenbaugh, Noah S.] Stanford Univ, Dept Earth Syst Sci, Stanford, CA 94305 USA.
[Singh, Deepti; Mankin, Justin S.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
[Mankin, Justin S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Horton, Daniel E.] Northwestern Univ, Dept Earth & Planetary Sci, Evanston, IL USA.
[Horton, Daniel E.; Diffenbaugh, Noah S.] Stanford Univ, Woods Inst Environm, Stanford, CA 94305 USA.
[Rajaratnam, Bala] Stanford Univ, Dept Stat, Stanford, CA 94305 USA.
RP Singh, D (reprint author), Stanford Univ, Dept Earth Syst Sci, Stanford, CA 94305 USA.; Singh, D (reprint author), Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
EM dsingh@ldeo.columbia.edu
OI Swain, Daniel/0000-0003-4276-3092
FU Lamont Doherty Postdoctoral Fellowship; Switzer Foundation; ARCS
Foundation; Earth Institute Postdoctoral Fellowship; US National Science
Foundation [DMS-CMG 1025465, AGS-1003823, DMS-1106642,
DMS-CAREER-1352656]; U.S. Air Force Office of Scientific Research
[FA9550-13-1-0043]; NSF AGS CAREER [0955283]; DOE Integrated Assessment
Research Program [DE-SC005171]
FX We thank the National Oceanic and Atmospheric Administration's NCDC for
access to historical temperature and geopotential height data sets,
PRISM Climate Group and University of Idaho for access to historical
temperature data sets, and NCAR for access to the CESM LENS simulations.
We also thank Nathaniel Johnson for providing us the Self-Organizing
Maps algorithm. Our work is supported by the Lamont Doherty Postdoctoral
Fellowship to D.S.; graduate fellowships from the Switzer Foundation and
the ARCS Foundation to D.L.S.; Earth Institute Postdoctoral Fellowship
to J.S.M.; US National Science Foundation grants DMS-CMG 1025465,
AGS-1003823, DMS-1106642, and DMS-CAREER-1352656; and U.S. Air Force
Office of Scientific Research grant award FA9550-13-1-0043 to B.R.; and
NSF AGS CAREER grant 0955283 and DOE Integrated Assessment Research
Program grant DE-SC005171 to N.S.D. Gridded 2 m temperatures,
geopotential heights, meridional winds, and omega from the NCEP R1 and 2
m temperatures from the NCEP North American Regional Reanalysis (NARR)
are available at the NOAA ESRL website
(http://www.esrl.noaa.gov/psd/data/gridded/). Gridded temperatures from
PRISM Climate Group and University of Idaho Metdata data sets are
available at their respective websites
(http://www.prism.oregonstate.edu/ and
http://metdata.northwestknowledge.net/). All analysis scripts used in
this study can be obtained by contacting Deepti Singh
(dsingh@ldeo.columbia.edu).
NR 56
TC 3
Z9 3
U1 10
U2 10
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 SEP
PY 2016
VL 121
IS 17
BP 9911
EP 9928
DI 10.1002/2016JD025116
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DY0YV
UT WOS:000384823000024
PM 27840780
ER
PT J
AU Payne, RC
Britt, AV
Chen, H
Kasting, JF
Catling, DC
AF Payne, Rebecca C.
Britt, Amber V.
Chen, Howard
Kasting, James F.
Catling, David C.
TI The response of Phanerozoic surface temperature to variations in
atmospheric oxygen concentration
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE atmospheric O-2 levels; surface temperature; Phanerozoic climate;
Cenomanian climate
ID MODEL; EVOLUTION; RECORD; EARTH; TIME; O-2; CO2
AB Recently, Poulsen et al. (2015) suggested that O-2 has played a major role in climate forcing during the Phanerozoic. Specifically, they argued that decreased O-2 levels during the Cenomanian stage of the middle Cretaceous (94-100Ma) could help explain the extremely warm climate during that time. The postulated warming mechanism involves decreased Rayleigh scattering by a thinner atmosphere, which reduces the planetary albedo and allows greater surface warming. This warming effect is then amplified by cloud feedbacks within their 3-D climate model. This increase in shortwave surface forcing, in their calculations, exceeds any decrease in the greenhouse effect caused by decreased O-2. Here we use a 1-D radiative-convective climate model (with no cloud feedback) to check their results. We also include a self-consistent calculation of the change in atmospheric ozone and its effect on climate. Our results are opposite to those of Poulsen et al.: we find that the climate warms by 1.4K at 35% O-2 concentrations as a result of increased pressure broadening of CO2 and H2O absorption lines and cools by 0.8K at 10% O-2 as a result of decreased pressure broadening. The surface temperature changes are only about 1K either way, though, for reasonable variations in Phanerozoic O-2 concentrations (10%-35% by volume). Hence, it seems unlikely that changes in atmospheric O-2 account for the warm climate of the Cenomanian. Other factors, such as a higher-than-expected sensitivity of climate to increased CO2 concentrations, may be required to obtain agreement with the paleoclimate data.
C1 [Payne, Rebecca C.; Britt, Amber V.; Kasting, James F.] Penn State Univ, Dept Geosci, State Coll, PA 16801 USA.
[Chen, Howard] Northwestern Univ, Dept Earth & Planetary Sci, Evanston, IL USA.
[Kasting, James F.] Penn State Astrobiol Res Ctr, University Pk, PA USA.
[Kasting, James F.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Kasting, James F.; Catling, David C.] NASA, Astrobiol Inst, Virtual Planetary Lab, Seattle, WA USA.
[Catling, David C.] Univ Washington, Dept Earth & Space Sci, Seattle, WA USA.
RP Payne, RC (reprint author), Penn State Univ, Dept Geosci, State Coll, PA 16801 USA.
EM rvp5143@psu.edu
FU Undergraduate Research Opportunities Program (UROP) at Boston
University; NASA's Exobiology and Astrobiology programs
FX We are grateful to Jing-Jun Liu for his help with the photochemical
analysis. H. C. thanks the Undergraduate Research Opportunities Program
(UROP) at Boston University for primarily funding the research while in
residence at Penn State University in State College in the summer of
2015. J.F.K. acknowledge financial support from NASA's Exobiology and
Astrobiology programs. Data can be obtained from R.C. Payne
(rvp5143@psu.edu).
NR 18
TC 0
Z9 0
U1 5
U2 5
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 SEP
PY 2016
VL 121
IS 17
BP 10089
EP 10096
DI 10.1002/2016JD025459
PG 8
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DY0YV
UT WOS:000384823000022
ER
PT J
AU Dong, XQ
Xi, BK
Qiu, SY
Minnis, P
Sun-Mack, S
Rose, F
AF Dong, Xiquan
Xi, Baike
Qiu, Shaoyue
Minnis, Patrick
Sun-Mack, Sunny
Rose, Fred
TI A radiation closure study of Arctic stratus cloud microphysical
properties using the collocated satellite-surface data and Fu-Liou
radiative transfer model
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE Arctic stratus cloud properties; radiation closure study; surface remote
sensing; satellite remote sensing
ID ANGULAR-DISTRIBUTION MODELS; GROUND-BASED MEASUREMENTS; ENERGY SYSTEM
INSTRUMENT; STRATIFORM CLOUDS; FLUX CALCULATION; TERRA SATELLITE; PART
I; CERES; BUDGET; RADAR
AB Retrievals of cloud microphysical properties based on passive satellite imagery are especially difficult over snow-covered surfaces because of the bright and cold surface. To help quantify their uncertainties, single-layered overcast liquid-phase Arctic stratus cloud microphysical properties retrieved by using the Clouds and the Earth's Radiant Energy System Edition 2 and Edition 4 (CERES Ed2 and Ed4) algorithms are compared with ground-based retrievals at the Atmospheric Radiation Measurement North Slope of Alaska (ARM NSA) site at Barrow, AK, during the period from March 2000 to December 2006. A total of 206 and 140 snow-free cases (R(sfc)0.3), and 108 and 106 snow cases (R-sfc>0.3), respectively, were selected from Terra and Aqua satellite passes over the ARM NSA site. The CERES Ed4 and Ed2 optical depth () and liquid water path (LWP) retrievals from both Terra and Aqua are almost identical and have excellent agreement with ARM retrievals under snow-free and snow conditions. In order to reach a radiation closure study for both the surface and top of atmosphere (TOA) radiation budgets, the ARM precision spectral pyranometer-measured surface albedos were adjusted (63.6% and 80% of the ARM surface albedos for snow-free and snow cases, respectively) to account for the water and land components of the domain of 30kmx30km. Most of the radiative transfer model calculated SWsfc and SWTOA fluxes by using ARM and CERES cloud retrievals and the domain mean albedos as input agree with the ARM and CERES flux observations within 10Wm(-2) for both snow-free and snow conditions. Sensitivity studies show that the ARM LWP and r(e) retrievals are less dependent on solar zenith angle (SZA), but all retrieved optical depths increase with SZA.
C1 [Dong, Xiquan; Xi, Baike; Qiu, Shaoyue] Univ North Dakota, Dept Atmospher Sci, Grand Forks, ND 58202 USA.
[Minnis, Patrick] NASA Langley Res Ctr, Hampton, VA USA.
[Sun-Mack, Sunny; Rose, Fred] SSAI Inc, Hampton, VA USA.
RP Dong, XQ (reprint author), Univ North Dakota, Dept Atmospher Sci, Grand Forks, ND 58202 USA.
EM dong@aero.und.edu
FU U.S. Department of Energy (DOE) Office of Energy Research, Office of
Health and Environmental Research, Environmental Sciences Division; NASA
CERES project at the University of North Dakota [NNX14AP84G]; DOE ARM
Program at NASA Langley [DE-SC0013896]
FX The ground-based measurements were obtained from the Atmospheric
Radiation Measurement (ARM) Program sponsored by the U.S. Department of
Energy (DOE) Office of Energy Research, Office of Health and
Environmental Research, Environmental Sciences Division. The data can be
downloaded from http://www.archive.arm.gov/. The satellite data were
obtained from the NASA CERES cloud working group at NASA Langley
Research Center. Special thanks to Seiji Kato for the useful discussion
about NASA Langley Modified Fu-Liou radiative transfer model. This
research was supported by the NASA CERES project under grant NNX14AP84G
at the University of North Dakota and by the DOE ARM Program under
contract DE-SC0013896 at NASA Langley. Dates and times corresponding to
the sample numbers used in several figures are available from the lead
author on request (dong@aero.und.edu).
NR 46
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U1 6
U2 6
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 SEP
PY 2016
VL 121
IS 17
BP 10175
EP 10198
DI 10.1002/2016JD025255
PG 24
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DY0YV
UT WOS:000384823000018
ER
PT J
AU Saide, PE
Thompson, G
Eidhammer, T
da Silva, AM
Pierce, RB
Carmichael, GR
AF Saide, Pablo E.
Thompson, Gregory
Eidhammer, Trude
da Silva, Arlindo M.
Pierce, R. Bradley
Carmichael, Gregory R.
TI Assessment of biomass burning smoke influence on environmental
conditions for multiyear tornado outbreaks by combining aerosol-aware
microphysics and fire emission constraints
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE biomass burning; severe weather; tornadoes; fires;
aerosol-cloud-radiation interactions; WRF
ID MARINE STRATOCUMULUS; SPATIAL-DISTRIBUTION; WEATHER FORECASTS; OPTICAL
DEPTH; WRF-CHEM; MODEL; IMPACTS; CLIMATE; PARAMETERIZATION; ASSIMILATION
AB We use the Weather Research and Forecasting (WRF) system to study the impacts of biomass burning smoke from Central America on several tornado outbreaks occurring in the U.S. during spring. The model is configured with an aerosol-aware microphysics parameterization capable of resolving aerosol-cloud-radiation interactions in a cost-efficient way for numerical weather prediction (NWP) applications. Primary aerosol emissions are included, and smoke emissions are constrained using an inverse modeling technique and satellite-based aerosol optical depth observations. Simulations turning on and off fire emissions reveal smoke presence in all tornado outbreaks being studied and show an increase in aerosol number concentrations due to smoke. However, the likelihood of occurrence and intensification of tornadoes is higher due to smoke only in cases where cloud droplet number concentration in low-level clouds increases considerably in a way that modifies the environmental conditions where the tornadoes are formed (shallower cloud bases and higher low-level wind shear). Smoke absorption and vertical extent also play a role, with smoke absorption at cloud-level tending to burn-off clouds and smoke absorption above clouds resulting in an increased capping inversion. Comparing these and WRF-Chem simulations configured with a more complex representation of aerosol size and composition and different optical properties, microphysics, and activation schemes, we find similarities in terms of the simulated aerosol optical depths and aerosol impacts on near-storm environments. This provides reliability on the aerosol-aware microphysics scheme as a less computationally expensive alternative to WRF-Chem for its use in applications such as NWP and cloud-resolving simulations.
C1 [Saide, Pablo E.] Natl Ctr Atmospher Res, Adv Study Program, POB 3000, Boulder, CO 80307 USA.
[Saide, Pablo E.] Natl Ctr Atmospher Res, Atmospher Chem Observat & Modeling Lab, POB 3000, Boulder, CO 80307 USA.
[Thompson, Gregory; Eidhammer, Trude] Natl Ctr Atmospher Res, Res Applicat Lab, POB 3000, Boulder, CO 80307 USA.
[da Silva, Arlindo M.] NASA, Goddard Space Flight Ctr, Global Modeling & Data Assimilat Off, Greenbelt, MD USA.
[Pierce, R. Bradley] NOAA, Satellite & Informat Serv NESDIS, Ctr Satellite Applicat & Res STAR, Madison, WI USA.
[Carmichael, Gregory R.] Univ Iowa, Ctr Global & Reg Environm Res, Iowa City, IA USA.
RP Saide, PE (reprint author), Natl Ctr Atmospher Res, Adv Study Program, POB 3000, Boulder, CO 80307 USA.; Saide, PE (reprint author), Natl Ctr Atmospher Res, Atmospher Chem Observat & Modeling Lab, POB 3000, Boulder, CO 80307 USA.
EM saide@ucar.edu
RI Pierce, Robert Bradley/F-5609-2010
OI Pierce, Robert Bradley/0000-0002-2767-1643
FU National Science Foundation
FX The National Center for Atmospheric Research is supported by the
National Science Foundation. Contact P.E. Saide (saide@ucar.edu) for
data and code requests. This work was carried out with the aid of NASA
grant NNXAF95G. A.M. da Silva is funded by NASA's Modeling and
Application Program. We acknowledge use of MOZART-4 global model output
available at http://www.acom.ucar.edu/wrf-chem/mozart.shtml. CALIPSO
data were obtained from the NASA Langley Research Center Atmospheric
Science Data Center (https://earthdata.nasa.gov/). The views, opinions,
and findings contained in this report are those of the author(s) and
should not be construed as an official National Oceanic and Atmospheric
Administration or U.S. Government position, policy, or decision.
NR 60
TC 0
Z9 0
U1 15
U2 15
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 SEP
PY 2016
VL 121
IS 17
BP 10294
EP 10311
DI 10.1002/2016JD025056
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DY0YV
UT WOS:000384823000014
ER
PT J
AU Sullivan, JT
Mcgee, TJ
Langford, AO
Alvarez, RJ
Senff, CJ
Reddy, PJ
Thompson, AM
Twigg, LW
Sumnicht, GK
Lee, P
Weinheimer, A
Knote, C
Long, RW
Hoff, RM
AF Sullivan, John T.
McGee, Thomas J.
Langford, Andrew O.
Alvarez, Raul J., II
Senff, Christoph J.
Reddy, Patrick J.
Thompson, Anne M.
Twigg, Laurence W.
Sumnicht, Grant K.
Lee, Pius
Weinheimer, Andrew
Knote, Christoph
Long, Russell W.
Hoff, Raymond M.
TI Quantifying the contribution of thermally driven recirculation to a
high-ozone event along the Colorado Front Range using lidar
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE ozone; air quality; remote sensing; lidar; air quality modeling; TOLNet
ID REGIONAL-SCALE FLOWS; MOUNTAINOUS TERRAIN; BOUNDARY-LAYER
AB A high-ozone (O-3) pollution episode was observed on 22 July 2014 during the concurrent Deriving Information on Surface Conditions from Column and Vertically Resolved Observations Relevant to Air Quality (DISCOVER-AQ) and Front Range Air Pollution and Photochemistry Experiment (FRAPPE) campaigns in northern Colorado. Surface O-3 monitors at three regulatory sites exceeded the Environmental Protection Agency (EPA) 2008 National Ambient Air Quality Standard (NAAQS) daily maximum 8h average (MDA8) of 75ppbv. To further characterize the polluted air mass and assess transport throughout the event, measurements are presented from O-3 and wind profilers, O-3-sondes, aircraft, and surface-monitoring sites. Observations indicate that thermally driven upslope flow was established throughout the Colorado Front Range during the pollution episode. As the thermally driven flow persisted throughout the day, O-3 concentrations increased and affected high-elevation Rocky Mountain sites. These observations, coupled with modeling analyses, demonstrate a westerly return flow of polluted air aloft, indicating that the mountain-plains solenoid circulation was established and impacted surface conditions within the Front Range.
C1 [Sullivan, John T.; McGee, Thomas J.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA.
[Langford, Andrew O.; Alvarez, Raul J., II; Senff, Christoph J.] NOAA, Earth Syst Res Lab, Boulder, CO USA.
[Senff, Christoph J.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Reddy, Patrick J.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA.
[Thompson, Anne M.] NASA, Goddard Space Flight Ctr, Earth Sci Div, Greenbelt, MD USA.
[Twigg, Laurence W.; Sumnicht, Grant K.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Lee, Pius] NOAA, Ctr Weather & Climate Predict, Air Resources Lab, College Pk, MD USA.
[Weinheimer, Andrew] Natl Ctr Atmospher Res, Atmospher Chem Observat & Modeling Lab, POB 3000, Boulder, CO 80307 USA.
[Knote, Christoph] Univ Munich, Meteorol Inst, Munich, Germany.
[Long, Russell W.] US EPA, Off Res & Dev, Res Triangle Pk, NC 27711 USA.
[Hoff, Raymond M.] Joint Ctr Earth Syst Technol, Baltimore, MD USA.
[Hoff, Raymond M.] Univ Maryland, Dept Atmospher Phys, Baltimore, MD 21201 USA.
RP Sullivan, JT (reprint author), NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD 20771 USA.
EM john.t.sullivan@nasa.gov
RI Langford, Andrew/D-2323-2009; Thompson, Anne /C-3649-2014; Manager, CSD
Publications/B-2789-2015
OI Langford, Andrew/0000-0002-2932-7061; Thompson, Anne
/0000-0002-7829-0920;
FU UMBC/JCET [374, 8306]; Maryland Department of the Environment (MDE)
[U00P4400079]; NOAA-CREST CCNY Foundation [49173B-02]; NASA/USRA
Postdoctoral Program at the Goddard Space Flight Center; NASA
DISCOVER-AQ [NNX10AR39G]; Pennsylvania State University; NASA
Tropospheric Chemistry Program; Tropospheric Ozone Lidar Network
(TOLNet)
FX Unless otherwise noted, all data used in this study can be found in the
DISCOVER-AQ data archive
(http://www-air.larc.nasa.gov/missions/discover-aq/), the FRAPPE data
archive (http://catalog.eol.ucar.edu/frappe), or the TOLNet data archive
(http://www-air.larc.nasa.gov/missions/TOLNet/). This work was supported
by UMBC/JCET (task 374, project 8306), the Maryland Department of the
Environment (MDE, contract U00P4400079), and NOAA-CREST CCNY Foundation
(subcontract 49173B-02). This research was supported by an appointment
to the NASA/USRA Postdoctoral Program at the Goddard Space Flight
Center. The Platteville Nittany Atmospheric Trailer and Integrated
Validation Experiment (NATIVE) operations were sponsored by NASA
DISCOVER-AQ grant NNX10AR39G and the Pennsylvania State University. The
authors gratefully acknowledge support provided by the NASA Tropospheric
Chemistry Program and the Tropospheric Ozone Lidar Network (TOLNet).
Thanks to the helpfulness and expertise of Ryan Stauffer, Hannah
Halliday, and Nikolai Balashov, who worked with the NATIVE trailer at
Platteville. Thanks to Debra Wicks Kollonige for providing her insight
and recommendations on this work. Thanks to Kenneth Pickering, Yonhua
Tang, Li Pan, and Barry Baker for their expertise in evaluating and
managing the CMAQ model output. Thanks to Timothy Coleman (NOAA ESRL
PSD) for providing the Greeley wind profiles. Thanks to the NOAA
Physical Science Division for their continued efforts in managing the
instrumentation and site coordination necessary for this work from the
300 m BAO Tower. Finally, thanks to the CDPHE for the continued efforts
to obtain observations at the many remote and urban sites throughout the
region used in this work. The views, opinions, and findings contained in
this report are those of the author(s) and should not be construed as an
official National Oceanic and Atmospheric Administration or U.S.
Government position, policy, or decision.
NR 34
TC 0
Z9 0
U1 8
U2 8
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 SEP
PY 2016
VL 121
IS 17
BP 10377
EP 10390
DI 10.1002/2016JD025229
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DY0YV
UT WOS:000384823000008
ER
PT J
AU Bokhorst, S
Pedersen, SH
Brucker, L
Anisimov, O
Bjerke, JW
Brown, RD
Ehrich, D
Essery, RLH
Heilig, A
Ingvander, S
Johansson, C
Johansson, M
Jonsdottir, IS
Inga, N
Luojus, K
Macelloni, G
Mariash, H
McLennan, D
Rosqvist, GN
Sato, A
Savela, H
Schneebeli, M
Sokolov, A
Sokratov, SA
Terzago, S
Vikhamar-Schuler, D
Williamson, S
Qiu, YB
Callaghan, TV
AF Bokhorst, Stef
Pedersen, Stine Hojlund
Brucker, Ludovic
Anisimov, Oleg
Bjerke, Jarle W.
Brown, Ross D.
Ehrich, Dorothee
Essery, Richard L. H.
Heilig, Achim
Ingvander, Susanne
Johansson, Cecilia
Johansson, Margareta
Jonsdottir, Ingibjorg Svala
Inga, Niila
Luojus, Kari
Macelloni, Giovanni
Mariash, Heather
McLennan, Donald
Rosqvist, Gunhild Ninis
Sato, Atsushi
Savela, Hannele
Schneebeli, Martin
Sokolov, Aleksandr
Sokratov, Sergey A.
Terzago, Silvia
Vikhamar-Schuler, Dagrun
Williamson, Scott
Qiu, Yubao
Callaghan, Terry V.
TI Changing Arctic snow cover: A review of recent developments and
assessment of future needs for observations, modelling, and impacts
SO AMBIO
LA English
DT Review
DE Climate change; Ecosystem services; Human health; Societal costs;
Indigenous; Snow
ID WINTER WARMING EVENTS; MICROWAVE BRIGHTNESS TEMPERATURE; LIGHT-ABSORBING
PARTICLES; GROUND-PENETRATING RADAR; LIQUID WATER-CONTENT; SEA-ICE;
SURFACE-AREA; ALBEDO FEEDBACK; CLIMATE MODELS; INFRARED REFLECTANCE
AB Snow is a critically important and rapidly changing feature of the Arctic. However, snow-cover and snowpack conditions change through time pose challenges for measuring and prediction of snow. Plausible scenarios of how Arctic snow cover will respond to changing Arctic climate are important for impact assessments and adaptation strategies. Although much progress has been made in understanding and predicting snow-cover changes and their multiple consequences, many uncertainties remain. In this paper, we review advances in snow monitoring and modelling, and the impact of snow changes on ecosystems and society in Arctic regions. Interdisciplinary activities are required to resolve the current limitations on measuring and modelling snow characteristics through the cold season and at different spatial scales to assure human well-being, economic stability, and improve the ability to predict manage and adapt to natural hazards in the Arctic region.
C1 [Bokhorst, Stef; Bjerke, Jarle W.] Norwegian Inst Nat Res NINA, FRAM High North Res Ctr Climate & Environm, POB 6606, N-9296 Tromso, Norway.
[Bokhorst, Stef] Vrije Univ Amsterdam, Dept Ecol Sci, De Boelelaan 1085, NL-1081 HV Amsterdam, Netherlands.
[Pedersen, Stine Hojlund] Aarhus Univ, Dept Biosci, Arctic Res Ctr, Frederiksborgvej 399, DK-4000 Roskilde, Denmark.
[Brucker, Ludovic] NASA, GSFC, Cryospher Sci Lab, Code 615, Greenbelt, MD 20771 USA.
[Brucker, Ludovic] Univ Space Res Assoc, Goddard Earth Sci Technol & Res Studies & Invest, Columbia, MD 21044 USA.
[Anisimov, Oleg] State Hydrol Inst Roshydromet, 23 Second Line VO, St Petersburg 199053, Russia.
[Anisimov, Oleg] North East Fed Univ, Int Ctr Sci & Educ Best, Yakutsk, Russia.
[Brown, Ross D.] Environm Canada Ouranos, Div Climate Res, 550 Sherbrooke St West,19th Floor, Montreal, PQ H3A 1B9, Canada.
[Ehrich, Dorothee] Univ Tromso, Dept Arctic & Marine Biol, N-9037 Tromso, Norway.
[Essery, Richard L. H.] Univ Edinburgh, Sch GeoSci, Edinburgh, Midlothian, Scotland.
[Heilig, Achim] Heidelberg Univ, Inst Environm Phys, Neuenheimer Feld 229, D-69120 Heidelberg, Germany.
[Ingvander, Susanne; Rosqvist, Gunhild Ninis] Stockholm Univ, Dept Phys Geog, S-10691 Stockholm, Sweden.
[Johansson, Cecilia] Uppsala Univ, Dept Earth Sci, Villavagen 16, S-75236 Uppsala, Sweden.
[Johansson, Margareta; Callaghan, Terry V.] Lund Univ, Dept Phys Geog & Ecosyst Sci, Solvegatan 12, S-22362 Lund, Sweden.
[Johansson, Margareta] Royal Swedish Acad Sci, POB 50005, S-10405 Stockholm, Sweden.
[Jonsdottir, Ingibjorg Svala] Univ Ctr Svalbard, POB 156, N-9171 Longyearbyen, Norway.
[Jonsdottir, Ingibjorg Svala] Univ Iceland, Fac Life & Environm Sci, Sturlugata 7, IS-101 Reykjavik, Iceland.
[Inga, Niila] Leavas Sami Commun, Box 53, S-98121 Kiruna, Sweden.
[Luojus, Kari] Finnish Meteorol Inst, Arctic Res, POB 503, Helsinki 00101, Finland.
[Macelloni, Giovanni] CNR, IFAC CNR, Inst Appl Phys Nello Carrara, Via Madonna del Piano 10, I-50019 Sesto Fiorentino, FI, Italy.
[Mariash, Heather] Environm Canada, Natl Wildlife Res Ctr, 1125 Colonel By Dr, Ottawa, ON K1A 0H3, Canada.
[McLennan, Donald] CHARS, 360 Albert St,Suite 1710, Ottawa, ON K1R 7X7, Canada.
[Rosqvist, Gunhild Ninis] Univ Bergen, Dept Earth Sci, N-5020 Bergen, Norway.
[Sato, Atsushi] Natl Res Inst Earth Sci & Disaster Prevent, Snow & Ice Res Ctr, 187-16 Suyoshi, Nagaoka, Niigata 9400821, Japan.
[Savela, Hannele] Univ Oulu, Thule Insitute, POB 7300, Oulu 90014, Finland.
[Schneebeli, Martin] WSL Inst Snow & Avalanche Res SLF, Fluelastr 11, CH-7260 Davos, Switzerland.
[Sokolov, Aleksandr] Russian Acad Sci, Arctic Res Stn, Inst Plant & Anim Ecol, Ural Branch, Labytnangi 629400, Russia.
[Sokolov, Aleksandr] State Org Yamal Nenets Autonomous Dist, Sci Ctr Arctic Studies, Salekhard, Russia.
[Sokratov, Sergey A.] Moscow MV Lomonosov State Univ, Arctic Environm Lab, Fac Geog, Leninskie Gory 1, Moscow 119991, Russia.
[Terzago, Silvia] Natl Res Council ISAC CNR, Inst Atmospher Sci & Climate, Corso Fiume 4, I-10133 Turin, Italy.
[Vikhamar-Schuler, Dagrun] Norwegian Meteorol Inst, Div Model & Climate Anal, R&D Dept, Postboks 43, N-0313 Oslo, Norway.
[Williamson, Scott] Univ Alberta, Dept Biol Sci, CW 405,Biol Sci Bldg, Edmonton, AB T6G 2E9, Canada.
[Qiu, Yubao] Chinese Acad Sci, Inst Remote Sensing & Digital Earth, Beijing 100094, Peoples R China.
[Qiu, Yubao] Cold Reg Initiat, Grp Earth Observat, Geneva, Switzerland.
[Callaghan, Terry V.] Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England.
[Callaghan, Terry V.] Natl Res Tomsk Stated Univ, 36 Lenin Ave, Tomsk 634050, Russia.
RP Bokhorst, S (reprint author), Norwegian Inst Nat Res NINA, FRAM High North Res Ctr Climate & Environm, POB 6606, N-9296 Tromso, Norway.
EM stefbokhorst@hotmail.com; shp@bios.au.dk; ludovic.brucker@nasa.gov;
oleg@oa7661.spb.edu; jarle.werner.bjerke@nina.no; ross.brown@ec.gc.ca;
dorothee.ehrich@uit.no; richard.essery@ed.ac.uk; achim.heilig@wsl.ch;
susanne.ingvander@natgeo.su.se; cecilia.johansson@met.uu.se;
margareta.johansson@nateko.lu.se; isj@hi.is; niila@laevas.se;
kari.luojus@fmi.fi; g.macelloni@ifac.cnr.it; heather.mariash@gmail.com;
donald.mclennan@polar.gc.ca; gunhild.rosqvist@natgeo.su.se;
asato@bosai.go.jp; hannele.savela@oulu.fi; martin.schneebeli@wsl.ch;
sokhol@yandex.ru; sokratov@geol.msu.ru; s.terzago@isac.cnr.it;
dagrun@met.no; snw@ualberta.ca; terry_callaghan@btinternet.com
RI Sokratov, Sergey/A-6602-2011; Ehrich, Dorothee/F-6492-2015; Schneebeli,
Martin/B-1063-2008; Brucker, Ludovic/A-8029-2010; Callaghan,
Terens/N-7640-2014;
OI Sokratov, Sergey/0000-0001-9265-2935; Ehrich,
Dorothee/0000-0002-3028-9488; Schneebeli, Martin/0000-0003-2872-4409;
Brucker, Ludovic/0000-0001-7102-8084; Essery,
Richard/0000-0003-1756-9095; Bjerke, Jarle/0000-0003-2721-1492
FU IASC ICARP III Activity grant
FX The writing of this paper was initiated by an IASC ICARP III Activity
grant to TVC enabling a workshop hosted by the European Environment
Agency. The authors acknowledge funding from their respective national
and international funding bodies, which has enabled the contribution of
all authors to this work.
NR 167
TC 5
Z9 5
U1 37
U2 37
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0044-7447
EI 1654-7209
J9 AMBIO
JI Ambio
PD SEP
PY 2016
VL 45
IS 5
BP 516
EP 537
DI 10.1007/s13280-016-0770-0
PG 22
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA DT6GD
UT WOS:000381580800002
PM 26984258
ER
PT J
AU McIntire, J
Moyer, D
Brown, SW
Lykke, KR
Waluschka, E
Oudrari, H
Xiong, XX
AF McIntire, Jeff
Moyer, David
Brown, Steven W.
Lykke, Keith R.
Waluschka, Eugene
Oudrari, Hassan
Xiong, Xiaoxiong
TI Monochromatic measurements of the JPSS-1 VIIRS polarization sensitivity
SO APPLIED OPTICS
LA English
DT Article
ID PERFORMANCE; CALIBRATION; SATELLITE; MODIS
AB Polarization sensitivity is a critical property that must be characterized for spaceborne remote sensing instruments designed to measure reflected solar radiation. Broadband testing of the first Joint Polar-orbiting Satellite System (JPSS-1) Visible Infrared Imaging Radiometer Suite (VIIRS) showed unexpectedly large polarization sensitivities for the bluest bands on VIIRS (centered between 400 and 600 nm). Subsequent ray trace modeling indicated that large diattenuation on the edges of the bandpass for these spectral bands was the driver behind these large sensitivities. Additional testing using the National Institute of Standards and Technology's Traveling Spectral Irradiance and Radiance Responsivity Calibrations Using Uniform Sources was added to the test program to verify and enhance the model. The testing was limited in scope to two spectral bands at two scan angles; nonetheless, this additional testing provided valuable insight into the polarization sensitivity. Analysis has shown that the derived diattenuation agreed with the broadband measurements to within an absolute difference of about 0.4% and that the ray trace model reproduced the general features of the measured data. Additionally, by deriving the spectral responsivity, the linear diattenuation is shown to be explicitly dependent on the changes in bandwidth with polarization state. (C) 2016 Optical Society of America
C1 [McIntire, Jeff; Oudrari, Hassan] Sci Syst Applicat Int, Lanham, MD 20706 USA.
[Moyer, David] Aerosp Corp, El Segundo, CA 90245 USA.
[Brown, Steven W.; Lykke, Keith R.] NIST, Gaithersburg, MD 20899 USA.
[Waluschka, Eugene; Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP McIntire, J (reprint author), Sci Syst Applicat Int, Lanham, MD 20706 USA.
EM jeffrey.mcintire@ssaihq.com
NR 16
TC 0
Z9 0
U1 5
U2 5
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 SEP
PY 2016
VL 55
IS 27
BP 7444
EP 7454
DI 10.1364/AO.55.007444
PG 11
WC Optics
SC Optics
GA DW9QO
UT WOS:000383996900001
PM 27661568
ER
PT J
AU Sun, JQ
Xiong, XX
Waluschka, E
Wang, MH
AF Sun, Junqiang
Xiong, Xiaoxiong
Waluschka, Eugene
Wang, Menghua
TI Suomi National Polar-Orbiting Partnership Visible Infrared Imaging
Radiometer Suite polarization sensitivity analysis
SO APPLIED OPTICS
LA English
DT Article
ID REFLECTIVE SOLAR BANDS; CALIBRATION; SPECTRORADIOMETER; PERFORMANCE;
DIFFUSER
AB The Visible Infrared Imaging Radiometer Suite (VIIRS) is one of five instruments onboard the Suomi National Polar-Orbiting Partnership (SNPP) satellite that launched from Vandenberg Air Force Base, California, on October 28, 2011. It is a whiskbroom radiometer that provides +/- 56.28 degrees scans of the Earth view. It has 22 bands, among which 14 are reflective solar bands (RSBs). The RSBs cover a wavelength range from 410 to 2250 nm. The RSBs of a remote sensor are usually sensitive to the polarization of incident light. For VIIRS, it is specified that the polarization factor should be smaller than 3% for 410 and 862 nm bands and 2.5% for other RSBs for the scan angle within +/- 45 degrees. Several polarization sensitivity tests were performed prelaunch for SNPP VIIRS. The first few tests either had large uncertainty or were less reliable, while the last one was believed to provide the more accurate information about the polarization property of the instrument. In this paper, the measured data in the last polarization sensitivity test are analyzed, and the polarization factors and phase angles are derived from the measurements for all the RSBs. The derived polarization factors and phase angles are band, detector, and scan angle dependent. For near-infrared bands, they also depend on the half-angle mirror side. Nevertheless, the derived polarization factors are all within the specification, although the strong detector dependence of the polarization parameters was not expected. Compared to the Moderate Resolution Imaging Spectroradiometer on both Aqua and Terra satellites, the polarization effect on VIIRS RSB is much smaller. (C) 2016 Optical Society of America
C1 [Sun, Junqiang; Wang, Menghua] NOAA, Natl Environm Satellite Data & Informat Serv, Ctr Satellite Applicat & Res, E RA3,5830 Univ Res Ct, College Pk, MD 20740 USA.
[Sun, Junqiang] Global Sci & Technol, 7855 Walker Dr,Suite 200, Greenbelt, MD 20770 USA.
[Xiong, Xiaoxiong; Waluschka, Eugene] NASA, Sci & Explorat Directorate, GSFC, Greenbelt, MD 20771 USA.
RP Sun, JQ (reprint author), NOAA, Natl Environm Satellite Data & Informat Serv, Ctr Satellite Applicat & Res, E RA3,5830 Univ Res Ct, College Pk, MD 20740 USA.; Sun, JQ (reprint author), Global Sci & Technol, 7855 Walker Dr,Suite 200, Greenbelt, MD 20770 USA.
EM junqiang.sun@noaa.gov
RI Wang, Menghua/F-5631-2010
OI Wang, Menghua/0000-0001-7019-3125
FU National Oceanic and Atmospheric Administration (NOAA) National
Aeronautics and Space Administration (NASA) Joint Polar Satellite System
FX National Oceanic and Atmospheric Administration (NOAA) National
Aeronautics and Space Administration (NASA) Joint Polar Satellite
System.
NR 31
TC 0
Z9 0
U1 5
U2 5
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 SEP
PY 2016
VL 55
IS 27
BP 7645
EP 7658
DI 10.1364/AO.55.007645
PG 14
WC Optics
SC Optics
GA DW9QO
UT WOS:000383996900027
PM 27661594
ER
PT J
AU Guerrero, G
Smolarkiewicz, PK
Dal Pino, EMD
Kosovichev, AG
Mansour, NN
AF Guerrero, G.
Smolarkiewicz, P. K.
de Gouveia Dal Pino, E. M.
Kosovichev, A. G.
Mansour, N. N.
TI UNDERSTANDING SOLAR TORSIONAL OSCILLATIONS FROM GLOBAL DYNAMO MODELS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: interior; Sun: magnetic fields; Sun: rotation
ID CONVECTION-ZONE; MERIDIONAL FLOW; CYCLE VARIATION; ROTATION; INTERIOR;
SURFACE; SUN
AB The phenomenon of solar "torsional oscillations" (TO) represents migratory zonal flows associated with the solar cycle. These flows are observed on the solar surface and, according to helioseismology, extend through the convection zone. We study the origin of the TO using results from a global MHD simulation of the solar interior that reproduces several of the observed characteristics of the mean-flows and magnetic fields. Our results indicate that the magnetic tension (MT) in the tachocline region is a key factor for the periodic changes in the angular momentum transport that causes the TO. The torque induced by the MT at the base of the convection zone is positive at the poles and negative at the equator. A rising MT torque at higher latitudes causes the poles to speed up, whereas a declining negative MT torque at the lower latitudes causes the equator to slow-down. These changes in the zonal flows propagate through the convection zone up to the surface. Additionally, our results suggest that it is the magnetic field at the tachocline that modulates the amplitude of the surface meridional flow rather than the opposite as assumed by flux-transport dynamo models of the solar cycle.
C1 [Guerrero, G.] Univ Fed Minas Gerais, Dept Phys, Av Antonio Carlos 6627, BR-31270901 Belo Horizonte, MG, Brazil.
[Smolarkiewicz, P. K.] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England.
[de Gouveia Dal Pino, E. M.] Univ Sao Paulo, Dept Astron, IAG USP, Rua Matao 1226, BR-05508090 Sao Paulo, SP, Brazil.
[Kosovichev, A. G.] New Jersey Inst Technol, Newark, NJ 07103 USA.
[Mansour, N. N.] NASA, Ames Res Ctr, Mountain View, CA 94040 USA.
RP Guerrero, G (reprint author), Univ Fed Minas Gerais, Dept Phys, Av Antonio Carlos 6627, BR-31270901 Belo Horizonte, MG, Brazil.
EM guerrero@fisica.ufmg.br; smolar@ecmwf.int; dalpino@astro.iag.usp.br;
alexander.g.kosovichev@njit.edu; Nagi.N.Mansour@nasa.gov
FU FAPEMIG [APQ-01168/14]; FAPESP [2013/10559-5, 2009/54006-4]; CNPq
[306598/2009-4]; NASA [NNX09AJ85g, NNX14AB70G]; European Research
Council under the European Union's Seventh Framework Programme (FP7/ERC)
[320375]
FX We thank the anonymous referee for insightful comments that helped to
improve the paper. This work was partly funded by FAPEMIG grant
APQ-01168/14 (GG), FAPESP grant 2013/10559-5 (EMGDP), CNPq grant
306598/2009-4 (EMGDP), and NASA grants NNX09AJ85g and NNX14AB70G. P.K.S.
is supported by funding received from the European Research Council
under the European Union's Seventh Framework Programme (FP7/2012/ERC
grant agreement no. 320375). The simulations were performed in the NASA
cluster Pleiades and the computing facilities of the Laboratory of
Astroinformatics (IAG/USP, NAT/Unicsul) supported by a FAPESP (grant
2009/54006-4).
NR 25
TC 0
Z9 0
U1 4
U2 4
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 SEP 1
PY 2016
VL 828
IS 1
AR L3
DI 10.3847/2041-8205/828/1/L3
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW9MZ
UT WOS:000383985500003
ER
PT J
AU Sterling, AC
Moore, RL
AF Sterling, Alphonse C.
Moore, Ronald L.
TI A MICROFILAMENT-ERUPTION MECHANISM FOR SOLAR SPICULES
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: chromosphere; Sun: filaments, prominences; Sun: flares; Sun:
magnetic fields; Supporting material: animations
ID X-RAY JETS; POLAR CORONAL HOLES; ACTIVE-REGION; II SPICULES; TELESCOPE;
EVOLUTION; HINODE; PARAMETERS; RESOLUTION; NETWORK
AB Recent investigations indicate that solar coronal jets result from eruptions of small-scale chromospheric filaments, called minifilaments; that is, the jets are produced by scaled-down versions of typical-sized filament eruptions. We consider whether solar spicules might in turn be scaled-down versions of coronal jets, being driven by eruptions of microfilaments. Assuming a microfilament' s size is about a spicule' s width (similar to 300 km), the estimated occurrence number plotted against the estimated size of erupting filaments, minifilaments, and microfilaments approximately follows a power-law distribution (based on counts of coronal mass ejections, coronal jets, and spicules), suggesting that many or most spicules could result from microfilament eruptions. Observed spicule-base Ca II brightenings plausibly result from such microfilament eruptions. By analogy with coronal jets, microfilament eruptions might produce spicules with many of their observed characteristics, including smooth rise profiles, twisting motions, and EUV counterparts. The postulated microfilament eruptions are presumably eruptions of twisted-core micro-magnetic bipoles that are similar to 1 ''.0 wide. These explosive bipoles might be built and destabilized by merging and cancelation of approximately a few to 100 G magnetic-flux elements of size less than or similar to 0 ''.5-1 ''.0. If, however, spicules are relatively more numerous than indicated by our extrapolated distribution, then only a fraction of spicules might result from this proposed mechanism.
C1 [Sterling, Alphonse C.; Moore, Ronald L.] Marshall Space Flight Ctr, Heliophys & Planetary Sci Off, ZP13, Huntsville, AL 35812 USA.
[Moore, Ronald L.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA.
RP Sterling, AC (reprint author), Marshall Space Flight Ctr, Heliophys & Planetary Sci Off, ZP13, Huntsville, AL 35812 USA.
EM alphonse.sterling@nasa.gov; ron.moore@nasa.gov
FU Heliophysics Division of NASA's Science Mission Directorate through the
Heliophysics Guest Investigator (HGI) Program; Hinode Project
FX The authors thank two referees for useful comments and interesting
discussions. This work was supported by funding from the Heliophysics
Division of NASA's Science Mission Directorate through the Heliophysics
Guest Investigator (HGI) Program, and the Hinode Project. We thank T.
Tarbell for assistance with SOT images. Hinode is a Japanese mission
developed and launched by ISAS/JAXA, with NAOJ as domestic partner and
NASA and STFC (UK) as international partners, and operated by these
agencies in co-operation with ESA and NSC (Norway). Figure 1 and Figures
3(g)-(i) and animations, adapted by permission from Macmillan Publishers
Ltd: Nature, Sterling et al. (2015), copyright 2015.
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 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 1
PY 2016
VL 828
IS 1
AR L9
DI 10.3847/2041-8205/828/1/L9
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW9MZ
UT WOS:000383985500009
ER
PT J
AU Wernet, MP
AF Wernet, Mark P.
TI Application of Tomo-PIV in a large-scale supersonic jet flow facility
SO EXPERIMENTS IN FLUIDS
LA English
DT Article
ID PARTICLE IMAGE VELOCIMETRY
AB Particle imaging velocimetry (PIV) has been used extensively at NASA GRC over the last 15 years to build a benchmark data set of hot and cold jet flow measurements in an effort to understand acoustic noise sources in high-speed jets. Identifying the noise sources in highspeed jets is critical for ultimately modifying the nozzle hardware design/operation and therefore reducing the jet noise. Tomographic PIV (Tomo-PIV) is an innovative approach for acquiring and extracting velocity information across extended volumes of a flow field, enabling the computation of additional fluid mechanical properties not typically available using traditional PIV techniques. The objective of this work was to develop and implement the Tomo-PIV measurement capability and apply it in a large-scale outdoor test facility, where seeding multiple flow streams and operating in the presence of daylight presents formidable challenges. The newly developed Tomo-PIV measurement capability was applied in both a subsonic M 0.9 flow and an under-expanded M 1.4 heated jet flow field. Measurements were also obtained using traditional two-component (2C) PIV and stereo PIV in the M 0.9 flow field for comparison and validation of the Tomo-PIV results. In the case of the M 1.4 flow, only the 2C PIV was applied to allow a comparison with the Tomo-PIV measurement. The Tomo-PIV fields-of-view covered 180 x 180 x 10 mm, and the reconstruction domains were 3500 x 3500 x 200 voxels. These Tomo-PIV measurements yielded all three components of vorticity across entire planes for the first time in heated supersonic jet flows and provided the first full 3D reconstruction of the Mach disk and oblique shock intersections inside of the barrel shocks. Measuring all three components of vorticity across multiple planes in the flow, potentially reduces the number of measurement configurations (streamwise and cross-stream PIV) required to fully characterize the mixing-enhanced nozzle flows routinely studied in aeroacoustics research.
C1 [Wernet, Mark P.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Wernet, MP (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM mark.p.wernet@nasa.gov
FU NASA's Fundamental Aeronautics' Transformational Tools and Technologies
Program
FX The author would like to thank NASA's Fundamental Aeronautics'
Transformational Tools and Technologies Program for their support of
this effort. The author also thanks Dr. Randy Locke, Dr. Adam Wroblewski
and Garrett Clayo for their efforts in the setting up and implementation
of the 2C PIV, SPIV and Tomo-PIV systems. The author thanks Dr. James
Bridges for helpful discussions and for the use of the SHJAR facility.
Lastly, the author thanks the staff at the AAPL for their dedication and
support in making these tests possible.
NR 33
TC 0
Z9 0
U1 5
U2 5
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 SEP
PY 2016
VL 57
IS 9
AR 144
DI 10.1007/s00348-016-2228-3
PG 24
WC Engineering, Mechanical; Mechanics
SC Engineering; Mechanics
GA DX2QM
UT WOS:000384215700007
ER
PT J
AU Tang, A
Kim, Y
Xu, Y
Chang, MCF
AF Tang, Adrian
Kim, Yanghyo
Xu, Yinuo
Chang, Mau-Chung Frank
TI A 5.8 GHz 54 Mb/s Backscatter Modulator for WLAN With Symbol
Pre-Distortion and Transmit Pulse Shaping
SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS
LA English
DT Article
DE CMOS backscatter link; pre-distortion; pulse shaping; reflector link
AB This letter discusses the implementation of microwave backscatter links in CMOS technology which are similar to existing systems at mid-UHF for RFID, but intended for use at the 5.8 GHz ISM band for supporting future low-power WLAN applications. In order for backscatter links to operate in highly channelized environments we introduce a pulse-shaping technique to reduce out-of-band emissions as well as a symbol pre-distortion technique to improve the constellation spacing. Both techniques are introduced into a 65 nm prototype backscatter modulator chip and are shown to operate with QPSK modulation at 54 Mb/s (typical of WLAN standards). The backscatter modulator chip was shown to consume 1.61 mW of power.
C1 [Tang, Adrian; Kim, Yanghyo; Xu, Yinuo; Chang, Mau-Chung Frank] Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90025 USA.
[Tang, Adrian] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Tang, A (reprint author), Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90025 USA.
EM atang@seas.ucla.edu; yanghyokim@ucla.edu; yinuo@ucla.edu;
mfchang@ee.ucla.edu
NR 4
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 1531-1309
EI 1558-1764
J9 IEEE MICROW WIREL CO
JI IEEE Microw. Wirel. Compon. Lett.
PD SEP
PY 2016
VL 26
IS 9
BP 729
EP 731
DI 10.1109/LMWC.2016.2597173
PG 3
WC Engineering, Electrical & Electronic
SC Engineering
GA DX0PV
UT WOS:000384067100029
ER
PT J
AU Lall, P
Mirza, KM
Harsha, M
Goebel, K
AF Lall, Pradeep
Mirza, Kazi Mahmud
Harsha, Mahendra
Goebel, Kai
TI Microstructural Indicators for Assessment of Effect of Prolonged and
Intermittent Storage on Reliability of Lead-free Electronics
SO IEEE TRANSACTIONS ON DEVICE AND MATERIALS RELIABILITY
LA English
DT Article
DE Materials reliability; integrated circuit reliability; soldering;
integrated circuit interconnections
ID BOUNDARY-SCAN; TESTABILITY; DESIGN; BIST; BIT
AB Electronic systems may be subjected to prolonged and intermittent periods of storage prior to deployment or usage. Prior studies have shown that the lead-free solder interconnects show measurable degradation in the mechanical properties even after the brief exposures to high temperature. In this paper, a method has been developed for determining the equivalent storage time to produce identical damage at a different temperature. Electronics subjected to accelerated tests often have a well-defined thermal profile for a specified period of time. Quantification of the thermal profile in field-deployed electronics may be often difficult because of the variance in the environment conditions and usage profile. There is a need for tools and techniques to quantify the damage in deployed systems in the absence of macroindicators of damage without the knowledge of prior stress history. The approach for mapping damage in the lead-free second-level interconnects between different thermal conditions is new. High-reliability applications, such as avionics and missile systems, may be often exposed to long periods of storage prior to deployment. The effect of storage at different temperature conditions can be mapped using the presented approach. A framework has been developed to investigate the system state and estimate the remaining useful life of the solder ball subjected to a variety of isothermal aging conditions, including 60 degrees C, 75 degrees C, and 125 degrees C for periods of time between 1 and 4 weeks. Data on damage precursors, including the rate of change in the normalized phase growth and the normalized IMC thickness, has been collected and analyzed to derive physics-based damage mapping relationships for aging. Mathematical relationships have been derived for the damage mapping to various thermal storage environments to facilitate determining an appropriate time-temperature combination to reach a particular level of damage state. Activation energy for the leading indicators of failure is also computed. Specific damage proxies examined include the phase-growth indicator and the intermetallic thickness. The viability of the approach has been demonstrated for the lead-free test assemblies subjected to multiple thermal aging at 60 degrees C, 75 degrees C, and 125 degrees C. Damage mapping relationships are derived from the data based on the two separate leading indicators.
C1 [Lall, Pradeep; Mirza, Kazi Mahmud; Harsha, Mahendra] Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA.
[Harsha, Mahendra] Skyworks Solut Inc, Woburn, MA 01801 USA.
[Goebel, Kai] NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
RP Lall, P (reprint author), Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA.
EM lall@auburn.edu; kmm0039@tigermail.auburn.edu;
mahendra.harsha@skyworksinc.com; kai.f.goebel@nasa.gov
OI Lall, Pradeep/0000-0002-4074-937X
NR 27
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 1530-4388
EI 1558-2574
J9 IEEE T DEVICE MAT RE
JI IEEE Trans. Device Mater. Reliab.
PD SEP
PY 2016
VL 16
IS 3
BP 304
EP 317
DI 10.1109/TDMR.2016.2597740
PG 14
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA DX0QP
UT WOS:000384069500005
ER
PT J
AU Thipphavong, DP
AF Thipphavong, David P.
TI Top-of-Climb Matching Method for Reducing Aircraft Trajectory Prediction
Errors
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT AIAA Guidance, Navigation, and Control (GNC) Conference / AIAA Infotech
at Aerospace Conference
CY AUG 19-22, 2013
CL Boston, MA
SP AIAA
AB The inaccuracies of the aircraft performance models used by trajectory predictors with regard to takeoff weight, thrust, climb profile, and other parameters result in altitude errors during the climb phase that often exceed the vertical separation standard of 1000 ft. This study investigates the potential reduction in altitude trajectory prediction errors that could be achieved for climbing flights if just one additional parameter is made available: top-of-climb time. The top-of-climb matching method developed and evaluated in this paper is straightforward: A set of candidate trajectory predictions is generated using different aircraft weight parameters, and the one that most closely matches top of climb in terms of time is selected. This algorithm was tested using more than 1000 climbing flights in Fort Worth Center. Compared with the baseline trajectory predictions of a real-time research prototype (Center/Terminal Radar Approach Control Automation System), the top-of-climb matching method reduced the altitude root mean square error for a 5min prediction time by 38%. It also decreased the percentage of flights with absolute altitude error greater than the vertical separation standard of 1000ft for the same look-ahead time from 55 to 30%.
C1 [Thipphavong, David P.] NASA, Ames Res Ctr, Flight Trajectory Dynam & Controls Branch, Mail Stop 210-10, Moffett Field, CA 94035 USA.
[Thipphavong, David P.] AIAA, Reston, VA 20191 USA.
RP Thipphavong, DP (reprint author), NASA, Ames Res Ctr, Flight Trajectory Dynam & Controls Branch, Mail Stop 210-10, Moffett Field, CA 94035 USA.; Thipphavong, DP (reprint author), AIAA, Reston, VA 20191 USA.
NR 10
TC 0
Z9 0
U1 1
U2 1
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 SEP-OCT
PY 2016
VL 53
IS 5
BP 1211
EP 1223
DI 10.2514/1.C032966
PG 13
WC Engineering, Aerospace
SC Engineering
GA DX3TS
UT WOS:000384297800003
ER
PT J
AU Brandon, JM
Morelli, EA
AF Brandon, Jay M.
Morelli, Eugene A.
TI Real-Time Onboard Global Nonlinear Aerodynamic Modeling from Flight Data
SO JOURNAL OF AIRCRAFT
LA English
DT Article; Proceedings Paper
CT AIAA Atmospheric Flight Mechanics Conference
CY JUN 16-20, 2014
CL Atlanta, GA
SP AIAA
ID IDENTIFICATION
AB Flight test and modeling techniques were developed to accurately identify global nonlinear aerodynamic models onboard an aircraft. The techniques were developed and demonstrated during piloted flight testing of an Aermacchi MB-326M Impala jet aircraft. Advanced piloting techniques and nonlinear modeling techniques based on fuzzy logic and multivariate orthogonal function methods were implemented with efficient onboard calculations and flight operations to achieve real-time maneuver monitoring, near-real-time global nonlinear aerodynamic modeling, and prediction validation testing in flight. Results demonstrated that global nonlinear aerodynamic models for a large portion of the flight envelope were identified rapidly and accurately using piloted flight test maneuvers during a single flight, with the final identified and validated models available before the aircraft landed.
C1 [Brandon, Jay M.] NASA, Langley Res Ctr, Flight Dynam Branch, Mail Stop 308, Hampton, VA 23681 USA.
[Morelli, Eugene A.] NASA, Langley Res Ctr, Dynam Syst & Control Branch, Mail Stop 308, Hampton, VA 23681 USA.
[Brandon, Jay M.; Morelli, Eugene A.] AIAA, Reston, VA 20191 USA.
RP Brandon, JM (reprint author), NASA, Langley Res Ctr, Flight Dynam Branch, Mail Stop 308, Hampton, VA 23681 USA.; Brandon, JM (reprint author), AIAA, Reston, VA 20191 USA.
NR 15
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 SEP-OCT
PY 2016
VL 53
IS 5
BP 1261
EP 1297
DI 10.2514/1.C033133
PG 37
WC Engineering, Aerospace
SC Engineering
GA DX3TS
UT WOS:000384297800007
ER
PT J
AU Su, WH
Swei, SSM
Zhu, GMG
AF Su, Weihua
Swei, Sean Shan-Min
Zhu, Guoming G.
TI Optimum Wing Shape of Highly Flexible Morphing Aircraft for Improved
Flight Performance
SO JOURNAL OF AIRCRAFT
LA English
DT Article
ID NONLINEAR AEROELASTICITY; DESIGN OPTIMIZATION; BODY AIRCRAFT; DYNAMICS;
AIRFOIL
AB In this paper, optimum wing bending and torsion deformations are explored for a mission adaptive, highly flexible morphing aircraft. The complete highly flexible aircraft is modeled using a strain-based geometrically nonlinear beam formulation, coupled with unsteady aerodynamics and six-degree-of-freedom rigid-body motions. Since there are no conventional discrete control surfaces for trimming the flexible aircraft, the design space for searching the optimum wing geometries is enlarged. To achieve high-performance flight, the wing geometry is best tailored according to the specific flight mission needs. In this study, the steady level flight and the coordinated turn flight are considered, and the optimum wing deformations with the minimum drag at these flight conditions are searched by using a modal-based optimization procedure, subject to the trim and other constraints. The numerical study verifies the feasibility of the modal-based optimization approach, and it shows the resulting optimum wing configuration and its sensitivity under different flight profiles.
C1 [Su, Weihua] Univ Alabama, Dept Aerosp Engn & Mech, Tuscaloosa, AL 35487 USA.
[Swei, Sean Shan-Min] NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA.
[Zhu, Guoming G.] Michigan State Univ, Dept Mech Engn, E Lansing, MI 48824 USA.
[Su, Weihua; Swei, Sean Shan-Min] AIAA, Reston, VA 20191 USA.
RP Su, WH (reprint author), Univ Alabama, Dept Aerosp Engn & Mech, Tuscaloosa, AL 35487 USA.; Su, WH (reprint author), AIAA, Reston, VA 20191 USA.
EM suw@eng.ua.edu; sean.s.swei@nasa.gov; zhug@egr.msu.edu
RI Su, Weihua/F-1561-2011
OI Su, Weihua/0000-0002-4458-0524
FU NASA Ames Research Center's Summer Faculty Fellowship; NASA Aeronautics
Research Mission Directorate's Team Seedling Fund; Convergent
Aeronautics Solutions project
FX The first author acknowledges sponsorship from the NASA Ames Research
Center's Summer Faculty Fellowship. The work was partially supported by
the NASA Aeronautics Research Mission Directorate's Team Seedling Fund
and the Convergent Aeronautics Solutions project.
NR 29
TC 0
Z9 0
U1 11
U2 11
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 SEP-OCT
PY 2016
VL 53
IS 5
BP 1305
EP 1316
DI 10.2514/1.C033490
PG 12
WC Engineering, Aerospace
SC Engineering
GA DX3TS
UT WOS:000384297800009
ER
PT J
AU Perry, B
AF Perry, Boyd, III
TI Results of National Advisory Committee for Aeronautics Report Number
496: Revisited
SO JOURNAL OF AIRCRAFT
LA English
DT Article
C1 [Perry, Boyd, III] NASA Langley Res Ctr, Aeroelast Branch, Hampton, VA 23681 USA.
RP Perry, B (reprint author), NASA Langley Res Ctr, Aeroelast Branch, Hampton, VA 23681 USA.
NR 7
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 SEP-OCT
PY 2016
VL 53
IS 5
BP 1561
EP +
DI 10.2514/1.C033663
PG 4
WC Engineering, Aerospace
SC Engineering
GA DX3TS
UT WOS:000384297800030
ER
PT J
AU Liao, L
Meneghini, R
Tokay, A
Bliven, LF
AF Liao, Liang
Meneghini, Robert
Tokay, Ali
Bliven, Larry F.
TI Retrieval of Snow Properties for Ku- and Ka-Band Dual-Frequency Radar
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID SINGLE-SCATTERING PROPERTIES; ICE PARTICLES; FALL SPEED; SIZE;
HYDROMETEORS; PARAMETERS; APPROXIMATION; DISDROMETER; CRYSTALS; DATABASE
AB The focus of this study is on the estimation of snow microphysical properties and the associated bulk parameters such as snow water content and water equivalent snowfall rate for Ku- and Ka-band dual-frequency radar. This is done by exploring a suitable scattering model and the proper particle size distribution (PSD) assumption that accurately represent, in the electromagnetic domain, the micro-/macrophysical properties of snow. The scattering databases computed from simulated aggregates for small-to-moderate particle sizes are combined with a simple scattering model for large particle sizes to characterize snow-scattering properties over the full range of particle sizes. With use of the single-scattering results, the snow retrieval lookup tables can be formed in a way that directly links the Ku- and Ka-band radar reflectivities to snow water content and equivalent snowfall rate without use of the derived PSD parameters. A sensitivity study of the retrieval results to the PSD and scattering models is performed to better understand the dual-wavelength retrieval uncertainties. To aid in the development of the Ku- and Ka-band dual-wavelength radar technique and to further evaluate its performance, self-consistency tests are conducted using measurements of the snow PSD and fall velocity acquired from the Snow Video Imager/Particle Image Probe (SVI/PIP) during the winter of 2014 at the NASA Wallops Flight Facility site in Wallops Island, Virginia.
C1 [Liao, Liang] Morgan State Univ, Goddard Earth Sci Technol & Res Program, Baltimore, MD 21239 USA.
[Meneghini, Robert] NASA, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA.
[Tokay, Ali] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA.
[Tokay, Ali] Joint Ctr Earth Syst Technol, Baltimore, MD USA.
[Bliven, Larry F.] NASA, Wallops Flight Facil, Wallops Isl, VA USA.
RP Liao, L (reprint author), NASA, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA.
EM liang.liao-1@nasa.gov
FU Dr. R. Kakar of NASA Headquarters under NASA's Precipitation Measurement
Mission (PMM) [NNH12ZDA001N-PMM]
FX This work is supported by Dr. R. Kakar of NASA Headquarters under NASA's
Precipitation Measurement Mission (PMM; Grant NNH12ZDA001N-PMM). The
authors also thank Mr. Jorel Torres of the South Dakota School of Mines
and Technology for providing and processing SVI/PIP data, and Dr.
Kwo-Sen Kuo of the University of Maryland for providing the scattering
database.
NR 40
TC 0
Z9 0
U1 3
U2 3
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
EI 1558-8432
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD SEP
PY 2016
VL 55
IS 9
BP 1845
EP 1858
DI 10.1175/JAMC-D-15-0355.1
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DX1QM
UT WOS:000384142100001
ER
PT J
AU Bedka, KM
Khlopenkov, K
AF Bedka, Kristopher M.
Khlopenkov, Konstantin
TI A Probabilistic Multispectral Pattern Recognition Method for Detection
of Overshooting Cloud Tops Using Passive Satellite Imager Observations
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID PROFILING RADAR OBSERVATIONS; STRATOSPHERIC WATER-VAPOR; GOES-R;
PRECIPITATION SYSTEMS; GLOBAL DISTRIBUTION; SEVERE WEATHER;
CLIMATE-CHANGE; CONVECTION
AB Deep convective updrafts often penetrate through the surrounding cirrus anvil and into the lower stratosphere. Cross-tropopause transport of ice, water vapor, and chemicals occurs within these "overshooting tops'' (OTs) along with a variety of hazardous weather conditions. OTs are readily apparent in satellite imagery, and, given the importance of OTs for weather and climate, a number of automated satellite-based detection methods have been developed. Some of these methods have proven to be relatively reliable, and their products are used in diverse Earth science applications. Nevertheless, analysis of these methods and feedback from product users indicate that use of fixed infrared temperature-based detection criteria often induces biases that can limit their utility for weather and climate analysis. This paper describes a new multispectral OT detection approach that improves upon those previously developed by minimizing use of fixed criteria and incorporating pattern recognition analyses to arrive at an OT probability product. The product is developed and validated using OT and non-OT anvil regions identified by a human within MODIS imagery. The product offered high skill for discriminating between OTs and anvils and matched 69% of human OT identifications for a particular probability threshold with a false-detection rate of 18%, outperforming previously existing methods. The false-detection rate drops to 1% when OT-induced texture detected within visible imagery is used to constrain the IR-based OT probability product. The OT probability product is also shown to improve severe-storm detection over the United States by 20% relative to the best existing method.
C1 [Bedka, Kristopher M.] NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA.
[Khlopenkov, Konstantin] Sci Syst & Applicat Inc, Hampton, VA USA.
RP Bedka, KM (reprint author), NASA, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA.
EM kristopher.m.bedka@nasa.gov
FU GOES-R Risk Reduction Research (R3) program
FX This research has been supported by the GOES-R Risk Reduction Research
(R3) program. In particular, we thank Dr. Steven Goodman, senior (chief)
scientist, GOES-R System Program, for his guidance and support
throughout this effort. We thank Patrick Minnis and Christopher Velden
for their advice and collaboration throughout the algorithm-development
process. We thank Cameron Homeyer for providing the WSR-88D data shown
in this paper. We also thank Jake Smith for manually identifying OT
locations in GOES-14 satellite imagery.
NR 41
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Z9 0
U1 2
U2 2
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
EI 1558-8432
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD SEP
PY 2016
VL 55
IS 9
BP 1983
EP 2005
DI 10.1175/JAMC-D-15-0249.1
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DX1QM
UT WOS:000384142100008
ER
PT J
AU Magi, BI
Winesett, T
Cecil, DJ
AF Magi, Brian I.
Winesett, Thomas
Cecil, Daniel. J.
TI Estimating Lightning from Microwave Remote Sensing Data
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID CLIMATE DATA RECORD; UNITED-STATES; SSM/I SENSORS; PART I; CLOUD;
THUNDERSTORMS; RATES; EARTH; FIRE; IMAGER/SOUNDER
AB This study evaluates a method for estimating the cloud-to-ground (CG) lightning flash rate from microwave remote sensing data. Defense Meteorological Satellite Program satellites have been in operation since 1987 and include global-viewing microwave sensors that capture thunderstorms as brightness temperature depressions. The National Lightning Detection Network (NLDN) has monitored CG lightning in the United States since 1997. This study investigates the relationship between CG lightning and microwave brightness temperature fields for the contiguous United States from April to September for the years 2005-12. The findings suggest that an exponential function, empirically fit to the NLDN and SSM/I data, provides lightning count measurements that agree to within 60%-70% with NLDN lightning, but with substantial misses and false alarms in the predictions. The discrepancies seem to be attributable to regional differences in thunderstorm characteristics that require a detailed study at smaller spatial scales to truly resolve, but snow at higher elevations also produces some anomalous microwave temperature depressions similar to those of thunderstorms. The results for the contiguous United States in this study are a step toward potentially using SSM/I data to estimate CG lightning around the world, although the sensitivity of the results to regional differences related to meteorological regimes would need further study.
C1 [Magi, Brian I.; Winesett, Thomas] Univ North Carolina Charlotte, Dept Geog & Earth Sci, 9201 Univ City Blvd, Charlotte, NC 28223 USA.
[Cecil, Daniel. J.] NASA Marshall Space Flight Ctr, Huntsville, AL USA.
RP Magi, BI (reprint author), Univ North Carolina Charlotte, Dept Geog & Earth Sci, 9201 Univ City Blvd, Charlotte, NC 28223 USA.
EM brian.magi@uncc.edu
OI Magi, Brian/0000-0001-8131-0083
FU North Carolina Space Grant Consortium's New Investigator Program; UNC
Charlotte faculty research grant; Lightning Imaging Sensor (LIS) team
via the NASA Tropical Rainfall Measuring Mission
FX The authors thank the staff at the Precipitation Research Group at
Colorado State University for maintaining and managing the SSM/I data
distribution. BIM and TW were partially supported by the North Carolina
Space Grant Consortium's New Investigator Program. BIM was also
partially supported by a UNC Charlotte faculty research grant. DJC was
supported through the Lightning Imaging Sensor (LIS) team via the NASA
Tropical Rainfall Measuring Mission.
NR 46
TC 0
Z9 0
U1 4
U2 4
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
EI 1558-8432
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD SEP
PY 2016
VL 55
IS 9
BP 2021
EP 2036
DI 10.1175/JAMC-D-15-0306.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DX1QM
UT WOS:000384142100010
ER
PT J
AU Huang, XL
Chen, XH
Zhou, DK
Liu, X
AF Huang, Xianglei
Chen, Xiuhong
Zhou, Daniel K.
Liu, Xu
TI An Observationally Based Global Band-by-Band Surface Emissivity Dataset
for Climate and Weather Simulations
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID SEA-SURFACE; ALGORITHM; DATABASE; WINDOW; MODEL; SNOW; ICE
AB While current atmospheric general circulation models (GCMs) still treat the surface as a blackbody in their longwave radiation scheme, recent studies suggest the need for taking realistic surface spectral emissivity into account. There have been few measurements available for the surface emissivity in the far IR (<650 cm(-1)). Based on first-principle calculation, the authors compute the spectral emissivity over the entire longwave spectrum for a variety of surface types. MODIS-retrieved mid-IR surface emissivity at 0.05 degrees x 0.05 degrees spatial resolution is then regressed against the calculated spectral emissivity to determine the surface type for each grid. The derived spectral emissivity data are then spatially averaged onto 0.5 degrees x 0.5 degrees grids and spectrally integrated onto the bandwidths used by the RRTMG_LW-a longwave radiation scheme widely used in current climate and numerical weather models. The band-by-band surface emissivity dataset is then compared with retrieved surface spectral emissivities from Infrared Atmospheric Sounding Interferometer (IASI) measurements. The comparison shows favorable agreement between two datasets in all the bands covered by the IASI measurements. The authors further use the dataset in conjunction with ERA-Interim to evaluate its impact on the top-of-atmosphere radiation budget. Depending on the blackbody surface assumptions used in the original calculation, the globally averaged difference caused by the inclusion of realistic surface emissivity ranges from -1.2 to -1.5 W m(-2) for clear-sky OLR and from -0.67 to -0.94 W m(-2) for all-sky OLR. Moreover, the difference is not spatially uniform and has a distinct spatial pattern.
C1 [Huang, Xianglei; Chen, Xiuhong] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
[Zhou, Daniel K.; Liu, Xu] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Huang, XL (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, 2455 Hayward St, Ann Arbor, MI 48109 USA.
EM xianglei@umich.edu
FU DOE Office of Biological and Environmental Research [DE-SC0012969]; NASA
[NNX15AC25G]
FX We wish to thank three anonymous reviewers for their thorough and
thoughtful comments, which improved the clarity of the presentation. The
ECMWF-Interim data were obtained from http://apps.ecmwf.int/datasets/.
The MODIS retrievals of surface emissivity were from
ftp://ftp.ssec.wisc.edu/pub/g_emis/. This research is supported by DOE
Office of Biological and Environmental Research under Grant DE-SC0012969
and by NASA under Grant NNX15AC25G awarded to the University of
Michigan.
NR 36
TC 0
Z9 0
U1 1
U2 1
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
EI 1520-0469
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD SEP
PY 2016
VL 73
IS 9
BP 3541
EP 3555
DI 10.1175/JAS-D-15-0355.1
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW8RP
UT WOS:000383923500011
ER
PT J
AU Guimond, SR
Heymsfield, GM
Reasor, PD
Didlake, AC
AF Guimond, Stephen R.
Heymsfield, Gerald M.
Reasor, Paul D.
Didlake, Anthony C., Jr.
TI The Rapid Intensification of Hurricane Karl (2010): New Remote Sensing
Observations of Convective Bursts from the Global Hawk Platform
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID TROPICAL CYCLONE INTENSIFICATION; HIGH-RESOLUTION SIMULATION;
INNER-CORE; PART I; 3-DIMENSIONAL PERTURBATIONS; DOPPLER RADAR; BONNIE
1998; EVOLUTION; EYEWALL; EYE
AB The evolution of rapidly intensifying Hurricane Karl (2010) is examined from a suite of remote sensing observations during the NASA Genesis and Rapid Intensification Processes (GRIP) field experiment. The novelties of this study are in the analysis of data from the airborne Doppler radar High-Altitude Imaging Wind and Rain Airborne Profiler (HI WRAP) and the new Global Hawk airborne platform that allows long endurance sampling of hurricanes. Supporting data from the High-Altitude Monolithic Microwave Integrated Circuit (MMIC) Sounding Radiometer (HAMSR) microwave sounder coincident with HIWRAP and coordinated flights with the NOAA WP-3D aircraft help to provide a comprehensive understanding of the storm. The focus of the analysis is on documenting and understanding the structure, evolution, and role of small-scale deep convective forcing in the storm intensification process. Deep convective bursts are sporadically initiated in the downshear quadrants of the storm and rotate into the upshear quadrants for a period of similar to 12 h during the rapid intensification. The aircraft data analysis indicates that the bursts are being formed and maintained through a combination of two main processes: 1) convergence generated from counterrotating mesovortex circulations and the larger vortex-scale flow and 2) the turbulent (scales of similar to 25 km) transport of anomalously warm, buoyant air from the eye to the eyewall at low levels. The turbulent mixing across the eyewall interface and forced convective descent adjacent to the bursts assists in carving out the eye of Karl, which leads to an asymmetric enhancement of the warm core. The mesovortices play a key role in the evolution of the features described above. The Global Hawk aircraft allowed an examination of the vortex response and axisymmetrization period in addition to the burst pulsing phase. A pronounced axisymmetric development of the vortex is observed following the pulsing phase that includes a sloped eyewall structure and formation of a clear, wide eye.
C1 [Guimond, Stephen R.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Guimond, Stephen R.; Heymsfield, Gerald M.; Didlake, Anthony C., Jr.] NASA, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA.
[Reasor, Paul D.] NOAA, Atlantic Oceanog & Meteorol Lab, Hurricane Res Div, Miami, FL 33149 USA.
[Didlake, Anthony C., Jr.] Oak Ridge Associated Univ, Oak Ridge, TN USA.
RP Guimond, SR (reprint author), NASA, Goddard Space Flight Ctr, Code 612, Greenbelt, MD 20771 USA.
EM stephen.guimond@nasa.gov
RI Reasor, Paul/B-2932-2014
OI Reasor, Paul/0000-0001-6407-017X
FU Heymsfield's NASA GRIP through NASA; Heymsfield's NASA HS3 through NASA;
NOAA; NASA; Institute of Geophysics and Planetary Physics (IGPP) at Los
Alamos National Laboratory
FX We thank Dr. Lihua Li, Matt McLinden, Martin Perrine, and Jaime
Cervantes for their engineering efforts on HIWRAP during GRIP. We also
thank the JPL HAMSR team for providing level 1B data used in this study,
which was obtained from NASA Global Hydrology Resource Center in
Huntsville, Alabama. Discussions with Dr. Scott Braun were useful and
helped to clarify the presentation of the data. Dr. Lin Tian helped with
early HIWRAP data processing. Author Guimond and coauthors Heymsfield
and Didlake were funded under Heymsfield's NASA GRIP and HS3 funding,
through NASA headquarters Program Manager Dr. Ramesh Kakar. Coauthor
Reasor was funded through NOAA base funds. The NASA weather program
under Dr. Ramesh Kakar supported GRIP. The first author was also
partially supported by the Institute of Geophysics and Planetary Physics
(IGPP) at Los Alamos National Laboratory. The first author thanks Robert
Kilgore for his work on the conceptual diagram. Finally, we thank Rob
Rogers and two anonymous reviewers for their very helpful comments.
NR 47
TC 1
Z9 1
U1 5
U2 5
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
EI 1520-0469
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD SEP
PY 2016
VL 73
IS 9
BP 3617
EP 3639
DI 10.1175/JAS-D-16-0026.1
PG 23
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW8RP
UT WOS:000383923500016
ER
PT J
AU Lin, Y
Wang, Y
Pan, BW
Hu, JX
Liu, YG
Zhang, RY
AF Lin, Yun
Wang, Yuan
Pan, Bowen
Hu, Jiaxi
Liu, Yangang
Zhang, Renyi
TI Distinct Impacts of Aerosols on an Evolving Continental Cloud Complex
during the RACORO Field Campaign
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID DEEP CONVECTIVE CLOUDS; FINE PARTICULATE MATTER; LONG-TERM IMPACTS;
ANTHROPOGENIC AEROSOLS; SHALLOW CUMULUS; MICROPHYSICS PARAMETERIZATION;
STRATOCUMULUS CLOUDS; ABSORBING AEROSOLS; RESOLVING MODEL; CLIMATE
MODELS
AB A continental cloud complex, consisting of shallow cumuli, a deep convective cloud (DCC), and stratus, is simulated by a cloud-resolving Weather Research and Forecasting Model to investigate the aerosol micro physical effect (AME) and aerosol radiative effect (ARE) on the various cloud regimes and their transitions during the Department of Energy Routine Atmospheric Radiation Measurement Aerial Facility Clouds with Low Optical Water Depths Optical Radiative Observations (RACORO) campaign. Under an elevated aerosol loading with AME only, a reduced cloudiness for the shallow cumuli and stratus resulted from more droplet evaporation competing with suppressed precipitation, but an enhanced cloudiness for the DCC is attributed to more condensation. With the inclusion of ARE, the shallow cumuli are suppressed owing to the thermodynamic effects of light-absorbing aerosols. The responses of DCC and stratus to aerosols are monotonic with AME only but nonmonotonic with both AME and ARE. The DCC is invigorated because of favorable convection and moisture conditions at night induced by daytime ARE, via the so-called aerosol-enhanced conditional instability mechanism. The results reveal that the overall aerosol effects on the cloud complex are distinct from the individual cloud types, highlighting that the aerosol cloud interactions for diverse cloud regimes and their transitions need to be evaluated to assess the regional and global climatic impacts.
C1 [Lin, Yun; Pan, Bowen; Hu, Jiaxi; Zhang, Renyi] Texas A&M Univ, College Stn, TX USA.
[Wang, Yuan] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Liu, Yangang] Brookhaven Natl Lab, Upton, NY 11973 USA.
RP Zhang, RY (reprint author), Texas A&M Univ, Dept Atmospher Sci, Oceanog & Meteorol Bldg,Room 1108,MS 3150, College Stn, TX 77843 USA.
EM renyi-zhang@tamu.edu
OI Lin, Yun/0000-0001-8222-0346
FU DOE's Earth System Modeling (ESM) Program via the FASTER project
[DOE-DE-AC02-98CH10886]; NASA [ROSES14-ACMAP, 105357-281945.02.31.03.24]
FX This research is supported by DOE's Earth System Modeling (ESM) Program
via the FASTER project (www.bnl.gov/faster), under Grant
DOE-DE-AC02-98CH10886. The RACORO field campaign was supported by DOE's
ARM program. We are grateful for discussions on RACORO with Dr. Andrew
Vogelmann at BNL and on aerosol microphysics effects on various clouds
with Dr. Jonathan H. Jiang at JPL. The data from the RACORO field
campaign, utilized only for education and research, are open to public
after registration and application. Supercomputing computational
facilities were provided by the Texas A&M University. Yuan Wang's
contribution to this work was sponsored by NASA ROSES14-ACMAP and was
carried at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA (Grant
105357-281945.02.31.03.24).
NR 93
TC 0
Z9 0
U1 9
U2 9
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
EI 1520-0469
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD SEP
PY 2016
VL 73
IS 9
BP 3681
EP 3700
DI 10.1175/JAS-D-15-0361.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW8RP
UT WOS:000383923500019
ER
PT J
AU Holt, LA
Alexander, MJ
Coy, L
Molod, A
Putman, W
Pawson, S
AF Holt, Laura A.
Alexander, M. Joan
Coy, Lawrence
Molod, Andrea
Putman, William
Pawson, Steven
TI Tropical Waves and the Quasi-Biennial Oscillation in a 7-km Global
Climate Simulation
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID GENERAL-CIRCULATION MODEL; COUPLED EQUATORIAL WAVES; QBO-LIKE
OSCILLATION; GRAVITY-WAVES; CONVECTION; TEMPERATURE; PARAMETERIZATION;
STRATOSPHERE; IMPROVEMENTS; VARIABILITY
AB This study investigates tropical waves and their role in driving a quasi-biennial oscillation (QBO)-like signal in stratospheric winds in a global 7-km-horizontal-resolution atmospheric general circulation model. The Nature Run (NR) is a 2-yr global mesoscale simulation of the Goddard Earth Observing System Model, version 5 (GEOS-5). In the tropics, there is evidence that the NR supports a broad range of convectively generated waves. The NR precipitation spectrum resembles the observed spectrum in many aspects, including the preference for westward-propagating waves. However, even with very high horizontal resolution and a healthy population of resolved waves, the zonal force provided by the resolved waves is still too low in the QBO region and parameterized gravity wave drag is the main driver of the NR-QBO-like oscillation (NR-QBO). The authors suggest that causes include coarse vertical resolution and excessive dissipation. Nevertheless, the very-high-resolution NR provides an opportunity to analyze the resolved wave forcing of the NR-QBO. In agreement with previous studies, large-scale Kelvin and small-scale waves contribute to the NR-QBO driving in eastward shear zones and small-scale waves dominate the NR-QBO driving in westward shear zones. Waves with zonal wavelength < 1000 km account for up to half of the small-scale (<3300 km) resolved wave forcing in eastward shear zones and up to 70% of the small-scale resolved wave forcing in westward shear zones of the NR-QBO.
C1 [Holt, Laura A.; Alexander, M. Joan] NorthWest Res Associates, 3380 Mitchell Lane, Boulder, CO 80301 USA.
[Coy, Lawrence; Putman, William; Pawson, Steven] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD USA.
[Coy, Lawrence] Sci Syst & Applicat Inc, Lanham, MD USA.
[Molod, Andrea] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
RP Holt, LA (reprint author), NorthWest Res Associates, 3380 Mitchell Lane, Boulder, CO 80301 USA.
EM laura@nwra.com
FU NASA Global Modeling and Assimilation Office [NNX14O76G]; NASA's
Modeling, Analysis and Prediction (MAP) program
FX We thank Dr. Ji-Eun Kim for providing the TRMM spectrum for Fig. 2, and
we thank three anonymous reviewers for their thoughtful and helpful
suggestions. This work is funded by the NASA Global Modeling and
Assimilation Office, Grant NNX14O76G. This work was also supported by
NASA's Modeling, Analysis and Prediction (MAP) program.
NR 51
TC 2
Z9 2
U1 5
U2 5
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
EI 1520-0469
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD SEP
PY 2016
VL 73
IS 9
BP 3771
EP 3783
DI 10.1175/JAS-D-15-0350.1
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW8RP
UT WOS:000383923500024
ER
PT J
AU Thurman, D
Poinsatte, P
Ameri, A
Culley, D
Raghu, S
Shyam, V
AF Thurman, Douglas
Poinsatte, Philip
Ameri, Ali
Culley, Dennis
Raghu, Surya
Shyam, Vikram
TI Investigation of Spiral and Sweeping Holes
SO JOURNAL OF TURBOMACHINERY-TRANSACTIONS OF THE ASME
LA English
DT Article
AB Surface infrared thermography, hotwire anemometry, and thermocouple surveys were performed on two new film cooling hole geometries: spiral/rifled holes and fluidic sweeping holes. The spiral holes attempt to induce large-scale vorticity to the film cooling jet as it exits the hole to prevent the formation of the kidney-shaped vortices commonly associated with film cooling jets. The fluidic sweeping hole uses a passive in-hole geometry to induce jet sweeping at frequencies that scale with blowing ratios. The spiral hole performance is compared to that of round holes with and without compound angles. The fluidic hole is of the diffusion class of holes and is therefore compared to a 777 hole and square holes. A patent-pending spiral hole design showed the highest potential of the nondiffusion-type hole configurations. Velocity contours and flow temperature were acquired at discreet cross sections of the downstream flow field. The passive fluidic sweeping hole shows the most uniform cooling distribution but suffers from low span-averaged effectiveness levels due to enhanced mixing. The data were taken at a Reynolds number of 11,000 based on hole diameter and freestream velocity. Infrared thermography was taken for blowing ratios of 1.0, 1.5, 2.0, and 2.5 at a density ratio of 1.05. The flow inside the fluidic sweeping hole was studied using 3D unsteady Reynolds-average Navier-Stokes (RANS).
C1 [Thurman, Douglas] US Army Res Lab, Cleveland, OH 44135 USA.
[Poinsatte, Philip; Culley, Dennis; Shyam, Vikram] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
[Ameri, Ali] Ohio State Univ, Dept Mech & Aerosp Engn, Columbus, OH 43210 USA.
[Raghu, Surya] Adv Fluid LLC, Columbia, MD 21045 USA.
RP Thurman, D (reprint author), US Army Res Lab, Cleveland, OH 44135 USA.
EM drthurman@nasa.gov; poinsatte@nasa.gov; ali.a.ameri@nasa.gov;
dennis.e.culley@nasa.gov; sraghu@advancedfluidics.com;
vikram.shyam-1@nasa.gov
FU NASA's Fundamental Aeronautics Program's Fixed Wing Project; NASA's
Center Innovation Fund
FX This work was funded by NASA's Fundamental Aeronautics Program's Fixed
Wing Project and NASA's Center Innovation Fund. The authors would also
like to thank Dr. Mark Wernet and Dr. Adam Wroblewski for the particle
image velocimetry results.
NR 15
TC 0
Z9 0
U1 0
U2 0
PU ASME
PI NEW YORK
PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0889-504X
EI 1528-8900
J9 J TURBOMACH
JI J. Turbomach.-Trans. ASME
PD SEP
PY 2016
VL 139
IS 9
AR 091007
DI 10.1115/1.4032839
PG 11
WC Engineering, Mechanical
SC Engineering
GA DX3BE
UT WOS:000384246800007
ER
PT J
AU Abarca, SF
Montgomery, MT
Braun, SA
Dunion, J
AF Abarca, Sergio F.
Montgomery, Michael T.
Braun, Scott A.
Dunion, Jason
TI On the Secondary Eyewall Formation of Hurricane Edouard (2014)
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID TROPICAL CYCLONES; RITA 2005; REPLACEMENT; INTENSITY; EVOLUTION;
DYNAMICS; VORTEX; CORE; CYCLE; FIELD
AB A first observationally based estimation of departures from gradient wind balance during secondary eyewall formation is presented. The study is based on the Atlantic Hurricane Edouard (2014). This storm was observed during the National Aeronautics and Space Administration's (NASA) Hurricane and Severe Storm Sentinel (HS3) experiment, a field campaign conducted in collaboration with the National Oceanic and Atmospheric Administration (NOAA). A total of 135 dropsondes are analyzed in two separate time periods: one named the secondary eyewall formation period and the other one referred to as the decaying double eyewalled storm period. During the secondary eyewall formation period, a time when the storm was observed to have only one eyewall, the diagnosed agradient force has a secondary maximum that coincides with the radial location of the secondary eyewall observed in the second period of study. The maximum spinup tendency of the radial influx of absolute vertical vorticity is within the boundary layer in the region of the eyewall of the storm and the spinup tendency structure elongates radially outward into the secondary region of supergradient wind, where the secondary wind maximum is observed in the second period of study. An analysis of the boundary layer averaged vertical structure of equivalent potential temperature reveals a conditionally unstable environment in the secondary eyewall formation region. These findings support the hypothesis that deep convective activity in this region contributed to spinup of the boundary layer tangential winds and the formation of a secondary eyewall that is observed during the decaying double eyewalled storm period.
C1 [Abarca, Sergio F.] Natl Ocean & Atmospher Adm, IM Syst Grp, Natl Ctr Environm Protect, Natl Weather Serv, College Pk, MD USA.
[Montgomery, Michael T.] Naval Postgrad Sch, Monterey, CA USA.
[Braun, Scott A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Dunion, Jason] Univ Miami, Cooperat Inst Marine & Atmospher Studies, Miami, FL USA.
[Dunion, Jason] NOAA, Atlantic Oceanog & Meteorol Lab, Hurricane Res Div, Miami, FL 33149 USA.
RP Abarca, SF (reprint author), NOAA, IM Syst Grp, NWS, NCEP, 5830 Univ Res Court, College Pk, MD 20740 USA.
EM sergio.abarca@noaa.gov
RI Dunion, Jason/B-1352-2014
OI Dunion, Jason/0000-0001-7489-0569
FU National Research Council (NRC) through Research Associateship Program;
Naval Postgraduate School (NPS) in Monterey, California; NSF
[AGS-1313948]; NOAA HFIP Grant [N0017315WR00048]; NASA HS3 Grant
[NNG11PK021]; U.S. Naval Postgraduate School
FX The first author gratefully acknowledges the support from the National
Research Council (NRC) through its Research Associateship Program; the
host institution, the Naval Postgraduate School (NPS) in Monterey,
California; and Scott Braun for the funding that made it possible for
him to participate in the H53 deployment during the 2014 hurricane
season. MTM acknowledges the support of NSF Grant AGS-1313948, NOAA HFIP
Grant N0017315WR00048, NASA HS3 Grant NNG11PK021, and the U.S. Naval
Postgraduate School.
NR 37
TC 0
Z9 0
U1 2
U2 2
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 SEP
PY 2016
VL 144
IS 9
BP 3321
EP 3331
DI 10.1175/MWR-D-15-0421.1
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW8RN
UT WOS:000383923300014
ER
PT J
AU Lee, JH
Biging, GS
Fisher, JB
AF Lee, Jun-Hak
Biging, Gregory S.
Fisher, Joshua B.
TI An Individual Tree-Based Automated Registration of Aerial Images to
Lidar Data in a Forested Area
SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING
LA English
DT Article
ID MULTISPECTRAL DATA FUSION; AIRBORNE LASER SCANNER; CROWN DETECTION;
LAND-COVER; DELINEATION; HEIGHT; CLASSIFICATION; RECONSTRUCTION;
SEGMENTATION; MOSAICKING
AB In this paper, we demonstrate an approach to align aerial images to airborne lidar data by using common object features (tree tops) from both data sets under the condition that conventional correlation-based approaches are challenging due to the fact that the spatial pattern of pixel gray-scale values in aerial images hardly exist in lidar data. We extracted tree tops by using an image processing technique called extended-maxima transformation from both aerial images and lidar data. Our approach was tested at the Angelo Coast Range Reserve on the South Fork Eel River forests in Mendocino County, California. Although the aerial images were acquired simultaneously with the lidar data, the images had only approximate exposure point locations and average flight elevation information, which mimicked the condition of limited information availability about the aerial images. Our results showed that this approach enabled us to align aerial images to airborne lidar data at the single-tree level with reasonable accuracy. With a local transformation model (piecewise linear model), the RMSE and the median absolute deviation (MAD) of the registration were 9.2 pixels (2.3 meters) and 6.8 pixels (1.41 meters), respectively. We expect our approach to be applicable to fine scale change detection for forest ecosystems and may serve to extract detailed forest biophysical parameters.
C1 [Lee, Jun-Hak] Univ Oregon, Dept Landscape Architecture, Eugene, OR 97403 USA.
[Biging, Gregory S.] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA.
[Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Lee, JH (reprint author), Univ Oregon, Dept Landscape Architecture, Eugene, OR 97403 USA.
EM junhaklee@uoregon.edu
FU W.S. Rosecrans Fellowship, Environmental Science, Policy, and
Management, University of California, Berkeley; National Aeronautics and
Space Administration
FX We gratefully acknowledge the use of lidar data sets supplied by Dr.
William E. Dietrich and the National Center of Airborne Laser Mapping
(NCALM). The first author was partially funded by the W.S. Rosecrans
Fellowship, Environmental Science, Policy, and Management, University of
California, Berkeley. Dr. Joshua B. Fisher contributed to this paper
through work by the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration.
NR 60
TC 0
Z9 0
U1 12
U2 12
PU AMER SOC PHOTOGRAMMETRY
PI BETHESDA
PA 5410 GROSVENOR LANE SUITE 210, BETHESDA, MD 20814-2160 USA
SN 0099-1112
EI 2374-8079
J9 PHOTOGRAMM ENG REM S
JI Photogramm. Eng. Remote Sens.
PD SEP
PY 2016
VL 82
IS 9
BP 699
EP 710
DI 10.14358/PERS.82.9.699
PG 12
WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing;
Imaging Science & Photographic Technology
SC Physical Geography; Geology; Remote Sensing; Imaging Science &
Photographic Technology
GA DX0NR
UT WOS:000384060300007
ER
PT J
AU Mendez-Villanueva, A
Suarez-Arrones, L
Rodas, G
Fernandez-Gonzalo, R
Tesch, P
Linnehan, R
Kreider, R
Di Salvo, V
AF Mendez-Villanueva, Alberto
Suarez-Arrones, Luis
Rodas, Gil
Fernandez-Gonzalo, Rodrigo
Tesch, Per
Linnehan, Richard
Kreider, Richard
Di Salvo, Valter
TI MRI-Based Regional Muscle Use during Hamstring Strengthening Exercises
in Elite Soccer Players
SO PLOS ONE
LA English
DT Article
ID MEDICAL-RESEARCH PROGRAM; PROFESSIONAL FOOTBALL; ECCENTRIC OVERLOAD;
NONUNIFORM CHANGES; INJURIES; PREVENTION; MECHANICS; STRAINS; SCIENCE;
RETURN
AB The present study examined site-specific hamstring muscles use with functional magnetic resonance imaging (MRI) in elite soccer players during strength training. Thirty-six players were randomized into four groups, each performing either Nordic hamstring, flywheel legcurl, Russian belt or the hip-extension conic-pulley exercise. The transverse relaxation time (T-2) shift from pre-to post-MRI were calculated for the biceps femoris long (BFI) and short (BFs) heads, semitendinosus (ST) and semimembranosus (SM) muscles at proximal, middle and distal areas of the muscle length. T-2 values increased substantially after flywheel leg-curl in all regions of the BFI (from 9 +/- 8 to 16 +/- 8%), BFs (41 +/- 6-71 +/- 11%), and ST (60 +/- 1-69 +/- 7%). Nordic hamstring induced a substantial T2 increase in all regions of the BFs (13 +/- 8-16 +/- 5%) and ST (15 +/- 7-17 +/- 5%). T-2 values after the Russian belt deadlift substantially increased in all regions of the BFI (6 +/- 4-7 +/- 5%), ST (8 +/- 3-11 +/- 2%), SM (6 +/- 4-10 +/- 4%), and proximal and distal regions of BFs (6 +/- 6-8 +/- 5%). T-2 values substantially increased after hip-extension conic-pulley only in proximal and middle regions of BFI (11 +/- 5-7 +/- 5%) and ST (7 +/- 3-12 +/- 4%). The relevance of such MRI-based inter-and intra-muscle use in designing more effective resistance training for improving hamstring function and preventing hamstring injuries in elite soccer players should be explored with more mechanistic studies.
C1 [Mendez-Villanueva, Alberto; Suarez-Arrones, Luis; Di Salvo, Valter] ASPIRE Acad, Football Performance & Sci Dept, Doha, Qatar.
[Suarez-Arrones, Luis] Pablo de Olavide Univ, Sports Dept, Seville, Spain.
[Rodas, Gil] Futbol Club Barcelona, Dept Med, Barcelona, Spain.
[Fernandez-Gonzalo, Rodrigo; Tesch, Per] Karolinska Inst, Dept Physiol & Pharmacol, Stockholm, Sweden.
[Linnehan, Richard] Johnson Space Ctr, Natl Aeronaut & Space Adm, Houston, TX USA.
[Kreider, Richard] Texas A&M Univ, Dept Hlth & Kinesiol, College Stn, TX USA.
[Di Salvo, Valter] Univ Rome Foro Italico, Dept Movement Human & Hlth Sci, Rome, Italy.
RP Mendez-Villanueva, A (reprint author), ASPIRE Acad, Football Performance & Sci Dept, Doha, Qatar.
EM jose.villanueva@aspire.qa
FU NPRP grant from the Qatar National Research Fund [NPRP 6-1526-3-363]
FX This study was made possible by NPRP grant #NPRP 6-1526-3-363 from the
Qatar National Research Fund (a member of Qatar Foundation). The funder
provided support in the form of salaries for authors LSA, RFG and PT,
but did not have any additional role in the study design, data
collection and analysis, decision to publish, or preparation of the
manuscript. The specific roles of these authors are articulated in the
'author contributions' section.
NR 31
TC 0
Z9 0
U1 14
U2 14
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 SEP 1
PY 2016
VL 11
IS 9
AR e0161356
DI 10.1371/journal.pone.0161356
PG 15
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DV3WN
UT WOS:000382855600024
PM 27583444
ER
PT J
AU Ayers, A
Miller, K
Park, J
Schwartz, L
Antcliff, R
AF Ayers, Alan
Miller, Kimberly
Park, Jongwon
Schwartz, Lawrence
Antcliff, Rich
TI The Hollywood Model Leveraging the Capabilities of Freelance Talent to
Advance Innovation and Reduce Risk
SO RESEARCH-TECHNOLOGY MANAGEMENT
LA English
DT Article
DE Hollywood model; Talent management; Futures; IRI2038; IRI Research
ID ERA
AB In 2013, the Industrial Research Institute (IRI) commissioned the IRI2038 foresight project to research how developments in technology, business processes, regulation and other spheres will impact the art and science of research and technology management over the next 25 years. That study defined three scenarios likely to shape the innovation process in coming years. One of those scenarios was the Hollywood model, in which scientists, engineers, and innovators no longer work for a single firm but rather contract out their services to individual projects and then move on to other projects and companies. Over the course of six months, an IRI Research working group conducted four workshops with R&D leaders at IRI member companies to explore how talent management would be affected in this scenario. The workshops identified challenges and opportunities associated with the Hollywood model as a paradigm for industrial R&D, focused around eight critical aspects of current talent management practice. Although the Hollywood model faces significant infrastructure and legal impediments today, its employment of external R&D workers with diverse experiences and perspectives is likely to create a greater opportunity for significant innovation.
C1 [Ayers, Alan] UConn, Storrs, CT 06269 USA.
[Ayers, Alan] IDCC, Doha, Qatar.
[Ayers, Alan] Research on Res Comm, Arlington, VA 22203 USA.
[Ayers, Alan] ROR Grp Rad Innovat & Levels Innovat, Arlington, TX USA.
[Miller, Kimberly] Sutton House Consulting LLC, Florence, OR USA.
[Miller, Kimberly] Cargills Global R&D Team, Minneapolis, MN USA.
[Miller, Kimberly] Univ St Thomas, Org Dev, St Paul, MN USA.
[Park, Jongwon] Korea Innovat Ctr, Washington, DC USA.
[Park, Jongwon] Arizona State Univ, Consortium Sci Policy & Outcomes, Tempe, AZ 85287 USA.
[Schwartz, Lawrence] IP Business Tech Solut, Menlo Pk, CA USA.
[Antcliff, Rich] NASA, Langley Res Ctr, Off Strateg Anal Commun & Business Dev, Hampton, VA 23665 USA.
RP Ayers, A (reprint author), UConn, Storrs, CT 06269 USA.; Ayers, A (reprint author), IDCC, Doha, Qatar.; Ayers, A (reprint author), Research on Res Comm, Arlington, VA 22203 USA.; Ayers, A (reprint author), ROR Grp Rad Innovat & Levels Innovat, Arlington, TX USA.
EM adayers@buildinnovation.com; kim@suttonhouseconsulting.com;
jpglobalconsultingllc@gmail.com; larryschwartz333@aol.com;
Richard.R.Antcliff@nasa.gov
NR 18
TC 0
Z9 0
U1 15
U2 15
PU INDUSTRIAL RESEARCH INST, INC
PI ARLINGTON
PA 2300 CLARENDON BLVD, STE 400, ARLINGTON, VA 22201 USA
SN 0895-6308
EI 1930-0166
J9 RES TECHNOL MANAGE
JI Res.-Technol. Manage.
PD SEP-OCT
PY 2016
VL 59
IS 5
BP 27
EP 37
DI 10.1080/08956308.2016.1208041
PG 11
WC Business; Engineering, Industrial; Management
SC Business & Economics; Engineering
GA DX6ZQ
UT WOS:000384535600009
ER
PT J
AU Haarig, M
Engelmann, R
Ansmann, A
Veselovskii, I
Whiteman, DN
Althausen, D
AF Haarig, Moritz
Engelmann, Ronny
Ansmann, Albert
Veselovskii, Igor
Whiteman, David N.
Althausen, Dietrich
TI 1064 nm rotational Raman lidar for particle extinction and lidar-ratio
profiling: cirrus case study
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID SPECTRAL-RESOLUTION LIDAR; ELASTIC-BACKSCATTER LIDAR; INDIAN AEROSOL
PLUME; MULTIWAVELENGTH LIDAR; SAHARAN DUST; WATER-VAPOR;
PHYSICAL-PROPERTIES; 6-WAVELENGTH LIDAR; OPTICAL-PROPERTIES; RETRIEVAL
AB For the first time, vertical profiles of the 1064 nm particle extinction coefficient obtained from Raman lidar observations at 1058 nm (nitrogen and oxygen rotational Raman backscatter) are presented. We applied the new technique in the framework of test measurements and performed several cirrus observations of particle backscatter and extinction coefficients, and corresponding extinction-to-backscatter ratios at the wavelengths of 355, 532, and 1064 nm. The cirrus backscatter coefficients were found to be equal for all three wavelengths keeping the retrieval uncertainties in mind. The multiple-scattering-corrected cirrus extinction coefficients at 355 nm were on average about 20-30% lower than the ones for 532 and 1064 nm. The cirrus-mean extinction-to-backscatter ratio (lidar ratio) was 31 +/- 5 sr (355 nm), 36 +/- 5 sr (532 nm), and 38 +/- 5 sr (1064 nm) in this single study. We further discussed the requirements needed to obtain aerosol extinction profiles in the lower troposphere at 1064 nm with good accuracy (20% relative uncertainty) and appropriate temporal and vertical resolution.
C1 [Haarig, Moritz; Engelmann, Ronny; Ansmann, Albert; Althausen, Dietrich] Leibniz Inst Tropospher Res, Leipzig, Germany.
[Veselovskii, Igor] Phys Instrumentat Ctr, Moscow, Russia.
[Whiteman, David N.] NASA, GSFC, Greenbelt, MD USA.
RP Haarig, M (reprint author), Leibniz Inst Tropospher Res, Leipzig, Germany.
EM haarig@tropos.de
FU Russian Science Foundation [16-17-10241]
FX We thank Johannes Buhl for providing Doppler lidar observations of
vertical velocity and estimated ice crystal sizes. Modeling of the
rotational Raman filter parameters was supported by the Russian Science
Foundation (project no. 16-17-10241).
NR 63
TC 0
Z9 0
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 SEP 1
PY 2016
VL 9
IS 9
BP 4269
EP 4278
DI 10.5194/amt-9-4269-2016
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW8FZ
UT WOS:000383891500002
ER
PT J
AU Diskin, B
Thomas, JL
Rumsey, CL
Schwoppe, A
AF Diskin, Boris
Thomas, James L.
Rumsey, Christopher L.
Schwoeppe, Axel
TI Grid-Convergence of Reynolds-Averaged Navier-Stokes Solutions for
Benchmark Flows in Two Dimensions
SO AIAA JOURNAL
LA English
DT Article
ID TURBULENCE MODEL; EULER EQUATIONS
AB A detailed grid-convergence study has been conducted to establish reference solutions corresponding to the one-equation linear eddy-viscosity Spalart-Allmaras turbulence model for two-dimensional turbulent flows around the NACA0012 airfoil and a flat plate. The study involved the three widely used codes CFL3D (NASA), FUN3D (NASA), and TAU (DLR, The German Aerospace Center), as well as families of uniformly refined structured grids that differed in the grid density patterns. Solutions computed by different codes on different grid families appeared to converge to the same continuous limit but exhibited strikingly different convergence characteristics. The grid resolution in the vicinity of geometric singularities, such as a sharp trailing edge, was found to be the major factor affecting accuracy and convergence of discrete solutions; the effects of this local grid resolution were more prominent than differences in discretization schemes and/or grid elements. The results reported for these relatively simple turbulent flows demonstrated that CFL3D, FUN3D, and TAU solutions were very similar on the finest grids used in the study, but even those grids were not sufficient to conclusively establish an asymptotic convergence order.
C1 [Diskin, Boris] Natl Inst Aerosp, MAE Dept, Hampton, VA 23666 USA.
[Thomas, James L.; Rumsey, Christopher L.] NASA Langley Res Ctr, Computat AeroSci Branch, Hampton, VA 23681 USA.
[Schwoeppe, Axel] German Aerosp Ctr, DLR, Inst Aerodynam & Flow Technol, D-38108 Braunschweig, Germany.
[Diskin, Boris] Univ Virginia, Charlottesville, VA 22904 USA.
RP Diskin, B (reprint author), Natl Inst Aerosp, MAE Dept, Hampton, VA 23666 USA.
FU NASA [NNL09AA00A]
FX The first author acknowledges support from NASA Cooperative Agreement
NNL09AA00A.
NR 38
TC 0
Z9 0
U1 3
U2 3
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 SEP
PY 2016
VL 54
IS 9
BP 2563
EP 2588
DI 10.2514/1.J054555
PG 26
WC Engineering, Aerospace
SC Engineering
GA DV8GN
UT WOS:000383175600002
ER
PT J
AU Pandya, MJ
Diskin, B
Thomas, JL
Frink, NT
AF Pandya, Mohagna J.
Diskin, Boris
Thomas, James L.
Frink, Neal T.
TI Improved Convergence and Robustness of USM3D Solutions on Mixed-Element
Grids
SO AIAA JOURNAL
LA English
DT Article; Proceedings Paper
CT 53rd AIAA Aerospace Sciences Meeting / AIAA Atmospheric Flight Mechanics
Conference / 17th AIAA Non-Deterministic Approaches Conference / AIAA
Science and Technology Forum and Exposition (SciTech) / AIAA Infotech at
Aerospace Conference
CY JAN 05-09, 2015
CL Kissimmee, FL
SP AIAA
ID EULER EQUATIONS; GENERATION; ALGORITHM; DYNAMICS; TETRUSS; FLOWS; CODES
AB Several improvements to the mixed-element USM3D discretization and defect-correction schemes have been made. A new methodology for nonlinear iterations, called the Hierarchical Adaptive Nonlinear Iteration Method, has been developed and implemented. The Hierarchical Adaptive Nonlinear Iteration Method provides two additional hierarchies around a simple and approximate preconditioner of USM3D. The hierarchies are a matrix-free linear solver for the exact linearization of Reynolds-averaged Navier-Stokes equations and a nonlinear control of the solution update. Two variants of the Hierarchical Adaptive Nonlinear Iteration Method are assessed on four benchmark cases, namely, a zero-pressure-gradient flat plate, a bump-in-channel configuration, the NACA 0012 airfoil, and a NASA Common Research Model configuration. The new methodology provides a convergence acceleration factor of 1.4 to 13 over the preconditioner-alone method representing the baseline solver technology.
C1 [Pandya, Mohagna J.] NASA Langley Res Ctr, Configurat Aerodynam Branch, Mail Stop 499, Hampton, VA 23681 USA.
[Diskin, Boris] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Thomas, James L.; Frink, Neal T.] NASA Langley Res Ctr, Computat Aerosci Branch, Mail Stop 499, Hampton, VA 23681 USA.
[Diskin, Boris] Univ Virginia, MAE Dept, Charlottesville, VA USA.
RP Pandya, MJ (reprint author), NASA Langley Res Ctr, Configurat Aerodynam Branch, Mail Stop 499, Hampton, VA 23681 USA.
NR 47
TC 0
Z9 0
U1 3
U2 3
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 SEP
PY 2016
VL 54
IS 9
BP 2589
EP 2610
DI 10.2514/1.J054545
PG 22
WC Engineering, Aerospace
SC Engineering
GA DV8GN
UT WOS:000383175600003
ER
PT J
AU Ceze, MA
Fidkowski, KJ
AF Ceze, Marco A.
Fidkowski, Krzysztof J.
TI High-Order Output-Based Adaptive Simulations of Turbulent Flow in Two
Dimensions
SO AIAA JOURNAL
LA English
DT Article
ID NAVIER-STOKES EQUATIONS; DISCONTINUOUS GALERKIN DISCRETIZATIONS; MESH
ADAPTATION; FLUID-DYNAMICS; PREDICTION
AB Output-based high-order adaptive results are presented for several benchmark two-dimensional turbulent-flow simulations. The discretization is a high-order discontinuous Galerkin finite element method, and the equations solved are compressible Navier-Stokes, Reynolds-averaged with a modified version of the Spalart-Allmaras one-equation model. Mesh refinement requirements are studied through automated output-based adaptation in which a discrete adjoint solution associated with an output (e.g., the drag coefficient) weights a fine-space residual and automatically selects the elements that need more resolution. The roles of high-order and mesh anisotropy are also investigated. Finally, differences are investigated between two mesh refinement strategies: hanging-node refinement of structured meshes versus metric-based remeshing of unstructured triangles.
C1 [Ceze, Marco A.] NASA Ames Res Ctr, Moffett Field, CA USA.
[Fidkowski, Krzysztof J.] Univ Michigan, Dept Aerosp Engn, Ann Arbor, MI 48109 USA.
[Ceze, Marco A.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA.
RP Ceze, MA (reprint author), NASA Ames Res Ctr, Moffett Field, CA USA.; Ceze, MA (reprint author), Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA.
EM marco.a.ceze@nasa.gov
FU U.S. Air Force Office of Scientific Research [FA9550-11-1-0081]
FX The authors acknowledge support from the U.S. Air Force Office of
Scientific Research under grant FA9550-11-1-0081.
NR 23
TC 0
Z9 0
U1 1
U2 1
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 SEP
PY 2016
VL 54
IS 9
BP 2611
EP 2625
DI 10.2514/1.J054517
PG 15
WC Engineering, Aerospace
SC Engineering
GA DV8GN
UT WOS:000383175600004
ER
PT J
AU Eisfeld, B
Rumsey, C
Togiti, V
AF Eisfeld, Bernhard
Rumsey, Chris
Togiti, Vamshi
TI Verification and Validation of a Second-Moment Closure Model (vol 54, pg
1524, 2016)
SO AIAA JOURNAL
LA English
DT Correction
C1 [Eisfeld, Bernhard; Togiti, Vamshi] DLR Inst Aerodynam & Flow Technol, D-38108 Braunschweig, Germany.
[Rumsey, Chris] NASA Langley Res Ctr, MS 128, Hampton, VA USA.
RP Eisfeld, B (reprint author), DLR Inst Aerodynam & Flow Technol, D-38108 Braunschweig, Germany.
NR 1
TC 0
Z9 0
U1 2
U2 2
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 SEP
PY 2016
VL 54
IS 9
BP 2925
EP 2925
DI 10.2514/1.J055336
PG 1
WC Engineering, Aerospace
SC Engineering
GA DV8GN
UT WOS:000383175600030
ER
PT J
AU Young, KE
Evans, CA
Hodges, KV
Bleacher, JE
Graff, TG
AF Young, Kelsey E.
Evans, Cynthia A.
Hodges, Kip V.
Bleacher, Jacob E.
Graff, Trevor G.
TI A review of the handheld X-ray fluorescence spectrometer as a tool for
field geologic investigations on Earth and in planetary surface
exploration
SO APPLIED GEOCHEMISTRY
LA English
DT Review
DE Handheld X-ray fluorescence spectrometer (hXRF); In situ geochemistry;
Planetary field geology; In situ field geologic instrument; Field
portable technology; Field spectroscopy
ID PORTABLE XRF; ROCKS; SAMPLES; DETECTOR; MARS; SOIL
AB X-ray fluorescence (XRF) spectroscopy is a well-established and commonly used technique in obtaining diagnostic compositional data on geological samples. Recently, developments in X-ray tube and detector technologies have resulted in miniaturized, field-portable instruments that enable new applications both in and out of standard laboratory settings. These applications, however, have not been extensively applied to geologic field campaigns. This study investigates the feasibility of using developing handheld XRF (hXRF) technology to enhance terrestrial field geology, with potential applications in planetary surface exploration missions. We demonstrate that the hXRF is quite stable, providing reliable and accurate data continuously over a several year period. Additionally, sample preparation is proved to have a marked effect on the strategy for collecting and assimilating hXRF data. While the hXRF is capable of obtaining data that are comparable to laboratory XRF analysis for several geologically-important elements (such as Si, Ca, Ti, and K), the instrument is unable to detect other elements (such as Mg and Na) reliably. While this limits the use of the hXRF, especially when compared to laboratory XRF techniques, the hXRF is still capable of providing the field user with significantly improved contextual awareness of a field site, and more work is needed to fully evaluate the potential of this instrument in more complex geologic environments. (C) 2016 The Authors. Published by Elsevier Ltd. This is an open access article under the CC BY-NC-ND license.
C1 [Young, Kelsey E.; Hodges, Kip V.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Evans, Cynthia A.; Graff, Trevor G.] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
[Bleacher, Jacob E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Graff, Trevor G.] Jacobs Engn Grp Inc, Houston, TX 77058 USA.
[Young, Kelsey E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Young, Kelsey E.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
RP Young, KE (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.; Young, KE (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.; Young, KE (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
EM Kelsey.E.Young@nasa.gov
RI Bleacher, Jacob/D-1051-2012
OI Bleacher, Jacob/0000-0002-8499-4828
FU GSRP (Graduate Student Researcher's Program) [NNX10AK72H]
FX The authors would like to thank Dr. Chris Condit for his thoughtful
review. The majority of this work was completed under the GSRP (Graduate
Student Researcher's Program) Grant Number NNX10AK72H as well as under
the RIS4E SSERVI team (Remote, In Situ and Synchrotron
Studies for Science and Exploration Solar System Exploration Research
Virtual Institute), led by Dr. Timothy Glotch at Stony Brook University.
The authors of this paper would also like to acknowledge Dr. Richard
Morris. Without his permission for access to the sample standards, this
work would not have been possible. In addition, we thank Dr. Stanley
Mertzman for his thoughtful discussions about calibrating against
laboratory data. We would also like to thank Dr. Carlton Allen and
Andrea Mosie for their assistance in both obtaining access to and
working with the lunar samples at NASA Johnson Space Center. Finally, we
thank Cameron Mercer for his figure organization insights. This is
SSERVI publication number SSERVI-2016-061.
NR 45
TC 1
Z9 1
U1 21
U2 21
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0883-2927
J9 APPL GEOCHEM
JI Appl. Geochem.
PD SEP
PY 2016
VL 72
BP 77
EP 87
DI 10.1016/j.apgeochem.2016.07.003
PG 11
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DW3DI
UT WOS:000383521900008
ER
PT J
AU Chirayath, V
Earle, SA
AF Chirayath, Ved
Earle, Sylvia A.
TI Drones that see through waves - preliminary results from airborne fluid
lensing for centimetre-scale aquatic conservation
SO AQUATIC CONSERVATION-MARINE AND FRESHWATER ECOSYSTEMS
LA English
DT Article; Proceedings Paper
CT 6th IUCN World Parks Congress
CY NOV, 2014
CL Sydney, AUSTRALIA
SP IUCN
DE fluid lensing; airborne remote sensing; coastal bathymetry; coral reef;
stromatolite; American Samoa; Shark Bay
AB 1. The use of fluid lensing technology on unmanned aerial vehicles (UAVs, or drones) is presented as a novel means for 3D imaging of aquatic ecosystems from above the water's surface at the centimetre scale. Preliminary results are presented from airborne fluid lensing campaigns conducted over the coral reefs of Ofu Island, American Samoa (2013) and the stromatolite reefs of Shark Bay, Western Australia (2014), covering a combined area of 15 km(2). These reef ecosystems were revealed with centimetre-scale 2D resolution, and an accompanying 3D bathymetry model was derived using fluid lensing, Structure from Motion and UAV position data. Data products were validated from in situ survey methods including underwater calibration targets, depth measurements and millimetre-scale high-dynamic-range gigapixel photogrammetry.
2. Fluid lensing is an experimental technology that uses water-transmitting wavelengths to passively image underwater objects at high-resolution by exploiting time-varying optical lensing events caused by surface waves. Fluid lensing data are captured from low-altitude, cost-effective electric UAVs to achieve multispectral imagery and bathymetry models at the centimetre scale over regional areas. As a passive system, fluid lensing is presently limited by signal-to-noise ratio and water column inherent optical properties to similar to 10 m depth over visible wavelengths in clear waters.
3. The datasets derived from fluid lensing present the first centimetre-scale images of a reef acquired from above the ocean surface, without wave distortion. The 3D multispectral data distinguish coral, fish and invertebrates in American Samoa, and reveal previously undocumented, morphologically distinct, stromatolite structures in Shark Bay. These findings suggest fluid lensing and multirotor electric drones represent a promising advance in the remote sensing of aquatic environments at the centimetre scale, or 'reef scale' relevant to the conservation of reef ecosystems. Pending further development and validation of fluid lensing methods, these technologies present a solution for large-scale 3D surveys of shallow aquatic habitats with centimetre-scale spatial resolution and hourly temporal sampling. Copyright (C) 2016 John Wiley & Sons, Ltd.
C1 [Chirayath, Ved] NASA, Ames Res Ctr, Lab Adv Sensing, Div Earth Sci, Moffett Field, CA 94035 USA.
RP Chirayath, V (reprint author), NASA, Ames Res Ctr, Mailstop 232-22, Moffett Field, CA 94305 USA.
EM ved.chirayath@nasa.gov
NR 15
TC 1
Z9 1
U1 17
U2 17
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1052-7613
EI 1099-0755
J9 AQUAT CONSERV
JI Aquat. Conserv.-Mar. Freshw. Ecosyst.
PD SEP
PY 2016
VL 26
SU 2
BP 237
EP 250
DI 10.1002/aqc.2654
PG 14
WC Environmental Sciences; Marine & Freshwater Biology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA DW5FL
UT WOS:000383668500017
ER
PT J
AU McCaig, HC
Stockton, A
Crilly, C
Chung, S
Kanik, I
Lin, Y
Zhong, F
AF McCaig, Heather C.
Stockton, Amanda
Crilly, Candice
Chung, Shirley
Kanik, Isik
Lin, Ying
Zhong, Fang
TI Supercritical Carbon Dioxide Extraction of Coronene in the Presence of
Perchlorate for In Situ Chemical Analysis of Martian Regolith
SO ASTROBIOLOGY
LA English
DT Article
DE Biomarkers; Carbon dioxide; In situ measurement; Mars; Search for Mars'
organics
ID POLYCYCLIC AROMATIC-HYDROCARBONS; MASS-SPECTROMETRY; ORGANIC-MATTER;
SUBCRITICAL WATER; METEORITE ALH84001; FLUID EXTRACTION; GALE CRATER;
MARS; MOLECULES; ORIGIN
AB The analysis of the organic compounds present in the martian regolith is essential for understanding the history and habitability of Mars, as well as studying the signs of possible extant or extinct life. To date, pyrolysis, the only technique that has been used to extract organic compounds from the martian regolith, has not enabled the detection of unaltered native martian organics. The elevated temperatures required for pyrolysis extraction can cause native martian organics to react with perchlorate salts in the regolith and possibly result in the chlorohydrocarbons that have been detected by in situ instruments. Supercritical carbon dioxide (SCCO2) extraction is an alternative to pyrolysis that may be capable of delivering unaltered native organic species to an in situ detector. In this study, we report the SCCO2 extraction of unaltered coronene, a representative polycyclic aromatic hydrocarbon (PAH), from martian regolith simulants, in the presence of 3 parts per thousand (ppth) sodium perchlorate. PAHs are a class of nonpolar molecules of astrobiological interest and are delivered to the martian surface by meteoritic infall. We also determined that the extraction efficiency of coronene was unaffected by the presence of perchlorate on the regolith simulant, and that no sodium perchlorate was extracted by SCCO2. This indicates that SCCO2 extraction can provide de-salted samples that could be directly delivered to a variety of in situ detectors. SCCO2 was also used to extract trace native fluorescent organic compounds from the martian regolith simulant JSC Mars-1, providing further evidence that SCCO2 extraction may provide an alternative to pyrolysis to enable the delivery of unaltered native organic compounds to an in situ detector on a future Mars rover.
C1 [McCaig, Heather C.; Crilly, Candice; Chung, Shirley; Kanik, Isik; Lin, Ying; Zhong, Fang] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Stockton, Amanda] Georgia Inst Technol, Atlanta, GA 30332 USA.
[Crilly, Candice] Occidental Coll, Los Angeles, CA 90041 USA.
RP Zhong, F (reprint author), CALTECH, Jet Prop Lab, M-S 70-24,4800 Oak Grove Dr, Pasadena, CA 91109 USA.; Lin, Y (reprint author), CALTECH, Jet Prop Lab, M-S 321-550,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ying.lin@jpl.nasa.gov; fang.zhong@jpl.nasa.gov
FU National Aeronautics and Space Administration (NASA); NASA Astrobiology
Science and Technology Instrument Development program
FX 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 (NASA)
and was supported by the NASA Astrobiology Science and Technology
Instrument Development program. The JPL author's copyright for this
paper is held by the California Institute of Technology. Government
sponsorship is acknowledged.
NR 48
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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 SEP
PY 2016
VL 16
IS 9
BP 703
EP 714
DI 10.1089/ast.2015.1443
PG 12
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA DW9IK
UT WOS:000383971100004
PM 27623199
ER
PT J
AU Misra, AK
Acosta-Maeda, TE
Sharma, SK
Mckay, CP
Gasda, PJ
Taylor, GJ
Lucey, PG
Flynn, L
Abedin, MN
Clegg, SM
Wiens, R
AF Misra, Anupam K.
Acosta-Maeda, Tayro E.
Sharma, Shiv K.
Mckay, Christopher P.
Gasda, Patrick J.
Taylor, G. Jeffrey
Lucey, Paul G.
Flynn, Luke
Abedin, M. Nurul
Clegg, Samuel M.
Wiens, Roger
TI "Standoff Biofinder" for Fast, Noncontact, Nondestructive, Large-Area
Detection of Biological Materials for Planetary Exploration
SO ASTROBIOLOGY
LA English
DT Article
DE Standoff Biofinder; Luminescence; Time-resolved fluorescence;
Biofluorescence; Planetary exploration; Planetary protection; Noncontact
nondestructive biodetection
ID LASER-INDUCED FLUORESCENCE; TIME-RESOLVED FLUORESCENCE; CHEMCAM
INSTRUMENT SUITE; REMOTE RAMAN; ULTRAVIOLET FLUORESCENCE; SPECTROSCOPIC
DETECTION; ROOM-TEMPERATURE; NUCLEIC-ACIDS; STEADY-STATE; EXCITATION
AB We developed a prototype instrument called the Standoff Biofinder, which can quickly locate biological material in a 500 cm(2) area from a 2 m standoff distance with a detection time of 0.1 s. All biogenic materials give strong fluorescence signals when excited with UV and visible lasers. In addition, the luminescence decay time of biogenic compounds is much shorter (<100 ns) than the micro-to millisecond decay time of transition metal ions and rare-earth ions in minerals and rocks. The Standoff Biofinder takes advantage of the short lifetime of biofluorescent materials to obtain real-time fluorescence images that show the locations of biological materials among luminescent minerals in a geological context. The Standoff Biofinder instrument will be useful for locating biological material during future NASA rover, lander, and crewed missions. Additionally, the instrument can be used for nondestructive detection of biological materials in unique samples, such as those obtained by sample return missions from the outer planets and asteroids. The Standoff Biofinder also has the capacity to detect microbes and bacteria on space instruments for planetary protection purposes.
C1 [Misra, Anupam K.; Acosta-Maeda, Tayro E.; Sharma, Shiv K.; Taylor, G. Jeffrey; Lucey, Paul G.; Flynn, Luke] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Mckay, Christopher P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Gasda, Patrick J.; Clegg, Samuel M.; Wiens, Roger] Los Alamos Natl Lab, Los Alamos, NM USA.
[Abedin, M. Nurul] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Misra, AK (reprint author), Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Sch Ocean & Earth Sci & Technol, 1680 East West Rd,POST 602, Honolulu, HI 96822 USA.
EM anupam@hawaii.edu
OI Gasda, Patrick/0000-0003-0895-1153; Clegg, Sam/0000-0002-0338-0948
FU NASA EPSCoR grant [NNX13AM98A]
FX This work has been supported by NASA EPSCoR grant NNX13AM98A. The
authors would like to thank Nancy Hulbirt and May Izumi for their
valuable help with figures and editing. Authors would like to thank the
reviewers for their valuable time in providing critical review and
constructive comments, which greatly helped improve the manuscript.
NR 83
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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 SEP
PY 2016
VL 16
IS 9
BP 715
EP 729
DI 10.1089/ast.2015.1400
PG 15
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA DW9IK
UT WOS:000383971100005
PM 27623200
ER
PT J
AU Bannister, MT
Kavelaars, JJ
Petit, JM
Gladman, BJ
Gwyn, SDJ
Chen, YT
Volk, K
Alexandersen, M
Benecchi, SD
Delsanti, A
Fraser, WC
Granvik, M
Grundy, WM
Guilbert-Lepoutre, A
Hestroffer, D
Ip, WH
Jakubik, M
Jones, RL
Kaib, N
Kavelaars, CF
Lacerda, P
Lawler, S
Lehner, MJ
Lin, HW
Lister, T
Lykawka, PS
Monty, S
Marsset, M
Murray-Clay, R
Noll, KS
Parker, A
Pike, RE
Rousselot, P
Rusk, D
Schwamb, ME
Shankman, C
Sicardy, B
Vernazza, P
Wang, SY
AF Bannister, Michele T.
Kavelaars, J. J.
Petit, Jean-Marc
Gladman, Brett J.
Gwyn, Stephen D. J.
Chen, Ying-Tung
Volk, Kathryn
Alexandersen, Mike
Benecchi, Susan D.
Delsanti, Audrey
Fraser, Wesley C.
Granvik, Mikael
Grundy, Will M.
Guilbert-Lepoutre, Aurelie
Hestroffer, Daniel
Ip, Wing-Huen
Jakubik, Marian
Jones, R. Lynne
Kaib, Nathan
Kavelaars, Catherine F.
Lacerda, Pedro
Lawler, Samantha
Lehner, Matthew J.
Lin, Hsing Wen
Lister, Tim
Lykawka, Patryk Sofia
Monty, Stephanie
Marsset, Michael
Murray-Clay, Ruth
Noll, Keith S.
Parker, Alex
Pike, Rosemary E.
Rousselot, Philippe
Rusk, David
Schwamb, Megan E.
Shankman, Cory
Sicardy, Bruno
Vernazza, Pierre
Wang, Shiang-Yu
TI THE OUTER SOLAR SYSTEM ORIGINS SURVEY. I. DESIGN AND FIRST-QUARTER
DISCOVERIES
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE Kuiper Belt: general; surveys
ID KUIPER-BELT OBJECTS; ABSOLUTE MAGNITUDE DISTRIBUTION; TRANS-NEPTUNIAN
POPULATIONS; SIZE DISTRIBUTION; DATA RELEASE; DYNAMICAL CLASSIFICATION;
ORBITAL STRUCTURE; SCATTERED DISK; PLANE; SEARCH
AB We report the discovery, tracking, and detection circumstances for 85 trans-Neptunian objects (TNOs) from the first 42 deg(2) of the Outer Solar System Origins Survey. This ongoing r-band solar system survey uses the 0.9 deg(2) field of view MegaPrime camera on the 3.6m Canada-France-Hawaii Telescope. Our orbital elements for these TNOs are precise to a fractional semimajor axis uncertainty <0.1%. We achieve this precision in just two oppositions, as compared to the normal three to five oppositions, via a dense observing cadence and innovative astrometric technique. These discoveries are free of ephemeris bias, a first for large trans-Neptunian surveys. We also provide the necessary information to enable models of TNO orbital distributions to be tested against our TNO sample. We confirm the existence of a cold "kernel" of objects within the main cold classical Kuiper Belt and infer the existence of an extension of the "stirred" cold classical Kuiper Belt to at least several au beyond the 2:1 mean motion resonance with Neptune. We find that the population model of Petit et al. remains a plausible representation of the Kuiper Belt. The full survey, to be completed in 2017, will provide an exquisitely characterized sample of important resonant TNO populations, ideal for testing models of giant planet migration during the early history of the solar system.
C1 [Bannister, Michele T.; Kavelaars, J. J.; Kavelaars, Catherine F.; Monty, Stephanie; Pike, Rosemary E.; Rusk, David; Shankman, Cory] Univ Victoria, Dept Phys & Astron, Elliott Bldg,3800 Finnerty Rd, Victoria, BC V8P 5C2, Canada.
[Bannister, Michele T.; Kavelaars, J. J.; Gwyn, Stephen D. J.; Lawler, Samantha] Natl Res Council Canada, NRC Herzberg Astron & Astrophys, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada.
[Petit, Jean-Marc; Rousselot, Philippe] Univ Bourgogne Franche Comte, CNRS, Inst UTINAM UMR6213, OSU Theta, F-25000 Besancon, France.
[Gladman, Brett J.; Alexandersen, Mike] Univ British Columbia, Dept Phys & Astron, Vancouver, BC, Canada.
[Chen, Ying-Tung; Alexandersen, Mike; Lehner, Matthew J.; Schwamb, Megan E.; Wang, Shiang-Yu] Acad Sinica, Inst Astron & Astrophys, 1 Roosevelt Rd,Sec 4, Taipei 10617, Taiwan.
[Chen, Ying-Tung; Alexandersen, Mike; Lehner, Matthew J.; Schwamb, Megan E.; Wang, Shiang-Yu] Natl Taiwan Univ, AS NTU11F, 1 Roosevelt Rd,Sec 4, Taipei 10617, Taiwan.
[Volk, Kathryn] Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab, 1629 Univ Blvd, Tucson, AZ 85721 USA.
[Benecchi, Susan D.] Planetary Sci Inst, 1700 East Ft Lowell,Suite 106, Tucson, AZ 85719 USA.
[Delsanti, Audrey] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France.
[Fraser, Wesley C.; Lacerda, Pedro] Queens Univ Belfast, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.
[Granvik, Mikael] Univ Helsinki, Dept Phys, POB 64, FI-00014 Helsinki, Finland.
[Granvik, Mikael] Finnish Geospatial Res Inst, POB 15, FI-02430 Masala, Finland.
[Grundy, Will M.] Lowell Observ, 1400 W Mars Hill Rd, Flagstaff, AZ 86001 USA.
[Hestroffer, Daniel] Univ Lille 1, Univ Paris 06, CNRS, IMCCE,Observ Paris,PSL Res Univ, F-75014 Paris, France.
[Ip, Wing-Huen; Lin, Hsing Wen] Natl Cent Univ, Inst Astron, Taoyuan, Taiwan.
[Ip, Wing-Huen] Macau Univ Sci & Technol, Space Sci Inst, Macau, Peoples R China.
[Jakubik, Marian] Slovak Acad Sci, Astron Inst, Tatranska Lomnica 05960, Slovakia.
[Jones, R. Lynne] Univ Washington, Washington, DC USA.
[Kaib, Nathan] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Lehner, Matthew J.] Univ Penn, Dept Phys & Astron, 209 S 33rd St, Philadelphia, PA 19104 USA.
Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Lehner, Matthew J.; Lister, Tim] Las Cumbres Observ Global Telescope Network Inc, 6740 Cortona Dr Suite 102, Goleta, CA 93117 USA.
[Lykawka, Patryk Sofia] Kinki Univ, Sch Interdisciplinary Social & Human Sci, Astron Grp, Higashiosaka, Osaka 577, Japan.
[Marsset, Michael] ESO, Alonso de Cordova 3107,1900 Casilla Vitacura, Santiago, Chile.
[Murray-Clay, Ruth] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Noll, Keith S.] NASA, Goddard Space Flight Ctr, Code 693, Greenbelt, MD 20771 USA.
[Parker, Alex] Southwest Res Inst, Boulder, CO USA.
[Sicardy, Bruno] Univ Paris 06, Univ Paris Diderot, CNRS UMR 8109, LESIA,Observ Paris, 5 Pl Jules Janssen, F-92195 Meudon, France.
RP Bannister, MT (reprint author), Univ Victoria, Dept Phys & Astron, Elliott Bldg,3800 Finnerty Rd, Victoria, BC V8P 5C2, Canada.
EM micheleb@uvic.ca
OI Volk, Kathryn/0000-0001-8736-236X; Bannister,
Michele/0000-0003-3257-4490; Sofia Lykawka, Patryk/0000-0003-0926-2448
FU National Research Council of Canada; National Science and Engineering
Research Council of Canada; Academia Sinica Postdoctoral Fellowship
FX This research was supported by funding from the National Research
Council of Canada and the National Science and Engineering Research
Council of Canada. This project could not have been a success without
the dedicated staff of the Canada France Hawaii telescope. The authors
recognize and acknowledge the sacred nature of Maunakea, and appreciate
the opportunity to observe from the mountain. This research has made use
of NASA's Astrophysics Data System, GNU parallel (Tange 2011), and many
Python packages, particularly astropy (The Astropy Collaboration et al.
2013), matplotlib (Hunter 2007) and SciPy (Jones et al. 2001); we thank
their contributors for their open-source efforts. MES is supported in
part by an Academia Sinica Postdoctoral Fellowship. Based on
observations obtained with MegaPrime/MegaCam, a joint project of the
Canada France Hawaii Telescope (CFHT) and CEA/DAPNIA, at CFHT which is
operated by the National Research Council (NRC) of Canada, the Institute
National des Sciences de l'universe of the Centre National de la
Recherche Scientifique (CNRS) of France, and the University of Hawaii.
This work is based in part on data produced and hosted at the Canadian
Astronomy Data Centre.
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD SEP
PY 2016
VL 152
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PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW7AV
UT WOS:000383804300018
ER
PT J
AU McCandliss, SR
Feldman, PD
Weaver, H
Fleming, B
Redwine, K
Li, MJ
Kutyrev, A
Moseley, SH
AF McCandliss, Stephan R.
Feldman, Paul D.
Weaver, Harold
Fleming, Brian
Redwine, Keith
Li, Mary J.
Kutyrev, Alexander
Moseley, S. Harvey
TI FAR-ULTRAVIOLET OBSERVATIONS OF COMET C/2012 S1 (ISON) FROM FORTIS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE general; comets: individual (C/2012 S1 (ISON), C/2001 Q4 (NEAT), C/2004
Q2 (MACHHOLZ)); molecular processes; Oort Cloud
ID SPECTROSCOPY; EVOLUTION; HYDROGEN
AB We have used the unique far-UV imaging capability offered by a sounding-rocket-borne instrument to acquire observations of C/2012 S1 (ISON) when its angular separation with respect to the Sun was 26.degrees 3 on 2013 November 20.49. At the time of observation, the comet's heliocentric distance and velocity relative to the Sun were r(h) = 0.43 au and (r) over dot(h) = -62.7 km s(-1). Images dominated by C I lambda 1657 and H I lambda 1216 were acquired over a 10(6) x 10(6) km(2) region. The water production rate implied by the Ly alpha observations is constrained to be Q(H2O)approximate to 8 x 10(29) s(-1) while the neutral carbon production rate was Q(C) approximate to 4 x 10(28) s(-1). The radial profile of C I was consistent with it being a dissociation product of a parent molecule with a lifetime tau similar to 5 x 10(4) s, favoring a parent other than CO. We constrain the Q(CO) production rate to 5(-7.5)(+1.5) x 10(28) s(-1) with 1 sigma errors derived from photon statistics. The upper limit on the Q(CO)/Q(H2O) is less than or similar to 6%.
C1 [McCandliss, Stephan R.; Feldman, Paul D.; Redwine, Keith] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Weaver, Harold] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Fleming, Brian] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Li, Mary J.; Kutyrev, Alexander; Moseley, S. Harvey] Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP McCandliss, SR (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
EM stephan@pha.jhu.edu
OI Feldman, Paul/0000-0002-9318-259X
FU Johns Hopkins University through NASA [NNX11AG54G, NNX14A178G]
FX The authors would like to acknowledge the sacrifices made by the
personnel associated with the NASA Sounding Rocket Program Office, their
Contractors, the Navy Launcher Team, and the Army Range Control at White
Sands Missile Range, all of whom showed exemplary dedication in carrying
out this time critical mission. We would also like to acknowledge the
innumerable, essential, and critical contributions of our JHU project
engineer, Russell Pelton, in providing support to this mission. Funding
for this work was provided to the Johns Hopkins University through NASA
sounding rocket grants No. NNX11AG54G and NNX14A178G.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD SEP
PY 2016
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AR 65
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PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW7AV
UT WOS:000383804300013
ER
PT J
AU Nugent, CR
Mainzer, A
Bauer, J
Cutri, RM
Kramer, EA
Grav, T
Masiero, J
Sonnett, S
Wright, EL
AF Nugent, C. R.
Mainzer, A.
Bauer, J.
Cutri, R. M.
Kramer, E. A.
Grav, T.
Masiero, J.
Sonnett, S.
Wright, E. L.
TI NEOWISE REACTIVATION MISSION YEAR TWO: ASTEROID DIAMETERS AND ALBEDOS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE minor planets, asteroids: general; surveys
ID MAIN-BELT ASTEROIDS; NEAR-EARTH OBJECTS; THERMAL-MODEL CALIBRATION;
INFRARED-SURVEY-EXPLORER; WISE/NEOWISE OBSERVATIONS; ABSOLUTE
MAGNITUDES; POPULATION; PERFORMANCE; FAMILIES; IDENTIFICATION
AB The Near-Earth Object Wide-Field Infrared Survey Explorer (NEOWISE) mission continues to detect, track, and characterize minor planets. We present diameters and albedos calculated from observations taken during the second year since the spacecraft was reactivated in late 2013. These include 207 near-Earth asteroids (NEAs) and 8885 other asteroids. Of the NEAs, 84% NEAs did not have previously measured diameters and albedos by the NEOWISE mission. Comparison of sizes and albedos calculated from NEOWISE measurements with those measured by occultations, spacecraft, and radar-derived shapes shows accuracy consistent with previous NEOWISE publications. Diameters and albedos fall within +/-similar to 20% and +/-similar to 40%, 1-sigma, respectively, of those measured by these alternate techniques. NEOWISE continues to preferentially discover near-Earth objects which are large (>100 m), and have low albedos.
C1 [Nugent, C. R.; Cutri, R. M.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Mainzer, A.; Bauer, J.; Kramer, E. A.; Masiero, J.; Sonnett, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Grav, T.] Planetary Sci Inst, Tucson, AZ USA.
[Wright, E. L.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
RP Nugent, CR (reprint author), CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
EM cnugent@ipac.caltech.edu
OI Cutri, Roc/0000-0002-0077-2305
FU NASA; Planetary Science Division of NASA; JPL Office of the CIO; 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; Collaborating
Institutions in the Dark Energy Survey; Ministerio da Ciencia,
Tecnologia e Inovacao (Brazil) [GS-2015A-LP-3, GS-2015B-LP-3]
FX 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 JPL/California Institute of Technology,
funded by NASA. This publication also makes use of data products from
NEOWISE, which is a project of the JPL/California Institute of
Technology, funded by the Planetary Science Division of NASA. The JPL
High Performance Computing Facility used for our simulations is
supported by the JPL Office of the CIO.; This project used data obtained
with the Dark Energy Camera (DECam), which was constructed by the Dark
Energy Survey (DES) collaboration. 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 Dark Energy Survey. 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.; This
publication makes use of 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).
Observing Program IDs: GS-2015A-LP-3, GS-2015B-LP-3.
NR 55
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW7AV
UT WOS:000383804300011
ER
PT J
AU Schneider, G
Grady, CA
Stark, CC
Gaspar, A
Carson, J
Debes, JH
Henning, T
Hines, DC
Jang-Condell, H
Kuchner, MJ
Perrin, M
Rodigas, TJ
Tamura, M
Wisniewski, JP
AF Schneider, Glenn
Grady, Carol A.
Stark, Christopher C.
Gaspar, Andras
Carson, Joseph
Debes, John H.
Henning, Thomas
Hines, Dean C.
Jang-Condell, Hannah
Kuchner, Marc J.
Perrin, Marshall
Rodigas, Timothy J.
Tamura, Motohide
Wisniewski, John P.
TI DEEP HST/STIS VISIBLE-LIGHT IMAGING OF DEBRIS SYSTEMS AROUND SOLAR
ANALOG HOSTS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE methods: observational; planet-disk interactions; stars: individual (HD
207129, HD 202628, HD 202917); stars: solar-type
ID MAIN-SEQUENCE STARS; INTERSTELLAR-MEDIUM; HD 207129; SPACE-TELESCOPE;
MOVING GROUP; DISK; PLANETS; RING; DUST; AGE
AB We present new Hubble Space Telescope observations of three a priori known starlight-scattering circumstellar debris systems (CDSs) viewed at intermediate inclinations around nearby close-solar analog stars: HD 207129, HD 202628, and HD 202917. Each of these CDSs possesses ring-like components that are more massive analogs of our solar system's Edgeworth-Kuiper Belt. These systems were chosen for follow-up observations to provide imaging with higher fidelity and better sensitivity for the sparse sample of solar-analog CDSs that range over two decades in systemic ages, with HD 202628 and HD 207129 (both similar to 2.3 Gyr) currently the oldest CDSs imaged in visible or near-IR light. These deep (10-14 ks) observations, made with six-roll point-spread-function template visible-light coronagraphy. using the Space Telescope Imaging Spectrograph, were designed to better reveal their angularly large debris rings of diffuse/low surface brightness, and for all targets probe their exo-ring environments for starlight-scattering materials that present observational challenges for current ground-based facilities and instruments. Contemporaneously also observing with a narrower occulter position, these observations additionally probe the CDS endo-ring environments that are seen to be relatively devoid of scatterers. We discuss the morphological, geometrical, and photometric properties of these CDSs also in the context of other CDSs hosted by FGK stars that we have previously imaged as a homogeneously observed ensemble. From this combined sample we report a general decay in quiescent-disk F-disk/F-star optical brightness similar to t(-0.8), similar to what is seen at thermal IR wavelengths, and CDSs with a significant diversity in scattering phase asymmetries, and spatial distributions of their starlight-scattering grains.
C1 [Schneider, Glenn; Gaspar, Andras] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.
[Schneider, Glenn; Gaspar, Andras] Univ Arizona, Dept Astron, 933 North Cherry Ave, Tucson, AZ 85721 USA.
[Grady, Carol A.] Eureka Sci, 2452 Delmer,Suite 100, Oakland, CA 96002 USA.
[Stark, Christopher C.; Kuchner, Marc J.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 20771 USA.
[Carson, Joseph] Coll Charleston, Dept Phys & Astron, 66 George St, Charleston, SC 29424 USA.
[Debes, John H.; Hines, Dean C.; Perrin, Marshall] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Henning, Thomas] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Jang-Condell, Hannah] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA.
[Rodigas, Timothy J.] Carnegie Inst Sci, Dept Terr Magnetism, 5241 Branch Rd NW, Washington, DC 20015 USA.
[Tamura, Motohide] Univ Tokyo, Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
[Wisniewski, John P.] Univ Oklahoma, HL Dodge Dept Phys & Astron, 440 West Brooks St, Norman, OK 73019 USA.
RP Schneider, G (reprint author), Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA.; Schneider, G (reprint author), Univ Arizona, Dept Astron, 933 North Cherry Ave, Tucson, AZ 85721 USA.
EM gschneider@as.arizona.edu
OI Gaspar, Andras/0000-0001-8612-3236
FU Association of Universities for Research in Astronomy, Inc., under NASA
[NAS 5-26555]; NASA through STScI [13786]; South Carolina Space Grant
Consortium; [12228]
FX Based on observations made with the NASA/ESA Hubble Space Telescope,
obtained at the Space Telescope Science Institute (STScI), which is
operated by the Association of Universities for Research in Astronomy,
Inc., under NASA contract NAS 5-26555. These observations are associated
with programs #13786 and 12228. Support for program #13786 was provided
by NASA through a grant from STScI. J. Carson acknowledges support from
the South Carolina Space Grant Consortium.
NR 42
TC 0
Z9 0
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD SEP
PY 2016
VL 152
IS 3
AR 64
DI 10.3847/0004-6256/152/3/64
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW7AV
UT WOS:000383804300012
ER
PT J
AU Hinkel, NR
Young, PA
Pagano, MD
Desch, SJ
Anbar, AD
Adibekyan, V
Blanco-Cuaresma, S
Carlberg, JK
Mena, ED
Liu, F
Nordlander, T
Sousa, SG
Korn, A
Gruyters, P
Heiter, U
Jofre, P
Santos, NC
Soubiran, C
AF Hinkel, Natalie R.
Young, Patrick A.
Pagano, Michael D.
Desch, Steven J.
Anbar, Ariel D.
Adibekyan, Vardan
Blanco-Cuaresma, Sergi
Carlberg, Joleen K.
Mena, Elisa Delgado
Liu, Fan
Nordlander, Thomas
Sousa, Sergio G.
Korn, Andreas
Gruyters, Pieter
Heiter, Ulrike
Jofre, Paula
Santos, Nuno C.
Soubiran, Caroline
TI A COMPARISON OF STELLAR ELEMENTAL ABUNDANCE TECHNIQUES AND MEASUREMENTS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE stars: abundances; stars: individual (HD 361, HD 10700, HD 121504, HD
202206); techniques: spectroscopic
ID METAL-POOR STARS; PLANET-HOST STARS; GENEVA-COPENHAGEN SURVEY; GALACTIC
CHEMICAL EVOLUTION; NEUTRAL HYDROGEN COLLISIONS; I OSCILLATOR-STRENGTHS;
SOLAR-TYPE STARS; WAY THICK DISK; DWARF STARS; OXYGEN ABUNDANCES
AB Stellar elemental abundances are important for understanding the fundamental properties of a star or stellar group, such as age and evolutionary history, as well as the composition of an orbiting planet. However, as abundance measurement techniques have progressed, there has been little standardization between individual methods and their comparisons. As a result, different stellar abundance procedures determine measurements that vary beyond the quoted error for the same elements within the same stars. The purpose of this paper is to better understand the systematic variations between methods and offer recommendations for producing more accurate results in the future. We invited a number of participants from around the world (Australia, Portugal, Sweden, Switzerland, and the United States) to calculate 10 element abundances (C, O, Na, Mg, Al, Si, Fe, Ni, Ba, and Eu) using the same stellar spectra for four stars (HD 361, HD 10700, HD 121504, and HD 202206). Each group produced measurements for each star using (1) their own autonomous techniques, (2) standardized stellar parameters, (3) a standardized line list, and (4) both standardized parameters and a line list. We present the resulting stellar parameters, absolute abundances, and a metric of data similarity that quantifies the homogeneity of the data. We conclude that standardization of some kind, particularly stellar parameters, improves the consistency between methods. However, because results did not converge as more free parameters were standardized, it is clear there are inherent issues within the techniques that need to be reconciled. Therefore, we encourage more conversation and transparency within the community such that stellar abundance determinations can be reproducible as well as accurate and precise.
C1 [Hinkel, Natalie R.; Young, Patrick A.; Pagano, Michael D.; Desch, Steven J.; Anbar, Ariel D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Adibekyan, Vardan; Mena, Elisa Delgado; Sousa, Sergio G.; Santos, Nuno C.] Univ Porto, Inst Astrofis & Ciencias Espaco, CAUP, Rua Estrelas, P-4150762 Oporto, Portugal.
[Blanco-Cuaresma, Sergi] Univ Geneva, Observ Geneve, CH-1290 Versoix, Switzerland.
[Carlberg, Joleen K.] NASA, Goddard Space Flight Ctr, Code 667, Greenbelt, MD 20771 USA.
[Carlberg, Joleen K.] Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA.
[Liu, Fan] Australian Natl Univ, Res Sch Astron & Astrophys, Cotter Rd, Weston, ACT 2611, Australia.
[Nordlander, Thomas; Korn, Andreas; Gruyters, Pieter; Heiter, Ulrike] Uppsala Univ, Dept Phys & Astron, Box 516, S-75120 Uppsala, Sweden.
[Gruyters, Pieter] Lund Observ, Dept Astron & Theoret Phys, Box 43, S-22100 Lund, Sweden.
[Jofre, Paula] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Santos, Nuno C.] Univ Porto, Fac Ciencias, Dept Fis & Astron, Rua Campo Alegre, P-4169007 Oporto, Portugal.
[Soubiran, Caroline] Univ Bordeaux, CNRS, LAB, UMR 5804, F-33270 Floirac, France.
RP Hinkel, NR (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
EM natalie.hinkel@gmail.com
FU NASA's Science Mission Directorate; Fundacao para a Ciencia e Tecnologia
(FCT, Portugal) [SFRH/BPD/76606/2011, SFRH/BPD/70574/2010]; Swedish
National Space Board (SNSB); FCT [IF/00169/2012, IF/00028/2014,
PTDC/FIS-AST/7073/2014 (POCI-01-0145-FEDER-007672),
PTDC/FIS-AST/1526/2014]; POPH/FSE (EC) by FEDER funding through the
program "Programa Operacional de Factores de Competitividade"
FX The authors would like to thank Paul Butler for providing the original
stellar spectra in addition to Eric Mamajek for his help determining
accurate stellar types for our sample. They would also like to thank the
anonymous referee for support and guidance, which has greatly improved
the manuscript. NRH would like to thank CHW3. The ASU team (NRH, PAY,
MDP, SJD, and ADA) acknowledge that the results reported herein
benefited from collaborations and/or information exchange within NASA's
Nexus for Exoplanet System Science (NExSS) research coordination network
sponsored by NASA's Science Mission Directorate. EDM and VA acknowledge
the support from the Fundacao para a Ciencia e Tecnologia (FCT,
Portugal) in the form of the grants SFRH/BPD/76606/2011 and
SFRH/BPD/70574/2010, respectively. JKC acknowledges partial support from
an appointment to the NASA Postdoctoral Program at the Goddard Space
Flight Center, administered by Universities Space Research Association
through a contract with NASA. TN, AK, and UH acknowledge support by the
Swedish National Space Board (SNSB). NCS and SGS acknowledge the support
from FCT through Investigador FCT contracts of reference IF/00169/2012
and IF/00028/2014, respectively, and POPH/FSE (EC) by FEDER funding
through the program "Programa Operacional de Factores de
Competitividade." The Porto group also acknowledges the support from FCT
in the form of grant reference PTDC/FIS-AST/7073/2014
(POCI-01-0145-FEDER-007672) and project PTDC/FIS-AST/1526/2014. This
research has made use of the SIMBAD database and VizieR catalog access
tools operated at CDS, Strasbourg, France, as well as the Exoplanet
Orbit Database at exoplanets.org.
NR 179
TC 1
Z9 1
U1 3
U2 3
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 SEP
PY 2016
VL 226
IS 1
AR 4
DI 10.3847/0067-0049/226/1/4
PG 66
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW9XF
UT WOS:000384015400004
ER
PT J
AU Paganini, L
Mumma, MJ
AF Paganini, L.
Mumma, M. J.
TI A SOLAR-PUMPED FLUORESCENCE MODEL FOR LINE-BY-LINE EMISSION INTENSITIES
IN THE B-X, A-X, AND X-X BAND SYSTEMS OF (CN)-C-12-N-14
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE astronomical databases: miscellaneous; comets: general; molecular data;
molecular processes; comets: individual; C/2014 Q2 (Lovejoy);
techniques: spectroscopic
ID OH PROMPT EMISSION; CHEMICAL-COMPOSITION; VIOLET SYSTEMS; COMETS; CN;
SPECTRUM; CYANOGEN; WATER; EXCITATION; MOLECULES
AB We present a new quantitative model for detailed solar-pumped fluorescent emission of the main isotopologue of CN. The derived fluorescence efficiencies permit estimation and interpretation of ro-vibrational infrared line intensities of CN in exospheres exposed to solar (or stellar) radiation. Our g-factors are applicable to astronomical observations of CN extending from infrared to optical wavelengths, and we compare them with previous calculations in the literature. The new model enables extraction of rotational temperature, column abundance, and production rate from astronomical observations of CN in the inner coma of comets. Our model accounts for excitation and de-excitation of rotational levels in the ground vibrational state by collisions, solar excitation to the A(2)Pi(i) and B-2 Sigma(+) electronically excited states followed by cascade to ro-vibrational levels of X-2 Sigma(+), and direct solar infrared pumping of ro-vibrational levels in the X-2 Sigma(+) state. The model uses advanced solar spectra acquired at high spectral resolution at the relevant infrared and optical wavelengths and considers the heliocentric radial velocity of the comet (the Swings effect) when assessing the exciting solar flux for a given transition. We present model predictions for the variation of fluorescence rates with rotational temperature and heliocentric radial velocity. Furthermore, we test our fluorescence model by comparing predicted and measured line-by-line intensities for X-2 Sigma(+) (1-0) in comet C/2014 Q2 (Lovejoy), thereby identifying multiple emission lines observed at IR wavelengths.
C1 [Paganini, L.; Mumma, M. J.] NASA, Goddard Ctr Astrobiol, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Paganini, L.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Paganini, L (reprint author), NASA, Goddard Ctr Astrobiol, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Paganini, L (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
FU NASA's Planetary Astronomy Program; Keck PI Data Award
FX The authors would like to thank David Schleicher and James S. A. Brooke
for interesting insights about this work. We also acknowledge support by
NASA's Planetary Astronomy Program (L.P., M.J.M.) and Keck PI Data Award
(L.P.), administered by the NASA Exoplanet Science Institute. Data were
obtained at the W. M. Keck Observatory from telescope time allocated to
the National Aeronautics and Space Administration through the agency's
scientific partnership with the California Institute of Technology and
the University of California. 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.
NR 61
TC 0
Z9 0
U1 1
U2 1
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 SEP
PY 2016
VL 226
IS 1
AR 3
DI 10.3847/0067-0049/226/1/3
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DW9XF
UT WOS:000384015400003
ER
PT J
AU Haarig, M
Engelmann, R
Ansmann, A
Veselovskii, I
Whiteman, DN
Althausen, D
AF Haarig, Moritz
Engelmann, Ronny
Ansmann, Albert
Veselovskii, Igor
Whiteman, David N.
Althausen, Dietrich
TI 1064 nm rotational Raman lidar for particle extinction and lidar-ratio
profiling: cirrus case study
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID SPECTRAL-RESOLUTION LIDAR; ELASTIC-BACKSCATTER LIDAR; INDIAN AEROSOL
PLUME; MULTIWAVELENGTH LIDAR; WATER-VAPOR; SAHARAN DUST;
PHYSICAL-PROPERTIES; 6-WAVELENGTH LIDAR; OPTICAL-PROPERTIES; RETRIEVAL
AB For the first time, vertical profiles of the 1064 nm particle extinction coefficient obtained from Raman lidar observations at 1058 nm (nitrogen and oxygen rotational Raman backscatter) are presented. We applied the new technique in the framework of test measurements and performed several cirrus observations of particle backscatter and extinction coefficients, and corresponding extinctiont-o-backscatter ratios at the wavelengths of 355, 532, and 1064 nm. The cirrus backscatter coefficients were found to be equal for all three wavelengths keeping the retrieval uncertainties in mind. The multiple-scattering-corrected cirrus extinction coefficients at 355 nm were on average about 20-30% lower than the ones for 532 and 1064 nm. The cirrus-mean extinction-to-backscatter ratio (lidar ratio) was 31 +/- 5 sr (355 nm), 36 +/- 5 sr (532 nm), and 38 +/- 5 sr (1064 nm) in this single study. We further discussed the requirements needed to obtain aerosol extinction profiles in the lower troposphere at 1064 nm with good accuracy (20% relative uncertainty) and appropriate temporal and vertical resolution.
C1 [Haarig, Moritz; Engelmann, Ronny; Ansmann, Albert; Althausen, Dietrich] Leibniz Inst Tropospher Res, Leipzig, Germany.
[Veselovskii, Igor] Phys Instrumentat Ctr, Moscow, Russia.
[Whiteman, David N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Haarig, M (reprint author), Leibniz Inst Tropospher Res, Leipzig, Germany.
EM haarig@tropos.de
FU Russian Science Foundation [16-17-10241]
FX We thank Johannes Buhl for providing Doppler lidar observations of
vertical velocity and estimated ice crystal sizes. Modeling of the
rotational Raman filter parameters was supported by the Russian Science
Foundation (project no. 16-17-10241).
NR 63
TC 0
Z9 0
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 SEP 1
PY 2016
VL 9
IS 9
BP 4269
EP 4278
DI 10.5194/amt-9-4269-2016
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW8LC
UT WOS:000383906300001
ER
PT J
AU Colman, DR
Feyhl-Buska, J
Fecteau, KM
Xu, HF
Shock, EL
Boyd, ES
AF Colman, Daniel R.
Feyhl-Buska, Jayme
Fecteau, Kristopher M.
Xu, Huifang
Shock, Everett L.
Boyd, Eric S.
TI Ecological differentiation in planktonic and sediment-associated
chemotrophic microbial populations in Yellowstone hot springs
SO FEMS MICROBIOLOGY ECOLOGY
LA English
DT Article
DE Yellowstone hot springs; chemotroph; thermophiles; archaea; Aquificales;
ecological differentiation
ID STREAMER BIOFILM COMMUNITIES; NATIONAL-PARK; GEOTHERMAL SPRINGS;
RIBOSOMAL-RNA; SP-NOV; HIGH-TEMPERATURE; GLOBAL PATTERNS; GEN. NOV.;
DIVERSITY; SULFUR
AB Chemosynthetic sediment and planktonic community composition and sizes, aqueous geochemistry and sediment mineralogy were determined in 15 non-photosynthetic hot springs in Yellowstone National Park (YNP). These data were used to evaluate the hypothesis that differences in the availability of dissolved or mineral substrates in the bulk fluids or sediments within springs coincides with ecologically differentiated microbial communities and their populations. Planktonic and sediment-associated communities exhibited differing ecological characteristics including community sizes, evenness and richness. pH and temperature influenced microbial community composition among springs, but within-spring partitioning of taxa into sediment or planktonic communities was widespread, statistically supported (P < 0.05) and could be best explained by the inferred metabolic strategies of the partitioned taxa. Microaerophilic genera of the Aquificales predominated in many of the planktonic communities. In contrast, taxa capable of mineral-based metabolism such as S-o oxidation/reduction or Fe-oxide reduction predominated in sediment communities. These results indicate that ecological differentiation within thermal spring habitats is common across a range of spring geochemistry and is influenced by the availability of dissolved nutrients and minerals that can be used in metabolism.The presence of minerals, such as elemental sulfur, that can support microbial metabolism promotes the ecological differentiation of sediment- and planktonic-associated microbial populations within Yellowstone National Park hot springs.The presence of minerals, such as elemental sulfur, that can support microbial metabolism promotes the ecological differentiation of sediment- and planktonic-associated microbial populations within Yellowstone National Park hot springs.
C1 [Colman, Daniel R.; Feyhl-Buska, Jayme; Boyd, Eric S.] Montana State Univ, Dept Microbiol & Immunol, POB 173520, Bozeman, MI 59717 USA.
[Fecteau, Kristopher M.; Shock, Everett L.] Arizona State Univ, Dept Chem & Biochem, Tempe, AZ 85287 USA.
[Xu, Huifang] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.
[Xu, Huifang; Shock, Everett L.; Boyd, Eric S.] NASA, Astrobiol Inst, Mountain View, CA 94035 USA.
[Shock, Everett L.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
RP Boyd, ES (reprint author), Montana State Univ, Dept Microbiol & Immunol, POB 173520, Bozeman, MI 59717 USA.
EM eboyd@montana.edu
FU National Aeronautics and Space Administration (NASA) Exobiology and
Evolutionary Biology [NNX13AI11G]; [EAR- 1529963]; [NNA15BB02A];
[NNA13AA94A]
FX This work was supported by a National Aeronautics and Space
Administration (NASA) Exobiology and Evolutionary Biology [grant number
NNX13AI11G] grant to ESB and a National Science Foundation grant [grant
number EAR- 1529963] to ELS. The NASA Astrobiology Institute is
supported by grant numbers NNA15BB02A (to ELS and ESB) and NNA13AA94A
(to HX and ESB).
NR 72
TC 1
Z9 1
U1 8
U2 8
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0168-6496
EI 1574-6941
J9 FEMS MICROBIOL ECOL
JI FEMS Microbiol. Ecol.
PD SEP
PY 2016
VL 92
IS 9
AR fiw137
DI 10.1093/femsec/fiw137
PG 13
WC Microbiology
SC Microbiology
GA DW8IL
UT WOS:000383898400011
ER
PT J
AU van Vliet, MTH
van Beek, LPH
Eisner, S
Florke, M
Wada, Y
Bierkens, MFP
AF van Vliet, M. T. H.
van Beek, L. P. H.
Eisner, S.
Floerke, M.
Wada, Y.
Bierkens, M. F. P.
TI Multi-model assessment of global hydropower and cooling water discharge
potential under climate change
SO GLOBAL ENVIRONMENTAL CHANGE-HUMAN AND POLICY DIMENSIONS
LA English
DT Article
DE Water resources; Water temperature; Hydropower; Cooling water; Climate
change; Global hydrological models
ID PACIFIC-NORTHWEST; POWER-GENERATION; CHANGE IMPACTS; MODEL; ELECTRICITY;
VALIDATION; TEMPERATURE; RESOURCES; HYDROLOGY; SCALE
AB Worldwide, 98% of total electricity is currently produced by thermoelectric power and hydropower. Climate change is expected to directly impact electricity supply, in terms of both water availability for hydropower generation and cooling water usage for thermoelectric power. Improved understanding of how climate change may impact the availability and temperature of water resources is therefore of major importance. Here we use a multi-model ensemble to show the potential impacts of climate change on global hydropower and cooling water discharge potential. For the first time, combined projections of streamflow and water temperature were produced with three global hydrological models (GHMs) to account for uncertainties in the structure and parametrization of these GHMs in both water availability and water temperature. The GHMs were forced with bias-corrected output of five general circulation models (GCMs) for both the lowest and highest representative concentration pathways (RCP2.6 and RCP8.5). The ensemble projections of streamflow and water temperature were then used to quantify impacts on gross hydropower potential and cooling water discharge capacity of rivers worldwide. We show that global gross hydropower potential is expected to increase between +2.4% (GCM-GHM ensemble mean for RCP 2.6) and +6.3% (RCP 8.5) for the 2080s compared to 1971-2000. The strongest increases in hydropower potential are expected for Central Africa, India, central Asia and the northern high-latitudes, with 18-33% of the world population living in these areas by the 2080s. Global mean cooling water discharge capacity is projected to decrease by 4.5-15% (2080s). The largest reductions are found for the United States, Europe, eastern Asia, and southern parts of South America, Africa and Australia, where strong water temperature increases are projected combined with reductions in mean annual streamflow. These regions are expected to affect 11-14% (for RCP2.6 and the shared socioeconomic pathway (SSP)1, SSP2, SSP4) and 41-51% (RCP8.5-SSP3, SSP5) of the world population by the 2080s. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [van Vliet, M. T. H.] Wageningen Univ, Water Syst & Global Change Grp, POB 47, NL-6700 AA Wageningen, Netherlands.
[van Vliet, M. T. H.; Wada, Y.] Int Inst Appl Syst Anal IIASA, Schlosspl 1, A-2361 Laxenburg, Austria.
[van Beek, L. P. H.; Wada, Y.; Bierkens, M. F. P.] Univ Utrecht, Dept Phys Geog, POB 80115, NL-3508 TC Utrecht, Netherlands.
[Eisner, S.; Floerke, M.] Univ Kassel, Ctr Environm Syst Res, Wilhelmshoher Allee 47, D-34109 Kassel, Germany.
[Wada, Y.] NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
[Wada, Y.] Columbia Univ, Ctr Climate Syst Res, 2880 Broadway, New York, NY 10025 USA.
[Bierkens, M. F. P.] Deltares, Soil & Groundwater Syst Unit, POB 80015, NL-3508 TA Utrecht, Netherlands.
RP van Vliet, MTH (reprint author), Wageningen Univ, Water Syst & Global Change Grp, POB 47, NL-6700 AA Wageningen, Netherlands.
EM michelle.vanvliet@wur.nl
RI van Beek, Rens/B-4904-2014
OI van Beek, Rens/0000-0002-4758-108X
FU Niels Stensen Fellowship; Veni-grant of NWO Earth and Life Sciences
(ALW) [863.14.008]
FX The Inter-Sectoral Impact Model Intercomparison Project (ISIMIP) is
kindly acknowledged for providing the bias-corrected general circulation
model output and gridded population projections for this study. Dr.
Michelle van Vliet was supported by a contribution from the Niels
Stensen Fellowship and a Veni-grant (project 863.14.008) of NWO Earth
and Life Sciences (ALW).
NR 58
TC 1
Z9 1
U1 8
U2 8
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0959-3780
EI 1872-9495
J9 GLOBAL ENVIRON CHANG
JI Glob. Environ. Change-Human Policy Dimens.
PD SEP
PY 2016
VL 40
BP 156
EP 170
DI 10.1016/j.gloenvcha.2016.07.007
PG 15
WC Environmental Sciences; Environmental Studies; Geography
SC Environmental Sciences & Ecology; Geography
GA DV9YD
UT WOS:000383297200014
ER
PT J
AU Holzmann, GJ
AF Holzmann, Gerard J.
TI Brace Yourself
SO IEEE SOFTWARE
LA English
DT Editorial Material
C1 [Holzmann, Gerard J.] Jet Prop Lab, Pasadena, CA 91125 USA.
RP Holzmann, GJ (reprint author), Jet Prop Lab, Pasadena, CA 91125 USA.
EM gholzmann@acm.org
NR 4
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 SEP-OCT
PY 2016
VL 33
IS 5
BP 34
EP 37
PG 4
WC Computer Science, Software Engineering
SC Computer Science
GA DV7DI
UT WOS:000383095900008
ER
PT J
AU Zhu, YY
Antao, DS
Chu, KH
Chen, SY
Hendricks, TJ
Zhang, TJ
Wang, EN
AF Zhu, Yangying
Antao, Dion S.
Chu, Kuang-Han
Chen, Siyu
Hendricks, Terry J.
Zhang, Tiejun
Wang, Evelyn N.
TI Surface Structure Enhanced Microchannel Flow Boiling
SO JOURNAL OF HEAT TRANSFER-TRANSACTIONS OF THE ASME
LA English
DT Article
DE microchannel flow boiling; surface microstructures; flow instabilities;
critical heat flux
ID CRITICAL HEAT-FLUX; PRESSURE-DROP; PIN FIN; MICROPILLAR ARRAYS; LIQUID;
PREDICTION; CHANNELS; REGIME; SINK
AB We investigated the role of surface microstructures in two-phase microchannels on suppressing flow instabilities and enhancing heat transfer. We designed and fabricated microchannels with well-defined silicon micropillar arrays on the bottom heated microchannel wall to promote capillary flow for thin film evaporation while facilitating nucleation only from the sidewalls. Our experimental results show significantly reduced temperature and pressure drop fluctuation especially at high heat fluxes. A critical heat flux (CHF) of 969 W/cm(2) was achieved with a structured surface, a 57% enhancement compared to a smooth surface. We explain the experimental trends for the CHF enhancement with a liquid wicking model. The results suggest that capillary flow can be maximized to enhance heat transfer via optimizing the microstructure geometry for the development of high performance two-phase microchannel heat sinks.
C1 [Zhu, Yangying; Antao, Dion S.; Chu, Kuang-Han; Chen, Siyu; Wang, Evelyn N.] MIT, Dept Mech Engn, Cambridge, MA 02139 USA.
[Hendricks, Terry J.] CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Zhang, Tiejun] Masdar Inst Sci & Technol, Dept Mech & Mat Engn, Bldg 1A,POB 54224, Abu Dhabi, U Arab Emirates.
RP Wang, EN (reprint author), MIT, Dept Mech Engn, Cambridge, MA 02139 USA.
EM yyzhu@mit.edu; dantao@mit.edu; flyjohn@gmail.com; chensiyu@mit.edu;
terry.j.hendricks@jpl.nasa.gov; tjzhang@masdar.ac.ae; enwang@mit.edu
FU Office of Naval Research (ONR) [N00014-15-1-2483]; Masdar Institute of
Science and Technology (Masdar Institute), Abu Dhabi, UAE
[02/MI/MI/CP/11/07633/GEN/G/00]; Massachusetts Institute of Technology
(MIT), Cambridge, MA [02/MI/MI/CP/11/07633/GEN/G/00]; Battelle Memorial
Institute; Air Force Office of Scientific Research (AFOSR);
Singapore-MIT Alliance for Research and Technology (SMART)
FX This work was partially funded by the Office of Naval Research (ONR)
with Dr. Mark Spector as program manager (N00014-15-1-2483), the
Cooperative Agreement between the Masdar Institute of Science and
Technology (Masdar Institute), Abu Dhabi, UAE and the Massachusetts
Institute of Technology (MIT), Cambridge, MA,-Reference
02/MI/MI/CP/11/07633/GEN/G/00, the Battelle Memorial Institute, the Air
Force Office of Scientific Research (AFOSR) and the Singapore-MIT
Alliance for Research and Technology (SMART). The research was
technically supported and encouraged by the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. The authors would also like to
acknowledge the MIT Microsystems Technology Lab for fabrication staff
support, help, and use of equipment.
NR 49
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U1 16
U2 16
PU ASME
PI NEW YORK
PA TWO PARK AVE, NEW YORK, NY 10016-5990 USA
SN 0022-1481
EI 1528-8943
J9 J HEAT TRANS-T ASME
JI J. Heat Transf.-Trans. ASME
PD SEP
PY 2016
VL 138
IS 9
AR 091501
DI 10.1115/1.4033497
PG 13
WC Thermodynamics; Engineering, Mechanical
SC Thermodynamics; Engineering
GA DW6TS
UT WOS:000383784700014
ER
PT J
AU Otto, SE
Trefny, CJ
Slater, JW
AF Otto, Samuel E.
Trefny, Charles J.
Slater, John W.
TI Inward-Turning Streamline-Traced Inlet Design Method Low-Boom Low-Drag
Applications
SO JOURNAL OF PROPULSION AND POWER
LA English
DT Article; Proceedings Paper
CT AIAA Propulsion and Energy Forum
CY JUL 27-29, 2015
CL Orlando, FL
SP AIAA
ID BUSEMANN-INLET; SPEEDS
AB A new design method for inward-turning streamline-traced inlets is presented. Resulting designs are intended for low-supersonic low-drag low-boom applications such as that required for NASA's proposed low-boom flight demonstration aircraft. A critical feature of these designs is the internal cowl lip angle that allows for little or no flow turning on the outer nacelle. Present methods using conical-flow Busemann parent flowfields have simply truncated, or otherwise modified, the stream-traced contours to include this internal cowl angle. Such modifications disrupt the parent flowfield, reducing inlet performance and flow uniformity. The method presented herein merges a conical flowfield that includes a leading shock with a truncated Busemann flowfield in a manner that minimizes unwanted interactions. A leading internal cowl angle is now inherent in the parent flowfield, and inlet contours traced from this flowfield retain its high performance and good flow uniformity. Computational fluid dynamics analysis of a candidate inlet design is presented that verifies the design technique, and it reveals a starting issue with the basic geometry. A minor modification to the cowl lip region is shown to eliminate this phenomenon, thereby allowing starting and smooth transition to subcritical operation as backpressure is increased. An inlet critical-point total pressure recovery of 96% is achieved based on computational fluid dynamics results for a Mach 1.7 freestream design. Correction for boundary-layer displacement thickness and sizing for a given engine airflow requirement are also discussed.
C1 [Otto, Samuel E.] Purdue Univ, Inlets & Nozzles Branch, W Lafayette, IN 47906 USA.
[Trefny, Charles J.; Slater, John W.] NASA, John H Glenn Res Ctr, Inlets & Nozzles Branch, 21000 Brookpark Rd Mail Stop 5-11, Cleveland, OH 44135 USA.
RP Otto, SE (reprint author), Purdue Univ, Inlets & Nozzles Branch, W Lafayette, IN 47906 USA.
NR 12
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U1 4
U2 4
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 SEP
PY 2016
VL 32
IS 5
BP 1178
EP 1189
DI 10.2514/1.B36028
PG 12
WC Engineering, Aerospace
SC Engineering
GA DW2MH
UT WOS:000383476000015
ER
PT J
AU Pokhrel, R
Gutermuth, R
Ali, B
Megeath, T
Pipher, J
Myers, P
Fischer, WJ
Henning, T
Wolk, SJ
Allen, L
Tobin, JJ
AF Pokhrel, R.
Gutermuth, R.
Ali, B.
Megeath, T.
Pipher, J.
Myers, P.
Fischer, W. J.
Henning, T.
Wolk, S. J.
Allen, L.
Tobin, J. J.
TI A Herschel-SPIRE survey of the Mon R2 giant molecular cloud: analysis of
the gas column density probability density function
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE ISM: clouds; ISM: individual objects: Mon R2; ISM: structure
ID YOUNG STELLAR CLUSTERS; GOULD BELT SURVEY; STAR-FORMATION; MONOCEROS R2;
INTERSTELLAR CLOUDS; REFLECTION NEBULAE; DUST TEMPERATURE; TURBULENCE;
ORION; RESOLUTION
AB We present a far-IR survey of the entire Mon R2 giant molecular cloud (GMC) with Herschel-Spectral and Photometric Imaging REceiver cross-calibrated with Planck-High Frequency Instrument data. We fit the spectral energy distributions of each pixel with a greybody function and an optimal beta value of 1.8. We find that mid-range column densities obtained from far-IR dust emission and near-IR extinction are consistent. For the entire GMC, we find that the column density histogram, or column density probability distribution function (N-PDF), is lognormal below similar to 10(21) cm(-2). Above this value, the distribution takes a power law form with an index of -2.15. We analyse the gas geometry, N-PDF shape, and young stellar object (YSO) content of a selection of subregions in the cloud. We find no regions with pure lognormal N-PDFs. The regions with a combination of lognormal and one power-law N-PDF have a YSO cluster and a corresponding centrally concentrated gas clump. The regions with a combination of lognormal and two power-law N-PDF have significant numbers of typically younger YSOs but no prominent YSO cluster. These regions are composed of an aggregate of closely spaced gas filaments with no concentrated dense gas clump. We find that for our fixed scale regions, the YSO count roughly correlates with the N-PDF power-law index. The correlation appears steeper for single power-law regions relative to two power-law regions with a high column density cut-off, as a greater dense gas mass fraction is achieved in the former. A stronger correlation is found between embedded YSO count and the dense gas mass among our regions.
C1 [Pokhrel, R.; Gutermuth, R.] Univ Massachusetts, Amherst, MA 01003 USA.
[Ali, B.] Space Sci Inst, Boulder, CO 80301 USA.
[Megeath, T.] Univ Toledo, 2801 W Bancroft St, Toledo, OH 43606 USA.
[Pipher, J.] Univ Rochester, 601 Elmwood Ave, Rochester, NY 14627 USA.
[Myers, P.; Wolk, S. J.] Harvard Univ, CFA, Cambridge, MA 02138 USA.
[Fischer, W. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Henning, T.] MPIA Heidelberg, Konigstuhl 17, D-69117 Heidelberg, Germany.
[Allen, L.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Tobin, J. J.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
RP Gutermuth, R (reprint author), Univ Massachusetts, Amherst, MA 01003 USA.
EM rgutermu@astro.umass.edu
FU NASA through JPL/Caltech [1489384]; NASA [NAS8-03060]; CSA (Canada);
NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy);
MCINN (Spain); SNSB (Sweden); STFC (UK); NASA (USA); BMVIT (Austria);
ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); CICT/MCT (Spain)
FX This work is based on observations made with Herschel, a European Space
Agency cornerstone mission with science instruments provided by
European-led Principal Investigator consortia and with significant
participation by NASA. Support for this work was provided by NASA
through an award issued by JPL/Caltech (contract number 1489384). SJW
was supported by NASA contract NAS8-03060. We are thankful to Stella
Offner, Mark Heyer, Grant Wilson and Ronald Snell from the University of
Massachusetts (UMASS), Amherst for helpful conversations, suggestions,
and feedback. We also thank Amy Stutz of the Max-Planck Institute for
Astronomy, Germany for important suggestions on the paper. We also thank
Bernhard Schulz and David Shupe from NASA Herschel Science Center for
helping us with data reduction. We are grateful to Manikarajamuthaly Sri
Saravana for helping us with technical aspects. Finally, we would like
to thank the anonymous referee for valuable comments and suggestions.
SPIRE has been developed by a consortium of institutes led by Cardiff
University (UK) and including University of Lethbridge (Canada); NAOC
(China); CEA, LAM(France); IFSI, University of Padua (Italy); IAC
(Spain); Stockholm Observatory (Sweden); Imperial College London, RAL,
UCL-MSSL, UKATC, University of Sussex (UK); Caltech, JPL, NHSC,
University of Colorado (USA). This development has been supported by
national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS
(France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA
(USA). PACS has been developed by a consortium of institutes led by MPE
(Germany) and including UVIE (Austria); KUL, CSL, IMEC (Belgium); CEA,
OAMP (France); MPIA (Germany); IFSI, OAP/AOT, OAA/CAISMI, LENS, SISSA
(Italy); IAC (Spain). This development has been supported by the funding
agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR
(Germany), ASI (Italy), and CICT/MCT (Spain).
NR 60
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U1 0
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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 SEP 1
PY 2016
VL 461
IS 1
BP 22
EP 35
DI 10.1093/mnras/stw1303
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DV9PE
UT WOS:000383272500003
ER
PT J
AU Archambault, S
Archer, A
Barnacka, A
Behera, B
Beilicke, M
Benbow, W
Berger, K
Bird, R
Bottcher, M
Buckley, JH
Bugaev, V
Cardenzana, JV
Cerruti, M
Chen, X
Christiansen, JL
Ciupik, L
Collins-Hughes, E
Connolly, MP
Cui, W
Dickinson, HJ
Dumm, J
Eisch, JD
Errando, M
Falcone, A
Federici, S
Feng, Q
Finley, JP
Fleischhack, H
Fortson, L
Furniss, A
Gillanders, GH
Godambe, S
Griffin, S
Griffiths, ST
Grube, J
Gyuk, G
Hakansson, N
Hanna, D
Holder, J
Hughes, G
Johnson, CA
Kaaret, P
Kar, P
Kertzman, M
Khassen, Y
Kieda, D
Krawczynski, H
Kumar, S
Lang, MJ
Madhavan, AS
Maier, G
McArthur, S
McCann, A
Meagher, K
Millis, J
Moriarty, P
Nelson, T
Nieto, D
de Bhroithe, AO
Ong, RA
Otte, AN
Park, N
Perkins, JS
Pohl, M
Popkow, A
Prokoph, H
Pueschel, E
Quinn, J
Ragan, K
Rajotte, J
Reyes, LC
Reynolds, PT
Richards, GT
Roache, E
Sembroski, GH
Shahinyan, K
Smith, AW
Staszak, D
Sweeney, K
Telezhinsky, I
Tucci, JV
Tyler, J
Varlotta, A
Vassiliev, VV
Wakely, SP
Welsing, R
Wilhelm, A
Williams, DA
Zitzer, B
AF Archambault, S.
Archer, A.
Barnacka, A.
Behera, B.
Beilicke, M.
Benbow, W.
Berger, K.
Bird, R.
Bottcher, M.
Buckley, J. H.
Bugaev, V.
Cardenzana, J. V.
Cerruti, M.
Chen, X.
Christiansen, J. L.
Ciupik, L.
Collins-Hughes, E.
Connolly, M. P.
Cui, W.
Dickinson, H. J.
Dumm, J.
Eisch, J. D.
Errando, M.
Falcone, A.
Federici, S.
Feng, Q.
Finley, J. P.
Fleischhack, H.
Fortson, L.
Furniss, A.
Gillanders, G. H.
Godambe, S.
Griffin, S.
Griffiths, S. T.
Grube, J.
Gyuk, G.
Hakansson, N.
Hanna, D.
Holder, J.
Hughes, G.
Johnson, C. A.
Kaaret, P.
Kar, P.
Kertzman, M.
Khassen, Y.
Kieda, D.
Krawczynski, H.
Kumar, S.
Lang, M. J.
Madhavan, A. S.
Maier, G.
McArthur, S.
McCann, A.
Meagher, K.
Millis, J.
Moriarty, P.
Nelson, T.
Nieto, D.
de Bhroithe, A. O'Faolain
Ong, R. A.
Otte, A. N.
Park, N.
Perkins, J. S.
Pohl, M.
Popkow, A.
Prokoph, H.
Pueschel, E.
Quinn, J.
Ragan, K.
Rajotte, J.
Reyes, L. C.
Reynolds, P. T.
Richards, G. T.
Roache, E.
Sembroski, G. H.
Shahinyan, K.
Smith, A. W.
Staszak, D.
Sweeney, K.
Telezhinsky, I.
Tucci, J. V.
Tyler, J.
Varlotta, A.
Vassiliev, V. V.
Wakely, S. P.
Welsing, R.
Wilhelm, A.
Williams, D. A.
Zitzer, B.
TI Discovery of very high energy gamma rays from 1ES 1440+122
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE BL Lacertae objects: general; gamma-rays: general
ID BL-LACERTAE OBJECTS; LARGE-AREA TELESCOPE; EXTRAGALACTIC BACKGROUND
LIGHT; INTERGALACTIC MAGNETIC-FIELD; ACTIVE GALACTIC NUCLEI; EINSTEIN
SLEW SURVEY; TEV BLAZARS; MULTIWAVELENGTH OBSERVATIONS; BRIGHT BLAZARS;
SOURCE CATALOG
AB The BL Lacertae object 1ES 1440+ 122 was observed in the energy range from 85 GeV to 30 TeV by the VERITAS array of imaging atmospheric Cherenkov telescopes. The observations, taken between 2008 May and 2010 June and totalling 53 h, resulted in the discovery of gamma-ray emission from the blazar, which has a redshift z = 0.163. 1ES 1440+ 122 is detected at a statistical significance of 5.5 standard deviations above the background with an integral flux of (2.8 +/- 0.7(stat) +/- 0.8sys) x 10(-12) cm(-2) s(-1) (1.2 per cent of the Crab Nebula's flux) above 200 GeV. The measured spectrum is described well by a power law from 0.2 to 1.3 TeV with a photon index of 3.1 +/- 0.4(stat) +/- 0.2(sys). Quasi-simultaneous multiwavelength data from the Fermi Large Area Telescope (0.3-300 GeV) and the Swift X-ray Telescope (0.2-10 keV) are additionally used to model the properties of the emission region. A synchrotron self-Compton model produces a good representation of the multiwavelength data. Adding an external-Compton or a hadronic component also adequately describes the data.
C1 [Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Rajotte, J.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Archer, A.; Beilicke, M.; Buckley, J. H.; Bugaev, V.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Barnacka, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Behera, B.; Chen, X.; Federici, S.; Fleischhack, H.; Hughes, G.; Maier, G.; de Bhroithe, A. O'Faolain; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Welsing, R.; Wilhelm, A.] DESY, Platanenallee 6, D-15738 Zeuthen, Germany.
[Benbow, W.; Cerruti, M.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Dept Phys & Astron, Bartol Res Inst, Newark, DE 19716 USA.
[Bird, R.; Collins-Hughes, E.; Khassen, Y.; Pueschel, E.; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Bottcher, M.] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa.
[Cardenzana, J. V.; Dickinson, H. J.; Eisch, J. D.; Madhavan, A. S.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Chen, X.; Federici, S.; Hakansson, N.; Pohl, M.; Telezhinsky, I.; Wilhelm, A.] Univ Potsdam, Inst Phys & Astron, D-14476 Golm, Germany.
[Christiansen, J. L.; Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA.
[Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Connolly, M. P.; Gillanders, G. H.; Lang, M. J.; Moriarty, P.] Natl Univ Ireland Galway, Sch Phys, Univ Rd, Galway, Ireland.
[Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Tucci, J. V.; Varlotta, A.] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA.
[Dumm, J.; Fortson, L.; Nelson, T.; Shahinyan, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Errando, M.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Falcone, A.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
[Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Godambe, S.] Bhabha Atom Res Ctr, Astrophys Sci Div, Bombay 400085, Maharashtra, India.
[Griffiths, S. T.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Van Allen Hall, Iowa City, IA 52242 USA.
[Kar, P.; Kieda, D.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[McArthur, S.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, 5640 S Ellis Ave, Chicago, IL 60637 USA.
[McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 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.
[Millis, J.] Anderson Univ, Dept Phys, 1100 East 5th St, Anderson, IN 46012 USA.
[Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Dublin Rd, Dublin, Ireland.
[Nieto, D.] Columbia Univ, Dept Phys, 538 W 120th St, New York, NY 10027 USA.
[Ong, R. A.; Popkow, A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Perkins, J. S.] NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Sci, Cork, Ireland.
[Sweeney, K.] Ohio Univ, Dept Phys & Astron, Clippinger Res Lab 251B, Athens, OH 45701 USA.
[Zitzer, B.] Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA.
RP Dumm, J (reprint author), Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
EM dumm@physics.umn.edu
FU US Department of Energy Office of Science; US National Science
Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation
Ireland [SFI 10/RFP/AST2748]; STFC in the UK; South African Department
of Science and Technology through the National Research Foundation under
NRF SARChI Chair [64789]
FX This research is supported by grants from the US Department of Energy
Office of Science, the US National Science Foundation and the
Smithsonian Institution, by NSERC in Canada, by Science Foundation
Ireland (SFI 10/RFP/AST2748), and by STFC in the UK. 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. M. Bottcher acknowledges
support by the South African Department of Science and Technology
through the National Research Foundation under NRF SARChI Chair grant
no. 64789. The VERITAS Collaboration is grateful to Trevor Weekes for
his seminal contributions and leadership in the field of VHE gamma-ray
astrophysics, which made this study possible.
NR 59
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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 SEP 1
PY 2016
VL 461
IS 1
BP 202
EP 208
DI 10.1093/mnras/stw1319
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DV9PE
UT WOS:000383272500017
ER
PT J
AU Sifon, C
Battaglia, N
Hasselfield, M
Menanteau, F
Barrientos, LF
Bond, JR
Crichton, D
Devlin, MJ
Dunner, R
Hilton, M
Hincks, AD
Hlozek, R
Huffenberger, KM
Hughes, JP
Infante, L
Kosowsky, A
Marsden, D
Marriage, TA
Moodley, K
Niemack, MD
Page, LA
Spergel, DN
Staggs, ST
Trac, H
Wollack, EJ
AF Sifon, Cristobal
Battaglia, Nick
Hasselfield, Matthew
Menanteau, Felipe
Felipe Barrientos, L.
Bond, J. Richard
Crichton, Devin
Devlin, Mark J.
Dunner, Rolando
Hilton, Matt
Hincks, Adam D.
Hlozek, Renee
Huffenberger, Kevin M.
Hughes, John P.
Infante, Leopoldo
Kosowsky, Arthur
Marsden, Danica
Marriage, Tobias A.
Moodley, Kavilan
Niemack, Michael D.
Page, Lyman A.
Spergel, David N.
Staggs, Suzanne T.
Hy Trac
Wollack, Edward J.
TI The Atacama Cosmology Telescope: dynamical masses for 44 SZ-selected
galaxy clusters over 755 square degrees
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: clusters: general; Galaxies: distances and redshifts;
cosmology: observations; large-scale structure of Universe
ID DIGITAL SKY SURVEY; SOUTH-POLE TELESCOPE; WEAK-LENSING MASSES;
ZELDOVICH-SELECTED CLUSTERS; ACT-CL J0102-4915; X-RAY-PROPERTIES;
SUNYAEV-ZELDOVICH; SCALING RELATIONS; VELOCITY DISPERSIONS; RICH
CLUSTERS
AB We present galaxy velocity dispersions and dynamical mass estimates for 44 galaxy clusters selected via the Sunyaev-Zel'dovich (SZ) effect by the Atacama Cosmology Telescope. Dynamical masses for 18 clusters are reported here for the first time. Using N-body simulations, we model the different observing strategies used to measure the velocity dispersions and account for systematic effects resulting from these strategies. We find that the galaxy velocity distributions may be treated as isotropic, and that an aperture correction of up to 7 per cent in the velocity dispersion is required if the spectroscopic galaxy sample is sufficiently concentrated towards the cluster centre. Accounting for the radial profile of the velocity dispersion in simulations enables consistent dynamical mass estimates regardless of the observing strategy. Cluster masses M200 are in the range (1-15) x 10(14)M(circle dot). Comparing with masses estimated from the SZ distortion assuming a gas pressure profile derived from X-ray observations gives a mean SZ-to-dynamical mass ratio of 1.10 +/- 0.13, but there is an additional 0.14 systematic uncertainty due to the unknown velocity bias; the statistical uncertainty is dominated by the scatter in the mass-velocity dispersion scaling relation. This ratio is consistent with previous determinations at these mass scales.
C1 [Sifon, Cristobal; Hughes, John P.] Gemini South Observ, Hilo, HI 96720 USA.
[Sifon, Cristobal] Leiden Univ, Leiden Observ, POB 513, NL-2300 RA Leiden, Netherlands.
[Battaglia, Nick; Hasselfield, Matthew; Hlozek, Renee; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA.
[Hasselfield, Matthew] Penn State Univ, Dept Astron & Astrophys, Davey Lab, 525 Davey Lab, University Pk, PA 16802 USA.
[Menanteau, Felipe] Univ Illinois, Natl Ctr Supercomp Applicat, 1205 W Clark St, Urbana, IL 61801 USA.
[Menanteau, Felipe] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA.
[Felipe Barrientos, L.; Dunner, Rolando; Infante, Leopoldo] Pontificia Univ Catolica, Fac Fis, Inst Astrofis, Casilla 306, Santiago 22, Chile.
[Bond, J. Richard] Canadian Inst Theoret Astrophys, 60 St George, Toronto, ON M5S 3H8, Canada.
[Crichton, Devin; Marriage, Tobias A.] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.
[Devlin, Mark J.; Marsden, Danica] Univ Penn, Dept Phys & Astron, 209 South 33rd St, Philadelphia, PA 19104 USA.
[Hilton, Matt; Moodley, Kavilan] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
[Hincks, Adam D.] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada.
[Hincks, Adam D.] Pontificia Univ Gregoriana, Piazza Pilotta 4, I-00187 Rome, Italy.
[Huffenberger, Kevin M.] Florida State Univ, Dept Phys, POB 3064350, Tallahassee, FL 32306 USA.
[Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, 136 Frelinghuysen Rd, Piscataway, NJ 08854 USA.
[Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Niemack, Michael D.] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA.
[Page, Lyman A.; Staggs, Suzanne T.] Princeton Univ, Joseph Henry Labs Phys, Jadwin Hall, Princeton, NJ 08544 USA.
[Hy Trac] Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA.
[Wollack, Edward J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Sifon, C (reprint author), Gemini South Observ, Hilo, HI 96720 USA.; Sifon, C (reprint author), Leiden Univ, Leiden Observ, POB 513, NL-2300 RA Leiden, Netherlands.
EM sifon@strw.leidenuniv.nl
RI Wollack, Edward/D-4467-2012; Trac, Hy/N-8838-2014;
OI Wollack, Edward/0000-0002-7567-4451; Trac, Hy/0000-0001-6778-3861;
Huffenberger, Kevin/0000-0001-7109-0099; Menanteau,
Felipe/0000-0002-1372-2534; Sifon, Cristobal/0000-0002-8149-1352
FU European Research Council under FP7 grant [279396]; FONDECYT [1120676];
NSF [1312380]; US National Science Foundation [AST-0408698, AST-0965625,
PHY-0855887, PHY-1214379]; Princeton University; University of
Pennsylvania; Canada Foundation for Innovation (CFI) award; Comision
Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT);
CFI under the auspices of Compute Canada; Government of Ontario; Ontario
Research Fund - Research Excellence; University of Toronto; Alfred P.
Sloan Foundation; National Science Foundation; US Department of Energy
Office of Science; Spanish MultiDark Consolider Project [CSD2009-00064]
FX CS acknowledges support from the European Research Council under FP7
grant number 279396 awarded to H. Hoekstra. NB and RH acknowledge
support from the iii Fellowship. LFB's research is supported by FONDECYT
under project 1120676. AK acknowledges support from NSF grant 1312380.
This work was supported by the US National Science Foundation through
awards AST-0408698 and AST-0965625 for the ACT project, as well as
awards PHY-0855887 and PHY-1214379. 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. Funding for SDSS-III has been
provided by the Alfred P. Sloan Foundation, the Participating
Institutions, the National Science Foundation, and the US Department of
Energy Office of Science. The SDSS-III web site is
http://www.sdss9.org/. The MultiDark Database used in this paper and the
web application providing online access to it were constructed as part
of the activities of the German Astrophysical Virtual Observatory as
result of a collaboration between the Leibniz-Institute for Astrophysics
Potsdam (AIP) and the Spanish MultiDark Consolider Project
CSD2009-00064. The Bolshoi and MultiDark simulations were run on the
NASA's Pleiades supercomputer at the NASA Ames Research Center. The MDPL
and the BigMD simulation suite have been performed in the Supermuc
supercomputer at LRZ using time granted by PRACE.
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J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP 1
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DI 10.1093/mnras/stw1284
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DV9PE
UT WOS:000383272500022
ER
PT J
AU Clavel, M
Tomsick, JA
Bodaghee, A
Chiu, JL
Fornasini, FM
Hong, J
Krivonos, R
Ponti, G
Rahoui, F
Stern, D
AF Clavel, M.
Tomsick, J. A.
Bodaghee, A.
Chiu, J. -L.
Fornasini, F. M.
Hong, J.
Krivonos, R.
Ponti, G.
Rahoui, F.
Stern, D.
TI IGR J18293-1213 is an eclipsing cataclysmic variable
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE binaries: eclipsing; stars: individual: IGR J18293-1213-white dwarfs;
X-rays: stars
ID X-RAY BINARIES; INTERMEDIATE POLARS; MILKY-WAY; EMISSION; MISSION;
REFLECTION; TELESCOPE; EVOLUTION; STARS; SKY
AB Studying the population of faint hard X-ray sources along the plane of the Galaxy is challenging because of high extinction and crowding, which make the identification of individual sources more difficult. IGR J18293-1213 is part of the population of persistent sources which have been discovered by the INTEGRAL satellite. We report on NuSTAR and Swift/XRT observations of this source, performed on 2015 September 11. We detected three eclipsing intervals in the NuSTAR light curve, allowing us to constrain the duration of these eclipses, Delta t = 30.8(-0.0)(+6.3) min, and the orbital period of the system, T = 6.92 +/- 0.01 h. Even though we only report an upper limit on the amplitude of a putative spin modulation, the orbital period and the hard thermal bremsstrahlung spectrum of IGR J18293-1213 provide strong evidence that this source is a magnetic cataclysmic variable. Our NuSTAR and Swift/XRT joint spectral analysis places strong constraints on the white dwarf mass M-wd = 0.78(-0.09)(+0.10) M-circle dot. Assuming that the mass to radius ratio of the companion star M star /R star = 1 (solar units) and using T, Delta t, and M-wd, we derived the mass of the companion star M-star = 0.82 +/- 0.01 M-circle dot, the orbital separation of the binary system a = 2.14 +/- 0.04 R-circle dot, and its orbital inclination compared to the line of sight i = (72 degrees.2(-0.0)(+2.4)) +/- 1 degrees.0.
C1 [Clavel, M.; Tomsick, J. A.; Chiu, J. -L.; Fornasini, F. M.] Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
[Bodaghee, A.] Georgia Coll, 231 W Hancock St, Milledgeville, GA 31061 USA.
[Fornasini, F. M.] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
[Hong, J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Krivonos, R.] Russian Acad Sci, Space Res Inst, Profsoyuznaya 84-32, Moscow 117997, Russia.
[Ponti, G.] Max Planck Inst Extraterr Phys, Gissenbachstr, D-85748 Garching, Germany.
[Rahoui, F.] European Southern Observ, Karl Schwarzchild Str 2, D-85748 Garching, Germany.
[Rahoui, F.] Harvard Univ, Dept Astron, 60 Garden St, Cambridge, MA 02138 USA.
[Stern, D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Clavel, M (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
EM maica.clavel@ssl.berkeley.edu
OI Clavel, Maica/0000-0003-0724-2742
FU NASA [NNG08FD60C]; National Aeronautics and Space Administration;
Russian Science Foundation [14-22-00271]; Bundesministerium fur
Wirtschaft und Technologie/Deutsches Zentrum fur Luftund Raumfahrt
(BMWI/DLR) [FKZ 50 OR 1408]
FX 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). RK acknowledges support from Russian
Science Foundation (grant 14-22-00271). GP acknowledges the
Bundesministerium fur Wirtschaft und Technologie/Deutsches Zentrum fur
Luftund Raumfahrt (BMWI/DLR, FKZ 50 OR 1408).
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J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP 1
PY 2016
VL 461
IS 1
BP 304
EP 311
DI 10.1093/mnras/stw1330
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DV9PE
UT WOS:000383272500026
ER
PT J
AU Joachimi, K
Gatuzz, E
Garcia, JA
Kallman, TR
AF Joachimi, Katerine
Gatuzz, Efrain
Garcia, Javier A.
Kallman, Timothy R.
TI On the detectability of CO molecules in the interstellar medium via
X-ray spectroscopy
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE techniques: spectroscopic; ISM: molecules; ISM: structure; X-rays: ISM
ID K-SHELL PHOTOABSORPTION; MILKY-WAY; ABSORPTION MODEL; XMM-NEWTON;
OXYGEN; BINARIES; CLOUDS; NEON; EDGE; PHOTOIONIZATION
AB We present a study of the detectability of CO molecules in the Galactic interstellar medium using high-resolution X-ray spectra obtained with the XMM-Newton Reflection Grating Spectrometer. We analysed 10 bright low mass X-ray binaries (LMXBs) to study the CO contribution in their line of sights. A total of 25 observations were fitted with the ISMabs X-ray absorption model which includes photoabsorption cross-sections for OI, OII, OIII and CO. We performed a Monte Carlo (MC) simulation analysis of the goodness of fit in order to estimate the significance of the CO detection. We determine that the statistical analysis prevents a significant detection of CO molecular X-ray absorption features, except for the lines of sight towards XTE J1718-330 and 4U 1636-53. In the case of XTE J1817-330, this is the first report of the presence of CO along its line of sight. Our results reinforce the conclusion that molecules have a minor contribution to the absorption features in the O K-edge spectral region. We estimate a CO column density lower limit to perform a significant detection with XMM-Newton of N(CO) > 6 x 10(16) cm(-2) for typical exposure times.
C1 [Joachimi, Katerine; Gatuzz, Efrain] Cent Univ Venezuela, Fac Ciencias, Escuela Fis, POB 20632, Caracas 1020A, Venezuela.
[Gatuzz, Efrain] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Garcia, Javier A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Kallman, Timothy R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Gatuzz, E (reprint author), Cent Univ Venezuela, Fac Ciencias, Escuela Fis, POB 20632, Caracas 1020A, Venezuela.; Gatuzz, E (reprint author), Max Planck Inst Astrophys, D-85741 Garching, Germany.
EM efraingatuzz@gmail.com; jajgarcia@gmail.com
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J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP 1
PY 2016
VL 461
IS 1
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EP 357
DI 10.1093/mnras/stw1371
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DV9PE
UT WOS:000383272500030
ER
PT J
AU Davies, LJM
Driver, SP
Robotham, ASG
Grootes, MW
Popescu, CC
Tuffs, RJ
Hopkins, A
Alpaslan, M
Andrews, SK
Bland-Hawthorn, J
Bremer, MN
Brough, S
Brown, MJI
Cluver, ME
Croom, S
da Cunha, E
Dunne, L
Lara-Lopez, MA
Liske, J
Loveday, J
Moffett, AJ
Owers, M
Phillipps, S
Sansom, AE
Taylor, EN
Michalowski, MJ
Ibar, E
Smith, M
Bourne, N
AF Davies, L. J. M.
Driver, S. P.
Robotham, A. S. G.
Grootes, M. W.
Popescu, C. C.
Tuffs, R. J.
Hopkins, A.
Alpaslan, M.
Andrews, S. K.
Bland-Hawthorn, J.
Bremer, M. N.
Brough, S.
Brown, M. J. I.
Cluver, M. E.
Croom, S.
da Cunha, E.
Dunne, L.
Lara-Lopez, M. A.
Liske, J.
Loveday, J.
Moffett, A. J.
Owers, M.
Phillipps, S.
Sansom, A. E.
Taylor, E. N.
Michalowski, M. J.
Ibar, E.
Smith, M.
Bourne, N.
TI GAMA/H-ATLAS: a meta-analysis of SFR indicators - comprehensive measures
of the SFR-M* relation and cosmic star formation history at z < 0.4
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: evolution; galaxies: star formation
ID MASS ASSEMBLY GAMA; DIGITAL SKY SURVEY; SPECTRAL ENERGY-DISTRIBUTION;
HIGH-REDSHIFT GALAXIES; DEEP FIELD SOUTH; FORMING GALAXIES; SPIRAL
GALAXIES; STELLAR MASS; MAIN-SEQUENCE; FORMATION RATES
AB We present a meta-analysis of star formation rate (SFR) indicators in the Galaxy And Mass Assembly (GAMA) survey, producing 12 different SFR metrics and determining the SFRM* relation for each. We compare and contrast published methods to extract the SFR from each indicator, using a well-defined local sample of morphologically selected spiral galaxies, which excludes sources which potentially have large recent changes to their SFR. The different methods are found to yield SFR-M* relations with inconsistent slopes and normalizations, suggesting differences between calibration methods. The recovered SFR-M* relations also have a large range in scatter which, as SFRs of the targets may be considered constant over the different time-scales, suggests differences in the accuracy by which methods correct for attenuation in individual targets. We then recalibrate all SFR indicators to provide new, robust and consistent luminosity-to-SFR calibrations, finding that the most consistent slopes and normalizations of the SFR-M* relations are obtained when recalibrated using the radiation transfer method of Popescu et al. These new calibrations can be used to directly compare SFRs across different observations, epochs and galaxy populations. We then apply our calibrations to the GAMA II equatorial data set and explore the evolution of star formation in the local Universe. We determine the evolution of the normalization to the SFR-M* relation from 0 < z < 0.35 - finding consistent trends with previous estimates at 0.3 < z < 1.2. We then provide the definitive z < 0.35 cosmic star formation history, SFR-M* relation and its evolution over the last 3 billion years.
C1 [Davies, L. J. M.; Driver, S. P.; Robotham, A. S. G.; Andrews, S. K.; Moffett, A. J.] Univ Western Australia, ICRAR, 35 Stirling Highway, Crawley, WA 6009, Australia.
[Driver, S. P.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Grootes, M. W.] ESA ESTEC SCI S, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands.
[Popescu, C. C.; Sansom, A. E.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
[Popescu, C. C.] Romanian Acad, Astron Inst, Str Cutitul Argint 5, Bucharest 040557, Romania.
[Tuffs, R. J.] Max Planck Inst Kernphys, Saupfercheckweg 1, D-69117 Heidelberg, Germany.
[Hopkins, A.; Brough, S.; Owers, M.] Australian Astron Observ, POB 915, N Ryde, NSW 1670, Australia.
[Alpaslan, M.] NASA, Ames Res Ctr, N232, Mountain View, CA 94034 USA.
[Bland-Hawthorn, J.; Croom, S.] Univ Sydney, Sch Phys A28, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Bremer, M. N.; Phillipps, S.] Univ Bristol, Sch Phys, Astrophys Grp, Tyndall Ave, Bristol BS8 1TL, Avon, England.
[Brown, M. J. I.] Monash Univ, Sch Phys & Astron, Clayton, Vic 3800, Australia.
[Cluver, M. E.] Univ Western Cape, Dept Phys & Astron, Robert Sobukwe Rd, ZA-7535 Bellville, South Africa.
[da Cunha, E.; Taylor, E. N.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, POB 218, Hawthorn, Vic 3122, Australia.
[Dunne, L.; Michalowski, M. J.; Bourne, N.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Dunne, L.; Smith, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Lara-Lopez, M. A.] Univ Nacl Autonoma Mexico, Inst Astron, AP 70-264, Mexico City 04510, DF, Mexico.
[Liske, J.] Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany.
[Loveday, J.] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
[Owers, M.] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia.
[Ibar, E.] Univ Valparaiso, Inst Fis & Astron, Avda Gran Bretana 1111, Valparaiso, Chile.
RP Davies, LJM (reprint author), Univ Western Australia, ICRAR, 35 Stirling Highway, Crawley, WA 6009, Australia.
EM luke.j.davies@uwa.edu.au
RI Brown, Michael/B-1181-2015;
OI Brown, Michael/0000-0002-1207-9137; Alpaslan, Mehmet/0000-0003-0321-1033
FU STFC (UK); ARC (Australia); AAO; UNAM through the PAPIIT project
[IA101315]; European Research Council Advanced Investigator grant Cosmic
Dust
FX GAMA is a joint European-Australasian project based around a
spectroscopic campaign using the Anglo-Australian Telescope. The GAMA
input catalogue is based on data taken from the Sloan Digital Sky Survey
and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the
GAMA regions is being obtained by a number of independent survey
programmes including GALEX MIS, VST KiDS, VISTA VIKING, WISE,
Herschel-ATLAS, GMRT and ASKAP providing UV-to-radio coverage. GAMA is
funded by the STFC (UK), the ARC (Australia), the AAO and the
participating institutions. The GAMA website is
http://www.gama-survey.org/.; MALL acknowledges support from UNAM
through the PAPIIT project IA101315. LD acknowledges support from
European Research Council Advanced Investigator grant Cosmic Dust.
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J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
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PY 2016
VL 461
IS 1
BP 458
EP 485
DI 10.1093/mnras/stw1342
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DV9PE
UT WOS:000383272500037
ER
PT J
AU Pieres, A
Santiago, B
Balbinot, E
Luque, E
Queiroz, A
da Costa, LN
Maia, MAG
Drlica-Wagner, A
Roodman, A
Abbott, TMC
Allam, S
Benoit-Levy, A
Bertin, E
Brooks, D
Buckley-Geer, E
Burke, DL
Rosell, AC
Kind, MC
Carretero, J
Cunha, CE
Desai, S
Diehl, HT
Eifler, TF
Finley, DA
Flaugher, B
Fosalba, P
Frieman, J
Gerdes, DW
Gruen, D
Gruendl, RA
Gutierrez, G
Honscheid, K
James, DJ
Kuehn, K
Kuropatkin, N
Lahav, O
Li, TS
Marshall, L
Martini, P
Miller, CJ
Miquel, R
Nichol, RC
Nord, B
Ogando, R
Plazas, AA
Romer, AK
Sanchez, E
Scarpine, V
Schubnell, M
Sevilla-Noarbe, I
Smith, RC
Soares-Santos, M
Sobreira, F
Suchyta, E
Swanson, MEC
Tarle, G
Thaler, J
Thomas, D
Tucker, DL
Walker, AR
AF Pieres, A.
Santiago, B.
Balbinot, E.
Luque, E.
Queiroz, A.
da Costa, L. N.
Maia, M. A. G.
Drlica-Wagner, A.
Roodman, A.
Abbott, T. M. C.
Allam, S.
Benoit-Levy, A.
Bertin, E.
Brooks, D.
Buckley-Geer, E.
Burke, D. L.
Rosell, A. Carnero
Kind, M. Carrasco
Carretero, J.
Cunha, C. E.
Desai, S.
Diehl, H. T.
Eifler, T. F.
Finley, D. A.
Flaugher, B.
Fosalba, P.
Frieman, J.
Gerdes, D. W.
Gruen, D.
Gruendl, R. A.
Gutierrez, G.
Honscheid, K.
James, D. J.
Kuehn, K.
Kuropatkin, N.
Lahav, O.
Li, T. S.
Marshall, L.
Martini, P.
Miller, C. J.
Miquel, R.
Nichol, R. C.
Nord, B.
Ogando, R.
Plazas, A. A.
Romer, A. K.
Sanchez, E.
Scarpine, V.
Schubnell, M.
Sevilla-Noarbe, I.
Smith, R. C.
Soares-Santos, M.
Sobreira, F.
Suchyta, E.
Swanson, M. E. C.
Tarle, G.
Thaler, J.
Thomas, D.
Tucker, D. L.
Walker, A. R.
TI Physical properties of star clusters in the outer LMC as observed by the
DES
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: statistical; Magellanic Cloud; galaxies: star clusters: general
ID LARGE-MAGELLANIC-CLOUD; COLOR-MAGNITUDE DIAGRAMS; CHEMICAL ENRICHMENT
HISTORY; SIMPLE STELLAR POPULATIONS; STRUCTURAL PARAMETERS; METALLICITY
RELATION; PHOTOMETRIC SYSTEMS; SOURCE EXTRACTION; AGE DISTRIBUTION; RED
CLUMP
AB The Large Magellanic Cloud (LMC) harbours a rich and diverse system of star clusters, whose ages, chemical abundances and positions provide information about the LMC history of star formation. We use Science Verification imaging data from the Dark Energy Survey (DES) to increase the census of known star clusters in the outer LMC and to derive physical parameters for a large sample of such objects using a spatially and photometrically homogeneous data set. Our sample contains 255 visually identified cluster candidates, of which 109 were not listed in any previous catalogue. We quantify the crowding effect for the stellar sample produced by the DES Data Management pipeline and conclude that the stellar completeness is < 10 per cent inside typical LMC cluster cores. We therefore reanalysed the DES co-add images around each candidate cluster and remeasured positions and magnitudes for their stars. We also implement a maximum-likelihood method to fit individual density profiles and colour-magnitude diagrams. For 117 (from a total of 255) of the cluster candidates (28 uncatalogued clusters), we obtain reliable ages, metallicities, distance moduli and structural parameters, confirming their nature as physical systems. The distribution of cluster metallicities shows a radial dependence, with no clusters more metal rich than [Fe/H] similar or equal to -0.7 beyond 8 kpc from the LMC centre. The age distribution has two peaks at similar or equal to 1.2 and similar or equal to 2.7 Gyr.
C1 [Pieres, A.; Santiago, B.; Luque, E.; Queiroz, A.] Univ Fed Rio Grande do Sul, Inst Fis, Caixa Postal 15051, BR-91501970 Porto Alegre, RS, Brazil.
[Pieres, A.; Santiago, B.; Luque, E.; Queiroz, A.; da Costa, L. N.; Maia, M. A. G.; Rosell, A. Carnero; Ogando, R.; Sobreira, F.] Lab Interinst E Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Balbinot, E.] Univ Surrey, Dept Phys, Guildford GU2 7XH, Surrey, England.
[da Costa, L. N.; Maia, M. A. G.; Rosell, A. Carnero; Ogando, R.] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Drlica-Wagner, A.; Allam, S.; Buckley-Geer, E.; Diehl, H. T.; Finley, D. A.; Flaugher, B.; Frieman, J.; Gutierrez, G.; Kuropatkin, N.; Nord, B.; Scarpine, V.; Soares-Santos, M.; Tucker, D. L.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA.
[Roodman, A.; Burke, D. L.; Cunha, C. E.; Frieman, J.; Gruen, D.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA.
[Roodman, A.; Burke, D. L.; Gruen, D.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA.
[Abbott, T. M. C.; James, D. J.; Smith, R. C.; Walker, A. R.] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile.
[Benoit-Levy, A.; Bertin, E.] CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France.
[Benoit-Levy, A.; Brooks, D.; Lahav, O.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England.
[Benoit-Levy, A.; Bertin, E.] Univ Paris 06, Sorbonne Univ, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France.
[Kind, M. Carrasco; Gruendl, R. A.] 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.; 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, IFAE, Campus UAB, E-08193 Barcelona, Spain.
[Desai, S.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany.
[Desai, S.] Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany.
[Eifler, T. F.; Plazas, A. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Gerdes, D. W.; Miller, C. J.; Schubnell, M.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Honscheid, K.; Martini, P.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Honscheid, K.] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA.
[Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia.
[Li, T. S.; Marshall, L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
[Li, T. S.; Marshall, L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
[Martini, P.] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA.
[Miller, C. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain.
[Nichol, R. C.; Thomas, D.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Romer, A. K.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England.
[Sanchez, E.; Sevilla-Noarbe, I.] Ctr Invest Energet Medioambientales & Tecnol CIEM, Madrid, Spain.
[Sobreira, F.] Univ Estadual Paulista, ICTP South Amer Inst Fundamental Res, Inst Fis Teor, Sao Paulo, Brazil.
[Suchyta, E.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Thaler, J.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA.
RP Pieres, A (reprint author), Univ Fed Rio Grande do Sul, Inst Fis, Caixa Postal 15051, BR-91501970 Porto Alegre, RS, Brazil.; Pieres, A (reprint author), Lab Interinst E Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil.
EM adriano.pieres@ufrgs.br; basilio.santiago@ufrgs.br;
e.balbinot@surrey.ac.uk
RI Ogando, Ricardo/A-1747-2010;
OI Ogando, Ricardo/0000-0003-2120-1154; Sobreira,
Flavia/0000-0002-7822-0658
FU Brazilian Institution CNPq; European Research Council [ERC-StG-335936];
US Department of Energy; US 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; Collaborating
Institutions in the Dark Energy Survey; National Science Foundation
[AST-1138766]; MINECO [AYA2012-39559, ESP2013-48274, FPA2013-47986];
Centro de Excelencia Severo Ochoa [SEV-2012-0234]; European Research
Council under the European Union [240672, 291329, 306478]
FX AdP acknowledges financial support from the Brazilian Institution CNPq.
EdB acknowledges financial support from the European Research Council
(ERC-StG-335936, CLUSTERS).; Funding for the DES Projects has been
provided by the US Department of Energy, the US 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 Dark Energy Survey.; 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.
Research leading to these results has received funding from the European
Research Council under the European Union's Seventh Framework Programme
(FP7/2007-2013) including ERC grant agreements 240672, 291329 and
306478.
NR 67
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U1 5
U2 5
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 SEP 1
PY 2016
VL 461
IS 1
BP 519
EP 541
DI 10.1093/mnras/stw1260
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DV9PE
UT WOS:000383272500041
ER
PT J
AU LeGrande, AN
Tsigaridis, K
Bauer, SE
AF LeGrande, Allegra N.
Tsigaridis, Kostas
Bauer, Susanne E.
TI Role of atmospheric chemistry in the climate impacts of stratospheric
volcanic injections
SO NATURE GEOSCIENCE
LA English
DT Article
ID WATER-VAPOR; NORTHERN MIDLATITUDES; ERUPTIONS; OZONE; PINATUBO; WINTER;
RECONSTRUCTIONS; SPECTROMETER; SENSITIVITY; AEROSOLS
AB The climate impact of a volcanic eruption is known to be dependent on the size, location and timing of the eruption. However, the chemistry and composition of the volcanic plume also control its impact on climate. It is not just sulfur dioxide gas, but also the coincident emissions of water, halogens and ash that influence the radiative and climate forcing of an eruption. Improvements in the capability of models to capture aerosol microphysics, and the inclusion of chemistry and aerosol microphysics modules in Earth system models, allow us to evaluate the interaction of composition and chemistry within volcanic plumes in a new way. These modelling efforts also illustrate the role of water vapour in controlling the chemical evolution - and hence climate impacts - of the plume. A growing realization of the importance of the chemical composition of volcanic plumes is leading to a more sophisticated and realistic representation of volcanic forcing in climate simulations, which in turn aids in reconciling simulations and proxy reconstructions of the climate impacts of past volcanic eruptions. More sophisticated simulations are expected to help, eventually, with predictions of the impact on the Earth system of any future large volcanic eruptions.
C1 [LeGrande, Allegra N.; Tsigaridis, Kostas; Bauer, Susanne E.] NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
[Tsigaridis, Kostas; Bauer, Susanne E.] Columbia Univ, Ctr Climate Syst Res, 2880 Broadway, New York, NY USA.
RP LeGrande, AN (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM allegra.n.legrande@nasa.gov; kostas.tsigaridis@columbia.edu
FU NASA High-End Computing (HEC) Program through the NASA Center for
Climate Simulation (NCCS) at Goddard Space Flight Center
FX We thank NASA GISS for institutional support. We also thank the NASA MAP
programme for continued support. 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 50
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U1 14
U2 14
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 1752-0894
EI 1752-0908
J9 NAT GEOSCI
JI Nat. Geosci.
PD SEP
PY 2016
VL 9
IS 9
BP 652
EP 655
DI 10.1038/NGEO2771
PG 4
WC Geosciences, Multidisciplinary
SC Geology
GA DV9TA
UT WOS:000383283700006
ER
PT J
AU Wooden, DH
Cook, AM
Colaprete, A
Glenar, DA
Stubbs, TJ
Shirley, M
AF Wooden, D. H.
Cook, A. M.
Colaprete, A.
Glenar, D. A.
Stubbs, T. J.
Shirley, M.
TI Evidence for a dynamic nanodust cloud enveloping the Moon
SO NATURE GEOSCIENCE
LA English
DT Article
ID GENERATED DUST CLOUDS; HYPERVELOCITY IMPACTS; PLANETARY SATELLITES;
COMET P/HALLEY; SURFACES; SPACE; FE
AB The exospheres that surround airless bodies such as the Moon are tenuous, atmosphere-like layers whose constituent particles rarely collide with one another. Some particles contained within such exospheres are the product of direct interactions between airless bodies and the space environment, and offer insights into space weathering processes. NASA's Lunar Atmosphere and Dust Environment Explorer (LADEE) mission studied the Moon's exospheric constituents in situ and detected a permanent dust exosphere(1) of particles with radii as small as 300 nm. Here we present evidence from LADEE spectral data for an additional fluctuating nanodust exosphere at the Moon containing a population of particles sufficiently dense to be detectable via scattered sunlight. We compare two anti-Sun spectral observations: one near the peak of the Quadrantid meteoroid stream, the other during a period of comparatively weak stream activity. The former shows a negative spectral slope consistent with backscattering of sunlight by nanodust grains with radii less than 20 to 30 nm; the latter has a flatter spectral slope. We hypothesize that a spatially and temporally variable nanodust exosphere may exist at the Moon, and that it is modulated by changes in meteoroid impact rates, such as during encounters with meteoroid streams. The findings suggest that similar nanodust exospheres-and the particle ejection and transport processes that form them-may occur at other airless bodies.
C1 [Wooden, D. H.; Cook, A. M.; Colaprete, A.; Shirley, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Cook, A. M.] Millenium Engn & Integrat Co, 350 North Akron Rd Bldg 19,Suite 2080, Moffett Field, CA 94035 USA.
[Glenar, D. A.] Univ Maryland Baltimore Cty, 1000 Hilltop Circle, Baltimore, MD 21250 USA.
[Stubbs, T. J.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
RP Wooden, DH (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM diane.wooden@nasa.gov
RI Stubbs, Timothy/I-5139-2013
OI Stubbs, Timothy/0000-0002-5524-645X
FU NASA Lunar Quest Program; LADEE Guest Observer Program; NASA's Science
Mission Directorate
FX LADEE UVS was supported through the NASA Lunar Quest Program. The
authors also acknowledge financial support from the LADEE Guest Observer
Program and NASA's Science Mission Directorate.
NR 29
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U1 5
U2 5
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 1752-0894
EI 1752-0908
J9 NAT GEOSCI
JI Nat. Geosci.
PD SEP
PY 2016
VL 9
IS 9
BP 665
EP +
DI 10.1038/NGEO2779
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA DV9TA
UT WOS:000383283700008
ER
PT J
AU Dhakal, B
Nicholson, DE
Saleeb, AF
Padula, SA
Vaidyanathan, R
AF Dhakal, B.
Nicholson, D. E.
Saleeb, A. F.
Padula, S. A., II
Vaidyanathan, R.
TI Three-dimensional deformation response of a NiTi shape memory
helical-coil actuator during thermomechanical cycling: experimentally
validated numerical model
SO SMART MATERIALS AND STRUCTURES
LA English
DT Article
DE experimental validation; NiTi; multi-axial; shape memory alloy; thermal
cycling; helical-coil actuators; springs
ID PERFORMANCE-CHARACTERISTICS; CONSTITUTIVE MODEL; ALLOYS; TRANSFORMATION;
EVOLUTION; PHASE
AB Shape memory alloy (SMA) actuators often operate under a complex state of stress for an extended number of thermomechanical cycles in many aerospace and engineering applications. Hence, it becomes important to account for multi-axial stress states and deformation characteristics (which evolve with thermomechanical cycling) when calibrating any SMA model for implementation in large-scale simulation of actuators. To this end, the present work is focused on the experimental validation of an SMA model calibrated for the transient and cyclic evolutionary behavior of shape memory Ni49.9Ti50.1, for the actuation of axially loaded helical-coil springs. The approach requires both experimental and computational aspects to appropriately assess the thermomechanical response of these multi-dimensional structures. As such, an instrumented and controlled experimental setup was assembled to obtain temperature, torque, degree of twist and extension, while controlling end constraints during heating and cooling of an SMA spring under a constant externally applied axial load. The computational component assesses the capabilities of a general, multi-axial, SMA material-modeling framework, calibrated for Ni49.9Ti50.1 with regard to its usefulness in the simulation of SMA helical-coil spring actuators. Axial extension, being the primary response, was examined on an axially-loaded spring with multiple active coils. Two different conditions of end boundary constraint were investigated in both the numerical simulations as well as the validation experiments: Case (1) where the loading end is restrained against twist (and the resulting torque measured as the secondary response) and Case (2) where the loading end is free to twist (and the degree of twist measured as the secondary response). The present study focuses on the transient and evolutionary response associated with the initial isothermal loading and the subsequent thermal cycles under applied constant axial load. The experimental results for the helical-coil actuator under two different boundary conditions are found to be within error to their counterparts in the numerical simulations. The numerical simulation and the experimental validation demonstrate similar transient and evolutionary behavior in the deformation response under the complex, inhomogeneous, multi-axial stress-state and large deformations of the helical-coil actuator. This response, although substantially different in magnitude, exhibited similar evolutionary characteristics to the simple, uniaxial, homogeneous, stress-state of the isobaric tensile tests results used for the model calibration. There was no significant difference in the axial displacement (primary response) magnitudes observed between Cases (1) and (2) for the number of cycles investigated here. The simulated secondary responses of the two cases evolved in a similar manner when compared to the experimental validation of the respective cases.
C1 [Dhakal, B.; Saleeb, A. F.] Univ Akron, Dept Civil Engn, 302 Buchtel Common, Akron, OH 44325 USA.
[Nicholson, D. E.; Vaidyanathan, R.] Univ Cent Florida, Dept Mat Sci & Engn, Dept Mech & Aerosp Engn, 4000 Cent Florida Blvd, Orlando, FL 32816 USA.
[Padula, S. A., II] NASA, Glenn Res Ctr, 21000 Brookpark Rd, Cleveland, OH 44135 USA.
RP Dhakal, B (reprint author), Univ Akron, Dept Civil Engn, 302 Buchtel Common, Akron, OH 44325 USA.
EM bd27@zips.uakron.edu
FU Fundamental Aeronautics Program, Fixed-Wing [NNH10ZEA001N-SFW1,
NNX11AI57A]; University of Central Florida
FX This work was supported by the Fundamental Aeronautics Program,
Fixed-Wing, Project No. NNH10ZEA001N-SFW1, Grant No: NNX11AI57A to the
University of Akron with the University of Central Florida as Sub
Contractor. The authors would like to acknowledge Dr S M Arnold for his
technical guidance and programmatic support during the different phases
of the project. The authors thank Dr O Benafan for helpful technical
discussions regarding the experiments.
NR 39
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U1 7
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0964-1726
EI 1361-665X
J9 SMART MATER STRUCT
JI Smart Mater. Struct.
PD SEP
PY 2016
VL 25
IS 9
AR 095056
DI 10.1088/0964-1726/25/9/095056
PG 16
WC Instruments & Instrumentation; Materials Science, Multidisciplinary
SC Instruments & Instrumentation; Materials Science
GA DW9SF
UT WOS:000384002200008
ER
PT J
AU Narapusetty, B
Murtugudde, R
Wang, H
Kumar, A
AF Narapusetty, Balachandrudu
Murtugudde, Raghu
Wang, Hui
Kumar, Arun
TI Ocean-atmosphere processes driving Indian summer monsoon biases in CFSv2
hindcasts
SO CLIMATE DYNAMICS
LA English
DT Article
DE CFSv2 forecast biases; Indian summer monsoon rainfall; Dry-land biases
ID WESTERN ARABIAN SEA; INTRASEASONAL OSCILLATIONS; RAINFALL VARIABILITY;
GLOBAL PRECIPITATION; ASIAN MONSOON; PREDICTION; CLIMATE; MODEL;
DYNAMICS
AB This paper analyzes the role of the Indian Ocean (IO) and the atmosphere biases in generating and sustaining large-scale precipitation biases over Central India (CI) during the Indian summer monsoon (ISM) in the climate forecast system version 2 (CFSv2) hindcasts that are produced by initializing the system each month from January 1982 to March 2011. The CFSv2 hindcasts are characterized by a systematic dry monsoon bias over CI that deteriorate with forecast lead-times and coexist with a wet bias in the tropical IO suggesting a large-scale interplay between coupled ocean-atmosphere and land biases. The biases evolving from spring-initialized forecasts are analyzed in detail to understand the evolution of summer biases. The northward migration of the Inter Tropical Convergence Zone (ITCZ) that typically crosses the equator in the IO sector during April in nature is delayed in the hindcasts when the forecast system is initialized in early spring. Our analyses show that the delay in the ITCZ coexists with wind and SST biases and the associated processes project onto the seasonal evolution of the coupled ocean-atmosphere features. This delay in conjunction with the SST and the wind biases during late spring and early summer contributes to excessive precipitation over the ocean and leading to a deficit in rainfall over CI throughout the summer. Attribution of bias to a specific component in a coupled forecast system is particularly challenging as seemingly independent biases from one component affect the other components or are affected by their feedbacks. In the spring-initialized forecasts, the buildup of deeper thermocline in association with warmer SSTs due to the enhanced Ekman pumping in the southwest IO inhibits the otherwise typical northward propagation of ITCZ in the month of April. Beyond this deficiency in the forecasts, two key ocean-atmosphere coupled mechanisms are identified; one in the Arabian Sea, where a positive windstress curl bias in conjunction with warmer SSTs lead to a weakening of Findlater jet and the other in the east equatorial IO where a remote forcing by the predominantly westerly bias in the western-central equatorial IO in the summer strengthen the seasonal downwelling Kelvin wave that in turn deepens the thermocline in the eastern IO. The equatorial Kelvin wave continues as a coastal Kelvin wave and disperses as Rossby waves off Sumatra and induces positive SST and precipitation biases in the eastern and southern Bay of Bengal. This study shows that the biases that first appear in winds lead to a cascade of coupled processes that exacerbate the subsequent biases by modulating the evolution of seasonal processes such as the annual Kelvin and Rossby waves and the cross-equatorial vertically integrated moisture transport. While this analysis does not offer any particular insights into improving the ISM forecasts, it is a foundational first step towards this goal.
C1 [Narapusetty, Balachandrudu; Murtugudde, Raghu] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Narapusetty, Balachandrudu] NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wang, Hui] INNOVIM, College Pk, MD USA.
[Wang, Hui] NOAA, NCEP, Climate Predict Ctr, College Pk, MD USA.
[Kumar, Arun] NOAA, NWS, NCEP, Climate Predict Ctr, College Pk, MD USA.
RP Narapusetty, B (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.; Narapusetty, B (reprint author), NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM bnarapus@umd.edu
FU Earth System Science Organization, Ministry of Earth Sciences,
Government of India [MM/SERP/Univ_Maryland_USA/2013/INT-16/002]
FX The authors gratefully acknowledge the financial support given by the
Earth System Science Organization, Ministry of Earth Sciences,
Government of India (MM/SERP/Univ_Maryland_USA/2013/INT-16/002) to
conduct this research under Monsoon Mission. The authors also
acknowledge Dr. Krishnan, Dr. Rajeevan, Dr. Shukla, and Dr. Kinter for
helpful comments and discussions.
NR 48
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U1 3
U2 3
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 SEP
PY 2016
VL 47
IS 5-6
BP 1417
EP 1433
DI 10.1007/s00382-015-2910-9
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DU3LK
UT WOS:000382112000005
ER
PT J
AU Stanfield, RE
Jiang, JH
Dong, XQ
Xi, BK
Su, H
Donner, L
Rotstayn, L
Wu, TW
Cole, J
Shindo, E
AF Stanfield, Ryan E.
Jiang, Jonathan H.
Dong, Xiquan
Xi, Baike
Su, Hui
Donner, Leo
Rotstayn, Leon
Wu, Tongwen
Cole, Jason
Shindo, Eiki
TI A quantitative assessment of precipitation associated with the ITCZ in
the CMIP5 GCM simulations
SO CLIMATE DYNAMICS
LA English
DT Article
DE GCM; Global climate models; GCM precipitation; Model precipitation;
AMIP; CMIP; CMIP5; Climate change; ITCZ; GCM bias
ID GENERAL-CIRCULATION MODEL; PACIFIC COLD-TONGUE; LARGE-SCALE MODELS;
INCLUDING MASS FLUXES; GLOBAL CLIMATE MODEL; EARTH SYSTEM MODEL; NASA
GISS CMIP5; PART I; CUMULUS CONVECTION; RAINFALL PRODUCTS
AB According to the Intergovernmental Panel on Climate Change 5th Assessment Report, the broad-scale features of precipitation as simulated by Phase 5 of the Coupled Model Intercomparison Project (CMIP5) are in modest agreement with observations, however, large systematic errors are found in the Tropics. In this study, a new algorithm has been developed to define the North Pacific Intertropical Convergence Zone (ITCZ) through several metrics, including: the centerline position of the ITCZ, the width of the ITCZ, and the magnitude of precipitation along the defined ITCZ. These metrics provide a quantitative analysis of precipitation associated with the ITCZ over the equatorial northern Pacific. Results from 29 CMIP5 Atmospheric Model Intercomparison Project (AMIP) Global Circulation Model (GCM) runs are compared with Global Precipitation Climatology Project (GPCP) and Tropical Rainfall Measuring Mission (TRMM) observations. Similarities and differences between the GCM simulations and observations are analyzed with the intent of quantifying magnitude-, location-, and width-based biases within the GCMs. Comparisons show that most of the GCMs tend to simulate a stronger, wider ITCZ shifted slightly northward compared to the ITCZ in GPCP and TRMM observations. Comparisons of CMIP and AMIP simulated precipitation using like-models were found to be nearly equally distributed, with roughly half of GCMs showing an increase (decrease) in precipitation when coupled (decoupled) from their respective ocean model. Further study is warranted to understand these differences.
C1 [Stanfield, Ryan E.; Dong, Xiquan; Xi, Baike] Univ North Dakota, Dept Atmospher Sci, 4149 Univ Ave Stop 9006, Grand Forks, ND 58202 USA.
[Jiang, Jonathan H.; Su, Hui] Jet Prop Lab, Pasadena, CA USA.
[Donner, Leo] Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Rotstayn, Leon] CSIRO, Clayton, Vic, Australia.
[Wu, Tongwen] China Meteorol Adm, Beijing Climate Ctr, Beijing, Peoples R China.
[Cole, Jason] Environm Canada, Canadian Ctr Climate Modeling & Anal, Toronto, ON, Canada.
[Shindo, Eiki] Japan Meteorol Agcy, Meteorol Res Inst, Tsukuba, Ibaraki, Japan.
RP Dong, XQ (reprint author), Univ North Dakota, Dept Atmospher Sci, 4149 Univ Ave Stop 9006, Grand Forks, ND 58202 USA.
EM dong@aero.und.edu
FU Jet Propulsion Laboratory (JPL), California Institute of Technology
under NASA; NASA CERES [NNX14AP84G]; EPSCoR projects; NASA [ROSES12-MAP,
ROSE13-NDOA]
FX We would like to acknowledge the contributions made by Trond Iversen,
for providing information and references on the NorESM model, and the
contributions made by Cyril Morcrette, for his comments and suggestions
related to HadGEM2-A model. The authors acknowledge the support by the
Jet Propulsion Laboratory (JPL), California Institute of Technology
under contract with NASA. The researchers at University of North Dakota
were supported by NASA CERES (NNX14AP84G) and EPSCoR projects, and the
researchers at JPL were supported by NASA ROSES12-MAP and ROSE13-NDOA
projects. Data were obtained from the CMIP5 ESGF PCMDI database at
http://pcmdi9.llnl.gov/esgf-web-fe/. GPCP and TRMM data are also
provided by the Obs4MIPS program and are available as well from the ESGF
PCMDI database at http://pcmdi9.llnl.gov/esgf-web-fe/. The GPCP SG
combined precipitation data were developed and computed at the
NASA/Goddard Space Flight Center's Mesoscale Atmospheric Processes
Laboratory - Atmospheres as a contribution to the GEWEX Global
Precipitation Climatology Project.
NR 64
TC 0
Z9 0
U1 7
U2 7
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 SEP
PY 2016
VL 47
IS 5-6
BP 1863
EP 1880
DI 10.1007/s00382-015-2937-y
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DU3LK
UT WOS:000382112000031
ER
PT J
AU Abdi, AM
Vrieling, A
Yengoh, GT
Anyamba, A
Seaquist, JW
Ummenhofer, CC
Ardo, J
AF Abdi, A. M.
Vrieling, A.
Yengoh, G. T.
Anyamba, A.
Seaquist, J. W.
Ummenhofer, C. C.
Ardo, J.
TI The El Nio - La Nia cycle and recent trends in supply and demand of net
primary productivity in African drylands
SO CLIMATIC CHANGE
LA English
DT Article
DE Sub-Saharan Africa; Drylands; El Nino-southern oscillation; Net primary
productivity; Climate variability
ID FOOD INSECURITY; CLIMATE; ECOSYSTEMS; PATTERNS; RAINFALL; ETHIOPIA;
CHARCOAL; ENSO
AB Inter-annual climatic variability over a large portion of sub-Saharan Africa is under the influence of the El Nio-Southern Oscillation (ENSO). Extreme variability in climate is a threat to rural livelihoods in sub-Saharan Africa, yet the role of ENSO in the balance between supply and demand of net primary productivity (NPP) over this region is unclear. Here, we analyze the impact of ENSO on this balance in a spatially explicit framework using gridded population data from the WorldPop project, satellite-derived data on NPP supply, and statistical data from the United Nations. Our analyses demonstrate that between 2000 and 2013 fluctuations in the supply of NPP associated with moderate ENSO events average +/- 2.8 g C m(-2) yr.(-1) across sub-Saharan drylands. The greatest sensitivity is in arid Southern Africa where a + 1 A degrees C change in the Nio-3.4 sea surface temperature index is associated with a mean change in NPP supply of -6.6 g C m(-2) yr.(-1). Concurrently, the population-driven trend in NPP demand averages 3.5 g C m(-2) yr.(-1) over the entire region with densely populated urban areas exhibiting the highest mean demand for NPP. Our findings highlight the importance of accounting for the role ENSO plays in modulating the balance between supply and demand of NPP in sub-Saharan drylands. An important implication of these findings is that increase in NPP demand for socio-economic metabolism must be taken into account within the context of climate-modulated supply.
C1 [Abdi, A. M.; Seaquist, J. W.; Ardo, J.] Lund Univ, Dept Phys Geog & Ecosyst Sci, Solvegatan 12, S-22362 Lund, Sweden.
[Vrieling, A.] Univ Twente, Fac Geoinformat Sci & Earth Observat, POB 217, NL-7500 AE Enschede, Netherlands.
[Yengoh, G. T.] Lund Univ, Ctr Sustainabil Studies, S-22362 Lund, Sweden.
[Anyamba, A.] Natl Aeronaut & Space Adm, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD USA.
[Ummenhofer, C. C.] Woods Hole Oceanog Inst, Dept Phys Oceanog, Woods Hole, MA 02543 USA.
RP Abdi, AM (reprint author), Lund Univ, Dept Phys Geog & Ecosyst Sci, Solvegatan 12, S-22362 Lund, Sweden.
EM hakim.abdi@gmail.com
RI Vrieling, Anton/B-2639-2012;
OI Vrieling, Anton/0000-0002-7979-1540; Abdi, PhD,
Abdulhakim/0000-0001-6486-8747
FU Swedish National Space Board [100/11]; Royal Physiographic Society in
Lund; Lund University Center for Studies of Carbon Cycle and Climate
Interactions (LUCCI); NSF [OCE-1203892]
FX We thank Dan Metcalfe, Lina Eklund, A.J. (Han) Dolman, and Katharina
Waha for their insight and comments during early stages of the
manuscript. We also thank the programming assistance provided by the
volunteers at the Stack Overflow and Cross Validated online communities.
Funding for this project was provided by the Swedish National Space
Board (contract no. 100/11 to J.A.). A.M.A. received support from the
Royal Physiographic Society in Lund and the Lund University Center for
Studies of Carbon Cycle and Climate Interactions (LUCCI). C.C.U. was
supported by NSF grant OCE-1203892.
NR 49
TC 0
Z9 0
U1 14
U2 14
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0165-0009
EI 1573-1480
J9 CLIMATIC CHANGE
JI Clim. Change
PD SEP
PY 2016
VL 138
IS 1-2
BP 111
EP 125
DI 10.1007/s10584-016-1730-1
PG 15
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DU3UT
UT WOS:000382138400009
ER
PT J
AU Morgan, D
Subramanian, GP
Chung, SJ
Hadaegh, FY
AF Morgan, Daniel
Subramanian, Giri P.
Chung, Soon-Jo
Hadaegh, Fred Y.
TI Swarm assignment and trajectory optimization using variable-swarm,
distributed auction assignment and sequential convex programming
SO INTERNATIONAL JOURNAL OF ROBOTICS RESEARCH
LA English
DT Article
ID FORMATION FLYING GUIDANCE; MODEL-PREDICTIVE CONTROL; SATELLITE CLUSTERS;
MULTIPLE ROBOTS; SPACECRAFT; ALGORITHM; STRATEGIES; OPTIMALITY; NETWORKS
AB This paper presents a distributed, guidance and control algorithm for reconfiguring swarms composed of hundreds to thousands of agents with limited communication and computation capabilities. This algorithm solves both the optimal assignment and collision-free trajectory generation for robotic swarms, in an integrated manner, when given the desired shape of the swarm ( without pre-assigned terminal positions). The optimal assignment problem is solved using a distributed auction assignment that can vary the number of target positions in the assignment, and the collision-free trajectories are generated using sequential convex programming. Finally, model predictive control is used to solve the assignment and trajectory generation in real time using a receding horizon. The model predictive control formulation uses current state measurements to resolve for the optimal assignment and trajectory. The implementation of the distributed auction algorithm and sequential convex programming using model predictive control produces the swarm assignment and trajectory optimization ( SATO) algorithm that transfers a swarm of robots or vehicles to a desired shape in a distributed fashion. Once the desired shape is uploaded to the swarm, the algorithm determines where each robot goes and how it should get there in a fuel-efficient, collision-free manner. Results of flight experiments using multiple quadcopters show the effectiveness of the proposed SATO algorithm.
C1 [Morgan, Daniel; Subramanian, Giri P.; Chung, Soon-Jo] Univ Illinois, Urbana, IL USA.
[Hadaegh, Fred Y.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Chung, SJ (reprint author), Univ Illinois, Dept Aerosp Engn, Urbana, IL 61801 USA.; Chung, SJ (reprint author), Univ Illinois, Coordinated Sci Lab, Urbana, IL 61801 USA.
EM sjchung@illinois.edu
FU National Aeronautics and Space Administration; NASA Office of the Chief
Technologist Space Technology Research Fellowship; Air Force Office of
Scientific Research (AFOSR) [FA95501210193]
FX This research was carried out in part at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. (C)2016 California Institute of
Technology. This work was supported by a NASA Office of the Chief
Technologist Space Technology Research Fellowship and an Air Force
Office of Scientific Research (AFOSR grant number FA95501210193).
Government sponsorship acknowledged.
NR 43
TC 1
Z9 1
U1 7
U2 7
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0278-3649
EI 1741-3176
J9 INT J ROBOT RES
JI Int. J. Robot. Res.
PD SEP
PY 2016
VL 35
IS 10
BP 1261
EP 1285
DI 10.1177/0278364916632065
PG 25
WC Robotics
SC Robotics
GA DV5PY
UT WOS:000382981300006
ER
PT J
AU Schonberg, WP
Hull, SM
AF Schonberg, William P.
Hull, Scott M.
TI Current Design Criteria for MMOD Impact of Metallic Pressurized Tanks
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
ID HYPERVELOCITY IMPACT; VESSELS
AB Most spacecraft have at least one pressurized vessel on board. For robotic spacecraft, it is usually a liquid propellant tank or battery. For human spacecraft, there are also pressurized living quarters and life-support systems. One of the design considerations of such spacecraft is the possible damage that might occur in the event of an on-orbit impact by a micrometeoroid or orbital debris (MMOD) particle. While considerable energy and effort has been expended in the study of the response of nonpressurized spacecraft components to these kinds of impacts, relatively few studies have been conducted on the pressurized elements of such spacecraft. In addition, the design criteria currently used by the National Aeronautics and Space Administration (NASA) for pressurized tanks operating in the MMOD environment have not been tested or scrutinized since they were first proposed nearly 45 years ago. This paper reviews current NASA design criteria for pressurized vessels and offers suggestions for next steps in their further development. (C) 2016 American Society of Civil Engineers.
C1 [Schonberg, William P.] Missouri Univ Sci & Technol, Dept Civil Architectural & Environm Engn, 1401 N Pine St, Rolla, MO 65409 USA.
[Hull, Scott M.] NASA, Goddard Space Flight Ctr, Mission Engn & Syst Anal Div, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
RP Schonberg, WP (reprint author), Missouri Univ Sci & Technol, Dept Civil Architectural & Environm Engn, 1401 N Pine St, Rolla, MO 65409 USA.
EM wschon@mst.edu
FU NASA/Jet Propulsion Laboratory; NASA/Engineering Safety Center
FX The authors wish to extend their gratitude to the NASA/Jet Propulsion
Laboratory and the NASA/Engineering Safety Center for providing the
support that made this study possible.
NR 24
TC 0
Z9 0
U1 1
U2 1
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
EI 1943-5525
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD SEP
PY 2016
VL 29
IS 5
DI 10.1061/(ASCE)AS.1943-5525.0000635
PG 4
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA DV7VJ
UT WOS:000383145800024
ER
PT J
AU Salinas, A
Altecor, A
Lizcano, M
Lozano, K
AF Salinas, A.
Altecor, A.
Lizcano, M.
Lozano, K.
TI Production of beta-Silicon Carbide Nanofibers using the Forcespinning
(R) Method
SO JOURNAL OF CERAMIC SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Silicon carbide; high-temperature materials; ceramic nanofibers;
Forcespinning (R)
ID FIBERS; NANOWIRES
AB Silicon carbide (SiC) nanofibers were produced on a large scale using the Forcespinning (R) method. Non-oxide ceramics such as SiC are known for their low density, oxidation resistance, thermal stability, and wear resistance. The nanofibers were prepared using a solution-based method with polystyrene and polycarbomethylsilane as the precursor materials. Fiber spinning was performed under different parameters to obtain high yield, fiber homogeneity, and small diameters. The fibers were spun under a controlled nitrogen environment to prevent fiber oxidation. The resultant nonwoven nanofiber mats were then subjected to different heat treatments to evaluate the effect of these on the crystalline structure. Characterization was conducted using scanning electron microscopy, x-ray diffraction, and thermogravimetric analysis. The results show high yield, semi-continuous bead-free nanofibers with diameters ranging from 280 nm to 2 micron depending on the selected processing parameters. The sintered precursors show formation of SiC nanofibers with a beta phase crystalline structure and oxygen content below 15 %.
C1 [Salinas, A.; Altecor, A.; Lozano, K.] Univ Texas Pan Amer, Dept Mech Engn, Edinburg, TX 78539 USA.
[Lizcano, M.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Salinas, A (reprint author), Univ Texas Pan Amer, Dept Mech Engn, Edinburg, TX 78539 USA.
EM asalinasz73@broncs.utpa.edu
FU National Science Foundation under DMR grant [1523577]
FX The authors gratefully acknowledge financial support received from the
National Science Foundation under DMR grant No. 1523577 (PREM- UTRGV-UMN
Partnership for Fostering Innovation by Bridging Excellence in Research
and Student Success). We are also grateful to the Biology Department at
the University of Texas Rio Grande Valley for allowing use of the EDS
instrument.
NR 26
TC 0
Z9 0
U1 5
U2 5
PU GOLLER VERLAG GMBH
PI BADEN BADEN
PA ASCHMATTSTRASSE 8, D-76532 BADEN BADEN, GERMANY
SN 2190-9385
J9 J CERAM SCI TECHNOL
JI J. Ceram. Sci. Technol.
PD SEP
PY 2016
VL 7
IS 3
BP 229
EP 234
DI 10.4416/JCST2016-00026
PG 6
WC Materials Science, Ceramics
SC Materials Science
GA DW0FO
UT WOS:000383316500002
ER
PT J
AU Li, T
Calvo, N
Yue, J
Russell, JM
Smith, AK
Mlynczak, MG
Chandran, A
Dou, XK
Liu, AZ
AF Li, Tao
Calvo, Natalia
Yue, Jia
Russell, James M., III
Smith, Anne K.
Mlynczak, Martin G.
Chandran, Amal
Dou, Xiankang
Liu, Alan Z.
TI Southern Hemisphere Summer Mesopause Responses to El Nino-Southern
Oscillation
SO JOURNAL OF CLIMATE
LA English
DT Article
ID STRATOSPHERE; ATMOSPHERE; MIDDLE; MODEL; TEMPERATURES; CIRCULATION; ENSO
AB In the Southern Hemisphere (SH) polar region, satellite observations reveal a significant upper-mesosphere cooling and a lower-thermosphere warming during warm ENSO events in December. An opposite pattern is observed in the tropical mesopause region. The observed upper-mesosphere cooling agrees with a climate model simulation. Analysis of the simulation suggests that enhanced planetary wave (PW) dissipation in the Northern Hemisphere (NH) high-latitude stratosphere during El Nino strengthens the Brewer-Dobson circulation and cools the equatorial stratosphere. This increases the magnitude of the SH stratosphere meridional temperature gradient and thus causes the anomalous stratospheric easterly zonal wind and early breakdown of the SH stratospheric polar vortex. The resulting perturbation to gravity wave (GW) filtering causes anomalous SH mesospheric eastward GW forcing and polar upwelling and cooling. In addition, constructive inference of ENSO and quasi-biennial oscillation (QBO) could lead to stronger stratospheric easterly zonal wind anomalies at the SH high latitudes in November and December and early breakdown of the SH stratospheric polar vortex during warm ENSO events in the easterly QBO phase (defined by the equatorial zonal wind at similar to 25 hPa). This would in turn cause much more SH mesospheric eastward GW forcing and much colder polar temperatures, and hence it would induce an early onset time of SH summer polar mesospheric clouds (PMCs). The opposite mechanism occurs during cold ENSO events in the westerly QBO phase. This implies that ENSO together with QBO could significantly modulate the breakdown time of SH stratospheric polar vortex and the onset time of SH PMC.
C1 [Li, Tao; Dou, Xiankang] Univ Sci & Technol China, Sch Earth & Space Sci, CAS Key Lab Geospace Environm, Hefei 230026, Anhui, Peoples R China.
[Li, Tao; Dou, Xiankang] Univ Sci & Technol China, Sch Earth & Space Sci, Mengcheng Natl Geophys Observ, Hefei 230026, Anhui, Peoples R China.
[Calvo, Natalia] Univ Complutense Madrid, Dept Fis Tierra 2, Madrid, Spain.
[Yue, Jia; Russell, James M., III] Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA.
[Smith, Anne K.] Natl Ctr Atmospher Res, Atmospher Chem Observat & Modeling Lab, POB 3000, Boulder, CO 80307 USA.
[Mlynczak, Martin G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Chandran, Amal] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[Liu, Alan Z.] Embry Riddle Aeronaut Univ, Dept Phys Sci, Daytona Beach, FL 32114 USA.
RP Li, T (reprint author), Univ Sci & Technol China, Sch Earth & Space Sci, 96 Jinzhai Rd, Hefei 230026, Anhui, Peoples R China.
EM litao@ustc.edu.cn
RI Dou, xiankang/M-9106-2013; Yue, Jia/D-8177-2011; Li, Tao/J-8950-2014
OI Li, Tao/0000-0002-5100-4429
FU National Natural Science Foundation of China [41225017, 41421063];
National Basic Research Program of China [2012CB825605]; NSF
[AGS-1115249, AGS-1110199]; Spanish Ministry of Economy and
Competitiveness through the PALEOSTRAT project [CGL2015-69699-R];
European Project under program [603557-STRATOCLIM, FP7-ENV.2013.6.1-2];
NASA AIM satellite mission; NASA TIMED satellite mission; NASA SABER
Grant [NNX15AD22G]; NASA TIMED satellite project; National Science
Foundation [AGS-1115249, AGS-1110199]
FX TL would like to thank Han-Li Liu and Chengyun Yang for helpful
discussion. TL and XD are supported by the National Natural Science
Foundation of China Grants 41225017 and 41421063 and the National Basic
Research Program of China Grant 2012CB825605. TL's visit to ERAU is
partially supported by the NSF Grants AGS-1115249 and AGS-1110199. NC
acknowledges partial support from the Spanish Ministry of Economy and
Competitiveness through the PALEOSTRAT project (Paleomodelization desde
una perspective estratoferica; Ref. CGL2015-69699-R) and the European
Project 603557-STRATOCLIM under program FP7-ENV.2013.6.1-2. JY is
supported by the NASA AIM and TIMED satellite missions. JMR is supported
under NASA SABER Grant NNX15AD22G. MGM is supported by the NASA TIMED
satellite project. AZL is supported by National Science Foundation
Grants AGS-1115249 and AGS-1110199. The WACCM 3.5 results were obtained
from the Atmospheric Chemistry Division at the National Center for
Atmospheric Research. The radiosonde dataset is downloaded from
http://www.geo.fu-berlin.de/en/met/ag/strat/produkte/qbo/index.html. We
want to thank Bodil Karlsson and two other anonymous reviewers for their
constructive comments on this paper.
NR 28
TC 1
Z9 1
U1 5
U2 5
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 SEP 1
PY 2016
VL 29
IS 17
BP 6319
EP 6328
DI 10.1175/JCLI-D-15-0816.1
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DV3DO
UT WOS:000382801400016
ER
PT J
AU Russell, RP
Lantukh, D
Broschart, SB
AF Russell, Ryan P.
Lantukh, Demyan
Broschart, Stephen B.
TI Heliotropic Orbits with Zonal Gravity and Shadow Perturbations:
Application at Bennu
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article
ID SOLAR-RADIATION PRESSURE; ASTEROID 101955 BENNU; PLANETARY OBLATENESS;
EVEN HARMONICS; DUST DYNAMICS; SATELLITE; DENSITY; MOTION
AB Heliotropic orbits provide long-lifetime low-altitude orbits in the presence of large J2 and solar radiation pressure perturbations. Formal inclusion of high-degree zonal gravity harmonics and simple shadowing provides a more realistic model to initiate the search for heliotropic orbits at irregular primitive bodies like Bennu, which is the target of the OSIRIS-Rex mission. The constrained, doubly averaged potential and the Lagrange planetary equations yield a single equation to enforce the heliotropic constraint. The equation is solved for inclinations across a range of semimajor axes and eccentricities, providing a surface of potential solutions. The fast process allows for MonteCarlo simulations to assess the likelihood of a heliotropic orbit existing in the presence of parameter uncertainty. The existence of heliotropic orbits is shown to be reasonably robust to uncertainty in the solar radiation pressure acceleration and reference gravity parameters for Bennu.
C1 [Russell, Ryan P.; Lantukh, Demyan] Univ Texas Austin, Dept Aerosp Engn & Engn Mech, Austin, TX 78712 USA.
[Broschart, Stephen B.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Russell, RP (reprint author), Univ Texas Austin, Dept Aerosp Engn & Engn Mech, Austin, TX 78712 USA.
EM ryan.russell@utexas.edu; demyan@utexas.edu;
Stephen.B.Broschart@jpl.nasa.gov
FU NASA Office of the Chief Technologist via a NASA Space Technology
Research Fellowship [NNX12AI77H]; W. M. Keck Foundation; NASA
FX This work was supported in part by the NASA Office of the Chief
Technologist via a NASA Space Technology Research Fellowship grant
(NNX12AI77H). In particular, the authors thank Claudia Meyer for
continued interest and support of the project. The authors also thank
the W. M. Keck Foundation for supporting, in part, the presented work
through the W. M. Keck Foundation Endowed Graduate Fellowship in
Engineering. Part of the work described here was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with NASA.
NR 22
TC 0
Z9 0
U1 2
U2 2
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 SEP
PY 2016
VL 39
IS 9
BP 1925
EP 1933
DI 10.2514/1.G001279
PG 9
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA DV9LH
UT WOS:000383261500001
ER
PT J
AU Swei, SSM
Fusco, JC
Nakamura, RH
AF Swei, Sean S. M.
Fusco, Jesse C.
Nakamura, Robert H.
TI Design of Sun-Safe Controllers for Lunar Atmosphere and Dust Environment
Explorer
SO JOURNAL OF GUIDANCE CONTROL AND DYNAMICS
LA English
DT Article
AB This paper presents the development of sun-safe controllers, which are designed to keep the spacecraft power positive and thermally balanced in the event an anomaly is detected. Employed by NASA's Lunar Atmosphere and Dust Environment Explorer, the controllers use the measured sun vector and the spacecraft body rates for feedback control. To improve the accuracy of sun vector estimation, the least-square minimization approach is applied to process the sensor data. A rotation with respect to the sun vector, which is proven to be effective in mitigating the momentum buildup due to the lunar gravity gradient, hence significantly extending the sun-safe duration, is commanded. To validate the controllers, the Lunar Atmosphere and Dust Environment Explorer spacecraft model engaging the sun-safe mode is first simulated and then compared with the actual Lunar Atmosphere and Dust Environment Explorer orbital flight data. The results demonstrate the applicability of the proposed sun-safe controllers.
C1 [Swei, Sean S. M.] NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA.
[Fusco, Jesse C.; Nakamura, Robert H.] NASA, Ames Res Ctr, Engn Syst Div, Moffett Field, CA 94035 USA.
RP Swei, SSM (reprint author), NASA, Ames Res Ctr, Intelligent Syst Div, Moffett Field, CA 94035 USA.
NR 9
TC 1
Z9 1
U1 0
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 SEP
PY 2016
VL 39
IS 9
BP 2022
EP 2033
DI 10.2514/1.G000270
PG 12
WC Engineering, Aerospace; Instruments & Instrumentation
SC Engineering; Instruments & Instrumentation
GA DV9LH
UT WOS:000383261500008
ER
PT J
AU Sung, K
Yu, SS
Pearson, J
Pirali, O
Tchana, FK
Manceron, L
AF Sung, Keeyoon
Yu, Shanshan
Pearson, John
Pirali, Olivier
Tchana, Fridolin Kwabia
Manceron, Laurent
TI Far-infrared (NH3)-N-14 line positions and intensities measured with a
FT-IR and AILES beamline, Synchrotron SOLEIL
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE Ammonia spectroscopy; Ammonia line intensity; NH3 far-infrared
transitions; Inversion-rotation; FT-IR measurements; AILES beamline
ID SELF-BROADENING COEFFICIENTS; LASER STARK SPECTROSCOPY;
MOLECULAR-SPECTROSCOPY; COLOGNE DATABASE; ENERGY-LEVELS; NH3; AMMONIA;
BANDS; MICROWAVE; STATE
AB Extensive measurements of line positions and intensities are reported for the inversion-rotation and rovibrational transitions of (NH3)-N-14 in the 50-660 cm(-1) region. This study analyzes high-resolution (0.00167 cm(-1), unapodized) Fourier-transform spectra of high purity (99.5%) normal ammonia sample obtained using the AILES beamline of Synchrotron SOLEIL. The experimental conditions are designed to study transitions with intensities weaker than 1 x 10(-22) cm(-1)/(molecule cm(-2)) at room temperature. Line positions and intensities of more than 2830 transitions of (NH3)-N-14 are measured and compiled after proper quality control; the features from minor isotopologues ((NH3)-N-15 and NH2D) and H2O are identified and excluded. Based on the predictions of recent work from the empirical Hamiltonian modeling, systematic quantum assignments are made for 2047 transitions from eight bands including four inversion rotation (gs, v(2), 2v(2), and v(4)) and four ro-vibrational bands (v(2)-gs, 2v(2)-v(2), v(4)-v(2), and 2v(2)-v(4)), as well as covering their Delta K = 3 forbidden transitions. The measured line positions for the assigned transitions are in an excellent agreement (typically better than 0.001 cm(-1)) with the predictions in a wide range of J and K for all the eight bands. The comparison with the HITRAN 2012 database is also satisfactory, although systematic offsets are seen for transitions with high J and K and those from weak bands. Also we note that out of the eight bands, the 2v(2)-v(4) has not been listed in the HITRAN 2012 database. Differences of 20% are seen between our measured and calculated intensities depending on the bands. For line positions, greater differences are found for some NH3 bands in HITRAN 2012 than recent predictions. Measurements of the individual line positions and intensities are presented for the eight bands, and the final spectroscopic line positions and intensities are compiled as an electronic supplement. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Sung, Keeyoon; Yu, Shanshan; Pearson, John] CALTECH, Jet Prop Lab, M-S 200-105,4800 Oak Grove Dr, Pasadena, CA 91125 USA.
[Pirali, Olivier; Manceron, Laurent] LOrme Merisiers St Aubin, Synchrotron SOLEIL, AILES Beamline, F-91192 Gif Sur Yvette, France.
[Pirali, Olivier] Univ Paris Saclay, Univ Paris 11, CNRS, ISMO, F-91405 Orsay, France.
[Tchana, Fridolin Kwabia] UPEC, CNRS, UMR 7583, LISA, 61 Ave Gen Gaulle, F-94010 Creteil, France.
[Tchana, Fridolin Kwabia] UPD, 61 Ave Gen Gaulle, F-94010 Creteil, France.
[Manceron, Laurent] Univ Paris 06, CNRS, UMR 8233, MONARIS, Paris, France.
RP Sung, K (reprint author), CALTECH, Jet Prop Lab, M-S 200-105,4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM ksung@jpl.nasa.gov
RI Yu, Shanshan/D-8733-2016; Sung, Keeyoon/I-6533-2015
FU Synchrotron SOLEIL [2013080]; Astrophysics Research and Analysis (APRA)
Program under the National Aeronautics and Space Administration; SOLEIL;
LISA
FX K. Sung and S. Yu are grateful to Linda R. Brown for useful discussion
on the NH3 spectroscopy and designing the experimental study.
The JPL authors also acknowledge the Synchrotron SOLEIL for granting us
with the AILES beamline time (project #2013080). Research described in
this work was performed at Jet Propulsion Laboratory, California
Institute of Technology, and was supported by the Astrophysics Research
and Analysis (APRA) Program under the National Aeronautics and Space
Administration. F.K.T. and L.M. acknowledge SOLEIL and LISA support.
NR 64
TC 0
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U1 4
U2 4
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 SEP
PY 2016
VL 327
SI SI
BP 1
EP 20
DI 10.1016/j.jms.2016.06.011
PG 20
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA DV8WY
UT WOS:000383218600001
ER
PT J
AU Orphal, J
Staehelin, J
Tamminen, J
Braathen, G
De Backer, MR
Bais, A
Balis, D
Barbe, A
Bhartia, PK
Birk, M
Burkholder, JB
Chance, K
von Clarmann, T
Cox, A
Degenstein, D
Evans, R
Flaud, JM
Flittner, D
Godin-Beekmann, S
Gorshelev, V
Gratien, A
Hare, E
Janssen, C
Kyrola, E
McElroy, T
McPeters, R
Pastel, M
Petersen, M
Petropavlovskikh, I
Picquet-Varrault, B
Pitts, M
Labow, G
Rotger-Languereau, M
Leblanc, T
Lerot, C
Liu, X
Moussay, P
Redondas, A
Van Roozendael, M
Sander, SP
Schneider, M
Serdyuchenko, A
Veefkind, P
Viallon, J
Viatte, C
Wagner, G
Weber, M
Wielgosz, RI
Zehner, C
AF Orphal, Johannes
Staehelin, Johannes
Tamminen, Johanna
Braathen, Geir
De Backer, Marie -Renee
Bais, Alkiviadis
Balis, Dimitris
Barbe, Alain
Bhartia, Pawan K.
Birk, Manfred
Burkholder, James B.
Chance, Kelly
von Clarmann, Thomas
Cox, Anthony
Degenstein, Doug
Evans, Robert
Flaud, Jean-Marie
Flittner, David
Godin-Beekmann, Sophie
Gorshelev, Viktor
Gratien, Aline
Hare, Edward
Janssen, Christof
Kyrola, Erkki
McElroy, Thomas
McPeters, Richard
Pastel, Maud
Petersen, Michael
Petropavlovskikh, Irina
Picquet-Varrault, Benedicte
Pitts, Michael
Labow, Gordon
Rotger-Languereau, Maud
Leblanc, Thierry
Lerot, Christophe
Liu, Xiong
Moussay, Philippe
Redondas, Alberto
Van Roozendael, Michel
Sander, Stanley P.
Schneider, Matthias
Serdyuchenko, Anna
Veefkind, Pepijn
Viallon, Joele
Viatte, Camille
Wagner, Georg
Weber, Mark
Wielgosz, Robert I.
Zehner, Claus
TI Absorption cross-sections of ozone in the ultraviolet and visible
spectral regions: Status report 2015
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE Ozone; Absorption; Cross sections; Atmosphere; Remote sensing; Reference
data
ID 10 MU-M; TEMPERATURE-DEPENDENCE; PROFILE RETRIEVALS; MONITORING
INSTRUMENT; UV SPECTROSCOPY; TOTAL COLUMN; STRAY LIGHT; NM REGION;
BREWER; O-3
AB The activity "Absorption Cross-Sections of Ozone" (ACSO) started in 2008 as a joint initiative of the International Ozone Commission (IO3C), the World Meteorological Organization (WMO) and the IGACO ("Integrated Global Atmospheric Chemistry Observations") O-3/UV subgroup to study, evaluate, and recommend the most suitable ozone absorption cross-section laboratory data to be used in atmospheric ozone measurements. The evaluation was basically restricted to ozone absorption cross-sections in the UV range with particular focus on the Huggins band. Up until now, the data of Bass and Paur published in 1985 (BP, 1985) are still officially recommended for such measurements. During the last decade it became obvious that BP (1985) cross-section data have deficits for use in advanced space-borne ozone measurements. At the same time, it was recognized that the origin of systematic differences in ground-based measurements of ozone required further investigation, in particular whether the BP (1985) cross-section data might contribute to these differences.
In ACSO, different sets of laboratory ozone absorption cross-section data (including their dependence on temperature) of the group of Reims (France) (Brion et al., 1993, 1998, 1992, 1995, abbreviated as BDM, 1995) and those of Serdyuchenko et al. (2014), and Gorshelev et al. (2014), (abbreviated as SER, 2014) were examined for use in atmospheric ozone measurements in the Huggins band.
In conclusion, ACSO recommends:
The spectroscopic data of BP (1985) should no longer be used for retrieval of atmospheric ozone measurements
For retrieval of ground-based instruments of total ozone and ozone profile measurements by the Umkehr method performed by Brewer and Dobson instruments data of SER (2014) are recommended to be used. When SER (2014) is used, the difference between total ozone measurements of Brewer and Dobson instruments are very small and the difference between Dobson measurements at AD and CD wavelength pairs are diminished.
For ground-based Light Detection and Ranging (LIDAR) measurements the use of BDM (1995) or SER (2014) is recommended.
For satellite retrieval the presently widely used data of BDM (1995) should be used because SER (2014) seems less suitable for retrievals that use wavelengths close to 300 nm due to a deficiency in the signal-to-noise ratio in the SER (2014) dataset.
The work of ACSO also showed:
The need to continue laboratory cross-section measurements of ozone of highest quality. The importance of careful characterization of the uncertainties of the laboratory measurements.
The need to extend the scope of such studies to other wavelength ranges (particularly to cover not only the Huggins band but also the comparison with the mid-infrared region).
The need for regular cooperation of experts in spectral laboratory measurements and specialists in atmospheric (ozone) measurements. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Orphal, Johannes; von Clarmann, Thomas; Schneider, Matthias] KIT, Inst Meteorol & Climate Res IMK, Karlsruhe, Germany.
[Staehelin, Johannes] Swiss Fed Inst Technol, Zurich, Switzerland.
[Tamminen, Johanna; Kyrola, Erkki] FMI, Helsinki, Finland.
[Braathen, Geir] WMO, Geneva, Switzerland.
[De Backer, Marie -Renee; Barbe, Alain; Rotger-Languereau, Maud] CNRS, GSMA, Reims, France.
[De Backer, Marie -Renee; Barbe, Alain] Univ Reims, Reims, France.
[Bais, Alkiviadis; Balis, Dimitris] Aristotele Univ Thessaloniki, Thessaloniki, Greece.
[Bhartia, Pawan K.; McPeters, Richard; Labow, Gordon] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Birk, Manfred; Wagner, Georg] German Aerosp Ctr DLR, Oberpfaffenhofen, Germany.
[Evans, Robert; Petropavlovskikh, Irina] Univ Colorado, CIRES, Boulder, CO 80309 USA.
[Chance, Kelly; Liu, Xiong] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
[Cox, Anthony] Univ Cambridge, Cambridge, England.
[Degenstein, Doug] Univ Saskatchewan, Saskatoon, SK, Canada.
[Flaud, Jean-Marie; Gratien, Aline; Picquet-Varrault, Benedicte] CNRS, LISA, Creteil, France.
[Flaud, Jean-Marie; Gratien, Aline; Picquet-Varrault, Benedicte] Univ Paris Est, Creteil, France.
[Flittner, David; Pitts, Michael] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Godin-Beekmann, Sophie; Pastel, Maud] CNRS, LATMOS, Paris, France.
[Godin-Beekmann, Sophie; Pastel, Maud] UVSQ, Paris, France.
[Gorshelev, Viktor; Serdyuchenko, Anna; Weber, Mark] Univ Bremen, Bremen, Germany.
[Hare, Edward] Environm Canada, Toronto, ON, Canada.
[Janssen, Christof] Univ Paris 06, Sorbonne Univ, LERMA, IPSL, Paris, France.
[Janssen, Christof] PSL Res Univ, Observ Paris, Paris, France.
[Janssen, Christof] CNRS, Paris, France.
[McElroy, Thomas] Univ Toronto, Toronto, ON, Canada.
[Petersen, Michael; Moussay, Philippe; Viallon, Joele; Wielgosz, Robert I.] BIPM, Sevres, France.
[Leblanc, Thierry; Sander, Stanley P.] NASA, JPL, Pasadena, CA USA.
[Lerot, Christophe; Van Roozendael, Michel] Belgian Inst Space Aeron BIRA IASB, Brussels, Belgium.
[Redondas, Alberto] State Meteorol Agcy AEMET, Izana, Spain.
[Veefkind, Pepijn] KNMI, De Bilt, Netherlands.
[Viatte, Camille] CALTECH, Pasadena, CA 91125 USA.
[Zehner, Claus] ESA, ESRIN, Frascati, Italy.
[Burkholder, James B.] NOAA, Earth Syst Res Lab, Div Chem Sci, Boulder, CO USA.
[Petropavlovskikh, Irina] NOAA, Global Monitoring Div, Boulder, CO USA.
[Petersen, Michael] Univ Neuchatel, CH-2000 Neuchatel, Switzerland.
RP Orphal, J (reprint author), KIT, Inst Meteorol & Climate Res IMK, Karlsruhe, Germany.
EM orphal@kit.edu
RI Schneider, Matthias/B-1441-2013; Liu, Xiong/P-7186-2014; Bais,
Alkiviadis/D-2230-2009; Tamminen, Johanna/D-7959-2014; Manager, CSD
Publications/B-2789-2015;
OI Liu, Xiong/0000-0003-2939-574X; Bais, Alkiviadis/0000-0003-3899-2001;
Tamminen, Johanna/0000-0003-3095-0069; Kyrola, Erkki/0000-0001-9197-9549
FU EU FP7 programme [284421]; NASA [NNX09AJ24G]
FX The work of Maud Pastel was performed in the frame of the NORS project
(Demonstration Network Of ground-based Remote Sensing Observations in
support of the Copernicus Atmospheric Service), funded by the EU FP7
programme under grant agreement no 284421. The work of Irina
Petropavlovskikh was supported by NASA Grant No. NNX09AJ24G (Enhancement
of ozone products from established Brewer ground-based networks for
validation of satellite-derived stratospheric ozone change). Johanna
Tamminen would like to thank the Finnish Academy INQUIRE project.
NR 76
TC 4
Z9 4
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 0022-2852
EI 1096-083X
J9 J MOL SPECTROSC
JI J. Mol. Spectrosc.
PD SEP
PY 2016
VL 327
SI SI
BP 105
EP 121
DI 10.1016/j.jms.2016.07.007
PG 17
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA DV8WY
UT WOS:000383218600006
ER
PT J
AU Dreessen, J
Sullivan, J
Delgado, R
AF Dreessen, Joel
Sullivan, John
Delgado, Ruben
TI Observations and impacts of transported Canadian wildfire smoke on ozone
and aerosol air quality in the Maryland region on June 9-12, 2015
SO JOURNAL OF THE AIR & WASTE MANAGEMENT ASSOCIATION
LA English
DT Article; Proceedings Paper
CT 7th International Workshop on Air Quality Forecasting Research (IWAQFR)
CY SEP 01-03, 2015
CL College Park, MD
ID VOLATILE ORGANIC-COMPOUNDS; SOUTHERN CALIFORNIA WILDFIRES; FOREST-FIRE
EMISSIONS; UNITED-STATES; PARTICULATE MATTER; NITROGEN-OXIDES;
CLIMATE-CHANGE; URBAN AREA; BOREAL; POLLUTION
AB Canadian wildfire smoke impacted air quality across the northern Mid-Atlantic (MA) of the United States during June 9-12, 2015. A multiday exceedance of the new 2015 70-ppb National Ambient Air Quality Standard (NAAQS) for ozone (O-3) followed, resulting in Maryland being incompliant with the Environmental Protection Agency's (EPA) revised 2015 O-3 NAAQS. Surface in situ, balloon-borne, and remote sensing observations monitored the impact of the wildfire smoke at Maryland air quality monitoring sites. At peak smoke concentrations in Maryland, wildfire-attributable volatile organic compounds (VOCs) more than doubled, while non-NOx oxides of nitrogen (NOz) tripled, suggesting long range transport of NOx within the smoke plume. Peak daily average PM2.5 was 32.5 mu g m(-3) with large fractions coming from black carbon (BC) and organic carbon (OC), with a synonymous increase in carbon monoxide (CO) concentrations. Measurements indicate that smoke tracers at the surface were spatially and temporally correlated with maximum 8-hr O-3 concentrations in the MA, all which peaked on June 11. Despite initial smoke arrival late on June 9, 2015, O-3 production was inhibited due to ultraviolet (UV) light attenuation, lower temperatures, and nonoptimal surface layer composition. Comparison of Community Multiscale Air Quality (CMAQ) model surface O-3 forecasts to observations suggests 14 ppb additional O-3 due to smoke influences in northern Maryland. Despite polluted conditions, observations of a nocturnal low-level jet (NLLJ) and Chesapeake Bay Breeze (BB) were associated with decreases in O-3 in this case. While infrequent in the MA, wildfire smoke may be an increasing fractional contribution to high-O-3 days, particularly in light of increased wildfire frequency in a changing climate, lower regional emissions, and tighter air quality standards.Implications: The presented event demonstrates how a single wildfire event associated with an ozone exceedance of the NAAQS can prevent the Baltimore region from complying with lower ozone standards. This relatively new problem in Maryland is due to regional reductions in NOx emissions that led to record low numbers of ozone NAAQS violations in the last 3 years. This case demonstrates the need for adequate means to quantify and justify ozone impacts from wildfires, which can only be done through the use of observationally based models. The data presented may also improve future air quality forecast models.
C1 [Dreessen, Joel] Maryland Dept Environm, Air Monitoring Program, 1800 Washington Blvd, Baltimore, MD 21230 USA.
[Sullivan, John] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD USA.
[Delgado, Ruben] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
RP Dreessen, J (reprint author), Maryland Dept Environm, Air Monitoring Program, 1800 Washington Blvd, Baltimore, MD 21230 USA.
EM joel.dreessen@maryland.gov
NR 64
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U1 19
U2 19
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.
PD SEP
PY 2016
VL 66
IS 9
SI SI
BP 842
EP 862
DI 10.1080/10962247.2016.1161674
PG 21
WC Engineering, Environmental; Environmental Sciences; Meteorology &
Atmospheric Sciences
SC Engineering; Environmental Sciences & Ecology; Meteorology & Atmospheric
Sciences
GA DV5IE
UT WOS:000382959700003
PM 26963934
ER
PT J
AU Albers, M
Zhu, S
Ayangeakaa, AD
Janssens, RVF
Gellanki, J
Ragnarsson, I
Alcorta, M
Baugher, T
Bertone, PF
Carpenter, MP
Chiara, CJ
Chowdhury, P
David, HM
Deacon, AN
DiGiovine, B
Gade, A
Hoffman, CR
Kondev, FG
Lauritsen, T
Lister, CJ
McCutchan, EA
Nair, C
Rogers, AM
Seweryniak, D
AF Albers, M.
Zhu, S.
Ayangeakaa, A. D.
Janssens, R. V. F.
Gellanki, J.
Ragnarsson, I.
Alcorta, M.
Baugher, T.
Bertone, P. F.
Carpenter, M. P.
Chiara, C. J.
Chowdhury, P.
David, H. M.
Deacon, A. N.
DiGiovine, B.
Gade, A.
Hoffman, C. R.
Kondev, F. G.
Lauritsen, T.
Lister, C. J.
McCutchan, E. A.
Nair, C.
Rogers, A. M.
Seweryniak, D.
TI Single-particle and collective excitations in Ni-62
SO PHYSICAL REVIEW C
LA English
DT Article
ID ROTATIONAL BANDS; TERMINATION; ISOTOPES; NUCLEUS; DECAY
AB Background: Level sequences of rotational character have been observed in several nuclei in the A = 60 mass region. The importance of the deformation-driving pi f(7/2) and nu g(9/2) orbitals on the onset of nuclear deformation is stressed.
Purpose: A measurement was performed in order to identify collective rotational structures in the relatively neutron-rich Ni-62 isotope.
Method: The Mg-26(Ca-48,2 alpha 4n gamma)Ni-62 complex reaction at beam energies between 275 and 320 MeV was utilized. Reaction products were identified in mass (A) and charge (Z) with the fragment mass analyzer (FMA) and gamma rays were detected with the Gammasphere array.
Results: Two collective bands, built upon states of single-particle character, were identified and sizable deformation was assigned to both sequences based on the measured transitional quadrupole moments, herewith quantifying the deformation at high spin.
Conclusions: Based on cranked Nilsson-Strutinsky calculations and comparisons with deformed bands in the A = 60 mass region, the two rotational bands are understood as being associated with configurations involving multiple f(7/2) protons and g(9/2) neutrons, driving the nucleus to sizable prolate deformation.
C1 [Albers, M.; Zhu, S.; Ayangeakaa, A. D.; Janssens, R. V. F.; Alcorta, M.; Bertone, P. F.; Carpenter, M. P.; Chiara, C. J.; David, H. M.; DiGiovine, B.; Hoffman, C. R.; Lauritsen, T.; Lister, C. J.; McCutchan, E. A.; Nair, C.; Rogers, A. M.; Seweryniak, D.] Argonne Natl Lab, Div Phys, Argonne, IL 60439 USA.
[Gellanki, J.] Univ Groningen, KVI CART, NL-9747 AA Groningen, Netherlands.
[Ragnarsson, I.] Lund Univ, LTH, Div Math Phys, S-22100 Lund, Sweden.
[Baugher, T.; Gade, A.] Michigan State Univ, Natl Superconducting Cyclotron Lab, E Lansing, MI 48824 USA.
[Baugher, T.; Gade, A.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Chiara, C. J.] Univ Maryland, Dept Chem & Biochem, College Pk, MD 20742 USA.
[Chowdhury, P.; Lister, C. J.; Rogers, A. M.] Univ Massachusetts Lowell, Dept Phys, Lowell, MA 01854 USA.
[Deacon, A. N.] Univ Manchester, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Kondev, F. G.] Argonne Natl Lab, Nucl Engn Div, 9700 S Cass Ave, Argonne, IL 60439 USA.
[Alcorta, M.] TRIUMF, 4004 Wesbrook Mall, Vancouver, BC V6T 2A3, Canada.
[Bertone, P. F.] Marshall Space Flight Ctr, Bldg 4600 Rideout Rd, Huntsville, AL 35812 USA.
[Chiara, C. J.] US Army Res Lab, Adelphi, MD 20783 USA.
[David, H. M.] GSI Helmholtzzentrum Schwerionenforsch GmbH, D-64291 Darmstadt, Germany.
[McCutchan, E. A.] Brookhaven Natl Lab, Natl Nucl Data Ctr, Upton, NY 11973 USA.
RP Albers, M (reprint author), Argonne Natl Lab, Div Phys, Argonne, IL 60439 USA.
RI Gade, Alexandra/A-6850-2008
OI Gade, Alexandra/0000-0001-8825-0976
FU US Department of Energy, Office of Science, Office of Nuclear Physics
[DE-AC02-06CH11357, DE-FG02-94ER40834, DE-FG02-94ER40848,
DE-FG02-08ER41556]; National Science Foundation [PHY-1102511]; Swedish
Research Council; United Kingdom Science and Technology Facilities
Council (STFC)
FX The authors thank J. P. Greene (ANL) for target preparation and the
ATLAS operations staff for the efficient running of the accelerator
during the experiment. This work was supported in part by the US
Department of Energy, Office of Science, Office of Nuclear Physics,
under Contract No. DE-AC02-06CH11357 and Grant Nos. DE-FG02-94ER40834,
DE-FG02-94ER40848, and DE-FG02-08ER41556, by the National Science
Foundation under Contract No. PHY-1102511, by the Swedish Research
Council, and by the United Kingdom Science and Technology Facilities
Council (STFC). This research used resources of ANL's ATLAS facility,
which is a DOE Office of Science User Facility.
NR 53
TC 0
Z9 0
U1 2
U2 2
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-9985
EI 2469-9993
J9 PHYS REV C
JI Phys. Rev. C
PD SEP 1
PY 2016
VL 94
IS 3
AR 034301
DI 10.1103/PhysRevC.94.034301
PG 10
WC Physics, Nuclear
SC Physics
GA DV6KZ
UT WOS:000383045700001
ER
PT J
AU Sherwood, B
AF Sherwood, Brent
TI Strategic map for exploring the ocean-world Enceladus
SO ACTA ASTRONAUTICA
LA English
DT Article
ID PLUME; FUTURE; LIFE
AB Among the many "ocean worlds" of our solar system, Enceladus appears unique in its combination of astrobiologically relevant and exploration-worthy attributes: extensive liquid-water ocean with active hydrothermal activity, containing salts and organics expressed predictably into space. The Enceladus south polar plume allows direct access to telltale molecules, ions, isotopes, and potential cytofragments in space. Plume mass spectroscopy and sample return, in situ investigation of surface fallback deposits, direct vent exploration, and eventually oceanographic exploration can all be envisioned. However, building consensus to fund such ambitious exploration hinges on acquiring key new data. A roadmap is essential. It could start with cost-capped onramps such as flythrough analysis of the plume, following up on Cassini measurements with modern instruments; and sample return of plume material for analysis on Earth. A methodical mission sequence in which each step depends on emergent results from prior missions would push in situ oceanographic exploration into the second half of this century. Even for this scenario, prioritization by the next planetary Decadal Survey would be pivotal. (C) 2016 IAA Published by Elsevier Ltd. All rights reserved.
C1 [Sherwood, Brent] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
RP Sherwood, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM brent.sherwood@jpl.nasa.gov
FU NASA
FX The author is grateful to several colleagues who shared insights that
were key to formulating the strategic analysis presented here: Linda
Spilker, Christophe Sotin, Jonathan Lunine, Kevin Hand, Hunter Waite,
Hajime Yano, Peter Tsou, and Carolyn Porco.
NR 21
TC 1
Z9 1
U1 9
U2 9
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
EI 1879-2030
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD SEP-OCT
PY 2016
VL 126
SI SI
BP 52
EP 58
DI 10.1016/j.actaastro.2016.04.013
PG 7
WC Engineering, Aerospace
SC Engineering
GA DU7RL
UT WOS:000382412200008
ER
PT J
AU Nag, S
Gatebe, CK
Miller, DW
de Weck, OL
AF Nag, Sreeja
Gatebe, Charles K.
Miller, David W.
de Weck, Olivier L.
TI Effect of satellite formations and imaging modes on global albedo
estimation
SO ACTA ASTRONAUTICA
LA English
DT Article
DE Small satellite; Formation flight; Cubesat; BRDF; Multi-angular; Remote
sensing; Constellation
ID AIRBORNE SPECTRAL MEASUREMENTS; MISSION; SURFACE; SPACE; CONSTELLATION;
ATMOSPHERE; OCEAN
AB We confirm the applicability of using small satellite formation flight for multi-angular earth observation to retrieve global, narrow band, narrow field-of-view albedo. The value of formation flight is assessed using a coupled systems engineering and science evaluation model, driven by Model Based Systems Engineering and Observing System Simulation Experiments. Albedo errors are calculated against bi-directional reflectance data obtained from NASA airborne campaigns made by the Cloud Absorption Radiometer for the seven major surface types, binned using MODIS' land cover map water, forest, cropland, grassland, snow, desert and cities. A full tradespace of architectures with three to eight satellites, maintainable orbits and imaging modes (collective payload pointing strategies) are assessed. For an arbitrary 4-sat formation, changing the reference, nadir-pointing satellite dynamically reduces the average albedo error to 0.003, from 0.006 found in the static reference case. Tracking pre-selected waypoints with all the satellites reduces the average error further to 0.001, allows better polar imaging and continued operations even with a broken formation. An albedo error of 0.001 translates to 136 W/m(2) or 0.4% in Earth's outgoing radiation error. Estimation errors are found to be independent of the satellites' altitude and inclination, if the nadir-looking is changed dynamically. The formation satellites are restricted to differ in only right ascension of planes and mean anomalies within slotted bounds. Three satellites in some specific formations show average albedo errors of less than 2% with respect to airborne, ground data and seven satellites in any slotted formation outperform the monolithic error of 3.6%. In fact, the maximum possible albedo error, purely based on angular sampling, of 12% for monoliths is outperformed by a five-satellite formation in any slotted arrangement and an eight satellite formation can bring that error down four fold to 3%. More than 70% ground spot overlap between the satellites is possible with 0.5 of pointing accuracy, 2 Km of GPS accuracy and commands uplinked once a day. The formations can be maintained at less than 1 m/s of monthly Delta V per satellite. (C) 2016 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Nag, Sreeja] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Nag, Sreeja] Bay Area Environm Res Inst, Petaluma, CA USA.
[Gatebe, Charles K.] Univ Space Res Org, NASA, Goddard Space Flight Ctr, Columbia, MD USA.
[Miller, David W.] MIT, NASA Headquarters, Cambridge, MA 02139 USA.
[de Weck, Olivier L.] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
RP Nag, S (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Nag, S (reprint author), Bay Area Environm Res Inst, Petaluma, CA USA.
EM sreejanag@alum.mit.edu; Charles.K.Gatebe@nasa.gov; millerd@mit.edu;
deweck@mit.edu
FU Schlumberger Faculty for the Future Fellowship (FFTF); NASA Earth and
Space Science Fellowship (NESSF)
FX The authors acknowledge the following people, without whose help this
paper in its present quality would not have been possible: Rajesh
Poudyal (GSFC) for extracting and post processing the BRDF data for the
CAR instrument, Warren Wiscombe (GSFC) for his contribution and
consistent drive toward Leonardo-BRDF which first proposed the concept
of formation flight for BRDF, Jacqueline LeMoigne (GSFC), Ralph Kahn
(GSFC), Kerri Cahoy (MIT), Daniel Selva (Cornell), Alexei Lyapustin
(GSFC) for their invaluable ideas toward making this study better and
three anonymous reviewers for their comments to improve its readability.
The primary author was funded by the Schlumberger Faculty for the Future
Fellowship (FFTF) and the NASA Earth and Space Science Fellowship
(NESSF).
NR 59
TC 1
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U1 8
U2 8
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
EI 1879-2030
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD SEP-OCT
PY 2016
VL 126
SI SI
BP 77
EP 97
DI 10.1016/j.actaastro.2016.04.004
PG 21
WC Engineering, Aerospace
SC Engineering
GA DU7RL
UT WOS:000382412200011
ER
PT J
AU Yang, FY
Nelson, B
Aziz, J
Carlino, R
Perez, AD
Faber, N
Foster, C
Frost, C
Henze, C
Karacalioglu, AG
Levit, C
Marshall, W
Mason, J
O'Toole, C
Swenson, J
Worden, SP
Stupl, J
AF Yang, Fan Yang
Nelson, Bron
Aziz, Jonathan
Carlino, Roberto
Perez, Andres Dono
Faber, Nicolas
Foster, Cyrus
Frost, Chad
Henze, Chris
Karacalioglu, Arif Goktug
Levit, Creon
Marshall, William
Mason, James
O'Toole, Conor
Swenson, Jason
Worden, Simon P.
Stupl, Jan
TI LightForce photon-pressure collision avoidance: Efficiency analysis in
the current debris environment and long-term simulation perspective
SO ACTA ASTRONAUTICA
LA English
DT Article
ID MODEL; NASA
AB This work provides an efficiency analysis of the LightForce space debris collision avoidance scheme in the current debris environment and describes a simulation approach to assess its impact on the long-term evolution of the space debris environment LightForce aims to provide just-in-time collision avoidance by utilizing photon pressure from ground-based industrial lasers. These ground stations impart minimal accelerations to increase the miss distance for a predicted conjunction between two objects. In the first part of this paper we will present research that investigates the short-term effect of a few systems consisting of 20 kW class lasers directed by 1.5 m diameter telescopes using adaptive optics. The results found such a network of ground stations to mitigate more than 85 percent of conjunctions and could lower the expected number of collisions in Low Earth Orbit (LEO) by an order of magnitude. While these are impressive numbers that indicate LightForce's utility in the short-term, the remaining 15 % of possible collisions contain (among others) conjunctions between two massive objects that would add large amount of debris if they collide. Still, conjunctions between massive objects and smaller objects can be mitigated. Hence, we choose to expand the capabilities of the simulation software to investigate the overall effect of a network of LightForce stations on the long-term debris evolution. In the second part of this paper, we will present the planned simulation approach for that effort. For the efficiency analysis of collision avoidance in the current debris environment, we utilize a simulation approach that uses the entire Two Line Element (TLE) catalog in LEO for a given day as initial input These objects are propagated for one year and an all-on-all conjunction analysis is performed. For conjunctions that fall below a range threshold, we calculate the probability of collision and record those values. To assess efficiency, we compare a baseline (without collision avoidance) conjunction analysis with an analysis where LightForce is active. Using that approach, we take into account that collision avoidance maneuvers could have effects on third objects. Performing all-on-all conjunction analyses for extended period of time requires significant computer resources; hence we implemented this simulation utilizing a highly parallel approach on the NASA Pleiades supercomputer. (C) 2016 Published by Elsevier Ltd. on behalf of IAA.
C1 [Yang, Fan Yang; Perez, Andres Dono] NASA, Ames Res Ctr, MEI, Washington, DC USA.
[Nelson, Bron] NASA, Ames Res Ctr, Comp Sci Corp, Washington, DC USA.
[Aziz, Jonathan] Univ Colorado, Boulder, CO 80309 USA.
[Carlino, Roberto] NASA, Ames Res Ctr, STC, Washington, DC USA.
[Faber, Nicolas; Stupl, Jan] NASA, Ames Res Ctr, SGT, Washington, DC 20546 USA.
[Foster, Cyrus; Levit, Creon; Marshall, William; Mason, James] Planet Labs, San Francisco, CA USA.
[Frost, Chad; Henze, Chris] NASA, Ames Res Ctr, Washington, DC USA.
[O'Toole, Conor] Univ Coll Dublin, NASA, Ames Res Ctr, Dublin, Ireland.
[Swenson, Jason] NASA, Ames Res Ctr, LMCO Space OPNS, Washington, DC USA.
[Worden, Simon P.] Breakthrough Prize Fdn, Stanford, CA USA.
RP Stupl, J (reprint author), NASA, Ames Res Ctr, SGT, Washington, DC 20546 USA.
EM jan.stupl@nasa.gov
FU center management at NASA Ames Research Center
FX We would like to thank our colleagues and the center management at NASA
Ames Research Center for continuing support. We also would like to thank
the NAIF SPICE team at JPL, especially Nat Bachman for providing a long
term version of their Earth orientation file. Special thanks go to Wang
Ting (Princeton) for sharing his area-to-mass ratio database and for
providing insight in a past implementation of the EVOLVE breakup model.
For useful discussions we would like to thank Gene Stansbery, Paula
Krisko, Carsten Wiedemann, Jonas Radtke and Holger Krag. We thank Andrew
Shacker for providing useful input for future versions of the software.
We thank Jonas Jonsson for useful discussions and his help editing this
paper.
NR 32
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U1 2
U2 2
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
EI 1879-2030
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD SEP-OCT
PY 2016
VL 126
SI SI
BP 411
EP 423
DI 10.1016/j.actaastro.2016.04.032
PG 13
WC Engineering, Aerospace
SC Engineering
GA DU7RL
UT WOS:000382412200042
ER
PT J
AU Guzzetti, D
Bosanac, N
Haapala, A
Howell, KC
Folta, DC
AF Guzzetti, Davide
Bosanac, Natasha
Haapala, Amanda
Howell, Kathleen C.
Folta, David C.
TI Rapid trajectory design in the Earth Moon ephemeris system via an
interactive catalog of periodic and quasi-periodic orbits
SO ACTA ASTRONAUTICA
LA English
DT Article; Proceedings Paper
CT IAF 66th International Astronautical Congress (IAC)
CY OCT, 2015
CL Jerusalem, ISRAEL
SP IAF
DE Multi-body systems; Three-body problem; Libration points; Quasi-periodic
solutions; Periodic solutions
ID LIBRATION POINTS
AB Upcoming missions and prospective design concepts in the Earth-Moon system extensively leverage multi-body dynamics that may facilitate access to strategic locations or reduce propellant usage. To incorporate these dynamical structures into the mission design process, Purdue University and the NASA Goddard Flight Space Center have initiated the construction of a trajectory design framework to rapidly access and compare solutions from the circular restricted three-body problem. This framework, based upon a 'dynamic' catalog of periodic and quasi-periodic orbits within the Earth-Moon system, can guide an end-to-end trajectory design in an ephemeris model. In particular, the inclusion of quasi-periodic orbits further expands the design space, potentially enabling the detection of additional orbit options. To demonstrate the concept of a 'dynamic' catalog, a prototype graphical interface is developed. Strategies to characterize and represent periodic and quasi-periodic information for interactive trajectory comparison and selection are discussed. Two sample applications for formation flying near the Earth-Moon 1,2 point and lunar space infrastructures are explored to demonstrate the efficacy of a 'dynamic' catalog for rapid trajectory design and validity in higher-fidelity models. (C) 2016 IAA. Published by Elsevier Ltd. All rights reserved.
C1 [Guzzetti, Davide; Bosanac, Natasha; Haapala, Amanda; Howell, Kathleen C.] Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA.
[Folta, David C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Haapala, Amanda] Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA.
RP Guzzetti, D (reprint author), Purdue Univ, Sch Aeronaut & Astronaut, W Lafayette, IN 47907 USA.
EM dguzzett@purdue.edu; nbosanac@purdue.edu; amanda.haapala@jhuapl.edu;
howell@purdue.edu; david.c.folta@nasa.gov
NR 31
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 0094-5765
EI 1879-2030
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD SEP-OCT
PY 2016
VL 126
SI SI
BP 439
EP 455
DI 10.1016/j.actaastro.2016.06.029
PG 17
WC Engineering, Aerospace
SC Engineering
GA DU7RL
UT WOS:000382412200044
ER
PT J
AU Rai, A
Robinson, JA
Tate-Brown, J
Buckley, N
Zell, M
Tasaki, K
Karabadzhak, G
Sorokin, IV
Pignataro, S
AF Rai, Amelia
Robinson, Julie A.
Tate-Brown, Judy
Buckley, Nicole
Zell, Martin
Tasaki, Kazuyuki
Karabadzhak, Georgy
Sorokin, Igor V.
Pignataro, Salvatore
TI Expanded benefits for humanity from the International Space Station
SO ACTA ASTRONAUTICA
LA English
DT Article
ID MICROGRAVITY; EXPERIENCE; RESOLUTION
AB In 2012, the International Space Station (ISS) (Fig. 1) partnership published the updated International Space Station Benefits for Humanity [1], a compilation of stories about the many benefits being realized in the areas of human health, Earth observations and disaster response, and global education. This compilation has recently been revised to include updated statistics on the impacts of the benefits, and new benefits that have developed since the first publication. Two new sections have also been added to the book, economic development of space and innovative technology. This paper will summarize the updates on behalf of the ISS Program Science Forum, made up of senior science representatives across the international partnership.
The new section on "Economic Development of Space" highlights case studies from public-private partnerships that are leading to a new economy in low earth orbit (LEO). Businesses provide both transportation to the ISS as well as some research facilities and services. These relationships promote a paradigm shift of government-funded, contractor-provided goods and services to commercially-provided goods purchased by government agencies. Other examples include commercial firms spending research and development dollars to conduct investigations on ISS and commercial service providers selling services directly to ISS users. This section provides examples of ISS as a test bed for new business relationships, and illustrates successful partnerships.
The second new section, "Innovative Technology," merges technology demonstration and physical science findings that promise to return Earth benefits through continued research. Robotic refueling concepts for life extensions of costly satellites in geo-synchronous orbit have applications to robotics in industry on Earth. Flame behavior experiments reveal insight into how fuel burns in microgravity leading to the possibility of improving engine efficiency on Earth. Nanostructures and smart fluids are examples of materials improvements that are being developed using data from ISS.
The publication also expands the benefits of research results in human health, environmental change and disaster response and in education activities developed to capture student imaginations in support of science, technology, engineering and mathematics, or STEM, education internationally. Applications to human health of the knowledge gained on ISS continue to grow and improve healthcare technologies and our understanding of human physiology. Distinct benefits return to Earth from the only orbiting multi-disciplinary laboratory of its kind. The ISS is a stepping stone for future space exploration by providing findings that develop LEO and improve life on our planet. (C) 2016 Published by Elsevier Ltd. on behalf of IAA.
C1 [Rai, Amelia; Robinson, Julie A.] NASA, Johnson Space Ctr, Washington, DC 20546 USA.
[Tate-Brown, Judy] Barrios Technol, Houston, TX 77058 USA.
[Buckley, Nicole] Canadian Space Agcy, Longueuil, PQ, Canada.
[Zell, Martin] European Space Agcy, Noordwijk, Netherlands.
[Tasaki, Kazuyuki] Japan Aerosp Explorat Agcy JAXA, Chofu, Tokyo, Japan.
[Karabadzhak, Georgy] TSNIIMASH, Kaliningrad, Russia.
[Sorokin, Igor V.] SP Korolev Rocket & Space Corp Energia, Korolev, Russia.
[Pignataro, Salvatore] Italian Space Agcy ASI, Rome, Italy.
RP Rai, A (reprint author), NASA, Johnson Space Ctr, Washington, DC 20546 USA.
EM amelia.e.rai@nasa.gov; julie.a.robinson@nasa.gov;
judy.tate-brown-1@nasa.gov; nicole.buckley@asc-csa.gc.ca;
martin.zell@esa.int; tasaki.kazuyuki@jaxa.jp; gfk@tsniimash.ru;
igor.v.sorokin@rsce.ru; salvatore.pignataro@asi.it
OI Robinson, Julie/0000-0002-6832-6459
NR 43
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U2 12
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PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0094-5765
EI 1879-2030
J9 ACTA ASTRONAUT
JI Acta Astronaut.
PD SEP-OCT
PY 2016
VL 126
SI SI
BP 463
EP 474
DI 10.1016/j.actaastro.2016.06.030
PG 12
WC Engineering, Aerospace
SC Engineering
GA DU7RL
UT WOS:000382412200046
ER
PT J
AU Arvani, B
Pierce, RB
Lyapustin, AI
Wang, YJ
Ghermandi, G
Teggi, S
AF Arvani, Barbara
Pierce, R. Bradley
Lyapustin, Alexei I.
Wang, Yujie
Ghermandi, Grazia
Teggi, Sergio
TI Seasonal monitoring and estimation of regional aerosol distribution over
Po valley, northern Italy, using a high-resolution MAIAC product
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Aerosol optical depth (AOD); High resolution aerosol retrieval;
Seasonality AOD-PM10 correlation; MAIAC; MODIS; PM10; Planetary boundary
layer (PBL)
ID AIR-QUALITY ASSESSMENT; MODIS 3 KM; PARTICULATE MATTER PREDICTIONS;
SOUTHEASTERN UNITED-STATES; OPTICAL DEPTH RETRIEVALS; PM2.5
CONCENTRATIONS; EPIDEMIOLOGIC EVIDENCE; AOD RETRIEVALS; BOUNDARY-LAYER;
SATELLITE DATA
AB In this work, the new 1 km-resolved Multi-Angle Implementation of Atmospheric Correction (MAIAC) algorithm is employed to characterize seasonal PM10 - AOD correlations over northern Italy. The accuracy of the new dataset is assessed compared to the widely used Moderate Resolution Imaging Spectroradiometer (MODIS) Collection 5.1 Aerosol Optical Depth (AOD) data, retrieved at 0.55 gm with spatial resolution of 10 km (MYD04_12). We focused on evaluating the ability of these two products to characterize both temporal and spatial distributions of aerosols within urban and suburban areas. Ground PM10 measurements were obtained from 73 of the Italian Regional Agency for Environmental Protection (ARPA) monitoring stations, spread across northern Italy, during a three-year period from 2010 to 2012. The Po Valley area (northern Italy) was chosen as the study domain because of its severe urban. air pollution, resulting from it having the highest population and industrial manufacturing density in the country, being located in a valley where two surrounding mountain chains favor the stagnation of pollutants. We found that the global correlations between the bin-averaged PM-to and AOD are R-2 = 0.83 and R-2 = 0.44 for MYD04_L2 and for MAIAC, respectively, suggesting a greater sensitivity of the high resolution product to small-scale deviations. However, the introduction of Relative Humidity (RH) and Planetary Boundary Layer (PBL) depth corrections allowed for a significant improvement to the bin averaged PM AOD correlation, which led to a similar performance: R-2 = 0.96 for MODIS and R-2 = 0.95 for MAIAC. Furthermore, the introduction of the PBL information in the corrected AOD values was found to be crucial in order to capture the clear seasonal cycle shown by measured PM10 values. The study allowed us to define four seasonal linear correlations that estimate PM10 concentrations satisfactorily from the remotely sensed MAIAC AOD retrieval. Overall, the results show that the high resolution provided by MAIAC retrieval data is much more relevant than the 10 km MODIS data to characterize PM10 in this region of Italy which has a pretty limited geographical domain but a broad variety of land usages and consequent particulate concentrations. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Arvani, Barbara; Ghermandi, Grazia; Teggi, Sergio] Univ Modena & Reggio Emilia, Dipartimento Ingn Enzo Ferrari, Via P Vivarelli 10, I-41125 Modena, Italy.
[Pierce, R. Bradley] NOAA NESDIS Adv Satellite Prod Branch, 1225 W Dayton St, Madison, WI 53706 USA.
[Lyapustin, Alexei I.] NASA, Goddard Space Flight Ctr, Code 613, Greenbelt, MD 20771 USA.
[Wang, Yujie] Univ Maryland Baltimore Cty, 1000 Hilltop Circle, Baltimore, MD 21228 USA.
RP Arvani, B (reprint author), Univ Modena & Reggio Emilia, Dipartimento Ingn Enzo Ferrari, Via P Vivarelli 10, I-41125 Modena, Italy.
EM barbara.arvani@unimore.it
RI Pierce, Robert Bradley/F-5609-2010;
OI Pierce, Robert Bradley/0000-0002-2767-1643; Teggi,
Sergio/0000-0001-7375-0599
FU Italian Ministero dell'Istruzione, dell' Universita e della Ricerca
(Project PRIN) [2010WLNFY2]
FX This research has been funded by the Italian Ministero dell'Istruzione,
dell' Universita e della Ricerca (Project PRIN2010-11, 2010WLNFY2). The
authors are thankful for Italian agencies ARPA Emilia-Romagna, ARPA
Lombardia, ARPA Piemonte, and ARPA Veneto for providing ground
PM10 data. The views, opinions, and findings contained in
this report are those of the author(s) and should not be construed as an
official National Oceanic and Atmospheric Administration or U.S.
Government position, policy, or decision.
NR 61
TC 1
Z9 1
U1 10
U2 11
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 SEP
PY 2016
VL 141
BP 106
EP 121
DI 10.1016/j.atmosenv.2016.06.037
PG 16
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DU1EL
UT WOS:000381950900010
ER
PT J
AU Dolan, W
Payne, VH
Kualwik, SS
Bowman, KW
AF Dolan, Wayana
Payne, Vivienne H.
Kualwik, Susan S.
Bowman, Kevin W.
TI Satellite observations of ethylene (C2H4) from the Aura Tropospheric
Emission Spectrometer: A scoping study
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Ethylene; Tropospheric Emission Spectrometer; Satellite remote sensing
ID ARCTAS; OZONE; AIRCRAFT; ISOPRENE; ATLANTIC; MISSION; IMPACT; FIRES;
TES; PAN
AB We present a study focusing on detection and initial quantitative estimates of ethylene (C2H4) in observations from the Tropospheric Emission Spectrometer (TES), a Fourier transform spectrometer aboard the Aura satellite that measures thermal infrared radiances with high spectral resolution (0.1 cm(-1)). We analyze observations taken in support of the 2008 Arctic Research of the Composition of the Troposphere from Aircraft and Satellites (ARCTAS) mission and demonstrate the feasibility of future development of C2H4 into a TES standard product. In the Northern Hemisphere, C2H4 is commonly associated with boreal fire plumes, motor vehicle exhaust and petrochemical emissions. It has a short lifetime (similar to 14-32 h) in the troposphere due to its reaction with OH and O-3. Chemical destruction of C2H4 in the atmosphere leads to the production of ozone and other species such as carbon monoxide (CO) and formaldehyde. Results indicate a correlation between C2H4 and CO in boreal fire plumes. Quantitative C2H4 estimates are sensitive to assumptions about the plume height and width. We find that C2H4 greater than 2-3 ppbv can be detected in a single TES observation (for a fire plume at 3 km altitude and 1.5 km width). Spatial averaging will be needed for surface-peaking profiles where TES sensitivity is lower. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Dolan, Wayana; Payne, Vivienne H.; Bowman, Kevin W.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Dolan, Wayana] Occidental Coll, Eagle Rock, CA USA.
[Kualwik, Susan S.] Bay Area Environm Res Inst Moffett Field, Moffett Field, CA USA.
RP Payne, VH (reprint author), Jet Prop Lab, M-S 233-200,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM vivienne.h.payne@jpl.nasa.gov
NR 31
TC 0
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U1 3
U2 3
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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 SEP
PY 2016
VL 141
BP 388
EP 393
DI 10.1016/j.atmosenv.2016.07.009
PG 6
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DU1EL
UT WOS:000381950900035
ER
PT J
AU Titos, G
Cazorla, A
Zieger, P
Andrews, E
Lyamani, H
Granados-Munoz, MJ
Olmo, FJ
Alados-Arboledas, L
AF Titos, G.
Cazorla, A.
Zieger, P.
Andrews, E.
Lyamani, H.
Granados-Munoz, M. J.
Olmo, F. J.
Alados-Arboledas, L.
TI Effect of hygroscopic growth on the aerosol light-scattering
coefficient: A review of measurements, techniques and error sources
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Review
DE Scattering enhancement; Water uptake; Hygroscopicity; Aerosol light
scattering
ID ALPINE SITE JUNGFRAUJOCH; OPTICAL-PROPERTIES; RELATIVE-HUMIDITY;
RADIATIVE PROPERTIES; IN-SITU; HUMIDIFICATION FACTORS; AMMONIUM-SULFATE;
WATER-UPTAKE; ACE-ASIA; ATMOSPHERIC AEROSOLS
AB Knowledge of the scattering enhancement factor,.f(RH), is important for an accurate description of direct aerosol radiative forcing. This factor is defined as the ratio between the scattering coefficient at enhanced relative humidity, RH, to a reference (dry) scattering coefficient. Here, we review the different experimental designs used to measure the scattering coefficient at dry and humidified conditions as well as the procedures followed to analyze the measurements. Several empirical parameterizations for the relationship between f(RH) and RH have been proposed in the literature. These parameterizations have been reviewed and tested using experimental data representative of different hygroscopic growth behavior and a new parameterization is presented. The potential sources of error in f(RH) are discussed. A Monte Carlo method is used to investigate the overall measurement uncertainty, which is found to be around 20-40% for moderately hygroscopic aerosols. The main factors contributing to this uncertainty are the uncertainty in RH measurement, the dry reference state and the nephelometer uncertainty. A literature survey of nephelometry-based f(RH) measurements is presented as a function of aerosol type. In general, the highest f(RH) values were measured in clean marine environments, with pollution having a major influence on f(RH). Dust aerosol tended to have the lowest reported hygroscopicity of any of the aerosol types studied. Major open questions and suggestions for future research priorities are outlined. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Titos, G.; Cazorla, A.; Lyamani, H.; Granados-Munoz, M. J.; Olmo, F. J.; Alados-Arboledas, L.] Univ Granada, Andalusian Inst Earth Syst Res, Granada 18006, Spain.
[Titos, G.; Cazorla, A.; Lyamani, H.; Granados-Munoz, M. J.; Olmo, F. J.; Alados-Arboledas, L.] Univ Granada, Dept Appl Phys, Granada 18071, Spain.
[Zieger, P.] Stockholm Univ, Bolin Ctr Climate Res, Dept Environm Sci & Analyt Chem, S-11418 Stockholm, Sweden.
[Andrews, E.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80305 USA.
[Titos, G.] IDAEA CSIC, Inst Environm Assessment & Water Res, Barcelona, Spain.
[Granados-Munoz, M. J.] CALTECH, NASA, Jet Prop Lab, Table Mt Facil, Wrightwood, CA USA.
RP Titos, G (reprint author), Univ Granada, Andalusian Inst Earth Syst Res, Granada 18006, Spain.
EM gtitos@ugr.es
RI Granados-Munoz, Maria Jose/G-9308-2014;
OI Granados-Munoz, Maria Jose/0000-0001-8718-5914; Titos Vela,
Gloria/0000-0003-3630-5079
FU Andalusia Regional Government [P10-RNM-6299, P12-RNM-2409]; FEDER
[CGL2013_45410-R]; Spanish Ministry of Economy and Competitiveness;
European Union [654109, ACTRIS-2]; Programa del Plan Propio de
Investigacion "Contrato Puente" of the University of Granada
FX This work was supported by the Andalusia Regional Government through
projects P10-RNM-6299 and P12-RNM-2409; by the Spanish Ministry of
Economy and Competitiveness and FEDER through project CGL2013_45410-R;
and by European Union's Horizon 2020 research and innovation programme
under grant agreement No 654109, ACTRIS-2. G. Titos was partially funded
by Programa del Plan Propio de Investigacion "Contrato Puente" of the
University of Granada. We thank the Stockholm International
Meteorological Institute (IMI) for travel support of G. Titos.
NR 90
TC 1
Z9 1
U1 20
U2 23
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 SEP
PY 2016
VL 141
BP 494
EP 507
DI 10.1016/j.atmosenv.2016.07.021
PG 14
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DU1EL
UT WOS:000381950900046
ER
PT J
AU Duval, S
Santini, JM
Lemaire, D
Chaspoul, F
Russell, MJ
Grimaldi, S
Nitschke, W
Schoepp-Cothenet, B
AF Duval, Simon
Santini, Joanne M.
Lemaire, David
Chaspoul, Florence
Russell, Michael J.
Grimaldi, Stephane
Nitschke, Wolfgang
Schoepp-Cothenet, Barbara
TI The H-bond network surrounding the pyranopterins modulates redox
cooperativity in the molybdenum-bisPGD cofactor in arsenite oxidase
SO BIOCHIMICA ET BIOPHYSICA ACTA-BIOENERGETICS
LA English
DT Article
DE Arsenite oxidase; Molybdenum enzyme; Optical spectroscopy; EPR
spectroscopy; Redox titrations
ID COLI NITRATE REDUCTASE; IRON-SULFUR CENTERS; PARAMAGNETIC-RESONANCE
SPECTROSCOPY; ESCHERICHIA-COLI; DIMETHYLSULFOXIDE REDUCTASE;
ALCALIGENES-FAECALIS; BINDING-SITE; SEMIQUINONE; OXIDATION; SUBUNIT
AB While the molybdenum cofactor in the majority of bisPGD enzymes goes through two consecutive 1-electron redox transitions, previous protein-film voltammetric results indicated the possibility of cooperative (n = 2) redox behavior in the bioenergetic enzyme arsenite oxidase (Aio). Combining equilibrium redox titrations, optical and EPR spectroscopies on concentrated samples obtained via heterologous expression, we unambiguously confirm this claim and quantify Aio's redox cooperativity. The stability constant, K-s of the Mo-v semi-reduced intermediate is found to be lower than 10(-3). Site-directed mutagenesis of residues in the vicinity of the Mo-cofactor demonstrates that the degree of redox cooperativity is sensitive to H-bonding interactions between the pyranopterin moieties and amino acid residues. Remarkably, in particular replacing the Gln-726 residue by Gly results in stabilization of (low-temperature) EPR-observable Mo-v with K-s = 4. As evidenced by comparison of room temperature optical and low temperature EPR titrations, the degree of stabilization is temperature dependent. This highlights the importance of room-temperature redox characterizations for correctly interpreting catalytic properties in this group of enzymes.
Geochemical and phylogenetic data strongly indicate that molybdenum played an essential biocatalytic roles in early life. Molybdenum's redox versatility and in particular the ability to show cooperative (n = 2) redox behavior provide a rationale for its paramount catalytic importance throughout the evolutionary history of life. Implications of the H-bonding network modulating Molybdenum's redox properties on details of a putative inorganic metabolism at life's origin are discussed. (C) 2016 Published by Elsevier B.V.
C1 [Duval, Simon; Grimaldi, Stephane; Nitschke, Wolfgang; Schoepp-Cothenet, Barbara] Aix Marseille Univ, CNRS, BIP UMR 7281, IMM FR 3479, 31 Chemin J Aiguier, F-13402 Marseille 20, France.
[Santini, Joanne M.] UCL, Inst Struct & Mol Biol, London WC1E 6BT, England.
[Lemaire, David] CEA Cadarache, Inst Biol Environm & Biotechnol, F-13108 St Paul Les Durance, France.
[Chaspoul, Florence] Aix Marseille Univ, IMBE, IRD CNRS UAPV, Fac Pharm, F-13005 Marseille, France.
[Russell, Michael J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RP Schoepp-Cothenet, B (reprint author), Aix Marseille Univ, CNRS, BIP UMR 7281, IMM FR 3479, 31 Chemin J Aiguier, F-13402 Marseille 20, France.
EM schoepp@imm.cnrs.fr
OI Grimaldi, Stephane/0000-0002-9559-6112
FU CNRS; CEA; Aix-Marseille University; ANR [11-BSV5-005-01]; NASA
Astrobiology Institute (Icy Worlds); French EPR network (RENARD)
[IR3443]
FX We thank Axel Magalon and Frederic Biaso for helpful discussions and
Pierre Ceccaldi for Nar preparation. Our work is funded by the CNRS,
CEA, Aix-Marseille University, ANR (Project MC2, 11-BSV5-005-01). MJR's
research was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration and with support by the NASA Astrobiology
Institute (Icy Worlds). The authors are grateful to the EPR facilities
available at the Aix-Marseille University EPR center, and to financial
support from the French EPR network (RENARD, IR3443).
NR 54
TC 0
Z9 0
U1 10
U2 10
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0005-2728
EI 0006-3002
J9 BBA-BIOENERGETICS
JI Biochim. Biophys. Acta-Bioenerg.
PD SEP
PY 2016
VL 1857
IS 9
BP 1353
EP 1362
DI 10.1016/j.bbabio.2016.05.003
PG 10
WC Biochemistry & Molecular Biology; Biophysics
SC Biochemistry & Molecular Biology; Biophysics
GA DV0EI
UT WOS:000382590400001
PM 27207587
ER
PT J
AU Gilman, E
Chaloupka, M
Swimmer, Y
Piovano, S
AF Gilman, Eric
Chaloupka, Milani
Swimmer, Yonat
Piovano, Susanna
TI A cross-taxa assessment of pelagic longline by-catch mitigation
measures: conflicts and mutual benefits to elasmobranchs
SO FISH AND FISHERIES
LA English
DT Article
DE At-vessel mortality; by-catch; circle hook; ray; shark; wire leader
ID SHARK ALOPIAS-SUPERCILIOSUS; EASTERN PACIFIC-OCEAN; TUNA THUNNUS-OBESUS;
SEA-TURTLE BYCATCH; CIRCLE HOOKS; POSTRELEASE SURVIVAL; RELATIVE
ABUNDANCE; DISCARD MORTALITY; ATLANTIC-OCEAN; NORTH-ATLANTIC
AB Elasmobranch mortality in pelagic longline fisheries poses a risk to some populations, alters the distribution of abundance between sympatric competitors, changing ecosystem structure, processes and stability. Individual and synergistic effects on elasmobranch catch and survival from pelagic longline gear factors, including methods prescribed to mitigate bycatch of other vulnerable taxa, were determined. Overall relative risk of higher circle vs. J-shaped hook shark catch rates conditioned on potentially informative moderators, from 30 studies, was estimated using an inverse-precision weighted mixed-effects meta-regression modelling approach. Sharks had a 1.20 times (95% CI: 1.03-1.39) significantly higher pooled relative risk of capture on circle hooks, with two significant moderators. The pooled relative risk estimate of ray circle hook catch from 15 studies was not significant (RR=1.22, 95% CI: 0.89-1.66) with no significant moderators. From a literature review, wire leaders had higher shark catch and haulback mortality than monofilament. Interacting effects of hook, bait and leader affect shark catch rates: hook shape and width and bait type determine hooking position and ability to sever monofilament leaders. Circle hooks increased elasmobranch catch, but reduced haulback mortality and deep hooking relative to J-shaped hooks of the same or narrower width. Using fish vs. squid for bait increased shark catch and deep hooking. Pelagic stingray (Pteroplatytrygon violacea) catch and mortality were lower on wider hooks. Using circle instead of J-shaped hooks and fish instead of squid for bait, while benefitting sea turtles, odontocetes and possibly seabirds, exacerbates elasmobranch catch and injury, therefore warranting fishery-specific assessments to determine relative risks.
C1 [Gilman, Eric] Nature Conservancy, Honolulu, HI USA.
[Gilman, Eric] Pelag Fisheries Res Serv, Honolulu, HI USA.
[Chaloupka, Milani] Univ Queensland, Ecol Modeling Serv, St Lucia, Qld 4067, Australia.
[Chaloupka, Milani] Univ Queensland, POB 6150, St Lucia, Qld 4067, Australia.
[Swimmer, Yonat] Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, 501 W Ocean Blvd, Long Beach, CA 90802 USA.
[Piovano, Susanna] Univ South Pacific, Laucala Campus,Private Mail Bag, Suva, Fiji.
RP Gilman, E (reprint author), 3661 Loulu St, Honolulu, HI 96822 USA.
EM EGilman@FisheriesResearchGroup.org
FU Sustainable Fisheries Fund Program of the Resources Legacy Fund; Nature
Conservancy
FX We are grateful for assistance provided by Victoria Jeffers, University
of Exeter, with compiling literature. We acknowledge the assistance
provided by Andre Afonso to correct copyediting errors in a table in
Afonso et al. (2012). We are grateful for clarifications provided by
John Watson and Daniel Foster on leader materials used in an experiment
from which findings were published in Watson et al. (2005), Epperly et
al. (2012), and Foster et al. (2012). Peer reviewer and journal editor
comments greatly improved the manuscript. The Sustainable Fisheries Fund
Program of the Resources Legacy Fund and The Nature Conservancy
contributed financial support for this study.
NR 160
TC 4
Z9 4
U1 16
U2 18
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1467-2960
EI 1467-2979
J9 FISH FISH
JI Fish. Fish.
PD SEP
PY 2016
VL 17
IS 3
BP 748
EP 784
DI 10.1111/faf.12143
PG 37
WC Fisheries
SC Fisheries
GA DU8VW
UT WOS:000382494600012
ER
PT J
AU Cavosie, AJ
Timms, NE
Erickson, TM
Hagerty, JJ
Horz, F
AF Cavosie, Aaron J.
Timms, Nicholas E.
Erickson, Timmons M.
Hagerty, Justin J.
Horz, Friedrich
TI Transformations to granular zircon revealed: Twinning, reidite, and ZrO2
in shocked zircon from Meteor Crater (Arizona, USA)
SO GEOLOGY
LA English
DT Article
ID U-PB; VREDEFORT IMPACT; SOUTH-AFRICA; METAMORPHISM; MICROSTRUCTURES;
DECOMPOSITION; DEFORMATION; BADDELEYITE; MINERALS; EVENTS
AB Granular zircon in impact environments has long been recognized but remains poorly understood due to lack of experimental data to identify mechanisms involved in its genesis. Meteor Crater in Arizona (USA) contains abundant evidence of shock metamorphism, including shocked quartz, the high-pressure polymorphs coesite and stishovite, diaplectic SiO2 glass, and lechatelierite (fused SiO2). Here we report the presence of granular zircon, a new shocked-mineral discovery at Meteor Crater, that preserve critical orientation evidence of specific transformations that occurred during formation at extreme impact conditions. The zircon grains occur as aggregates of sub-micrometer neoblasts in highly shocked Coconino Sandstone (CS) comprised of lechatelierite. Electron backscatter diffraction shows that each grain consists of multiple domains, some with boundaries disoriented by 65 degrees around < 110 >, a known {112} shock-twin orientation. Other domains have {001} in alignment with {110} of neighboring domains, consistent with the former presence of the high-pressure ZrSiO4 polymorph reidite. Additionally, nearly all zircon preserve ZrO2 + SiO2, providing evidence of partial dissociation. The genesis of CS granular zircon started with detrital zircon that experienced shock twinning and reidite formation at pressures from 20 to 30 GPa, ultimately yielding a phase that retained crystallographic memory; this phase subsequently recrystallized to systematically oriented zircon neoblasts, and in some areas partially dissociated to ZrO2. The lechatelierite matrix, experimentally constrained to form at >2000 degrees C, provided the ultrahigh-temperature environment for zircon dissociation (similar to 1670 degrees C) and neoblast formation. The capacity of granular zircon to preserve a cumulative pressure-temperature record has not been recognized previously, and provides a new method for investigating histories of impact-related mineral transformations in the crust at conditions far beyond those at which most rocks melt.
C1 [Cavosie, Aaron J.; Timms, Nicholas E.; Erickson, Timmons M.] Curtin Univ, Dept Appl Geol, TIGeR Inst Geosci Res, Perth, WA 6102, Australia.
[Cavosie, Aaron J.] Univ Wisconsin, Dept Geosci, Astrobiol Inst, NASA, Madison, WI 53706 USA.
[Cavosie, Aaron J.] Univ Puerto Rico, Dept Geol, Mayaguez, PR 00681 USA.
[Hagerty, Justin J.] USGS, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
[Horz, Friedrich] NASA, Johnson Space Ctr, Dept Sci, Jets,HX5,ARES, Houston, TX 77058 USA.
RP Cavosie, AJ (reprint author), Curtin Univ, Dept Appl Geol, TIGeR Inst Geosci Res, Perth, WA 6102, Australia.; Cavosie, AJ (reprint author), Univ Wisconsin, Dept Geosci, Astrobiol Inst, NASA, Madison, WI 53706 USA.; Cavosie, AJ (reprint author), Univ Puerto Rico, Dept Geol, Mayaguez, PR 00681 USA.
OI Erickson, Timmons/0000-0003-4520-7294
FU National Science Foundation [EAR-1145118]; USGS Meteor Crater Sample
Collection; NASA Astrobiology program; Curtin Research Fellowship;
Microscopy and Microanalysis Facility at Curtin University
FX B. Hess prepared the sample. Editor J.B. Murphy, S. Kamo, W. Cordua, and
an anonymous reviewer provided helpful comments. Support was provided by
the National Science Foundation (grant EAR-1145118), the USGS Meteor
Crater Sample Collection, the NASA Astrobiology program, a Curtin
Research Fellowship, and the Microscopy and Microanalysis Facility at
Curtin University.
NR 32
TC 3
Z9 3
U1 5
U2 5
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 SEP
PY 2016
VL 44
IS 9
BP 703
EP 706
DI 10.1130/G38043.1
PG 4
WC Geology
SC Geology
GA DU9FV
UT WOS:000382522700004
ER
PT J
AU Wang, YS
Hyyppa, J
Liang, XL
Kaartinen, H
Yu, XW
Lindberg, E
Holmgren, J
Qin, YC
Mallet, C
Ferraz, A
Torabzadeh, H
Morsdorf, F
Zhu, LL
Liu, JB
Alho, P
AF Wang, Yunsheng
Hyyppa, Juha
Liang, Xinlian
Kaartinen, Harri
Yu, Xiaowei
Lindberg, Eva
Holmgren, Johan
Qin, Yuchu
Mallet, Clement
Ferraz, Antonio
Torabzadeh, Hossein
Morsdorf, Felix
Zhu, Lingli
Liu, Jingbin
Alho, Petteri
TI International Benchmarking of the Individual Tree Detection Methods for
Modeling 3-D Canopy Structure for Silviculture and Forest Ecology Using
Airborne Laser Scanning
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Airborne laser scanning (ALS); benchmark; canopy structure; crown class;
individual tree detection (ITD); LiDAR; point cloud; subordinate tree
ID LIDAR POINT CLOUD; SEGMENTATION; CROWNS; STANDS
AB Canopy structure plays an essential role in biophysical activities in forest environments. However, quantitative descriptions of a 3-D canopy structure are extremely difficult because of the complexity and heterogeneity of forest systems. Airborne laser scanning (ALS) provides an opportunity to automatically measure a 3-D canopy structure in large areas. Compared with other point cloud technologies such as the image-based Structure from Motion, the power of ALS lies in its ability to penetrate canopies and depict subordinate trees. However, such capabilities have been poorly explored so far. In this paper, the potential of ALS-based approaches in depicting a 3-D canopy structure is explored in detail through an international benchmarking of five recently developed ALS-based individual tree detection (ITD) methods. For the first time, the results of the ITD methods are evaluated for each of four crown classes, i.e., dominant, codominant, intermediate, and suppressed trees, which provides insight toward understanding the current status of depicting a 3-D canopy structure using ITD methods, particularly with respect to their performances, potential, and challenges. This benchmarking study revealed that the canopy structure plays a considerable role in the detection accuracy of ITD methods, and its influence is even greater than that of the tree species as well as the species composition in a stand. The study also reveals the importance of utilizing the point cloud data for the detection of intermediate and suppressed trees. Different from what has been reported in previous studies, point density was found to be a highly influential factor in the performance of the methods that use point cloud data. Greater efforts should be invested in the point-based or hybrid ITD approaches to model the 3-D canopy structure and to further explore the potential of high-density and multiwavelengths ALS data.
C1 [Wang, Yunsheng; Hyyppa, Juha; Liang, Xinlian; Kaartinen, Harri; Yu, Xiaowei; Zhu, Lingli; Liu, Jingbin; Alho, Petteri] FGI, Finnish Geospatial Res Inst, Dept Remote Sensing & Photogrammetry, Masala 02431, Finland.
[Wang, Yunsheng; Alho, Petteri] Univ Turku, Geog Sect, Dept Geog & Geol, Turku 20014, Finland.
[Hyyppa, Juha; Liang, Xinlian; Kaartinen, Harri; Yu, Xiaowei; Zhu, Lingli; Liu, Jingbin] Acad Finland, Ctr Excellence Laser Scanning Res, Helsinki 00531, Finland.
[Lindberg, Eva; Holmgren, Johan] Swedish Univ Agr Sci, Dept Forest Resource Management, S-90183 Umea, Sweden.
[Qin, Yuchu; Mallet, Clement; Ferraz, Antonio] Univ Paris Est, IGN, MATIS, F-94160 Paris, France.
[Ferraz, Antonio] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Torabzadeh, Hossein; Morsdorf, Felix] Univ Zurich, Remote Sensing Labs, CH-8057 Zurich, Switzerland.
[Torabzadeh, Hossein] Bu Ali Sina Univ, Dept Civil Engn, Hamadan 651784161, Iran.
RP Liang, XL (reprint author), FGI, Finnish Geospatial Res Inst, Dept Remote Sensing & Photogrammetry, Masala 02431, Finland.
EM xinlian.liang@fgi.fi
RI Alho, Petteri/B-7989-2013; Ferraz, Antonio/D-9662-2017;
OI Alho, Petteri/0000-0001-5252-9609; Ferraz, Antonio/0000-0002-5328-5471;
Mallet, Clement/0000-0002-2675-165X
FU Finnish Academy through project "Centre of Excellence in Laser Scanning
Research (CoE-LaSR)" [272195]; Finnish Academy through project
"Interaction of Lidar/Radar Beams with Forests Using Mini-UAV and Mobile
Forest Tomography" [259348]; Finnish Academy through project "Competence
Based Growth Through Integrated Disruptive Technologies of 3-D
Digitalization, Robotics, Geospatial Information and Image
Processing/Computing Point Cloud Ecosystem" [293389]; European Community
[606971]; French National Research Agency through the FORESEE Project
[ANR-2010-BIOE-008]; Jet Propulsion Laboratory through the NASA
Postdoctoral Program; Oak Ridge Associated Universities through a
contract with NASA
FX This work was supported in part by the Finnish Academy through projects
"Centre of Excellence in Laser Scanning Research (CoE-LaSR)" under Grant
272195, "Interaction of Lidar/Radar Beams with Forests Using Mini-UAV
and Mobile Forest Tomography" under Grant 259348, and "Competence Based
Growth Through Integrated Disruptive Technologies of 3-D Digitalization,
Robotics, Geospatial Information and Image Processing/Computing Point
Cloud Ecosystem" under Grant 293389 and in part by the European
Community's Seventh Framework Program (FP7/2007-2013) under Grant
Agreement 606971. The work of Y. Qin, C. Mallet, and A. Ferraz was
supported by the French National Research Agency through the FORESEE
Project under Grant ANR-2010-BIOE-008. The work of A. Ferraz was
supported by the Jet Propulsion Laboratory through the NASA Postdoctoral
Program, which was administrated by the Oak Ridge Associated
Universities through a contract with NASA. Y. Wang, J. Hyyppa, and X.
Liang contributed equally to this work.
NR 24
TC 1
Z9 1
U1 22
U2 22
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 SEP
PY 2016
VL 54
IS 9
BP 5011
EP 5027
DI 10.1109/TGRS.2016.2543225
PG 17
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA DV1NZ
UT WOS:000382689300001
ER
PT J
AU Smith, GL
Thomas, S
Priestley, KJ
Walikainen, D
AF Smith, G. Louis
Thomas, Susan
Priestley, Kory J.
Walikainen, Dale
TI Tropical Mean Fluxes: A Tool for Calibration and Validation of CERES
Radiometers
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Clouds and the earth's radiant energy system (CERES); in-flight
calibration; radiation budget; radiometry; remote sensing; validation
ID RADIANT ENERGY SYSTEM; DATA RECORD VALIDATION; ABOARD EOS TERRA; FLIGHT
MODEL 5; INSTRUMENTS ABOARD; OCEAN MEASUREMENTS; CLOUDS; PERFORMANCE;
SENSORS
AB The Clouds and the Earth's Radiant Energy System (CERES) instrument requires in-flight calibration and validation to maintain its accuracy during orbit operations over an extended period. An internal calibration system provides calibration for the three channels; however, there is no device for calibration of the shortwave response of the total channel. A three-channel comparison technique has been developed to calibrate the shortwave response of the total channel using the tropical oceans as a vicarious calibration target. The difference between day and night outgoing longwave radiances (OLR) averaged over the tropical oceans is used to validate the day OLR. This paper evaluates the efficacy of the technique. A relation is computed at night between the window channel radiance and the OLR retrieved from the total channel for each month for each instrument. The relation has a standard deviation of 0.28 W.m(-2).sr(-1). Given 120 months of data, the precision of the curved line faired through these data is better than 0.05 W.m(-2).sr(-1). A bias is found between FM-1 and FM-3 of 0.3 W.m(-2).sr(-1), which is taken to be the accuracy with which the total channels can be calibrated with the internal blackbodies. This result includes the differences of longwave spectral responses of the instruments. The tropical mean OLR is between 87.4 and 90.2 W.m(-2).sr(-1) at night, with a standard deviation of 0.44 for FM-1 and 0.47 W.m(-2).sr(-1) for FM-3. The average difference between day and night tropical mean from the four instruments is 0.6 +/- 0.09 W.m(-2).sr(-1) over their data periods.
C1 [Smith, G. Louis; Thomas, Susan; Walikainen, Dale] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
[Priestley, Kory J.] Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA.
RP Smith, GL (reprint author), Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
EM g.l.smith@nasa.gov
FU Earth Science Directorate of the National Aeronautics and Space
Administration through the Science Directorate of the Langley Research
Center (LaRC); LaRC through Space Sciences Applications, Inc
FX This work was supported by the Earth Science Directorate of the National
Aeronautics and Space Administration through the Science Directorate of
the Langley Research Center (LaRC). The work of G. L. Smith, S. Thomas
and D. Walikainen was supported by LaRC through a contract with Space
Sciences Applications, Inc.
NR 25
TC 0
Z9 0
U1 4
U2 4
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 SEP
PY 2016
VL 54
IS 9
BP 5135
EP 5142
DI 10.1109/TGRS.2016.2556581
PG 8
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA DV1NZ
UT WOS:000382689300010
ER
PT J
AU Polivka, TN
Wang, J
Ellison, LT
Hyer, EJ
Ichoku, CM
AF Polivka, Thomas N.
Wang, Jun
Ellison, Luke T.
Hyer, Edward J.
Ichoku, Charles M.
TI Improving Nocturnal Fire Detection With the VIIRS Day-Night Band
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Day-night band (DNB); fire detection; fires; gas flares; Visible
Infrared Imaging Radiometer Suite (VIIRS); visible light at night;
wildfires
ID PIXEL-BASED CALCULATION; RADIATIVE POWER; SENSITIVITY-ANALYSIS;
SATELLITE DETECTION; INITIAL ASSESSMENT; SOUTH-AMERICA; INFRARED DATA;
GAS FLARES; SCAR-B; MODIS
AB Building on existing techniques for satellite remote sensing of fires, this paper takes advantage of the day-night band (DNB) aboard the Visible Infrared Imaging Radiometer Suite (VIIRS) to develop the Firelight Detection Algorithm (FILDA), which characterizes fire pixels based on both visible-light and infrared (IR) signatures at night. By adjusting fire pixel selection criteria to include visible-light signatures, FILDA allows for significantly improved detection of pixels with smaller and/or cooler subpixel hotspots than the operational Interface Data Processing System (IDPS) algorithm. VIIRS scenes with near-coincident Advanced Spaceborne Thermal Emission and Reflection (ASTER) overpasses are examined after applying the operational VIIRS fire product algorithm and including a modified "candidate fire pixel selection" approach from FILDA that lowers the 4-mu m brightness temperature (BT) threshold but includes a minimum DNB radiance. FILDA is shown to be effective in detecting gas flares and characterizing fire lines during large forest fires (such as the Rim Fire in California and High Park fire in Colorado). Compared with the operational VIIRS fire algorithm for the study period, FILDA shows a large increase (up to 90%) in the number of detected fire pixels that can be verified with the finer resolution ASTER data (90 m). Part (30%) of this increase is likely due to a combined use of DNB and lower 4-mu m BT thresholds for fire detection in FILDA. Although further studies are needed, quantitative use of the DNB to improve fire detection could lead to reduced response times to wildfires and better estimate of fire characteristics (smoldering and flaming) at night.
C1 [Polivka, Thomas N.; Wang, Jun] Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE 68588 USA.
[Ellison, Luke T.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Ellison, Luke T.; Ichoku, Charles M.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hyer, Edward J.] Naval Res Lab, Marine Meteorol Div, Monterey, CA 93943 USA.
RP Polivka, TN (reprint author), Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE 68588 USA.
EM thomas.polivka@huskers.unl.edu; jwangjun@gmail.com;
luke.ellison@nasa.gov; edward.hyer@nrlmry.navy.mil;
charles.ichoku@nasa.gov
RI Hyer, Edward/E-7734-2011; Wang, Jun/A-2977-2008
OI Hyer, Edward/0000-0001-8636-2026; Wang, Jun/0000-0002-7334-0490
FU NASA
FX This work was supported in part by the NASA Suomi NPP Program and
Applied Science Program managed by John A. Haynes and Lawrence A. Friedl
and in part by the Interdisciplinary Studies (IDS) Program directed by
J. Kaye and administered through the Radiation Sciences Program managed
by Hal B. Maring. The work of T. Polivka was also supported by the NASA
Nebraska Space Grant.
NR 75
TC 0
Z9 0
U1 10
U2 10
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 SEP
PY 2016
VL 54
IS 9
BP 5503
EP 5519
DI 10.1109/TGRS.2016.2566665
PG 17
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA DV1NZ
UT WOS:000382689300038
ER
PT J
AU Khan, A
van Driel, M
Bose, M
Giardini, D
Ceylan, S
Yan, J
Clinton, J
Euchner, F
Lognonne, P
Murdoch, N
Mimoun, D
Panning, M
Knapmeyer, M
Banerdt, WB
AF Khan, A.
van Driel, M.
Bose, M.
Giardini, D.
Ceylan, S.
Yan, J.
Clinton, J.
Euchner, F.
Lognonne, P.
Murdoch, N.
Mimoun, D.
Panning, M.
Knapmeyer, M.
Banerdt, W. B.
TI Single-station and single-event marsquake location and inversion for
structure using synthetic Martian waveforms
SO PHYSICS OF THE EARTH AND PLANETARY INTERIORS
LA English
DT Article
DE Mars; Waveforms; Marsquakes; Interior structure; Surface waves;
Body-waves; Travel times; Surface-wave overtones; Inversion
ID LUNAR MANTLE; GEOPHYSICAL CONSTRAINTS; INTERIOR STRUCTURE; TIDAL
DISSIPATION; SEISMIC DETECTION; MARS; MODEL; EARTH; CORE; MOON
AB In anticipation of the upcoming InSight mission, which is expected to deploy a single seismic station on the Martian surface in November 2018, we describe a methodology that enables locating marsquakes and obtaining information on the interior structure of Mars. The method works sequentially and is illustrated using single representative 3 -component seismograms from two separate events: a relatively large teleseismic event (Mw5.1) and a small-to-moderate-sized regional event (M(w)3.8). Location and origin time of the event is determined probabilistically from observations of Rayleigh waves and body-wave arrivals. From the recording of surface waves, averaged fundamental-mode group velocity dispersion data can be extracted and, in combination with body-wave arrival picks, inverted for crust and mantle structure. In the absence of Martian seismic data, we performed full waveform computations using a spectral element method (AxiSEM) to compute seismograms down to a period of 1 s. The model (radial profiles of density, P- and S-wave-speed, and attenuation) used for this purpose is constructed on the basis of an average Martian mantle composition and model areotherm using thermodynamic principles, mineral physics data, and viscoelastic modeling. Noise was added to the synthetic seismic data using an up-todate noise model that considers a whole series of possible noise sources generated in instrument and Iander, including wind-, thermal-, and pressure-induced effects and electromagnetic noise. The examples studied here, which are based on the assumption of spherical symmetry, show that we are able to determine epicentral distance and origin time to accuracies of similar to 0.5-1 degrees and +/- 3-6 s, respectively. For the events and the particular noise level chosen, information on Rayleigh-wave group velocity dispersion in the period range similar to 14-48 s (M(w)5.1) and similar to 14-34 s (M(w)3.8) could be determined. Stochastic inversion of dispersion data in combination with body-wave travel time information for interior structure, allows us to constrain mantle velocity structure to an uncertainty of 5%. Employing the travel times obtained with the initially inverted models, we are able to locate additional body-wave arrivals including depth phases, surface and Moho (multiple) reflections that may otherwise elude visual identification. This expanded data set is reinverted to refine interior structure models and source parameters (epicentral distance and origin time). (C) 2016 Elsevier B.V. All rights reserved.
C1 [Khan, A.; van Driel, M.; Bose, M.; Giardini, D.; Ceylan, S.; Yan, J.; Euchner, F.] Swiss Fed Inst Technol, Inst Geophys, Zurich, Switzerland.
[Bose, M.; Clinton, J.] Swiss Fed Inst Technol, Swiss Seismol Serv, Zurich, Switzerland.
[Lognonne, P.] Inst Phys Globe Paris, Paris, France.
[Murdoch, N.; Mimoun, D.] Univ Toulouse, ISAE SUPAERO, DEOS Syst Spatiaux, Toulouse, France.
[Panning, M.] Univ Florida, Dept Geol Sci, Gainesville, FL USA.
[Knapmeyer, M.] DLR, Inst Planetary Res, Berlin, Germany.
[Banerdt, W. B.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Khan, A (reprint author), Swiss Fed Inst Technol, Inst Geophys, Zurich, Switzerland.
EM amir.khan@erdw.ethz.ch
RI Lognonne, Philippe/F-8846-2010; Panning, Mark/B-3805-2011
OI Panning, Mark/0000-0002-2041-3190
FU Swiss National Science Foundation (SNF-ANR project) [157133]; Swiss
National Supercomputing Centre (CSCS) [s528]
FX We would like to thank Lapo Boschi and an anonymous reviewer for
comments on the manuscript. We would also like to acknowledge Francis
Nimmo for sharing his visco-elastic attenuation code. This work was
supported by grants from the Swiss National Science Foundation (SNF-ANR
project 157133 "Seismology on Mars") and from the Swiss National
Supercomputing Centre (CSCS) under project ID s528. Numerical
computations have also been performed on the ETH cluster Brutus.
NR 89
TC 1
Z9 1
U1 9
U2 9
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 SEP
PY 2016
VL 258
BP 28
EP 42
DI 10.1016/j.pepi.2016.05.017
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DU7SK
UT WOS:000382414700003
ER
PT J
AU McClelland, M
Campbell, M
Estlin, T
AF McClelland, Mark
Campbell, Mark
Estlin, Tara
TI Qualitative relational mapping and navigation for planetary rovers
SO ROBOTICS AND AUTONOMOUS SYSTEMS
LA English
DT Article
DE Navigation; Qualitative spatial reasoning; Qualitative methods; Mapping;
Landmark navigation
ID MOBILE ROBOTS; MAP; CONSISTENCY; INFORMATION; SPACE; SLAM
AB This paper presents a novel method for qualitative mapping of large scale spaces which decouples the mapping problem from that of position estimation. The proposed framework makes use of a graphical representation of the world in order to build a map consisting of qualitative constraints on the geometric relationships between landmark triplets. This process allows a mobile robot to extract information about landmark positions using a set of minimal sensors in the absence of GPS. A novel measurement method based on camera imagery is presented which extends previous work from the field of Qualitative Spatial Reasoning. A Branch-and-Bound approach is taken to solve a set of non-convex feasibility problems required for generating off-line operator lookup tables and on-line measurements, which are fused into the map using an iterative graph update. A navigation approach for travel between distant landmarks is developed, using estimates of the Relative Neighborhood Graph extracted from the qualitative map in order to generate a sequence of landmark objectives based on proximity. Average and asymptotic performance of the mapping algorithm is evaluated using Monte Carlo tests on randomly generated maps, and a data-driven simulation is presented for a robot traversing the Jet Propulsion Laboratory Mars Yard while building a relational map. These results demonstrate that the system can be effectively used to build a map sufficiently complete and accurate for long-distance navigation as well as other applications. (C) 2016 Elsevier B.V. All rights reserved.
C1 [McClelland, Mark; Campbell, Mark] Cornell Univ, Dept Mech & Aerosp Engn, Ithaca, NY 14853 USA.
[Estlin, Tara] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[McClelland, Mark] Cornell Univ, Mech Engn, Ithaca, NY 14853 USA.
[Campbell, Mark] Cornell Univ, Sibley Sch Mech & Aerosp Engn, Ithaca, NY 14853 USA.
[Estlin, Tara] Mission Syst & Operat Div, Pasadena, CA USA.
RP McClelland, M (reprint author), Cornell Univ, Dept Mech & Aerosp Engn, Ithaca, NY 14853 USA.; McClelland, M (reprint author), Cornell Univ, Mech Engn, Ithaca, NY 14853 USA.
EM mjm496@cornell.edu; mc288@cornell.edu; Tara.Estlin@jpl.nasa.gov
RI Campbell, Mark/F-8312-2013
OI Campbell, Mark/0000-0003-0775-4297
FU National Science Foundation [IIS-1320490]; NASA Graduate Student
Research Program
FX The research presented in this paper has been supported by National
Science Foundation grant IIS-1320490 and a fellowship from the NASA
Graduate Student Research Program. This work was performed by Cornell
University and by the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration.
NR 31
TC 0
Z9 0
U1 7
U2 7
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0921-8890
EI 1872-793X
J9 ROBOT AUTON SYST
JI Robot. Auton. Syst.
PD SEP
PY 2016
VL 83
BP 73
EP 86
DI 10.1016/j.robot.2016.05.017
PG 14
WC Automation & Control Systems; Computer Science, Artificial Intelligence;
Robotics
SC Automation & Control Systems; Computer Science; Robotics
GA DU6SB
UT WOS:000382343800006
ER
PT J
AU Patarasuk, R
Gurney, KR
O'Keeffe, D
Song, Y
Huang, JH
Rao, P
Buchert, M
Lin, JC
Mendoza, D
Ehleringer, JR
AF Patarasuk, Risa
Gurney, Kevin Robert
O'Keeffe, Darragh
Song, Yang
Huang, Jianhua
Rao, Preeti
Buchert, Martin
Lin, John C.
Mendoza, Daniel
Ehleringer, James R.
TI Urban high-resolution fossil fuel CO2 emissions quantification and
exploration of emission drivers for potential policy applications
SO URBAN ECOSYSTEMS
LA English
DT Article
DE Residential; Onroad; STIRPAT; Urban carbon; Hestia; Bottom-up approach
ID HOUSEHOLD ENERGY-CONSUMPTION; GREENHOUSE-GAS EMISSIONS; CARBON-DIOXIDE
SOURCES; SEA-LEVEL RISE; CLIMATE-CHANGE; INTEGRATED APPROACH; IMPACT;
SECTOR; MODEL; LIFE
AB Fossil fuel carbon dioxide (FFCO2) emissions are the largest driver of anthropogenic climate change. Approximately three-quarters of the world's fossil fuels carbon dioxide emissions are generated in urban areas. We used the Hestia high resolution approach to quantify FFCO2 for Salt Lake County, Utah, USA and demonstrate the importance of high resolution quantification to urban emissions mitigation policymaking. We focus on the residential and onroad sectors across both urbanized and urbanizing parts of the valley. Stochastic Impact by Regression on Population, Affluence, and Technology (STIRPAT) regression models using sociodemographic data at the census block group level shows that population, per capita income, and building age exhibit positive relationships while household size shows a negative relationship with FFCO2 emissions. Compact development shows little effect on FFCO2 emissions in this domain. FFCO2 emissions in high income block groups is twice as sensitive to income than low income block groups. Emissions are four times as sensitive to household size in low-income versus high-income block groups. These results suggest that policy options targeting personal responsibility or knowledge feedback loops may be the most effective strategies. Examples include utility bill performance comparison or publicly available energy maps identifying high-emitting areas. Within the onroad sector, high emissions density (FFCO2/km) is associated with primary roads, while high emissions intensity (FFCO2/VMT) is associated with secondary roads. Opportunities exist for alignment of public transportation extension with remaining high emission road segments, offering a prioritization of new onroad transportation policy in Salt Lake County.
C1 [Patarasuk, Risa; Gurney, Kevin Robert; O'Keeffe, Darragh; Song, Yang; Huang, Jianhua] Arizona State Univ, Sch Life Sci, POB 874501, Tempe, AZ 85287 USA.
[Gurney, Kevin Robert; O'Keeffe, Darragh] Arizona State Univ, Global Inst Sustainabil, POB 875502, Tempe, AZ 85287 USA.
[Rao, Preeti] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Buchert, Martin] Univ Utah, Global Change & Sustainabil Ctr, 155 South 1452 East, Salt Lake City, UT USA.
[Lin, John C.; Mendoza, Daniel] Univ Utah, Dept Atmospher Sci, 135 South 1460 East, Salt Lake City, UT 84112 USA.
[Ehleringer, James R.] Univ Utah, Dept Biol, 257 South 1400 East, Salt Lake City, UT 84112 USA.
RP Patarasuk, R (reprint author), Arizona State Univ, Sch Life Sci, POB 874501, Tempe, AZ 85287 USA.
EM risa.patarasuk@asu.edu
OI Buchert, Martin/0000-0001-5974-001X; Rao, Preeti/0000-0002-5549-0583
FU Department of Energy [DE-SC-001-0624]; National Science Foundation
[EF-01241286]; National Institute of Standards and Technology
[70NANB14H321]; National Oceanic and Atmospheric Administration Climate
Program Office's Atmospheric Chemistry, Carbon Cycle, and Climate
Program [NA14OAR4310178]
FX This research was supported by grants from the Department of Energy
DE-SC-001-0624, the National Science Foundation grant EF-01241286,
National Institute of Standards and Technology grant 70NANB14H321, and
National Oceanic and Atmospheric Administration Climate Program Office's
Atmospheric Chemistry, Carbon Cycle, and Climate Program grant
NA14OAR4310178. We also would like to thank Jerome Zenger, Kevin Bell,
and Semih Yildiz for assisting with the data collection and inquiry.
NR 109
TC 1
Z9 1
U1 19
U2 19
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1083-8155
EI 1573-1642
J9 URBAN ECOSYST
JI Urban Ecosyst.
PD SEP
PY 2016
VL 19
IS 3
BP 1013
EP 1039
DI 10.1007/s11252-016-0553-1
PG 27
WC Biodiversity Conservation; Ecology; Environmental Sciences; Urban
Studies
SC Biodiversity & Conservation; Environmental Sciences & Ecology; Urban
Studies
GA DV1HB
UT WOS:000382670600001
ER
PT J
AU Liu, YC
Xu, YH
Hicks, MC
Avedisian, CT
AF Liu, Yu Cheng
Xu, Yuhao
Hicks, Michael C.
Avedisian, C. Thomas
TI Comprehensive study of initial diameter effects and other observations
on convection-free droplet combustion in the standard atmosphere for
n-heptane, n-octane, and n-decane
SO COMBUSTION AND FLAME
LA English
DT Article
DE Droplet combustion; Microgravity; Extinction; Radiation; Low temperature
combustion; Soot formation
ID MICROGRAVITY CONDITIONS; SOOT FORMATION; FUEL DROPLETS; BURNING RATE;
COOL-FLAMES; LOW-GRAVITY; EXTINCTION; MIXTURES; VAPORIZATION; RADIATION
AB This paper reports the results of a comprehensive experimental study on the effect of initial droplet diameter (Do) over a very wide range (0.5 mm < D-0 < 5 mm) on the spherically symmetric droplet burning characteristics in the standard atmosphere of three alkanes - n-heptane, n-octane and n-decane - that are representative of components found in petroleum-based transportation fuels and their surrogates. Spherical symmetry in the burning process was promoted by carrying out the experiments in a reduced convection (stagnant ambience) and buoyancy (low gravity) environment using the facilities of a ground based drop tower for D-0 < 0.8 mm and a spaced-based platform (the International Space Station) for D-0 > 1.0 mm.
The results show that for Do greater than about 2 mm, K decreases with increasing Do in an early period of burning and with the data being correlated in the form K similar to D-0(-n) based on a scale analysis of an energy balance on the flame. For Do larger than approximately 2 mm the droplet flames often disappeared indicating an extinction mechanism that was speculated to be due to radiative losses from the flame. Concurrently, measurements of wideband radiation dropped significantly and the burning rate gradually approached pure evaporation.
In some instances for n-heptane and n-octane radiative extinction was accompanied by droplet evaporation rates that were significantly higher than evaporation in a hot ambience which persisted for a significant fraction of the burning history before decreasing to evaporation in a cold ambience. An energy balance on the drop related the flame temperature to droplet diameter from which it was predicted that flame temperatures after ignition were greater than 1200 K before dropping to under approximately 800 K and remaining constant thereafter until eventually reaching near ambient conditions. This intermediate regime of burning was conjectured to be associated with a low temperature combustion process. The transition to this intermediate regime upon radiative extinction was occasionally accompanied by flame oscillations, the origin of which was uncertain but could have been initiated by motion of the droplet owing to the deployment process. (C) 2016 The Combustion Institute. Published by Elsevier Inc. All rights reserved.
C1 [Liu, Yu Cheng] Univ Michigan Flint, Dept Comp Sci Engn & Phys, Flint, MI 48502 USA.
[Xu, Yuhao; Avedisian, C. Thomas] Cornell Univ, Sibley Sch Mech & Aerosp Engn, Ithaca, NY 14853 USA.
[Hicks, Michael C.] NASA, Glenn Res Ctr, Combust & Reacting Syst Branch, Cleveland, OH 44135 USA.
[Liu, Yu Cheng] Tsinghua Univ, Ctr Combust Energy, Beijing 100084, Peoples R China.
RP Avedisian, CT (reprint author), Cornell Univ, Sibley Sch Mech & Aerosp Engn, Ithaca, NY 14853 USA.
EM cta2@cornell.edu
OI Liu, Yu Cheng/0000-0001-7954-717X
FU National Administration of Space and Aeronautics (NASA) [NNX08AI51G]
FX This work was supported by the National Administration of Space and
Aeronautics (NASA) under Grants NNX08AI51G to Cornell University (where
the ground-based experiments were carried out). The authors are pleased
to acknowledge Drs. Vedha Nayagam and Daniel Dietrich of NASA-Glenn who
offered insights regarding data analysis and combustion physics of some
of the observed trends and assistance with some of the reported
experiments. Messrs Jeff Rah, Koffi Trenou, Wei-Chih Kuo and Anthony
Savas of Cornell provided assistance with the experiments reported here
and analyses of the data. The interest of F.A. Williams (UC-San Diego),
F.L. Dryer (Princeton), T. Farouk (U. South Carolina), and B.D. Shaw
(UC-Davis)) is also greatly appreciated.
NR 60
TC 4
Z9 4
U1 10
U2 12
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0010-2180
EI 1556-2921
J9 COMBUST FLAME
JI Combust. Flame
PD SEP
PY 2016
VL 171
BP 27
EP 41
DI 10.1016/j.combustfiame.2016.05.013
PG 15
WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary;
Engineering, Chemical; Engineering, Mechanical
SC Thermodynamics; Energy & Fuels; Engineering
GA DU9CE
UT WOS:000382513000003
ER
PT J
AU de Wit, J
Wakeford, HR
Gillon, M
Lewis, NK
Valenti, JA
Demory, BO
Burgasser, AJ
Burdanov, A
Delrez, L
Jehin, E
Lederer, SM
Queloz, D
Triaud, AHMJ
Van Grootel, V
AF de Wit, Julien
Wakeford, Hannah R.
Gillon, Michael
Lewis, Nikole K.
Valenti, Jeff A.
Demory, Brice-Olivier
Burgasser, Adam J.
Burdanov, Artem
Delrez, Laetitia
Jehin, Emmanuel
Lederer, Susan M.
Queloz, Didier
Triaud, Amaury H. M. J.
Van Grootel, Valerie
TI A combined transmission spectrum of the Earth-sized exoplanets
TRAPPIST-1 b and c
SO NATURE
LA English
DT Article
ID HUBBLE-SPACE-TELESCOPE; HABITABLE-ZONE; LIGHT CURVES; SUPER-EARTHS; GJ
1214B; SPECTROSCOPY; ATMOSPHERES; PLANETS; KEPLER; EVAPORATION
AB Three Earth-sized exoplanets were recently discovered close to the habitable zone(1,2) of the nearby ultracool dwarf star TRAPPIST-1 (ref. 3). The nature of these planets has yet to be determined, as their masses remain unmeasured and no observational constraint is available for the planetary population surrounding ultracool dwarfs, of which the TRAPPIST-1 planets are the first transiting example. Theoretical predictions span the entire atmospheric range, from depleted to extended hydrogen-dominated atmospheres(4-8). Here we report observations of the combined transmission spectrum of the two inner planets during their simultaneous transits on 4 May 2016. The lack of features in the combined spectrum rules out doud-free hydrogen-dominated atmospheres for each planet at >= 10 sigma levels; TRAPPIST-1 b and c are therefore unlikely to have an extended gas envelope as they occupy a region of parameter space in which high-altitude cloud/haze formation is not expected to be significant for hydrogen-dominated atmospheres(9). Many denser atmospheres remain consistent with the featureless transmission spectrum from a cloud-free water-vapour atmosphere to a Venus-like one.
C1 [de Wit, Julien] MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Wakeford, Hannah R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gillon, Michael; Burdanov, Artem; Delrez, Laetitia; Jehin, Emmanuel; Van Grootel, Valerie] Univ Liege, Inst Astrophys & Geophys, Allee 6 Aout 19C, B-4000 Liege, Belgium.
[Lewis, Nikole K.; Valenti, Jeff A.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
[Demory, Brice-Olivier; Queloz, Didier] Cavendish Lab, Astrophys Grp, 19 JJ Thomson Ave, Cambridge CB3 0HE, England.
[Burgasser, Adam J.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Lederer, Susan M.] NASA, Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA.
[Triaud, Amaury H. M. J.] Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
RP de Wit, J (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM jdewit@mit.edu
OI Wakeford, Hannah/0000-0003-4328-3867
FU NASA through Space Telescope Science Institute [HST-GO-14500]; European
Research Council (ERC) [336480]; Action de Recherche Concertee (ARC) by
Wallonia-Brussels Federation; NASA; Fund for Research Training in
Industry and Agriculture of the FRS-FNRS
FX This work is based on observations made with the NASA/ESA Hubble Space
Telescope that were obtained at the Space Telescope Science Institute,
which is operated by the Association of Universities for Research in
Astronomy, Inc. These observations are associated with program
HST-GO-14500 (principal investigator J.d.W.), support for which was
provided by NASA through a grant from the Space Telescope Science
Institute. The research leading to our results was funded in part by the
European Research Council (ERC) under the FP/2007-2013 ERC grant 336480,
and through an Action de Recherche Concertee (ARC) grant financed by the
Wallonia-Brussels Federation. H.R.W. acknowledges support through an
appointment to the NASA Postdoctoral Program at Goddard Space Flight
Center, administered by the Universities Space Research Association
through a contract with NASA. M.G. is Research Associate at the Belgian
Fonds (National) de la Recherche Scientifique (FRS-FNRS). L.D.
acknowledges support of the Fund for Research Training in Industry and
Agriculture of the FRS-FNRS. We thank D. Taylor, S. Deustua, P.
McCullough, and N. Reid for their assistance in planning and executing
our observations. We are also grateful for discussions with Z.
Berta-Thompson and Pierre Magain about this study and manuscript. We
thank the ATLAS and PHOENIX teams for providing stellar models.
NR 26
TC 6
Z9 6
U1 12
U2 15
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 SEP 1
PY 2016
VL 537
IS 7618
BP 69
EP 72
DI 10.1038/nature18641
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DU7XC
UT WOS:000382426900039
PM 27437572
ER
PT J
AU Sears, DWG
AF Sears, Derek W. G.
TI The CO chondrites: Major recent Antarctic finds, their thermal and
radiation history, and describing the metamorphic history of members of
the class
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
DE CO chondrites; Metamorphism; Thermoluminescence; Antarctic meteorites
ID UNEQUILIBRATED ORDINARY CHONDRITES; NATURAL THERMOLUMINESCENCE;
CARBONACEOUS CHONDRITES; TERRESTRIAL AGES; TYPE-3 CHONDRITES;
OXYGEN-ISOTOPE; PARENT-BODY; METEORITES; LUMINESCENCE; ORBITS
AB Thermoluminescence (TL) properties of 29 CO chondrites from the Miller Range (MIL) and five chondrites from the Dominion Range (DOM) have been measured. MIL has a relatively strong natural TL signal (19.6 +/- 14.7 krad), while some of the DOM samples have a very weak natural TL signal (<1 krad) whereas others resemble the MIL meteorites. I argue that MIL and some of the DOM samples had a normal perihelion (similar to 1.0 AU) and terrestrial age of similar to 450-700 ka, while some of the DOM samples have a terrestrial age of similar to 100 ka but a perihelion of similar to 0.8 AU. The DOM meteorites also show considerable heterogeneity in their induced TL properties, also suggesting that the DOM fragments represent more than one fall. The induced TL data for the MIL samples studied here are consistent with them all being from a single fragmented meteorite. Small (50 mg) chips have TL properties similar to 500 mg chips, so that the smaller chips are representative, although samples taken from original masses less than similar to 2 g have low natural TL suggesting that they were heated during atmospheric fall. The properties of CO chondrites are reviewed in terms of their petrologic types. Correlations between TL sensitivity, the most quantitative technique for evaluating metamorphic alteration in CO chondrites, and data for olivine composition and heterogeneity, matrix composition, inert gas content, metal composition (Ni, Co, and Cr in the kamacite), bulk carbon, C and O isotopes, graphite ordering, spectral reflectance at 0.8 mu m, and textural characteristics of the ameboid olivine and Ca-rich inclusions are examined. The petrographic types appear to be largely metamorphic in origin with perhaps a minor role for metasomatism. Contrary to recent proposals it is here argued that petrologic type definitions should (1) be specific enough to be meaningful, but broad enough to be simple in application and robust to new developments, (2) be descriptive and not interpretative, (3) should not oversimplify and obscure important class-to-class differences, and (4) take account of all the available information, while avoiding reliance on any one technique or single observation whose application is based on interpretation. With these considerations in mind the petrographic type definitions for CO chondrites are restated and the petrologic type of 3.2 assigned to both the MIL and DOM CO chondrites. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Sears, Derek W. G.] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Space Sci & Astrobiol Div MS 245 3, Mountain View, CA 94035 USA.
RP Sears, DWG (reprint author), NASA, Ames Res Ctr, Bay Area Environm Res Inst, Space Sci & Astrobiol Div MS 245 3, Mountain View, CA 94035 USA.
FU NASA's Solar System Exploration and Research Virtual Institute
FX I am grateful to Tim Lee and Chris McKay for providing facilities and an
exciting research environment at NASA Ames Research Center and I am
grateful to Mark Sittloh and his colleagues at the Bay Area
Environmental Research Institute for management support. I am also
grateful to the Antarctic Meteorite Working Group for providing the
samples and the Meteorite Processing Laboratory at Johnson Space Center
for so capably handling the sampling. I am also grateful to Hazel Sears
for reviewing and proofing this paper, David Sears for help with the
statistical analysis, four anonymous journal reviewers who provided much
appreciated reviews (which included the suggestion to include Fig. 7),
and Chris Herd for organizing these reviews. Finally, I am pleased to
acknowledge the Field Investigations to Enable Solar System Science and
Exploration team of NASA's Solar System Exploration and Research Virtual
Institute (PI: Jennifer Heldmann) for financial support.
NR 54
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 0016-7037
EI 1872-9533
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD SEP 1
PY 2016
VL 188
BP 106
EP 124
DI 10.1016/j.gca.2016.05.033
PG 19
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DS4LN
UT WOS:000380752700007
ER
PT J
AU Robinson, KL
Barnes, JJ
Nagashima, K
Thomen, A
Franchi, IA
Huss, GR
Anand, M
Taylor, GJ
AF Robinson, Katharine L.
Barnes, Jessica J.
Nagashima, Kazuhide
Thomen, Aurelien
Franchi, Ian A.
Huss, Gary R.
Anand, Mahesh
Taylor, G. Jeffrey
TI Water in evolved lunar rocks: Evidence for multiple reservoirs
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
DE Moon; Lunar volatiles; Apatite; Water; H isotopes
ID SILICATE-LIQUID-IMMISCIBILITY; HOSTED MELT INCLUSIONS; TERRESTRIAL
PLANETS; VOLCANIC GLASSES; MG-SUITE; VOLATILE ABUNDANCES; QUARTZ
MONZODIORITE; CRYSTAL-CHEMISTRY; COOLING HISTORY; OXYGEN FUGACITY
AB We have measured the abundance and isotopic composition of water in apatites from several lunar rocks representing Potassium (K), Rare Earth Elements (REE), and Phosphorus (P) - KREEP - rich lithologies, including felsites, quartz monzodiorites (QMDs), a troctolite, and an alkali anorthosite. The H-isotope data from apatite provide evidence for multiple reservoirs in the lunar interior. Apatite measurements from some KREEP-rich intrusive rocks display moderately elevated delta D signatures, while other samples show delta D signatures similar to the range known for the terrestrial upper mantle. Apatite grains in Apollo 15 quartz monzodiorites have the lowest delta D values measured from the Moon so far (as low as -749 parts per thousand), and could potentially represent a D-depleted reservoir in the lunar interior that had not been identified until now. Apatite in all of these intrusive rocks contains <267 ppm H2O, which is relatively low compared to apatites from the majority of studied mare basalts (200 to >6500 ppm H2O). Complexities in partitioning of volatiles into apatite make this comparison uncertain, but measurements of residual glass in KREEP basalt fragments in breccia 15358 independently show that the KREEP basaltic magmas were low in water. The source of 15358 contained similar to 10 ppm H2O, about an order of magnitude lower than the source of the Apollo 17 pyroclastic glass beads, suggesting potential variations in the distribution of water in the lunar interior. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Robinson, Katharine L.; Nagashima, Kazuhide; Thomen, Aurelien; Huss, Gary R.; Taylor, G. Jeffrey] Hawaii Inst Geophys & Planetol, 1680 East West Rd,POST 602, Honolulu, HI 96822 USA.
[Robinson, Katharine L.; Huss, Gary R.; Taylor, G. Jeffrey] Univ Hawaii, NASA Astrobiol Inst, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
[Robinson, Katharine L.; Huss, Gary R.; Taylor, G. Jeffrey] Univ Hawaii Manoa, Geol & Geophys, 1680 East West Rd,POST 602, Honolulu, HI 96822 USA.
[Barnes, Jessica J.; Franchi, Ian A.; Anand, Mahesh] Open Univ, Planetary & Space Sci, Walton Hall, Milton Keynes MK7 6AA, Bucks, England.
[Anand, Mahesh] Nat Hist Museum, Dept Earth Sci, Cromwell Rd, London SW7 5BD, England.
RP Robinson, KL (reprint author), Open Univ, Planetary & Space Sci, Walton Hall, Milton Keynes MK7 6AA, Bucks, England.
EM katie.robinson@open.ac.uk
FU National Aeronautics and Space Administration through the NASA
Astrobiology Institute through the Office of Space Science [NNA09DA77A];
NASA Lunar Advanced Science and Exploration Research [NNX11AE85G]; Solar
System Exploration Research Virtual Institute (through the Center for
Lunar Science and Exploration) [NNA14AB07A]; Bullard Foundation; STFC
[ST/I001298/1, ST/L000776/1]
FX The authors thank Romain Tartese for his assistance in collecting data
and for highly useful discussions. This research was supported by the
National Aeronautics and Space Administration through the NASA
Astrobiology Institute under Cooperative Agreement No. NNA09DA77A issued
through the Office of Space Science, by NASA Lunar Advanced Science and
Exploration Research Grant NNX11AE85G, the Solar System Exploration
Research Virtual Institute (through the Center for Lunar Science and
Exploration cooperative agreement NNA14AB07A, David Kring, PI), and by
The Bullard Foundation. STFC are also thanked for a PhD studentship to
JJB and research grants to MA (Grant no. ST/I001298/1 and ST/L000776/1).
We thank three anonymous reviewers and associate editor Alexander
Nemchin for insightful and critical comments that helped improve the
quality of the manuscript.
NR 115
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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 SEP 1
PY 2016
VL 188
BP 244
EP 260
DI 10.1016/j.gca.2016.05.030
PG 17
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DS4LN
UT WOS:000380752700014
ER
PT J
AU Peretyazhko, TS
Fox, A
Sutter, B
Niles, PB
Adams, M
Morris, RV
Ming, DW
AF Peretyazhko, T. S.
Fox, A.
Sutter, B.
Niles, P. B.
Adams, M.
Morris, R. V.
Ming, D. W.
TI Synthesis of akaganeite in the presence of sulfate: Implications for
akaganeite formation in Yellowknife Bay, Gale Crater, Mars
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
DE Mars; Gale crater; Yellowknife Bay; Fe oxides; Akaganeite
ID ACID-MINE DRAINAGE; BETA-FEOOH; AQUEOUS-SOLUTIONS; REFLECTANCE
SPECTROSCOPY; SPECTRAL PROPERTIES; FORCED HYDROLYSIS; MERIDIANI-PLANUM;
X-RAY; IRON; JAROSITE
AB Akaganeite, a Cl-bearing Fe(III) (hydr)oxide, has been recently discovered in Yellowknife Bay in Gale crater on Mars by the Mars Science Laboratory (MSL) Curiosity Rover. Akaganeite was associated with sulfate and sulfide minerals at Yellowknife Bay indicating that sulfate ions could be present in solution during akaganeite formation. The mechanism and conditions of akaganeite formation in the Yellowknife Bay mudstone are unknown. We investigated formation of akaganeite through hydrolysis of ferric chloride solution in the presence of 0, 0.01, 0.05, 0.1 and 0.2 M sulfate and at initial pH of 1.5, 2 and 4 at 90 degrees C. Mineralogy of the precipitated Fe(III) phases was characterized by X-ray diffraction and infrared spectroscopy. The precipitates were also acid digested to determine total sulfate and chloride contents. Akaganeite and natrojarosite formed at initial solution pH of 1.5; akaganeite, goethite and natrojarosite precipitated in initial pH 2 solutions and goethite, hematite and 2-line ferrihydrite precipitated at initial solution pH of 4. Sulfate addition did not inhibit akaganeite formation. Increasing initial solution sulfate concentrations resulted in increasing sulfate to chloride ratio in the precipitated akaganeite. Infrared spectroscopy revealed akaganeite bands at similar to 2 mu m (H2O combination band) and at similar to 2.46 mu m (OH combination band). The H2O combination band position linearly correlated with total chloride content in akaganeite. Overall, laboratory studies demonstrated formation of akaganeite at initial sulfate concentration <= 0.2 M (sulfate to chloride molar ratio <= 0.3) and pH <= 2, implying that those conditions might prevail (perhaps as micro-environments) during akaganeite formation in Yellowknife Bay mudstone. The occurrence of Fe(II) sulfides (pyrite and pyrrhotite) in Yellowknife Bay mudstone is a potential acidity source. Dissolution of sulfide minerals might occur under localized oxidizing waterlimiting Cl-rich conditions creating favorable environments for akaganeite formation. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Peretyazhko, T. S.; Sutter, B.] NASA, Jacobs, Johnson Space Ctr, Houston, TX 77058 USA.
[Fox, A.] Indiana Univ, Bloomington, IN 47406 USA.
[Niles, P. B.; Morris, R. V.; Ming, D. W.] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
[Adams, M.] Univ Hawaii, Hilo, HI 96720 USA.
RP Peretyazhko, TS (reprint author), NASA, Jacobs, Johnson Space Ctr, Houston, TX 77058 USA.
EM tanya.peretyazhko@nasa.gov
FU Summer Intern Scholarship of Lunar and Planetary Institute; NASA Mars
Science Laboratory Mission grants; NASA Solar System Workings grant
[15-SSW15_2-0074]
FX We are grateful to Z. Peng for performing ICP-MS analysis and K. Pando
and D. Locke for help with ion chromatography. We thank Dr. Bishop and
two anonymous reviewers for valuable suggestions and comments that help
to improve the quality of the manuscript. We thank the Associate Editor
Dr. Catalano for handling the manuscript. A. Fox acknowledges a Summer
Intern Scholarship of Lunar and Planetary Institute. This work was
supported by NASA Mars Science Laboratory Mission grants and by NASA
Solar System Workings grant #15-SSW15_2-0074. The data presented in
figures could be provided upon request.
NR 76
TC 0
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U1 18
U2 25
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 SEP 1
PY 2016
VL 188
BP 284
EP 296
DI 10.1016/j.gca.2016.06.002
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA DS4LN
UT WOS:000380752700016
ER
PT J
AU Ting, DZ
Soibel, A
Hoglund, L
Hill, CJ
Keo, SA
Fisher, A
Gunapala, SD
AF Ting, David Z.
Soibel, Alexander
Hoeglund, Linda
Hill, Cory J.
Keo, Sam A.
Fisher, Anita
Gunapala, Sarath D.
TI High-Temperature Characteristics of an InAsSb/AlAsSb n(+)Bn Detector
SO JOURNAL OF ELECTRONIC MATERIALS
LA English
DT Article
DE Infrared detector; unipolar barrier; nBn; mid-wavelength infrared
AB The high-temperature characteristics of a mid-wavelength infrared (MWIR) detector based on the Maimon-Wicks InAsSb/AlAsSb nBn architecture was analyzed. The dark current characteristics are examined in reference to recent minority carrier lifetime results. The difference between the responsivity and absorption quantum efficiency (QE) at shorter wavelengths is clarified in terms of preferential absorption of higher-energy photons in the top contact layer, which cannot provide reverse-bias photo-response due to the AlAsSb electron blocking layer and strong recombination. Although the QE does not degrade when the operating temperature increases to 325 K, the turn-on bias becomes larger at higher temperatures. This behavior was originally attributed to the change in the valence band alignment between the absorber and top contact layers caused by the shift in Fermi level with temperature. In this work, we demonstrated the inadequacy of the original description, and offer a more likely explanation based on temperature-dependent band-bending effects.
C1 [Ting, David Z.; Soibel, Alexander; Hoeglund, Linda; Hill, Cory J.; Keo, Sam A.; Fisher, Anita; Gunapala, Sarath D.] NASA, Jet Prop Lab, Ctr Infrared Photodetectors, M-S302-231,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Soibel, Alexander; Hoeglund, Linda; Hill, Cory J.; Keo, Sam A.; Fisher, Anita; Gunapala, Sarath D.] CALTECH, Pasadena, CA 91109 USA.
RP Ting, DZ (reprint author), NASA, Jet Prop Lab, Ctr Infrared Photodetectors, M-S302-231,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM David.Z.Ting@jpl.nasa.gov
NR 8
TC 2
Z9 2
U1 11
U2 11
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0361-5235
EI 1543-186X
J9 J ELECTRON MATER
JI J. Electron. Mater.
PD SEP
PY 2016
VL 45
IS 9
BP 4680
EP 4685
DI 10.1007/s11664-016-4633-z
PG 6
WC Engineering, Electrical & Electronic; Materials Science,
Multidisciplinary; Physics, Applied
SC Engineering; Materials Science; Physics
GA DS9CM
UT WOS:000381080000027
ER
PT J
AU Suhir, E
Ghaffarian, R
AF Suhir, E.
Ghaffarian, R.
TI Board level drop test: exact solution to the problem of the nonlinear
dynamic response of a PCB to the drop impact
SO JOURNAL OF MATERIALS SCIENCE-MATERIALS IN ELECTRONICS
LA English
DT Article
AB An analytical predictive model has been developed for the evaluation of the nonlinear dynamic response of a printed-circuit-board (PCB) to the drop impact during board-level testing. The hypothesis of "heavy-and-flexible" PCB is used in the analysis: the surface-mounted-devices (SMDs) are assumed to be small enough not to affect the PCB's flexural rigidity, but their masses have been considered and accounted for by "spreading out" the SMD total mass over the PCB surface. The analysis is restricted to the fundamental mode of vibrations, and the method of principal coordinates is used to evaluate the response. The exact solution to the nonlinear differential equation for the principal coordinate has been obtained. Another important finding is that the nonlinear amplitudes were determined even without solving the nonlinear differential equation of motion. The main objective of the analysis is to provide design guidelines for constructing a feasible experimental setup. A simply supported board is suggested as the most appropriate structure for an adequate test vehicle: the experimental data for such a board, as far as the behavior of the solder material in the second level of interconnections is concerned, can be easily and reliably interpreted and extrapolated for the practical use. The developed model enables one to predict the induced bending moments and the in-plane (membrane) forces that could be applied in the subsequent analyses to the PCB areas in the proximity of the package and its solder joint interconnections.
C1 [Suhir, E.] 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 21
TC 1
Z9 1
U1 10
U2 10
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 SEP
PY 2016
VL 27
IS 9
BP 9423
EP 9430
DI 10.1007/s10854-016-4988-1
PG 8
WC Engineering, Electrical & Electronic; Materials Science,
Multidisciplinary; Physics, Applied; Physics, Condensed Matter
SC Engineering; Materials Science; Physics
GA DT0FY
UT WOS:000381159800074
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 THE IN-PHASE REFLECTION BANDWIDTH THEORETICAL LIMIT OF ARTIFICIAL
MAGNETIC CONDUCTORS BASED ON TRANSMISSION LINE MODEL
SO MICROWAVE AND OPTICAL TECHNOLOGY LETTERS
LA English
DT Article
DE artificial magnetic conductors (AMCs); transmission line model;
bandwidth limitation
ID HIGH-IMPEDANCE SURFACES; FREQUENCY; ANTENNAS; ABSORBERS; DESIGN
AB Based on the transmission line model, the in-phase reflection (IPR) bandwidth theoretical limit using a function of permeability (l) and thickness (h) of the substrate as well as center frequency of IPR (f) was expressed. An experimental design strategy was further derived from this function for creating novel artificial magnetic conductors (AMCs). To date, they have successfully designed, simulated, and experimentally verified this proposed strategy with various AMCs, where the bandwidth ratio to the theoretical limit can be achieved by as high as 98.5%. This newly proposed theoretical limit function was further evaluated in two-ways, (1) our theoretical limit was compared with previously reported literature values, and (2) literature values were recalculated using our function. Herein, it was concluded that their IPR bandwidth theoretical limit function provided most restrictive and accurate value, and their AMC design strategy has showed evident advantages over literature. (C) 2016 Wiley Periodicals, Inc.
C1 [Xie, Yunsong; Chen, Yunpeng] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Fan, Xin] Univ Denver, Dept Phys & Astron, Newark, DE 19716 USA.
[Wilson, Jeffrey D.; Simons, Rainee N.; Xiao, John Q.] Glenn Res Ctr, Natl Aeronaut & Space Adm, Cleveland, OH USA.
RP Xiao, JQ (reprint author), Glenn Res Ctr, Natl Aeronaut & Space Adm, Cleveland, OH USA.
EM jqx@udel.edu
FU National Aeronautics and Space Administration (NASA) [NNX11AQ29A]
FX This work was supported by the National Aeronautics and Space
Administration (NASA) under Grant No. NNX11AQ29A.
NR 22
TC 0
Z9 0
U1 6
U2 7
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0895-2477
EI 1098-2760
J9 MICROW OPT TECHN LET
JI Microw. Opt. Technol. Lett.
PD SEP
PY 2016
VL 58
IS 9
BP 2257
EP 2261
DI 10.1002/mop.30024
PG 6
WC Engineering, Electrical & Electronic; Optics
SC Engineering; Optics
GA DS7DW
UT WOS:000380944000052
ER
PT J
AU Bianco, WT
Landis, R
AF Bianco, William T.
Landis, Robert
TI Engineering cooperation: How Americans and Russians manage joint
operation of the International Space Station
SO INTERNATIONAL AREA STUDIES REVIEW
LA English
DT Article
DE Cooperation; prisoners' dilemma; new economics of organization;
International Space Station; NASA
AB The 1990s agreements that created the International Space Station (ISS) described the effort as a partnership of equals, a joint venture between organizations that remained independent in terms of many procedures, norms, goals, and the assumptions underlying these factors. As a result, successful joint ISS operations required the participants, most notably the American and Russian space programs, to reconcile different procedures, norms, and training regimes, as well as the beliefs that underlie these practices. Drawing on a combination of operational experience, first-hand observation, and interviews, this paper focuses on how the two programs reduced conflict and engendered cooperation. It also uses the ISS experience to consider how future joint efforts can be designed to minimize conflict between international partners.
C1 [Bianco, William T.] Indiana Univ, Woodburn Hall 210, Bloomington, IN 47401 USA.
[Landis, Robert] NASA Headquarters, Washington, DC USA.
RP Bianco, WT (reprint author), Indiana Univ, Woodburn Hall 210, Bloomington, IN 47401 USA.
EM wbianco@indiana.edu
NR 12
TC 0
Z9 0
U1 4
U2 4
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 2233-8659
EI 2049-1123
J9 INT AREA STUD REV
JI Int. Area Stud. Rev.
PD SEP
PY 2016
VL 19
IS 3
BP 197
EP 209
DI 10.1177/2233865916636834
PG 13
WC International Relations
SC International Relations
GA DT6WT
UT WOS:000381626100001
ER
PT J
AU Ghods, M
Johnson, L
Lauer, M
Grugel, RN
Tewari, SN
Poirier, DR
AF Ghods, M.
Johnson, L.
Lauer, M.
Grugel, R. N.
Tewari, S. N.
Poirier, D. R.
TI Macrosegregation in Al-7Si alloy caused by abrupt cross-section change
during directional solidification
SO JOURNAL OF CRYSTAL GROWTH
LA English
DT Article
DE Directional solidification; Cross-section change; Computer simulation;
Fluid flows; Segregation; Aluminum alloys
ID PB-SN ALLOYS; DENDRITIC SOLIDIFICATION; NATURAL-CONVECTION; METALLIC
ALLOYS; SUPERALLOY CASTINGS; GRAIN STRUCTURES; RAYLEIGH NUMBER;
CRYSTAL-GROWTH; TURBINE-BLADES; BINARY-ALLOYS
AB Hypoeutectic Al-7 wt.% Si alloys were directionally solidified vertically downward in cylindrical molds that incorporated an abrupt cross-section decrease (9.5 mm to 3.2 mm diameter) which, after 5 cm, reverted back to 9.5 mm diameter in a Bridgman furnace; two constant growth speeds and thermal gradients were investigated. Thermosolutal convection and cross-section-change-induced shrinkage flow effects on macrosegregation were investigated. Dendrite clustering and extensive radial macro segregation was seen, particularly in the larger cross-sections, before contraction and after expansion, this more evident at the lower growth speed. This alloy shows positive longitudinal macrosegregation near cross-section decrease followed by negative macrosegregation right after it; the extent of macro segregation, however, decreases with increasing growth speed. Primary dendrite steepling intensified as solidification proceeded into the narrower section and negative longitudinal macrosegregation was seen on the re-entrant shelves at expansion. A two-dimensional model accounting for both shrinkage and thermo-solutal convection was used to simulate solidification and the resulting mushy-zone steepling and macrosegregation. The experimentally observed longitudinal and radial macrosegregation associated with the cross-section changes during directional solidification of an Al-75i alloy is well captured by the numerical simulations. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Ghods, M.; Johnson, L.; Tewari, S. N.] Cleveland State Univ, Chem & Biomed Engn Dept, Cleveland, OH 44114 USA.
[Lauer, M.; Poirier, D. R.] Univ Arizona, Dept Mat Sci & Engn, Tucson, AZ 85721 USA.
[Grugel, R. N.] NASA, Marshall Space Flight Space Ctr, Huntsville, AL 35811 USA.
[Johnson, L.] Avery Dennison Corp, Painesville, OH 44077 USA.
[Lauer, M.] ME Elecmetal Inc, Duluth, MN 55808 USA.
RP Ghods, M (reprint author), Cleveland State Univ, Chem & Biomed Engn Dept, Cleveland, OH 44114 USA.
EM ghods.masoud@gmail.com
FU NASA [NX10AV40G, NNX14AM18G]; Sandia National Laboratories Campus
Executive Fellowship program
FX This work was supported by NASA Grant NX10AV40G and NNX14AM18G. The
Al-7% Si alloys for our current research were kindly provided by Dr. Men
G. Chu at ALCOA Technical Center. M. Lauer would like to acknowledge
support from the Sandia National Laboratories Campus Executive
Fellowship program.
NR 54
TC 1
Z9 1
U1 6
U2 6
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-0248
EI 1873-5002
J9 J CRYST GROWTH
JI J. Cryst. Growth
PD SEP 1
PY 2016
VL 449
BP 134
EP 147
DI 10.1016/j.jcrysgro.2016.06.010
PG 14
WC Crystallography; Materials Science, Multidisciplinary; Physics, Applied
SC Crystallography; Materials Science; Physics
GA DS5RT
UT WOS:000380840700022
ER
PT J
AU Ryoo, MS
Matthies, L
AF Ryoo, M. S.
Matthies, Larry
TI First-Person Activity Recognition: Feature, Temporal Structure, and
Prediction
SO INTERNATIONAL JOURNAL OF COMPUTER VISION
LA English
DT Article
ID CLASSIFICATION
AB This paper discusses the problem of recognizing interaction-level human activities from a first-person viewpoint. The goal is to enable an observer (e.g., a robot or a wearable camera) to understand 'what activity others are performing to it' from continuous video inputs. These include friendly interactions such as 'a person hugging the observer' as well as hostile interactions like 'punching the observer' or 'throwing objects at the observer', whose videos involve a large amount of camera ego-motion caused by physical interactions. The paper investigates multi-channel kernels to integrate global and local motion information, and presents a new activity learning/recognition methodology that explicitly considers temporal structures displayed in first-person activity videos. Furthermore, we present a novel algorithm for early recognition (i.e., prediction) of activities from first-person videos, which allows us to infer ongoing activities at their early stage. In our experiments, we not only show classification results with segmented videos, but also confirm that our new approach is able to detect activities from continuous videos and perform early recognition reliably.
C1 [Ryoo, M. S.; Matthies, Larry] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
RP Ryoo, MS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
EM mryoo@jpl.nasa.gov
FU National Aeronautics and Space Administration; Army Research Laboratory
FX 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. This
research was sponsored by the Army Research Laboratory and was
accomplished under Cooperative Agreement Number W911NF-10-2-0016.
NR 33
TC 0
Z9 0
U1 7
U2 10
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0920-5691
EI 1573-1405
J9 INT J COMPUT VISION
JI Int. J. Comput. Vis.
PD SEP
PY 2016
VL 119
IS 3
SI SI
BP 307
EP 328
DI 10.1007/s11263-015-0847-4
PG 22
WC Computer Science, Artificial Intelligence
SC Computer Science
GA DS0FE
UT WOS:000380270000007
ER
PT J
AU Barre, J
Edwards, D
Worden, H
Arellano, A
Gaubert, B
Da Silva, A
Lahoz, W
Anderson, J
AF Barre, Jerome
Edwards, David
Worden, Helen
Arellano, Avelino
Gaubert, Benjamin
Da Silva, Arlindo
Lahoz, William
Anderson, Jeffrey
TI On the feasibility of monitoring carbon monoxide in the lower
troposphere from a constellation of northern hemisphere geostationary
satellites: Global scale assimilation experiments (Part II)
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Atmospheric composition; Global scale; Geostationary constellation;
Remote sensing; OSSE; Carbon monoxide; CO lifetime; Long-range transport
of pollution; Data assimilation
ID EARTH SYSTEM MODEL; CHEMISTRY; OZONE; AEROSOLS; CO; EMISSIONS; GASES;
BIAS
AB This paper describes the second phase of an Observing System Simulation Experiment (OSSE) that utilizes the synthetic measurements from a constellation of satellites measuring atmospheric composition from geostationary (GEO) Earth orbit presented in part I of the study. Our OSSE is focused on carbon monoxide observations over North America, East Asia and Europe where most of the anthropogenic sources are located. Here we assess the impact of a potential GEO constellation on constraining northern hemisphere (NH) carbon monoxide (CO) using data assimilation. We show how cloud cover affects the GEO constellation data density with the largest cloud cover (i.e., lowest data density) occurring during Asian summer. We compare the modeled state of the atmosphere (Control Run), before CO data assimilation, with the known "true" state of the atmosphere (Nature Run) and show that our setup provides realistic atmospheric CO fields and emission budgets. Overall, the Control Run underestimates CO concentrations in the northern hemisphere, especially in areas close to CO sources. Assimilation experiments show that constraining CO close to the main anthropogenic sources significantly reduces errors in NH CO compared to the Control Run. We assess the changes in error reduction when only single satellite instruments are available as compared to the full constellation. We find large differences in how measurements for each continental scale observation system affect the hemispherical improvement in long-range transport patterns, especially due to seasonal cloud cover. A GEO constellation will provide the most efficient constraint on NH CO during winter when CO lifetime is longer and increments from data assimilation associated with source regions are advected further around the globe. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Barre, Jerome; Edwards, David; Worden, Helen; Gaubert, Benjamin; Anderson, Jeffrey] NCAR, Boulder, CO USA.
[Arellano, Avelino] Univ Arizona, Tucson, AZ USA.
[Da Silva, Arlindo] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Lahoz, William] NILU, Kjeller, Norway.
RP Barre, J (reprint author), NCAR, Boulder, CO USA.
EM barre@ucar.edu
OI Arellano, Avelino/0000-0002-2615-5831
FU NASA [NNX09AH03G S02, NNX11AI10G, NNX11AG63G]; National Science
Foundation
FX This work was partly supported by NASA grants NNX09AH03G S02, NNX11AI10G
and NNX11AG63G. The National Center for Atmospheric Research is
sponsored by the National Science Foundation. The Climate Simulation
Laboratory at NCAR's Computational and Information Systems Laboratory
(CISL) provided computing resources. We would like to acknowledge
high-performance computing support from Yellowstone
(ark:/85065/d7wd3xhc) provided by NCAR's CISL. We also thank the
reviewers for their constructive comments.
NR 29
TC 0
Z9 0
U1 6
U2 16
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 SEP
PY 2016
VL 140
BP 188
EP 201
DI 10.1016/j.atmosenv.2016.06.001
PG 14
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DR7MG
UT WOS:000380083200018
ER
PT J
AU Hamill, P
Giordano, M
Ward, C
Giles, D
Holben, B
AF Hamill, Patrick
Giordano, Marco
Ward, Carolyne
Giles, David
Holben, Brent
TI An AERONET-based aerosol classification using the Mahalanobis distance
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Atmospheric aerosols; Aerosol typing; AERONET; Mahalanobis distance;
Seasonal aerosol variation; High AOD events
ID OPTICAL-PROPERTIES; ABSORPTION; MODELS; TRANSPORT; POLLUTION; MIXTURES;
NETWORK; CHINA; DUST; SIZE
AB We present an aerosol classification based on AERONET aerosol data from 1993 to 2012. We used the AERONET Level 2.0 almucantar aerosol retrieval products to define several reference aerosol clusters which are characteristic of the following general aerosol types: Urban-Industrial, Biomass Burning, Mixed Aerosol, Dust, and Maritime. The classification of a particular aerosol observation as one of these aerosol types is determined by its five-dimensional Mahalanobis distance to each reference cluster. We have calculated the fractional aerosol type distribution at 190 AERONET sites, as well as the monthly variation in aerosol type at those locations. The results are presented on a global map and individually in the supplementary material. Our aerosol typing is based on recognizing that different geographic regions exhibit characteristic aerosol types. To generate reference clusters we only keep data points that lie within a Mahalanobis distance of 2 from the centroid. Our aerosol characterization is based on the AERONET retrieved quantities, therefore it does not include low optical depth values. The analysis is based on "point sources" (the AERONET sites) rather than globally distributed values. The classifications obtained will be useful in interpreting aerosol retrievals from satellite borne instruments. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Hamill, Patrick] San Jose State Univ, San Jose, CA 95192 USA.
[Hamill, Patrick] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Giordano, Marco] Univ Nevada, Reno, NV 89557 USA.
[Giordano, Marco] Desert Res Inst, Reno, NV USA.
[Ward, Carolyne] Calif State Univ Long Beach, Long Beach, CA 90840 USA.
[Giles, David; Holben, Brent] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Hamill, P (reprint author), San Jose State Univ, San Jose, CA 95192 USA.; Hamill, P (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM patrick.hamill@sjsu.edu
NR 60
TC 0
Z9 0
U1 8
U2 14
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 SEP
PY 2016
VL 140
BP 213
EP 233
DI 10.1016/j.atmosenv.2016.06.002
PG 21
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DR7MG
UT WOS:000380083200020
ER
PT J
AU Creamean, JM
White, AB
Minnis, P
Palikonda, R
Spangenberg, DA
Prather, KA
AF Creamean, Jessie M.
White, Allen B.
Minnis, Patrick
Palikonda, Rabindra
Spangenberg, Douglas A.
Prather, Kimberly A.
TI The relationships between insoluble precipitation residues, clouds, and
precipitation over California's southern Sierra Nevada during winter
storms
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Aerosol-cloud-precipitation interactions; Ice nucleation; Cloud
glaciation; Sierra nevada
ID SEEDER-FEEDER MECHANISM; MINERAL DUST PARTICLES; MIXED-PHASE CLOUDS;
ICE-NUCLEATION; NORTHERN CALIFORNIA; ATMOSPHERIC RIVERS; OROGRAPHIC
PRECIPITATION; AQUEOUS SAMPLES; ASIAN AEROSOLS; BARRIER JETS
AB Ice formation in orographic mixed -phase clouds can enhance precipitation and depends on the type of aerosols that serve as ice nucleating particles (INPs). The resulting precipitation from these clouds is a viable source of water, especially for regions such as the California Sierra Nevada. Thus, a better understanding of the sources of INPs that impact orographic clouds is important for assessing water availability in California. This study presents a multi -site, multi -year analysis of single -particle insoluble residues in precipitation samples that likely influenced cloud ice and precipitation formation above Yosemite National Park. Dust and biological particles represented the dominant fraction of the residues (64% on average). Cloud glaciation, determined using satellite observations, not only depended on high cloud tops (>5.9 km) and low temperatures (<-23 degrees C), but also on the presence of what were likely dust and biological INPs. The greatest prevalence of ice -phase clouds occurred in conjunction with biologically -rich residues and mineral dust rich in calcium, followed by iron and aluminosilicates. Dust and biological particles are known to be efficient INPs, thus these residues likely influenced ice formation in clouds above the sites and subsequent precipitation quantities reaching the surface during events with similar meteorology. The goal of this study is to use precipitation chemistry information to gain a better understanding of the potential sources of INPs in the south-central Sierra Nevada, where cloud -aerosol precipitation interactions are poorly understood and where mixed -phase orographic clouds represent a key element in the generation of precipitation and thus the water supply in California. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Creamean, Jessie M.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Creamean, Jessie M.; White, Allen B.] NOAA, Earth Syst Res Lab, Div Phys Sci, Boulder, CO USA.
[Minnis, Patrick] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Palikonda, Rabindra; Spangenberg, Douglas A.] Sci Syst & Applicat Inc, Hampton, VA USA.
[Prather, Kimberly A.] Univ Calif San Diego, Dept Chem & Biochem, La Jolla, CA 92093 USA.
[Prather, Kimberly A.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
RP Creamean, JM (reprint author), NOAA, Earth Syst Res Lab, 325 Broadway,R-PSD2, Boulder, CO 80305 USA.
EM jessie.creamean@noaa.gov
RI Prather, Kimberly/A-3892-2008;
OI Prather, Kimberly/0000-0003-3048-9890; Creamean,
Jessie/0000-0003-3819-5600
FU National Research Council Research Associate Program
[EA133F-10-CN-0187]; NASA Modeling, Analysis, and Prediction Program;
DOE ARM Program
FX The authors would like to acknowledge the staff at the National Park
Service at Yosemite National Park for sample collection, including Katy
Warner, who organized the collection protocols, Rebecca Rising, and Rob
and Laura Pilewski. Ryan Spackman (NOAH/Science and Technology
Corporation) and Daniel Murphy (NOAH) provided insightful feedback. We
would also like to acknowledge the California Nevada River Forecast
Center (CNRFC) and DWR for providing the HADS data and CASTNET for
providing the meteorological measurements at YOS. The GPS WCR site data
was courtesy of the Plate Boundary Observatory (PBO) network operated by
UNAVCO. Thanks to Chris Yost for providing the satellite validation
results. Jessie Creamean was partially supported by the National
Research Council Research Associate Program (contract number
EA133F-10-CN-0187). Patrick Minnis, Rabindra Palikonda, and Doug
Spangenberg were supported by the NASA Modeling, Analysis, and
Prediction Program and DOE ARM Program. Data presented in the manuscript
tables and figures are available by email request to the corresponding
author.
NR 91
TC 1
Z9 1
U1 14
U2 25
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 SEP
PY 2016
VL 140
BP 298
EP 310
DI 10.1016/j.atmosenv.2016.06.016
PG 13
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DR7MG
UT WOS:000380083200026
ER
PT J
AU Nyhan, M
Sobolevsky, S
Kang, CG
Robinson, P
Corti, A
Szell, M
Streets, D
Lu, ZF
Britter, R
Barrett, SRH
Ratti, C
AF Nyhan, Marguerite
Sobolevsky, Stanislav
Kang, Chaogui
Robinson, Prudence
Corti, Andrea
Szell, Michael
Streets, David
Lu, Zifeng
Britter, Rex
Barrett, Steven R. H.
Ratti, Carlo
TI Predicting vehicular emissions in high spatial resolution using
pervasively measured transportation data and microscopic emission's
model
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Air quality; Transportation; Emissions; Microscopic emissions model;
Microscopic vehicle movement
ID AIR-POLLUTION; LOS-ANGELES; VEHICLE; MORTALITY; CITIES; VARIABILITY;
REDUCTION; EVOLUTION; NETWORKS; QUALITY
AB Air pollution related to traffic emissions pose an especially significant problem in cities; this is due to its adverse impact on human health and well-being. Previous studies which have aimed to quantify emissions from the transportation sector have been limited by either simulated or coarsely resolved traffic volume data. Emissions inventories form the basis of urban pollution models, therefore in this study, Global Positioning System (GPS) trajectory data from a taxi fleet of over 15,000 vehicles were analyzed with the aim of predicting air pollution emissions for Singapore. This novel approach enabled the quantification of instantaneous drive cycle parameters in high spatio-temporal resolution, which provided the basis for a microscopic emissions model. Carbon dioxide (CO2), nitrogen oxides (NOx), volatile organic compounds (VOCs) and particulate matter (PM) emissions were thus estimated. Highly localized areas of elevated emissions levels were identified, with a spatio-temporal precision not possible with previously used methods for estimating emissions. Relatively higher emissions areas were mainly concentrated in a few districts that were the Singapore Downtown Core area, to the north of the central urban region and to the east of it. Daily emissions quantified for the total motor vehicle population of Singapore were found to be comparable to another emissions dataset Results demonstrated that high resolution spatio-temporal vehicle traces detected using GPS in large taxi fleets could be used to infer highly localized areas of elevated acceleration and air pollution emissions in cities, and may become a complement to traditional emission estimates, especially in emerging cities and countries where reliable fine-grained urban air quality data is not easily available. This is the first study of its kind to investigate measured microscopic vehicle movement in tandem with microscopic emissions modeling for a substantial study domain. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Nyhan, Marguerite; Robinson, Prudence; Britter, Rex; Ratti, Carlo] MIT, SENSEable City Lab, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
[Sobolevsky, Stanislav] NYU, Ctr Urban Sci & Progress, New York, NY USA.
[Kang, Chaogui] Wuhan Univ, Wuhan, Hubei, Peoples R China.
[Corti, Andrea] Politecn Milan, 32 Piazza Leonardo da Vinci, Milan, Italy.
[Szell, Michael] Northeastern Univ, Dept Phys, Ctr Complex Network Res, Boston, MA 02115 USA.
[Streets, David; Lu, Zifeng] NASA, Argonne Natl Lab, Lemont, IL USA.
[Barrett, Steven R. H.] MIT, Dept Aeronaut & Astronaut, Cambridge, MA 02139 USA.
RP Nyhan, M (reprint author), MIT, SENSEable City Lab, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM mnyhan@mit.edu
OI Kang, Chaogui/0000-0002-0122-9419
FU MIT SENSEable City Lab Consortium; Singapore-MIT Alliance for Research &
Technology program
FX All the authors wish to thank the MIT SENSEable City Lab Consortium and
the Singapore-MIT Alliance for Research & Technology program for
supporting the research. M. Nyhan would like to thank Fulbright and the
Irish Environmental Protection Agency. The authors would also like to
acknowledge Dr. Luc Int. Panis for providing advice on some modeling
aspects of the study.
NR 68
TC 1
Z9 1
U1 30
U2 43
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 SEP
PY 2016
VL 140
BP 352
EP 363
DI 10.1016/j.atmosenv.2016.06.018
PG 12
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA DR7MG
UT WOS:000380083200031
ER
PT J
AU Villac, BF
Anderson, RL
Pini, AJ
AF Villac, Benjamin F.
Anderson, Rodney L.
Pini, Alex J.
TI Computer Aided Ballistic Orbit Classification Around Small Bodies
SO JOURNAL OF THE ASTRONAUTICAL SCIENCES
LA English
DT Article
DE Trajectory design; Periodic orbits; Clustering; Data mining; Asteroid
missions
ID INVARIANT-MANIFOLDS; TRAJECTORY DESIGN; RESONANCE; TRANSFERS; VESTA
AB Orbital dynamics around small bodies are as varied as the shapes and dynamical states of these bodies. While various classes of orbits have been analyzed in detail, the global overview of relevant ballistic orbits at particular bodies is not easily computed or organized. Yet, correctly categorizing these orbits will ease their future use in the overall trajectory design process. This paper overviews methods that have been used to organize orbits, focusing on periodic orbits in particular, and introduces new methods based on clustering approaches.
C1 [Villac, Benjamin F.] Ai Solut Inc, 4500 Forbes Blvd,Suite 300, Lanham, MD 20706 USA.
[Anderson, Rodney L.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 301-121, Pasadena, CA 91109 USA.
[Pini, Alex J.] NASA, GSFC, Ai Solut Inc, B28 N278, Greenbelt, MD 20771 USA.
RP Villac, BF (reprint author), Ai Solut Inc, 4500 Forbes Blvd,Suite 300, Lanham, MD 20706 USA.
EM benjamin.villac@ai-solutions.com
FU AMMOS technology development task
FX This research has been sponsored by the AMMOS technology development
task. A portion of the research presented in this paper has been carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration.
NR 60
TC 0
Z9 0
U1 23
U2 23
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 0021-9142
EI 2195-0571
J9 J ASTRONAUT SCI
JI J. Astronaut. Sci.
PD SEP
PY 2016
VL 63
IS 3
BP 175
EP 205
DI 10.1007/s40295-016-0089-x
PG 31
WC Engineering, Aerospace
SC Engineering
GA DR7SW
UT WOS:000380101000001
ER
PT J
AU Stickle, WB
Lindeberg, M
Rice, SD
Munley, K
Reed, V
AF Stickle, William B.
Lindeberg, Mandy
Rice, Stanley D.
Munley, Kathleen
Reed, Victoria
TI Seasonal changes in the thermal regime and gastropod tolerance to
temperature and desiccation stress in the rocky intertidal zone in
Southeast Alaska
SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY
LA English
DT Article
DE Thermal regime; Temperature probes; Vertical gastropod zonation;
Desiccation tolerance; Temperature tolerance
ID HEAT-SHOCK RESPONSE; CLIMATE-CHANGE; PHYSIOLOGICAL ECOLOGY; GENUS
PETROLISTHES; VERTICAL ZONATION; PORCELAIN CRABS; LIMITS; ACCLIMATION;
PATTERNS; TEGULA
AB Low tide emersion of intertidal fauna in the inside passage from Puget Sound, WA to Skagway, AK produces more extreme emersion temperatures than on the outer continental coastline because the timing of low tides increases the potential for summer high temperatures and winter low temperatures. This study documents seasonal changes in water/aerial temperatures at different tidal heights in 2007-2008 and the summer of 2015 and reports the high emersion temperature (5 h) and desiccation tolerance of three species of rocky shore gastropods. Vertical transects of probes were deployed at Bridget Cove at +5.0 m (above the tidal range), +3.5, +2.5 m, +1.5 m and 0 m. Two additional probes were partially buried at +1.5 m; burial ameliorated freezing temperatures. Duration of emersion increased with intertidal height and was of longer duration at +3.5 m during Neap tides and at +1.5 and 0 m during Spring tides. Monthly measures of temperature were: average temperature, monthly maximum, average daily monthly maximum, average daily monthly minimum, and monthly minimum. Monthly maximum air temperature increased with tidal height. Winter average daily monthly minimum fell below 0 degrees C at the +3.5, +2.5, and +1.5 m tidal heights for the aerially exposed probes. The number of days when emersion temperature fell below 0 degrees C increased with intertidal height as did the number of hours per day. High temperature emersion tolerance of Nucella lamellosa, Nucella lima and Littorina sitkana varied directly with their intertidal range but their desiccation tolerance did not suggesting that desiccation is not an abiotic stressor in this temperate rain forest intertidal zone. The LT50 temperature (5 h) was considerably above recorded monthly maximum temperatures in the vertical range of N. lamellosa and L. sitkana but the LT50 of N. lima was very near the maximum monthly temperature at +2.5 m. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Stickle, William B.; Munley, Kathleen] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA.
[Lindeberg, Mandy; Rice, Stanley D.] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Lab, Juneau, AK 99801 USA.
[Reed, Victoria] Louisiana State Univ, Div Comp Sci & Engn, Baton Rouge, LA 70803 USA.
RP Stickle, WB (reprint author), Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA.
EM zostic@lsu.edu
NR 39
TC 1
Z9 1
U1 30
U2 58
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 SEP
PY 2016
VL 482
BP 56
EP 63
DI 10.1016/j.jembe.2016.04.011
PG 8
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA DQ7EW
UT WOS:000379370700006
ER
PT J
AU Babcock, C
Finley, AO
Cook, BD
Weiskittel, A
Woodall, CW
AF Babcock, Chad
Finley, Andrew O.
Cook, Bruce D.
Weiskittel, Aaron
Woodall, Christopher W.
TI Modeling forest biomass and growth: Coupling long-term inventory and
LiDAR data
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE LiDAR; Forest biomass; Biomass growth; Temporal misalignment; Long-term
forest inventory; Bayesian hierarchical models; Markov Chain Monte
Carlo; Gaussian process; Geospatial
ID ABOVEGROUND BIOMASS; CANOPY HEIGHT; CARBON; AIRBORNE; REGRESSION;
VARIABLES; COMPLEX; MISSION; PLOTS
AB Combining spatially-explicit long-term forest inventory and remotely sensed information from Light Detection and Ranging (LiDAR) datasets through statistical models can be a powerful tool for predicting and mapping above-ground biomass (AGB) at a range of geographic scales. We present and examine a novel modeling approach to improve prediction of AGB and estimate AGB growth using LiDAR data. The proposed model accommodates temporal misalignment between field measurements and remotely sensed data a problem pervasive in such settings by including multiple time-indexed measurements at plot locations to estimate AGB growth. We pursue a Bayesian modeling framework that allows for appropriately complex parameter associations and uncertainty propagation through to prediction. Specifically, we identify a space-varying coefficients model to predict and map AGB and its associated growth simultaneously. The proposed model is assessed using LiDAR data acquired from NASA Goddard's LiDAR, Hyper-spectral & Thermal imager and field inventory data from the Penobscot Experimental Forest in Bradley, Maine. The proposed model outperformed the time-invariant counterpart models in predictive performance as indicated by a substantial reduction in root mean squared error. The proposed model adequately accounts for temporal misalignment through the estimation of forest AGB growth and accommodates residual spatial dependence. Results from this analysis suggest that future AGB models informed using remotely sensed data, such as LiDAR, may be improved by adapting traditional modeling frameworks to account for temporal misalignment and spatial dependence using random effects. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Babcock, Chad] Univ Washington, Sch Environm & Forest Sci, Seattle, WA 98195 USA.
[Finley, Andrew O.] Michigan State Univ, Dept Forestry, E Lansing, MI 48824 USA.
[Cook, Bruce D.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Code 618, Greenbelt, MD 20742 USA.
[Weiskittel, Aaron] Univ Maine, Sch Forest Resources, Orono, ME 04469 USA.
[Woodall, Christopher W.] US Forest Serv, USDA, No Res Stn, Forest Inventory & Anal Program, 1992 Folwell Ave, St Paul, MN 55114 USA.
RP Babcock, C (reprint author), Univ Washington, Sch Environm & Forest Sci, Seattle, WA 98195 USA.
OI Babcock, Chad/0000-0001-9597-4462
FU U.S. Forest Service [USFS 15-JV-11242307-116]; National Science
Foundation (NSF) [DMS-1513481, EF-1137309, EF-1241874, EF-1253225]; NASA
Carbon Monitoring System grants
FX Data for this study were provided by a unit of the Northern Research
Station, U.S. Forest Service, located at the Penobscot Experimental
Forest in Maine. Significant funding for collection of these data was
provided by the U.S. Forest Service (USFS 15-JV-11242307-116). Andrew
Finley was supported by National Science Foundation (NSF) DMS-1513481,
EF-1137309, EF-1241874, and EF-1253225, as well as NASA Carbon
Monitoring System grants.
NR 52
TC 0
Z9 0
U1 29
U2 84
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 SEP 1
PY 2016
VL 182
BP 1
EP 12
DI 10.1016/j.rse.2016.04.014
PG 12
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA DQ3HP
UT WOS:000379093700001
ER
PT J
AU Huesca, M
Garcia, M
Roth, KL
Casas, A
Ustin, SL
AF Huesca, Margarita
Garcia, Mariano
Roth, Keely L.
Casas, Angeles
Ustin, Susan L.
TI Canopy structural attributes derived from AVIRIS imaging spectroscopy
data in a mixed broadleaf/conifer forest
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Canopy structure; AVIRIS; LiDAR; Random forest; Structural types
ID SPECTRAL MIXTURE ANALYSIS; REMOTE-SENSING DATA; VEGETATION INDEXES;
HYPERSPECTRAL DATA; AIRBORNE LIDAR; WATER-CONTENT; NITROGEN-CONTENT;
ABOVEGROUND BIOMASS; SPATIAL-PATTERNS; LANDSAT IMAGERY
AB There is a well-established need within the remote sensing community for improved estimation and understanding of canopy structure and its influence on the retrieval of leaf biochemical properties. The main goal of this research was to assess the potential of optical spectral information from NASA's Airborne Visible/Infrared Imaging Spectrometer (AVIRIS) to discriminate different canopy structural types. In the first phase, we assessed the relationships between optical metrics and canopy structural parameters obtained from LiDAR in terms of different canopy structural attributes (biomass (i.e., area under Vegetation Vertical Profile, VVPint), canopy height and vegetation complexity). Secondly, we identified and classified different "canopy structural types" by integrating several structural traits using Random Forests (RF). The study area is a heterogeneous forest in Sierra National Forest in California (USA). AVIRIS optical properties were analyzed by means of several sets of variables, including single narrow band reflectance and 1st derivative, sub-pixel cover fractions, narrow-band indices, spectral absorption features, optimized normalized difference indices and Principal Component Analysis (PCA) components. Our results demonstrate that optical data contain structural information that can be retrieved. The first principal component, used as a proxy for albedo, was the most strongly correlated optical metric with vegetation complexity, and it also correlated well with biomass (VVPint) and height. In conifer forests, the shade fraction was especially correlated to vegetation complexity, while water-sensitive optical metrics had high correlations with biomass (VVPint). Single spectral band analysis results showed that correlations differ in magnitude and in direction, across the spectrum and by vegetation type and structural variable. This research illustrates the potential of AVIRIS to analyze canopy structure and to distinguish several structural types in a heterogeneous forest. Furthermore, RF using optical metrics derived from AVIRIS proved to be a powerful technique to generate maps of structural attributes. The results emphasize the importance of using the whole optical spectrum, since all spectral regions contributed to canopy structure assessment (C) 2016 Elsevier Inc. All rights reserved.
C1 [Huesca, Margarita; Roth, Keely L.; Casas, Angeles; Ustin, Susan L.] Univ Calif Davis, CSTARS, Land Air & Water Resources Dept, Davis, CA 95616 USA.
[Garcia, Mariano] Univ Leicester, Ctr Landscape & Climate Res, Leicester LE1 7RH, Leics, England.
[Garcia, Mariano] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Huesca, M (reprint author), Univ Calif Davis, CSTARS, Davis, CA 95616 USA.
EM mhuescamartinez@ucdavis.edu
FU HyspIRI Planning Mission (NASA Grant) [NNX12AP87G]; Marie Curie IOF
(ForeStMap - 3D Forest Structure Monitoring and Mapping) [629376]
FX This research was conducted within the framework of the HyspIRI Planning
Mission (NASA Grant # NNX12AP87G). Mariano Garcia is supported by the
Marie Curie IOF (ForeStMap - 3D Forest Structure Monitoring and Mapping,
Project Reference: 629376). The contents on this paper reflect only the
authors' views and not the views of the European Commission. I would
like to thank NEON for providing the LiDAR data and the NASA JPL AVIRIS
team for collecting and preprocessing the hyperspectral data. I would
also thank the anonymous reviewers for their help in improving the
manuscript.
NR 129
TC 3
Z9 3
U1 21
U2 40
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 SEP 1
PY 2016
VL 182
BP 208
EP 226
DI 10.1016/j.rse.2016.04.020
PG 19
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA DQ3HP
UT WOS:000379093700016
ER
PT J
AU Malakar, NK
Hulley, GC
AF Malakar, Nabin K.
Hulley, Glynn C.
TI A water vapor scaling model for improved land surface temperature and
emissivity separation of MODIS thermal infrared data
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE MODIS; Land surface temperature; Atmospheric correction; Thermal
infrared; Emissivity; Validation; Infrared image sensors; Remote sensing
ID ATMOSPHERIC CORRECTION; SOIL RESPIRATION; ENERGY-BALANCE; AVHRR DATA;
ASTER; ALGORITHM; PRODUCTS; VALIDATION; RADIOMETER; SATELLITE
AB We present an improved water vapor scaling (WVS) model for atmospherically correcting MODIS thermal infrared (TIR) bands in the temperature emissivity separation (TES) algorithm. TES is used to retrieve the land surface temperature and emissivity (LST&E) from MODIS TIR bands 29, 31, and 32. The WVS model improves the accuracy of the atmospheric correction parameters in TES on a band-by-band and pixel-by-pixel basis. We used global atmospheric radiosondes profiles to generate view angle and day-night-dependent WVS coefficients that are valid for all MODIS scan angles up to 65. We demonstrate the effects of applying the improved WVS model on the retrieval accuracy of MODIS-TES (MODTES) LST&E using a case study for a granule over the southwest USA during very warm and moist monsoonal atmospheric conditions. Furthermore, a comprehensive validation of the MODTES LST&E retrieval was performed over two sites at the quartz-rich Algodones Dunes in California and a grassland site in Texas, USA using three full years of MODIS Aqua data. Results from the case study showed that absolute errors in the emissivity retrieval for the three MODIS TIR bands were reduced on average from 1.4% to 0.4% when applying the WVS method. A Radiance-based method was used to validate the MODTES LST retrievals for and the results showed that application of the WVS method with the MODTES algorithm led to significant reduction in both bias and root mean square error (RMSE) of the LST retrievals at both sites. When the WVS model was applied, LST RMSE's were reduced on average from 1.3 K to 1.0 K at the Algodones Dunes site, and from 1.2 K to 0.7 K at the Texas Grassland site. This study demonstrated that the WVS atmospheric correction model is critical for retrieving MODTES LST with <1 K accuracy and emissivity with <1% consistently for a wide range of challenging atmospheric conditions and land surface types. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Malakar, Nabin K.; Hulley, Glynn C.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Malakar, NK (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Nabin.K.Malakar@jpl.nasa.gov
OI Malakar, Nabin/0000-0002-4816-6304
FU NASA ROSES grant [NRA NNH13ZDA001N]
FX 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. This
study is supported by the NASA ROSES 2013 grant (NRA NNH13ZDA001N).
NR 53
TC 1
Z9 1
U1 16
U2 29
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 SEP 1
PY 2016
VL 182
BP 252
EP 264
DI 10.1016/j.rse.2016.04.023
PG 13
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA DQ3HP
UT WOS:000379093700018
ER
PT J
AU Cho, Y
Sugita, S
Miura, YN
Okazaki, R
Iwata, N
Morota, T
Kameda, S
AF Cho, Yuichiro
Sugita, Seiji
Miura, Yayoi N.
Okazaki, Ryuji
Iwata, Naoyoshi
Morota, Tomokatsu
Kameda, Shingo
TI An in-situ K-Ar isochron dating method for planetary landers using a
spot-by-spot laser-ablation technique
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE In-situ geochronology; K-Ar dating; Planetary missions; Laser-induced
breakdown spectroscopy; Noble gas mass spectrometry
ID INNER SOLAR-SYSTEM; LUNAR CATACLYSM; GALE CRATER; MARS; CHRONOLOGY;
ORIGIN; AGES; MASS; GEOCHRONOLOGY; STRATIGRAPHY
AB Age is essential information for interpreting the geologic record on planetary surfaces. Although crater counting has been widely used to estimate the planetary surface ages, crater chronology in the inner solar system is largely built on radiometric age data from limited sites on the Moon. This has resulted in major uncertainty in planetary chronology. Because opportunities for sample-return missions are limited, in-situ geochronology measurements from one-way lander/rover missions are extremely valuable. Here we developed an in-situ isochron-based dating method using the K-Ar system, with K and Ar in a single rock sample extracted locally by laser ablation and measured using laser-induced breakdown spectroscopy (LIBS) and a quadrupole mass spectrometer (QMS), respectively. We built an experimental system combining flight equivalent instruments and measured K-Ar ages for mineral samples with known ages (similar to 1.8 Ga) and K contents (1-8 wt%); we achieved precision of 20% except for a mineral with low mechanical strength. Furthermore, validation measurements with two natural rocks (gneiss slabs) obtained K-Ar isochron ages and initial Ar-40 consistent with known values for both cases. This result supports that our LIBS-MS approach can derive both isochron ages and contributions of non-in situ radiogenic Ar-40 from natural rocks. Error assessments suggest that the absolute ages of key geologic events including the Noachian/Hesperian- and the Hesperian/Amazonian-transition can be dated with 10-20% errors for a rock containing similar to 1 wt% K2O, greatly reducing the uncertainty of current crater chronology models on Mars. (C) 2016 Elsevier Ltd. All rights reserved.
C1 [Cho, Yuichiro; Sugita, Seiji] Univ Tokyo, Dept Earth & Planetary Sci, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan.
[Cho, Yuichiro; Kameda, Shingo] Rikkyo Univ, Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan.
[Miura, Yayoi N.] Univ Tokyo, Earthquake Res Inst, Bunkyo Ku, 1-1-1 Yayoi, Tokyo 1130032, Japan.
[Okazaki, Ryuji] Kyushu Univ, Dept Earth & Planetary Sci, Nishi Ku, 744 Motooka, Fukuoka 8190395, Japan.
[Iwata, Naoyoshi] Yamagata Univ, Dept Earth & Environm Sci, 1-4-12 Kojirakawa, Yamagata 9908560, Japan.
[Morota, Tomokatsu] Nagoya Univ, Dept Earth & Planetary Sci, Chikusa Ku, Nagoya, Aichi 4648601, Japan.
[Cho, Yuichiro] NASA, Marshall Space Flight Ctr, 320 Sparkman Dr, Huntsville, AL 35805 USA.
RP Cho, Y (reprint author), Rikkyo Univ, Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan.
EM cho@rikkyo.ac.jp
RI Iwata, Naoyoshi/B-7554-2008
OI Iwata, Naoyoshi/0000-0002-0017-9130
FU Institute of Space and Aeronautical Science (ISAS)/Japan Aerospace
Exploration Agency (JAXA); Japan Society for the Promotion of Science
(JSPS) [26247092]; JSPS [15K17796]
FX The authors are grateful to two anonymous reviewers whose careful
reading of this paper led to a number of significant improvements. This
study was supported by funds from the Institute of Space and
Aeronautical Science (ISAS)/Japan Aerospace Exploration Agency (JAXA)
and by Japan Society for the Promotion of Science (JSPS) Grant-in-Aid in
Scientific Research Grant Number 26247092. Y. Cho was supported by JSPS
Grant-in-Aid for Young Scientists (B.) Grant Number 15K17796. The
authors thank Keisuke Nagao of the University of Tokyo for providing the
mineral samples. We would like to thank Takahiko Yagi, Ehime University,
and Hirotada Goto, the University of Tokyo for assistance in making the
pellet samples with a cubic press at the Institute of Solid State
Physics, the University of Tokyo. The authors thank Naoto Ishikawa of
Kyoto University and the 41st and 42nd Japanese Antarctic Research
Expedition Program for acquiring the gneiss samples. Asako Takamasa in
Japan Agency for Marine-Earth Science and Technology (JAMSTEC) is
acknowledged for separating biotites from the gneiss rocks. We are
thankful to Kenji Mibe at Earthquake Research Institute, the University
of Tokyo, for preparing a basaltic glass sample used for Ar
measurements. All data and programs used for producing the results in
this paper are available from the lead author on request
(cho@rikkyo.ac.jp).
NR 59
TC 1
Z9 1
U1 10
U2 21
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD SEP 1
PY 2016
VL 128
BP 14
EP 29
DI 10.1016/j.pss.2016.05.004
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DQ1LA
UT WOS:000378961300002
ER
PT J
AU Guo, JP
Liu, H
Wang, F
Huang, JF
Xia, F
Lou, MY
Wu, YR
Jiang, JH
Xie, T
Zhaxi, YZ
Yung, YL
AF Guo, Jianping
Liu, Huan
Wang, Fu
Huang, Jingfeng
Xia, Feng
Lou, Mengyun
Wu, Yerong
Jiang, Jonathan H.
Xie, Tao
Zhaxi, Yangzong
Yung, Yuk L.
TI Three-dimensional structure of aerosol in China: A perspective from
multi-satellite observations
SO ATMOSPHERIC RESEARCH
LA English
DT Article
DE CALIOP; Dust; Smoke; Frequency of occurrence; China
ID AIR-POLLUTION; INDUCED VARIABILITY; EASTERN CHINA; NORTH-AMERICA; WARM
CLOUDS; TRANSPORT; PRECIPITATION; DUST; ATMOSPHERE; ATLANTIC
AB Using eight years (2006-2014) of passive (MODIS/Aqua and OMI/Aura) and active (CALIOP/CALIPSO) satellite measurements of aerosols, we yield a three-dimensional (3D) distribution of the frequency of occurrence (FoO) of aerosols over China. As an indicator of the vertical heterogeneity of aerosol layers detected by CALIOP, two types of Most Probable Height (MPH), including MPH_FoO and MPH_AOD, are deduced. The FoO of "Total Aerosol" reveals significant geographical dependence. Eastern China showed much stronger aerosol FoD than northwestern China. The FoO vertical structures of aerosol layer are strongly dependent on altitudes. Among the eight typical ROls analyzed, aerosol layers over the Gobi Desert have the largest occurrence probability located at an altitude as high as 2.83 km, as compared to 126 km over Beijing-Tianjin-Hebei. The diurnal variation (nighttime-daytime) in MPH_AOD varies from an altitude as low as 0.07 km over the Sichuan basin to 0.27 km over the Gobi Desert, whereas the magnitude of the diurnal variation in terms of MPH_AOD is six times as large as the MPH_FoO, mostly attributable to the day/night lidar SNR difference. Also, the 3D distribution of dust and smoke aerosols was presented. The multi-sensor synergized 3D observations of dust aerosols, frequently observed in the zonal belt of 38 degrees N-45 degrees N, is markedly different from that of smoke aerosols that are predominantly located in the eastern and southern parts. The 3D FoO distribution of dust indicates a west-to-east passageway of dust originating from the westernmost Taklimakan Desert all the way to North China Plain (NCP). The findings from the multi-sensor synergetic observations greatly improved our understanding on the long-range aerosol dispersion, transport and passageway over China. (C) 2016 Elsevier B.V. All rights reserved.
C1 [Guo, Jianping; Liu, Huan; Xia, Feng; Lou, Mengyun] Chinese Acad Meteorol Sci, State Key Lab Severe Weather, Beijing 100081, Peoples R China.
[Wang, Fu] China Meteorol Adm, Natl Satellite Meteorol Ctr, Beijing 100081, Peoples R China.
[Huang, Jingfeng] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
[Wu, Yerong] Delft Univ Technol, Geosci & Remote Sensing Fac Civil Engn & Geosci, NL-2628 CN Delft, Netherlands.
[Jiang, Jonathan H.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Xie, Tao] Guangzhou MapUniverse Technol Co Ltd, Guangzhou 510070, Guangdong, Peoples R China.
[Guo, Jianping; Zhaxi, Yangzong] Tibetan Inst Atmospher Environm & Sci, Lhasa 850000, Peoples R China.
[Yung, Yuk L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Guo, JP (reprint author), Chinese Acad Meteorol Sci, 46 Zhong Guan Cun South Ave, Beijing 100081, Peoples R China.
EM jpguo@camscma.cn
RI Huang, Jingfeng/D-7336-2012
OI Huang, Jingfeng/0000-0002-8779-2922
FU Ministry of Science and Technology of the People's Republic of China
[2014BAC16B01]; Natural Science Foundation of China [91544217, 41471301,
41171294]; Chinese Academy of Meteorological Sciences [2014R18];
Guangdong Provincial Science and Technology Plan Projects
[2014A010101151]; NASA; California Institute of Technology
FX This work was carried out under the auspices of the Ministry of Science
and Technology of the People's Republic of China (Grant no.
2014BAC16B01), the Natural Science Foundation of China (Grant nos.
91544217, 41471301 and 41171294), the Chinese Academy of Meteorological
Sciences (Grant no. 2014R18), and Guangdong Provincial Science and
Technology Plan Projects (Grant no. 2014A010101151). The MODIS AOD data
used in this study were also, acquired as part of the NASA's Earth-Sun
System Division and archived and distributed by the Goddard Earth
Sciences (GES) Data and Information Services Center (DISC) Distributed
Active Archive Center (DAAC). Authors JHJ and YY thank the support by
the NASA sponsored Jet Propulsion Laboratory and by the California
Institute of Technology.
NR 52
TC 3
Z9 3
U1 13
U2 26
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 SEP 1
PY 2016
VL 178
BP 580
EP 589
DI 10.1016/j.atmosres.2016.05.010
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DP2YY
UT WOS:000378360700049
ER
PT J
AU Langseth, BJ
Schueller, AM
Shertzer, KW
Craig, JK
Smith, JW
AF Langseth, Brian J.
Schueller, Amy M.
Shertzer, Kyle W.
Craig, J. Kevin
Smith, Joseph W.
TI Management implications of temporally and spatially varying catchability
for the Gulf of Mexico menhaden fishery
SO FISHERIES RESEARCH
LA English
DT Article
DE Catchability; Hypoxia; Spatio-temporal variation; Stock assessment; Gulf
menhaden
ID STOCK ASSESSMENT MODELS; BROWN SHRIMP; HYPOXIA; PERFORMANCE; ABUNDANCE;
YIELD; AREA
AB Catchability relates fishing effort to fishing mortality, and is an important component in fishery stock assessment models. Mis-specifying catchability can lead to inaccurate estimation of model parameters and bias in the determination of stock status. The Gulf of Mexico has one of the largest seasonal occurrences of hypoxia in the world and it overlaps in time and space with the Gulf menhaden Brevoortia patronus fishery, potentially leading to temporal and spatial patterns in stock distribution and thus catchability. These patterns are not currently modeled in the Gulf menhaden stock assessment. To better understand the implications of spatial and temporal patterns in catchability due to hypoxia, we constructed an operating model of Gulf menhaden fishery dynamics under various assumptions of spatial coverages and temporal patterns, and used the output from the operating model as input into estimation models with alternative approaches on modeling catchability. Under the most extreme assumptions about the spatial coverage and magnitude of variation in catchability, median absolute error in estimates of fishing mortality and spawning stock reference points (F-30% and S-30%) was 73% and 29%, respectively, and median absolute error in estimates of fishing mortality and spawning stock based stock status was 23% and 79%, supporting the notion that errors in catchability are important. Under more reasonable assumptions, median absolute error declined to 20% and 2.9% for F-30% and S-30%, respectively, and to 3.8% and 2.4% for fishing mortality and spawning stock-based stock status, respectively. Modeling catchability as a random walk further reduced median absolute error to 5.0% for F-30% and 1.4% for S-30%, but slightly increased median absolute error for stock status indicators to 4.0% and 3.3%. Our results show generally that the spatial coverage, temporal pattern, and estimation approach of catchability affects the influence of mis-specifying catchability; and show specifically that the Gulf menhaden stock assessment is robust to the effects of hypoxia on catchability if assuming random-walk catchability. Published by Elsevier B.V.
C1 [Langseth, Brian J.; Schueller, Amy M.; Shertzer, Kyle W.; Craig, J. Kevin; Smith, Joseph W.] NOAA, Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, 101 Pivers Isl Rd, Beaufort, NC 28516 USA.
[Langseth, Brian J.] NOAA, Natl Marine Fisheries Serv, Pacific Islands Fisheries Sci Ctr, 1845 Wasp Blvd,Bldg 176, Honolulu, HI 96818 USA.
RP Langseth, BJ (reprint author), NOAA, Natl Marine Fisheries Serv, Pacific Islands Fisheries Sci Ctr, 1845 Wasp Blvd,Bldg 176, Honolulu, HI 96818 USA.
EM brian.langseth@noaa.gov
FU Fisheries and the Environment (FATE) Program of the National Oceanic and
Atmospheric Administration (NOAA)
FX We thank A. Yau and K. Siegfried, J. Thorson, and an anonymous reviewer
for contributions to previous drafts of the manuscript. This research
was supported by a grant from the Fisheries and the Environment (FATE)
Program of the National Oceanic and Atmospheric Administration (NOAA).
The views expressed herein are those of the authors and do not
necessarily reflect the view of NOAA or any of its subagencies.
NR 42
TC 0
Z9 0
U1 21
U2 25
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0165-7836
EI 1872-6763
J9 FISH RES
JI Fish Res.
PD SEP
PY 2016
VL 181
BP 186
EP 197
DI 10.1016/j.fishres.2016.04.013
PG 12
WC Fisheries
SC Fisheries
GA DP0LS
UT WOS:000378181900019
ER
PT J
AU Pajola, M
Rossato, S
Carter, J
Baratti, E
Pozzobon, R
Erculiani, MS
Coradini, M
McBride, K
AF Pajola, Maurizio
Rossato, Sandro
Carter, John
Baratti, Emanuele
Pozzobon, Riccardo
Erculiani, Marco Sergio
Coradini, Marcello
McBride, Karen
TI Eridania Basin: An ancient paleolake floor as the next landing site for
the Mars 2020 rover
SO ICARUS
LA English
DT Article
DE Mars, surface; Geological processes; Spectroscopy; Image processing;
Exobiology
ID ORBITER LASER ALTIMETER; EMISSION SPECTROMETER EXPERIMENT; LACUSTRINE
ENVIRONMENTS; PHYSICAL-PROPERTIES; THERMAL INERTIA; MARTIAN SURFACE;
GLOBAL SURVEYOR; MAADIM-VALLIS; CRATER LAKES; ORIGIN
AB The search for traces of past Martian life is directly connected to ancient paleolakes, where ponding water or low-energy water fluxes were present for long time intervals. The Eridania paleolakes system, located along the 180 meridian, is one of the largest lacustrine environments that were once present on Mars. Morphological features suggest that it was constituted by connected depressions filled by water to maximum depths of similar to 2400 m and a volume of at least 562,000 km(3). We focused our attention on the northern side of the Eridania Basin, where high-albedo, uneven patches of material characterized by the absence of dust are present. Based on OMEGA and CRISM orbital imaging spectroscopy data, a large clay-bearing unit has been identified there. In particular, a set of aqueous minerals in present in the stratigraphy, being visible through erosional windows in the first several tens of meters of the sedimentary sequence. Below this capping unit, a thin Al-rich clay stratum attributable to Al-smectite and/or kaolins is present. This overlies a Fe-rich clay stratum, attributable to the nontronite smectite. At the base of the mineralogic sequence a stratum that could be either a zeolite or more likely a hydrated sulfate is present. In addition, small deposits of alunite (a rare phase on Mars), and jarosite are here found at several locations. Such stratigraphy is interpreted as originating from a surface weathering process similar to terrestrial abiotic pedogenesis; nonetheless, possible exobiologic processes can be also invoked to explain it. NASA's Spirit rover landed on Gusev crater in 2004, near the mouth of the Ma'adim Vallis, which connects this crater with the considered paleolakes system. The Eridania site provides the unique opportunity to complete the measurements obtained in Gusev crater, while investigating the exposed mineralogical sequence in its depositionary setting. In addition, the extremely favorable landing parameters, such as elevation, slope, roughness, rock distribution, thermal inertia and dust coverage, support this location as a possible landing site for the NASA Mars 2020 rover. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Pajola, Maurizio] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Pajola, Maurizio; Erculiani, Marco Sergio] Univ Padua, Ctr Studies & Act Space G Colombo, Via Venezia 15, I-35131 Padua, Italy.
[Rossato, Sandro; Pozzobon, Riccardo] Univ Padua, Geosci Dept, I-3513 Padua, Italy.
[Carter, John] Univ Paris 11, IAS, F-91405 Orsay, France.
[Baratti, Emanuele] Univ Bologna, Dept DICAM, Sch Civil Engn, I-40136 Bologna, Italy.
[Coradini, Marcello] European Space Agcy, F-75015 Paris, France.
[Coradini, Marcello] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[McBride, Karen] Univ Calif Los Angeles, Los Angeles, CA 90024 USA.
RP Pajola, M (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM maurizio.pajola@nasa.gov
OI Pajola, Maurizio/0000-0002-3144-1277; Coradini,
Marcello/0000-0002-1711-3197
NR 142
TC 0
Z9 0
U1 13
U2 24
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 SEP 1
PY 2016
VL 275
BP 163
EP 182
DI 10.1016/j.icarus.2016.03.029
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DO8FB
UT WOS:000378016900012
ER
PT J
AU Meriggiola, R
Iess, L
Stiles, BW
Lunine, JI
Mitri, G
AF Meriggiola, Rachele
Iess, Luciano
Stiles, Bryan. W.
Lunine, Jonathan. I.
Mitri, Giuseppe
TI The rotational dynamics of Titan from Cassini RADAR images
SO ICARUS
LA English
DT Article
DE Titan, interior; Satellites, dynamics; Geophysics
ID INTERNAL STRUCTURE; GRAVITY-FIELD; OCEAN; TOPOGRAPHY; OBLIQUITY; STATE;
SHAPE; ICE
AB Between 2004 and 2009 the RADAR instrument of the Cassini mission provided 31 SAR images of Titan. We tracked the position of 160 surface landmarks as a function of time in order to monitor the rotational dynamics of Titan. We generated and processed RADAR observables using a least squares fit to determine the updated values of the rotational parameters. We provide a new rotational model of Titan, which includes updated values for spin pole location, spin rate, precession and nutation terms. The estimated pole location is compatible with the occupancy of a Cassini state 1. We found a synchronous value of the spin rate (22.57693 deg/day), compatible at a 3-sigma level with IAU predictions. The estimated obliquity is equal to 0.31, incompatible with the assumption of a rigid body with fully-damped pole and a moment of inertia factor of 0.34, as determined by gravity measurements. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Meriggiola, Rachele; Iess, Luciano] Univ Roma La Sapienza, Dipartimento Ingn Meccan & Aerospaziale, Via Eudossiana 18, I-00184 Rome, Italy.
[Stiles, Bryan. W.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Lunine, Jonathan. I.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
[Mitri, Giuseppe] Univ Nantes, Lab Planetol & Geodynam Nantes, Nantes, France.
RP Meriggiola, R (reprint author), Univ Roma La Sapienza, Dipartimento Ingn Meccan & Aerospaziale, Via Eudossiana 18, I-00184 Rome, Italy.
EM rachele.meriggiola@uniromal.it
RI IESS, Luciano/F-4902-2011
OI IESS, Luciano/0000-0002-6230-5825
FU Cassini Project
FX We thank W. Jacobson and the Cassini Navigation Team (JPL) for the
provided support on the error source analysis. Support by the Cassini
Project is gratefully acknowledged. JIL is grateful for support from the
Cassini Project. A portion of the work 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.
NR 33
TC 3
Z9 3
U1 2
U2 2
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 SEP 1
PY 2016
VL 275
BP 183
EP 192
DI 10.1016/j.icarus.2016.01.019
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DO8FB
UT WOS:000378016900013
ER
PT J
AU Gautier, T
Schmitz-Afonso, I
Touboul, D
Szopa, C
Buch, A
Carrasco, N
AF Gautier, Thomas
Schmitz-Afonso, Isabelle
Touboul, David
Szopa, Cyril
Buch, Arnaud
Carrasco, Nathalie
TI Development of HPLC-Orbitrap method for identification of N-bearing
molecules in complex organic material relevant to planetary environments
SO ICARUS
LA English
DT Article
DE Titan, atmosphere; Atmospheres, chemistry; Organic chemistry; Prebiotic
chemistry
ID TITANS THOLINS PRODUCTION; COMETARY ICE ANALOGS; MASS-SPECTROMETRY;
HEXAMETHYLENETETRAMINE HMT; PREBIOTIC CHEMISTRY; INTERSTELLAR ICE;
SOLID-STATE; PRODUCTS; MELAMINE; SPECTROSCOPY
AB Although the cassini Spacecraft and the Huygens Lander provided vast information about Titan atmospheric chemistry and the formation of its aerosols, the exact composition of these aerosols still remains unknown. A fruitful proxy to investigate these aerosols is the use of laboratory experiments that allow producing and studying analogs of Titan aerosol, the so-called tholins. Even when produced in the laboratory, unveiling the exact composition of the aerosol remains problematic due to the high complexity of the material. Numerous advances have been recently made using high-resolution mass spectrometry (HRMS) (Pernot et al. [2010] Anal. Chem. 82, 1371; Somogyi et al. [2012] Int. J. Mass Spectrom. 316-318, 157-163; Gautier et al. [2014] Earth Planet. Sci. Lett. 404, 33-42) that allowed the separation of isobaric compounds and a robust identification of chemical species composing tholins regarding their molecular formulae. Nevertheless isomeric species cannot be resolved by a simple mass measurement. We propose here an analysis of tholins by high performance liquid chromatography (HPLC) coupled to HRMS to unveil this isomeric ambiguity for some of the major tholins compounds. By comparing chromatograms obtained when analyzing tholins and chemical standards, we strictly identified seven molecules in our tholins samples: melamine, cyanoguanidine, 6-methyl-1,3,5-triazine-2,4-diamine, 2,4,6-triaminopyrimidine, 3-amino-1,2,4-triazole, 3,5-Dimethyl-1,2,4-triazole and 2,4-diamino-1,3,5-triazine. Several molecules, including hexamethylenetriamine (HMT) were not present at detectable levels in our sample. The use for the first time of a coupled HPLC-HRMS technique applied to tholins study demonstrated the interest of such a technique compared to single high-resolution mass spectrometry for the study of tholins composition. (C) 2016 Elsevier Inc. All rights reserved.
C1 [Gautier, Thomas] NASA, Goddard Space Flight Ctr, Code 699,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
[Gautier, Thomas; Szopa, Cyril; Carrasco, Nathalie] Univ Paris 06, UVSQ Univ Paris Saclay, LATMOS IPSL, F-78280 Guyancourt, France.
[Schmitz-Afonso, Isabelle; Touboul, David] Univ Paris 11, ICSN, CNRS UPR 2301, 1 Ave Terrasse, F-91198 Gif Sur Yvette, France.
[Schmitz-Afonso, Isabelle] Normandie Univ, COBRA, UMR 6014, 1 Rue Tesniere, F-76821 Mont St Aignan, France.
[Schmitz-Afonso, Isabelle] Univ Rouen, INSA Rouen, CNRS, FR3038,IRCOF, 1 Rue Tesniere, F-76821 Mont St Aignan, France.
[Szopa, Cyril; Carrasco, Nathalie] Inst Univ France, 103 Bvd St Michel, F-75005 Paris, France.
[Buch, Arnaud] Ecole Cent Paris, LGPM, F-92295 Chatenay Malabry, France.
RP Gautier, T (reprint author), NASA, Goddard Space Flight Ctr, Code 699,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM thomas.j.gautier@nasa.gov
RI Carrasco, Nathalie/D-2365-2012; szopa, cyril/C-6865-2015
OI Carrasco, Nathalie/0000-0002-0596-6336; szopa, cyril/0000-0002-0090-4056
FU French Program National de Planetologie (PNP); European Research Council
(ERC Starting Grant PRIMCHEM) [636829]
FX The research presented in this paper was partially funded through the
French Program National de Planetologie (PNP). NC acknowledges the
European Research Council for their financial support (ERC Starting
Grant PRIMCHEM, Grant agreement no. 636829). TG acknowledges the NASA
Postdoctoral Program at the Goddard Space Flight Center, administered by
Oak Ridge Associated Universities.
NR 33
TC 0
Z9 0
U1 12
U2 25
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 SEP 1
PY 2016
VL 275
BP 259
EP 266
DI 10.1016/j.icarus.2016.03.007
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA DO8FB
UT WOS:000378016900021
ER
PT J
AU Leon, JJD
Fryauf, DM
Cormia, RD
Zhang, MXM
Samuels, K
Williams, RS
Kobayashi, NP
AF Leon, Juan J. Diaz
Fryauf, David M.
Cormia, Robert D.
Zhang, Min-Xian Max
Samuels, Kathryn
Williams, R. Stanley
Kobayashi, Nobuhiko P.
TI Reflectometry-Ellipsometry Reveals Thickness, Growth Rate, and Phase
Composition in Oxidation of Copper
SO ACS APPLIED MATERIALS & INTERFACES
LA English
DT Article
DE copper oxide; reflectometry; ellipsometry; memristor; volatile
conductive bridge
ID THIN-FILMS; NATIVE OXIDATION; SINGLE-CRYSTAL; OXIDE; SURFACES; KINETICS;
BULK; XPS
AB The oxidation of copper is a complicated process. Copper oxide develops two stable phases at room temperature and standard pressure (RTSP): cuprous oxide (Cu2O) and cupric oxide (CuO). Both phases:have different optical and electrical characteristics that make them interesting for applications such as solar cells or resistive switching devices. For a given application, it is necessary to selectively control oxide thickness and cupric/cuprous oxide phase volume fraction. The thickness and composition of a copper oxide film growing on the surface of copper widely depend on the characteristics of as-deposited copper. In this Research Article, two samples, copper films prepared by two different deposition techniques, electron-beam evaporation and, sputtering, were studied. As the core part of the study, the formation of the oxidized copper was analyzed routinely over a period of 253 days using spectroscopic polarized reflectometry-spectroscopic ellipsometry (RE). An effective medium approximation (EMA) model was used to fit the RE data. The RE measurements were complemented and validated by using X-ray photoelectron spectroscopy (XPS), atomic force microscopy (AFM) and X-ray diffraction (XRD). Our results show that the two samples oxidized under identical laboratory ambient conditions (RTSP, 87% average relative humidity) developed unique oxide films following an inverse-logarithmic growth rate with thickness and composition different from each other over time. Discussion is focused on the ability of RE to simultaneously extract thickness (i.e., growth rate) and composition of copper oxide films and on plausible physical mechanisms responsible for unique oxidation habits observed in the two copper samples. It appears that extended surface characteristics (i.e., surface roughness and grain boundaries) and preferential crystalline orientation of as deposited polycrystalline copper films control the growth kinetics of the copper oxide film. Analysis based on a noncontact and nondestructive measurement, such as RE, to extract key material parameters is beneficial for conveniently understanding the oxidation process that would ultimately enable copper oxide-based devices at manufacturing scales.
C1 [Leon, Juan J. Diaz; Fryauf, David M.; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA.
[Leon, Juan J. Diaz; Fryauf, David M.; Kobayashi, Nobuhiko P.] Univ Calif Santa Cruz, Nanostruct Energy Convers Technol & Res NECTAR, Adv Studies Labs, NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
[Cormia, Robert D.] Foothill Coll, Los Altos, CA 94022 USA.
[Zhang, Min-Xian Max; Samuels, Kathryn; Williams, R. Stanley] Hewlett Packard Labs, Palo Alto, CA 94304 USA.
RP Leon, JJD (reprint author), Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA.; Leon, JJD (reprint author), Univ Calif Santa Cruz, Nanostruct Energy Convers Technol & Res NECTAR, Adv Studies Labs, NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
EM jdiazleo@ucsc.edu
RI Williams, R. Stanley/A-8281-2009
OI Williams, R. Stanley/0000-0003-0213-4259
FU NSF [DMR-1126845]
FX We would like to acknowledge the Scott Oliver lab at the University of
California Santa Cruz for the work of Jesse Hauser in X-ray
diffractometry using a Rigaku SmartLab X-ray diffractometer, funded by
the NSF Major Research Instrument (MRI) Program under Grant DMR-1126845.
We would also like to thank Vince Crist (XPS international) for helpful
assistance in interpreting the XPS data.
NR 36
TC 0
Z9 0
U1 30
U2 30
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 AUG 31
PY 2016
VL 8
IS 34
BP 22337
EP 22344
DI 10.1021/acsami.6b06626
PG 8
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary
SC Science & Technology - Other Topics; Materials Science
GA DU9CP
UT WOS:000382514100060
ER
PT J
AU Nedoluha, GE
Connor, BJ
Mooney, T
Barrett, JW
Parrish, A
Gomez, RM
Boyd, I
Allen, DR
Kotkamp, M
Kremser, S
Deshler, T
Newman, P
Santee, ML
AF Nedoluha, Gerald E.
Connor, Brian J.
Mooney, Thomas
Barrett, James W.
Parrish, Alan
Gomez, R. Michael
Boyd, Ian
Allen, Douglas R.
Kotkamp, Michael
Kremser, Stefanie
Deshler, Terry
Newman, Paul
Santee, Michelle L.
TI 20 years of ClO measurements in the Antarctic lower stratosphere
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID CHLORINE MONOXIDE; SPRING STRATOSPHERE; LOW ALTITUDES; OZONE;
REANALYSIS; SATELLITE; CHEMISTRY; CIO
AB We present 20 years (1996-2015) of austral springtime measurements of chlorine monoxide (ClO) over Antarctica from the Chlorine Oxide Experiment (ChlOE1) ground-based millimeter wave spectrometer at Scott Base, Antarctica, as well 12 years (2004-2015) of ClO measurements from the Aura Microwave Limb Sounder (MLS). From August onwards we observe a strong increase in lower stratospheric ClO, with a peak column amount usually occurring in early September. From mid-September onwards we observe a strong decrease in ClO. In order to study interannual differences, we focus on a 3-week period from 28 August to 17 September for each year and compare the average column ClO anomalies. These column ClO anomalies are shown to be highly correlated with the average ozone mass deficit for September and October of each year. We also show that anomalies in column ClO are strongly anti-correlated with 30 hPa temperature anomalies, both on a daily and an interannual timescale. Making use of this anti-correlation we calculate the linear dependence of the interannual variations in column ClO on interannual variations in temperature. By making use of this relationship, we can better estimate the underlying trend in the total chlorine (Cl-y = HCl + ClONO2 + HOCl + 2 x Cl-2 + 2 x Cl2O2 + ClO + Cl). The resultant trends in Cl-y, which determine the long-term trend in ClO, are estimated to be -0.5 +/- 0.2, -1.4 +/- 0.9, and -0.6 +/- 0.4% year(-1), for zonal MLS, Scott Base MLS (both 2004-2015), and ChlOE (1996-2015) respectively. These trends are within 1 sigma of trends in stratospheric Cl-y previously found at other latitudes. The decrease in ClO is consistent with the trend expected from regulations enacted under the Montreal Protocol.
C1 [Nedoluha, Gerald E.; Gomez, R. Michael; Allen, Douglas R.] Naval Res Lab, Washington, DC 20375 USA.
[Connor, Brian J.; Mooney, Thomas; Boyd, Ian] BC Sci Consulting LLC, Stony Brook, NY USA.
[Barrett, James W.] SUNY Stony Brook, Stony Brook, NY 11794 USA.
[Parrish, Alan] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Kotkamp, Michael] Natl Inst Water & Atmospher Res, Lauder, New Zealand.
[Kremser, Stefanie] Bodeker Sci, Alexandra, New Zealand.
[Deshler, Terry] Univ Wyoming, Dept Atmospher Sci, Laramie, WY 82071 USA.
[Newman, Paul] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Santee, Michelle L.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Nedoluha, GE (reprint author), Naval Res Lab, Washington, DC 20375 USA.
EM nedoluha@nrl.navy.mil
OI /0000-0002-3573-7083
FU NASA under the Upper Atmosphere Research Program; Naval Research
Laboratory; Office of Naval Research; National Aeronautics and Space
Administration
FX This project was funded by NASA under the Upper Atmosphere Research
Program, by the Naval Research Laboratory, and by the Office of Naval
Research. We would like to acknowledge the many Antarctica New Zealand
technicians who have supported the daily operation of ChlOE over two
decades of measurements. We also acknowledge the logistical support that
Antarctica New Zealand has supplied over this period. Work at the Jet
Propulsion Laboratory, California Institute of Technology, was carried
out under a contract with the National Aeronautics and Space
Administration. Sonde temperature data were collected under support from
the National Science Foundation.
NR 30
TC 1
Z9 1
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 AUG 30
PY 2016
VL 16
IS 16
BP 10725
EP 10734
DI 10.5194/acp-16-10725-2016
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW6EZ
UT WOS:000383743600002
ER
PT J
AU Dolant, C
Langlois, A
Montpetit, B
Brucker, L
Roy, A
Royer, A
AF Dolant, Caroline
Langlois, Alexandre
Montpetit, Benoit
Brucker, Ludovic
Roy, Alexandre
Royer, Alain
TI Development of a rain-on-snow detection algorithm using passive
microwave radiometry
SO HYDROLOGICAL PROCESSES
LA English
DT Article
DE snow; passive microwave; rain-on-snow; extreme winter events
ID THERMAL-CONDUCTIVITY; ACTIVE LAYER; IMPACTS; TEMPERATURE; SVALBARD;
CLIMATE; EVENTS; MODEL; ICE
AB Currently observed climate warming in the Arctic has numerous consequences. Of particular relevance, the precipitation regime is modified where mixed and liquid precipitation can occur during the winter season leading to rain-on-snow (ROS) events. This phenomenon is responsible for ice crust formation, which has a significant impact on ecosystems (such as biological, hydrological, ecological and physical processes). The spatially and temporally sporadic nature of ROS events makes the phenomenon difficult to monitor using meteorological observations. This paper focuses on the detection of ROS events using passive microwave (PMW) data from a modified brightness temperature (T-B) gradient approach at 19 and 37GHz. The approach presented here was developed empirically for observed ROS events with coincident ground-based PMW measurements in Sherbrooke, Quebec, Canada. It was then tested in Nunavik, Quebec, with the Advanced Microwave Scanning Radiometer for the Earth Observing System (AMSR-E). We obtained a detection accuracy of 57, 71 and 89% for ROS detection for three AMSR-E grid cells with a maximum error of 7% when considering all omissions and commissions with regard to the total number of AMSR-E passes throughout the winter period. Copyright (c) 2016 John Wiley & Sons, Ltd.
C1 [Dolant, Caroline; Langlois, Alexandre; Montpetit, Benoit; Roy, Alexandre; Royer, Alain] Univ Sherbrooke, Ctr Applicat & Rech Teledetect CARTEL, Sherbrooke, PQ J1K 2R1, Canada.
[Dolant, Caroline; Langlois, Alexandre; Montpetit, Benoit; Royer, Alain] Ctr Etud Nord, Kuujjuarapik, PQ, Canada.
[Montpetit, Benoit] Environm Canada, Canadian Ice Serv, Ottawa, ON, Canada.
[Brucker, Ludovic] NASA, Goddard Space Flight Ctr, Cryospher Sci Lab, Code 615, Greenbelt, MD 20771 USA.
[Brucker, Ludovic] Univ Space Res Assoc, Goddard Earth Sci Technol & Res Studies & Invest, Columbia, MD 21044 USA.
RP Dolant, C (reprint author), Univ Sherbrooke, Ctr Applicat & Rech Teledetect CARTEL, Sherbrooke, PQ J1K 2R1, Canada.
EM caroline.dolant@USherbrooke.ca
RI Brucker, Ludovic/A-8029-2010
OI Brucker, Ludovic/0000-0001-7102-8084
FU Natural Sciences and Engineering Research Council of Canada (NSERC);
Centre for Northern Studies; EnviroNorth; Canadian Foundation for
Innovation (CFI)
FX Funding for this research was provided by the Natural Sciences and
Engineering Research Council of Canada (NSERC), the Centre for Northern
Studies, EnviroNorth and the Canadian Foundation for Innovation (CFI).
Thanks to the National Snow and Ice Data Center (NSIDC) for satellite
data access. The authors would also like to thank the Universite de
Sherbrooke and the Centre d'Applications et de Recherches en
TELedetection (CARTEL) for logistical and administrative support.
NR 46
TC 3
Z9 3
U1 10
U2 10
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0885-6087
EI 1099-1085
J9 HYDROL PROCESS
JI Hydrol. Process.
PD AUG 30
PY 2016
VL 30
IS 18
BP 3184
EP 3196
DI 10.1002/hyp.10828
PG 13
WC Water Resources
SC Water Resources
GA DW2IU
UT WOS:000383466900006
ER
PT J
AU Bonnett, C
Troxel, MA
Hartley, W
Amara, A
Leistedt, B
Becker, MR
Bernstein, GM
Bridle, SL
Bruderer, C
Busha, MT
Kind, MC
Childress, MJ
Castander, FJ
Chang, C
Crocce, M
Davis, TM
Eifler, TF
Frieman, J
Gangkofner, C
Gaztanaga, E
Glazebrook, K
Gruen, D
Kacprzak, T
King, A
Kwan, J
Lahav, O
Lewis, G
Lidman, C
Lin, H
MacCrann, N
Miquel, R
O'Neill, CR
Palmese, A
Peiris, HV
Refregier, A
Rozo, E
Rykoff, ES
Sadeh, I
Sanchez, C
Sheldon, E
Uddin, S
Wechsler, RH
Zuntz, J
Abbott, T
Abdalla, FB
Allam, S
Armstrong, R
Banerji, M
Bauer, AH
Benoit-Levy, A
Bertin, E
Brooks, D
Buckley-Geer, E
Burke, DL
Capozzi, D
Rosell, AC
Carretero, J
Cunha, CE
D'Andrea, CB
da Costa, LN
DePoy, DL
Desai, S
Diehl, HT
Dietrich, JP
Doel, P
Neto, AF
Fernandez, E
Flaugher, B
Fosalba, P
Gerdes, DW
Gruendl, RA
Honscheid, K
Jain, B
James, DJ
Jarvis, M
Kim, AG
Kuehn, K
Kuropatkin, N
Li, TS
Lima, M
Maia, MAG
March, M
Marshall, JL
Martini, P
Melchior, P
Miller, CJ
Neilsen, E
Nichol, RC
Nord, B
Ogando, R
Plazas, AA
Reil, K
Romer, AK
Roodman, A
Sako, M
Sanchez, E
Santiago, B
Smith, RC
Soares-Santos, M
Sobreira, F
Suchyta, E
Swanson, MEC
Tarle, G
Thaler, J
Thomas, D
Vikram, V
Walker, AR
AF Bonnett, C.
Troxel, M. A.
Hartley, W.
Amara, A.
Leistedt, B.
Becker, M. R.
Bernstein, G. M.
Bridle, S. L.
Bruderer, C.
Busha, M. T.
Kind, M. Carrasco
Childress, M. J.
Castander, F. J.
Chang, C.
Crocce, M.
Davis, T. M.
Eifler, T. F.
Frieman, J.
Gangkofner, C.
Gaztanaga, E.
Glazebrook, K.
Gruen, D.
Kacprzak, T.
King, A.
Kwan, J.
Lahav, O.
Lewis, G.
Lidman, C.
Lin, H.
MacCrann, N.
Miquel, R.
O'Neill, C. R.
Palmese, A.
Peiris, H. V.
Refregier, A.
Rozo, E.
Rykoff, E. S.
Sadeh, I.
Sanchez, C.
Sheldon, E.
Uddin, S.
Wechsler, R. H.
Zuntz, J.
Abbott, T.
Abdalla, F. B.
Allam, S.
Armstrong, R.
Banerji, M.
Bauer, A. H.
Benoit-Levy, A.
Bertin, E.
Brooks, D.
Buckley-Geer, E.
Burke, D. L.
Capozzi, D.
Carnero Rosell, A.
Carretero, J.
Cunha, C. E.
D'Andrea, C. B.
da Costa, L. N.
DePoy, D. L.
Desai, S.
Diehl, H. T.
Dietrich, J. P.
Doel, P.
Fausti Neto, A.
Fernandez, E.
Flaugher, B.
Fosalba, P.
Gerdes, D. W.
Gruendl, R. A.
Honscheid, K.
Jain, B.
James, D. J.
Jarvis, M.
Kim, A. G.
Kuehn, K.
Kuropatkin, N.
Li, T. S.
Lima, M.
Maia, M. A. G.
March, M.
Marshall, J. L.
Martini, P.
Melchior, P.
Miller, C. J.
Neilsen, E.
Nichol, R. C.
Nord, B.
Ogando, R.
Plazas, A. A.
Reil, K.
Romer, A. K.
Roodman, A.
Sako, M.
Sanchez, E.
Santiago, B.
Smith, R. C.
Soares-Santos, M.
Sobreira, F.
Suchyta, E.
Swanson, M. E. C.
Tarle, G.
Thaler, J.
Thomas, D.
Vikram, V.
Walker, A. R.
CA Dark Energy Survey Collaboration
TI Redshift distributions of galaxies in the Dark Energy Survey Science
Verification shear catalogue and implications for weak lensing
SO PHYSICAL REVIEW D
LA English
DT Article
ID STAR-FORMING GALAXIES; LARGE-SCALE STRUCTURE; PHOTO-Z PERFORMANCE; VLT
DEEP SURVEY; PHOTOMETRIC REDSHIFTS; DATA RELEASE; PRECISION COSMOLOGY;
SURVEY REQUIREMENTS; SHAPE MEASUREMENT; NEURAL-NETWORKS
AB We present photometric redshift estimates for galaxies used in the weak lensing analysis of the Dark Energy Survey Science Verification (DES SV) data. Four model-or machine learning-based photometric redshift methods-ANNZ2, BPZ calibrated against BCC-Ufig simulations, SKYNET, and TPZ-are analyzed. For training, calibration, and testing of these methods, we construct a catalogue of spectroscopically confirmed galaxies matched against DES SV data. The performance of the methods is evaluated against the matched spectroscopic catalogue, focusing on metrics relevant for weak lensing analyses, with additional validation against COSMOS photo-z's. From the galaxies in the DES SV shear catalogue, which have mean redshift 0.72 +/- 0.01 over the range 0.3 < z < 1.3, we construct three tomographic bins with means of z = {0.45; 0.67; 1.00}. These bins each have systematic uncertainties delta z <= 0.05 in the mean of the fiducial SKYNET photo-z (dz). We propagate the errors in the redshift distributions through to their impact on cosmological parameters estimated with cosmic shear, and find that they cause shifts in the value of sigma(8) of approximately 3%. This shift is within the one sigma statistical errors on sigma(8) for the DES SV shear catalogue. We further study the potential impact of systematic differences on the critical surface density, Sigma(crit), finding levels of bias safely less than the statistical power of DES SV data. We recommend a final Gaussian prior for the photo-z bias in the mean of n(z) of width 0.05 for each of the three tomographic bins, and show that this is a sufficient bias model for the corresponding cosmology analysis.
C1 [Bonnett, C.; Miquel, R.; Sanchez, C.; Carretero, J.; Fernandez, E.] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain.
[Troxel, M. A.; Bridle, S. L.; MacCrann, N.; Zuntz, J.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England.
[Hartley, W.; Amara, A.; Bruderer, C.; Chang, C.; Kacprzak, T.; Refregier, A.] ETH, Dept Phys, Wolfgang Pauli Str 16, CH-8093 Zurich, Switzerland.
[Leistedt, B.; Lahav, O.; Palmese, A.; Peiris, H. V.; Sadeh, I.; Abdalla, F. B.; Benoit-Levy, A.; Brooks, D.; Doel, P.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England.
[Becker, M. R.; Busha, M. T.] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA.
[Becker, M. R.; Rykoff, E. S.; Wechsler, R. H.; Burke, D. L.; Cunha, C. E.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA.
[Bernstein, G. M.; Eifler, T. F.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[King, A.] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia.
[Kind, M. Carrasco; Gruendl, R. A.] 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.
[Castander, F. J.; Crocce, M.; Gaztanaga, E.; Bauer, A. H.; Carretero, J.; Fosalba, P.] IEEC CSIC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, Barcelona 08193, Spain.
[Eifler, T. F.; Abdalla, F. B.; Plazas, A. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Frieman, J.; Lin, H.; Allam, S.; Buckley-Geer, E.; Diehl, H. T.; Flaugher, B.; Kuropatkin, N.; Neilsen, E.; Nord, B.; Soares-Santos, M.; Sobreira, F.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA.
[Frieman, J.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Kwan, J.; Vikram, V.] Argonne Natl Lab, 9700 South Cass Ave, Lemont, IL 60439 USA.
[Lidman, C.; Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia.
[Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain.
[Rozo, E.] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA.
[Rykoff, E. S.; Wechsler, R. H.; Burke, D. L.; Reil, K.; Roodman, A.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA.
[Glazebrook, K.; Uddin, S.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Abbott, T.; James, D. J.; Smith, R. C.; Walker, A. R.] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile.
[Armstrong, R.] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA.
[Banerji, M.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
[Banerji, M.] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England.
[Bertin, E.] Inst Astrophys, CNRS, UMR 7095, F-75014 Paris, France.
[Bertin, E.] Univ Paris 06, Sorbonne Univ, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Capozzi, D.; D'Andrea, C. B.; Nichol, R. C.; Thomas, D.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Carnero Rosell, A.; da Costa, L. N.; Fausti Neto, A.; Lima, M.; Maia, M. A. G.; Ogando, R.; Santiago, B.; Sobreira, F.] Lab Interinst Eastron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil.
[Carnero Rosell, A.; da Costa, L. N.; Maia, M. A. G.; Ogando, R.] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil.
[DePoy, D. L.; Li, T. S.; Marshall, J. L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
[DePoy, D. L.; Li, T. S.; Marshall, J. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
[Desai, S.] Univ Munich, Dept Phys, Scheinerstr 1, D-81679 Munich, Germany.
[Gangkofner, C.; Sheldon, E.; Desai, S.; Dietrich, J. P.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany.
[Gruen, D.; Dietrich, J. P.] Univ Munich, Univ Sternwarte, Fak Phys, Scheinerstr 1, D-81679 Munich, Germany.
[Gerdes, D. W.; Miller, C. J.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Gruen, D.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany.
[Honscheid, K.; Martini, P.; Melchior, P.; Suchyta, E.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Honscheid, K.; Melchior, P.; Suchyta, E.] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA.
[Kim, A. G.] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA.
[Martini, P.] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA.
[Miller, C. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Romer, A. K.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England.
[Sanchez, E.] CIEMAT, Madrid, Spain.
[Santiago, B.] Univ Fed Rio Grande do Sul, Inst Fis, Caixa Postal 15051, BR-91501970 Porto Alegre, RS, Brazil.
[Thaler, J.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA.
[Lima, M.] Univ Sao Paulo, Inst Fis, Dept Fis Matemat, CP 66318, BR-05314970 Sao Paulo, SP, Brazil.
[Lewis, G.] South East Phys Network, SEPnet, Southampton, Hants, England.
[Davis, T. M.; O'Neill, C. R.] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia.
[Childress, M. J.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia.
[Sheldon, E.] Brookhaven Natl Lab, Bldg 510, Upton, NY 11973 USA.
[Gangkofner, C.] Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany.
RP Bonnett, C (reprint author), Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain.
RI Lima, Marcos/E-8378-2010; Ogando, Ricardo/A-1747-2010; Davis,
Tamara/A-4280-2008; Gaztanaga, Enrique/L-4894-2014;
OI Ogando, Ricardo/0000-0003-2120-1154; Davis, Tamara/0000-0002-4213-8783;
Gaztanaga, Enrique/0000-0001-9632-0815; Abdalla,
Filipe/0000-0003-2063-4345; Sobreira, Flavia/0000-0002-7822-0658
FU European Research Council [240672]; DFG Cluster of Excellence Origin and
Structure of the Universe; 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 e Tecnologia; 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; Eidgenossische
Technische Hochschule (ETH) Zurich; Fermi National Accelerator
Laboratory; University of Edinburgh; 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 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; Australian Astronomical Observatory [A/2013B/012];
Australian Research Council Centre of Excellence for All-sky
Astrophysics (CAASTRO) [CE110001020]; Swiss National Science Foundation
[200021_14944, 200021_143906]; Alfred P. Sloan Foundation; National
Science Foundation; U.S. Department of Energy Office of Science;
University of Arizona; Brazilian Participation Group; Brookhaven
National Laboratory; 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; Max Planck
Institute for Astrophysics; Max Planck Institute for Extraterrestrial
Physics; New Mexico State University; New York University; Pennsylvania
State University; Princeton University; Spanish Participation Group;
University of Tokyo; University of Utah; Vanderbilt University;
University of Virginia; University of Washington; Yale University; ESO
Telescopes at the La Silla Paranal Observatory [179.A-2004, 177.A-3016]
FX We are grateful for the extraordinary contributions of our CTIO
colleagues and the DECam Construction, Commissioning and Science
Verification teams in achieving the excellent instrument and telescope
conditions that have made this work possible. The success of this
project also relies critically on the expertise and dedication of the
DES Data Management group. M. T., S. B., N. M., and J. Z. acknowledge
support from the European Research Council in the form of a Starting
Grant with number 240672. D. G. acknowledges the support by the DFG
Cluster of Excellence Origin and Structure of the Universe. 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 e Tecnologia, the
Deutsche Forschungsgemeinschaft and the Collaborating Institutions in
the Dark Energy Survey. C. G. acknowledges the support by the DFG
Cluster of Excellence Origin and Structure of the Universe. 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 Eidgenossische Technische
Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the
University of Edinburgh, 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 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. Based in part on observations taken at
the Australian Astronomical Observatory under program A/2013B/012. Parts
of this research were conducted by the Australian Research Council
Centre of Excellence for All-sky Astrophysics (CAASTRO), through project
number CE110001020. This work was supported in part by grants
200021_14944 and 200021_143906 from the Swiss National Science
Foundation. 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.; r 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, 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. Based on observations made with ESO Telescopes at the La
Silla Paranal Observatory under programme ID 179.A-2004. Based on
observations made with ESO Telescopes at the La Silla Paranal
Observatory under programme ID 177.A-3016. This paper is Fermilab
publication FERMILAB-PUB-15-306 and DES publication DES2015-0060. This
paper has gone through internal review by the DES Collaboration.
NR 95
TC 10
Z9 10
U1 5
U2 5
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 AUG 30
PY 2016
VL 94
IS 4
AR 042005
DI 10.1103/PhysRevD.94.042005
PG 26
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA DU4IW
UT WOS:000382177300001
ER
PT J
AU Frankenberg, C
Thorpe, AK
Thompson, DR
Hulley, G
Kort, EA
Vance, N
Borchardt, J
Krings, T
Gerilowski, K
Sweeney, C
Conley, S
Bue, BD
Aubrey, AD
Hook, S
Green, RO
AF Frankenberg, Christian
Thorpe, Andrew K.
Thompson, David R.
Hulley, Glynn
Kort, Eric Adam
Vance, Nick
Borchardt, Jakob
Krings, Thomas
Gerilowski, Konstantin
Sweeney, Colm
Conley, Stephen
Bue, Brian D.
Aubrey, Andrew D.
Hook, Simon
Green, Robert O.
TI Airborne methane remote measurements reveal heavy-tail flux distribution
in Four Corners region
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE methane; Four Corners; remote sensing; heavy-tail
ID IMAGING SPECTROMETER AVIRIS; MATCHED-FILTER DETECTION; GAS PRODUCTION
SITES; EMISSION RATES; UNITED-STATES; TRACE GASES; RETRIEVAL;
QUANTIFICATION; SPECTROSCOPY; CO2
AB Methane (CH4) impacts climate as the second strongest anthropogenic greenhouse gas and air quality by influencing tropospheric ozone levels. Space-based observations have identified the Four Corners region in the Southwest United States as an area of large CH4 enhancements. We conducted an airborne campaign in Four Corners during April 2015 with the next-generation Airborne Visible/Infrared Imaging Spectrometer (near-infrared) and Hyperspectral Thermal Emission Spectrometer (thermal infrared) imaging spectrometers to better understand the source of methane by measuring methane plumes at 1-to 3-m spatial resolution. Our analysis detected more than 250 individual methane plumes from fossil fuel harvesting, processing, and distributing infrastructures, spanning an emission range from the detection limit similar to 2 kg/h to 5 kg/h through similar to 5,000 kg/h. Observed sources include gas processing facilities, storage tanks, pipeline leaks, and well pads, as well as a coal mine venting shaft. Overall, plume enhancements and inferred fluxes follow a lognormal distribution, with the top 10% emitters contributing 49 to 66% to the inferred total point source flux of 0.23 Tg/y to 0.39 Tg/y. With the observed confirmation of a lognormal emission distribution, this airborne observing strategy and its ability to locate previously unknown point sources in real time provides an efficient and effective method to identify and mitigate major emissions contributors over a wide geographic area. With improved instrumentation, this capability scales to spaceborne applications [Thompson DR, et al. (2016) Geophys Res Lett 43(12): 6571-6578]. Further illustration of this potential is demonstrated with two detected, confirmed, and repaired pipeline leaks during the campaign.
C1 [Frankenberg, Christian] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Frankenberg, Christian; Thorpe, Andrew K.; Thompson, David R.; Hulley, Glynn; Vance, Nick; Bue, Brian D.; Aubrey, Andrew D.; Hook, Simon; Green, Robert O.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Kort, Eric Adam] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
[Borchardt, Jakob; Krings, Thomas; Gerilowski, Konstantin] Univ Bremen, Inst Environm Phys, D-28334 Bremen, Germany.
[Sweeney, Colm] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Sweeney, Colm] NOAA, Global Monitoring Div, Earth Syst Res Lab, Boulder, CO 80305 USA.
[Conley, Stephen] Sci Aviat, Boulder, CO 80301 USA.
[Conley, Stephen] Univ Calif Davis, Dept Land Air & Water Resources, Davis, CA 95616 USA.
RP Frankenberg, C (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.; Frankenberg, C (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM cfranken@caltech.edu
RI Kort, Eric/F-9942-2012; Frankenberg, Christian/A-2944-2013
OI Kort, Eric/0000-0003-4940-7541; Frankenberg,
Christian/0000-0002-0546-5857
FU NASA Headquarters; state of Bremen; University of Bremen; National
Oceanic and Atmospheric Administration AC4 program [NA14OAR0110139]
FX We thank the AVIRIS-NG flight and instrument teams, including Michael
Eastwood, Sarah Lundeen, Scott Nolte, Mark Helmlinger, and Betina Pavri.
Didier Keymeulen and Joseph Boardman assisted with the real-time system.
We also thank the HyTES flight and instrument teams, including Bjorn
Eng, Jonathan Mihaly, Seth Chazanoff, and Bill Johnson. We thank the
organizers and all the participants in the TOPDOWN campaign for the
fruitful collaboration. We thank NASA Headquarters, in particular Jack
Kaye, for funding this flight campaign, which augmented the overall Twin
Otter Projects Defining Oil/Gas Well Emissions (TOPDOWN) campaign. J.B.,
T.K., and K.G. were funded by the state of Bremen and University of
Bremen. E.A.K. and C.S. were supported, in part, by the National Oceanic
and Atmospheric Administration AC4 program under Grant NA14OAR0110139.
NR 23
TC 3
Z9 3
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 AUG 30
PY 2016
VL 113
IS 35
BP 9734
EP 9739
DI 10.1073/pnas.1605617113
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DV7BL
UT WOS:000383090700039
PM 27528660
ER
PT J
AU Zhang, RY
Peng, JF
Wang, Y
Hu, M
AF Zhang, Renyi
Peng, Jianfei
Wang, Yuan
Hu, Min
TI Rate and timescale of black carbon aging regulate direct radiative
forcing
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Letter
ID AEROSOLS; IMPACTS; CHINA
C1 [Zhang, Renyi; Peng, Jianfei] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
[Zhang, Renyi; Peng, Jianfei] Texas A&M Univ, Dept Chem, College Stn, TX 77843 USA.
[Zhang, Renyi; Peng, Jianfei; Hu, Min] Peking Univ, Coll Environm Sci & Engn, State Key Joint Lab Environm Simulat & Pollut Con, Beijing 100871, Peoples R China.
[Wang, Yuan] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
RP Zhang, RY (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.; Zhang, RY (reprint author), Texas A&M Univ, Dept Chem, College Stn, TX 77843 USA.; Zhang, RY; Hu, M (reprint author), Peking Univ, Coll Environm Sci & Engn, State Key Joint Lab Environm Simulat & Pollut Con, Beijing 100871, Peoples R China.
EM renyi-zhang@tamu.edu; minhu@pku.edu.cn
RI Peng, Jianfei/F-1438-2015
NR 10
TC 0
Z9 0
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 AUG 30
PY 2016
VL 113
IS 35
BP E5094
EP E5095
DI 10.1073/pnas.1610241113
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA DV7BL
UT WOS:000383090700002
PM 27555593
ER
PT J
AU Feyhl-Buska, J
Chen, YF
Jia, CL
Wang, JX
Zhang, CLL
Boyd, ES
AF Feyhl-Buska, Jayme
Chen, Yufei
Jia, Chengling
Wang, Jin-Xiang
Zhang, Chuanlun L.
Boyd, Eric S.
TI Influence of Growth Phase, pH, and Temperature on the Abundance and
Composition of Tetraether Lipids in the Thermoacidophile Picrophilus
torridus
SO FRONTIERS IN MICROBIOLOGY
LA English
DT Article
DE tetraether; GDGT; GTGT; growth phase; temperature; pH; thermoacidophile;
stress
ID FATTY-ACID-COMPOSITION; TERRESTRIAL HOT-SPRINGS; LOWER PEARL RIVER;
SOUTH CHINA SEA; MEMBRANE-LIPIDS; POLAR LIPIDS;
NITROSOPUMILUS-MARITIMUS; ARCHAEBACTERIAL LIPIDS; THERMOPHILIC ARCHAEA;
MASS-SPECTROMETRY
AB The abundance and composition of glycerol dibiphytanyl glycerol tetraether (GDGT) and glycerol tribiphytanyl glycerol tetraether (GTGT) lipids were determined as a function of growth phase as a proxy for nutrient availability, the pH of growth medium, and incubation temperature in cultures of the thermoacidophile Picrophilus torridus. Regardless of the cultivation condition, the abundance of GDGTs and GTGTs was greater in the polar than core fraction, with a marked decrease in core GDGTs in cultures harvested during log phase growth. These data are consistent with previous suggestions indicating that core GDGTs are re-functionalized during polar lipid synthesis. Under all conditions examined, polar lipids were enriched in a GDGT with 2 cyclopentyl rings (GDGT-2), indicating GDGT-2 is the preferred lipid in this taxon. However, lag or stationary phase grown cells or cells subjected to pH or thermal stress were enriched in GDGTs with 4, 5, or 6 rings and depleted in GDGTs with 1, 2, 3, rings relative to log phase cells grown under optimal conditions. Variation in the composition of polar GDGT lipids in cells harvested during various growth phases tended to be greater than in cells cultivated over a pH range of 0.31.1 and a temperature range of 5363 degrees C. These results suggest that the growth phase, the pH of growth medium, and incubation temperature are all important factors that shape the composition of tetraether lipids in Picrophilus. The similarity in enrichment of GDGTs with more rings in cultures undergoing nutrient, pH, and thermal stress points to GDGT cyclization as a generalized physiological response to stress in this taxon.
C1 [Feyhl-Buska, Jayme; Boyd, Eric S.] Montana State Univ, Dept Microbiol & Immunol, Bozeman, MT 59717 USA.
[Chen, Yufei; Jia, Chengling; Wang, Jin-Xiang; Zhang, Chuanlun L.] Tongji Univ, State Key Lab Marine Geol, Shanghai, Peoples R China.
[Boyd, Eric S.] NASA, Astrobiol Inst, Mountain View, CA 94043 USA.
[Feyhl-Buska, Jayme] Univ Southern Calif, Dept Earth Sci, Los Angeles, CA USA.
[Wang, Jin-Xiang] Univ Bremen, MARUM Ctr Marine Environm Sci, Bremen, Germany.
RP Boyd, ES (reprint author), Montana State Univ, Dept Microbiol & Immunol, Bozeman, MT 59717 USA.; Boyd, ES (reprint author), NASA, Astrobiol Inst, Mountain View, CA 94043 USA.
EM eboyd@montana.edu
FU National Science Foundation [PIRE-0968421]; National Natural Science
Foundation of China [40972211, 41373072]; National Science Foundation
Research Experience for Undergraduates grant [DBI REU 1005223]; NASA
Astrobiology Institute [NNA15BB02A]; NASA Exobiology and Evolutionary
Biology Program [NNX13AI11G]
FX This work was supported by grants from the National Science Foundation
(PIRE-0968421) to CZ and EB and from the National Natural Science
Foundation of China (40972211 and 41373072) to CZ. A National Science
Foundation Research Experience for Undergraduates grant (DBI REU
1005223) supported JF during the completion of this work. EB
acknowledges support from the NASA Astrobiology Institute (NNA15BB02A)
and the NASA Exobiology and Evolutionary Biology Program (NNX13AI11G).
Two reviewers are acknowledged for comments which significantly improved
this manuscript.
NR 60
TC 0
Z9 0
U1 8
U2 8
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 AUG 30
PY 2016
VL 7
AR 1323
DI 10.3389/fmicb.2016.01323
PG 12
WC Microbiology
SC Microbiology
GA DU3KC
UT WOS:000382108200001
PM 27625636
ER
PT J
AU Mandra, S
Zhu, Z
Wang, WL
Perdomo-Ortiz, A
Katzgraber, HG
AF Mandra, Salvatore
Zhu, Zheng
Wang, Wenlong
Perdomo-Ortiz, Alejandro
Katzgraber, Helmut G.
TI Strengths and weaknesses of weak-strong cluster problems: A detailed
overview of state-of-the-art classical heuristics versus quantum
approaches
SO PHYSICAL REVIEW A
LA English
DT Article
ID MONTE-CARLO; SPIN-GLASS; OPTIMIZATION; COMPUTATION; ANNEALERS; QUBITS
AB To date, a conclusive detection of quantum speedup remains elusive. Recently, a team by Google Inc. [V. S. Denchev et al., Phys. Rev. X 6, 031015 (2016)] proposed a weak-strong cluster model tailored to have tall and narrow energy barriers separating local minima, with the aim to highlight the value of finite-range tunneling. More precisely, results from quantum Monte Carlo simulations as well as the D-Wave 2X quantum annealer scale considerably better than state-of-the-art simulated annealing simulations. Moreover, the D-Wave 2X quantum annealer is similar to 10(8) times faster than simulated annealing on conventional computer hardware for problems with approximately 10(3) variables. Here, an overview of different sequential, nontailored, as well as specialized tailored algorithms on the Google instances is given. We show that the quantum speedup is limited to sequential approaches and study the typical complexity of the benchmark problems using insights from the study of spin glasses.
C1 [Mandra, Salvatore] Harvard Univ, Dept Chem & Chem Biol, 12 Oxford St, Cambridge, MA 02138 USA.
[Zhu, Zheng; Wang, Wenlong; Katzgraber, Helmut G.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
[Perdomo-Ortiz, Alejandro] NASA, Ames Res Ctr, Quantum Artificial Intelligence Lab, Moffett Field, CA 94035 USA.
[Perdomo-Ortiz, Alejandro] Univ Calif Santa Cruz, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Katzgraber, Helmut G.] Santa Fe Inst, 1399 Hyde Pk Rd, Santa Fe, NM 87501 USA.
[Katzgraber, Helmut G.] Coventry Univ, Appl Math Res Ctr, Coventry CV1 5FB, W Midlands, England.
RP Mandra, S (reprint author), Harvard Univ, Dept Chem & Chem Biol, 12 Oxford St, Cambridge, MA 02138 USA.
EM smandra@fas.harvard.edu; zzwtgts@tamu.edu; wenlong@physics.umass.edu;
alejandro.perdomoortiz@nasa.gov; hgk@tamu.edu
FU NSF [DMR-1151387]; NASA [NNX14AF62G]; Office of the Director of National
Intelligence (ODNI), Intelligence Advanced Research Projects Activity
(IARPA), via MIT Lincoln Laboratory Air Force [FA8721-05-C-0002]
FX We thank the Google Quantum A. I. Lab members for sharing their QMC and
SA data, multiple discussions, as well as making the weak-strong cluster
instances available to us. We also thank A. Aspuru-Guzik, F. Hamze, A.J.
Ochoa, and Eleanor G. Rieffel for many fruitful discussions, as well as
H. Munoz-Bauza for help with the graphics. H.G.K. and W.W. acknowledge
support from the NSF (Grant No. DMR-1151387). H.G.K. thanks D. Humm,
M.P. White, T. Keller, H. Blumenthal, and P. Bocuse for inspiration
during the initial stages of the manuscript. S.M. was supported by NASA
(Sponsor Award No. NNX14AF62G). We thank the Texas Advanced Computing
Center (TACC) at The University of Texas at Austin for providing HPC
resources (Stampede Cluster) and Texas A&M University for access to
their Ada and Lonestar clusters. This research is based upon work
supported in part by the Office of the Director of National Intelligence
(ODNI), Intelligence Advanced Research Projects Activity (IARPA), via
MIT Lincoln Laboratory Air Force Contract No. FA8721-05-C-0002.
NR 80
TC 2
Z9 2
U1 1
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 AUG 29
PY 2016
VL 94
IS 2
AR 022337
DI 10.1103/PhysRevA.94.022337
PG 13
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA DU2BR
UT WOS:000382016400003
ER
PT J
AU Matsuyama, I
Nimmo, F
Keane, JT
Chan, NH
Taylor, GJ
Wieczorek, MA
Kiefer, WS
Williams, JG
AF Matsuyama, Isamu
Nimmo, Francis
Keane, James T.
Chan, Ngai H.
Taylor, G. Jeffrey
Wieczorek, Mark A.
Kiefer, Walter S.
Williams, James G.
TI GRAIL, LLR, and LOLA constraints on the interior structure of the Moon
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE lunar interior
ID DEEP LUNAR INTERIOR; SEISMIC DATA; POLYCRYSTALLINE OLIVINE;
FREQUENCY-DEPENDENCE; CHANDLER-WOBBLE; TIDAL RESPONSE; GRAVITY-FIELD;
GIANT IMPACT; MARE BASALTS; MODEL
AB The interior structure of the Moon is constrained by its mass, moment of inertia, and k(2) and h(2) tidal Love numbers. We infer the likely radius, density, and (elastic limit) rigidity of all interior layers by solving the inverse problem using these observational constraints assuming spherical symmetry. Our results do not favor the presence of a low rigidity transition layer between a liquid outer core and mantle. If a transition layer exists, its rigidity is constrained to 43-9+26GPa, with a preference for the high rigidity values. Therefore, if a transition layer exists, it is more likely to have a rigidity similar to that of the mantle (approximate to 70GPa). The total (solid and liquid) core mass fraction relative to the lunar mass is constrained to 0.0098-0.0094+0.0066 and 0.0198-0.0049+0.0026 for interior structures with and without a transition layer, respectively, narrowing the range of possible giant impact formation scenarios.
C1 [Matsuyama, Isamu; Keane, James T.; Chan, Ngai H.] Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Nimmo, Francis] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA.
[Taylor, G. Jeffrey] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Wieczorek, Mark A.] Inst Phys Globe Paris, Paris, France.
[Kiefer, Walter S.] Lunar & Planetary Inst, 3303 NASA Rd 1, Houston, TX 77058 USA.
[Williams, James G.] Inst Technol, Jet Prop Lab, Pasadena, CA USA.
RP Matsuyama, I (reprint author), Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
EM isa@lpl.arizona.edu
RI Wieczorek, Mark/G-6427-2010;
OI Wieczorek, Mark/0000-0001-7007-4222; Matsuyama,
Isamu/0000-0002-2917-8633; Kiefer, Walter/0000-0001-6741-5460
FU NASA's Discovery Program
FX The GRAIL mission is supported by NASA's Discovery Program and is
performed under contract to the Massachusetts Institute of Technology
and the Jet Propulsion Laboratory, California Institute of Technology. A
portion of the research described in this paper was carried out at the
Jet Propulsion Laboratory of the California Institute of Technology,
under a contract with the National Aeronautics and Space Administration.
Government sponsorship is acknowledged. The data used are listed in the
references and tables.
NR 51
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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 AUG 28
PY 2016
VL 43
IS 16
BP 8365
EP 8375
DI 10.1002/2016GL069952
PG 11
WC Geosciences, Multidisciplinary
SC Geology
GA DX5TC
UT WOS:000384443800005
ER
PT J
AU Way, MJ
Del Genio, AD
Kiang, NY
Sohl, LE
Grinspoon, DH
Aleinov, I
Kelley, M
Clune, T
AF Way, M. J.
Del Genio, Anthony D.
Kiang, Nancy Y.
Sohl, Linda E.
Grinspoon, David H.
Aleinov, Igor
Kelley, Maxwell
Clune, Thomas
TI Was Venus the first habitable world of our solar system?
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE ancient Venus; habitability
ID EARTH; ATMOSPHERE; WATER; PLANETS; EVOLUTION; HYDROGEN; OCEAN;
DEUTERIUM; ROTATION; HISTORY
AB Present-day Venus is an inhospitable place with surface temperatures approaching 750K and an atmosphere 90 times as thick as Earth's. Billions of years ago the picture may have been very different. We have created a suite of 3-D climate simulations using topographic data from the Magellan mission, solar spectral irradiance estimates for 2.9 and 0.715 Gya, present-day Venus orbital parameters, an ocean volume consistent with current theory, and an atmospheric composition estimated for early Venus. Using these parameters we find that such a world could have had moderate temperatures if Venus had a prograde rotation period slower than similar to 16 Earth days, despite an incident solar flux 46-70% higher than Earth receives. At its current rotation period, Venus's climate could have remained habitable until at least 0.715 Gya. These results demonstrate the role rotation and topography play in understanding the climatic history of Venus-like exoplanets discovered in the present epoch.
C1 [Way, M. J.; Del Genio, Anthony D.; Kiang, Nancy Y.; Sohl, Linda E.; Aleinov, Igor; Kelley, Maxwell] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Way, M. J.] Uppsala Univ, Dept Astron & Space Phys, Uppsala, Sweden.
[Sohl, Linda E.; Aleinov, Igor] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
[Grinspoon, David H.] Planetary Sci Inst, Tucson, AZ USA.
[Clune, Thomas] NASA, Global Modeling & Assimilat Off, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Way, MJ (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.; Way, MJ (reprint author), Uppsala Univ, Dept Astron & Space Phys, Uppsala, Sweden.
EM michael.j.way@nasa.gov
OI Way, Michael/0000-0003-3728-0475
FU NASA Astrobiology Program through the Nexus for Exoplanet System Science
(NExSS) research coordination network - NASA's Science Mission
Directorate; NASA Goddard Space Flight Center ROCKE-3D Science Task
Group funding
FX This research was supported by the NASA Astrobiology Program through the
Nexus for Exoplanet System Science (NExSS) research coordination network
sponsored by NASA's 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. This research has made
use of NASA's Astrophysics Data System Bibliographic Services. Thanks to
Jeffrey A. Jonas, Kostas Tsigaridis, and David S. Amundsen for their
assistance in this work and thanks to June Wang at Washington University
in St. Louis for help with the Magellan PDS data. We also thank referee
Norman Sleep for his constructive comments. The data products associated
with this paper can be obtained by contacting the first author Michael
J. Way.
NR 53
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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 AUG 28
PY 2016
VL 43
IS 16
BP 8376
EP 8383
DI 10.1002/2016GL069790
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA DX5TC
UT WOS:000384443800006
ER
PT J
AU Scheuchl, B
Mouginot, J
Rignot, E
Morlighem, M
Khazendar, A
AF Scheuchl, B.
Mouginot, J.
Rignot, E.
Morlighem, M.
Khazendar, A.
TI Grounding line retreat of Pope, Smith, and Kohler Glaciers, West
Antarctica, measured with Sentinel-1a radar interferometry data
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE Grounding Line; Synthetic Aperture Radar; Sentinel-1
ID AMUNDSEN SEA EMBAYMENT; ICE-SHEET; PINE ISLAND; SHELF; WIDESPREAD;
STABILITY; GREENLAND; CRYOSAT-2; THWAITES; SURFACE
AB We employ Sentinel-1a C band satellite radar interferometry data in Terrain Observation with Progressive Scans mode to map the grounding line and ice velocity of Pope, Smith, and Kohler glaciers, in West Antarctica, for the years 2014-2016 and compare the results with those obtained using Earth Remote Sensing Satellites (ERS-1/2) in 1992, 1996, and 2011. We observe an ongoing, rapid grounding line retreat of Smith at 2km/yr (40km since 1996), an 11km retreat of Pope (0.5km/yr), and a 2km readvance of Kohler since 2011. The variability in glacier retreat is consistent with the distribution of basal slopes, i.e., fast along retrograde beds and slow along prograde beds. We find that several pinning points holding Dotson and Crosson ice shelves disappeared since 1996 due to ice shelf thinning, which signal the ongoing weakening of these ice shelves. Overall, the results indicate that ice shelf and glacier retreat in this sector remain unabated.
C1 [Scheuchl, B.; Mouginot, J.; Rignot, E.; Morlighem, M.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
[Rignot, E.; Khazendar, A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Scheuchl, B (reprint author), Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA.
EM bscheuch@uci.edu
FU National Aeronautics and Space Administration's Cryospheric Science
Program; National Aeronautics and Space Administration's MEaSUREs
program
FX This work was performed at the University of California, Irvine, and at
the Jet Propulsion Laboratory, California Institute of Technology, under
a grant from the National Aeronautics and Space Administration's
Cryospheric Science Program and MEaSUREs program. The authors gratefully
acknowledge the European Space Agency and the USGS for providing the
data. SAR data acquisition was coordinated by the Polar Space Task
Group. The 2014 grounding line is available at NSIDC as part of the
updated MEaSUREs InSAR based grounding line product.
NR 39
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U2 12
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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 AUG 28
PY 2016
VL 43
IS 16
BP 8572
EP 8579
DI 10.1002/2016GL069287
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA DX5TC
UT WOS:000384443800029
ER
PT J
AU Peyser, CE
Yin, JJ
Landerer, FW
Cole, JE
AF Peyser, Cheryl E.
Yin, Jianjun
Landerer, Felix W.
Cole, Julia E.
TI Pacific sea level rise patterns and global surface temperature
variability
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE sea level rise; Pacific; warming hiatus; global temperature
ID WESTERN TROPICAL PACIFIC; OCEAN HEAT UPTAKE; WARMING HIATUS;
INTENSIFICATION; CIRCULATION; ATLANTIC; TRENDS
AB During 1998-2012, climate change and sea level rise (SLR) exhibit two notable features: a slowdown of global surface warming (hiatus) and a rapid SLR in the tropical western Pacific. To quantify their relationship, we analyze the long-term control simulations of 38 climate models. We find a significant and robust correlation between the east-west contrast of dynamic sea level (DSL) in the Pacific and global mean surface temperature (GST) variability on both interannual and decadal time scales. Based on linear regression of the multimodel ensemble mean, the anomalously fast SLR in the western tropical Pacific observed during 1998-2012 indicates suppression of a potential global surface warming of 0.16 degrees 0.06 degrees C. In contrast, the Pacific contributed 0.29 degrees 0.10 degrees C to the significant interannual GST increase in 1997/1998. The Pacific DSL anomalies observed in 2015 suggest that the strong El Nino in 2015/2016 could lead to a 0.21 degrees 0.07 degrees C GST jump.
C1 [Peyser, Cheryl E.; Yin, Jianjun; Cole, Julia E.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA.
[Landerer, Felix W.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA USA.
RP Yin, JJ (reprint author), Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA.
EM yin@email.arizona.edu
FU Strategic University Research Partnership Program of the NASA Jet
Propulsion Laboratory [1492484/NNN12AA01C]
FX We thank many observation and modeling centers for making their data
available. We thank the anonymous reviewers for detailed reviews and P.
Goddard, S. Griffies, S. Malyshev, J. Pelletier, J. Russell, and R.
Stouffer for discussion. The work was supported by the Strategic
University Research Partnership Program of the NASA Jet Propulsion
Laboratory (grant # 1492484/NNN12AA01C). The work of F.W.L. was
performed at the Jet Propulsion Laboratory, California Institute of
Technology under a contract with NASA. The observational, reanalysis,
and model data used in this study can be accessed from the URLs found in
the section 2. For all other data inquiries, please contact Cheryl
Peyser (peyser@email.arizona.edu).
NR 31
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SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD AUG 28
PY 2016
VL 43
IS 16
BP 8662
EP 8669
DI 10.1002/2016GL069401
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA DX5TC
UT WOS:000384443800039
ER
PT J
AU Lyu, F
Cummer, SA
Briggs, M
Marisaldi, M
Blakeslee, RJ
Bruning, E
Wilson, JG
Rison, W
Krehbiel, P
Lu, GP
Cramer, E
Fitzpatrick, G
Mailyan, B
McBreen, S
Roberts, OJ
Stanbro, M
AF Lyu, Fanchao
Cummer, Steven A.
Briggs, Michael
Marisaldi, Martino
Blakeslee, Richard J.
Bruning, Eric
Wilson, Jennifer G.
Rison, William
Krehbiel, Paul
Lu, Gaopeng
Cramer, Eric
Fitzpatrick, Gerard
Mailyan, Bagrat
McBreen, Sheila
Roberts, Oliver J.
Stanbro, Matthew
TI Ground detection of terrestrial gamma ray flashes from distant radio
signals
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE terrestrial gamma ray flashes; energetic in-cloud pulses; lightning;
ground detection
ID ALTITUDE
AB Terrestrial gamma ray flashes (TGFs) are brief bursts of energetic gammy-ray photons generated during thunderstorms, which have been detected almost exclusively by satellite-based instruments. Here we present three lines of evidence which includes the three out of three simultaneously observed pairs, the same occurrence contexts, and the consistent estimated occurrence rate, which indicate a direct relationship between a subset of TGFs and a class of energetic radio signal easily detectable by ground-based sensors. This connection indicates that these gamma ray and radio emissions are two views of the same phenomenon and further enable detection of these TGFs from ground distant radio signals alone. Besides dramatically increasing the detection rate of TGFs, this ground detection approach can identify TGFs in continental and coastal areas that are at latitudes too high for present TGF-detecting satellites and will provide more insights into the mechanism of TGF production.
C1 [Lyu, Fanchao; Cummer, Steven A.] Duke Univ, Dept Elect & Comp Engn, Durham, NC 27708 USA.
[Briggs, Michael; Cramer, Eric; Fitzpatrick, Gerard; Mailyan, Bagrat] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA.
[Briggs, Michael; Stanbro, Matthew] Univ Alabama, Dept Space Sci, Huntsville, AL 35899 USA.
[Marisaldi, Martino] INAF IASF Bologna, Bologna, Italy.
[Marisaldi, Martino] Univ Bergen, Dept Phys & Technol, Birkeland Ctr Space Sci, Bergen, Norway.
[Blakeslee, Richard J.] NASA, Marshall Space Flight Ctr, Huntsville, AL USA.
[Bruning, Eric] Texas Tech Univ, Dept Geosci, Atmospher Sci Grp, Lubbock, TX 79409 USA.
[Wilson, Jennifer G.] NASA, Kennedy Space Ctr, Kennedy Space Ctr, FL USA.
[Rison, William; Krehbiel, Paul] New Mexico Inst Min & Technol, Langmuir Lab Atmospher Res, Geophys Res Ctr, Socorro, NM 87801 USA.
[Lu, Gaopeng] Chinese Acad Sci, Inst Atmospher Phys, Key Lab Middle Atmosphere & Global Environm Obser, Beijing, Peoples R China.
[Lu, Gaopeng] Nanjing Univ Informat Sci & Technol, Collaborat Innovat Ctr Forecast & Evaluat Meteoro, Nanjing, Jiangsu, Peoples R China.
[Cramer, Eric] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA.
[Fitzpatrick, Gerard; McBreen, Sheila; Roberts, Oliver J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
RP Cummer, SA (reprint author), Duke Univ, Dept Elect & Comp Engn, Durham, NC 27708 USA.
EM cummer@ee.duke.edu
RI Roberts, Oliver/N-6284-2016
OI Roberts, Oliver/0000-0002-7150-9061
FU National Science Foundation Dynamic and Physical Meteorology program
[ATM-1047588]; DARPA Nimbus program [HR0011-10-10059]; Science
Foundation Ireland [12/IP/1288]
FX The authors would like to acknowledge the support from the National
Science Foundation Dynamic and Physical Meteorology program through
grant ATM-1047588 and the DARPA Nimbus program through grant
HR0011-10-10059. The authors would like to thank those colleges at
Florida Institute of Technology, University of Oklahoma, University of
Mississippi, and Kansas State University which assist us with the
operation of LF networks. We thank Vaisala Inc. for providing the
real-time lightning data which enabled us to start the investigation.
O.J.R. and S.M.B. acknowledge support from Science Foundation Ireland
under grant 12/IP/1288. We thank the Fermi team for providing the
Fermi-GBM gamma ray data
(http://fermi.gsfc.nasa.gov/ssc/data/access/gbm/). The recent TGF
catalog can be accessed on the website
(http://fermi.gsfc.nasa.gov/ssc/data/access/gbm/tgf/). All data are
available by request (cummer@ee.duke.edu). The authors would like to
thank two anonymous reviewers for their comments to improve the paper.
NR 31
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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 AUG 28
PY 2016
VL 43
IS 16
BP 8728
EP 8734
DI 10.1002/2016GL070154
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA DX5TC
UT WOS:000384443800047
ER
PT J
AU Kahn, BH
Huang, XL
Stephens, GL
Collins, WD
Feldman, DR
Su, H
Wong, S
Yue, Q
AF Kahn, Brian H.
Huang, Xianglei
Stephens, Graeme L.
Collins, William D.
Feldman, Daniel R.
Su, Hui
Wong, Sun
Yue, Qing
TI ENSO regulation of far- and mid-infrared contributions to clear-sky OLR
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE far infrared; clear sky; tropics; ENSO; upper troposphere; water vapor
ID SEA-SURFACE TEMPERATURE; TROPICAL DEEP CONVECTION; WATER-VAPOR; EL-NINO;
CHANGING CLIMATE; CLOUDS; TROPOSPHERE; DEPENDENCE; SIGNATURE; RADIATION
AB NASA Aqua-derived thermodynamic profiles, calculated spectral clear-sky outgoing longwave radiation (OLR), and vertical velocity fields from meteorological reanalyses are combined to determine the relative proportion of the far-infrared (FIR) and mid-infrared (MIR) spectral contributions to the total clear-sky OLR during different phases of El Nino-Southern Oscillation (ENSO). In the ascending branch of the tropical circulation, the spatial variance of upper tropospheric water vapor is shown to be larger during La Nina than El Nino and is consistent with zonal symmetry changes in the tropical waveguide and associated tropical-extratropical mixing. In the descending branch, upper tropospheric water vapor shows weaker coupling to lower layers that is evidenced by changes in the ratio of FIR to MIR in the clear-sky OLR. Diagnostics from the Geophysical Fluid Dynamics Laboratory AM3 model simulation are generally similar to satellite data, but the ratio of FIR to MIR is 5-10% larger with respect to dynamic regime.
C1 [Kahn, Brian H.; Stephens, Graeme L.; Su, Hui; Wong, Sun; Yue, Qing] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Huang, Xianglei] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
[Collins, William D.; Feldman, Daniel R.] Lawrence Berkeley Natl Lab, Climate & Ecosyst Div, Berkeley, CA USA.
[Collins, William D.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
RP Kahn, BH (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM brian.h.kahn@jpl.nasa.gov
RI Collins, William/J-3147-2014; Yue, Qing/F-4619-2017
OI Collins, William/0000-0002-4463-9848; Yue, Qing/0000-0002-3559-6508
FU JPL; University of Michigan; NASA [NNX14AJ50G]; U.S. Department of
Energy, Office of Science, Office of Biological and Environmental
Research, Terrestrial Ecosystem Science and Atmospheric System Research
programs [DE-ACO2-05CH11231]
FX A portion of this research was carried out at the Jet Propulsion
Laboratory (JPL), California Institute of Technology, under a contract
with the National Aeronautics and Space Administration. We thank two
anonymous reviewers for very constructive feedback and insights that led
to an improved manuscript. B. Kahn was supported by Strategic University
Research Partnership (SURP) proposal between JPL and the University of
Michigan. X. Huang was supported by NASA under grant NNX14AJ50G awarded
to the University of Michigan. D. Feldman and W. Collins acknowledge
support by the U.S. Department of Energy, Office of Science, Office of
Biological and Environmental Research, Terrestrial Ecosystem Science and
Atmospheric System Research programs, under award DE-ACO2-05CH11231. The
AIRS version 6 data sets were processed by and obtained from the Goddard
Earth Services Data and Information Services Center
(http://daac.gsfc.nasa.gov/). The MERRA data sets were processed by and
obtained from the NASA Goddard's Global Modeling and Assimilation Office
(GMAO). Copyright 2016. All rights reserved. Government sponsorship
acknowledged.
NR 43
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U1 6
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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 AUG 28
PY 2016
VL 43
IS 16
BP 8751
EP 8759
DI 10.1002/2016GL070263
PG 9
WC Geosciences, Multidisciplinary
SC Geology
GA DX5TC
UT WOS:000384443800050
ER
PT J
AU Wu, LH
Hasekamp, O
van Diedenhoven, B
Cairns, B
Yorks, JE
Chowdhary, J
AF Wu, Lianghai
Hasekamp, Otto
van Diedenhoven, Bastiaan
Cairns, Brian
Yorks, John E.
Chowdhary, Jacek
TI Passive remote sensing of aerosol layer height using near-UV multiangle
polarization measurements
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE aerosol layer height
ID RESEARCH SCANNING POLARIMETER; RADIATIVE-TRANSFER MODEL;
PHOTOPOLARIMETRIC MEASUREMENTS; SPECTRAL-RESOLUTION; OPTICAL-PROPERTIES;
RETRIEVAL; OCEAN; SENSITIVITY; LIDAR; BAND
AB We demonstrate that multiangle polarization measurements in the near-UV and blue part of the spectrum are very well suited for passive remote sensing of aerosol layer height. For this purpose we use simulated measurements with different setups (different wavelength ranges, with and without polarization, different polarimetric accuracies) as well as airborne measurements from the Research Scanning Polarimeter (RSP) obtained over the continental USA. We find good agreement of the retrieved aerosol layer height from RSP with measurements from the Cloud Physics Lidar showing a mean absolute difference of less than 1km. Furthermore, we found that the information on aerosol layer height is provided for large part by the multiangle polarization measurements with high accuracy rather than the multiangle intensity measurements. The information on aerosol layer height is significantly decreased when the shortest RSP wavelength (410nm) is excluded from the retrieval and is virtually absent when 550nm is used as shortest wavelength.
C1 [Wu, Lianghai; Hasekamp, Otto] SRON Netherlands Inst Space Res, Utrecht, Netherlands.
[van Diedenhoven, Bastiaan] Columbia Univ, Ctr Climate Syst Res, New York, NY USA.
[van Diedenhoven, Bastiaan; Cairns, Brian; Chowdhary, Jacek] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Yorks, John E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Chowdhary, Jacek] Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA.
RP Wu, LH (reprint author), SRON Netherlands Inst Space Res, Utrecht, Netherlands.
EM l.wu@sron.nl
FU NASA Radiation Sciences Program
FX The RSP data are available from NASA Goddard Institute for Space Studies
(http://data.giss.nasa.gov/pub/rsp/). The RSP data from the SEAC4RS and
PODEX field experiments that are used in this study were funded by the
NASA Radiation Sciences Program managed by Hal Maring and by the NASA
Earth Science Division as part of the preformulation study for the
Aerosol Cloud and ocean Ecosystem (ACE) mission. The CPL data are
provided by NASA Goddard Space Flight Center from the Web site at
http://cpl.gsfc.nasa.gov/.
NR 42
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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 AUG 28
PY 2016
VL 43
IS 16
BP 8783
EP 8790
DI 10.1002/2016GL069848
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA DX5TC
UT WOS:000384443800054
ER
PT J
AU Newman, PA
Coy, L
Pawson, S
Lait, LR
AF Newman, P. A.
Coy, L.
Pawson, S.
Lait, L. R.
TI The anomalous change in the QBO in 2015-2016
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
DE QBO
ID QUASI-BIENNIAL OSCILLATION; EQUATORIAL STRATOSPHERE;
GENERAL-CIRCULATION; WIND; MODEL
AB The quasi-biennial oscillation (QBO) is a tropical lower stratospheric, downward propagating zonal wind variation, with an average period of similar to 8months. The QBO has been constantly documented since 1953. Here we describe the evolution of the QBO during the Northern Hemisphere winter of 2015-2016 using radiosonde observations and meteorological reanalyses. Normally, the QBO would show a steady downward propagation of the westerly phase. In 2015-2016, there was an anomalous upward displacement of this westerly phase from similar to 30hPa to 15hPa. These westerlies impinge on or cutoff the normal downward propagation of the easterly phase. In addition, easterly winds develop at 40hPa. Comparisons to tropical wind statistics for the 1953 to present record demonstrate that this 2015-2016 QBO disruption is unprecedented.
C1 [Newman, P. A.; Coy, L.; Pawson, S.; Lait, L. R.] NASA, GSFC, Greenbelt, MD 20771 USA.
[Coy, L.] SSAI, Lanham, MD USA.
[Lait, L. R.] Morgan State Univ, Baltimore, MD 21239 USA.
RP Newman, PA (reprint author), NASA, GSFC, Greenbelt, MD 20771 USA.
EM paul.a.newman@nasa.gov
FU NASA Modeling, Analysis, and Prediction program; NASA Atmospheric
Composition Modeling and Analysis Program
FX The help of Eric R. Nash and Gerald Ziemke is greatly appreciated. This
research was performed with funding from the NASA Modeling, Analysis,
and Prediction program and the NASA Atmospheric Composition Modeling and
Analysis Program. The MERRA-2 reanalysis fields were obtained from the
NASA Earth Observing System Data and Information System
(https://earthdata.nasa.gov). The monthly mean QBO data for the
1953-1978 period were obtained from the Freie Universitat Berlin
(http://www.geo.fu-berlin.de/en/met/ag/strat/produkte/qbo/). Daily
global radiosondes have been collected at NASA/GSFC and are provided
from the Global Telecommunications System (available via the NOAA/NCEP
web site: ftp://ftp.cpc.ncep.noaa.gov/wd53rl/rsonde/).
NR 16
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U1 6
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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 AUG 28
PY 2016
VL 43
IS 16
BP 8791
EP 8797
DI 10.1002/2016GL070373
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA DX5TC
UT WOS:000384443800055
ER
PT J
AU Mackie, CJ
Candian, A
Huang, XC
Maltseva, E
Petrignani, A
Oomens, J
Mattioda, AL
Buma, WJ
Lee, TJ
Tielens, AGGM
AF Mackie, Cameron J.
Candian, Alessandra
Huang, Xinchuan
Maltseva, Elena
Petrignani, Annemieke
Oomens, Jos
Mattioda, Andrew L.
Buma, Wybren Jan
Lee, Timothy J.
Tielens, Alexander G. G. M.
TI The anharmonic quartic force field infrared spectra of five non-linear
polycyclic aromatic hydrocarbons: Benz[a]anthracene, chrysene,
phenanthrene, pyrene, and triphenylene
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
ID EMISSION FEATURES; SPECTROSCOPY; PAHS; MOLECULES; GRAPHENE; DATABASE;
RINGS; IONS
AB The study of interstellar polycyclic aromatic hydrocarbons (PAHs) relies heavily on theoretically predicted infrared spectra. Most earlier studies use scaled harmonic frequencies for band positions and the double harmonic approximation for intensities. However, recent high-resolution gas-phase experimental spectroscopic studies have shown that the harmonic approximation is not sufficient to reproduce experimental results. In our previous work, we presented the anharmonic theoretical spectra of three linear PAHs, showing the importance of including anharmonicities into the theoretical calculations. In this paper, we continue this work by extending the study to include five non-linear PAHs (benz[a]anthracene, chrysene, phenanthrene, pyrene, and triphenylene), thereby allowing us to make a full assessment of how edge structure, symmetry, and size influence the effects of anharmonicities. The theoretical anharmonic spectra are compared to spectra obtained under matrix isolation low-temperature conditions, low-resolution, high-temperature gas-phase conditions, and high-resolution, low-temperature gas-phase conditions. Overall, excellent agreement is observed between the theoretical and experimental spectra although the experimental spectra show subtle but significant differences. Published by AIP Publishing.
C1 [Mackie, Cameron J.; Candian, Alessandra; Petrignani, Annemieke; Tielens, Alexander G. G. M.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
[Huang, Xinchuan] SETI Inst, 189 Bernardo Ave,Suite 100, Mountain View, CA 94043 USA.
[Maltseva, Elena; Petrignani, Annemieke; Buma, Wybren Jan] Univ Amsterdam, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.
[Petrignani, Annemieke; Oomens, Jos] Radboud Univ Nijmegen, Toernooiveld 7, NL-6525 ED Nijmegen, Netherlands.
[Mattioda, Andrew L.; Lee, Timothy J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Mackie, CJ (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
EM mackie@strw.leidenuniv.nl
RI Buma, Wybren Jan/F-6691-2011; Lee, Timothy/K-2838-2012; HUANG,
XINCHUAN/A-3266-2013;
OI Buma, Wybren Jan/0000-0002-1265-8016; Petrignani,
Annemieke/0000-0002-6116-5867; Candian, Alessandra/0000-0002-5431-4449
FU Advanced European Research Council [246976]; Spinoza award; Dutch
Astrochemistry Network - Netherlands Organization for Scientific
Research, NWO; NWO Exacte Wetenschappen [MP-270-13, MP-264]; NWO
[639.041.543, 723.014.007]; NASA [12-APRA12-0107]; NASA/SETI
[NNX15AF45A]; National Aeronautics and Space Administration through the
NASA Astrobiology Institute through the Science Mission Directorate
[NNH13ZDA017C]
FX The authors would like to thank the two anonymous reviewers for their
helpful comments that improved the clarity of the manuscript. The
spectroscopic study of interstellar PAHs at Leiden Observatory has been
supported through the Advanced European Research Council Grant No.
246976, a Spinoza award, and through the Dutch Astrochemistry Network
funded by the Netherlands Organization for Scientific Research, NWO.
Computing time has been made available by NWO Exacte Wetenschappen
(Project Nos. MP-270-13 and MP-264) and calculations were performed at
the LISA Linux cluster of the SurfSARA supercomputer center in Almere,
The Netherlands. A.C. acknowledges NWO for a VENI grant (639.041.543).
A.P. acknowledges NWO for a VIDI grant (723.014.007). X.H. and T.J.L.
gratefully acknowledge support from the NASA 12-APRA12-0107 grant. X.H.
acknowledges the support from NASA/SETI Co-op Agreement NNX15AF45A. This
material is based upon work supported by the National Aeronautics and
Space Administration through the NASA Astrobiology Institute under
Cooperative Agreement Notice NNH13ZDA017C issued through the Science
Mission Directorate.
NR 44
TC 3
Z9 3
U1 17
U2 17
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 AUG 28
PY 2016
VL 145
IS 8
AR 084313
DI 10.1063/1.4961438
PG 10
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA DW8AL
UT WOS:000383875500034
PM 27586928
ER
PT J
AU Battaglia, A
Mroz, K
Lang, T
Tridon, F
Tanelli, S
Tian, L
Heymsfield, GM
AF Battaglia, A.
Mroz, K.
Lang, Tim
Tridon, F.
Tanelli, S.
Tian, Lin
Heymsfield, Gerald M.
TI Using a multiwavelength suite of microwave instruments to investigate
the microphysical structure of deep convective cores
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID DUAL-WAVELENGTH RADAR; HYDROMETEOR IDENTIFICATION ALGORITHM;
RAIN-PROFILING ALGORITHM; MULTIPLE-SCATTERING; PART II; PRECIPITATION
RETRIEVAL; LIQUID WATER; CLOUD; ATTENUATION; RADIOMETER
AB Due to the large natural variability of its microphysical properties, the characterization of solid precipitation is a longstanding problem. Since in situ observations are unavailable in severe convective systems, innovative remote sensing retrievals are needed to extend our understanding of such systems. This study presents a novel technique able to retrieve the density, mass, and effective diameter of graupel and hail in severe convection through the combination of airborne microwave remote sensing instruments. The retrieval is applied to measure solid precipitation properties within two convective cells observed on 23-24 May 2014 over North Carolina during the IPHEx campaign by the NASA ER-2 instrument suite. Between 30 and 40 degrees of freedom of signal are associated with the measurements, which is insufficient to provide full microphysics profiling. The measurements have the largest impact on the retrieval of ice particle sizes, followed by ice water contents. Ice densities are mainly driven by a priori assumptions, though low relative errors in ice densities suggest that in extensive regions of the convective system, only particles with densities larger than 0.4 g/cm(3) are compatible with the observations. This is in agreement with reports of large hail on the ground and with hydrometeor classification derived from ground-based polarimetric radars observations. This work confirms that multiple scattering generated by large ice hydrometeors in deep convection is relevant for airborne radar systems already at Ku band. A fortiori, multiple scattering will play a pivotal role in such conditions also for Ku band spaceborne radars (e.g., the GPM Dual Precipitation Radar).
C1 [Battaglia, A.; Mroz, K.] Univ Leicester, Natl Ctr Earth Observat, Leicester, Leics, England.
[Battaglia, A.; Tridon, F.] Univ Leicester, Dept Phys & Astron, Earth Observat Sci, Leicester, Leics, England.
[Lang, Tim] NASA Marshall Space Flight Ctr, Huntsville, AL USA.
[Tanelli, S.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Tian, Lin; Heymsfield, Gerald M.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
[Tian, Lin] Morgan State Univ, Goddard Earth Sci Technol & Res Program, Baltimore, MD 21239 USA.
RP Battaglia, A (reprint author), Univ Leicester, Natl Ctr Earth Observat, Leicester, Leics, England.; Battaglia, A (reprint author), Univ Leicester, Dept Phys & Astron, Earth Observat Sci, Leicester, Leics, England.
EM a.battaglia@leicester.ac.uk
RI Tridon, Frederic/M-4127-2013;
OI Tridon, Frederic/0000-0002-0436-283X; Battaglia,
Alessandro/0000-0001-9243-3484
FU project "Calibration and validation studies over the North Atlantic and
UK for the Global Precipitation Mission" - UK NERC [NE/L007169/1]; NASA
ACE Mission formulation; GPM Ground Validation; NASA Airborne Instrument
Technology Transition (AITT); ACE; GPM GV; NASA
FX The work done by A. Battaglia and F. Tridon was funded by the project
"Calibration and validation studies over the North Atlantic and UK for
the Global Precipitation Mission" funded by the UK NERC (NE/L007169/1).
The forward radar model code was courteously provided by R. Hogan
(http://www.met.rdg.ac.uk/clouds/multiscatter/). This research used the
ALICE High Performance Computing Facility at the University of
Leicester. CRS was supported by the NASA ACE Mission formulation. HIWRAP
was supported by GPM Ground Validation. EXRAD was supported by the NASA
Airborne Instrument Technology Transition (AITT). ER-2 flights were
jointly sponsored by GPM ground validation and the ACE Decadal Mission
study. AMPRs participation was supported by GPM GV. Timothy Lang was
supported by GPM GV. The work performed by Simone Tanelli was carried
out at the Jet Propulsion Laboratory, California Institute of Technology
under a contract with NASA in support to the preformulation phase
studies for the ACE mission concept and to the GPM Science Team. NEXRAD
data were obtained from NOAA via the online data set hosted by Amazon
Web Services. NEXRAD processing code is available from
https://github.com/ARM-DOE/pyart,
https://github.com/CSU-Radarmet/CSU_RadarTools, and
https://github.com/nasa/DualPol. AMPR processing code is available from
https://github.com/nasa/PyAMPR.
NR 62
TC 0
Z9 0
U1 7
U2 7
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 AUG 27
PY 2016
VL 121
IS 16
BP 9356
EP 9381
DI 10.1002/2016JD025269
PG 26
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DZ9OQ
UT WOS:000386207200006
PM 27708991
ER
PT J
AU Li, JLF
Wang, YH
Lee, T
Waliser, D
Lee, WL
Yu, JY
Chen, YC
Fetzer, E
Hasson, A
AF Li, J. -L. F.
Wang, Yi-Hui
Lee, Tong
Waliser, Duane
Lee, Wei-Liang
Yu, Jia-Yuh
Chen, Yi-Chun
Fetzer, Eric
Hasson, Audrey
TI The impacts of precipitating cloud radiative effects on ocean surface
evaporation, precipitation, and ocean salinity in coupled GCM
simulations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID GLOBAL WATER CYCLE; GENERAL-CIRCULATION MODEL; ABRUPT CLIMATE-CHANGE;
THERMOHALINE CIRCULATION; FLUX CORRECTION; PART I; CMIP3; VARIABILITY;
ARGO; INTENSIFICATION
AB The coupled global climate model (GCM) fidelity in representing upper ocean salinity including near sea surface bulk salinity (SSS) is evaluated in this study, with a focus on the Pacific Ocean. The systematic biases in ocean surface evaporation (E) minus precipitation (P) and SSS are found to be fairly similar in the twentieth century simulations of the Coupled Model Intercomparison Phase 3 (CMIP3) and Phase 5 (CMIP5) relative to the observations. One of the potential causes of the CMIP model biases is the missing representation of the radiative effects of precipitating hydrometeors (i.e., snow) in most CMIP models. To examine the radiative effect of cloud snow on SSS, sensitivity experiments with and without such effect are conducted by the National Center for Atmospheric Research-coupled Community Earth System Model (CESM). This study investigates the difference in SSS between sensitivity experiments and its relationship with atmospheric circulation, E - P and air-sea heat fluxes. It is found that the exclusion of the cloud snow radiative effect in CESM produces weaker Pacific trade winds, resulting in enhanced precipitation, reduced evaporation, and a reduction of the upper ocean salinity in the tropical and subtropical Pacific. The latter results in an improved comparison with climatological upper ocean bulk salinity. The introduction of cloud snow also altered the budget terms that maintain the time-mean salinity in the mixed layer.
C1 [Li, J. -L. F.; Wang, Yi-Hui; Lee, Tong; Waliser, Duane; Fetzer, Eric; Hasson, Audrey] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Li, J. -L. F.; Lee, Tong; Waliser, Duane; Fetzer, Eric] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
[Lee, Wei-Liang; Chen, Yi-Chun] Acad Sinica, Res Ctr Environm Change, Taipei, Taiwan.
[Yu, Jia-Yuh] Natl Cent Univ, Dept Atmospher Sci, Taoyuan, Taiwan.
RP Li, JLF (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.; Li, JLF (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
EM Juilin.F.Li@jpl.nasa.gov
FU Earth Science Program, the Modeling, Analysis, and Prediction (MAP)
[NNH12ZDA001N ROSES 2012]; ATMOS COMP [NNH12ZDA001N-CCST]; NDOA;
National Aeronautics and Space Administration (NASA); NASA Physical
Oceanography Program; NASA; Ministry of Science and Technology of Taiwan
[NSC100-2119-M-001-029-MY5, NSC102-2111-M-001-009]
FX We acknowledge PCMDI/DOE and the WCRP's WGCM for their roles in making
CMIP3/CMIP5 available. We thank Qing Yue and Graeme Stephens for their
useful comments. The contribution by J.L.L. and D.E.W. to this study
were carried out on behalf of the Jet Propulsion Laboratory, California
Institute of Technology, under contracts of NNH12ZDA001N ROSES 2012,
Earth Science Program, the Modeling, Analysis, and Prediction (MAP), and
ATMOS COMP 2013 (NNH12ZDA001N-CCST) and J.J.L. under NDOA with the
National Aeronautics and Space Administration (NASA) as well as T.L.
from NASA Physical Oceanography Program. This work has been supported in
part by the NASA Making Earth System Data Records for Use in Research
Environments (MEaSUREs) programs. W.L.L. was supported by Ministry of
Science and Technology of Taiwan under contracts
NSC100-2119-M-001-029-MY5 and NSC102-2111-M-001-009. The subsurface
ocean salinity data from the World Ocean Atlas 2009 (WOA09) is used in
this study and can be found in
http://www.nodc.noaa.gov/OC5/WOA09/pr_woa09.html. The long-term mean
evaporation is based on the Objectively Analyzed air-sea Fluxes (OAFlux)
product [Yu and Weller,]. The OAFlux project began in 1958, and its
utilization of satellite-based, high-resolution ocean surface vector
winds since July 1987 weights the long-term mean in favor of the late
twentieth century and can be found at http://oaflux.whoi.edu/. The
long-term mean precipitation is obtained from the Global Precipitation
Climatology Project (GPCP)
(http://www.esrl.noaa.gov/psd/data/gridded/data.gpcp.html).
NR 72
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 AUG 27
PY 2016
VL 121
IS 16
BP 9474
EP 9491
DI 10.1002/2016JD024911
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DZ9OQ
UT WOS:000386207200012
ER
PT J
AU Wen, GY
Marshak, A
Varnai, T
Levy, R
AF Wen, Guoyong
Marshak, Alexander
Varnai, Tamas
Levy, Robert
TI Testing the two-layer model for correcting near-cloud reflectance
enhancement using LES/SHDOM-simulated radiances
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID RADIATIVE-TRANSFER; CALIPSO OBSERVATIONS; AEROSOL PROPERTIES; BROKEN
CLOUDS; MODIS; PRODUCTS; VALIDATION; SCATTERING; SATELLITE; SURFACE
AB A transition zone exists between cloudy skies and clear sky; such that, clouds scatter solar radiation into clear-sky regions. From a satellite perspective, it appears that clouds enhance the radiation nearby. We seek a simple method to estimate this enhancement, since it is so computationally expensive to account for all three-dimensional (3-D) scattering processes. In previous studies, we developed a simple two-layer model (2LM) that estimated the radiation scattered via cloud-molecular interactions. Here we have developed a new model to account for cloud-surface interaction (CSI). We test the models by comparing to calculations provided by full 3-D radiative transfer simulations of realistic cloud scenes. For these scenes, the Moderate Resolution Imaging Spectroradiometer (MODIS)-like radiance fields were computed from the Spherical Harmonic Discrete Ordinate Method (SHDOM), based on a large number of cumulus fields simulated by the University of California, Los Angeles (UCLA) large eddy simulation (LES) model. We find that the original 2LM model that estimates cloud-air molecule interactions accounts for 64% of the total reflectance enhancement and the new model (2LM + CSI) that also includes cloud-surface interactions accounts for nearly 80%. We discuss the possibility of accounting for cloud-aerosol radiative interactions in 3-D cloud-induced reflectance enhancement, which may explain the remaining 20% of enhancements. Because these are simple models, these corrections can be applied to global satellite observations (e.g., MODIS) and help to reduce biases in aerosol and other clear-sky retrievals.
C1 [Wen, Guoyong; Marshak, Alexander; Varnai, Tamas; Levy, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Wen, Guoyong] Morgan State Univ, GESTAR, Baltimore, MD 21239 USA.
[Varnai, Tamas] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
RP Wen, GY (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.; Wen, GY (reprint author), Morgan State Univ, GESTAR, Baltimore, MD 21239 USA.
EM Guoyong.Wen-1@nasa.gov
RI Marshak, Alexander/D-5671-2012; Levy, Robert/M-7764-2013
OI Levy, Robert/0000-0002-8933-5303
FU NASA Radiation Program; NASA CALIPSO project; NASA Terra/Aqua projects
FX We gratefully acknowledge support for this research by the NASA
Radiation Program managed by Hal Maring, the NASA CALIPSO project
supervised by David Considine, and the NASA Terra/Aqua projects managed
by Paula Bontempi. We also thank Frank Evans for providing the results
of radiative transfer calculations for cumulus fields from Large-Eddy
Simulations.
NR 45
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 AUG 27
PY 2016
VL 121
IS 16
BP 9661
EP 9674
DI 10.1002/2016JD025021
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DZ9OQ
UT WOS:000386207200023
ER
PT J
AU Lang, TJ
Lyons, WA
Cummer, SA
Fuchs, BR
Dolan, B
Rutledge, SA
Krehbiel, P
Rison, W
Stanley, M
Ashcraft, T
AF Lang, Timothy J.
Lyons, Walter A.
Cummer, Steven A.
Fuchs, Brody R.
Dolan, Brenda
Rutledge, Steven A.
Krehbiel, Paul
Rison, William
Stanley, Mark
Ashcraft, Thomas
TI Observations of two sprite-producing storms in Colorado
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID CHARGE MOMENT CHANGES; SEVERE THUNDERSTORM ELECTRIFICATION; MESOSCALE
CONVECTIVE SYSTEMS; CONTINENTAL UNITED-STATES; LIGHTNING FLASH RATE;
PART II; PRECIPITATION; RADAR; STEPS; ELVES
AB Two sprite-producing thunderstorms were observed on 8 and 25 June 2012 in northeastern Colorado by a combination of low-light cameras, a lightning mapping array, polarimetric and Doppler radars, the National Lightning Detection Network, and charge moment change measurements. The 8 June event evolved from a tornadic hailstorm to a larger multicellular system that produced 21 observed positive sprites in 2 h. The majority of sprites occurred during a lull in convective strength, as measured by total flash rate, flash energy, and radar echo volume. Mean flash area spiked multiple times during this period; however, total flash rates still exceeded 60 min(-1), and portions of the storm featured a complex anomalous charge structure, with midlevel positive charge near -20 degrees C. The storm produced predominantly positive cloud-to-ground lightning. All sprite-parent flashes occurred on the northeastern flank of the storm, where strong westerly upper level flow was consistent with advection of charged precipitation away from convection, providing a pathway for stratiform lightning. The 25 June event was another multicellular hailstorm with an anomalous charge structure that produced 26 positive sprites in less than 1 h. The sprites again occurred during a convective lull, with relatively weaker reflectivity and lower total flash rate but relatively larger mean flash area. However, all sprite parents occurred in or near convection and tapped charge layers in adjacent anvil cloud. The results demonstrate the sprite production by convective ground strokes in anomalously charged storms and also indicate that sprite production and convective vigor are inversely related in mature storms.
C1 [Lang, Timothy J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Lyons, Walter A.] FMA Res Inc, Ft Collins, CO USA.
[Cummer, Steven A.] Duke Univ, Durham, NC USA.
[Fuchs, Brody R.; Dolan, Brenda; Rutledge, Steven A.] Colorado State Univ, Ft Collins, CO 80523 USA.
[Krehbiel, Paul; Rison, William; Stanley, Mark] New Mexico Inst Min & Technol, Socorro, NM 87801 USA.
[Ashcraft, Thomas] Heliotown Observ, Lamy, NM USA.
RP Lang, TJ (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM timothy.j.lang@nasa.gov
OI Fuchs, Brody/0000-0002-7629-0687
FU NASA; Defense Advanced Research Project Agency (DARPA); National Science
Foundation (NSF); NSF; National Oceanic and Atmospheric Administration
(NOAA)
FX Pat Kennedy, Dave Brunkow, Jim George, and Bob Bowie all contributed to
the CSU-CHILL and CSU-Pawnee radar scanning on the storm days analyzed
in this study, and thus, important data sets would not have been
available without their help. CSU radar data and COLMA data from DC3 are
available from the National Center for Atmospheric Research (NCAR;
http://data.eol.ucar.edu/master_list/?project=DC3). NEXRAD volumetric
radar data are available from Amazon Web Services
(https://aws.amazon.com/noaa-big-data/nexrad/), while MRMS data are
available from the National Severe Storms Laboratory
(http://www.nssl.noaa.gov/projects/mrms/). NLDN data are available from
the NASA Global Hydrology Resource Center
(https://ghrc.nsstc.nasa.gov/home/). Sounding data were obtained from
the University of Wyoming
(http://weather.uwyo.edu/upperair/sounding.html). Key open source
software packages used in this study include Py-ART
(http://arm-doe.github.io/pyart/), ARTview
(https://github.com/nguy/artview), lmatools
(https://github.com/deeplycloudy/lmatools), CSU_RadarTools
(https://github.com/CSU-Radarmet/CSU_RadarTools), DualPol
(https://github.com/nasa/DualPol), MMM-Py
(https://github.com/nasa/MMM-Py), SkewT
(https://pypi.python.org/pypi/SkewT), and SHARPpy
(http://sharppy.github.io/SHARPpy/). CEDRIC and SPRINT can be obtained
from NCAR (https://wiki.ucar.edu/display/raygridding/Home) along with
other useful radar software, such as Radx
(https://www.ral.ucar.edu/projects/titan/docs/radial_formats/radx.html).
Contact the first author (timothy.j.lang@nasa.gov) for access to other
data sets, such as sprite imagery and CMCN measurements. Lang also can
provide access to customized analysis software, such as CLEAR and XLMA.
Funding for this work was provided by the NASA Lightning Imaging Sensor
(LIS) project, the Defense Advanced Research Project Agency (DARPA)
Nimbus program, and the National Science Foundation (NSF) Physical
Meteorology and Lower Atmosphere Observing Facilities programs. DC3 was
made possible by the financial and logistical support of NSF, NASA, and
the National Oceanic and Atmospheric Administration (NOAA). The views,
opinions, and findings in this report are those of the authors and
should not be construed as an official NASA or U.S. Government position,
policy, or decision.
NR 85
TC 0
Z9 0
U1 7
U2 7
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 AUG 27
PY 2016
VL 121
IS 16
BP 9675
EP 9695
DI 10.1002/2016JD025299
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DZ9OQ
UT WOS:000386207200024
ER
PT J
AU Fast, JD
Berg, LK
Zhang, K
Easter, RC
Ferrare, RA
Hair, JW
Hostetler, CA
Liu, Y
Ortega, I
Sedlacek, A
Shilling, JE
Shrivastava, M
Springston, SR
Tomlinson, JM
Volkamer, R
Wilson, J
Zaveri, RA
Zelenyuk, A
AF Fast, Jerome D.
Berg, Larry K.
Zhang, Kai
Easter, Richard C.
Ferrare, Richard A.
Hair, Johnathan W.
Hostetler, Chris A.
Liu, Ying
Ortega, Ivan
Sedlacek, Arthur, III
Shilling, John E.
Shrivastava, Manish
Springston, Stephen R.
Tomlinson, Jason M.
Volkamer, Rainer
Wilson, Jacqueline
Zaveri, Rahul A.
Zelenyuk, Alla
TI Model representations of aerosol layers transported from North America
over the Atlantic Ocean during the Two-Column Aerosol Project
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID COMMUNITY ATMOSPHERE MODEL; PHASE FRAGMENTATION REACTIONS; CLOUD
MICROPHYSICS SCHEME; SPECTRAL-RESOLUTION LIDAR; CARBON VERTICAL
PROFILES; GLOBAL CLIMATE MODEL; LONG-RANGE TRANSPORT; LOW-VOLATILITY
SOA; BASIS-SET APPROACH; ORGANIC AEROSOL
AB The ability of the Weather Research and Forecasting model with chemistry (WRF-Chem) version 3.7 and the Community Atmosphere Model version 5.3 (CAM5) in simulating profiles of aerosol properties is quantified using extensive in situ and remote sensing measurements from the Two-Column Aerosol Project (TCAP) conducted during July of 2012. TCAP was supported by the U.S. Department of Energy's Atmospheric Radiation Measurement program and was designed to obtain observations within two atmospheric columns; one fixed over Cape Cod, Massachusetts, and the other several hundred kilometers over the ocean. The performance is quantified using most of the available aircraft and surface measurements during July, and 2 days are examined in more detail to identify the processes responsible for the observed aerosol layers. The higher-resolution WRF-Chem model produced more aerosol mass in the free troposphere than the coarser-resolution CAM5 model so that the fraction of aerosol optical thicknessabove the residual layer from WRF-Chem was more consistent with lidar measurements. We found that the free troposphere layers are likely due to mean vertical motions associated with synoptic-scale convergence that lifts aerosols from the boundary layer. The vertical displacement and the time period associated with upward transport in the troposphere depend on the strength of the synoptic system and whether relatively high boundary layer aerosol concentrations are present where convergence occurs. While a parameterization of subgrid scale convective clouds applied in WRF-Chem modulated the concentrations of aerosols aloft, it did not significantly change the overall altitude and depth of the layers.
C1 [Fast, Jerome D.; Berg, Larry K.; Zhang, Kai; Easter, Richard C.; Liu, Ying; Shilling, John E.; Shrivastava, Manish; Tomlinson, Jason M.; Wilson, Jacqueline; Zaveri, Rahul A.; Zelenyuk, Alla] Pacific Northwest Natl Lab, Richland, WA 99352 USA.
[Ferrare, Richard A.; Hair, Johnathan W.; Hostetler, Chris A.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Ortega, Ivan; Volkamer, Rainer] Univ Colorado, Dept Chem, Boulder, CO 80309 USA.
[Sedlacek, Arthur, III; Springston, Stephen R.] Brookhaven Natl Lab, Upton, NY 11973 USA.
RP Fast, JD (reprint author), Pacific Northwest Natl Lab, Richland, WA 99352 USA.
EM jerome.fast@pnl.gov
RI Zhang, Kai/F-8415-2010; Volkamer, Rainer/B-8925-2016
OI Zhang, Kai/0000-0003-0457-6368; Volkamer, Rainer/0000-0002-0899-1369
FU Office of Science of the U.S. Department of Energy; DOE ARM
[DE-SC0006730]; National Science Foundation; [DE-A06-76RLO976 1830]
FX This research was supported by the Office of Science of the U.S.
Department of Energy as part of the Atmospheric Radiation Measurement
(ARM) and Atmospheric System Research (ASR) programs. The Pacific
Northwest National Laboratory (PNNL) is operated by DOE by the Battelle
Memorial Institute under contract DE-A06-76RLO976 1830. We thank the
contributions of numerous individuals, including the G-1 flight crew (M.
Hubbell, W. Svancara, J. Hone, and E. Dukes), King Air flight crew (R.
Yasky, L. Kagey, M. Wusk, D. Bowser, S. Sims, D. Riddick, and G.
Slover), staff from the Cape Cod National Seashore (Superintendent G.
Price, L. McKean, C. Skowron, and B. Dougan), Cape Cod National Seashore
Atlantic Research and Learning Center, and the radiosonde launch team
from the Provincetown Center for Coastal Studies (M. Dunn, S. Greene, C.
Hudak, L. Ludwig, J. Melander, D. Minsky, K. Shorr, S. Sollog, D.
Towler, E. Larson, D. Dionne, C. Skowron). Support for the HSRL-2 flight
operations during TCAP was provided by the DOE ARM program, Interagency
Agreement DE-SC0006730, while support for the development of HSRL-2 was
provided by the NASA Science Mission Directorate, ESTO, AITT, and
Radiation Science Programs. The NOAA-MFRSR measurements were supported
by NOAA GOES-R Cal/Val Activities within NOAA's National Environmental
Satellite, Data, and Information Service. We thank Joseph Michalsky
(NOAA) for providing the AOD measurements from the MFRSR instrument,
Louisa Emmons (NCAR) for providing the MOZART global chemistry model
output, Christine Wiedinmyer (NCAR) for providing the fire emissions
inventory, Stuart McKeen (NOAA) for processing the 2011 NEI, Michael
Sprenger and Heini Wernli (ETH) for providing the Lagrangian Analysis
Tool LAGRANTO for the CAM5 back trajectory calculations, and Po-Lun Ma
(PNNL) for assisting with the set up of CAM5. The Environmental
Molecular Science Laboratory (EMSL), a DOE Office of Science User
Facility located at PNNL, provided computational resources for the
WRF-Chem simulations. For the CAM5 simulations, we would like to
acknowledge the computing support from Yellowstone (ark:/85065/d7wd3xhc)
provided by NCAR's Computational and Information Systems Laboratory
(sponsored by the National Science Foundation) and from the PNNL
Institutional Computing (PIC). Data used in this manuscript are
available from the ARM data archive (www.archive.arm.gov) or from the
corresponding author (jerome.fast@pnnl.gov).
NR 108
TC 1
Z9 1
U1 8
U2 8
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 AUG 27
PY 2016
VL 121
IS 16
BP 9814
EP 9848
DI 10.1002/2016JD025248
PG 35
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DZ9OQ
UT WOS:000386207200031
ER
PT J
AU Li, JY
Mao, JQ
Min, KE
Washenfelder, RA
Brown, SS
Kaiser, J
Keutsch, FN
Volkamer, R
Wolfe, GM
Hanisco, TF
Pollack, IB
Ryerson, TB
Graus, M
Gilman, JB
Lerner, BM
Warneke, C
de Gouw, JA
Middlebrook, AM
Liao, J
Welti, A
Henderson, BH
McNeill, VF
Hall, SR
Ullmann, K
Donner, LJ
Paulot, F
Horowitz, LW
AF Li, Jingyi
Mao, Jingqiu
Min, Kyung-Eun
Washenfelder, Rebecca A.
Brown, Steven S.
Kaiser, Jennifer
Keutsch, Frank N.
Volkamer, Rainer
Wolfe, Glenn M.
Hanisco, Thomas F.
Pollack, Ilana B.
Ryerson, Thomas B.
Graus, Martin
Gilman, Jessica B.
Lerner, Brian M.
Warneke, Carsten
de Gouw, Joost A.
Middlebrook, Ann M.
Liao, Jin
Welti, Andre
Henderson, Barron H.
McNeill, V. Faye
Hall, Samuel R.
Ullmann, Kirk
Donner, Leo J.
Paulot, Fabien
Horowitz, Larry W.
TI Observational constraints on glyoxal production from isoprene oxidation
and its contribution to organic aerosol over the Southeast United States
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID RADICAL-INITIATED OXIDATION; MASTER CHEMICAL MECHANISM; METHYL VINYL
KETONE; GAS-PHASE; ATMOSPHERIC CHEMISTRY; TROPOSPHERIC DEGRADATION;
HETEROGENEOUS CHEMISTRY; AIRCRAFT MEASUREMENTS; PARTICULATE MATTER;
PEROXY-RADICALS
AB We use a 0-D photochemical box model and a 3-D global chemistry-climate model, combined with observations from the NOAA Southeast Nexus (SENEX) aircraft campaign, to understand the sources and sinks of glyoxal over the Southeast United States. Box model simulations suggest a large difference in glyoxal production among three isoprene oxidation mechanisms (AM3ST, AM3B, and Master Chemical Mechanism (MCM) v3.3.1). These mechanisms are then implemented into a 3-D global chemistry-climate model. Comparison with field observations shows that the average vertical profile of glyoxal is best reproduced by AM3ST with an effective reactive uptake coefficient.glyx of 2 x 10(-3) and AM3B without heterogeneous loss of glyoxal. The two mechanisms lead to 0-0.8 mu gm(-3) secondary organic aerosol (SOA) from glyoxal in the boundary layer of the Southeast U.S. in summer. We consider this to be the lower limit for the contribution of glyoxal to SOA, as other sources of glyoxal other than isoprene are not included in our model. In addition, we find that AM3B shows better agreement on both formaldehyde and the correlation between glyoxal and formaldehyde (RGF = [GLYX]/[HCHO]), resulting from the suppression of d-isoprene peroxy radicals. We also find that MCM v3.3.1 may underestimate glyoxal production from isoprene oxidation, in part due to an underestimated yield from the reaction of isoprene epoxydiol (IEPOX) peroxy radicals with HO2. Our work highlights that the gas-phase production of glyoxal represents a large uncertainty in quantifying its contribution to SOA.
C1 [Li, Jingyi; Mao, Jingqiu; Paulot, Fabien] Princeton Univ, Program Atmospher & Ocean Sci, Princeton, NJ 08544 USA.
[Mao, Jingqiu; Donner, Leo J.; Paulot, Fabien; Horowitz, Larry W.] NOAA, Geophys Fluid Dynam Lab, Princeton, NJ 08540 USA.
[Min, Kyung-Eun; Washenfelder, Rebecca A.; Brown, Steven S.; Pollack, Ilana B.; Ryerson, Thomas B.; Graus, Martin; Gilman, Jessica B.; Lerner, Brian M.; Warneke, Carsten; de Gouw, Joost A.; Middlebrook, Ann M.; Liao, Jin; Welti, Andre] NOAA, Div Chem Sci, Earth Syst Res Lab, Boulder, CO USA.
[Min, Kyung-Eun; Washenfelder, Rebecca A.; Volkamer, Rainer; Pollack, Ilana B.; Graus, Martin; Gilman, Jessica B.; Lerner, Brian M.; Warneke, Carsten; de Gouw, Joost A.; Liao, Jin; Welti, Andre] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Min, Kyung-Eun] Gwangju Inst Sci & Technol, Sch Environm Sci & Engn, Gwangju, South Korea.
[Brown, Steven S.; Volkamer, Rainer] Univ Colorado, Dept Chem & Biochem, Campus Box 215, Boulder, CO 80309 USA.
[Kaiser, Jennifer; Keutsch, Frank N.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Keutsch, Frank N.] Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA.
[Wolfe, Glenn M.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Wolfe, Glenn M.; Hanisco, Thomas F.] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Lab, Greenbelt, MD USA.
[Pollack, Ilana B.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Graus, Martin] Univ Innsbruck, Inst Atmospher & Cryospher Sci, Innsbruck, Austria.
[Welti, Andre] Leibniz Inst Tropospher Res, Leipzig, Germany.
[Henderson, Barron H.] Univ Florida, Dept Environm Engn Sci, Engn Sch Sustainable Infrastruct & Environm, Gainesville, FL 32611 USA.
[McNeill, V. Faye] Columbia Univ, Dept Chem Engn, New York, NY USA.
[Hall, Samuel R.; Ullmann, Kirk] Natl Ctr Atmospher Res, Atmospher Chem Observat & Modeling Lab, POB 3000, Boulder, CO 80307 USA.
RP Mao, JQ (reprint author), Princeton Univ, Program Atmospher & Ocean Sci, Princeton, NJ 08544 USA.; Mao, JQ (reprint author), NOAA, Geophys Fluid Dynam Lab, Princeton, NJ 08540 USA.
EM Jingqiu.Mao@noaa.gov
RI Volkamer, Rainer/B-8925-2016; Graus, Martin/E-7546-2010; Mao,
Jingqiu/F-2511-2010; de Gouw, Joost/A-9675-2008; Gilman,
Jessica/E-7751-2010; Pollack, Ilana/F-9875-2012; Washenfelder,
Rebecca/E-7169-2010; Middlebrook, Ann/E-4831-2011; Wolfe,
Glenn/D-5289-2011; Brown, Steven/I-1762-2013; Manager, CSD
Publications/B-2789-2015
OI Volkamer, Rainer/0000-0002-0899-1369; Graus, Martin/0000-0002-2025-9242;
Mao, Jingqiu/0000-0002-4774-9751; de Gouw, Joost/0000-0002-0385-1826;
Gilman, Jessica/0000-0002-7899-9948; Washenfelder,
Rebecca/0000-0002-8106-3702; Middlebrook, Ann/0000-0002-2984-6304;
FU NOAA Climate Program Office [NA13OAR4310071, NA14OAR4320106]; NOAA
Atmospheric Chemistry, Climate, and Carbon Cycle (AC4) program; EPA
[83540601]; NASA [NNH10ZDA001N-SEAC4RS]; NASA Headquarters under the
NASA Earth and Space Science Fellowship Program [NNX14AK97H]; NSF EAGER
[AGS-1452317]; NSF [AGS-1546136]
FX The authors thank Charles A. Brock (NOAA) for providing the aerosol size
data, Vaishali Naik (UCAR/NOAA) for providing the emission inventories
from the SENEX campaign, and William Cooke for the help with convection
scheme of the AM3 model. J.L., J.M., and L.W.H. acknowledge supports by
the NOAA Climate Program Office grant NA13OAR4310071 and NA14OAR4320106.
K.E.M., R.A.W., and S.S.B. acknowledge the support from the NOAA
Atmospheric Chemistry, Climate, and Carbon Cycle (AC4) program. J.K.,
F.N.K., G.M.W., and T.F.H. are grateful for the support from EPA Science
to Achieve Results program grant 83540601 and NASA grant
NNH10ZDA001N-SEAC4RS. J. Kaiser acknowledges support from NASA
Headquarters under the NASA Earth and Space Science Fellowship Program
grant NNX14AK97H. R.V. is grateful for the support from NSF EAGER award
AGS-1452317. V.F.M. acknowledges support from NSF (AGS-1546136). We
thank the staff at the NOAA Aircraft Operations Center and the WP-3D
flight crew for their help in instrumenting the aircraft and for
conducting the flights. Special thanks go to Songmiao Fan (NOAA) for the
helpful discussions. This research has not been subjected to any EPA
review and therefore does not necessarily reflect the views of the
agency, and no official endorsement should be inferred. Observational
data sets and modeling results are available upon request to the
corresponding author (Jingqiu.Mao@noaa.gov).
NR 92
TC 0
Z9 0
U1 19
U2 19
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 AUG 27
PY 2016
VL 121
IS 16
BP 9849
EP 9861
DI 10.1002/2016JD025331
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DZ9OQ
UT WOS:000386207200032
ER
PT J
AU Ware, J
Kort, EA
DeCola, P
Duren, R
AF Ware, John
Kort, Eric A.
DeCola, Phil
Duren, Riley
TI Aerosol lidar observations of atmospheric mixing in Los Angeles:
Climatology and implications for greenhouse gas observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID BOUNDARY-LAYER HEIGHT; AIR-POLLUTANT TRANSPORT; FIELD-OF-VIEW; CO2
EMISSIONS; COASTAL ENVIRONMENT; SIMULATIONS; BACKSCATTER; DEPENDENCE;
SYSTEM; DEPTH
AB Atmospheric observations of greenhouse gases provide essential information on sources and sinks of these key atmospheric constituents. To quantify fluxes from atmospheric observations, representation of transport-especially vertical mixing-is a necessity and often a source of error. We report on remotely sensed profiles of vertical aerosol distribution taken over a 2 year period in Pasadena, California. Using an automated analysis system, we estimate daytime mixing layer depth, achieving high confidence in the afternoon maximum on 51% of days with profiles from a Sigma Space Mini Micropulse LiDAR (MiniMPL) and on 36% of days with a Vaisala CL51 ceilometer. We note that considering ceilometer data on a logarithmic scale, a standard method, introduces, an offset in mixing height retrievals. The mean afternoon maximum mixing height is 770 m Above Ground Level in summer and 670 m in winter, with significant day-to-day variance (within season sigma = 220 m approximate to 30%). Taking advantage of the MiniMPL's portability, we demonstrate the feasibility of measuring the detailed horizontal structure of the mixing layer by automobile. We compare our observations to planetary boundary layer (PBL) heights from sonde launches, North American regional reanalysis (NARR), and a custom Weather Research and Forecasting (WRF) model developed for greenhouse gas (GHG) monitoring in Los Angeles. NARR and WRF PBL heights at Pasadena are both systematically higher than measured, NARR by 2.5 times; these biases will cause proportional errors in GHG flux estimates using modeled transport. We discuss how sustained lidar observations can be used to reduce flux inversion error by selecting suitable analysis periods, calibrating models, or characterizing bias for correction in post processing.
C1 [Ware, John] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Ware, John; Kort, Eric A.] Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
[DeCola, Phil] Sigma Space Corp, Lanham, MD USA.
[Duren, Riley] NASA, Jet Prop Lab, Pasadena, CA USA.
RP Ware, J (reprint author), Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.; Ware, J (reprint author), Univ Michigan, Dept Climate & Space Sci & Engn, Ann Arbor, MI 48109 USA.
EM johnware@umich.edu
RI Kort, Eric/F-9942-2012
OI Kort, Eric/0000-0003-4940-7541
FU NASA [NNN12AA01C]; NASA
FX This work was supported by NASA under grant NNN12AA01C. Portions of this
work were performed at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with NASA. We thank Taylor Jones
for assistance in setting up and operating the MiniMPL instrument and
Athena Sparks for help with data preprocessing. We thank Vineet Yadav
for generating and providing WRF model output. NARR data provided by the
NOAA/OAR/ESRL PSD, Boulder, Colorado, USA, from their Web site at
http://www.esrl.noaa.gov/psd/. The authors would also like to thank the
Megacities Carbon Project team for useful discussion and feedback.
Mixing depth data will be available through the Megacities Carbon
Project portal at https://megacities.jpl.nasa.gov. To obtain a copy of
the analysis system used to generate the estimates, please contact the
authors at johnware@umich.edu.
NR 50
TC 0
Z9 0
U1 6
U2 6
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 AUG 27
PY 2016
VL 121
IS 16
BP 9862
EP 9878
DI 10.1002/2016JD024953
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DZ9OQ
UT WOS:000386207200033
PM 27867786
ER
PT J
AU Mezuman, K
Bauer, SE
Tsigaridis, K
AF Mezuman, Keren
Bauer, Susanne E.
Tsigaridis, Kostas
TI Evaluating secondary inorganic aerosols in three dimensions
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID GENERAL-CIRCULATION MODEL; AQUEOUS-PHASE-TRANSITIONS; TROPOSPHERIC
OZONE; GODDARD-INSTITUTE; ATMOSPHERIC AEROSOLS; AMMONIUM-NITRATE;
UNITED-STATES; GLOBAL-MODEL; MINERAL DUST; EMISSIONS
AB The spatial distribution of aerosols and their chemical composition dictates whether aerosols have a cooling or a warming effect on the climate system. Hence, properly modeling the three-dimensional distribution of aerosols is a crucial step for coherent climate simulations. Since surface measurement networks only give 2-D data, and most satellites supply integrated column information, it is thus important to integrate aircraft measurements in climate model evaluations. In this study, the vertical distribution of secondary inorganic aerosol (i.e., sulfate, ammonium, and nitrate) is evaluated against a collection of 14 AMS flight campaigns and surface measurements from 2000 to 2010 in the USA and Europe. GISS ModelE2 is used with multiple aerosol microphysics (MATRIX, OMA) and thermodynamic (ISOR-ROPIA II, EQSAM) configurations. Our results show that the MATRIX microphysical scheme improves the model performance for sulfate, but that there is a systematic underestimation of ammonium and nitrate over the USA and Europe in all model configurations. In terms of gaseous precursors, nitric acid concentrations are largely underestimated at the surface while overestimated in the higher levels of the model. Heterogeneous reactions on dust surfaces are an important sink for nitric acid, even high in the troposphere. At high altitudes, nitrate formation is calculated to be ammonia limited. The underestimation of ammonium and nitrate in polluted regions is most likely caused by a too simplified treatment of the NH3 / NH4+ partitioning which affects the HNO3 / NO3- partitioning.
C1 [Mezuman, Keren] Columbia Univ, Earth & Environm Sci, New York, NY USA.
[Mezuman, Keren; Bauer, Susanne E.; Tsigaridis, Kostas] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Bauer, Susanne E.; Tsigaridis, Kostas] Columbia Univ, Ctr Climate Syst Res, New York, NY 10027 USA.
RP Bauer, SE (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.; Bauer, SE (reprint author), Columbia Univ, Ctr Climate Syst Res, New York, NY 10027 USA.
EM susanne.bauer@columbia.edu
FU NASA; NASA High-End Computing (HEC) Program through NASA Center for
Climate Simulation (NCCS) at Goddard Space Flight Center; NASA's
Atmospheric Composition Modeling and Analysis Program (ACMAP)
[NNX15AE36G]
FX Climate modeling at GISS is supported by the NASA Modeling, Analysis,
and Prediction program. 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. SEB and KT
acknowledge funding from NASA's Atmospheric Composition Modeling and
Analysis Program (ACMAP), contract number NNX15AE36G. We acknowledge the
IMPROVE monitoring program for providing data. EMEP measurement data
were extracted from the EBAS database, which is maintained and further
developed by the Norwegian Institute for Air Research (NILU). We
acknowledge the Toolsets for Airborne Data (TAD)
website:https://tad.larc.nasa.gov, as well as the site
https://sites.google.com/site/amsglobaldatabase/ maintained by the Zhang
and Jimenez groups.
NR 70
TC 1
Z9 1
U1 15
U2 15
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 AUG 26
PY 2016
VL 16
IS 16
BP 10651
EP 10669
DI 10.5194/acp-16-10651-2016
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW6EW
UT WOS:000383743200002
ER
PT J
AU Adams, C
Normand, EN
McLinden, CA
Bourassa, AE
Lloyd, ND
Degenstein, DA
Krotkov, NA
Rivas, MB
Boersma, KF
Eskes, H
AF Adams, Cristen
Normand, Elise N.
McLinden, Chris A.
Bourassa, Adam E.
Lloyd, Nicholas D.
Degenstein, Douglas A.
Krotkov, Nickolay A.
Rivas, Maria Belmonte
Boersma, K. Folkert
Eskes, Henk
TI Limb-nadir matching using non-coincident NO2 observations: proof of
concept and the OMI-minus-OSIRIS prototype product
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID OZONE MONITORING INSTRUMENT; TROPOSPHERIC NO2; NITROGEN-DIOXIDE;
STRATOSPHERIC OZONE; RETRIEVAL ALGORITHM; MIDDLE ATMOSPHERE; COLUMN
RETRIEVAL; SCIAMACHY; SATELLITE; MISSION
AB A variant of the limb-nadir matching technique for deriving tropospheric NO2 columns is presented in which the stratospheric component of the NO2 slant column density (SCD) measured by the Ozone Monitoring Instrument (OMI) is removed using non-coincident profiles from the Optical Spectrograph and InfraRed Imaging System (OSIRIS). In order to correct their mismatch in local time and the diurnal variation of stratospheric NO2 OSIRIS profiles, which were measured just after sunrise, were mapped to the local time of OMI observations using a photochemical box model. Following the profile time adjustment, OSIRIS NO2 stratospheric vertical column densities (VCDs) were calculated. For profiles that did not reach down to the tropopause, VCDs were adjusted using the photochemical model. Using air mass factors from the OMI Standard Product (SP), a new tropospheric NO2 VCD product -referred to as OMI-minus-OSIRIS (OmO) - was generated through limb-nadir matching. To accomplish this, the OMI total SCDs were scaled using correction factors derived from the next-generation SCDs that improve upon the spectral fitting used for the current operational products. One year, 2008, of OmO was generated for 60 degrees S to 60 degrees N and a cursory evaluation was performed. The OmO product was found to capture the main features of tropospheric NO2, including a background value of about 0.3 x 10(15) molecules cm(-2) over the tropical Pacific and values comparable to the OMI operational products over anthropogenic source areas. While additional study is required, these results suggest that a limb-nadir matching approach is feasible for the removal of stratospheric NO2 measured by a polar orbiter from a nadir-viewing instrument in a geostationary orbit such as Tropospheric Emissions: Monitoring of Pollution (TEMPO) or Sentinel-4.
C1 [Adams, Cristen; Normand, Elise N.; Bourassa, Adam E.; Lloyd, Nicholas D.; Degenstein, Douglas A.] Univ Saskatchewan, Inst Space & Atmospher Studies, Saskatoon, SK, Canada.
[Adams, Cristen] Alberta Environm & Pk, Alberta Environm Monitoring & Sci Div, Edmonton, AB, Canada.
[McLinden, Chris A.] Environm Canada, Air Qual Res Div, Toronto, ON, Canada.
[Krotkov, Nickolay A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Rivas, Maria Belmonte; Boersma, K. Folkert; Eskes, Henk] Royal Netherlands Meteorol Inst KNMI, De Bilt, Netherlands.
[Boersma, K. Folkert] Wageningen Univ, Meteorol & Air Qual Grp, Wageningen, Netherlands.
RP Adams, C (reprint author), Univ Saskatchewan, Inst Space & Atmospher Studies, Saskatoon, SK, Canada.; Adams, C (reprint author), Alberta Environm & Pk, Alberta Environm Monitoring & Sci Div, Edmonton, AB, Canada.
EM cristenlfadams@gmail.com
RI Boersma, Klaas/H-4559-2012
OI Boersma, Klaas/0000-0002-4591-7635
FU Natural Sciences and Engineering Research Council (Canada); Canadian
Space Agency; Sweden (SNSB); Canada (CSA); France (CNES); Finland
(Tekes)
FX This work was supported by the Natural Sciences and Engineering Research
Council (Canada) and the Canadian Space Agency. Odin is a Swedish-led
satellite project funded jointly by Sweden (SNSB), Canada (CSA), France
(CNES), and Finland (Tekes). The authors thank David Plummer for the
provision of climatological fields from the Canadian Middle Atmosphere
Model. Thanks to Sergey Marchenko for providing the OMI SCD bias
correction factors. Thank you also to Chris Roth for help with the
OSIRIS database.
NR 56
TC 1
Z9 1
U1 3
U2 3
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 AUG 26
PY 2016
VL 9
IS 8
BP 4103
EP 4122
DI 10.5194/amt-9-4103-2016
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW7PH
UT WOS:000383842900001
ER
PT J
AU Aguilar, M
Alpat, B
Alpat, B
Ambrosi, G
Arruda, L
Attig, N
Aupetit, S
Azzarello, P
Bachlechner, A
Barao, F
Barrau, A
Barrin, L
Bartoloni, A
Basara, L
Basegmez-du Pree, S
Battarbee, M
Battiston, R
Bazo, J
Becker, U
Behlmann, M
Beischer, B
Berdugo, J
Bertucci, B
Bindi, V
Boella, G
de Boer, W
Bollweg, K
Bonnivard, V
Borgia, B
Boschini, MJ
Bourquin, M
Bueno, EF
Burger, J
Cadoux, F
Cai, XD
Capell, M
Caroff, S
Casaus, J
Castellini, G
Cernuda, I
Cervelli, F
Chae, MJ
Chang, YH
Chen, AI
Chen, GM
Chen, HS
Cheng, L
Chou, HY
Choumilov, E
Choutko, V
Chung, CH
Clark, C
Clavero, R
Coignet, G
Consolandi, C
Contin, A
Corti, C
Coste, B
Creus, W
Crispoltoni, M
Cui, Z
Dai, YM
Delgado, C
Della Torre, S
Demirkoz, MB
Derome, L
Di Falco, S
Dimiccoli, F
Diaz, C
von Doetinchem, P
Dong, F
Donnini, F
Duranti, M
D'Urso, D
Egorov, A
Eline, A
Eronen, T
Feng, J
Fiandrini, E
Finch, E
Fisher, P
Formato, V
Galaktionov, Y
Gallucci, G
Garcia, B
Garcia-Lopez, RJ
Gargiulo, C
Gast, H
Gebauer, I
Gervasi, M
Ghelfi, A
Giovacchini, F
Goglov, P
Gomez-Coral, DM
Gong, J
Goy, C
Grabski, V
Grandi, D
Graziani, M
Guerri, I
Guo, KH
Habiby, M
Haino, S
Han, KC
He, ZH
Heil, M
Hoffman, J
Hsieh, TH
Huang, H
Huang, ZC
Huh, C
Incagli, M
Ionica, M
Jang, WY
Jinchi, H
Kang, SC
Kanishev, K
Kim, GN
Kim, KS
Kirn, T
Konak, C
Kounina, O
Kounine, A
Koutsenko, V
Krafczyk, MS
La Vacca, G
Laudi, E
Laurenti, G
Lazzizzera, I
Lebedev, A
Lee, HT
Lee, SC
Leluc, C
Li, HS
Li, JQ
Li, JQ
Li, Q
Li, TX
Li, W
Li, ZH
Li, ZY
Lim, S
Lin, CH
Lipari, P
Lippert, T
Liu, D
Liu, H
Lu, SQ
Lu, YS
Luebelsmeyer, K
Luo, F
Luo, JZ
Lv, SS
Majka, R
Mana, C
Marin, J
Martin, T
Martinez, G
Masi, N
Maurin, D
Menchaca-Rocha, A
Meng, Q
Mo, DC
Morescalchi, L
Mott, P
Nelson, T
Ni, JQ
Nikonov, N
Nozzoli, F
Nunes, P
Oliva, A
Orcinha, M
Palmonari, F
Palomares, C
Paniccia, M
Pauluzzi, M
Pensotti, S
Pereira, R
Picot-Clemente, N
Pilo, F
Pizzolotto, C
Plyaskin, V
Pohl, M
Poireau, V
Putze, A
Quadrani, L
Qi, XM
Qin, X
Qu, ZY
Raiha, T
Rancoita, PG
Rapin, D
Ricol, JS
Rodriguez, I
Rosier-Lees, S
Rozhkov, A
Rozza, D
Sagdeev, R
Sandweiss, J
Saouter, P
Schael, S
Schmidt, SM
von Dratzig, AS
Schwering, G
Seo, ES
Shan, BS
Shi, JY
Siedenburg, T
Son, D
Song, JW
Sun, WH
Tacconi, M
Tang, XW
Tang, ZC
Tao, L
Tescaro, D
Ting, SCC
Ting, SM
Tomassetti, N
Torsti, J
Turkoglu, C
Urban, T
Vagelli, V
Valente, E
Vannini, C
Valtonen, E
Acosta, MV
Vecchi, M
Velasco, M
Vialle, JP
Vitale, V
Vitillo, S
Wang, LQ
Wang, NH
Wang, QL
Wang, X
Wang, XQ
Wang, ZX
Wei, CC
Weng, ZL
Whitman, K
Wienkenhover, J
Willenbrock, M
Wu, H
Wu, X
Xia, X
Xiong, RQ
Xu, W
Yan, Q
Yang, J
Yang, M
Yang, Y
Yi, H
Yu, YJ
Yu, ZQ
Zeissler, S
Zhang, C
Zhang, J
Zhang, JH
Zhang, SD
Zhang, SW
Zhang, Z
Zheng, ZM
Zhu, ZQ
Zhuang, HL
Zhukov, V
Zichichi, A
Zimmermann, N
Zuccon, P
AF Aguilar, M.
Alpat, B.
Alpat, B.
Ambrosi, G.
Arruda, L.
Attig, N.
Aupetit, S.
Azzarello, P.
Bachlechner, A.
Barao, F.
Barrau, A.
Barrin, L.
Bartoloni, A.
Basara, L.
Basegmez-du Pree, S.
Battarbee, M.
Battiston, R.
Bazo, J.
Becker, U.
Behlmann, M.
Beischer, B.
Berdugo, J.
Bertucci, B.
Bindi, V.
Boella, G.
de Boer, W.
Bollweg, K.
Bonnivard, V.
Borgia, B.
Boschini, M. J.
Bourquin, M.
Bueno, E. F.
Burger, J.
Cadoux, F.
Cai, X. D.
Capell, M.
Caroff, S.
Casaus, J.
Castellini, G.
Cernuda, I.
Cervelli, F.
Chae, M. J.
Chang, Y. H.
Chen, A. I.
Chen, G. M.
Chen, H. S.
Cheng, L.
Chou, H. Y.
Choumilov, E.
Choutko, V.
Chung, C. H.
Clark, C.
Clavero, R.
Coignet, G.
Consolandi, C.
Contin, A.
Corti, C.
Coste, B.
Creus, W.
Crispoltoni, M.
Cui, Z.
Dai, Y. M.
Delgado, C.
Della Torre, S.
Demirkoz, M. B.
Derome, L.
Di Falco, S.
Dimiccoli, F.
Diaz, C.
von Doetinchem, P.
Dong, F.
Donnini, F.
Duranti, M.
D'Urso, D.
Egorov, A.
Eline, A.
Eronen, T.
Feng, J.
Fiandrini, E.
Finch, E.
Fisher, P.
Formato, V.
Galaktionov, Y.
Gallucci, G.
Garcia, B.
Garcia-Lopez, R. J.
Gargiulo, C.
Gast, H.
Gebauer, I.
Gervasi, M.
Ghelfi, A.
Giovacchini, F.
Goglov, P.
Gomez-Coral, D. M.
Gong, J.
Goy, C.
Grabski, V.
Grandi, D.
Graziani, M.
Guerri, I.
Guo, K. H.
Habiby, M.
Haino, S.
Han, K. C.
He, Z. H.
Heil, M.
Hoffman, J.
Hsieh, T. H.
Huang, H.
Huang, Z. C.
Huh, C.
Incagli, M.
Ionica, M.
Jang, W. Y.
Jinchi, H.
Kang, S. C.
Kanishev, K.
Kim, G. N.
Kim, K. S.
Kirn, Th.
Konak, C.
Kounina, O.
Kounine, A.
Koutsenko, V.
Krafczyk, M. S.
La Vacca, G.
Laudi, E.
Laurenti, G.
Lazzizzera, I.
Lebedev, A.
Lee, H. T.
Lee, S. C.
Leluc, C.
Li, H. S.
Li, J. Q.
Li, J. Q.
Li, Q.
Li, T. X.
Li, W.
Li, Z. H.
Li, Z. Y.
Lim, S.
Lin, C. H.
Lipari, P.
Lippert, T.
Liu, D.
Liu, Hu
Lu, S. Q.
Lu, Y. S.
Luebelsmeyer, K.
Luo, F.
Luo, J. Z.
Lv, S. S.
Majka, R.
Mana, C.
Marin, J.
Martin, T.
Martinez, G.
Masi, N.
Maurin, D.
Menchaca-Rocha, A.
Meng, Q.
Mo, D. C.
Morescalchi, L.
Mott, P.
Nelson, T.
Ni, J. Q.
Nikonov, N.
Nozzoli, F.
Nunes, P.
Oliva, A.
Orcinha, M.
Palmonari, F.
Palomares, C.
Paniccia, M.
Pauluzzi, M.
Pensotti, S.
Pereira, R.
Picot-Clemente, N.
Pilo, F.
Pizzolotto, C.
Plyaskin, V.
Pohl, M.
Poireau, V.
Putze, A.
Quadrani, L.
Qi, X. M.
Qin, X.
Qu, Z. Y.
Raiha, T.
Rancoita, P. G.
Rapin, D.
Ricol, J. S.
Rodriguez, I.
Rosier-Lees, S.
Rozhkov, A.
Rozza, D.
Sagdeev, R.
Sandweiss, J.
Saouter, P.
Schael, S.
Schmidt, S. M.
von Dratzig, A. Schulz
Schwering, G.
Seo, E. S.
Shan, B. S.
Shi, J. Y.
Siedenburg, T.
Son, D.
Song, J. W.
Sun, W. H.
Tacconi, M.
Tang, X. W.
Tang, Z. C.
Tao, L.
Tescaro, D.
Ting, Samuel C. C.
Ting, S. M.
Tomassetti, N.
Torsti, J.
Turkoglu, C.
Urban, T.
Vagelli, V.
Valente, E.
Vannini, C.
Valtonen, E.
Acosta, M. Vazquez
Vecchi, M.
Velasco, M.
Vialle, J. P.
Vitale, V.
Vitillo, S.
Wang, L. Q.
Wang, N. H.
Wang, Q. L.
Wang, X.
Wang, X. Q.
Wang, Z. X.
Wei, C. C.
Weng, Z. L.
Whitman, K.
Wienkenhover, J.
Willenbrock, M.
Wu, H.
Wu, X.
Xia, X.
Xiong, R. Q.
Xu, W.
Yan, Q.
Yang, J.
Yang, M.
Yang, Y.
Yi, H.
Yu, Y. J.
Yu, Z. Q.
Zeissler, S.
Zhang, C.
Zhang, J.
Zhang, J. H.
Zhang, S. D.
Zhang, S. W.
Zhang, Z.
Zheng, Z. M.
Zhu, Z. Q.
Zhuang, H. L.
Zhukov, V.
Zichichi, A.
Zimmermann, N.
Zuccon, P.
CA AMS Collaboration
TI Antiproton Flux, Antiproton-to-Proton Flux Ratio, and Properties of
Elementary Particle Fluxes in Primary Cosmic Rays Measured with the
Alpha Magnetic Spectrometer on the International Space Station
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID ABSORPTION CROSS-SECTIONS; GEOMAGNETIC REFERENCE FIELD; DARK-MATTER;
RICH DETECTOR; ANTI-PROTONS; AMS-02 TRD; GEV-C; POSITRONS; NUCLEI;
CARBON
AB A precision measurement by AMS of the antiproton flux and the antiproton-to-proton flux ratio in primary cosmic rays in the absolute rigidity range from 1 to 450 GV is presented based on 3.49 x 10(5) antiproton events and 2.42 x 10(9) proton events. The fluxes and flux ratios of charged elementary particles in cosmic rays are also presented. In the absolute rigidity range similar to 60 to similar to 500 GV, the antiproton (p) over bar, proton p, and positron e(+) fluxes are found to have nearly identical rigidity dependence and the electron e(-) flux exhibits a different rigidity dependence. Below 60 GV, the ((p) over bar /p), ((p) over bar /e(+)), and (p/e(+)) flux ratios each reaches a maximum. From similar to 60 to similar to 500 GV, the ((p) over bar /p), ((p) over bar /e(+)), and (p/e(+)) flux ratios show no rigidity dependence. These are new observations of the properties of elementary particles in the cosmos.
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[Bachlechner, A.; Beischer, B.; Chung, C. H.; Gast, H.; Kirn, Th.; Luebelsmeyer, K.; Nikonov, N.; Raiha, T.; Schael, S.; von Dratzig, A. Schulz; Schwering, G.; Siedenburg, T.; Wienkenhover, J.; Zhukov, V.; Zimmermann, N.] Rhein Westfal TH Aachen, JARA FAME, D-52056 Aachen, Germany.
[Demirkoz, M. B.; Konak, C.; Turkoglu, C.] Middle E Tech Univ, Dept Phys, TR-06800 Ankara, Turkey.
[Caroff, S.; Coignet, G.; Goy, C.; Poireau, V.; Putze, A.; Rosier-Lees, S.; Tao, L.; Vialle, J. P.] CNRS IN2P3, Lab Annecy Le Vieux Phys Particules LAPP, F-74941 Annecy Le Vieux, France.
[Li, W.; Shan, B. S.; Zheng, Z. M.] Beihang Univ BUAA, Beijing 100191, Peoples R China.
[Dai, Y. M.; Wang, Q. L.; Yu, Y. J.] Chinese Acad Sci, Inst Elect Engn IEE, Beijing 100190, Peoples R China.
[Bachlechner, A.; Basegmez-du Pree, S.; Chen, G. M.; Chen, H. S.; Li, Z. H.; Lu, Y. S.; Tang, X. W.; Tang, Z. C.; Wang, X. Q.; Yang, M.; Yu, Z. Q.; Zhang, C.; Zhang, S. W.; Zhuang, H. L.] Chinese Acad Sci, Inst High Energy Phys IHEP, Beijing 100049, Peoples R China.
[Contin, A.; Laurenti, G.; Masi, N.; Palmonari, F.; Quadrani, L.; Zichichi, A.] Ist Nazl Fis Nucl, Sez Bologna, I-40126 Bologna, Italy.
[Contin, A.; Palmonari, F.; Quadrani, L.; Zichichi, A.] Univ Bologna, I-40126 Bologna, Italy.
[Becker, U.; Behlmann, M.; Burger, J.; Cai, X. D.; Capell, M.; Chen, A. I.; Choumilov, E.; Choutko, V.; Egorov, A.; Eline, A.; Fisher, P.; Galaktionov, Y.; Goglov, P.; Heil, M.; Hsieh, T. H.; Kounina, O.; Kounine, A.; Koutsenko, V.; Krafczyk, M. S.; Lebedev, A.; Li, J. Q.; Plyaskin, V.; Rozhkov, A.; Sun, W. H.; Ting, Samuel C. C.; Ting, S. M.; Wang, X.; Weng, Z. L.; Willenbrock, M.; Xu, W.; Yan, Q.; Zhang, J.; Zhang, S. D.; Zhang, Z.; Zhu, Z. Q.; Zuccon, P.] MIT, Cambridge, MA 02139 USA.
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[Sagdeev, R.] Univ Maryland, East West Ctr Space Sci, College Pk, MD 20742 USA.
[Picot-Clemente, N.; Seo, E. S.] Univ Maryland, IPST, College Pk, MD 20742 USA.
[Huh, C.; Jang, W. Y.; Kang, S. C.; Kim, G. N.; Kim, K. S.; Lim, S.; Son, D.] Kyungpook Natl Univ, CHEP, Daegu 41566, South Korea.
[Castellini, G.] CNR IROE, I-50125 Florence, Italy.
[Barrin, L.; Crispoltoni, M.; Formato, V.; Gargiulo, C.; Laudi, E.; Ting, Samuel C. C.] European Org Nucl Res CERN, CH-1211 Geneva 23, Switzerland.
[Azzarello, P.; Bourquin, M.; Cadoux, F.; Habiby, M.; Leluc, C.; Paniccia, M.; Pohl, M.; Rapin, D.; Saouter, P.; Vitillo, S.; Wu, X.] Univ Geneva, DPNC, CH-1211 Geneva 4, Switzerland.
[Aupetit, S.; Barrau, A.; Bonnivard, V.; Derome, L.; Ghelfi, A.; Maurin, D.; Ricol, J. S.; Tomassetti, N.] CNRS IN2P3, LPSC, F-38026 Grenoble, France.
[Aupetit, S.; Barrau, A.; Bonnivard, V.; Derome, L.; Ghelfi, A.; Maurin, D.; Ricol, J. S.; Tomassetti, N.] Univ Grenoble Alpes, F-38026 Grenoble, France.
[Guo, K. H.; He, Z. H.; Huang, Z. C.; Li, T. X.; Lv, S. S.; Mo, D. C.; Ni, J. Q.; Qi, X. M.; Wang, Z. X.] Sun Yat Sen Univ SYSU, Guangzhou 510275, Guangdong, Peoples R China.
[Bindi, V.; Consolandi, C.; Corti, C.; von Doetinchem, P.; Hoffman, J.; Nelson, T.; Pereira, R.; Whitman, K.] Univ Hawaii, Dept Phys & Astron, Honolulu, HI 96822 USA.
[Bollweg, K.; Clark, C.; Martin, T.; Mott, P.; Urban, T.] NASA, Johnson Space Ctr JSC, Jacobs Engn & Business Integra, Houston, TX 77058 USA.
[Attig, N.; Lippert, T.; Schmidt, S. M.] Julich Supercomp Ctr, D-52425 Julich, Germany.
[Attig, N.; Lippert, T.; Schmidt, S. M.] Res Ctr Julich, JARA FAME, D-52425 Julich, Germany.
[de Boer, W.; Gebauer, I.; Zeissler, S.] KIT, Inst Expt Kernphys, D-76128 Karlsruhe, Germany.
[Clavero, R.; Garcia-Lopez, R. J.; Tescaro, D.; Acosta, M. Vazquez] IAC, E-38205 San Cristobal la Laguna, Spain.
[Clavero, R.; Garcia-Lopez, R. J.; Tescaro, D.; Acosta, M. Vazquez] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Arruda, L.; Barao, F.; Nunes, P.; Orcinha, M.] Lab Instrumentacao & Fis Expt Particulas LIP, P-1000 Lisbon, Portugal.
[Han, K. C.; Jinchi, H.] Natl Chung Shan Inst Sci & Technol NCSIST, Taoyuan 32546, Taiwan.
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[Gomez-Coral, D. M.; Grabski, V.; Menchaca-Rocha, A.] Univ Nacl Autonoma Mexico, Inst Fis, Mexico City 01000, DF, Mexico.
[Boella, G.; Boschini, M. J.; Della Torre, S.; Gervasi, M.; Grandi, D.; La Vacca, G.; Pensotti, S.; Rancoita, P. G.; Rozza, D.; Tacconi, M.] Ist Nazl Fis Nucl, Sez Milano Bicocca, I-20126 Milan, Italy.
[Boella, G.; Gervasi, M.; Pensotti, S.] Univ Milano Bicocca, I-20126 Milan, Italy.
[Dong, F.; Gong, J.; Li, J. Q.; Li, Q.; Luo, J. Z.; Meng, Q.; Shi, J. Y.; Wu, H.; Xiong, R. Q.; Yi, H.; Zhang, J. H.] Southeast Univ SEU, Nanjing 210096, Jiangsu, Peoples R China.
[Finch, E.; Majka, R.; Sandweiss, J.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
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[Battiston, R.; Dimiccoli, F.; Kanishev, K.; Lazzizzera, I.] Univ Trento, I-38123 Povo, Trento, Italy.
[Bartoloni, A.; Borgia, B.; Lipari, P.; Valente, E.] Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy.
[Borgia, B.; Valente, E.] Univ Roma La Sapienza, I-00185 Rome, Italy.
[Bueno, E. F.; Vecchi, M.] Univ Sao Paulo, Inst Fis Sao Carlos, CP 369, BR-13560970 Sao Carlos, SP, Brazil.
[Chae, M. J.; Yang, J.] Ewha Womans Univ, Dept Phys, Seoul 120750, South Korea.
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[Li, H. S.; Yang, Y.] Natl Cheng Kung Univ, Tainan 70101, Taiwan.
[Lee, H. T.] Acad Sinica Grid Ctr ASGC, Taipei 11529, Taiwan.
[Feng, J.; Haino, S.; Huang, H.; Lee, S. C.; Li, Z. Y.; Lin, C. H.; Liu, D.; Lu, S. Q.; Qu, Z. Y.; Wei, C. C.] Acad Sinica, Inst Phys, Taipei 11529, Taiwan.
[Battarbee, M.; Eronen, T.; Torsti, J.; Valtonen, E.] Univ Turku, Dept Phys & Astron, Space Res Lab, FI-20014 Turku, Finland.
ASI, I-00133 Rome, Italy.
[Bazo, J.] PUCP, Dept Ciencias, Lima 32, Peru.
[Bachlechner, A.; D'Urso, D.; Nozzoli, F.; Pizzolotto, C.; Vitale, V.] ASDC, I-00133 Rome, Italy.
[Feng, J.; Li, Z. Y.; Lu, S. Q.] Sun Yat Sen Univ, Guangzhou 510275, Guangdong, Peoples R China.
[Huang, H.; Zhang, J.] Wuhan Univ, Wuhan 430072, Peoples R China.
[Li, J. Q.; Zhang, S. D.] Harbin Inst Technol HIT, Harbin 150001, Peoples R China.
[Liu, Hu] Huazhong Univ Sci & Technol HUST, Wuhan 430074, Peoples R China.
[Morescalchi, L.] Univ Siena, I-53100 Siena, Italy.
[Putze, A.] CNRS, Lab Annecy le Vieux Phys Theor LAPTh, F-74941 Annecy Le Vieux, France.
[Putze, A.] Univ Savoie Mt Blanc, F-74941 Annecy Le Vieux, France.
[Qin, X.; Xia, X.] Shandong Univ SDU, Jinan 250100, Shandong, Peoples R China.
[Qu, Z. Y.] Nankai Univ, Tianjin 300071, Peoples R China.
[Sun, W. H.] Southeast Univ SEU, Nanjing 210096, Jiangsu, Peoples R China.
[Wei, C. C.] Chinese Acad Sci, Inst Theoretial Phys, Beijing 100190, Peoples R China.
[Zhu, Z. Q.] Jilin Univ, Jilin 130012, Peoples R China.
RI Vecchi, Manuela/J-9180-2014; Sao Carlos Institute of Physics,
IFSC/USP/M-2664-2016; Paniccia, Mercedes/A-4519-2017; Delgado,
Carlos/K-7587-2014;
OI Paniccia, Mercedes/0000-0001-8482-2703; Delgado,
Carlos/0000-0002-7014-4101; Corti, Claudio/0000-0001-9127-7133;
Morescalchi, Luca/0000-0002-7819-8139; Bertucci,
Bruna/0000-0001-7584-293X; La Vacca, Giuseppe/0000-0002-2168-9447; Della
Torre, Stefano/0000-0002-7669-0859
FU Sao Paulo Research Foundation (FAPESP), Brazil [2014/19149-7,
2014/50747-8, 2015-50378-5]; CAS, China; NSFC, China; MOST, China; NLAA,
China; provincial government of Shandong, China; provincial government
of Jiangsu, China; provincial government of Guangdong, China; China
Scholarship Council, China; Finnish Funding Agency for Innovation
(Tekes), Finland [40361/01, 40518/03]; Academy of Finland, Finland
[258963]; CNRS, France; IN2P3, France; CNES, France; Enigmass, France;
ANR, France; Pascale Ehrenfreund, Germany; DLR, Germany; JARA-HPC,
Germany [JARA0052]; INFN, Italy [2013-002-R.0, 2014-037-R.0]; ASI, Italy
[2013-002-R.0, 2014-037-R.0]; CHEP Grants at Kyungpook National
University, Korea [NRF-2009-0080142, NRF-2012-010226]; CHEP Grants at
Ewha Womans University, Korea [NRF-2013-004883]; Consejo Nacional de
Ciencia y Tecnologia, Mexico; UNAM, Mexico; FCT, Portugal
[PTDC/FIS/122567/2010]; CIEMAT, Spain; IAC, Spain; CDTI, Spain;
SEIDI-MINECO, Spain [AYA2012-39526-C02-(01/02),
ESP2015-71662-C2-(1-P/2-P), SEV-2011-0187, SEV-2015-0548,
MDM-2015-0509]; Swiss National Science Foundation (SNSF), federal and
cantonal authorities, Switzerland; Academia Sinica, Taiwan; Ministry of
Science and Technology (MOST), Taiwan [103-2112-M-006-018-MY3,
104-2112-M-001-027, CDA-105-M06]; Turkish Atomic Energy Authority at
METU, Turkey; NSF Grant, USA [1455202]; Wyle Laboratories Grant, USA
[2014/T72497]; NASA NESSF Grant, USA [HELIO15F-0005]
FX We thank former NASA Administrator Daniel S. Goldin for his dedication
to the legacy of the ISS as a scientific laboratory and his decision for
NASA to fly AMS as a DOE payload. We also acknowledge the continuous
support of the NASA leadership including Charles Bolden and William H.
Gerstenmaier and of the JSC and MSFC flight control teams which has
allowed AMS to operate optimally on the ISS for five years. We are
grateful for the support of Jim Siegrist and his staff of the DOE. We
also acknowledge the continuous support from MIT and its School of
Science, Michael Sipser, Marc Kastner, Ernest Moniz, Richard Milner, and
Boleslaw Wyslouch. Research supported by Sao Paulo Research Foundation
(FAPESP) Grants No. 2014/19149-7, No. 2014/50747-8, and No.
2015-50378-5, Brazil; CAS, NSFC, MOST, NLAA, the provincial governments
of Shandong, Jiangsu, Guangdong, and the China Scholarship Council,
China; the Finnish Funding Agency for Innovation (Tekes) Grants No.
40361/01 and No. 40518/03 and the Academy of Finland Grant No. 258963,
Finland; CNRS, IN2P3, CNES, Enigmass, and the ANR, France; Pascale
Ehrenfreund, DLR, and JARA-HPC under Project No. JARA0052, Germany; INFN
and ASI under ASI-INFN Agreements No. 2013-002-R.0 and No. 2014-037-R.0,
Italy; CHEP Grants No. NRF-2009-0080142 and No. NRF-2012-010226 at
Kyungpook National University and No. NRF-2013-004883 at Ewha Womans
University, Korea; the Consejo Nacional de Ciencia y Tecnologia and
UNAM, Mexico; FCT under Grant No. PTDC/FIS/122567/2010, Portugal;
CIEMAT, IAC, CDTI, and SEIDI-MINECO under Grants No.
AYA2012-39526-C02-(01/02), No. ESP2015-71662-C2-(1-P/2-P), No.
SEV-2011-0187, No. SEV-2015-0548, and No. MDM-2015-0509, Spain; the
Swiss National Science Foundation (SNSF), federal and cantonal
authorities, Switzerland; Academia Sinica and the Ministry of Science
and Technology (MOST) under Grants No. 103-2112-M-006-018-MY3, No.
104-2112-M-001-027, and No. CDA-105-M06, former President of Academia
Sinica Yuan-Tseh Lee, and former Ministers of MOST Maw-Kuen Wu and
Luo-Chuan Lee, Taiwan; the Turkish Atomic Energy Authority at METU,
Turkey; and NSF Grant No. 1455202, Wyle Laboratories Grant No.
2014/T72497, and NASA NESSF Grant No. HELIO15F-0005, USA. We gratefully
acknowledge the strong support from CERN including Rolf-Dieter Heuer and
Fabiola Gianotti, from the CERN IT department and Bernd Panzer-Steindel,
and from the European Space Agency including Johann-Dietrich Worner and
Simonetta Di Pippo. We are grateful for important discussions with
Fiorenza Donato, Jonathan Ellis, Jonathan Feng, Igor Moskalenko, Michael
Salamon, Subir Sarkar, Joachim Trumper, Michael S. Turner, Steven
Weinberg, and Arnold Wolfendale.
NR 85
TC 8
Z9 8
U1 27
U2 27
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 AUG 26
PY 2016
VL 117
IS 9
AR 091103
DI 10.1103/PhysRevLett.117.091103
PG 10
WC Physics, Multidisciplinary
SC Physics
GA DU1ZE
UT WOS:000382008900001
PM 27610839
ER
PT J
AU Leblanc, T
Sica, RJ
van Gijsel, JAE
Godin-Beekmann, S
Haefele, A
Trickl, T
Payen, G
Gabarrot, F
AF Leblanc, Thierry
Sica, Robert J.
van Gijsel, Joanna A. E.
Godin-Beekmann, Sophie
Haefele, Alexander
Trickl, Thomas
Payen, Guillaume
Gabarrot, Frank
TI Proposed standardized definitions for vertical resolution and
uncertainty in the NDACC lidar ozone and temperature algorithms - Part
1: Vertical resolution
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID RAMAN LIDAR; STRATOSPHERIC OZONE; RAYLEIGH; DIFFERENTIATION; RETRIEVAL;
PROFILES; DENSITY
AB A standardized approach for the definition and reporting of vertical resolution of the ozone and temperature lidar profiles contributing to the Network for the Detection for Atmospheric Composition Change (NDACC) database is proposed. Two standardized definitions homogeneously and unequivocally describing the impact of vertical filtering are recommended.
The first proposed definition is based on the width of the response to a finite-impulse-type perturbation. The response is computed by convolving the filter coefficients with an impulse function, namely, a Kronecker delta function for smoothing filters, and a Heaviside step function for derivative filters. Once the response has been computed, the proposed standardized definition of vertical resolution is given by Delta z = delta z x H-FWHM, where delta z is the lidar's sampling resolution and H-FWHM is the full width at half maximum (FWHM) of the response, measured in sampling intervals.
The second proposed definition relates to digital filtering theory. After applying a Laplace transform to a set of filter coefficients, the filter's gain characterizing the effect of the filter on the signal in the frequency domain is computed, from which the cut-off frequency f(C), defined as the frequency at which the gain equals 0.5, is computed. Vertical resolution is then defined by Delta z = delta z/(2f(C)). Unlike common practice in the field of spectral analysis, a factor 2 f(C) instead of f(C) is used here to yield vertical resolution values nearly equal to the values obtained with the impulse response definition using the same filter coefficients. When using either of the proposed definitions, unsmoothed signals yield the best possible vertical resolution Delta z = delta z (one sampling bin).
Numerical tools were developed to support the implementation of these definitions across all NDACC lidar groups. The tools consist of ready-to-use "plug-in" routines written in several programming languages that can be inserted into any lidar data processing software and called each time a filtering operation occurs in the data processing chain.
When data processing implies multiple smoothing operations, the filtering information is analytically propagated through the multiple calls to the routines in order for the standardized values of vertical resolution to remain theoretically and numerically exact at the very end of data processing.
C1 [Leblanc, Thierry] CALTECH, Jet Prop Lab, Wrightwood, CA 92397 USA.
[Sica, Robert J.] Univ Western Ontario, Dept Phys & Astron, London, ON, Canada.
[van Gijsel, Joanna A. E.] Royal Netherlands Meteorol Inst KNMI, Bilthoven, Netherlands.
[Godin-Beekmann, Sophie] CNRS INSU, LATMOS IPSL, Paris, France.
[Haefele, Alexander] Meteoswiss, Payerne, Switzerland.
[Trickl, Thomas] IMK IFU, Karlsruhe Inst Technol, Garmisch Partenkirchen, Germany.
[Payen, Guillaume; Gabarrot, Frank] Univ Le Reunion, Observ Sci, CNRS, St Denis De La Reunion, Reunion.
[Payen, Guillaume; Gabarrot, Frank] Univ Reunion, UMS3365, St Denis De La Reunion, Reunion.
RP Leblanc, T (reprint author), CALTECH, Jet Prop Lab, Wrightwood, CA 92397 USA.
EM thierry.leblanc@jpl.nasa.gov
RI Trickl, Thomas/F-7331-2010
FU VALID project; Canadian National Sciences and Engineering Research
Council
FX This work was initiated in response to the 2010 call for international
teams of experts in earth and space science by the International Space
Science Institute (ISSI) in Bern, Switzerland. It could not have been
performed without the travel and logistical support of ISSI. Part of the
work described in this report was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under agreements with
the National Aeronautics and Space Administration. Part of this work was
carried out in support of the VALID project. Robert J. Sica would like
to acknowledge the support of the Canadian National Sciences and
Engineering Research Council for support of the University of Western
Ontario lidar work. The team would also like to acknowledge J. Bandoro
for his help in the design of the MATLAB filtering tools.
NR 29
TC 3
Z9 3
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 AUG 25
PY 2016
VL 9
IS 8
BP 4029
EP 4049
DI 10.5194/amt-9-4029-2016
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW6YY
UT WOS:000383798500001
ER
PT J
AU Leblanc, T
Sica, RJ
van Gijsel, JAE
Godin-Beekmann, S
Haefele, A
Trickl, T
Payen, G
Liberti, G
AF Leblanc, Thierry
Sica, Robert J.
van Gijsel, Joanna A. E.
Godin-Beekmann, Sophie
Haefele, Alexander
Trickl, Thomas
Payen, Guillaume
Liberti, Gianluigi
TI Proposed standardized definitions for vertical resolution and
uncertainty in the NDACC lidar ozone and temperature algorithms - Part
2: Ozone DIAL uncertainty budget
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID ABSORPTION CROSS-SECTIONS; FOURIER-TRANSFORM SPECTROSCOPY; O-2 HERZBERG
BANDS; STRATOSPHERIC OZONE; RAYLEIGH-SCATTERING; UV SPECTROSCOPY; NM
REGION; NO2; TROPOSPHERE; SPECTRA
AB A standardized approach for the definition, propagation, and reporting of uncertainty in the ozone differential absorption lidar data products contributing to the Network for the Detection for Atmospheric Composition Change (NDACC) database is proposed. One essential aspect of the proposed approach is the propagation in parallel of all independent uncertainty components through the data processing chain before they are combined together to form the ozone combined standard uncertainty.
The independent uncertainty components contributing to the overall budget include random noise associated with signal detection, uncertainty due to saturation correction, background noise extraction, the absorption cross sections of O-3, NO2, SO2, and O-2, the molecular extinction cross sections, and the number densities of the air, NO2, and SO2. The expression of the individual uncertainty components and their step-by-step propagation through the ozone differential absorption lidar (DIAL) processing chain are thoroughly estimated. All sources of uncertainty except detection noise imply correlated terms in the vertical dimension, which requires knowledge of the covariance matrix when the lidar signal is vertically filtered. In addition, the covariance terms must be taken into account if the same detection hardware is shared by the lidar receiver channels at the absorbed and non-absorbed wavelengths.
The ozone uncertainty budget is presented as much as possible in a generic form (i.e., as a function of instrument performance and wavelength) so that all NDACC ozone DIAL investigators across the network can estimate, for their own instrument and in a straightforward manner, the expected impact of each reviewed uncertainty component. In addition, two actual examples of full uncertainty budget are provided, using nighttime measurements from the tropospheric ozone DIAL located at the Jet Propulsion Laboratory (JPL) Table Mountain Facility, California, and nighttime measurements from the JPL stratospheric ozone DIAL located at Mauna Loa Observatory, Hawai'i.
C1 [Leblanc, Thierry] CALTECH, Jet Prop Lab, Wrightwood, CA 92397 USA.
[Sica, Robert J.] Univ Western Ontario, Dept Phys & Astron, London, ON, Canada.
[van Gijsel, Joanna A. E.] Royal Netherlands Meteorol Inst KNMI, Bilthoven, Netherlands.
[Godin-Beekmann, Sophie] CNRS INSU, LATMOS IPSL, Paris, France.
[Haefele, Alexander] Meteoswiss, Payerne, Switzerland.
[Trickl, Thomas] IMK IFU, Karlsruhe Inst Technol, Garmisch Partenkirchen, Germany.
[Payen, Guillaume] Univ La Reunion, Observ Sci, CNRS, St Denis De La Reunion, France.
[Payen, Guillaume] Univ Reunion, UMS3365, St Denis De La Reunion, France.
[Liberti, Gianluigi] ISAC CNR, Via Fosso Cavaliere 100, I-00133 Rome, Italy.
RP Leblanc, T (reprint author), CALTECH, Jet Prop Lab, Wrightwood, CA 92397 USA.
EM thierry.leblanc@jpl.nasa.gov
RI Trickl, Thomas/F-7331-2010
FU European Space Agency VALID project; Canadian National Sciences and
Engineering Research Council
FX This work was initiated in response to the 2010 call for international
teams of experts in Earth and Space Science by the International Space
Science Institute (ISSI) in Bern, Switzerland. It could not have been
performed without the travel and logistical support of ISSI. Part of the
work described in this paper was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under agreements with
the National Aeronautics and Space Administration. Part of this work was
carried out in support of the European Space Agency VALID project.
Robert J. Sica would like to acknowledge the support of the Canadian
National Sciences and Engineering Research Council for support of the
University of Western Ontario lidar work.
NR 58
TC 2
Z9 2
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 AUG 25
PY 2016
VL 9
IS 8
BP 4051
EP 4078
DI 10.5194/amt-9-4051-2016
PG 28
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA DW6YY
UT WOS:000383798500002
ER
PT J
AU Leblanc, T
Sica, RJ
van Gijsel, JAE
Haefele, A
Payen, G
Liberti, G
AF Leblanc, Thierry
Sica, Robert J.
van Gijsel, Joanna A. E.
Haefele, Alexander
Payen, Guillaume
Liberti, Gianluigi
TI Proposed standardized definitions for vertical resolution and
uncertainty in the NDACC lidar ozone and temperature algorithms - Part
3: Temperature uncertainty budget
SO ATMOSPHERIC MEASUREMENT TECHNIQUES
LA English
DT Article
ID ABSORPTION CROSS-SECTIONS; RAYLEIGH-SCATTER; RAMAN LIDAR; MIDDLE
ATMOSPHERE; NO2 ABSORPTION; NM REGION; SPECTRA; MODEL; VALIDATION; RANGE
AB A standardized approach for the definition, propagation, and reporting of uncertainty in the temperature lidar data products contributing to the Network for the Detection for Atmospheric Composition Change (NDACC) database is proposed. One important aspect of the proposed approach is the ability to propagate all independent uncertainty components in parallel through the data processing chain. The individual uncertainty components are then combined together at the very last stage of processing to form the temperature combined standard uncertainty.
The identified uncertainty sources comprise major components such as signal detection, saturation correction, background noise extraction, temperature tie-on at the top of the profile, and absorption by ozone if working in the visible spectrum, as well as other components such as molecular extinction, the acceleration of gravity, and the molecular mass of air, whose magnitudes depend on the instrument, data processing algorithm, and altitude range of interest.
The expression of the individual uncertainty components and their step-by-step propagation through the temperature data processing chain are thoroughly estimated, taking into account the effect of vertical filtering and the merging of multiple channels. All sources of uncertainty except detection noise imply correlated terms in the vertical dimension, which means that covariance terms must be taken into account when vertical filtering is applied and when temperature is integrated from the top of the profile. Quantitatively, the uncertainty budget is presented in a generic form (i.e., as a function of instrument performance and wavelength), so that any NDACC temperature lidar investigator can easily estimate the expected impact of individual uncertainty components in the case of their own instrument.
Using this standardized approach, an example of uncertainty budget is provided for the