FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Yu, HB
Remer, LA
Kahn, RA
Chin, M
Zhang, Y
AF Yu, Hongbin
Remer, Lorraine A.
Kahn, Ralph A.
Chin, Mian
Zhang, Yan
TI Satellite perspective of aerosol intercontinental transport: From
qualitative tracking to quantitative characterization
SO ATMOSPHERIC RESEARCH
LA English
DT Article
DE Aerosols; Particulate matter; Satellite remote sensing; Long-range
transport
ID RESOLUTION IMAGING SPECTRORADIOMETER; SUN PHOTOMETER MEASUREMENTS; SMOKE
INJECTION HEIGHTS; OPTICAL DEPTH RETRIEVAL; SAHARAN DUST TRANSPORT;
TO-BACKSCATTER RATIO; NORTH-AFRICAN DUST; FOREST-FIRE SMOKE;
AIR-POLLUTION; A-TRAIN
AB Evidence of aerosol intercontinental transport (ICT) is both widespread and compelling. Model simulations suggest that ICT could significantly affect regional air quality and climate, but the broad inter-model spread of results underscores a need of constraining model simulations with measurements. Satellites have inherent advantages over in situ measurements to characterize aerosol ICT, because of their spatial and temporal coverage. Significant progress in satellite remote sensing of aerosol properties during the Earth Observing System (EOS) era offers the opportunity to increase quantitative characterization and estimates of aerosol ICT beyond the capability of pre-EOS era satellites that could only qualitatively track aerosol plumes. EOS satellites also observe emission strengths and injection heights of some aerosols, aerosol precursors, and aerosol-related gases, which can help characterize aerosol ICT. We review how the current generation of satellite measurements have been used to (1) characterize the evolution of aerosol plumes (e.g., both horizontal and vertical transport, and properties) on an episodic basis, (2) understand the seasonal and inter-annual variations of aerosol ICT and their control factors, (3) estimate the export and import fluxes of aerosols, and (4) evaluate and constrain model simulations. Substantial effort is needed to further explore an integrated approach using measurements from on-orbit satellites (e.g., A-Train synergy) for observational characterization and model constraint of aerosol intercontinental transport and to develop advanced sensors for future missions. (C) 2013 Elsevier B.V. All rights reserved.
C1 [Yu, Hongbin] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
[Yu, Hongbin; Kahn, Ralph A.; Chin, Mian; Zhang, Yan] NASA, Goddard Space Flight Ctr, Earth Sci Directorate, Greenbelt, MD 20771 USA.
[Remer, Lorraine A.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Zhang, Yan] Univ Space Res Assoc, Columbia, MD 21044 USA.
RP Yu, HB (reprint author), NASA, Goddard Space Flight Ctr, Climate & Radiat Lab, Code 613, Greenbelt, MD 20771 USA.
EM Hongbin.Yu@nasa.gov
RI Yu, Hongbin/C-6485-2008; Liu, Yanan/J-3680-2012; Chin, Mian/J-8354-2012;
Kahn, Ralph/D-5371-2012
OI Yu, Hongbin/0000-0003-4706-1575; Kahn, Ralph/0000-0002-5234-6359
FU NASA [NNXAH66G, NNX11AJ91G]; NASA Modeling
FX HY, LAR, MC, and YZ acknowledge the NASA support of this work via
NNXAH66G (The Science of Terra and Aqua program) and NNX11AJ91G
(Atmospheric Composition Modeling and Analysis - ACMAP program), both
managed by Richard Eckman. MC was also supported in part by NASA
Modeling, Analysis, and Projection program managed by David Considine.
The work of RK was supported in part by NASA's Climate and Radiation
Research and Analysis Program under Hal Maring, ACIVIAP program under
Richard Eckman, and the EOS-MISR instrument project. We thank anonymous
reviewers for insightful comments that have helped improve the quality
of the paper.
NR 266
TC 19
Z9 19
U1 4
U2 46
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 APR 28
PY 2013
VL 124
BP 73
EP 100
DI 10.1016/j.atmosres.2012.12.013
PG 28
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 125QQ
UT WOS:000317556800007
ER
PT J
AU Pokhrel, YN
Fan, Y
Miguez-Macho, G
Yeh, PJF
Han, SC
AF Pokhrel, Yadu N.
Fan, Ying
Miguez-Macho, Gonzalo
Yeh, Pat J. -F.
Han, Shin-Chan
TI The role of groundwater in the Amazon water cycle: 3. Influence on
terrestrial water storage computations and comparison with GRACE
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID CLIMATE EXPERIMENT GRACE; SEQUENCE BENEATH FOREST; FLOODPLAIN LAKE;
GRAVITY RECOVERY; BASIN; HYDROLOGY; VARIABILITY; BEHAVIOR; BALANCE;
EVAPOTRANSPIRATION
AB We explore the mechanisms whereby groundwater influences terrestrial water storage (TWS) in the Amazon using GRACE observations and two contrasting versions of the LEAF-Hydro-Flood hydrological model: one with and the other without an interactive groundwater. We find that, first, where the water table is shallow as in northwestern Amazonia and floodplains elsewhere, subsurface stores (vadose zone and groundwater) are nearly saturated year-round, hence river and flooding dominate TWS variation; where the water table is deep as in southeastern Amazonia, the large subsurface storage capacity holds the infiltrated water longer before releasing it to streams, hence the subsurface storage dominates TWS variation. Second, over the whole Amazon, the subsurface water contribution far exceeds surface water contribution to total TWS variations. Based on LEAF-Hydro-Flood simulations, 71% of TWS change is from subsurface water, 24% from flood water, and 5% from water in river channels. Third, the subsurface store includes two competing terms, soil water in the vadose zone and groundwater below the water table. As the water table rises, the length of vadose zone is shortened and hence the change in groundwater store is accompanied by an opposite change in soil water store resulting in their opposite phase and contributions to total TWS. We conclude that the inclusion of a prognostic groundwater store and its interactions with the vadose zone, rivers, and floodplains in hydrological simulations enhances seasonal amplitudes and delays seasonal peaks of TWS anomaly, leading to an improved agreement with GRACE observations.
C1 [Pokhrel, Yadu N.; Fan, Ying] Rutgers State Univ, Dept Earth & Planetary Sci, New Brunswick, NJ 08854 USA.
[Miguez-Macho, Gonzalo] Univ Santiago de Compostela, Fac Phys, Nonlinear Phys Grp, Galicia, Spain.
[Yeh, Pat J. -F.] UNESCO, Int Ctr Water Hazard & Risk Management ICHARM, Tsukuba, Ibaraki, Japan.
[Han, Shin-Chan] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
RP Pokhrel, YN (reprint author), Rutgers State Univ, Dept Earth & Planetary Sci, New Brunswick, NJ 08854 USA.
EM yadupokhrel@eps.rutgers.edu
RI Han, Shin-Chan/A-2022-2009; Pokhrel, Yadu /J-6440-2013; YEH,
Pat/B-2758-2011
OI Pokhrel, Yadu /0000-0002-1367-216X; YEH, Pat/0000-0001-7629-3362
FU National Science Foundation; NASA's Earth Surface and Interior program;
GRACE projects; [NSF-AGS-1045110]; [EPA-STAR-RD834190]
FX Funding comes from NSF-AGS-1045110 and EPA-STAR-RD834190. Computation
support comes from CESGA (Centro de Supercomputacion de Galicia)
Supercomputer Center at the Universidade de Santiago de Compostela,
Galicia, Spain, and the Climate Simulation Laboratory at NCAR's
Computational and Information Systems Laboratory, sponsored by the
National Science Foundation and other agencies. SCH is supported by
NASA's Earth Surface and Interior program and GRACE projects.
NR 72
TC 24
Z9 24
U1 1
U2 41
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 APR 27
PY 2013
VL 118
IS 8
BP 3233
EP 3244
DI 10.1002/jgrd.50335
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 155JQ
UT WOS:000319744200016
ER
PT J
AU Zhu, L
Henze, DK
Cady-Pereira, KE
Shephard, MW
Luo, M
Pinder, RW
Bash, JO
Jeong, GR
AF Zhu, L.
Henze, D. K.
Cady-Pereira, K. E.
Shephard, M. W.
Luo, M.
Pinder, R. W.
Bash, J. O.
Jeong, G. -R.
TI Constraining U.S. ammonia emissions using TES remote sensing
observations and the GEOS-Chem adjoint model
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID AIR-QUALITY MODELS; UNITED-STATES; PART II; NITROGEN; POLLUTION;
NITRATE; TRENDS; PM2.5; VARIABILITY; SENSITIVITY
AB Ammonia (NH3) has significant impacts on biodiversity, eutrophication, and acidification. Widespread uncertainty in the magnitude and seasonality of NH3 emissions hinders efforts to address these issues. In this work, we constrain U. S. NH3 sources using observations from the TES satellite instrument with the GEOS-Chem model and its adjoint. The inversion framework is first validated using simulated observations. We then assimilate TES observations for April, July, and October of 2006 through 2009. The adjoint-based inversion allows emissions to be adjusted heterogeneously; they are found to increase in California throughout the year, increase in different regions of the West depending upon season, and exhibit smaller increases and occasional decreases in the Eastern U. S. Evaluations of the inversion using independent surface measurements show reduced model underestimates of surface NH3 and wet deposited NHx in April and October; however, the constrained simulation in July leads to overestimates of these quantities, while TES observations are still under predicted. Modeled sulfate and nitrate aerosols concentrations do not change significantly, and persistent nitrate overestimation is noted, consistent with previous studies. Overall, while satellite-based constraints on NH3 emissions improve model simulations in several aspects, additional assessment at higher horizontal resolution of spatial sampling bias, nitric acid formation, and diurnal variability and bi-directionality of NH3 sources may be necessary to enhance year-round model performance across the full range of gas and aerosol evaluations.
C1 [Zhu, L.; Henze, D. K.; Jeong, G. -R.] Univ Colorado, Dept Mech Engn, Boulder, CO 80309 USA.
[Cady-Pereira, K. E.] Atmospher & Environm Res Inc, Lexington, MA USA.
[Shephard, M. W.] Atmospher & Climate Applicat Inc, East Gwillimbury, ON, Canada.
[Shephard, M. W.] Environm Canada, Toronto, ON, Canada.
[Luo, M.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Pinder, R. W.; Bash, J. O.; Jeong, G. -R.] US EPA, Res Triangle Pk, NC 27711 USA.
RP Henze, DK (reprint author), Univ Colorado, Dept Mech Engn, Boulder, CO 80309 USA.
EM daven.henze@colorado.edu
RI Bash, Jesse/E-9688-2013; Pinder, Robert/F-8252-2011; Chem,
GEOS/C-5595-2014;
OI Pinder, Robert/0000-0001-6390-7126; Bash, Jesse/0000-0001-8736-0102
FU NASA [NNX09AN77G, NNX10AG63G]; EPA STAR [RD834559]
FX This work is supported by NASA grants NNX09AN77G and NNX10AG63G and EPA
STAR award RD834559. While this manuscript has been reviewed by the
Environmental Protection Agency and approved for publication, it may not
reflect official agency views or policies.
NR 58
TC 41
Z9 42
U1 5
U2 39
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 APR 27
PY 2013
VL 118
IS 8
BP 3355
EP 3368
DI 10.1002/jgrd.50166
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 155JQ
UT WOS:000319744200028
ER
PT J
AU Tiscareno, MS
Mitchell, CJ
Murray, CD
Di Nino, D
Hedman, MM
Schmidt, J
Burns, JA
Cuzzi, JN
Porco, CC
Beurle, K
Evans, MW
AF Tiscareno, Matthew S.
Mitchell, Colin J.
Murray, Carl D.
Di Nino, Daiana
Hedman, Matthew M.
Schmidt, Juergen
Burns, Joseph A.
Cuzzi, Jeffrey N.
Porco, Carolyn C.
Beurle, Kevin
Evans, Michael W.
TI Observations of Ejecta Clouds Produced by Impacts onto Saturn's Rings
SO SCIENCE
LA English
DT Article
ID F RING; BOMBARDMENT
AB We report observations of dusty clouds in Saturn's rings, which we interpret as resulting from impacts onto the rings that occurred between 1 and 50 hours before the clouds were observed. The largest of these clouds was observed twice; its brightness and cant angle evolved in a manner consistent with this hypothesis. Several arguments suggest that these clouds cannot be due to the primary impact of one solid meteoroid onto the rings, but rather are due to the impact of a compact stream of Saturn-orbiting material derived from previous breakup of a meteoroid. The responsible interplanetary meteoroids were initially between 1 centimeter and several meters in size, and their influx rate is consistent with the sparse prior knowledge of smaller meteoroids in the outer solar system.
C1 [Tiscareno, Matthew S.; Hedman, Matthew M.; Evans, Michael W.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
[Mitchell, Colin J.; Di Nino, Daiana; Porco, Carolyn C.] Space Sci Inst, CICLOPS, Boulder, CO 80301 USA.
[Murray, Carl D.; Beurle, Kevin] Queen Mary Univ London, Astron Unit, London E1 4NS, England.
[Schmidt, Juergen] Univ Oulu, Dept Phys, Astron Div, FI-90014 Oulu, Finland.
[Schmidt, Juergen] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Burns, Joseph A.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Burns, Joseph A.] Cornell Univ, Coll Engn, Ithaca, NY 14853 USA.
[Cuzzi, Jeffrey N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Tiscareno, MS (reprint author), Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
EM matthewt@astro.cornell.edu
FU NASA Cassini Data Analysis program [NNX08AQ72G, NNX10AG67G]; Cassini
project; Science and Technology Facilities Council [ST/F007566/1]
FX We thank M. Showalter for helpful discussions and for the use of Mie
scattering code. We thank the Cassini project and the Cassini Imaging
Team for making these observations possible. M. S. T. acknowledges
funding from the NASA Cassini Data Analysis program (NNX08AQ72G and
NNX10AG67G) and the Cassini project. C. D. M. acknowledges funding from
the Science and Technology Facilities Council (grant ST/F007566/1).
NR 21
TC 11
Z9 11
U1 1
U2 11
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD APR 26
PY 2013
VL 340
IS 6131
BP 460
EP 464
DI 10.1126/science.1233524
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 131SQ
UT WOS:000318016700037
PM 23620048
ER
PT J
AU Bhatia, AK
AF Bhatia, A. K.
TI Hybrid theory of P-wave electron-Li2+ elastic scattering and
photoabsorption in two-electron systems
SO PHYSICAL REVIEW A
LA English
DT Article
ID PHOTOIONIZATION CROSS-SECTIONS; PHASE-SHIFTS; HYDROGEN; HE;
PHOTODETACHMENT; HELIUM; RESONANCES; ENERGIES; FEEDBACK; STATES
AB In previous papers [Bhatia, Phys. Rev. A 85, 052708 (2012); 86, 032709 (2012)] electron-hydrogen and electron-He+ P-wave scattering phase shifts were calculated using the hybrid theory. This method is extended to the singlet and triplet electron-Li2+ P-wave scattering in the elastic region, where the correlation functions are of Hylleraas type. The short-range and long-range correlations are included in the Schrodinger equation at the same time, by using a combination of a modified method of polarized orbitals and the optical potential formalism. Phase shifts are compared to those obtained by other methods. The present calculation requires very few correlation functions to obtain accurate results which are rigorous lower bounds to the exact phase shifts. The continuum functions obtained in this method are used to calculate photodetachment and photoionization cross sections of two-electron systems H-, He, and Li+. Cross sections of the metastable S-1,S-3 states of He, and Li+ are also calculated. These cross sections are calculated in the elastic region and compared with previous calculations. Using these cross sections, the Maxwellian-averaged radiative-recombination rates at various electron temperatures are also calculated. DOI: 10.1103/PhysRevA.87.042705
C1 NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
RP Bhatia, AK (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
NR 37
TC 4
Z9 4
U1 1
U2 11
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1050-2947
J9 PHYS REV A
JI Phys. Rev. A
PD APR 25
PY 2013
VL 87
IS 4
AR 042705
DI 10.1103/PhysRevA.87.042705
PG 9
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 133XC
UT WOS:000318173200006
ER
PT J
AU Galley, CR
Behunin, RO
Hu, BL
AF Galley, Chad R.
Behunin, Ryan O.
Hu, B. L.
TI Oscillator-field model of moving mirrors in quantum optomechanics
SO PHYSICAL REVIEW A
LA English
DT Article
ID RESOLVED-SIDE-BAND; ELECTROMAGNETIC-FIELD; MICROMECHANICAL OSCILLATOR;
RADIATION-PRESSURE; PARTICLE CREATION; DIMENSIONAL SPACE; DISPERSIVE
MIRROR; STATE REDUCTION; MASTER EQUATION; BROWNIAN-MOTION
AB We present a microphysics model for the kinematics and dynamics of optomechanics describing the coupling between an optical field, modeled here by a massless scalar field, and the internal and mechanical degrees of freedom of a movable mirror. Instead of implementing boundary conditions on the field, we introduce an internal degree of freedom and its dynamics to describe the mirror's reflectivity. Depending on parameter values, the internal degrees of freedom of the mirror in this model capture a range of its optical activities, from those exhibiting broadband reflective properties to those reflecting only in a narrow band. After establishing the model we show how appropriate parameter choices lead to other well-known optomechanical models, including those of Barton and Calogeracos [Ann. Phys. (NY) 238, 227 (1995)], Calogeracos and Barton, Ann. Phys. (NY) 238, 268 (1995), Law [Phys. Rev. A 51, 2537 (1995)], and Golestanian and Kardar [Phys. Rev. Lett. 78, 3421 (1997); Phys. Rev. A 58, 1713 (1998)]. As a simple illustrative application we derive classical radiation pressure cooling from this model. We then connect our microphysics model to the common descriptions of a moving mirror coupled to radiation pressure (e. g., with Nx coupling, where N is the photon number and x is the mirror displacement), making explicit the underlying assumptions made in these phenomenological models. Our model is also applicable to the lesser explored case of small N, which existing models based on sideband approximations [Kimble et al., Phys. Rev. D 65, 022002 (2001)] have not addressed. Interestingly, we also find that slow-moving mirrors in our model can be described by the ubiquitous Brownian motion model of quantum open systems. The scope of applications of this model ranges from a full quantum-mechanical treatment of radiation pressure cooling and quantum entanglement between macroscopic mirrors to the back reaction of Hawking radiation on black-hole evaporation in a moving mirror analog. DOI: 10.1103/PhysRevA.87.043832
C1 [Galley, Chad R.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Galley, Chad R.] CALTECH, Pasadena, CA 91106 USA.
[Behunin, Ryan O.] Los Alamos Natl Lab, Ctr Nonlinear Studies, Los Alamos, NM 87545 USA.
[Behunin, Ryan O.] Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA.
[Hu, B. L.] Univ Maryland, Joint Quantum Inst, College Pk, MD 20742 USA.
[Hu, B. L.] Univ Maryland, Maryland Ctr Fundamental Phys, College Pk, MD 20742 USA.
[Hu, B. L.] Hong Kong Univ Sci & Technol, Inst Adv Study, Kowloon, Hong Kong, Peoples R China.
[Hu, B. L.] Hong Kong Univ Sci & Technol, Dept Phys, Kowloon, Hong Kong, Peoples R China.
RP Galley, CR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA.
FU NASA; NIST Gaithersburg grant; US Department of Energy through the LANL
LDRD program; NSF [PHY-0801368]
FX C.G. was supported in part by an appointment to the NASA Postdoctoral
Program at the Jet Propulsion Laboratory administered by Oak Ridge
Associated Universities through a contract with NASA and in part by a
NIST Gaithersburg grant awarded to the University of Maryland when this
work was started. R. B. gratefully acknowledges the support of the US
Department of Energy through the LANL LDRD program. B. L. H. wishes to
thank Prof. Jason Twamley, director of the Centre for Quantum Computer
Technology at Macquarie University, for his warm hospitality in
February-March 2011 during which this work was partly carried out. His
research was partially supported by NSF Grant No. PHY-0801368 to the
University of Maryland.
NR 101
TC 3
Z9 3
U1 2
U2 16
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1050-2947
J9 PHYS REV A
JI Phys. Rev. A
PD APR 24
PY 2013
VL 87
IS 4
AR 043832
DI 10.1103/PhysRevA.87.043832
PG 21
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 131AV
UT WOS:000317963700006
ER
PT J
AU Hansen, J
Sato, M
Ruedy, R
AF Hansen, James
Sato, Makiko
Ruedy, Reto
TI Reply to Stone et al.: Human-made role in local temperature extremes
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Letter
C1 [Hansen, James; Sato, Makiko] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Hansen, James; Sato, Makiko] Columbia Univ, Earth Inst, New York, NY 10025 USA.
[Ruedy, Reto] Trinnovim LLC, New York, NY 10025 USA.
RP Hansen, J (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
EM james.e.hansen@nasa.gov
NR 4
TC 3
Z9 3
U1 0
U2 8
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 APR 23
PY 2013
VL 110
IS 17
BP E1544
EP E1544
DI 10.1073/pnas.1301494110
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 140TE
UT WOS:000318677300002
PM 23745185
ER
PT J
AU Galley, CR
AF Galley, Chad R.
TI Classical Mechanics of Nonconservative Systems
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
AB Hamilton's principle of stationary action lies at the foundation of theoretical physics and is applied in many other disciplines from pure mathematics to economics. Despite its utility, Hamilton's principle has a subtle pitfall that often goes unnoticed in physics: it is formulated as a boundary value problem in time but is used to derive equations of motion that are solved with initial data. This subtlety can have undesirable effects. I present a formulation of Hamilton's principle that is compatible with initial value problems. Remarkably, this leads to a natural formulation for the Lagrangian and Hamiltonian dynamics of generic nonconservative systems, thereby filling a long-standing gap in classical mechanics. Thus, dissipative effects, for example, can be studied with new tools that may have applications in a variety of disciplines. The new formalism is demonstrated by two examples of nonconservative systems: an object moving in a fluid with viscous drag forces and a harmonic oscillator coupled to a dissipative environment. DOI: 10.1103/PhysRevLett.110.174301
C1 [Galley, Chad R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Galley, Chad R.] CALTECH, Pasadena, CA 91125 USA.
RP Galley, CR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM crgalley@tapir.caltech.edu
FU Jet Propulsion Laboratory
FX I thank Y. Chen, C. Cutler, K. Hawbaker, A. Leibovich, H. Miao, E.
Poisson, I. Rothstein, G. Schafer, L. Stein, A. Tolley, M. Vallisneri,
and especially A. Zenginoglu for discussions and comments of previous
drafts. This work was supported in part by an appointment to the NASA
Postdoctoral Program at the Jet Propulsion Laboratory administered by
the Oak Ridge Associated Universities through a contract with NASA.
NR 15
TC 45
Z9 45
U1 0
U2 18
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD APR 22
PY 2013
VL 110
IS 17
AR 174301
DI 10.1103/PhysRevLett.110.174301
PG 5
WC Physics, Multidisciplinary
SC Physics
GA 129CK
UT WOS:000317815800009
PM 23679733
ER
PT J
AU Cantrell, JH
Yost, WT
AF Cantrell, John H.
Yost, William T.
TI Acoustic nonlinearity and cumulative plastic shear strain in cyclically
loaded metals
SO JOURNAL OF APPLIED PHYSICS
LA English
DT Article
ID WAVY SLIP METALS; HARMONIC-GENERATION; ULTRASONIC-WAVES; FATIGUE DAMAGE
AB Cyclic loading leads to microstructural changes in metals that result in substantial increases in the material nonlinearity. Two quite distinct approaches for quantifying the nonlinearity via a material nonlinearity parameter assessed directly from acoustic harmonic generation measurements have emerged-the Cantrell model and the model of Kim et al. The Cantrell model quantifies the nonlinearity in terms of lattice anharmonicity, dislocation plasticity, and crack growth as independent sources of nonlinearity arising from the accumulated plastic shear strain. The approach of Kim et al. links the cumulative plastic shear strain directly to a change in the third-order elastic constants of the material. We show that although the model of Kim et al. has the advantage of expediency, the Cantrell model reflects much more accurately the dependence of the nonlinearity parameter on the state of fatigue.
C1 [Cantrell, John H.; Yost, William T.] NASA, Res Directorate, Langley Res Ctr, Hampton, VA 23681 USA.
RP Cantrell, JH (reprint author), NASA, Res Directorate, Langley Res Ctr, Hampton, VA 23681 USA.
EM john.h.cantrell@nasa.gov; William.t.yost@nasa.gov
NR 19
TC 8
Z9 9
U1 0
U2 14
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0021-8979
J9 J APPL PHYS
JI J. Appl. Phys.
PD APR 21
PY 2013
VL 113
IS 15
AR 153506
DI 10.1063/1.4801885
PG 6
WC Physics, Applied
SC Physics
GA 134YJ
UT WOS:000318251400012
ER
PT J
AU Dobler, JT
Harrison, FW
Browell, EV
Lin, B
McGregor, D
Kooi, S
Choi, Y
Ismail, S
AF Dobler, Jeremy T.
Harrison, F. Wallace
Browell, Edward V.
Lin, Bing
McGregor, Doug
Kooi, Susan
Choi, Yonghoon
Ismail, Syed
TI Atmospheric CO2 column measurements with an airborne intensity-modulated
continuous wave 1.57 mu m fiber laser lidar
SO APPLIED OPTICS
LA English
DT Article
ID DIFFERENTIAL ABSORPTION LIDAR; CARBON-DIOXIDE; CW LIDAR; SYSTEM; SPACE
AB The 2007 National Research Council (NRC) Decadal Survey on Earth Science and Applications from Space recommended Active Sensing of CO2 Emissions over Nights, Days, and Seasons (ASCENDS) as a midterm, Tier II, NASA space mission. ITT Exelis, formerly ITT Corp., and NASA Langley Research Center have been working together since 2004 to develop and demonstrate a prototype laser absorption spectrometer for making high-precision, column CO2 mixing ratio measurements needed for the ASCENDS mission. This instrument, called the multifunctional fiber laser lidar (MFLL), operates in an intensity-modulated, continuous wave mode in the 1.57 mu m CO2 absorption band. Flight experiments have been conducted with the MFLL on a Lear-25, UC-12, and DC-8 aircraft over a variety of different surfaces and under a wide range of atmospheric conditions. Very high-precision CO2 column measurements resulting from high signal-to-noise ratio (>1300) column optical depth (OD) measurements for a 10 s (similar to 1 km) averaging interval have been achieved. In situ measurements of atmospheric CO2 profiles were used to derive the expected CO2 column values, and when compared to the MFLL measurements over desert and vegetated surfaces, the MFLL measurements were found to agree with the in situ-derived CO2 columns to within an average of 0.17% or similar to 0.65 ppmv with a standard deviation of 0.44% or similar to 1.7 ppmv. Initial results demonstrating ranging capability using a swept modulation technique are also presented. (C) 2013 Optical Society of America
C1 [Dobler, Jeremy T.; McGregor, Doug] Exelis Inc, Ft Wayne, IN 46818 USA.
[Harrison, F. Wallace; Lin, Bing; Ismail, Syed] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Browell, Edward V.] NASA, Langley Res Ctr, STARSS Affiliate 2, Hampton, VA 23681 USA.
[Kooi, Susan; Choi, Yonghoon] Sci Syst & Applicat Inc, Hampton, VA 23666 USA.
RP Dobler, JT (reprint author), Exelis Inc, 1919 W Cook Rd, Ft Wayne, IN 46818 USA.
EM Jeremy.Dobler@exelisinc.com
NR 43
TC 35
Z9 35
U1 4
U2 25
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
J9 APPL OPTICS
JI Appl. Optics
PD APR 20
PY 2013
VL 52
IS 12
BP 2874
EP 2892
DI 10.1364/AO.52.002874
PG 19
WC Optics
SC Optics
GA 130NB
UT WOS:000317923700044
PM 23669700
ER
PT J
AU Sorek-Hamer, M
Cohen, A
Levy, RC
Ziv, B
Broday, DM
AF Sorek-Hamer, M.
Cohen, A.
Levy, R. C.
Ziv, B.
Broday, D. M.
TI Classification of dust days by satellite remotely sensed aerosol
products
SO INTERNATIONAL JOURNAL OF REMOTE SENSING
LA English
DT Article
ID FINE PARTICULATE MATTER; GROUND-BASED MEASUREMENTS; AIR-POLLUTION;
OPTICAL DEPTH; PREDICTION SYSTEM; DAILY MORTALITY; HEART-DISEASE; MODIS;
QUALITY; PM2.5
AB Considerable progress in satellite remote sensing (SRS) of dust particles has been seen in the last decade. From an environmental health perspective, such an event detection, after linking it to ground particulate matter (PM) concentrations, can proxy acute exposure to respirable particles of certain properties (i.e. size, composition, and toxicity). Being affected considerably by atmospheric dust, previous studies in the Eastern Mediterranean, and in Israel in particular, have focused on mechanistic and synoptic prediction, classification, and characterization of dust events. In particular, a scheme for identifying dust days (DD) in Israel based on ground PM10 (particulate matter of size smaller than 10 m) measurements has been suggested, which has been validated by compositional analysis. This scheme requires information regarding ground PM10 levels, which is naturally limited in places with sparse ground-monitoring coverage. In such cases, SRS may be an efficient and cost-effective alternative to ground measurements. This work demonstrates a new model for identifying DD and non-DD (NDD) over Israel based on an integration of aerosol products from different satellite platforms (Moderate Resolution Imaging Spectroradiometer (MODIS) and Ozone Monitoring Instrument (OMI)). Analysis of ground-monitoring data from 2007 to 2008 in southern Israel revealed 67 DD, with more than 88% occurring during winter and spring. A Classification and Regression Tree (CART) model that was applied to a database containing ground monitoring (the dependent variable) and SRS aerosol product (the independent variables) records revealed an optimal set of binary variables for the identification of DD. These variables are combinations of the following primary variables: the calendar month, ground-level relative humidity (RH), the aerosol optical depth (AOD) from MODIS, and the aerosol absorbing index (AAI) from OMI. A logistic regression that uses these variables, coded as binary variables, demonstrated 93.2% correct classifications of DD and NDD. Evaluation of the combined CARTlogistic regression scheme in an adjacent geographical region (Gush Dan) demonstrated good results. Using SRS aerosol products for DD and NDD, identification may enable us to distinguish between health, ecological, and environmental effects that result from exposure to these distinct particle populations.
C1 [Sorek-Hamer, M.; Cohen, A.; Broday, D. M.] Technion Israel Inst Technol, Haifa, Israel.
[Levy, R. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Ziv, B.] Open Univ Israel, Raanana, Israel.
RP Broday, DM (reprint author), Technion Israel Inst Technol, Haifa, Israel.
EM dbroday@tx.technion.ac.il
RI Levy, Robert/M-7764-2013;
OI Levy, Robert/0000-0002-8933-5303; Broday, David/0000-0002-6525-3979
FU Israel Ministry of Science and Technology; Israel Council for Higher
Education
FX MSH was supported by scholarships from the Israel Ministry of Science
and Technology and from the Israel Council for Higher Education. Data
were obtained from the Goddard Earth Science Data Center in NASA GSFC,
Israel Ministry of Environment Protection, Israel Electric Company, and
the Ashdod-Ashkelon Association of Municipalities for the Environment.
The study was done within the Technion Center of Excellence in Exposure
Science and Environmental Health (TCEEH).
NR 56
TC 8
Z9 8
U1 1
U2 26
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 0143-1161
J9 INT J REMOTE SENS
JI Int. J. Remote Sens.
PD APR 20
PY 2013
VL 34
IS 8
BP 2672
EP 2688
DI 10.1080/01431161.2012.748991
PG 17
WC Remote Sensing; Imaging Science & Photographic Technology
SC Remote Sensing; Imaging Science & Photographic Technology
GA 109UG
UT WOS:000316393800002
ER
PT J
AU O'Connell, J
Connolly, J
Vermote, EF
Holden, NM
AF O'Connell, Jerome
Connolly, John
Vermote, Eric F.
Holden, Nicholas M.
TI Radiometric normalization for change detection in peatlands: a modified
temporal invariant cluster approach
SO INTERNATIONAL JOURNAL OF REMOTE SENSING
LA English
DT Article
ID ENHANCED VEGETATION INDEX; REPUBLIC-OF-IRELAND; LAND-COVER CHANGE;
CARBON STOCKS; TIME-SERIES; IMAGERY; MODIS; REFLECTANCE; REMOTE
AB Radiometric normalization is a vital stage in any change detection study due to the complex interactions of radiance and irradiance between the Earth's surface and atmosphere. Compensation for variables such as sun's angle, surface profile, atmospheric conditions, and sensor calibration coefficients are essential in achieving a radiometrically stable data base of multi-temporal, multi-spectral imagery for a change detection study. In this study, five Landsat Enhanced Thematic Mapper Plus (ETM+) images taken over the east coast of Ireland in 2001 were geometrically corrected and topographically normalized for further processing and analysis. Assessment of various vegetation indices showed that the enhanced vegetation index 2 (EVI2) gave the highest accuracy in identifying the various vegetation types and habitats in the Wicklow Mountains National Park. The initial analysis of radiometric normalization with temporal invariant clusters (TICs) gave poor results due to the spectral heterogeneity of urban pixels within each image. A revised TIC subset normalized method was developed using regional growth parameters in urban environments to limit the spatial and spectral extent of pixels used in the TIC scene normalization process. Correlation analysis between the TIC-subset-normalized ETM+ data and Landsat Ecosystem Disturbance Adaptive Processing System (LEDAPS) absolute corrected data produced coefficient of determination (R-2) values between 0.88 and 0.98. Such results demonstrated the robustness of the TIC subset normalization procedure when correcting for atmospheric variability between images while maintaining spectral integrity. Statistical analysis on master slave and TIC-subset-normalized slave data using cumulative distribution curves derived from image histograms showed an 86.93% reduction in the maximum difference between master and slave data due to the TIC subset normalization process. This procedure of radiometric normalization is suitable in landscapes with a low density of spectrally stable targets.
C1 [O'Connell, Jerome; Holden, Nicholas M.] Natl Univ Ireland Univ Coll Dublin, Sch Biosyst Engn, Agr & Food Sci Ctr, Dublin 4, Ireland.
[Connolly, John] Natl Univ Ireland Univ Coll Cork, Dept Geog, Cork, Ireland.
[Vermote, Eric F.] NASA, Goddard Space Flight Ctr, Terr Informat Syst Branch, Greenbelt, MD 20771 USA.
RP O'Connell, J (reprint author), Univ Leeds, Fac Biol Sci, Sch Biol, Leeds LS2 9JT, W Yorkshire, England.
EM J.O'Connell@leeds.ac.uk
RI Connolly, John/A-2925-2014; Connolly, John/A-8976-2013; O Connell,
Jerome/M-6517-2014
OI Connolly, John/0000-0002-2897-9711; Connolly, John/0000-0002-2897-9711;
O Connell, Jerome/0000-0002-4782-1549
FU Environmental Protection Agency of Ireland (EPA) under the STRIVE
fellowship
FX The authors wish to thank the Environmental Protection Agency of Ireland
(EPA) for their financial support under the STRIVE fellowship. The
authors also wish to thank the US Geological Survey for providing access
to the ETM+ data, as well as the NPWS for supplying habitat maps of the
Wicklow Mountains National Park.
NR 53
TC 6
Z9 6
U1 0
U2 13
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 0143-1161
J9 INT J REMOTE SENS
JI Int. J. Remote Sens.
PD APR 20
PY 2013
VL 34
IS 8
BP 2905
EP 2924
DI 10.1080/01431161.2012.752886
PG 20
WC Remote Sensing; Imaging Science & Photographic Technology
SC Remote Sensing; Imaging Science & Photographic Technology
GA 109UG
UT WOS:000316393800014
ER
PT J
AU Bentz, MC
Denney, KD
Grier, CJ
Barth, AJ
Peterson, BM
Vestergaard, M
Bennert, VN
Canalizo, G
De Rosa, G
Filippenko, AV
Gates, EL
Greene, JE
Li, WD
Malkan, MA
Pogge, RW
Stern, D
Treu, T
Woo, JH
AF Bentz, Misty C.
Denney, Kelly D.
Grier, Catherine J.
Barth, Aaron J.
Peterson, Bradley M.
Vestergaard, Marianne
Bennert, Vardha N.
Canalizo, Gabriela
De Rosa, Gisella
Filippenko, Alexei V.
Gates, Elinor L.
Greene, Jenny E.
Li, Weidong
Malkan, Matthew A.
Pogge, Richard W.
Stern, Daniel
Treu, Tommaso
Woo, Jong-Hak
TI THE LOW-LUMINOSITY END OF THE RADIUS-LUMINOSITY RELATIONSHIP FOR ACTIVE
GALACTIC NUCLEI
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: nuclei; galaxies: photometry; galaxies:
Seyfert
ID BROAD-LINE REGION; BLACK-HOLE MASSES; SEYFERT 1 GALAXIES; REVERBERATION
MAPPING DATA; BRIGHT QUASAR SURVEY; HOST-GALAXY; COSMIC EVOLUTION;
INTRINSIC SCATTER; SCALING RELATIONS; ASTRONOMICAL DATA
AB We present an updated and revised analysis of the relationship between the H beta broad-line region (BLR) radius and the luminosity of the active galactic nucleus (AGN). Specifically, we have carried out two-dimensional surface brightness decompositions of the host galaxies of nine new AGNs imaged with the Hubble Space Telescope Wide Field Camera 3. The surface brightness decompositions allow us to create "AGN-free" images of the galaxies, from which we measure the starlight contribution to the optical luminosity measured through the ground-based spectroscopic aperture. We also incorporate 20 new reverberation-mapping measurements of the H beta time lag, which is assumed to yield the average H beta BLR radius. The final sample includes 41 AGNs covering four orders of magnitude in luminosity. The additions and updates incorporated here primarily affect the low-luminosity end of the R-BLR-L relationship. The best fit to the relationship using a Bayesian analysis finds a slope of alpha = 0.533(-0.033)(+0.035), consistent with previous work and with simple photoionization arguments. Only two AGNs appear to be outliers from the relationship, but both of them have monitoring light curves that raise doubt regarding the accuracy of their reported time lags. The scatter around the relationship is found to be 0.19 +/- 0.02 dex, but would be decreased to 0.13 dex by the removal of these two suspect measurements. A large fraction of the remaining scatter in the relationship is likely due to the inaccurate distances to the AGN host galaxies. Our results help support the possibility that the R-BLR-L relationship could potentially be used to turn the BLRs of AGNs into standardizable candles. This would allow the cosmological expansion of the universe to be probed by a separate population of objects, and over a larger range of redshifts.
C1 [Bentz, Misty C.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA.
[Denney, Kelly D.; Vestergaard, Marianne] Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark.
[Grier, Catherine J.; Peterson, Bradley M.; De Rosa, Gisella; Pogge, Richard W.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Barth, Aaron J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Peterson, Bradley M.; Pogge, Richard W.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA.
[Vestergaard, Marianne] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Bennert, Vardha N.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 93407 USA.
[Canalizo, Gabriela] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[Filippenko, Alexei V.; Li, Weidong] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Gates, Elinor L.] Univ Calif Observ Lick Observ, Mt Hamilton, CA 95140 USA.
[Greene, Jenny E.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Malkan, Matthew A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Treu, Tommaso] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Woo, Jong-Hak] Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul, South Korea.
RP Bentz, MC (reprint author), Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA.
EM bentz@chara.gsu.edu
RI Woo, Jong-Hak/A-2790-2014; Vestergaard, Marianne/M-5247-2014;
OI Vestergaard, Marianne/0000-0001-9191-9837; Barth,
Aaron/0000-0002-3026-0562
FU Space Telescope Science Institute [HST GO-11662]; NASA [NAS5-26555];
European Union [300553]; NSF [AST-1108835, AST-1008882, AST-1108665,
AST-1211916]; TABASGO Foundation; Christopher R. Redlich Fund; National
Research Foundation of Korea (NRF); Korean government [2012-006087]
FX This work is based on observations with the NASA/ESA Hubble Space
Telescope. We are grateful for support of this work through grant HST
GO-11662 from the Space Telescope Science Institute, which is operated
by the Association of Universities for Research in Astronomy, Inc.,
under NASA contract NAS5-26555. K.D.D. has received funding from the
People Programme (Marie Curie Actions) of the European Union's Seventh
Framework Programme FP7/2007-2013/ under REA grant agreement No. 300553.
A.J.B. acknowledges support from NSF grant AST-1108835. B.M.P., C.J.G.,
G.D.R., and R.W.P. acknowledge support from NSF grant AST-1008882 to
Ohio State University. A.V.F. is grateful for the support of NSF grants
AST-1108665 and AST-1211916, the TABASGO Foundation, and the Christopher
R. Redlich Fund. The work of D.S. was carried out at Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
NASA. J.H.W. acknowledges the support by the National Research
Foundation of Korea (NRF) grant funded by the Korean government (No.
2012-006087). This research has made use of the NASA/IPAC Extragalactic
Database (NED) which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration and the SIMBAD database, operated
at CDS, Strasbourg, France. We dedicate this paper to the memory of our
dear friend and colleague, Weidong Li, whose tireless dedication to the
Katzman Automatic Imaging Telescope (KAIT) significantly contributed to
the success of LAMP; his premature, tragic passing has deeply saddened
us. We thank the Dark Cosmology Center for their hospitality during the
Improving Black Hole Masses in Active Galaxies workshop in July 2012,
which provided a venue for conversations that improved this work.
NR 102
TC 155
Z9 155
U1 0
U2 10
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2013
VL 767
IS 2
AR 149
DI 10.1088/0004-637X/767/2/149
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 122VR
UT WOS:000317346800052
ER
PT J
AU Heinze, AN
Metchev, S
Apai, D
Flateau, D
Kurtev, R
Marley, M
Radigan, J
Burgasser, AJ
Artigau, E
Plavchan, P
AF Heinze, Aren N.
Metchev, Stanimir
Apai, Daniel
Flateau, Davin
Kurtev, Radostin
Marley, Mark
Radigan, Jacqueline
Burgasser, Adam J.
Artigau, Etienne
Plavchan, Peter
TI WEATHER ON OTHER WORLDS. I. DETECTION OF PERIODIC VARIABILITY IN THE L3
DWARF DENIS-P J1058.7-1548 WITH PRECISE MULTI-WAVELENGTH PHOTOMETRY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE brown dwarfs; stars: individual (DENIS-P J1058.7-1548); stars: low-mass;
stars: rotation starspots; stars: variables: general; techniques:
photometric
ID EFFECTIVE TEMPERATURE SCALE; TIME-SERIES OBSERVATIONS; BRIGHT ULTRACOOL
DWARFS; SPITZER-SPACE-TELESCOPE; INFRARED ARRAY CAMERA; SKY SURVEY
2MASS; SPECTRAL TYPE-L; LOW-MASS STARS; BROWN DWARF; T-DWARFS
AB Photometric monitoring from warm Spitzer reveals that the L3 dwarf DENIS-P J1058.7-1548 varies sinusoidally in brightness with a period of 4.25(-0.16)(+0.26) hr and an amplitude of 0.388% +/- 0.043% (peak-to-valley) in the 3.6 mu m band, confirming the reality of a 4.31 +/- 0.31 hr periodicity detected in J-band photometry from the SOAR telescope. The J-band variations are a factor of 2.17 +/- 0.35 larger in amplitude than those at 3.6 mu m, while 4.5 mu m Spitzer observations yield a 4.5 mu m/3.6 mu m amplitude ratio of only 0.23 +/- 0.15, consistent with zero 4.5 mu m variability. This wide range in amplitudes indicates rotationally modulated variability due to magnetic phenomena and/or inhomogeneous cloud cover. Weak Ha emission indicates some magnetic activity, but it is difficult to explain the observed amplitudes by magnetic phenomena unless they are combined with cloud inhomogeneities (which might have a magnetic cause). However, inhomogeneous cloud cover alone can explain all our observations, and our data align with theory in requiring that the regions with the thickest clouds also have the lowest effective temperature. Combined with published v sin(i) results, our rotation period yields a 95% confidence lower limit of R-* >= 0.111 R-circle dot, suggesting upper limits of 320 Myr and 0.055 M-circle dot on the age and mass. These limits should be regarded cautiously because of similar to 3 sigma inconsistencies with other data; however, a lower limit of 45 degrees. on the inclination is more secure. DENIS-P J1058.7-1548 is only the first of nearly two dozen low-amplitude variables discovered and analyzed by the Weather on Other Worlds project.
C1 [Heinze, Aren N.; Metchev, Stanimir] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Apai, Daniel; Flateau, Davin] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
[Apai, Daniel; Flateau, Davin] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Apai, Daniel; Flateau, Davin] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Kurtev, Radostin] Univ Valparaiso, Fac Ciencias, Dept Fis & Astron, Valparaiso, Chile.
[Marley, Mark] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Radigan, Jacqueline] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Burgasser, Adam J.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Artigau, Etienne] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Artigau, Etienne] Univ Montreal, Observ Mt Megantic, Montreal, PQ H3C 3J7, Canada.
[Plavchan, Peter] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
RP Heinze, AN (reprint author), SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
EM aren.heinze@stonybrook.edu; stanimir.metchev@stonybrook.edu
RI Marley, Mark/I-4704-2013;
OI Marley, Mark/0000-0002-5251-2943
FU NASA through the Spitzer Exploration Science Program Weather on Other
Worlds (program) [GO 80179]; ADAP [NNX11AB18G]; Proyecto [DIUV23/2009];
Centro de Astrofisica de Valparaiso; FONDECYT [1130140]; Space Telescope
Science Institute under U.S. Government [NAG W-2166]
FX We thank Didier Saumon for supplying us with files containing the model
spectra of Saumon & Marley (2008), which we have used to construct our
two-phase models of DENIS 1058. This research was supported by NASA
through the Spitzer Exploration Science Program Weather on Other Worlds
(program GO 80179) and ADAP award NNX11AB18G. This research is also
based on observations obtained at the Southern Astrophysical Research
(SOAR) telescope, which is a joint project of the Ministerio da Ciencia,
Tecnologia, e Inovacao (MCTI) da Republica Federativa do Brasil, the U.
S. National Optical Astronomy Observatory (NOAO), the University of
North Carolina at Chapel Hill (UNC), and Michigan State University
(MSU). The SOAR observations reported herein were made under Chilean
program CN2012A-055. Radostin Kurtev acknowledges support from Proyecto
DIUV23/2009, Centro de Astrofisica de Valparaiso, and FONDECYT through
grant 1130140. We thank Nikole Lewis for supplying us with IDL code to
measure the noise pixel parameter of our data, for allowing us to read
the draft version of her paper describing uses of this parameter in IRAC
photometry, and for additional helpful advice. This publication makes
use of the SIMBAD online database, operated at CDS, Strasbourg, France,
and the VizieR online database (see Ochsenbein et al. 2000). This
publication makes use of data products from the Two Micron All Sky
Survey, which is a joint project of the University of Massachusetts and
the Infrared Processing and Analysis Center/ California Institute of
Technology, funded by the National Aeronautics and Space Administration
and the National Science Foundation. We have also made extensive use of
information and code from Press et al. (1992). We have used digitized
images from the Palomar Sky Survey (available from
http://stdatu.stsci.edu/cgi-bin/dss_form), which were produced at the
Space Telescope Science Institute under U.S. Government grant NAG
W-2166. The images of these surveys are based on photographic data
obtained using the Oschin Schmidt Telescope on Palomar Mountain and the
UK Schmidt Telescope.
NR 86
TC 27
Z9 27
U1 1
U2 9
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2013
VL 767
IS 2
AR 173
DI 10.1088/0004-637X/767/2/173
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 122VR
UT WOS:000317346800076
ER
PT J
AU Huber, D
Chaplin, WJ
Christensen-Dalsgaard, J
Gilliland, RL
Kjeldsen, H
Buchhave, LA
Fischer, DA
Lissauer, JJ
Rowe, JF
Sanchis-Ojeda, R
Basu, S
Handberg, R
Hekker, S
Howard, AW
Isaacson, H
Karoff, C
Latham, DW
Lund, MN
Lundkvist, M
Marcy, GW
Miglio, A
Aguirre, VS
Stello, D
Arentoft, T
Barclay, T
Bedding, TR
Burke, CJ
Christiansen, JL
Elsworth, YP
Haas, MR
Kawaler, SD
Metcalfe, TS
Mullally, F
Thompson, SE
AF Huber, Daniel
Chaplin, William J.
Christensen-Dalsgaard, Jorgen
Gilliland, Ronald L.
Kjeldsen, Hans
Buchhave, Lars A.
Fischer, Debra A.
Lissauer, Jack J.
Rowe, Jason F.
Sanchis-Ojeda, Roberto
Basu, Sarbani
Handberg, Rasmus
Hekker, Saskia
Howard, Andrew W.
Isaacson, Howard
Karoff, Christoffer
Latham, David W.
Lund, Mikkel N.
Lundkvist, Mia
Marcy, Geoffrey W.
Miglio, Andrea
Aguirre, Victor Silva
Stello, Dennis
Arentoft, Torben
Barclay, Thomas
Bedding, Timothy R.
Burke, Christopher J.
Christiansen, Jessie L.
Elsworth, Yvonne P.
Haas, Michael R.
Kawaler, Steven D.
Metcalfe, Travis S.
Mullally, Fergal
Thompson, Susan E.
TI FUNDAMENTAL PROPERTIES OF KEPLER PLANET-CANDIDATE HOST STARS USING
ASTEROSEISMOLOGY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: late-type; stars: oscillations; techniques:
photometric; techniques: spectroscopic
ID SOLAR-LIKE OSCILLATIONS; TRANSIT TIMING OBSERVATIONS; 1ST 4 MONTHS;
STELLAR EVOLUTION DATABASE; FINE GUIDANCE SENSOR; MAIN-SEQUENCE STARS;
RED-GIANT STARS; SUN-LIKE STAR; EXTRASOLAR PLANETS; INPUT CATALOG
AB We have used asteroseismology to determine fundamental properties for 66 Kepler planet-candidate host stars, with typical uncertainties of 3% and 7% in radius and mass, respectively. The results include new asteroseismic solutions for four host stars with confirmed planets (Kepler-4, Kepler-14, Kepler-23 and Kepler-25) and increase the total number of Kepler host stars with asteroseismic solutions to 77. A comparison with stellar properties in the planet-candidate catalog by Batalha et al. shows that radii for subgiants and giants obtained from spectroscopic follow-up are systematically too low by up to a factor of 1.5, while the properties for unevolved stars are in good agreement. We furthermore apply asteroseismology to confirm that a large majority of cool main-sequence hosts are indeed dwarfs and not misclassified giants. Using the revised stellar properties, we recalculate the radii for 107 planet candidates in our sample, and comment on candidates for which the radii change from a previously giant-planet/brown-dwarf/stellar regime to a sub-Jupiter size or vice versa. A comparison of stellar densities from asteroseismology with densities derived from transit models in Batalha et al. assuming circular orbits shows significant disagreement for more than half of the sample due to systematics in the modeled impact parameters or due to planet candidates that may be in eccentric orbits. Finally, we investigate tentative correlations between host-star masses and planet-candidate radii, orbital periods, and multiplicity, but caution that these results may be influenced by the small sample size and detection biases.
C1 [Huber, Daniel; Lissauer, Jack J.; Rowe, Jason F.; Barclay, Thomas; Burke, Christopher J.; Christiansen, Jessie L.; Haas, Michael R.; Mullally, Fergal; Thompson, Susan E.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Chaplin, William J.; Miglio, Andrea; Elsworth, Yvonne P.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Chaplin, William J.; Christensen-Dalsgaard, Jorgen; Kjeldsen, Hans; Handberg, Rasmus; Karoff, Christoffer; Lund, Mikkel N.; Lundkvist, Mia; Aguirre, Victor Silva; Stello, Dennis; Arentoft, Torben; Bedding, Timothy R.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark.
[Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
[Fischer, Debra A.; Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Sanchis-Ojeda, Roberto] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Hekker, Saskia] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Isaacson, Howard; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Stello, Dennis; Bedding, Timothy R.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
[Kawaler, Steven D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Metcalfe, Travis S.] Space Sci Inst, Boulder, CO 80301 USA.
RP Huber, D (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM daniel.huber@nasa.gov
RI Howard, Andrew/D-4148-2015;
OI Lund, Mikkel Norup/0000-0001-9214-5642; Lundkvist, Mia
Sloth/0000-0002-8661-2571; Fischer, Debra/0000-0003-2221-0861; Handberg,
Rasmus/0000-0001-8725-4502; Kawaler, Steven/0000-0002-6536-6367; Howard,
Andrew/0000-0001-8638-0320; Bedding, Timothy/0000-0001-5943-1460;
Buchhave, Lars A./0000-0003-1605-5666; Metcalfe,
Travis/0000-0003-4034-0416; Karoff, Christoffer/0000-0003-2009-7965;
Bedding, Tim/0000-0001-5222-4661; Basu, Sarbani/0000-0002-6163-3472
FU NASA's Science Mission Directorate; NSF [AST-1105930]; Netherlands
Organisation for Scientific Research (NWO); NASA [NNX13AE91G]; Danish
National Research Foundation [DNRF106]; ASTERISK project (ASTERoseismic
Investigations with SONG and Kepler); European Research Council [267864]
FX We thank Willie Torres, Josh Winn, and our anonymous referee for helpful
comments and discussions. We furthermore gratefully acknowledge the
entire Kepler team and everyone involved in the Kepler mission for
making this paper possible. Funding for the Kepler mission is provided
by NASA's Science Mission Directorate. D.H. is supported by an
appointment to the NASA Postdoctoral Program at Ames Research Center,
administered by Oak Ridge Associated Universities through a contract
with NASA. S.B. acknowledges NSF grant AST-1105930. S.H. acknowledges
financial support from the Netherlands Organisation for Scientific
Research (NWO). T.S.M. acknowledges NASA grant NNX13AE91G. Funding for
the Stellar Astrophysics Centre is provided by The Danish National
Research Foundation (Grant DNRF106). The research is supported by the
ASTERISK project (ASTERoseismic Investigations with SONG and Kepler)
funded by the European Research Council (Grant agreement No.: 267864).
NR 153
TC 108
Z9 108
U1 1
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2013
VL 767
IS 2
AR 127
DI 10.1088/0004-637X/767/2/127
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 122VR
UT WOS:000317346800030
ER
PT J
AU Nissanke, S
Kasliwal, M
Georgieva, A
AF Nissanke, Samaya
Kasliwal, Mansi
Georgieva, Alexandra
TI IDENTIFYING ELUSIVE ELECTROMAGNETIC COUNTERPARTS TO GRAVITATIONAL WAVE
MERGERS: AN END-TO-END SIMULATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: close; catalogs; gamma-ray burst: general; gravitational
waves; stars: neutron; surveys Online-only material: color figures
ID GAMMA-RAY BURSTS; NEUTRON-STAR MERGERS; OBSERVATORY SUPERNOVA SEARCH;
COMPACT OBJECT MERGERS; HOST GALAXY; BINARY INSPIRALS; TRANSIENT EVENTS;
DRIVEN WIND; JET BREAKS; R-PROCESS
AB Combined gravitational wave (GW) and electromagnetic (EM) observations of compact binary mergers should enable detailed studies of astrophysical processes in the strong-field gravity regime. This decade, ground-based GW interferometers promise to routinely detect compact binary mergers. Unfortunately, networks of GW interferometers have poor angular resolution on the sky and their EM signatures are predicted to be faint. Therefore, a challenging goal will be to unambiguously pinpoint the EM counterparts of GW mergers. We perform the first comprehensive end-to-end simulation that focuses on: (1) GW sky localization, distance measures, and volume errors with two compact binary populations and four different GW networks; (2) subsequent EM detectability by a slew of multiwavelength telescopes; and (3) final identification of the merger counterpart amidst a sea of possible astrophysical false positives. First, we find that double neutron star binary mergers can be detected out to a maximum distance of 400 Mpc (or 750 Mpc) by three (or five) detector GW networks, respectively. Neutron-star-black-hole binary mergers can be detected a factor of 1.5 further out; their median to maximum sky localizations are 50-170 deg(2) (or 6-65 deg(2)) for a three (or five) detector GW network. Second, by optimizing depth, cadence, and sky area, we quantify relative fractions of optical counterparts that are detectable by a suite of different aperture-size telescopes across the globe. Third, we present five case studies to illustrate the diversity of scenarios in secure identification of the EM counterpart. We discuss the case of a typical binary, neither beamed nor nearby, and the challenges associated with identifying an EM counterpart at both low and high Galactic latitudes. For the first time, we demonstrate how construction of low-latency GW volumes in conjunction with local universe galaxy catalogs can help solve the problem of false positives. We conclude with strategies that would best prepare us for successfully identifying the elusive EM counterpart of a GW merger.
C1 [Nissanke, Samaya; Georgieva, Alexandra] CALTECH, Pasadena, CA 91125 USA.
[Nissanke, Samaya] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kasliwal, Mansi] Carnegie Inst Sci, Pasadena, CA 91101 USA.
RP Nissanke, S (reprint author), CALTECH, Pasadena, CA 91125 USA.
FU National Aeronautics and Space Administration
FX We are very grateful to Jean-Michel Desert, Dale Frail, Chris Hirata,
Shri Kulkarni, and Setu Mohta for careful reading of the manuscript. We
thank Ernazar Abdikamalov, Paul Groot, Gregg Hallinan, Brian Metzger,
Sterl Phinney, Tony Piro, Tom Prince, Jon Sievers, and Linqing Wen for
useful discussions. S.M.N. thanks the ITC for hospitality and
discussions there with Edo Berger and Josh Grindlay. We thank Anand
Sengupta and Tarun Souradeep for providing LIGO India's (previously
referred to as IndIGO) position and orientation. We thank Haixing Miao
for providing the anticipated advanced LIGO noise curve with optical
squeezing and Masaki Ando, Larry Price, and Stan Whitcomb for KAGRA and
LIGO follow-up references. We thank Neil Gehrels, David Kaplan, Peter
Nugent, and Fang Yuan for providing specifications of Lobster-ISS, WIYN,
La Silla Quest, and Skymapper, respectively. Some of the simulations
were performed using the Sunnyvale cluster at CITA. Part of this work
was performed at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration. Government sponsorship acknowledged.
NR 117
TC 103
Z9 103
U1 0
U2 7
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 APR 20
PY 2013
VL 767
IS 2
AR 124
DI 10.1088/0004-637X/767/2/124
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 122VR
UT WOS:000317346800027
ER
PT J
AU Quintana, EV
Rowe, JF
Barclay, T
Howell, SB
Ciardi, DR
Demory, BO
Caldwell, DA
Borucki, WJ
Christiansen, JL
Jenkins, JM
Klaus, TC
Fulton, BJ
Morris, RL
Sanderfer, DT
Shporer, A
Smith, JC
Still, M
Thompson, SE
AF Quintana, Elisa V.
Rowe, Jason F.
Barclay, Thomas
Howell, Steve B.
Ciardi, David R.
Demory, Brice-Olivier
Caldwell, Douglas A.
Borucki, William J.
Christiansen, Jessie L.
Jenkins, Jon M.
Klaus, Todd C.
Fulton, Benjamin J.
Morris, Robert L.
Sanderfer, Dwight T.
Shporer, Avi
Smith, Jeffrey C.
Still, Martin
Thompson, Susan E.
TI CONFIRMATION OF HOT JUPITER KEPLER-41b VIA PHASE CURVE ANALYSIS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; techniques: photometric
ID EXTRASOLAR GIANT PLANETS; ATMOSPHERIC CHARACTERIZATION; ELLIPSOIDAL
VARIATIONS; SOPHIE VELOCIMETRY; LIGHT CURVES; HIGH ALBEDO; LOW-MASS;
COMPANIONS; PHOTOMETRY; DISCOVERY
AB We present high precision photometry of Kepler-41, a giant planet in a 1.86 day orbit around a G6V star that was recently confirmed through radial velocity measurements. We have developed a new method to confirm giant planets solely from the photometric light curve, and we apply this method herein to Kepler-41 to establish the validity of this technique. We generate a full phase photometric model by including the primary and secondary transits, ellipsoidal variations, Doppler beaming, and reflected/emitted light from the planet. Third light contamination scenarios that can mimic a planetary transit signal are simulated by injecting a full range of dilution values into the model, and we re-fit each diluted light curve model to the light curve. The resulting constraints on the maximum occultation depth and stellar density combined with stellar evolution models rules out stellar blends and provides a measurement of the planet's mass, size, and temperature. We expect about two dozen Kepler giant planets can be confirmed via this method.
C1 [Quintana, Elisa V.; Rowe, Jason F.; Caldwell, Douglas A.; Christiansen, Jessie L.; Jenkins, Jon M.; Morris, Robert L.; Smith, Jeffrey C.; Thompson, Susan E.] SETI Inst, Mountain View, CA 94043 USA.
[Barclay, Thomas] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
[Howell, Steve B.; Borucki, William J.; Sanderfer, Dwight T.; Still, Martin] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Ciardi, David R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Demory, Brice-Olivier] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Klaus, Todd C.] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
[Fulton, Benjamin J.; Shporer, Avi] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA.
[Fulton, Benjamin J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
RP Quintana, EV (reprint author), SETI Inst, 189 Bernardo Ave,Suite 100, Mountain View, CA 94043 USA.
EM elisa.quintana@nasa.gov
RI Caldwell, Douglas/L-7911-2014;
OI Caldwell, Douglas/0000-0003-1963-9616; Ciardi,
David/0000-0002-5741-3047; Demory, Brice-Olivier/0000-0002-9355-5165
FU NASA Science Mission directorate; NASA [NAS5-26555]; NASA Office of
Space Science [NNX09AF08G]
FX This paper includes data collected by the Kepler mission. Funding for
the Kepler mission is provided by the NASA Science Mission directorate.
Some/all of the data presented in this paper were obtained from the
Mikulski Archive for Space Telescopes (MAST). STScI is operated by the
Association of Universities for Research in Astronomy, Inc., under NASA
contract NAS5-26555. Support for MAST for non-HST data is provided by
the NASA Office of Space Science via grant NNX09AF08G and by other
grants and contracts.
NR 45
TC 19
Z9 19
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2013
VL 767
IS 2
AR 137
DI 10.1088/0004-637X/767/2/137
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 122VR
UT WOS:000317346800040
ER
PT J
AU Titarchuk, L
Seifina, E
Frontera, F
AF Titarchuk, Lev
Seifina, Elena
Frontera, Filippo
TI SPECTRAL STATE EVOLUTION OF 4U 1820-30: THE STABILITY OF THE SPECTRAL
INDEX OF THE COMPTONIZATION TAIL
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; radiation mechanisms:
non-thermal; stars: individual (4U 1820-30)
ID X-RAY BINARIES; QUASI-PERIODIC OSCILLATIONS; ENERGY CONCENTRATOR
SPECTROMETER; PHOTOSPHERIC RADIUS EXPANSION; BLACK-HOLE BINARIES;
NEUTRON-STAR; ASTRONOMY SATELLITE; TIMING EXPLORER; MXB 1728-34;
XMM-NEWTON
AB We analyze the X-ray spectra and their timing properties of the compact X-ray binary 4U 1820-30. We establish spectral transitions in this source seen with BeppoSAX and the Rossi X-ray Timing Explorer (RXTE). During the RXTE observations (1996-2009), the source was in the soft state approximately similar to 75% of the time making the lower banana and upper banana transitions combined with long-term low-high state transitions. We reveal that all of the X-ray spectra of 4U 1820-30 are fit by a combination of a thermal (Blackbody) component, a Comptonization component (COMPTB), and a Gaussian-line component. Thus, using this spectral analysis, we find that the photon power-law index Gamma of the Comptonization component is almost unchangeable (Gamma similar to 2), while the electron temperature kT(e) changes from 2.9 to 21 keV during these spectral events. We also establish that for these spectral events the normalization of the COMPTB component (which is proportional to the mass accretion rate (M) over dot) increases by a factor of eight when kT(e) decreases from 21 keV to 2.9 keV. Previously, this index stability effect was also found analyzing X-ray data for the Z-source GX 340+0 and for the atolls 4U 1728-34 and GX 3+1. Thus, we can suggest that this spectral stability property is a spectral signature of an accreting neutron star source. On the other hand, in a black hole binary Gamma monotonically increases with (M) over dot and ultimately its value saturates at large (M) over dot.
C1 [Titarchuk, Lev; Frontera, Filippo] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy.
[Titarchuk, Lev] George Mason Univ, Fairfax, VA 22030 USA.
[Titarchuk, Lev] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
[Seifina, Elena] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia.
RP Titarchuk, L (reprint author), Univ Ferrara, Dipartimento Fis, Via Saragat 1, I-44122 Ferrara, Italy.
EM titarchuk@fe.infn.it; seif@sai.msu.ru; frontera@fe.infn.it
NR 64
TC 8
Z9 8
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2013
VL 767
IS 2
AR 160
DI 10.1088/0004-637X/767/2/160
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 122VR
UT WOS:000317346800063
ER
PT J
AU Winebarger, A
Tripathi, D
Mason, HE
Del Zanna, G
AF Winebarger, Amy
Tripathi, Durgesh
Mason, Helen E.
Del Zanna, Giulio
TI DOPPLER SHIFTS IN ACTIVE REGION MOSS USING SOHO/SUMER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: atmosphere; Sun: corona; Sun: transition region; Sun: UV radiation
ID EUV IMAGING SPECTROMETER; TRANSITION-REGION; CORONAL-EXPLORER; HINODE
EIS; SUMER TELESCOPE; LOOP MODELS; DYNAMICS; FLOWS; RESOLUTION; SPECTRUM
AB The velocity of the plasma at the footpoint of hot loops in active region cores can be used to discriminate between different heating frequencies. Velocities on the order of a few kilometers per second would indicate low-frequency heating on sub-resolution strands, while velocities close to zero would indicate high-frequency (steady) heating. To discriminate between these two values requires accurate velocity measurements; previous velocity measurements suffer from large uncertainties, mainly due to the lack of an absolute wavelength reference scale. In this paper, we determine the velocity in the loop footpoints using observations from Solar Ultraviolet Measurements of Emitted Radiation (SUMER) on Solar and Heliospheric Observatory. We use neutral spectral lines to determine the wavelength scale of the observations with an uncertainty in the absolute velocity of <3.5 km s(-1) and co-aligned Transition Region and Coronal Explorer (TRACE) images to identify footpoint regions. We studied three different active regions and found average redshifts in the Ne VIII 770 angstrom emission line (formed at 6 x 10(5) K) of 5.17 +/- 5.37 km s(-1) and average redshifts in the C IV 1548 and 1550 angstrom emission lines (formed at 1 x 10(5) K) of 13.94 +/- 4.93 km s(-1) and 14.91 +/- 6.09 km s(-1), respectively. We find no correlation between the brightness in the spectral line and the measured velocity, nor do we find correlation between the Ne VIII and C IV velocities measured co-spatially and co-temporally. SUMER scanned two of the active regions twice; in those active regions we find positive correlation between the co-spatial velocities measured during the first and second scans. These results provide definitive and quantitative measurements for comparisons with simulations of different coronal heating mechanisms.
C1 [Winebarger, Amy] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Tripathi, Durgesh] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Mason, Helen E.; Del Zanna, Giulio] Univ Cambridge, Dept Appl Math & Theoret Phys, Cambridge CB3 0WA, England.
RP Winebarger, A (reprint author), NASA, George C Marshall Space Flight Ctr, VP 62, Huntsville, AL 35812 USA.
RI Tripathi, Durgesh/D-9390-2012
OI Tripathi, Durgesh/0000-0003-1689-6254
FU NASA SRT program; DST under Fast Track Scheme [SERB/F/3369/2012-2013];
STFC (UK)
FX A.R.W. was supported by the NASA SR&T program for this work. D. T.
acknowledges the support from DST under Fast Track Scheme
(SERB/F/3369/2012-2013). G.D.Z. and H. E. M. acknowledge support from
STFC (UK). SOHO is a mission of international collaboration between ESA
and NASA.
NR 50
TC 8
Z9 8
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2013
VL 767
IS 2
AR 107
DI 10.1088/0004-637X/767/2/107
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 122VR
UT WOS:000317346800010
ER
PT J
AU Sonbas, E
MacLachlan, GA
Shenoy, A
Dhuga, KS
Parke, WC
AF Sonbas, E.
MacLachlan, G. A.
Shenoy, A.
Dhuga, K. S.
Parke, W. C.
TI A NEW CORRELATION BETWEEN GRB X-RAY FLARES AND THE PROMPT EMISSION
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE gamma-ray burst: general; methods: data analysis
ID INTERNAL SHOCKS; ENGINE ACTIVITY; LIGHT CURVES; BURSTS; SWIFT;
VARIABILITY; MODEL; LONG; LUMINOSITY; LAG
AB From a sample of gamma-ray bursts (GRBs) detected by the Fermi and Swift missions, we have extracted the minimum variability timescales for temporal structures in the light curves associated with the prompt emission and X-ray flares. A comparison of this variability timescale with pulse parameters such as rise times, determined via pulse-fitting procedures, and spectral lags, extracted via the cross-correlation function, indicates a tight correlation between these temporal features for both the X-ray flares and the prompt emission. These correlations suggest a common origin for the production of X-ray flares and the prompt emission in GRBs.
C1 [Sonbas, E.] Adiyaman Univ, Dept Phys, TR-02040 Adiyaman, Turkey.
[Sonbas, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[MacLachlan, G. A.; Shenoy, A.; Dhuga, K. S.; Parke, W. C.] George Washington Univ, Dept Phys, Washington, DC 20052 USA.
RP Sonbas, E (reprint author), Adiyaman Univ, Dept Phys, TR-02040 Adiyaman, Turkey.
EM edasonbas@yahoo.com
FU Swift mission
FX This work made use of data supplied by the UK Swift Science Data Centre
at the University of Leicester. The work of E.S. was partially supported
through the Swift mission (PI: N. Gehrels) and is gratefully
acknowledged.
NR 30
TC 2
Z9 2
U1 0
U2 9
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 20
PY 2013
VL 767
IS 2
AR L28
DI 10.1088/2041-8205/767/2/L28
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 123SN
UT WOS:000317411100008
ER
PT J
AU Blaber, EA
Dvorochkin, N
Lee, C
Alwood, JS
Yousuf, R
Pianetta, P
Globus, RK
Burns, BP
Almeida, EAC
AF Blaber, Elizabeth A.
Dvorochkin, Natalya
Lee, Chialing
Alwood, Joshua S.
Yousuf, Rukhsana
Pianetta, Piero
Globus, Ruth K.
Burns, Brendan P.
Almeida, Eduardo A. C.
TI Microgravity Induces Pelvic Bone Loss through Osteoclastic Activity,
Osteocytic Osteolysis, and Osteoblastic Cell Cycle Inhibition by
CDKN1a/p21
SO PLOS ONE
LA English
DT Article
ID MATRIX METALLOPROTEINASES MMPS; SKELETAL-MUSCLE; GENE-EXPRESSION;
TRABECULAR BONE; SPACE-FLIGHT; SIMULATED MICROGRAVITY; GROWING RATS;
BED-REST; TGF-BETA; IN-VITRO
AB Bone is a dynamically remodeled tissue that requires gravity-mediated mechanical stimulation for maintenance of mineral content and structure. Homeostasis in bone occurs through a balance in the activities and signaling of osteoclasts, osteoblasts, and osteocytes, as well as proliferation and differentiation of their stem cell progenitors. Microgravity and unloading are known to cause osteoclast-mediated bone resorption; however, we hypothesize that osteocytic osteolysis, and cell cycle arrest during osteogenesis may also contribute to bone loss in space. To test this possibility, we exposed 16-week-old female C57BL/6J mice (n = 8) to microgravity for 15-days on the STS-131 space shuttle mission. Analysis of the pelvis by mu CT shows decreases in bone volume fraction (BV/TV) of 6.29%, and bone thickness of 11.91%. TRAP-positive osteoclast-covered trabecular bone surfaces also increased in microgravity by 170% (p = 0.004), indicating osteoclastic bone degeneration. High-resolution X-ray nanoCT studies revealed signs of lacunar osteolysis, including increases in cross-sectional area (+17%, p = 0.022), perimeter (+14%, p = 0.008), and canalicular diameter (+6%, p = 0.037). Expression of matrix metalloproteinases (MMP) 1, 3, and 10 in bone, as measured by RT-qPCR, was also up-regulated in microgravity (+12.94, +2.98 and +16.85 fold respectively, p<0.01), with MMP10 localized to osteocytes, and consistent with induction of osteocytic osteolysis. Furthermore, expression of CDKN1a/p21 in bone increased 3.31 fold (p<0.01), and was localized to osteoblasts, possibly inhibiting the cell cycle during tissue regeneration as well as conferring apoptosis resistance to these cells. Finally the apoptosis inducer Trp53 was down-regulated by -1.54 fold (p<0.01), possibly associated with the quiescent survival-promoting function of CDKN1a/p21. In conclusion, our findings identify the pelvic and femoral region of the mouse skeleton as an active site of rapid bone loss in microgravity, and indicate that this loss is not limited to osteoclastic degradation. Therefore, this study offers new evidence for microgravity-induced osteocytic osteolysis, and CDKN1a/p21-mediated osteogenic cell cycle arrest.
C1 [Blaber, Elizabeth A.; Dvorochkin, Natalya; Lee, Chialing; Alwood, Joshua S.; Yousuf, Rukhsana; Globus, Ruth K.; Almeida, Eduardo A. C.] NASA, Ames Res Ctr, Space Biosci Div, Moffett Field, CA 94035 USA.
[Blaber, Elizabeth A.; Burns, Brendan P.] Univ New S Wales, Sch Biotechnol & Biomol Sci, Sydney, NSW, Australia.
[Pianetta, Piero] SLAC Natl Accelerator Lab, Stanford Synchrotron Radiat Lightsource, Menlo Pk, CA USA.
RP Almeida, EAC (reprint author), NASA, Ames Res Ctr, Space Biosci Div, Moffett Field, CA 94035 USA.
EM e.almeida@nasa.gov
OI BURNS, BRENDAN/0000-0002-2962-2597
FU [NASA-NNH08ZTT003]
FX This work was supported by NASA-NNH08ZTT003. The funders had no role in
study design, data collection and analysis, decision to publish, or
preparation of the manuscript.
NR 75
TC 34
Z9 37
U1 2
U2 36
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 APR 18
PY 2013
VL 8
IS 4
AR e61372
DI 10.1371/journal.pone.0061372
PG 15
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 130IU
UT WOS:000317908700027
PM 23637819
ER
PT J
AU Riechers, DA
Bradford, CM
Clements, DL
Dowell, CD
Perez-Fournon, I
Ivison, RJ
Bridge, C
Conley, A
Fu, H
Vieira, JD
Wardlow, J
Calanog, J
Cooray, A
Hurley, P
Neri, R
Kamenetzky, J
Aguirre, JE
Altieri, B
Arumugam, V
Benford, DJ
Bethermin, M
Bock, J
Burgarella, D
Cabrera-Lavers, A
Chapman, SC
Cox, P
Dunlop, JS
Earle, L
Farrah, D
Ferrero, P
Franceschini, A
Gavazzi, R
Glenn, J
Solares, EAG
Gurwell, MA
Halpern, M
Hatziminaoglou, E
Hyde, A
Ibar, E
Kovacs, A
Krips, M
Lupu, RE
Maloney, PR
Martinez-Navajas, P
Matsuhara, H
Murphy, EJ
Naylor, BJ
Nguyen, HT
Oliver, SJ
Omont, A
Page, MJ
Petitpas, G
Rangwala, N
Roseboom, IG
Scott, D
Smith, AJ
Staguhn, JG
Streblyanska, A
Thomson, AP
Valtchanov, I
Viero, M
Wang, L
Zemcov, M
Zmuidzinas, J
AF Riechers, Dominik A.
Bradford, C. M.
Clements, D. L.
Dowell, C. D.
Perez-Fournon, I.
Ivison, R. J.
Bridge, C.
Conley, A.
Fu, Hai
Vieira, J. D.
Wardlow, J.
Calanog, J.
Cooray, A.
Hurley, P.
Neri, R.
Kamenetzky, J.
Aguirre, J. E.
Altieri, B.
Arumugam, V.
Benford, D. J.
Bethermin, M.
Bock, J.
Burgarella, D.
Cabrera-Lavers, A.
Chapman, S. C.
Cox, P.
Dunlop, J. S.
Earle, L.
Farrah, D.
Ferrero, P.
Franceschini, A.
Gavazzi, R.
Glenn, J.
Solares, E. A. Gonzalez
Gurwell, M. A.
Halpern, M.
Hatziminaoglou, E.
Hyde, A.
Ibar, E.
Kovacs, A.
Krips, M.
Lupu, R. E.
Maloney, P. R.
Martinez-Navajas, P.
Matsuhara, H.
Murphy, E. J.
Naylor, B. J.
Nguyen, H. T.
Oliver, S. J.
Omont, A.
Page, M. J.
Petitpas, G.
Rangwala, N.
Roseboom, I. G.
Scott, D.
Smith, A. J.
Staguhn, J. G.
Streblyanska, A.
Thomson, A. P.
Valtchanov, I.
Viero, M.
Wang, L.
Zemcov, M.
Zmuidzinas, J.
TI A dust-obscured massive maximum-starburst galaxy at a redshift of 6.34
SO NATURE
LA English
DT Article
ID STAR-FORMING GALAXIES; SIMILAR-TO 6; MOLECULAR GAS; SUBMILLIMETER
GALAXIES; EARLY UNIVERSE; HOST GALAXY; QUASARS; DISKS; FIELD
AB Massive present-day early-type (elliptical and lenticular) galaxies probably gained the bulk of their stellar mass and heavy elements through intense, dust-enshrouded starbursts-that is, increased rates of star formation-in the most massive dark-matter haloes at early epochs. However, it remains unknown how soon after the Big Bang massive starburst progenitors exist. The measured redshift (z) distribution of dusty, massive starbursts has long been suspected to be biased low in z owing to selection effects(1), as confirmed by recent findings of systems with redshifts as high as similar to 5 (refs 2-4). Here we report the identification of a massive starburst galaxy at z = 6.34 through a submillimetre colour-selection technique. We unambiguously determined the redshift from a suite of molecular and atomic fine-structure cooling lines. These measurements reveal a hundred billion solar masses of highly excited, chemically evolved interstellar medium in this galaxy, which constitutes at least 40 per cent of the baryonic mass. A 'maximum starburst' converts the gas into stars at a rate more than 2,000 times that of the Milky Way, a rate among the highest observed at any epoch. Despite the overall downturn in cosmic star formation towards the highest redshifts(5), it seems that environments mature enough to form the most massive, intense starbursts existed at least as early as 880 million years after the Big Bang.
C1 [Riechers, Dominik A.; Bradford, C. M.; Dowell, C. D.; Bridge, C.; Vieira, J. D.; Cooray, A.; Bock, J.; Kovacs, A.; Murphy, E. J.; Nguyen, H. T.; Viero, M.; Zemcov, M.; Zmuidzinas, J.] CALTECH, Pasadena, CA 91125 USA.
[Riechers, Dominik A.] Cornell Univ, Ithaca, NY 14853 USA.
[Bradford, C. M.; Dowell, C. D.; Bock, J.; Naylor, B. J.; Nguyen, H. T.; Zemcov, M.; Zmuidzinas, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Clements, D. L.; Hyde, A.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England.
[Perez-Fournon, I.; Cabrera-Lavers, A.; Ferrero, P.; Martinez-Navajas, P.; Streblyanska, A.] Inst Astrofis Canarias, E-38200 Tenerife, Spain.
[Perez-Fournon, I.; Cabrera-Lavers, A.; Ferrero, P.; Martinez-Navajas, P.; Streblyanska, A.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain.
[Ivison, R. J.; Ibar, E.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ivison, R. J.; Arumugam, V.; Dunlop, J. S.; Roseboom, I. G.; Thomson, A. P.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Conley, A.; Earle, L.; Glenn, J.; Maloney, P. R.] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA.
[Fu, Hai; Wardlow, J.; Calanog, J.; Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Hurley, P.; Oliver, S. J.; Roseboom, I. G.; Smith, A. J.; Wang, L.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England.
[Neri, R.; Cox, P.; Krips, M.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France.
[Kamenetzky, J.; Glenn, J.; Rangwala, N.] Univ Colorado, Dept Astrophys & Planetary Sci, CASA UCB 389, Boulder, CO 80309 USA.
[Aguirre, J. E.; Lupu, R. E.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Altieri, B.; Valtchanov, I.] European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain.
[Benford, D. J.; Staguhn, J. G.] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bethermin, M.] Univ Paris Diderot, CEA Saclay, Lab AIM Paris Saclay, CEA,DSM,Irfu,CNRS, F-91191 Gif Sur Yvette, France.
[Bethermin, M.] Univ Paris 11, IAS, F-91405 Orsay, France.
[Bethermin, M.] CNRS, UMR 8617, F-91405 Orsay, France.
[Burgarella, D.] Aix Marseille Univ, CNRS, Lab Astrophys Marseille, UMR7326, F-13388 Marseille, France.
[Cabrera-Lavers, A.] Grantecan SA, Ctr Astrofis La Palma, E-38712 Brena Baja, La Palma, Spain.
[Chapman, S. C.; Solares, E. A. Gonzalez] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA.
[Franceschini, A.] Univ Padua, Dipartimento Fis & Astron, I-35122 Padua, Italy.
[Gavazzi, R.; Omont, A.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Gurwell, M. A.; Petitpas, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Halpern, M.; Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Hatziminaoglou, E.] ESO, D-85748 Garching, Germany.
[Kovacs, A.] Univ Minnesota, Inst Astrophys, Minneapolis, MN 55455 USA.
[Matsuhara, H.] Japan Aerosp & Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Murphy, E. J.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Page, M. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Staguhn, J. G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
RP Riechers, DA (reprint author), CALTECH, 1200 East Calif Blvd,MC 249-17, Pasadena, CA 91125 USA.
EM dr@astro.cornell.edu
RI sebastianovitsch, stepan/G-8507-2013; Lupu, Roxana/P-9060-2014; Wardlow,
Julie/C-9903-2015; Kovacs, Attila/C-1171-2010; Ivison, R./G-4450-2011;
Benford, Dominic/D-4760-2012;
OI Lupu, Roxana/0000-0003-3444-5908; Wardlow, Julie/0000-0003-2376-8971;
Kovacs, Attila/0000-0001-8991-9088; Ivison, R./0000-0001-5118-1313;
Benford, Dominic/0000-0002-9884-4206; Scott,
Douglas/0000-0002-6878-9840; Bethermin, Matthieu/0000-0002-3915-2015;
Altieri, Bruno/0000-0003-3936-0284
NR 30
TC 160
Z9 160
U1 1
U2 30
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD APR 18
PY 2013
VL 496
IS 7445
BP 329
EP 333
DI 10.1038/nature12050
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 126FV
UT WOS:000317599200030
PM 23598341
ER
PT J
AU Su, H
Jiang, JH
Zhai, CX
Perun, VS
Shen, JT
Del Genio, A
Nazarenko, LS
Donner, LJ
Horowitz, L
Seman, C
Morcrette, C
Petch, J
Ringer, M
Cole, J
von Salzen, K
Mesquita, MDS
Iversen, T
Kristjansson, JE
Gettelman, A
Rotstayn, L
Jeffrey, S
Dufresne, JL
Watanabe, M
Kawai, H
Koshiro, T
Wu, TW
Volodin, EM
L'Ecuyer, T
Teixeira, J
Stephens, GL
AF Su, Hui
Jiang, Jonathan H.
Zhai, Chengxing
Perun, Vince S.
Shen, Janice T.
Del Genio, Anthony
Nazarenko, Larissa S.
Donner, Leo J.
Horowitz, Larry
Seman, Charles
Morcrette, Cyril
Petch, Jon
Ringer, Mark
Cole, Jason
von Salzen, Knut
Mesquita, Michel D. S.
Iversen, Trond
Kristjansson, Jon Egill
Gettelman, Andrew
Rotstayn, Leon
Jeffrey, Stephen
Dufresne, Jean-Louis
Watanabe, Masahiro
Kawai, Hideaki
Koshiro, Tsuyoshi
Wu, Tongwen
Volodin, Evgeny M.
L'Ecuyer, Tristan
Teixeira, Joao
Stephens, Graeme L.
TI Diagnosis of regime-dependent cloud simulation errors in CMIP5 models
using "A-Train" satellite observations and reanalysis data
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE Clouds; Climate Model; Satellite Observation; CMIP5; A-Train;
large-scale regimes; conditional sampling; model error diagnosis
ID GENERAL-CIRCULATION MODEL; GLOBAL CLIMATE MODEL; ATMOSPHERE;
VARIABILITY; SENSITIVITY; TROPOSPHERE; CONVECTION; MASS
AB The vertical distributions of cloud water content (CWC) and cloud fraction (CF) over the tropical oceans, produced by 13 coupled atmosphere-ocean models submitted to the Phase 5 of Coupled Model Intercomparison Project (CMIP5), are evaluated against CloudSat/CALIPSO observations as a function of large-scale parameters. Available CALIPSO simulator CF outputs are also examined. A diagnostic framework is developed to decompose the cloud simulation errors into large-scale errors, cloud parameterization errors and covariation errors. We find that the cloud parameterization errors contribute predominantly to the total errors for all models. The errors associated with large-scale temperature and moisture structures are relatively greater than those associated with large-scale midtropospheric vertical velocity and lower-level divergence. All models capture the separation of deep and shallow clouds in distinct large-scale regimes; however, the vertical structures of high/low clouds and their variations with large-scale parameters differ significantly from the observations. The CWCs associated with deep convective clouds simulated in most models do not reach as high in altitude as observed, and their magnitudes are generally weaker than CloudSat total CWC, which includes the contribution of precipitating condensates, but are close to CloudSat nonprecipitating CWC. All models reproduce maximum CF associated with convective detrainment, but CALIPSO simulator CFs generally agree better with CloudSat/CALIPSO combined retrieval than the model CFs, especially in the midtroposphere. Model simulated low clouds tend to have little variation with large-scale parameters except lower-troposphere stability, while the observed low cloud CWC, CF, and cloud top height vary consistently in all large-scale regimes.
C1 [Su, Hui; Jiang, Jonathan H.; Zhai, Chengxing; Perun, Vince S.; Shen, Janice T.; Teixeira, Joao; Stephens, Graeme L.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Del Genio, Anthony; Nazarenko, Larissa S.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Donner, Leo J.; Horowitz, Larry; Seman, Charles] Geophys Fluid Dynam Lab, Princeton, NJ USA.
[Morcrette, Cyril; Petch, Jon] UK Met Off, Exeter, Devon, England.
[Ringer, Mark] UK Met Off Hadley Ctr MOHC, Exeter, Devon, England.
[Cole, Jason; von Salzen, Knut] Environm Canada, CCCMA, Victoria, BC, Canada.
[Mesquita, Michel D. S.] Uni Res, BCCR, Bergen, Norway.
[Iversen, Trond] NCC, Meteorologisk Inst, Oslo, Norway.
[Kristjansson, Jon Egill] Univ Oslo, Oslo, Norway.
[Gettelman, Andrew] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Rotstayn, Leon] CSIRO, Aspendale, Vic, Australia.
[Watanabe, Masahiro] Univ Tokyo, Atmospher & Ocean Res Inst, Model Interdisciplinary Res Climate MIROC, Chiba, Japan.
[Kawai, Hideaki; Koshiro, Tsuyoshi] Japan Meteorol Agcy, MRI, Tsukuba, Ibaraki, Japan.
[Wu, Tongwen] China Meteorol Adm, BCC, Beijing, Peoples R China.
[Volodin, Evgeny M.] Russian Acad Sci, Inst Numer Math, Moscow, Russia.
[L'Ecuyer, Tristan] Univ Wisconsin, Madison, WI USA.
RP Su, H (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Hui.Su@jpl.nasa.gov
RI L'Ecuyer, Tristan/C-7040-2013; Rotstayn, Leon/A-1756-2012; Horowitz,
Larry/D-8048-2014; Morcrette, Cyril/H-7282-2012; L'Ecuyer,
Tristan/E-5607-2012; Dufresne, Jean-Louis/I-5616-2015; Ringer,
Mark/E-7294-2013; Mesquita, Michel d. S./C-3414-2009; Koshiro,
Tsuyoshi/O-7183-2016
OI Cole, Jason/0000-0003-0450-2748; Rotstayn, Leon/0000-0002-2385-4223;
Horowitz, Larry/0000-0002-5886-3314; Morcrette,
Cyril/0000-0002-4240-8472; L'Ecuyer, Tristan/0000-0002-7584-4836;
Dufresne, Jean-Louis/0000-0003-4764-9600; Ringer,
Mark/0000-0003-4014-2583; Mesquita, Michel d. S./0000-0002-4556-5414;
Koshiro, Tsuyoshi/0000-0003-2971-7446
FU NASA ROSES COUND; AST; NEWS
FX We thank the funding support from NASA ROSES COUND, AST, and NEWS, the
CloudSat/CALIPSO mission teams and relevant satellite mission projects.
We acknowledge PCMDI for archiving CMIP5 model simulations and the ECMWF
Data Server for ECMWF Interim Reanalysis data. This work was carried out
at the Jet Propulsion Laboratory, California Institute of Technology,
under contract with NASA.
NR 56
TC 37
Z9 37
U1 1
U2 45
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 16
PY 2013
VL 118
IS 7
BP 2762
EP 2780
DI 10.1029/2012JD018575
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 153QT
UT WOS:000319618300006
ER
PT J
AU Xiang, B
Miller, SM
Kort, EA
Santoni, GW
Daube, BC
Commane, R
Angevine, WM
Ryerson, TB
Trainer, MK
Andrews, AE
Nehrkorn, T
Tian, HQ
Wofsy, SC
AF Xiang, Bin
Miller, Scot M.
Kort, Eric A.
Santoni, Gregory W.
Daube, Bruce C.
Commane, Roisin
Angevine, Wayne M.
Ryerson, Tom B.
Trainer, Michael K.
Andrews, Arlyn E.
Nehrkorn, Thomas
Tian, Hanqin
Wofsy, Steven C.
TI Nitrous oxide (N2O) emissions from California based on 2010 CalNex
airborne measurements
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE nitrous oxide; emissions; California; fertilizer
ID SPATIAL VARIABILITY; NORTH-AMERICA; STILT MODEL; WATER; SOIL;
ECOSYSTEMS; METHANE; FIELD
AB Nitrous oxide (N2O) is an important gas for climate and for stratospheric chemistry, with a lifetime exceeding 100years. Global concentrations have increased steadily since the 18th century, apparently due to human-associated emissions, principally from the application of nitrogen fertilizers. However, quantitative studies of agricultural emissions at large spatial scales are lacking, inhibited by the difficulty of measuring small enhancements in atmospheric concentration. Here we derive regional emission rates for N2O in the agricultural heartland of California based on analysis of in-situ airborne atmospheric observations collected using a new quantum cascade laser spectrometer. The data were obtained on board the NOAA WP-3 research aircraft during the CalNex (California Research at the Nexus of Air Quality and Climate Change) program in late spring 2010. We coupled the WRF (weather research and forecasting) model, a meso-scale meteorology model, with the STILT (stochastic time-inverted Lagrangian transport) model, a Lagrangian particle dispersion model, to link our in-situ airborne observations to surface emissions. We then used a variety of statistical methods to identify source areas and to optimize emission rates. Our results are consistent with the view that fertilizer application is the largest source of N2O in the Central Valley. The spatial distribution of surface emissions, based on California land use and activity maps, was very different than indicated in the leading emission inventory (EDGAR 4.0). Our estimated total emission flux of N2O for California in May and June was 3 - 4 times larger than the annual mean given for the state by EDGAR and other inventories, indicating a strong seasonal variation. We estimated the statewide total annual emissions of N2O to be 0.042 +/- 0.011 Tg N/year, roughly equivalent to inventory values if we account for seasonal variations using observations obtained in the midwestern United States. This state total N2O emission is 20.5 Tg CO2 equivalent (100year global warming potential=310 CO2 eq/g N2O), accounting for approximately 4% of the state total greenhouse gas emissions.
C1 [Xiang, Bin; Miller, Scot M.; Santoni, Gregory W.; Daube, Bruce C.; Commane, Roisin; Wofsy, Steven C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Xiang, Bin; Miller, Scot M.; Santoni, Gregory W.; Daube, Bruce C.; Commane, Roisin; Wofsy, Steven C.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA.
[Kort, Eric A.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Angevine, Wayne M.; Ryerson, Tom B.; Trainer, Michael K.; Andrews, Arlyn E.] NOAA, Boulder, CO USA.
[Nehrkorn, Thomas] Atmospher & Environm Res Inc, Lexington, MA USA.
[Tian, Hanqin] Auburn Univ, Sch Forestry & Wildlife Sci, Auburn, AL 36849 USA.
RP Xiang, B (reprint author), Harvard Univ, Sch Engn & Appl Sci, 20 Oxford St, Cambridge, MA 02138 USA.
EM bxiang@seas.harvard.edu
RI Xiang, Bin/E-8034-2012; Commane, Roisin/E-4835-2016; Manager, CSD
Publications/B-2789-2015; Andrews, Arlyn/K-3427-2012; Angevine,
Wayne/H-9849-2013; Trainer, Michael/H-5168-2013; Ryerson,
Tom/C-9611-2009; Tian, Hanqin/A-6484-2012; Kort, Eric/F-9942-2012;
Xiang, Bin/M-2812-2013
OI Nehrkorn, Thomas/0000-0003-0637-3468; Commane,
Roisin/0000-0003-1373-1550; Angevine, Wayne/0000-0002-8021-7116; Tian,
Hanqin/0000-0002-1806-4091; Kort, Eric/0000-0003-4940-7541;
FU NASA [NNX09AJ94G, NNX11AG47G, NNX09AU40G]; NSF [ATM-083091-2]; NOAA
[NA09OAR4310122, NA11OAR4310158]
FX This study was supported by the following grants to Harvard University:
NASA NNX09AJ94G, NNX11AG47G, and NNX09AU40G; NSF ATM-083091-2; and NOAA
NA09OAR4310122 and NA11OAR4310158. We are grateful to the flight crew of
the NOAA P-3 for safely executing a difficult flight mission. B. X.
thanks Jasna Pittman for helpful comments on the manuscript. E.A.K.
thanks the W. M. Keck Institute for Space Studies for support. Portions
of this work were performed at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with NASA.
NR 38
TC 6
Z9 6
U1 2
U2 42
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 16
PY 2013
VL 118
IS 7
BP 2809
EP 2820
DI 10.1002/jgrd.50189
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 153QT
UT WOS:000319618300009
ER
PT J
AU Dessler, AE
Loeb, NG
AF Dessler, A. E.
Loeb, N. G.
TI Impact of dataset choice on calculations of the short-term cloud
feedback
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE cloud feedback; energy budget
ID CLIMATE FEEDBACKS; MODELS; SYSTEM
AB Dessler [2010, hereafter D10] estimated the magnitude of the cloud feedback in response to short-term climate variations and concluded that it was likely positive, with an average magnitude of +0.50 +/- 0.75W/m2/K. This paper investigates the sensitivity of D10's results to the choice of clear-sky top-of-atmosphere flux (Rclear-sky), surface temperature (Ts), and reanalysis data sets. Most of the alternative Rclear-sky data sets produce cloud feedbacks that are close to D10, differing by 0.2-0.3W/m2/K. An exception is the Terra SSF1deg Rclear-sky product, which produces an overall negative cloud feedback. However, a critical examination of those data leads us to conclude that that result is due to problems in the Terra Rclear-sky arising from issues with cloud clearing prior to July 2001. Eliminating the problematic early portion yields a cloud feedback in good agreement with D10. We also present an alternative calculation of the cloud feedback that does not require an estimate of Rclear-sky, and this calculation also produces a positive cloud feedback in agreement with D10. The various Ts data sets produce cloud feedbacks that differ by as much as 0.8W/m2/K. The choice of reanalysis, used as a source of Rclear-sky or as adjustments for the cloud radiative forcing, has a small impact on the inferred cloud feedback. Overall, these results confirm the robustness of D10's estimate of a likely positive feedback.
C1 [Dessler, A. E.] Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
[Loeb, N. G.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Dessler, AE (reprint author), Texas A&M Univ, Dept Atmospher Sci, College Stn, TX 77843 USA.
EM adessler@tamu.edu
RI Dessler, Andrew/G-8852-2012
OI Dessler, Andrew/0000-0003-3939-4820
FU NSF [AGS-1012665]
FX This work was supported by NSF grant AGS-1012665 to Texas A&M
University. We thank Mark Zelinka and Troy Masters for their comments on
this paper.
NR 18
TC 6
Z9 6
U1 1
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 16
PY 2013
VL 118
IS 7
BP 2821
EP 2826
DI 10.1002/jgrd.50199
PG 6
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 153QT
UT WOS:000319618300010
ER
PT J
AU Meyer, TC
Lang, TJ
Rutledge, SA
Lyons, WA
Cummer, SA
Lu, GP
Lindsey, DT
AF Meyer, Tiffany C.
Lang, Timothy J.
Rutledge, Steven A.
Lyons, Walter A.
Cummer, Steven A.
Lu, Gaopeng
Lindsey, Daniel T.
TI Radar and lightning analyses of gigantic jet-producing storms
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE Lightning; Gigantic Jet; Thunderstorm
ID BLUE JETS; ELECTRICAL DISCHARGES; TORNADIC STORM; THUNDERSTORMS;
REFLECTIVITY; THUNDERCLOUD; IONOSPHERE; EVOLUTION; STARTERS; VELOCITY
AB An analysis of thunderstorm environment, structure, and evolution associated with six gigantic jets (five negative polarity, one positive) was conducted. Three of these gigantic jets were observed within detection range of very high frequency lightning mapping networks. All six were within range of operational radars and two-dimensional lightning network coverage: five within the National Lightning Detection Network and one within the Global Lightning Detection (GLD360) network. Most of the storms producing the jets formed in moist tropical or tropical-like environments (precipitable water ranged from 37 to 62 kg m-2, and 0-6 km shear from 3.5 to 24.8 m s-1), featuring high convective available potential energy (1200-3500 J kg-1) and low lifted indices (-2.8 to -6.4). The storms had maximum radar reflectivity factors of 54 to 62 dBZ, and 10 dBZ echo contours reached 14-17 km. Storms covered by three-dimensional lightning mappers were near peak altitude of lightning activity (modes of the vertical distributions of radio sources were at altitudes colder than -50 degrees C) and vertical reflectivity intensity, with overshooting echo tops around the times of their jets. Two of the other three jet-producing storms produced their jet around the time of a convective surge as indicated by radar data and likely featured overshooting tops. The observations suggest a link between convective surges, overshooting tops, and the occurrence of gigantic jets, similar to prior modeling studies.
C1 [Meyer, Tiffany C.; Lang, Timothy J.; Rutledge, Steven A.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Meyer, Tiffany C.] Natl Weather Serv, Warning Decis Training Branch, Norman, OK USA.
[Lang, Timothy J.] NASA, Marshall Space Flight Ctr ZP11, Huntsville, AL 35812 USA.
[Lyons, Walter A.] FMA Res Inc, Ft Collins, CO USA.
[Cummer, Steven A.; Lu, Gaopeng] Duke Univ, Elect & Comp Engn Dept, Durham, NC USA.
[Lindsey, Daniel T.] NOAA, NESDIS, STAR, RAMMB, Ft Collins, CO USA.
RP Lang, TJ (reprint author), NASA, Marshall Space Flight Ctr ZP11, Huntsville, AL 35812 USA.
EM tjlangco@gmail.com
RI Lu, Gaopeng/D-9011-2012; Cummer, Steven/A-6118-2008; Lindsey,
Dan/F-5607-2010;
OI Cummer, Steven/0000-0002-0002-0613; Lindsey, Dan/0000-0002-0967-5683;
Lang, Timothy/0000-0003-1576-572X
FU DARPA Nimbus program
FX This work was supported by the DARPA Nimbus program. The authors thank
Vaisala, Inc. for providing the NLDN and GLD360 data used in this study.
Without the observations of the gigantic jets, this study would not have
been possible. The Florida, Oklahoma, and Puerto Rico gigantic jets were
observed by Joel Gonzalez in Florida, by Kevin Palivec in Texas, and by
Frankie Lucena in Puerto Rico, respectively. The authors thank the
editors and reviewers of this manuscript for their assistance in
improving it.
NR 52
TC 7
Z9 7
U1 0
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 16
PY 2013
VL 118
IS 7
BP 2872
EP 2888
DI 10.1002/jgrd.50302
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 153QT
UT WOS:000319618300015
ER
PT J
AU Tesche, M
Wandinger, U
Ansmann, A
Althausen, D
Muller, D
Omar, AH
AF Tesche, M.
Wandinger, U.
Ansmann, A.
Althausen, D.
Mueller, D.
Omar, A. H.
TI Ground-based validation of CALIPSO observations of dust and smoke in the
Cape Verde region
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE CALIPSO; SAMUM; lidar; mineral dust; remote sensing; validation
ID AEROSOL OPTICAL DEPTH; SPECTRAL-RESOLUTION LIDAR; NORTH-AFRICAN DUST;
SAHARAN DUST; AERONET MEASUREMENTS; RAMAN LIDAR; MODIS-AQUA; EXTINCTION;
TRANSPORT; PROFILES
AB Ground-based Raman lidar measurements during the second Saharan Mineral Dust Experiment (SAMUM-2) in 2008 were used for validation of measurements of the lidar aboard the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) satellite within the dusty environment of the Cape Verde region. SAMUM-2 featured two one-month campaigns in January/February and May/June 2008 to cover different modes of aerosol transport to the tropical Atlantic: dust from northern Africa and biomass-burning smoke from western Africa during winter, and pure Saharan dust during summer. During the investigated time period, 33 CALIPSO overflights occurred at a distance of less than 500 km from the location of the ground-based lidar. Fifteen out of these 33 cases were found suitable for comparing the findings of the two instruments. The parameters for this comparison are the particle backscatter coefficient at 532 and 1064 nm, the extinction coefficient, the lidar ratio (aerosol type), and the particle depolarization ratio at 532 nm, as well as the backscatter-related angstrom ngstrom exponent for the wavelength pair 532/1064 nm. Best agreement was found for the 532 nm backscatter coefficient, while the 532 nm extinction coefficient is underestimated by up to 30%. The latter is due to the use of an effective dust lidar ratio that gives reliable backscatter coefficients but is not suitable to transform these to extinction coefficients. CALIPSO particle depolarization ratios provided in the current (version 3.01) aerosol profile product were found to be affected by a computing error and should be calculated from the perpendicular and total particle backscatter coefficients provided in the same data file. CALIPSO aerosol classification was found to be mostly correct but a demand for homogeneous aerosol layers could improve the retrieval. Suggestions for the improvement of the CALIPSO retrieval by introducing iterative procedures are provided.
C1 [Tesche, M.] Stockholm Univ, Dept Appl Environm Sci ITM, SE-11418 Stockholm, Sweden.
[Wandinger, U.; Ansmann, A.; Althausen, D.; Mueller, D.] Leibniz Inst Tropospher Res TROPOS, Leipzig, Germany.
[Mueller, D.] NASA, Langley Res Ctr, Sci Syst & Applicat Inc, Hampton, VA 23665 USA.
[Mueller, D.] Univ Hertfordshire, Dept Phys Astron & Math, Hatfield AL10 9AB, Herts, England.
[Omar, A. H.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Tesche, M (reprint author), Stockholm Univ, Dept Appl Environm Sci ITM, Svante Arrhenius Vag 8, SE-11418 Stockholm, Sweden.
EM matthias.tesche@itm.su.se
RI Wandinger, Ulla/E-3348-2014; MUELLER, DETLEF/F-1010-2015; Omar,
Ali/D-7102-2017;
OI MUELLER, DETLEF/0000-0002-0203-7654; Omar, Ali/0000-0003-1871-9235;
Tesche, Matthias/0000-0003-0096-4785
FU Deutsche Forschungsgemeinschaft (DFG) [FOR 539]
FX We like to thank Mark Vaughan for his help and criticism regarding the
present paper. The SAMUM research group was funded by the Deutsche
Forschungsgemeinschaft (DFG) under grant FOR 539. CALIPSO data used in
this study were obtained from the NASA Langley Research Center
Atmospheric Science Data Center (http://eosweb.larc.nasa.gov).
NR 48
TC 26
Z9 26
U1 3
U2 17
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD APR 16
PY 2013
VL 118
IS 7
BP 2889
EP 2902
DI 10.1002/jgrd.50248
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 153QT
UT WOS:000319618300016
ER
PT J
AU Nicolae, D
Nemuc, A
Muller, D
Talianu, C
Vasilescu, J
Belegante, L
Kolgotin, A
AF Nicolae, D.
Nemuc, A.
Mueller, D.
Talianu, C.
Vasilescu, J.
Belegante, L.
Kolgotin, A.
TI Characterization of fresh and aged biomass burning events using
multiwavelength Raman lidar and mass spectrometry
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE biomass burning aerosols; lidar; AMS; aerosol microphysical properties;
aerosol mass spectrometry
ID MICROPHYSICAL PARTICLE PARAMETERS; AEROSOL OPTICAL-PROPERTIES;
BACKSCATTER LIDAR; SMOKE; REGULARIZATION; EXTINCTION; INVERSION;
RETRIEVAL; AIRCRAFT; CAMPAIGN
AB This paper focuses on optical and microphysical properties of long-range transported biomass burning (BB) aerosols and their variation with atmospheric evolution (ageing), as observed by a multiwavelength Raman lidar, part of EARLINET (European Aerosol LIdar NETwork). Chemical analysis of the atmospheric aerosol was done using a colocated aerosol mass spectrometer (AMS). One relevant optical parameter for the ageing process is the angstrom ngstrom exponent. In our study, we find that it decreases from 2 for fresh to 1.4-0.5 for aged smoke particles. The ratio of lidar (extinction-to-backscatter) ratios (LR532/LR355) changes rapidly from values <1 for fresh to >1 for aged particles. The imaginary part of the refractive index is the most sensitive microphysical parameter. It decreases sharply from 0.05 to less than 0.01 for fresh and aged smoke particles, respectively. Single-scattering albedo (SSA) varies from 0.74 to 0.98 depending on aerosol age and source. The AMS was used to measure the marker ions of wood-burning particles during 2 days of measurements when the meteorological conditions favored the downward mixing of aerosols from lofted layers. Particle size distribution and particle effective radius from both AMS and lidar are similar, i.e., particle effective radii were approximately 0.27 mu m for fresh BB aerosol particles. Microphysical aerosol properties from inversion of the lidar data agree with similar studies carried out in different regions on the globe. Our study shows that the angstrom ngstrom exponent LR532/LR355 and the imaginary part of the refractive index can be used to clearly distinguish between fresh and aged smoke particles.
C1 [Nicolae, D.; Nemuc, A.; Talianu, C.; Vasilescu, J.; Belegante, L.] Natl Inst Res & Dev Optoelect, RO-77125 Magurele, Ilfov, Romania.
[Mueller, D.] Leibniz Inst Tropospher Res IfT, Leipzig, Germany.
[Mueller, D.] GIST, Kwangju, South Korea.
[Mueller, D.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Kolgotin, A.] Phys Instrumentat Ctr, Moscow, Russia.
RP Nemuc, A (reprint author), Natl Inst Res & Dev Optoelect, 409 Atomistilor St, RO-77125 Magurele, Ilfov, Romania.
EM anca@inoe.ro
RI Vasilescu, Jeni/C-2336-2011; Belegante, Livio/B-5812-2012; MUELLER,
DETLEF/F-1010-2015; Nicolae, Doina/I-4999-2016
OI MUELLER, DETLEF/0000-0002-0203-7654;
FU Romanian National Authority for Scientific Research, CNCS-UEFISCDI
[PN-II-RU-PD-2011-3-0082, PN 09-27 01 03]; European Community
[262254-ACTRIS]; Korea Meteorological Administration Research and
Development Program [CATER 2012-7080]
FX This work was supported by a grant of the Romanian National Authority
for Scientific Research, CNCS-UEFISCDI, project no.
PN-II-RU-PD-2011-3-0082 and grant no. PN 09-27 01 03 and by the European
Community's FP7-INFRASTRUCTURES-2010-1 under grant agreement no.
262254-ACTRIS. This work was also funded by the Korea Meteorological
Administration Research and Development Program under grant CATER
2012-7080.
NR 57
TC 19
Z9 19
U1 5
U2 34
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 APR 16
PY 2013
VL 118
IS 7
BP 2956
EP 2965
DI 10.1002/jgrd.50324
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 153QT
UT WOS:000319618300020
ER
PT J
AU Eriksson, S
Rastatter, L
AF Eriksson, S.
Rastaetter, L.
TI Alfven Mach number and IMF clock angle dependencies of sunward flow
channels in the magnetosphere
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID FLUX-TRANSFER EVENTS; FIELD; SASH
AB Interplanetary coronal mass ejections associated with strong interplanetary magnetic field (IMF) By have been shown to enhance the neutral density in low Earth orbit. The enhancement has been linked to strong downward Poynting fluxes embedded within ionospheric channels of significant sunward ExB drift (2000-3000 m/s). Here we present MHD results describing the magnetospheric counterpart of the ionospheric flow channel that Defense Meteorological Satellite Program (DMSP) encountered on 15 May 2005. It is shown that the clock angle of maximum sunward flow (theta(FC)) depends on the IMF clock angle theta(FC) = alpha * theta(IMF) -1.3 degrees with alpha = (0.30, 0.38, 0.43, 0.45) at X = (4, 2, 0, -2) R-E. This is poleward of the magnetic null point region. The flow also depends on the solar wind Alfven Mach number Vx = Vx0 - delta v * M-A. The critical M-A = Vx0 / delta V for Vx = 0 decreases from M-A = 3.42 (X = 4 R-E) to M-A = 2.40 (X = -2 R-E). The low M-A and theta(IMF) conditions that characterized the X = 2 RE flow and resulted in strong Poynting flux occurred for 16% of all 167 h in 1998-2008 with Dst < -180 nT.
C1 [Eriksson, S.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[Rastaetter, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Eriksson, S (reprint author), Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
EM eriksson@lasp.colorado.edu
RI Rastaetter, Lutz/D-4715-2012;
OI Rastaetter, Lutz/0000-0002-7343-4147; Eriksson,
Stefan/0000-0002-5619-1577
FU NSF [AGS-1144154]
FX S.E. acknowledges support by NSF grant AGS-1144154.
NR 21
TC 4
Z9 4
U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 16
PY 2013
VL 40
IS 7
DI 10.1002/grl.50307
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 148BP
UT WOS:000319217600001
ER
PT J
AU Knipp, D
Kilcommons, L
Hunt, L
Mlynczak, M
Pilipenko, V
Bowman, B
Deng, Y
Drake, K
AF Knipp, D.
Kilcommons, L.
Hunt, L.
Mlynczak, M.
Pilipenko, V.
Bowman, B.
Deng, Y.
Drake, K.
TI Thermospheric damping response to sheath-enhanced geospace storms
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID ION-CYCLOTRON WAVES; NITRIC-OXIDE; SABER EXPERIMENT; PLASMA SHEET;
SOLAR-WIND; ART.; DENSITY; CHAMP; MODEL
AB We show evidence that solar wind density enhancements and pressure pulses can lead to intense low-energy particle precipitation and an associated, but unexpected, damping of thermospheric density response. Ground-based indices, used as proxies for thermospheric energy deposition, fail to capture these interactions in forecasting algorithms. Superposed epoch comparison of a group of poorly specified neutral density storms suggests an event-chain of (1) multi-hour, pre-storm solar wind density enhancement, followed by solar wind dynamic pressure pulses that trigger excess low-energy particle flux to the upper atmosphere; (2) enhanced production of thermospheric Nitric Oxide (NO) by precipitating particles and storm heating; (3) NO infrared cooling and damping of the thermosphere; and (4) mis-forecast of neutral density. In the control storms, these features are absent or muted. We discuss the roles of solar wind pre-conditioning and solar cycle dependency in the problem storms. These problem neutral-density storms reveal an element of "geo-effectiveness" that highlights competition between hydrodynamic aspects of the solar wind and other interplanetary drivers.
C1 [Knipp, D.; Kilcommons, L.] Univ Colorado, Boulder, CO 80309 USA.
[Knipp, D.] NCAR, High Altitude Observ, Boulder, CO USA.
[Knipp, D.] Space Environm Technol, Pacific Palisades, CA USA.
[Hunt, L.] Sci Syst & Applicat Inc, Hampton, VA USA.
[Mlynczak, M.] NASA, Sci Directorate, Langley Res Ctr, Hampton, VA USA.
[Pilipenko, V.] Space Res Inst, Moscow, Russia.
[Bowman, B.] USAF, Space Command, Colorado Springs, CO USA.
[Deng, Y.] Univ Texas Arlington, Dept Phys, Arlington, TX USA.
RP Knipp, D (reprint author), Univ Colorado, Boulder, CO 80309 USA.
EM delores.knipp@colorado.edu
FU AFOSR [FA9550-07-1-0565]; NRC fellowship at NOAA's Space Weather
Prediction Center; [AFRL FA9453-12-1-0244]; [AFSOR FA9550-12-1-0264];
[NSFATM1025089]; [NSFATM0955629]; [AFOSR 1210429]; [MJE-NSF
ATM-0827903]
FX We are grateful to F. Rich, M. Engebretson, C. Lin, E. Sutton, G.
Wilson, E. Zesta, H. Luhr, W. Wang, S. Solomon, J. Raeder. R. Redmon, M.
G. McHarg, and A. Richmond for fruitful discussions. We used particle
data from the DMSP archive at the National Geophysical Data Center. We
made extensive use of the NASA OMNIweb database. Kyoto University,
Kyoto, Japan, provided Dst data to OMNIweb. The following grants
supported this work: DK and LK-AFRL FA9453-12-1-0244, AFSOR
FA9550-12-1-0264, and NSFATM1025089; YD-NSFATM0955629 and AFOSR 1210429;
and VP and MJE-NSF ATM-0827903. Early aspects of this work were
supported by AFOSR FA9550-07-1-0565 and an NRC fellowship at NOAA's
Space Weather Prediction Center to DK.
NR 38
TC 12
Z9 12
U1 0
U2 13
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 16
PY 2013
VL 40
IS 7
DI 10.1002/grl.50197
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 148BP
UT WOS:000319217600002
ER
PT J
AU Parkinson, CL
Comiso, JC
AF Parkinson, Claire L.
Comiso, Josefino C.
TI On the 2012 record low Arctic sea ice cover: Combined impact of
preconditioning and an August storm
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID DECLINE
AB A new record low Arctic sea ice extent for the satellite era, 3.4 x 10(6) km(2), was reached on 13 September 2012; and a new record low sea ice area, 3.0 x 10(6) km(2), was reached on the same date. Preconditioning through decades of overall ice reductions made the ice pack more vulnerable to a strong storm that entered the central Arctic in early August 2012. The storm caused the separation of an expanse of 0.4 x 10(6) km(2) of ice that melted in total, while its removal left the main pack more exposed to wind and waves, facilitating the main pack's further decay. Future summer storms could lead to a further acceleration of the decline in the Arctic sea ice cover and should be carefully monitored.
C1 [Parkinson, Claire L.; Comiso, Josefino C.] NASA, Cryospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Parkinson, CL (reprint author), NASA, Cryospher Sci Lab, Goddard Space Flight Ctr, Code 615, Greenbelt, MD 20771 USA.
EM Claire.L.Parkinson@nasa.gov
RI Parkinson, Claire/E-1747-2012
OI Parkinson, Claire/0000-0001-6730-4197
FU Cryospheric Sciences Program at NASA Headquarters
FX The authors thank Rob Gersten of ADNET/RSIS and Larry Stock of SGT for
their support in the creation of the figures and the Cryospheric
Sciences Program at NASA Headquarters for funding the work. They also
thank Ian Simmonds and Harry Stern for many valuable comments on the
manuscript.
NR 36
TC 124
Z9 130
U1 4
U2 60
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 APR 16
PY 2013
VL 40
IS 7
DI 10.1002/grl.50349
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 148BP
UT WOS:000319217600019
ER
PT J
AU Richter, N
Poland, MP
Lundgren, PR
AF Richter, Nicole
Poland, Michael P.
Lundgren, Paul R.
TI TerraSAR-X interferometry reveals small-scale deformation associated
with the summit eruption of Kilauea Volcano, Hawai'i
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
AB On 19 March 2008, a small explosive eruption at the summit of Kilauea Volcano, Hawai'i, heralded the formation of a new vent along the east wall of Halema'uma'u Crater. In the ensuing years, the vent widened due to collapses of the unstable rim and conduit wall; some collapses impacted an actively circulating lava pond and resulted in small explosive events. We used synthetic aperture radar data collected by the TerraSAR-X satellite, a joint venture between the German Aerospace Center (DLR) and EADS Astrium, to identify and analyze small-scale surface deformation around the new vent during 2008-2012. Lidar data were used to construct a digital elevation model to correct for topographic phase, allowing us to generate differential interferograms with a spatial resolution of about 3m in Kilauea's summit area. These interferograms reveal subsidence within about 100m of the rim of the vent. Small baseline subset time series analysis suggests that the subsidence rate is not constant and, over time, may provide an indication of vent stability and potential for rim and wall collapse-information with obvious hazard implications. The deformation is not currently detectable by other space- or ground-based techniques.
C1 [Richter, Nicole] Univ Jena, Dept Earth Observat, Jena, Germany.
[Lundgren, Paul R.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Richter, N (reprint author), Univ Jena, Dept Earth Observat, Jena, Germany.
EM nrichter@gfz-potsdam.de
OI Poland, Michael/0000-0001-5240-6123
FU German Academic Exchange Service (DAAD); German Aerospace Center (DLR)
through the Hawaii Supersite [GEO0747, GEO0875]; National Aeronautics
and Space Administration at the Jet Propulsion Laboratory, California
Institute of Technology
FX We are grateful to Tim Orr for providing the vent area data. We also
thank Don Swanson, Rowena Lohman, and an anonymous referee for reviews
that improved the manuscript. This research was completed as part of
Richter's M. S. thesis at the University of Jena, supported by
Christiane Schmullius and with funding provided by the German Academic
Exchange Service (DAAD). The LIDAR data were provided by Adam Soule
(Woods Hole Oceanographic Institute). TerraSAR-X data were provided by
the German Aerospace Center (DLR) through the Hawaii Supersite (projects
GEO0747 and GEO0875). Part of the research described in this paper was
supported under contract with the National Aeronautics and Space
Administration at the Jet Propulsion Laboratory, California Institute of
Technology.
NR 15
TC 8
Z9 9
U1 1
U2 10
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 16
PY 2013
VL 40
IS 7
DI 10.1002/grl.50286
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 148BP
UT WOS:000319217600005
ER
PT J
AU Periyakaruppan, A
Gandhiraman, RP
Meyyappan, M
Koehne, JE
AF Periyakaruppan, Adaikkappan
Gandhiraman, Ram P.
Meyyappan, M.
Koehne, Jessica E.
TI Label-Free Detection of Cardiac Troponin-I Using Carbon Nanofiber Based
Nanoelectrode Arrays
SO ANALYTICAL CHEMISTRY
LA English
DT Article
ID ELECTROCHEMICAL IMPEDANCE SPECTROSCOPY; PROTEIN ADSORPTION; BIOSENSORS;
MYOGLOBIN; BIOCHIPS; ANTIBODY; SERUM
AB A label-free biosensor is presented using carbon nanofiber (CNF) nanoelectrode arrays for the detection of cardiac troponin-I in the early diagnosis of myocardial infarction. Immobilization of anti-cTnI Ab on CNFs and the detection of human-cTnI were examined using electrochemical impedance spectroscopy and cyclic voltammetry techniques. Each step of the modification process was monitored, and the results show changes in electrical capacitance or resistance to charge transfer due to the specificity of corresponding adsorption of Ab-Ag interaction. The immunosensor demonstrates a good selectivity and high sensitivity against human-cTnI analytes and is capable of detecting cTnI at concentrations as low as similar to 0.2 ng/mL, which is 25 times lower than that possible by conventional methods. Analysis of the electrode at various stages using atomic force microscopy and X-ray reflectivity provides information on the surface roughness and orientation of the antibody.
C1 [Periyakaruppan, Adaikkappan; Gandhiraman, Ram P.; Meyyappan, M.; Koehne, Jessica E.] NASA, Ctr Nanotechnol, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Koehne, JE (reprint author), NASA, Ctr Nanotechnol, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM jessica.e.koehne@nasa.gov
RI Gandhiraman, Ram Prasad/B-7004-2013
OI Gandhiraman, Ram Prasad/0000-0001-8957-7938
FU NASA URC [NNX08BA47A]; Science Foundation Ireland [10/CE/B1821-STTF 11]
FX A.P. acknowledges Dr. Olufisayo Jejelowo and Dr. Adebayo Oyekan of Texas
Southern University and Dr. Govindarajan Ramesh of Norfolk State
University for their support. A.P. is a visiting Postdoctoral Fellow
from TSU, Houston, supported by a NASA URC contract to TSU (NNX08BA47A).
R.P.G. is a visiting research scholar from Dublin City University,
Ireland under the Science Foundation Ireland fellowship 10/CE/B1821-STTF
11. The authors acknowledge Dr. Apurva Mehta and Dr. Michael F. Toney
from Stanford Synchrotron Radiation Light Source (SSRL), Stanford
University for their help in X ray reflectivity measurement.
NR 35
TC 46
Z9 46
U1 7
U2 95
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0003-2700
EI 1520-6882
J9 ANAL CHEM
JI Anal. Chem.
PD APR 16
PY 2013
VL 85
IS 8
BP 3858
EP 3863
DI 10.1021/ac302801z
PG 6
WC Chemistry, Analytical
SC Chemistry
GA 128UI
UT WOS:000317794800012
PM 23384128
ER
PT J
AU Rand, E
Periyakaruppan, A
Tanaka, Z
Zhang, DA
Marsh, MP
Andrews, RJ
Lee, KH
Chen, B
Meyyappan, M
Koehne, JE
AF Rand, Emily
Periyakaruppan, Adaikkappan
Tanaka, Zuki
Zhang, David A.
Marsh, Michael P.
Andrews, Russell J.
Lee, Kendall H.
Chen, Bin
Meyyappan, M.
Koehne, Jessica E.
TI A carbon nanofiber based biosensor for simultaneous detection of
dopamine and serotonin in the presence of ascorbic acid
SO BIOSENSORS & BIOELECTRONICS
LA English
DT Article
DE Biosensor; Dopamine; Serotonin; Carbon nanofiber; Nanoelectrode array
ID NANOTUBE NANOELECTRODE ARRAYS; ELECTROCHEMICAL DETECTION; URIC-ACID;
ELECTRODES; FILM; BRAIN; MICROELECTRODES; VOLTAMMETRY; SELECTIVITY;
FABRICATION
AB A biosensor based on an array of vertically aligned carbon nanofibers (CNFs) grown by plasma enhanced chemical vapor deposition is found to be effective for the simultaneous detection of dopamine (DA) and serotonin (5-HT) in the presence of excess ascorbic acid (AA). The CNF electrode outperforms the conventional glassy carbon electrode (GCE) for both selectivity and sensitivity. Using differential pulse voltammetry (DPV), three distinct peaks are seen for the CNF electrode at 0.13 V, 0.45 V, and 0.70 V for the ternary mixture of AA, DA, and 5-HT. In contrast, the analytes are indistinguishable in a mixture using a GCE. For the CNF electrode, the detection limits are 50 nM for DA and 250 nM for 5-HT. Published by Elsevier B.V.
C1 [Rand, Emily; Periyakaruppan, Adaikkappan; Zhang, David A.; Andrews, Russell J.; Chen, Bin; Meyyappan, M.; Koehne, Jessica E.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
[Tanaka, Zuki; Chen, Bin] Univ Calif Santa Cruz, Dept Elect Engn, Santa Cruz, CA 95064 USA.
[Marsh, Michael P.; Lee, Kendall H.] Mayo Clin, Dept Neurosurg, Rochester, MN 55905 USA.
[Lee, Kendall H.] Mayo Clin, Dept Physiol & Biomed Engn, Rochester, MN 55905 USA.
RP Koehne, JE (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
EM Jessica.E.Koehne@nasa.gov
RI Periyakaruppan, Adaikkappan/B-7398-2013
OI Periyakaruppan, Adaikkappan/0000-0002-0395-6564
FU NIH [R01-NS75013]; NASA URC Contract [NNx08BA47A]
FX This work was in part supported by an NIH Grant (R01-NS75013) to Mayo
Clinic. AP was supported by a NASA URC Contract to Texas Southern
University (NNx08BA47A) as a visiting Postdoctoral Fellow. The authors
would like to thank Patrick Wilhite and Anshul Vyas of Santa Clara
University for helpful discussions regarding carbon nanofiber growth.
NR 30
TC 40
Z9 42
U1 4
U2 137
PU ELSEVIER ADVANCED TECHNOLOGY
PI OXFORD
PA OXFORD FULFILLMENT CENTRE THE BOULEVARD, LANGFORD LANE, KIDLINGTON,
OXFORD OX5 1GB, OXON, ENGLAND
SN 0956-5663
J9 BIOSENS BIOELECTRON
JI Biosens. Bioelectron.
PD APR 15
PY 2013
VL 42
BP 434
EP 438
DI 10.1016/j.bios.2012.10.080
PG 5
WC Biophysics; Biotechnology & Applied Microbiology; Chemistry, Analytical;
Electrochemistry; Nanoscience & Nanotechnology
SC Biophysics; Biotechnology & Applied Microbiology; Chemistry;
Electrochemistry; Science & Technology - Other Topics
GA 158EH
UT WOS:000319951700072
PM 23228495
ER
PT J
AU Yamaguchi, A
Mikouchi, T
Ito, M
Shirai, N
Barrat, JA
Messenger, S
Ebihara, M
AF Yamaguchi, A.
Mikouchi, T.
Ito, M.
Shirai, N.
Barrat, J. A.
Messenger, S.
Ebihara, M.
TI Experimental evidence of fast transport of trace elements in planetary
basaltic crusts by high temperature metamorphism
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE elemental transport; planetary basalts; metamorphism; geochemistry;
chronology
ID RARE-EARTH ELEMENTS; METEORITE SAMPLES; ION MICROPROBE; EUCRITES;
DIFFUSION; ABUNDANCES; EVOLUTION; MIGRATION; HISTORY; IMPACT
AB Incompatible elements (IEs) such as K, P, Ti, and rare earth elements (REEs) provide important constraints on the geochemistry and chronology of basaltic meteorites, most of which experienced complicated post-crystallization histories. These elements are immobile under subsolidus conditions because of their slow diffusion rates in planetary basalt minerals such as pyroxene and plagioclase. Thus, IEs are considered to preserve in most cases, reliable records of formation processes, even in ancient rocks that have undergone moderate thermal processing. However, observations of natural planetary samples suggest that melting of IE accessory carrier phases enhances the mobilization of such elements. Here we show that IEs are rapidly transported by near-solidus partial melting of highly IE-enriched minor phases including Ca-phosphate and Ti-rich phases. These partial melts occur as interconnected veins along cracks and fractures, and as thin films on surfaces of pore spaces, indicating that the melt mobilization is driven by surface tension. The melt transport provides the necessary condition for melt migration consistent with the presence of the depleted basaltic eucrites. Also, reaction between major minerals pyroxene and plagioclase, and partial melts may cause disturbance and resetting of some isotopic systems. These results have important implications for a range of geochemical investigations. In particular, the elemental fractionation resulting from such partial melting may result in improper age determinations. (C) 2013 Elsevier B.V. All rights reserved.
C1 [Yamaguchi, A.] Natl Inst Polar Res, Tachikawa, Tokyo 1908518, Japan.
[Yamaguchi, A.] Grad Univ Adv Sci, Sch Multidisciplinary Sci, Dept Polar Sci, Tachikawa, Tokyo 1908518, Japan.
[Mikouchi, T.] Univ Tokyo, Dept Earth & Planetary Sci, Tokyo 1130033, Japan.
[Ito, M.] USRA Houston, Lunar & Planetary Inst, Houston, TX 77058 USA.
[Ito, M.; Messenger, S.] NASA, Robert M Walker Lab Space Sci, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA.
[Shirai, N.; Ebihara, M.] Tokyo Metropolitan Univ, Grad Sch Sci, Hachioji, Tokyo 1920397, Japan.
[Barrat, J. A.] Univ Europeenne Bretagne, UBO IUEM, CNRS UMR 6538, F-29280 Plouzane, France.
RP Yamaguchi, A (reprint author), Natl Inst Polar Res, Tachikawa, Tokyo 1908518, Japan.
EM yamaguch@nipr.ac.jp
FU Ministry of Education, Science, and Technology, Japan, NIPR [KP-6]; NASA
FX This work is partly supported by a Grant-in-Aid for Scientific Research
from Ministry of Education, Science, and Technology, Japan, NIPR
Research Project Funds, KP-6, and by a NASA Origins Program Grant to
S.M., and Cosmochemistry Program to S.M. and M.I. We thank reviewers, C.
Floss and anonymous reviewers for constructing reviews, and B. Marty for
editorial assistance.
NR 32
TC 8
Z9 8
U1 1
U2 17
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-821X
J9 EARTH PLANET SC LETT
JI Earth Planet. Sci. Lett.
PD APR 15
PY 2013
VL 368
BP 101
EP 109
DI 10.1016/j.epsl.2013.02.036
PG 9
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 160AH
UT WOS:000320087900011
ER
PT J
AU de Groot, WJ
Cantin, AS
Flannigan, MD
Soja, AJ
Gowman, LM
Newbery, A
AF de Groot, William J.
Cantin, Alan S.
Flannigan, Michael D.
Soja, Amber J.
Gowman, Lynn M.
Newbery, Alison
TI A comparison of Canadian and Russian boreal forest fire regimes
SO FOREST ECOLOGY AND MANAGEMENT
LA English
DT Article
DE Carbon emissions; Fire behaviour; Fire ecology; Fire weather; Fuels
ID CROWN FIRE; MANAGEMENT; SYSTEM
AB Boreal forest dynamics are largely driven by disturbance, and fire is a prevalent force of change across the boreal circumpolar region. North American and Eurasian boreal fire regimes are known to be very different but there are few quantitative comparison studies. Russian and Canadian boreal fire regimes are compared using fire weather, fire statistics, fire behaviour, and C emissions data from two large study areas. Fuel consumption, head fire intensity, and C emissions were modelled using fire weather data, fuels data and burned area polygons for all large (200+ ha) fires that occurred in the study areas during 2001-2007. Fire behaviour and C emissions of each large fire were simulated with the Canadian Fire Effects Model (CanFIRE) using fuel type and fuel load data of the burned areas, and Canadian Forest Fire Weather Index System parameters, as interpolated to the fire from the weather station network on the average active fire date. In the Russian study area located in central Siberia, there was an annual average of 1441.9 large fires per 100 M ha of forest land that burned 1.89 M ha (average large fire size = 1312 ha, mean fire return interval = 52.9 years) with an average fire intensity of 4858 kW m(-1). In the western Canada study area, there was an annual average of 93.7 large fires per 100 M ha of forest land that burned 0.56 M ha of forest (average large fire size = 5930 ha, mean fire return interval = 179.9 years) with an average fire intensity of 6047 kW m(-1). The 2001-2007 fire size distribution and annual area burned in the Canadian study area were very similar to 1970-2009 statistics, although large fire frequency was higher and average large fire size was smaller. Similar long-term fire statistics for Russia currently do not exist for comparison. The C emissions rate (t ha(-1) of burned area) was 53% higher in the Canadian study area due to higher pre-burn forest floor fuel loads and higher fuel consumption by crown fires. However, the Russian study area had much higher total C emissions (per 100 M ha of forest area) because of greater annual area burned. The Russian C emissions estimate in this study is likely conservative due to low forest floor fuel load estimates in available datasets. Fire regime differences are discussed in terms of fuel, weather, and fire ecology. Crown Copyright (C) 2012 Published by Elsevier B.V. All rights reserved.
C1 [de Groot, William J.; Cantin, Alan S.; Gowman, Lynn M.; Newbery, Alison] Canadian Forest Serv, Nat Resources Canada, Sault Ste Marie, ON P6A 2E5, Canada.
[Flannigan, Michael D.] Univ Alberta, Dept Renewable Resources, Edmonton, AB T6G 2H1, Canada.
[Soja, Amber J.] NASA, Natl Inst Aerosp, Langley Res Ctr, Climate Sci Branch, Hampton, VA 23681 USA.
[Soja, Amber J.] NASA, Natl Inst Aerosp, Langley Res Ctr, Chem & Dynam Branch, Hampton, VA 23681 USA.
RP de Groot, WJ (reprint author), Canadian Forest Serv, Nat Resources Canada, 1219 Queen St East, Sault Ste Marie, ON P6A 2E5, Canada.
EM bill.degroot@nrcan.gc.ca
RI Flannigan, Michael/G-6996-2015
OI Flannigan, Michael/0000-0002-9970-5363
FU USDA Forest Service; NASA Land Cover Land Use Change (LCLUC) program;
NASA Terrestrial Ecosystems (TE) program; NASA InterDisciplinary Science
(IDS) program
FX Ji-Zhong Jin provided historical fire weather data for Russia. Sara
Bennett conducted GIS analyses. Doug McRae, Brian Stocks, and Sue Canard
provided valuable expertise and advice. We gratefully acknowledge
support provided by the USDA Forest Service and NASA Land Cover Land Use
Change (LCLUC), Terrestrial Ecosystems (TE) and InterDisciplinary
Science (IDS) programs.
NR 52
TC 44
Z9 44
U1 8
U2 74
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0378-1127
J9 FOREST ECOL MANAG
JI For. Ecol. Manage.
PD APR 15
PY 2013
VL 294
SI SI
BP 23
EP 34
DI 10.1016/j.foreco.2012.07.033
PG 12
WC Forestry
SC Forestry
GA 125MW
UT WOS:000317544900004
ER
PT J
AU Fu, LL
Haines, BJ
AF Fu, Lee-Lueng
Haines, Bruce J.
TI The challenges in long-term altimetry calibration for addressing the
problem of global sea level change
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Altimetry; Calibration; Sea level change
ID TOPEX MICROWAVE RADIOMETER; PRECISION ORBIT DETERMINATION; TERRESTRIAL
REFERENCE FRAME; CLIMATE DATA RECORD; SATELLITE ALTIMETRY; ABSOLUTE
CALIBRATION; TOPOGRAPHY MISSION; GEOCENTER MOTION; TOPEX/POSEIDON;
JASON-1
AB Long-term change of the global sea level resulting from climate change has become an issue of great societal interest. The advent of the technology of satellite altimetry has modernized the study of sea level on both global and regional scales. In combination with in situ observations of the ocean density and space observations of Earth's gravity variations, satellite altimetry has become an essential component of a global observing system for monitoring and understanding sea level change. The challenge of making sea level measurements with sufficient accuracy to discern long-term trends and allow the patterns of natural variability to be distinguished from those linked to anthropogenic forcing rests largely on the long-term efforts of altimeter calibration and validation. The issues of long-term calibration for the various components of the altimeter measurement system are reviewed in the paper. The topics include radar altimetry, the effects of tropospheric water vapor, orbit determination, gravity field, tide gauges, and the terrestrial reference frame. The necessity for maintaining a complete calibration effort and the challenges of sustaining it into the future are discussed. (C) 2012 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Fu, Lee-Lueng; Haines, Bruce J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Fu, LL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM llf@jpl.nasa.gov; bruce.j.haines@jpl.nasa.gov
FU National Aeronautic and Space Administration; Jason-1 Project;
OSTM/Jason-2 Project
FX The research presented in the paper was carried out at the Jet
Propulsion Laboratory (JPL), California Institute of Technology, under
contract with the National Aeronautic and Space Administration. Support
from the Jason-1 and OSTM/Jason-2 Projects is acknowledged. We are
grateful for input from three anonymous reviewers, as well as Xiaoping
Wu, Shannon Brown and Shailen Desai at JPL.; (C) 2012 California
Institute of Technology. Government sponsorship acknowledged.
NR 101
TC 17
Z9 17
U1 1
U2 23
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD APR 15
PY 2013
VL 51
IS 8
BP 1284
EP 1300
DI 10.1016/j.asr.2012.06.005
PG 17
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 129XZ
UT WOS:000317878600002
ER
PT J
AU Melachroinos, SA
Lemoine, FG
Zelensky, NP
Rowlands, DD
Luthcke, SB
Bordyugov, O
AF Melachroinos, S. A.
Lemoine, F. G.
Zelensky, N. P.
Rowlands, D. D.
Luthcke, S. B.
Bordyugov, O.
TI The effect of geocenter motion on Jason-2 orbits and the mean sea level
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Jason-2; Geocenter motion; GPS; SLRIDORIS; Mean sea level error
ID TERRESTRIAL REFERENCE FRAME; GPS; MODEL; TOPEX/POSEIDON; TRACKING;
SERVICE; SERIES; DORIS; EARTH; SLR
AB We compute a series of Jason-2 GPS and SLR/DORIS-based orbits using ITRF2005 and the std0905 standards (Lemoine et al., 2010). Our GPS and SLR/DOR/S orbit data sets span a period of 2 years from cycle 3 (July 2008) to cycle 74 (July 2010). We extract the Jason-2 orbit frame translational parameters per cycle by the means of a Helmert transformation between a set of reference orbits and a set of test orbits. We compare the annual terms of these time-series to the annual terms of two different geocenter motion models where biases and trends have been removed. Subsequently, we include the annual terms of the modeled geocenter motion as a degree-1 loading displacement correction to the GPS and SLR/DORIS tracking network of the POD process. Although the annual geocenter motion correction would reflect a stationary signal in time, under ideal conditions, the whole geocenter motion is a non-stationary process that includes secular trends. Our results suggest that our GSFC Jason-2 GPS-based orbits are closely tied to the center of mass (CM) of the Earth consistent with our current force modeling, whereas GSFC's SLR/DORIS-based orbits are tied to the origin of ITRF2005, which is the center of figure (CF) for sub-secular scales. We quantify the GPS and SLR/DORIS orbit centering and how this impacts the orbit radial error over the globe, which is assimilated into mean sea level (MSL) error, from the omission of the annual term of the geocenter correction. We find that for the SLR/DORIS std0905 orbits, currently used by the oceanographic community, only the negligence of the annual term of the geocenter motion correction results in a - 4.67 +/- 3.40 mm error in the Z-component of the orbit frame which creates 1.06 +/- 2.66 mm of systematic error in the MSL estimates, mainly due to the uneven distribution of the oceans between the North and South hemisphere. (C) 2012 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Melachroinos, S. A.; Lemoine, F. G.; Zelensky, N. P.; Rowlands, D. D.; Luthcke, S. B.; Bordyugov, O.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Branch, Greenbelt, MD 20771 USA.
[Melachroinos, S. A.; Zelensky, N. P.; Bordyugov, O.] SGT Inc, Greenbelt, MD USA.
RP Melachroinos, SA (reprint author), NASA, Goddard Space Flight Ctr, Planetary Geodynam Branch, Greenbelt, MD 20771 USA.
EM Smelachroinos@sgt-inc.com; Frank.G.Lemoine@nasa.gov
RI Lemoine, Frank/D-1215-2013; Rowlands, David/D-2751-2012
FU NASA [NNH09ZDA001N-IDS, NNH07ZDA001N-OSTST]
FX This research was supported by the following NASA Programs:
NNH09ZDA001N-IDS: Interdisciplinary Research in Earth Science (IDS) and
NNH07ZDA001N-OSTST: Ocean Surface Topography Science Team. We thank the
two anonymous reviewers, Dr. Xavier Collilieux and the editor Dr. Pascal
Willis for their constructive comments on this manuscript.
NR 45
TC 7
Z9 7
U1 0
U2 9
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD APR 15
PY 2013
VL 51
IS 8
BP 1323
EP 1334
DI 10.1016/j.asr.2012.06.004
PG 12
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 129XZ
UT WOS:000317878600005
ER
PT J
AU Haines, BJ
Desai, SD
Born, GH
AF Haines, Bruce J.
Desai, Shailen D.
Born, George H.
TI GPS monitoring of vertical seafloor motion at Platform Harvest
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE GPS positioning; Altimeter calibration; Seafloor subsidence; Sea level
ID HEIGHT TIME-SERIES; ABSOLUTE CALIBRATION; CROSS-CALIBRATION; RADAR
ALTIMETERS; JASON-1; TOPEX/POSEIDON; SURFACE; SATELLITE; RECEIVER; PHASE
AB We describe results from two decades of monitoring vertical seafloor motion at the Harvest oil platform, NASA's prime verification site for the TOPEX/Poseidon and Jason series of reference altimeter missions. Using continuous GPS observations, we refine estimates of the platform subsidence due most likely to fluid withdrawal linked to oil production and describe the impact on estimates of stability for the altimeter measurement systems. The cumulative seafloor subsidence over 20 yrs is approximately 10 cm, but the rate does not appear constant. The apparent non-linear nature of the vertical motion, coupled with long-period GPS errors, implies that the quality of the seafloor motion estimates is not uniform over the 20-yr period. For the Jason-1 era (2002-2009), competing estimates for the subsidence show agreement to better than 1 mm yr(-1). Longer durations of data are needed before the seafloor motion estimates for the Jason-2 era (2008-present) can approach this level of accuracy. (C) 2012 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Haines, Bruce J.; Desai, Shailen D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Born, George H.] Univ Colorado, Colorado Ctr Astrodynam Res, Boulder, CO 80310 USA.
RP Haines, BJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MIS 238-600, Pasadena, CA 91109 USA.
EM bruce.j.haines@jpl.nasa.gov
FU NASA
FX We are indebted to Dave Stowers (JPL) and UNAVCO for their support of
the GPS component of the Harvest experiment, and to Christina Selle
(JPL) for her significant efforts in reprocessing the historical GPS
data for improved orbit and clock products. The Harvest research
activities are funded by the NASA Physical Oceanography Program. We are
grateful to Eric Lindstrom and Lee Fu for advancing the Harvest
experiment and for assisting with the renewal of interagency agreements
needed for experiment upgrades. Production data for the Arguello
Reservoir were obtained from the U. S. Bureau of Ocean Energy
Management. We thank three anonymous reviewers for their comments and
suggestions, which have led to important improvements in the paper. A
portion of the work described in this paper was performed at the Jet
Propulsion Laboratory, California Institute of Technology under contract
with the National Aeronautics and Space Administration.
NR 50
TC 2
Z9 2
U1 0
U2 6
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD APR 15
PY 2013
VL 51
IS 8
BP 1369
EP 1382
DI 10.1016/j.asr.2012.11.008
PG 14
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 129XZ
UT WOS:000317878600008
ER
PT J
AU Willis, P
Mertikas, S
Argus, DF
Bock, O
AF Willis, Pascal
Mertikas, Stelios
Argus, Don F.
Bock, Olivier
TI DORIS and GPS monitoring of the Gavdos calibration site in Crete
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE DORIS; GPS; Satellite altimetry calibration; Gavdos; Troposphere
ID ABSOLUTE CALIBRATION; PLATE KINEMATICS; CONSTRAINTS; SATELLITE; JASON-1;
TOPEX/POSEIDON; DEFORMATION; GRADIENTS; ITRF2008; NETWORK
AB Due to its specific geographical location as well as its geodetic equipment (DORIS, GNSS, microwave transponder and tide gauges), the Gavdos station in Crete, Greece is one of the very few sites around the world used for satellite altimetry calibration. To investigate the quality of the Gavdos geodetic coordinates and velocities, we analyzed and compared here DORIS and GPS-derived results obtained during several years of observations. The DORIS solution is the latest ignwd11 solution at IGN, expressed in ITRF2008, while the GPS solution was obtained using the GAMIT software package. Current results show that 1-2 mm/yr agreement can be obtained for 3-D velocity, showing a good agreement with current geophysical models. In particular, the agreement obtained for the vertical velocity is around 0.3-0.4 mm/yr, depending on the terrestrial reference frame. As a by-product of these geodetic GPS and DORIS results, Zenith Tropospheric Delays (ZTDs) estimations were also compared in 2010 between these two techniques, and compared to ECMWF values, showing a 6.6 mm agreement in dispersion without any significant difference between GPS and DORIS (with a 97.6% correlation), but with a 13-14 mm agreement in dispersion when comparing to ECMWF model (with only about 90% correlation for both techniques). These tropospheric delay estimations could also provide an external calibration of the tropospheric correction used for the geophysical data of satellite altimetry missions. (C) 2012 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Willis, Pascal] Inst Natl Informat Geog & Forestiere, Direct Tech, F-94165 St Mande, France.
[Willis, Pascal] UFR STEP, Inst Phys Globe Paris, PRES Sorbonne Paris Cite, F-75013 Paris, France.
[Mertikas, Stelios] Tech Univ Crete, Dept Mineral Resources Engn, Geodesy & Geomat Engn Lab, Khania 73100, Greece.
[Argus, Don F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bock, Olivier] Inst Natl Informat Geog & Forestiere, LAREG, F-77455 Marne La Vallee, France.
RP Willis, P (reprint author), Inst Natl Informat Geog & Forestiere, Direct Tech, 2 Ave Pasteur, F-94165 St Mande, France.
EM pascal.willis@ign.fr; mertikas@mred.tuc.gr; Donald.F.Argus@jpl.nasa.gov;
olivier.bock@ign.fr
RI Willis, Pascal/A-8046-2008
OI Willis, Pascal/0000-0002-3257-0679
FU National Aeronautics and Space Administration (NASA); FP7-REGPOT-2008-1
(SOFIA) [229885]; European Commission
FX This work was supported by the Centre National d'Etudes Spatiales
(CNES). It is based on observations with DORIS embarked on SPOTs,
TOPEX/Poseidon, Envisat, Jason-2 and Cryosat-2 satellites. Don Argus
performed research at Jet Propulsion Laboratory, under contract with the
National Aeronautics and Space Administration (NASA). This work has been
supported by the FP7-REG-POT-2008-1, Project No. 229885 (SOFIA),
sponsored by the European Commission. The help and support of Mr. X.
Frantzis for the GAMIT processing is much appreciated. This paper is
IPGP contribution number 3305.
NR 43
TC 1
Z9 1
U1 2
U2 18
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
EI 1879-1948
J9 ADV SPACE RES
JI Adv. Space Res.
PD APR 15
PY 2013
VL 51
IS 8
BP 1438
EP 1447
DI 10.1016/j.asr.2012.08.006
PG 10
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 129XZ
UT WOS:000317878600012
ER
PT J
AU Lowe, KT
Maisto, P
Byun, G
Simpson, RL
Verkamp, M
Danehy, PM
Tiemsin, PI
Wohl, CJ
AF Lowe, K. Todd
Maisto, Pietro
Byun, Gwibo
Simpson, Roger L.
Verkamp, Max
Danehy, Paul M.
Tiemsin, Pacita I.
Wohl, Christopher J.
TI Laser velocimetry with fluorescent dye-doped polystyrene microspheres
SO OPTICS LETTERS
LA English
DT Article
AB Simultaneous Mie scattering and laser-induced fluorescence (LIF) signals are obtained from individual polystyrene latex microspheres dispersed in an air flow. Microspheres less than 1 mu m mean diameter were doped with two organic fluorescent dyes, Rhodamine B (RhB) and dichlorofluorescein (DCF), intended either to provide improved particle-based flow velocimetry in the vicinity of surfaces or to provide scalar flow information (e. g., marking one of two fluid streams). Both dyes exhibit measureable fluorescence signals that are on the order of 10(-3) to 10(-4) times weaker than the simultaneously measured Mie signals. It is determined that at the conditions measured, 95.5% of RhB LIF signals and 32.2% of DCF signals provide valid laser-Doppler velocimetry measurements compared with the Mie scattering validation rate with 6.5 W of 532 nm excitation, while RhB excited with 1.0 W incident laser power still exhibits 95.4% valid velocimetry signals from the LIF channel. The results suggest that the method is applicable to wind tunnel measurements near walls where laser flare can be a limiting factor and monodisperse particles are essential.
C1 [Lowe, K. Todd; Maisto, Pietro] Virginia Tech Univ, Dept Aerosp & Ocean Engn, Blacksburg, VA 24061 USA.
[Byun, Gwibo; Simpson, Roger L.] AUR Inc, Blacksburg, VA 24060 USA.
[Verkamp, Max; Danehy, Paul M.; Tiemsin, Pacita I.; Wohl, Christopher J.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Lowe, KT (reprint author), Virginia Tech Univ, Dept Aerosp & Ocean Engn, Blacksburg, VA 24061 USA.
EM kelowe@vt.edu
FU NASA ARMD Seedling Fund; NIA Cooperative Agreement [NNL09AA00A]
FX The authors acknowledge the support of the NASA ARMD Seedling Fund and
NIA Cooperative Agreement NNL09AA00A.
NR 10
TC 2
Z9 2
U1 3
U2 29
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 0146-9592
J9 OPT LETT
JI Opt. Lett.
PD APR 15
PY 2013
VL 38
IS 8
BP 1197
EP 1199
PG 3
WC Optics
SC Optics
GA 125ZG
UT WOS:000317580200004
PM 23595429
ER
PT J
AU Odom, B
AF Odom, Brian
TI Encyclopedia of the US Presidency: A Historical Reference
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 [Odom, Brian] NASA, Marshall Space & Flight Ctr, Huntsville, AL 35811 USA.
RP Odom, B (reprint author), NASA, Marshall Space & Flight Ctr, Huntsville, AL 35811 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU REED BUSINESS INFORMATION
PI NEW YORK
PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD APR 15
PY 2013
VL 138
IS 7
BP 110
EP 110
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 124IW
UT WOS:000317458000253
ER
PT J
AU Yao, YJ
Liang, SL
Cheng, J
Liu, SM
Fisher, JB
Zhang, XD
Jia, K
Zhao, X
Qing, QM
Zhao, B
Han, SJ
Zhou, GS
Zhou, GY
Li, YL
Zhao, SH
AF Yao, Yunjun
Liang, Shunlin
Cheng, Jie
Liu, Shaomin
Fisher, Joshua B.
Zhang, Xudong
Jia, Kun
Zhao, Xiang
Qing, Qiming
Zhao, Bin
Han, Shijie
Zhou, Guangsheng
Zhou, Guoyi
Li, Yuelin
Zhao, Shaohua
TI MODIS-driven estimation of terrestrial latent heat flux in China based
on a modified Priestley-Taylor algorithm
SO AGRICULTURAL AND FOREST METEOROLOGY
LA English
DT Article
DE Latent heat flux; Evapotranspiration; Priestley-Taylor; MODIS; China
ID SURFACE-ENERGY BALANCE; NET PRIMARY PRODUCTION; AMAZON RAIN-FORESTS;
REMOTE-SENSING DATA; EVAPOTRANSPIRATION ALGORITHM; COMBINATION THEORY;
THERMAL INERTIA; CARBON-DIOXIDE; SATELLITE DATA; LAND SURFACES
AB Because of China's large size, satellite observations are necessary for estimation of the land surface latent heat flux (LE). We describe here a satellite-driven Priestley-Taylor (PT)-based algorithm constrained by the Normalized Difference Vegetation Index (NDVI) and Apparent Thermal Inertia (ATI) derived from temperature change over time. We compare to the satellite-driven PT-based approach, PT-JPL, and validate both models using data collected from 16 eddy covariance flux towers in China. Like PT-JPL, our proposed algorithm avoids the computational complexities of aerodynamic resistance parameters. We run the algorithms with monthly Moderate Resolution Imaging Spectroradiometer (MODIS) products (0.05 degrees resolution), including albedo, Land Surface Temperature (LST), surface emissivity, and NDVI; and, Insolation from the Japan Aerospace Exploration Agency (JAXA). We find good agreement between our estimates of monthly LE and field-measured LE, with respective Root Mean Square Error (RMSE) and bias differences of 12.5 Wm(-2) and -6.4Wm(-2). As compared with PT-JPL, our proposed algorithm has higher correlations with ground-measurements. Between 2001 and 2010, LE shows generally negative trends in most regions of China, though positive LE trends occur over 39% of the region, primarily in Northeast, North and South China. Our results indicate that the variations of terrestrial LE are responding to large-scale droughts and afforestation caused by human activity with direct links to terrestrial energy exchange, both spatially and temporally. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Yao, Yunjun; Liang, Shunlin; Cheng, Jie; Jia, Kun; Zhao, Xiang] Beijing Normal Univ, State Key Lab Remote Sensing Sci, Beijing 100875, Peoples R China.
[Yao, Yunjun; Liang, Shunlin; Cheng, Jie; Jia, Kun; Zhao, Xiang] Chinese Acad Sci, Inst Remote Sensing Applicat, Beijing, Peoples R China.
[Yao, Yunjun; Liang, Shunlin; Cheng, Jie; Jia, Kun; Zhao, Xiang] Beijing Normal Univ, Coll Global Change & Earth Syst Sci, Beijing 100875, Peoples R China.
[Liang, Shunlin] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Liu, Shaomin] Beijing Normal Univ, Sch Geog, State Key Lab Remote Sensing Sci, Beijing 100875, Peoples R China.
[Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zhang, Xudong] Chinese Acad Forestry, Inst Forestry, Beijing 100091, Peoples R China.
[Qing, Qiming] Peking Univ, Inst Remote Sensing & GIS, Beijing 100871, Peoples R China.
[Zhao, Bin] Fudan Univ, Minist Educ Key Lab Biodivers Sci & Ecol Engn, Shanghai 200433, Peoples R China.
[Han, Shijie] Chinese Acad Sci, Inst Appl Ecol, Shenyang 110016, Peoples R China.
[Zhou, Guangsheng] Chinese Acad Sci, Inst Bot, Lab Quantitat Vegetat Ecol, Beijing 100093, Peoples R China.
[Zhou, Guoyi; Li, Yuelin] Chinese Acad Sci, South China Bot Garden, Guangzhou 510650, Guangdong, Peoples R China.
[Zhao, Shaohua] Environm Satellite Ctr, Minist Environm Protect, Beijing 100094, Peoples R China.
RP Yao, YJ (reprint author), Beijing Normal Univ, Coll Global Change & Earth Syst Sci, Beijing 100875, Peoples R China.
EM boyyunjun@163.com
RI Zhao, Bin/E-5349-2010; Zhao, Bin/I-3651-2013; Li, Yuelin/D-7249-2011;
Cheng, Jie/G-2039-2011; liang, shunlin/C-2809-2015; rslab,
water/O-7043-2015;
OI Zhao, Bin/0000-0002-3530-2469; Fisher, Joshua/0000-0003-4734-9085
FU Special Foundation for Free Exploration of State Laboratory of Remote
Sensing Science [ZY12-11]; Natural Science Fund of China [41201331,
40901167, 41101313]; High-Tech Research and Development Program of China
[2009AA122100]; Advance Research Program of Civil Aerospace Technology
FX The authors thank the anonymous reviewers for their critical and helpful
comments and suggestions. The authors would like to thank Dr. Xianhong
Xie, Dr. Wenping Yuan, Dr. Xianglan Li, Dr. Xiaotong Zhang, Dr. Bo Jiang
and Dr. Liang Sun from the College of Global Change and Earth System
Science, Beijing Normal University, China, for their suggestions. The
authors would like to thank Dr. Qibing Wang from the State Key Labratory
of Vegetation and Environmental Change, Institute of Botany, Chinese
Academy of Sciences, for his help. The authors would also like to extend
their thanks to China Meteorological Administration (CMA) for providing
ground-measured meteorological data. Latent heat flux, net radiation,
shortwave solar radiation and corresponding meteorological observations
were obtained from the Coordinated Enhanced Observation Project (CEOP)
in arid and semi-arid regions of northern China
(http://observation.tea.ac.cn/), the water experiments of Environmental
and Ecological Science Data Center for West China
(http://westdc.westgis.ac.cn/water), the Atmosphere Radiation
Measurement (ARM) Program of the U.S. Department of Energy
(http://www.archive.arm.gov/), the ChinaFlux network
(http://www.chinaflux.org/index/index.asp), the Japan Aerospace
Exploration Agency (JAXA)
(http://suzaku.eorcjaxajp/GLI/data/final/landpar/index.html). DEM data
was derived from Shuttle Radar Topography Mission (STRM) DEM data
(http://datamirror.csdb.cn/dem/searchjsp). The monthly PDSI products
were derived from the NCAR CGD's Climate Analysis Section dataset
(http://www.cgd.ucar.edu/cas/catalog/cljmind/pdsi.html). MODIS NDVI,
LST, albedo and land cover satellite products were obtained online
(http://reverb.echo.nasa.gov/reverb). This work was partially supported
by the Special Foundation for Free Exploration of State Laboratory of
Remote Sensing Science (Grant No. ZY12-11), the Natural Science Fund of
China (No. 41201331, No. 40901167 and No. 41101313), the High-Tech
Research and Development Program of China (No. 2009AA122100), the
Advance Research Program of Civil Aerospace Technology: Research on the
Key Techniques in Remote Sensing Data Processing for Solid Surface
Elements Extraction. J.B.F. contributed to this paper from the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
NR 80
TC 33
Z9 38
U1 4
U2 91
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-1923
EI 1873-2240
J9 AGR FOREST METEOROL
JI Agric. For. Meteorol.
PD APR 15
PY 2013
VL 171
BP 187
EP 202
DI 10.1016/j.agrformet.2012.11.016
PG 16
WC Agronomy; Forestry; Meteorology & Atmospheric Sciences
SC Agriculture; Forestry; Meteorology & Atmospheric Sciences
GA 111HS
UT WOS:000316513000018
ER
PT J
AU Derkowski, A
Bristow, TF
Wampler, JM
Srodon, J
Marynowski, L
Elliott, WC
Chamberlain, CP
AF Derkowski, Arkadiusz s
Bristow, Thomas F.
Wampler, J. M.
Srodon, Jan
Marynowski, Leszek
Elliott, W. Crawford
Chamberlain, C. Page
TI Hydrothermal alteration of the Ediacaran Doushantuo Formation in the
Yangtze Gorges area (South China)
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID K-AR; ILLITE-SMECTITE; CLAY-MINERALS; NEOPROTEROZOIC DOUSHANTUO;
TRIOCTAHEDRAL SMECTITE; THERMAL MATURITY; LAYER SILICATES; DISTURBED
BELT; ROCK EXTRACTS; CAP CARBONATE
AB The geochemical and fossil record preserved in the Ediacaran age (635-551 Ma) Doushantuo Formation of South China has been extensively examined to explore the impact of changing climate and the oxidation state of the oceans on the development and distribution of early multicellular life. In the Yangtze Gorges area, this formation shows many of the geochemical trends and features thought to typify global ocean chemistry in the Ediacaran Period, but there are indications that post-sedimentary processes modified these signals. This study of clay minerals and organic matter builds a more detailed picture of the type and degree of post-sedimentary alteration at different stratigraphic levels of the formation and focuses on how this alteration influenced stable carbon and oxygen isotope records.
In the cratonward Jiulongwan and Huajipo sections of the Doushantuo Formation, its lower part (Members 1 and 2) consists largely of dolomitic shale, rich in authigenic saponite that crystallized in an alkaline sedimentary basin. Saponite has been altered to chlorite via corrensite across tens of meters of strata in lower Member 2, with increased alteration downward toward the cap dolostone. The greater chloritization is accompanied by lower delta O-18 and higher delta D values of trioctahedral clays. This pattern of alteration of trioctahedral clays is likely due to hydrothermal fluid activity in the underlying, relatively permeable Nantuo Formation and cap dolostone. A concomitant increase of solid bitumen reflectance toward the base of the formation supports this idea. In the uppermost part of the formation in the Yangtze Gorges area (Member 4), a typical open water marine dolomitic shale rich in illite and organic matter, increases in the methylphenanthrenes ratio index and solid bitumen reflectance correlate with decrease of the bulk rock K/Al ratio upward, providing evidence for hot fluid migration above the nearly impermeable shale.
Clay from the upper part of the formation is enriched in O-18, but not in D, relative to clay from the lower parts, indicating progressive O-18-enrichment of hydrothermal fluids that percolated upward and laterally through permeable O-18-rich carbonates. A maximum hydrothermal-alteration temperature of similar to 200 degrees C is estimated from a calibration curve for illitization during burial diagenesis, but given that the hydrothermal activity probably occurred in short pulses, the temperature could have been much higher. K-Ar ages are consistent across different size fractions of fine illite from Member 4 shale (similar to 430 Ma) and from a K-bentonite bed near the base of Member 2 in the Jiuqunao section (similar to 325 Ma), similar to 25 km from Jiulongwan and Huajipo. These age values show that the diagenetic illite of the Doushantuo Formation is a product of either deep burial diagenesis overprinted by spatially limited hydrothermal activity or of two localized hydrothermal events.
Patterns of carbonate C-13 and O-18 depletion in the basal Doushantuo Formation are similar to chloritization trends and O-18 variation in diagenetic clay minerals. Given independent evidence for C-13 depletion of hydrothermal fluids, these trends indicate carbonate-fluid isotope exchange commensurate with the degree of post-sedimentary alteration, supporting a model of lithologically controlled differential diagenesis induced by hydrothermal fluids as the main control on C and O isotope variability in this stratigraphic interval. This model could potentially explain other notable delta C-13 excursions higher up in Member 3. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Derkowski, Arkadiusz s; Srodon, Jan] Polish Acad Sci, Res Ctr Krakow, Inst Geol Sci, PL-31002 Krakow, Poland.
[Bristow, Thomas F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Wampler, J. M.; Elliott, W. Crawford] Georgia State Univ, Dept Geosci, Atlanta, GA 30302 USA.
[Marynowski, Leszek] Univ Silesia, Fac Earth Sci, PL-41200 Sosnowiec, Poland.
[Chamberlain, C. Page] Stanford Univ, Dept Environm Earth Syst Sci, Stanford, CA 94305 USA.
RP Derkowski, A (reprint author), Polish Acad Sci, Res Ctr Krakow, Inst Geol Sci, Senacka 1, PL-31002 Krakow, Poland.
EM ndderkow@cyf-kr.edu.pl
NR 101
TC 15
Z9 15
U1 1
U2 74
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 APR 15
PY 2013
VL 107
BP 279
EP 298
DI 10.1016/j.gca.2013.01.015
PG 20
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 100QA
UT WOS:000315714700019
ER
PT J
AU Keller, LP
Messenger, S
AF Keller, Lindsay P.
Messenger, Scott
TI On the origins of GEMS grains: A reply
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Editorial Material
ID INTERPLANETARY DUST; MICROMETEORITES; ABUNDANCES; COMETS; STARS; IRON
AB The Comment by Bradley challenges our chemical and isotopic measurements of GEMS grains, arguing that pervasive infiltration of silicone oil and sample heating undermine our comparisons with equally uncertain interstellar grain compositions. However, we have already shown that such effects are negligible and cannot account for the extraordinary chemical variability of GEMS grains. Our data are also in excellent agreement with previous GEMS grain chemical analyses, and with GEMS grains in micrometeorites and within IDPs recently collected without the use of silicone oil. The order of magnitude variations in element abundances displayed by GEMS grains rule out a common origin by the extensive chemical and isotopic homogenization of circumstellar grains, as proposed by Bradley. The vast majority of GEMS grains also do not have radial compositional gradients, crystalline "relict" cores, or rims of condensed materials indicative of radiation exposure. The average element abundances of GEMS grains differ significantly and systematically from solar abundances and from those inferred for interstellar silicates based on element depletion patterns. A few GEMS grains have highly anomalous O isotopic compositions consistent with a condensation origin in evolved O-rich stellar envelopes and supernovae. Yet, on average, GEMS grains have O isotopic compositions very near to terrestrial and meteoritic values. These and other observations discussed in our paper place a strict upper limit on the number of GEMS grains that have preserved presolar origins. Published by Elsevier Ltd.
C1 [Keller, Lindsay P.; Messenger, Scott] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Keller, LP (reprint author), NASA, Lyndon B Johnson Space Ctr, Mail Code KR,2101 NASA Pkwy, Houston, TX 77058 USA.
EM Lindsay.P.Keller@nasa.gov
NR 21
TC 8
Z9 8
U1 0
U2 8
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD APR 15
PY 2013
VL 107
BP 341
EP 344
DI 10.1016/j.gca.2012.11.012
PG 4
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 100QA
UT WOS:000315714700023
ER
PT J
AU Vazquez-Cuervo, J
Dewitte, B
Chin, TM
Armstrong, EM
Purca, S
Alburqueque, E
AF Vazquez-Cuervo, Jorge
Dewitte, Boris
Chin, Toshio M.
Armstrong, Edward M.
Purca, Sara
Alburqueque, Edward
TI An analysis of SST gradients off the Peruvian Coast: The impact of going
to higher resolution
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Sea surface temperatures; Coastal/upwelling studies; Upwelling;
Satellite derived; Objective interpolation
ID SEA-SURFACE TEMPERATURE; CALIFORNIA CURRENT SYSTEM; PROJECT
AB The Peruvian Coastal Upwelling System (PCUS) is one of the most productive fisheries in the world. Upwelling events are associated with changes in the magnitude and location of frontal structures. SST gradients from four different data sets, NCDC, REMSS, OSTIA, and MUR are compared in two test areas off the PCUS: Paita (5 degrees S) and Pisco (14 degrees S). In both areas gradients derived from the MUR data set show greater magnitudes, as well as larger seasonal cycles. Off Pisco, the magnitude of the seasonal cycle of 2.2 degrees C/100 km in MUR is larger than the one derived from the lower resolution data sets. All data sets at Pisco exhibit a seasonal cycle that peaks in late Austral summer and early fall. Hovmoller diagrams calculated at 5.5 degrees S, 10.5 degrees S, and 14.5 degrees S show clearly defined offshore maxima in the cross-shore gradients for all the data sets. Upwelling scales determined by the distance to the first maxima vary depending on the data set used. At 5.5 degrees S upwelling scales vary from 10 km for MUR to 50 km for NCDC At 14.5 degrees S the scales vary from 20 km for MUR to 40 km for OSTIA. All four data sets show similar large-scale structures associated with the Peruvian upwelling. However, MUR shows finer scale structures that are most likely due to submesoscale to mesoscale eddies. Sub-sampled MUR 1 km data at the 25 km, 9 km, and 4 km resolutions compare well in magnitude and phase with the lower resolution products. Agreement in gradient magnitude between the lower resolution data sets and the MUR sub-sampled at their respective resolutions implies that the pixel-to-pixel analysis noise in MUR is at a similar level as the other data sets. (c) 2013 Elsevier Inc. All rights reserved.
C1 [Vazquez-Cuervo, Jorge; Chin, Toshio M.; Armstrong, Edward M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Dewitte, Boris] IRD, LEGOS, Toulouse, France.
[Purca, Sara] Inst Mar Peru, Cello, Peru.
[Alburqueque, Edward] Univ Nacl Mayor San Marcos, Lima, Peru.
RP Vazquez-Cuervo, J (reprint author), CALTECH, Jet Prop Lab, M-S 300-323,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Jorge.Vazquez@jpl.nasa.gov
OI Purca, Sara/0000-0001-8751-1476
FU National Aeronautics and Space Administration at the Jet Propulsion
Laboratory, California Institute of Technology
FX The work was carried out under contract with the National Aeronautics
and Space Administration at the Jet Propulsion Laboratory, California
Institute of Technology. The authors gratefully thank Instituto del Mar
del Peru (IMARPE) for providing both scientific and technical support.
The authors also thank three anonymous reviewers for their hardwork and
thoughtful reviews in significantly improving this manuscript.
NR 32
TC 13
Z9 13
U1 2
U2 36
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD APR 15
PY 2013
VL 131
BP 76
EP 84
DI 10.1016/j.rse.2012.12.010
PG 9
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 098JZ
UT WOS:000315546900006
ER
PT J
AU Hassanin, AH
Said, MA
Seyam, AFM
AF Hassanin, Ahmed H.
Said, Magdi A.
Seyam, Abdel-Fattah M.
TI Composite Porous Membrane for Protecting High-Performance Fibers from
Ultraviolet-Visible Radiation
SO JOURNAL OF APPLIED POLYMER SCIENCE
LA English
DT Article
DE composites; degradation; membranes; nanoparticles; nanowires and
nanocrystals; radiation
ID P-PHENYLENEBENZOBISOXAZOLE FIBERS; TIO2 NANOPARTICLES; ARAMID FIBERS;
MECHANISMS
AB High-strength fibers are used to produce high-strength-to-weight-ratio materials for applications such as composites, soft and hard body armor, bulletproof vests, and tendons for scientific balloons. Unfortunately, these fibers degrade when they are exposed to ultraviolet-visible (UV-vis) radiation. The objective of this research was to develop systems to improve the UV resistance of such fibers. Composite porous membranes from a polyurethane (PU) matrix loaded with rutile titanium dioxide (TiO2) nanoparticles were developed to protect a braid made of polybenzobisoxazole (PBO) yarns. The PU membranes loaded with TiO2 nanoparticles were prepared by a phase-inversion technique. The effects of the amount of TiO2 nanoparticles on the composite membrane morphological structure and UV-vis light transmission were evaluated. The results show that when the concentration of TiO2 nanoparticles was increased, the porosity of the membrane and its UV-vis blocking effectiveness increased. The UV-vis protection was evaluated by the wrapping of the PBO braid with the composite membranes and exposed to UV-vis radiation. The strength loss of the PBO fiber due to exposure was decreased from 75% for the unprotected sample to 7.8% for the protected sample in the PU loaded with 4% TiO2 nanoparticles. (C) 2012 Wiley Periodicals, Inc. J. Appl. Polym. Sci. 128: 1297-1303, 2013
C1 [Hassanin, Ahmed H.; Seyam, Abdel-Fattah M.] N Carolina State Univ, Coll Text, Raleigh, NC 27695 USA.
[Said, Magdi A.] NASA, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
RP Seyam, AFM (reprint author), N Carolina State Univ, Coll Text, Raleigh, NC 27695 USA.
EM aseyam@ncsu.edu
RI hassanin, ahmed/A-4718-2017
FU NASA, Balloon Research and Development Laboratory [NNXlOAE26G]
FX This work was funded by NASA, Balloon Research and Development
Laboratory (grant number NNXlOAE26G). The authors thank Rahul Vallabh of
North Carolina State University College of Textiles for his valuable
suggestions.
NR 18
TC 1
Z9 1
U1 2
U2 66
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0021-8995
J9 J APPL POLYM SCI
JI J. Appl. Polym. Sci.
PD APR 15
PY 2013
VL 128
IS 2
SI SI
BP 1297
EP 1303
DI 10.1002/app.38476
PG 7
WC Polymer Science
SC Polymer Science
GA 089RD
UT WOS:000314926800049
ER
PT J
AU Bauschlicher, CW
Ricca, A
AF Bauschlicher, Charles W., Jr.
Ricca, Alessandra
TI On the calculation of the vibrational frequencies of C6H4
SO CHEMICAL PHYSICS LETTERS
LA English
DT Article
ID GAUSSIAN-BASIS SETS; ORTHO-BENZYNE; ELECTRON CORRELATION; ENERGY;
THERMOCHEMISTRY; APPROXIMATION; EXCHANGE
AB DFT and CCSD(T) frequencies are compared with experiment for ortho-benzyne (C6H4). Four bands are found to be in disagreement with experiment at the DFT level. Surprisingly the CCSD(T) method only brings the triple bond stretch into agreement with experiment, but leaves a sizable difference with experiment for the other three bands. The results for three isotopologues suggests that all of the differences cannot be attributed to resonances. Additional experimental work on ortho-benzyne appears warranted. Published by Elsevier B.V.
C1 [Bauschlicher, Charles W., Jr.] NASA, Ames Res Ctr, Space Technol Div, Moffett Field, CA 94035 USA.
[Ricca, Alessandra] SETI Inst, Mountain View, CA 94043 USA.
RP Bauschlicher, CW (reprint author), NASA, Ames Res Ctr, Space Technol Div, Mail Stop 230-3, Moffett Field, CA 94035 USA.
EM Charles.W.Bauschlicher@nasa.gov; Alessandra.Ricca-1@nasa.gov
FU NASA's Astronomy and Physics Research and Analysis (APRA) program
[NNX07AH02G]; Astrophysics Theory and Fundamental Physics (ATFP) program
[NNX09AD18G]
FX A.R. thank the NASA's Astronomy and Physics Research and Analysis (APRA)
(NNX07AH02G) and Astrophysics Theory and Fundamental Physics (ATFP)
(NNX09AD18G) programs for their generous support of this work.
NR 25
TC 2
Z9 2
U1 0
U2 14
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0009-2614
EI 1873-4448
J9 CHEM PHYS LETT
JI Chem. Phys. Lett.
PD APR 12
PY 2013
VL 566
BP 1
EP 3
DI 10.1016/j.cplett.2013.02.048
PG 3
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 122WO
UT WOS:000317349300001
ER
PT J
AU Baker, DN
Kanekal, SG
Hoxie, VC
Henderson, MG
Li, X
Spence, HE
Elkington, SR
Friedel, RHW
Goldstein, J
Hudson, MK
Reeves, GD
Thorne, RM
Kletzing, CA
Claudepierre, SG
AF Baker, D. N.
Kanekal, S. G.
Hoxie, V. C.
Henderson, M. G.
Li, X.
Spence, H. E.
Elkington, S. R.
Friedel, R. H. W.
Goldstein, J.
Hudson, M. K.
Reeves, G. D.
Thorne, R. M.
Kletzing, C. A.
Claudepierre, S. G.
TI A Long-Lived Relativistic Electron Storage Ring Embedded in Earth's
Outer Van Allen Belt
SO SCIENCE
LA English
DT Article
ID RADIATION BELT; INNER MAGNETOSPHERE; CRRES; ACCELERATION; PROTONS;
MISSION; SAMPEX
AB Since their discovery more than 50 years ago, Earth's Van Allen radiation belts have been considered to consist of two distinct zones of trapped, highly energetic charged particles. The outer zone is composed predominantly of megaelectron volt (MeV) electrons that wax and wane in intensity on time scales ranging from hours to days, depending primarily on external forcing by the solar wind. The spatially separated inner zone is composed of commingled high-energy electrons and very energetic positive ions (mostly protons), the latter being stable in intensity levels over years to decades. In situ energy-specific and temporally resolved spacecraft observations reveal an isolated third ring, or torus, of high-energy (>2 MeV) electrons that formed on 2 September 2012 and persisted largely unchanged in the geocentric radial range of 3.0 to similar to 3.5 Earth radii for more than 4 weeks before being disrupted (and virtually annihilated) by a powerful interplanetary shock wave passage.
C1 [Baker, D. N.; Hoxie, V. C.; Li, X.; Elkington, S. R.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
[Kanekal, S. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Henderson, M. G.; Friedel, R. H. W.; Reeves, G. D.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Spence, H. E.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
[Goldstein, J.] SW Res Inst, Space Sci & Engn Div, San Antonio, TX USA.
[Hudson, M. K.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA.
[Thorne, R. M.] Univ Calif Los Angeles, Dept Atmospher & Ocean Sci, Los Angeles, CA USA.
[Kletzing, C. A.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Claudepierre, S. G.] Aerosp Corp, Los Angeles, CA 90009 USA.
RP Baker, DN (reprint author), Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA.
EM daniel.baker@lasp.colorado.edu
RI Spence, Harlan/A-1942-2011; Friedel, Reiner/D-1410-2012; Henderson,
Michael/A-3948-2011;
OI Reeves, Geoffrey/0000-0002-7985-8098; Friedel,
Reiner/0000-0002-5228-0281; Henderson, Michael/0000-0003-4975-9029;
Kletzing, Craig/0000-0002-4136-3348; Spence, Harlan/0000-0002-2526-2205
FU RBSP-Energetic Particle Composition and Thermal Plasma Suite; Johns
Hopkins University Applied Physics Laboratory (JHU/APL) [967399,
921649]; NASA [NAS5-01072]
FX This work was supported by RBSP-Energetic Particle Composition and
Thermal Plasma Suite funding provided by the Johns Hopkins University
Applied Physics Laboratory (JHU/APL) contract no. 967399, Electric and
Magnetic Field Instrument Suite and Integrated Science (EMFISIS) work
was supported on JHU/APL contract no. 921649, and both were funded under
NASA's Prime contract no. NAS5-01072. All Van Allen Probes observations
used in this study, along with display and analysis software, are
publicly available at the Web site www.rbsp-ect.lanl.gov.
NR 26
TC 90
Z9 92
U1 1
U2 28
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD APR 12
PY 2013
VL 340
IS 6129
BP 186
EP 190
DI 10.1126/science.1233518
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 122TQ
UT WOS:000317341400053
PM 23450000
ER
PT J
AU Rury, AS
AF Rury, Aaron S.
TI Examining resonant inelastic spontaneous scattering of classical
Laguerre-Gauss beams from molecules
SO PHYSICAL REVIEW A
LA English
DT Article
ID RAY-EMISSION SPECTRA; RAMAN-SCATTERING; COHERENT CONTROL; LASER MODES;
INTERFERENCE; SPECTROSCOPY; DYNAMICS; EXCITATIONS; DIAMOND; LIGHT
AB This paper treats theoretically the spontaneous resonant inelastic scattering of Laguerre-Gauss (LG) beams from the vibrations of complex polyatomic molecules within the semiclassical framework. We develop an interaction Hamiltonian that accounts for the position of the molecule within the excitation beam to derive the effective differential scattering cross section of a classical LG beam from a molecule using the frequency-domain third-order nonlinear optical response function. To gain physical insight, we utilize a model vibronic molecule to study the changes to this scattering process. For specific molecular parameters including vibrational frequency and relative displacement of the involved electronic states, this investigation shows that an incident LG beam asymmetrically enhances one of two participating excitation transitions causing modulation of the interference present in the scattering process. This modulation allows a pathway to coherent control of resonant inelastic scattering from complex, polyatomic molecules. We discuss the possible application of this control to the resonant x-ray inelastic scattering (RIXS) of small polyatomic molecules central to applications ranging from single-molecule electronics to solar energy science. DOI: 10.1103/PhysRevA.87.043408
C1 [Rury, Aaron S.] Univ Michigan, Appl Phys Program, Ann Arbor, MI 48109 USA.
[Rury, Aaron S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Rury, AS (reprint author), Univ Michigan, Appl Phys Program, Ann Arbor, MI 48109 USA.
EM arury@caltech.edu
OI Rury, Aaron/0000-0002-1836-1424
FU Defense Threat Reduction Agency-Joint Science and Technology Office for
Chemical and Biological Defense [HDTRA1-09-1-0005]
FX The author thanks R. J. Sension, P. R. Berman, D. G. Steel, and R. M.
Freeling for useful discussions. This work was supported by the Defense
Threat Reduction Agency-Joint Science and Technology Office for Chemical
and Biological Defense (Grant No. HDTRA1-09-1-0005).
NR 48
TC 7
Z9 7
U1 0
U2 16
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1050-2947
J9 PHYS REV A
JI Phys. Rev. A
PD APR 11
PY 2013
VL 87
IS 4
AR 043408
DI 10.1103/PhysRevA.87.043408
PG 18
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 123KQ
UT WOS:000317388700006
ER
PT J
AU Kothadia, R
Kulecz, WB
Kofman, IS
Black, AJ
Grier, JW
Schlegel, TT
AF Kothadia, Roshni
Kulecz, Walter B.
Kofman, Igor S.
Black, Adam J.
Grier, James W.
Schlegel, Todd T.
TI New System for Digital to Analog Transformation and Reconstruction of
12-Lead ECGs
SO PLOS ONE
LA English
DT Article
ID COMPUTER-PROGRAMS; ELECTROCARDIOGRAMS; REPRODUCIBILITY; CONVERTERS;
DISEASE
AB Introduction: We describe initial validation of a new system for digital to analog conversion (DAC) and reconstruction of 12-lead ECGs. The system utilizes an open and optimized software format with a commensurately optimized DAC hardware configuration to accurately reproduce, from digital files, the original analog electrocardiographic signals of previously instrumented patients. By doing so, the system also ultimately allows for transmission of data collected on one manufacturer's 12-lead ECG hardware/software into that of any other.
Materials and Methods: To initially validate the system, we compared original and post-DAC re-digitized 12-lead ECG data files (similar to 5-minutes long) in two types of validation studies in 10 patients. The first type quantitatively compared the total waveform voltage differences between the original and re-digitized data while the second type qualitatively compared the automated electrocardiographic diagnostic statements generated by the original versus re-digitized data.
Results: The grand-averaged difference in root mean squared voltage between the original and re-digitized data was 20.8 mu V per channel when re-digitization involved the same manufacturer's analog to digital converter (ADC) as the original digitization, and 28.4 mu V per channel when it involved a different manufacturer's ADC. Automated diagnostic statements generated by the original versus reconstructed data did not differ when using the diagnostic algorithm from the same manufacturer on whose device the original data were collected, and differed only slightly for just 1 of 10 patients when using a third-party diagnostic algorithm throughout.
Conclusion: Original analog 12-lead ECG signals can be reconstructed from digital data files with accuracy sufficient for clinical use. Such reconstructions can readily enable automated second opinions for difficult-to-interpret 12-lead ECGs, either locally or remotely through the use of dedicated or cloud-based servers.
C1 [Kothadia, Roshni] Natl Space Biomed Res Inst, Houston, TX USA.
[Kulecz, Walter B.; Kofman, Igor S.] Wyle Sci Technol & Engn Grp, Houston, TX USA.
[Black, Adam J.] Univ Minnesota, Minneapolis, MN USA.
[Grier, James W.] N Dakota State Univ, Fargo, ND 58105 USA.
[Schlegel, Todd T.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Schlegel, TT (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
EM todd.t.schlegel@nasa.gov
FU National Space Biomedical Research Institute summer student internship
program; NASA Johnson Space Center's Internal Research and Development
funds
FX Support for this work was provided by the National Space Biomedical
Research Institute summer student internship program (RK) and the NASA
Johnson Space Center's Internal Research and Development funds (TTS).
The funders had no role in study design, data collection and analysis,
decision to publish, or preparation of the manuscript.
NR 10
TC 2
Z9 2
U1 0
U2 4
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD APR 11
PY 2013
VL 8
IS 4
AR e61076
DI 10.1371/journal.pone.0061076
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 123JA
UT WOS:000317383200040
PM 23613787
ER
PT J
AU Connerney, J
AF Connerney, Jack
TI SOLAR SYSTEM Saturn's ring rain
SO NATURE
LA English
DT Editorial Material
ID MODEL; IONOSPHERE; EVOLUTION
C1 NASA, Planetary Magnetospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Connerney, J (reprint author), NASA, Planetary Magnetospheres Lab, Goddard Space Flight Ctr, Code 695, Greenbelt, MD 20771 USA.
EM jack.connerney@nasa.gov
RI connerney, john/I-5127-2013;
OI connerney, jack/0000-0001-7478-6462
NR 18
TC 3
Z9 3
U1 1
U2 10
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD APR 11
PY 2013
VL 496
IS 7444
BP 178
EP 179
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 122VM
UT WOS:000317346300032
PM 23579675
ER
PT J
AU O'Donoghue, J
Stallard, TS
Melin, H
Jones, GH
Cowley, SWH
Miller, S
Baines, KH
Blake, JSD
AF O'Donoghue, J.
Stallard, T. S.
Melin, H.
Jones, G. H.
Cowley, S. W. H.
Miller, S.
Baines, K. H.
Blake, J. S. D.
TI The domination of Saturn's low-latitude ionosphere by ring 'rain'
SO NATURE
LA English
DT Article
ID GIANT PLANET ATMOSPHERES; H-3(+); MODEL
AB Saturn's ionosphere is produced when the otherwise neutral atmosphere is exposed to a flow of energetic charged particles or solar radiation(1). At low latitudes the solar radiation should result in a weak planet-wide glow in the infrared, corresponding to the planet's uniform illumination by the Sun(2). The observed electron density of the low-latitude ionosphere, however, is lower and its temperature higher than predicted by models(3-5). A planet-to-ring magnetic connection has been previously suggested, in which an influx of water from the rings could explain the lower-than-expected electron densities in Saturn's atmosphere(6-8). Here we report the detection of a pattern of features, extending across a broad latitude band from 25 to 60 degrees, that is superposed on the lower-latitude background glow, with peaks in emission that map along the planet's magnetic field lines to gaps in Saturn's rings. This pattern implies the transfer of charged species derived from water from the ring-plane to the ionosphere, an influx on a global scale, flooding between 30 to 43 per cent of the surface of Saturn's upper atmosphere. This ring 'rain' is important in modulating ionospheric emissions and suppressing electron densities.
C1 [O'Donoghue, J.; Stallard, T. S.; Melin, H.; Cowley, S. W. H.; Blake, J. S. D.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Jones, G. H.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Jones, G. H.; Miller, S.] Univ London Birkbeck Coll, Ctr Planetary Sci, London WC1E 6BT, England.
[Miller, S.] UCL, Dept Phys & Astron, Atmospher Phys Lab, London WC1E 6BT, England.
[Baines, K. H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP O'Donoghue, J (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
EM jod3@ion.le.ac.uk
RI Jones, Geraint/C-1682-2008;
OI Stallard, Tom/0000-0003-3990-670X; Jones, Geraint/0000-0002-5859-1136;
O'Donoghue, James/0000-0002-4218-1191
FU UK Science and Technology Facilities Council (STFC)
FX The data presented here were obtained at the W. M. Keck Observatory,
which is operated as a scientific partnership among the California
Institute of Technology, the University of California and NASA. The
observations were made to support the Cassini auroral campaign. Ring
profile data were provided by the Planetary Rings Node
website18. Discussions within the international team led by
T. S. S. on 'Comparative Jovian Aeronomy' have greatly benefited this
work; this was hosted by the International Space Science Institute
(ISSI). The UK Science and Technology Facilities Council (STFC)
supported this work through the PhD Studentship of J.O'D. and grant
support for T. S. S., H. M. and G.H.J.
NR 18
TC 16
Z9 16
U1 1
U2 16
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD APR 11
PY 2013
VL 496
IS 7444
BP 193
EP 195
DI 10.1038/nature12049
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 122VM
UT WOS:000317346300035
PM 23579676
ER
PT J
AU Bodnarik, JG
Burger, DM
Burger, A
Evans, LG
Parsons, AM
Schweitzer, JS
Starr, RD
Stassun, KG
AF Bodnarik, J. G.
Burger, D. M.
Burger, A.
Evans, L. G.
Parsons, A. M.
Schweitzer, J. S.
Starr, R. D.
Stassun, K. G.
TI Time-resolved neutron/gamma-ray data acquisition for in situ subsurface
planetary geochemistry
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS
SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT
LA English
DT Article
DE Elemental analysis; Pulsed neutron generator; Time-tagged data
acquisition; Optimized time-gating; Time-dependent neutron and gamma-ray
detection
ID GAMMA-RAY; ACTIVE NEUTRON; SPECTROMETER; SURFACE; MARS
AB The current gamma-ray/neutron instrumentation development effort at NASA Goddard Space Flight Center aims to extend the use of active pulsed neutron interrogation techniques to probe the subsurface elemental composition of planetary bodies in situ. Previous NASA planetary science missions, that used neutron and/or gamma-ray spectroscopy instruments, have relied on neutrons produced from galactic cosmic rays. One of the distinguishing features of this effort is the inclusion of a high intensity 14.1 MeV pulsed neutron generator synchronized with a custom data acquisition system to time each event relative to the pulse. With usually only one opportunity to collect data, it is difficult to set a priori time-gating windows to obtain the best possible results. Acquiring time-tagged, event-by-event data from nuclear induced reactions provides raw data sets containing channel/energy, and event time for each gamma ray or neutron detected. The resulting data set can be plotted as a function of time or energy using optimized analysis windows after the data are acquired. Time windows can now be chosen to produce energy spectra that yield the most statistically significant and accurate elemental composition results that can be derived from the complete data set. The advantages of post-processing gamma-ray time-tagged event-by-event data in experimental tests using our prototype instrument will be demonstrated. Published by Elsevier B.V.
C1 [Bodnarik, J. G.; Parsons, A. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bodnarik, J. G.; Stassun, K. G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA.
[Burger, D. M.] Vanderbilt Univ, Nashville, TN 37235 USA.
[Burger, A.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA.
[Evans, L. G.] Comp Sci Corp, Lanham, MD 20706 USA.
[Schweitzer, J. S.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA.
[Starr, R. D.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA.
RP Bodnarik, JG (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd,Code 691, Greenbelt, MD 20771 USA.
EM julia.g.bodnarik@nasa.gov; dan.burger@vanderbilt.edu; aburger@fisk.edu;
larry.g.evans@nasa.gov; ann.m.parsons@nasa.gov; schweitz@phys.uconn.edu;
richard.d.starr@nasa.gov; keivan.stassun@vanderbilt.edu
FU NASA; NSF; Tennessee Space
FX We would like to thank S.L. Floyd, M. Namkung, and S.F. Nowicki for
assistance with acquiring the data. We would like to thank R. Forsythe
for assistance with the data analysis. We would like to thank J.I.
Trombka and T.P. McClanahan for many useful discussions. We are indebted
to NASA, NSF, and the Tennessee Space Grant for partial support of this
research.
NR 20
TC 9
Z9 9
U1 1
U2 23
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-9002
J9 NUCL INSTRUM METH A
JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc.
Equip.
PD APR 11
PY 2013
VL 707
BP 135
EP 142
DI 10.1016/j.nima.2012.12.110
PG 8
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Nuclear; Physics, Particles & Fields
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 090CI
UT WOS:000314956100020
ER
PT J
AU Aartsen, MG
Abbasi, R
Abdou, Y
Ackermann, M
Adams, J
Aguilar, JA
Ahlers, M
Altmann, D
Auffenberg, J
Bai, X
Baker, M
Barwick, SW
Baum, V
Bay, R
Beattie, K
Beatty, JJ
Bechet, S
Tjus, JB
Becker, KH
Bell, M
Benabderrahmane, ML
BenZvi, S
Berdermann, J
Berghaus, P
Berley, D
Bernardini, E
Bernhard, A
Bertrand, D
Besson, DZ
Bindig, D
Bissok, M
Blaufuss, E
Blumenthal, J
Boersma, DJ
Bohaichuk, S
Bohm, C
Bose, D
Boser, S
Botner, O
Brayeur, L
Brown, AM
Bruijn, R
Brunner, J
Buitink, S
Carson, M
Casey, J
Casier, M
Chirkin, D
Christy, B
Clark, K
Clevermann, F
Cohen, S
Cowen, DF
Silva, AHC
Danninger, M
Daughhetee, J
Davis, JC
De Clercq, C
De Ridder, S
Desiati, P
de Vries-Uiterweerd, G
de With, M
DeYoung, T
Diaz-Velez, JC
Dreyer, J
Dunkman, M
Eagan, R
Eberhardt, B
Eisch, J
Ellsworth, RW
Engdegard, O
Euler, S
Evenson, PA
Fadiran, O
Fazely, AR
Fedynitch, A
Feintzeig, J
Feusels, T
Filimonov, K
Finley, C
Fischer-Wasels, T
Flis, S
Franckowiak, A
Franke, R
Frantzen, K
Fuchs, T
Gaisser, TK
Gallagher, J
Gerhardt, L
Gladstone, L
Glusenkamp, T
Goldschmidt, A
Golup, G
Goodman, JA
Gora, D
Grant, D
Gross, A
Gurtner, M
Ha, C
Ismail, AH
Hallgren, A
Halzen, F
Hanson, K
Heereman, D
Heimann, P
Heinen, D
Helbing, K
Hellauer, R
Hickford, S
Hill, GC
Hoffman, KD
Hoffmann, R
Homeier, A
Hoshina, K
Huelsnitz, W
Hulth, PO
Hultqvist, K
Hussain, S
Ishihara, A
Jacobi, E
Jacobsen, J
Japaridze, GS
Jero, K
Jlelati, O
Kaminsky, B
Kappes, A
Karg, T
Karle, A
Kelley, JL
Kiryluk, J
Kislat, F
Klas, J
Klein, SR
Kohne, JH
Kohnen, G
Kolanoski, H
Kopke, L
Kopper, C
Kopper, S
Koskinen, DJ
Kowalski, M
Krasberg, M
Kroll, G
Kunnen, J
Kurahashi, N
Kuwabara, T
Labare, M
Landsman, H
Larson, MJ
Lesiak-Bzdak, M
Leute, J
Lunemann, J
Madsen, J
Maruyama, R
Mase, K
Matis, HS
McNally, F
Meagher, K
Merck, M
Meszaros, P
Meures, T
Miarecki, S
Middell, E
Milke, N
Miller, J
Mohrmann, L
Montaruli, T
Morse, R
Nahnhauer, R
Naumann, U
Niederhausen, H
Nowicki, SC
Nygren, DR
Obertacke, A
Odrowski, S
Olivas, A
Olivo, M
O'Murchadha, A
Panknin, S
Paul, L
Pepper, JA
de los Heros, CP
Pfendner, C
Pieloth, D
Pirk, N
Posselt, J
Price, PB
Przybylski, GT
Radel, L
Rawlins, K
Redl, P
Resconi, E
Rhode, W
Ribordy, M
Richman, M
Riedel, B
Rodrigues, JP
Rott, C
Ruhe, T
Ruzybayev, B
Ryckbosch, D
Saba, SM
Salameh, T
Sander, HG
Santander, M
Sarkar, S
Schatto, K
Scheel, M
Scheriau, F
Schmidt, T
Schmitz, M
Schoenen, S
Schoneberg, S
Schonherr, L
Schonwald, A
Schukraft, A
Schulte, L
Schulz, O
Seckel, D
Seo, SH
Sestayo, Y
Seunarine, S
Sheremata, C
Smith, MWE
Soiron, M
Soldin, D
Spiczak, GM
Spiering, C
Stamatikos, M
Stanev, T
Stasik, A
Stezelberger, T
Stokstad, RG
Stossl, A
Strahler, EA
Strom, R
Sullivan, GW
Taavola, H
Taboada, I
Tamburro, A
Ter-Antonyan, S
Tilav, S
Toale, PA
Toscano, S
Usner, M
van der Drift, D
van Eijndhoven, N
Van Overloop, A
van Santen, J
Vehring, M
Voge, M
Vraeghe, M
Walck, C
Waldenmaier, T
Wallraff, M
Wasserman, R
Weaver, C
Wellons, M
Wendt, C
Westerhoff, S
Whitehorn, N
Wiebe, K
Wiebusch, CH
Williams, DR
Wissing, H
Wolf, M
Wood, TR
Woschnagg, K
Xu, C
Xu, DL
Xu, XW
Yanez, JP
Yodh, G
Yoshida, S
Zarzhitsky, P
Ziemann, J
Zierke, S
Zilles, A
Zoll, M
AF Aartsen, M. G.
Abbasi, R.
Abdou, Y.
Ackermann, M.
Adams, J.
Aguilar, J. A.
Ahlers, M.
Altmann, D.
Auffenberg, J.
Bai, X.
Baker, M.
Barwick, S. W.
Baum, V.
Bay, R.
Beattie, K.
Beatty, J. J.
Bechet, S.
Tjus, J. Becker
Becker, K. -H.
Bell, M.
Benabderrahmane, M. L.
BenZvi, S.
Berdermann, J.
Berghaus, P.
Berley, D.
Bernardini, E.
Bernhard, A.
Bertrand, D.
Besson, D. Z.
Bindig, D.
Bissok, M.
Blaufuss, E.
Blumenthal, J.
Boersma, D. J.
Bohaichuk, S.
Bohm, C.
Bose, D.
Boeser, S.
Botner, O.
Brayeur, L.
Brown, A. M.
Bruijn, R.
Brunner, J.
Buitink, S.
Carson, M.
Casey, J.
Casier, M.
Chirkin, D.
Christy, B.
Clark, K.
Clevermann, F.
Cohen, S.
Cowen, D. F.
Silva, A. H. Cruz
Danninger, M.
Daughhetee, J.
Davis, J. C.
De Clercq, C.
De Ridder, S.
Desiati, P.
de Vries-Uiterweerd, G.
de With, M.
DeYoung, T.
Diaz-Velez, J. C.
Dreyer, J.
Dunkman, M.
Eagan, R.
Eberhardt, B.
Eisch, J.
Ellsworth, R. W.
Engdegard, O.
Euler, S.
Evenson, P. A.
Fadiran, O.
Fazely, A. R.
Fedynitch, A.
Feintzeig, J.
Feusels, T.
Filimonov, K.
Finley, C.
Fischer-Wasels, T.
Flis, S.
Franckowiak, A.
Franke, R.
Frantzen, K.
Fuchs, T.
Gaisser, T. K.
Gallagher, J.
Gerhardt, L.
Gladstone, L.
Gluesenkamp, T.
Goldschmidt, A.
Golup, G.
Goodman, J. A.
Gora, D.
Grant, D.
Gross, A.
Gurtner, M.
Ha, C.
Ismail, A. Haj
Hallgren, A.
Halzen, F.
Hanson, K.
Heereman, D.
Heimann, P.
Heinen, D.
Helbing, K.
Hellauer, R.
Hickford, S.
Hill, G. C.
Hoffman, K. D.
Hoffmann, R.
Homeier, A.
Hoshina, K.
Huelsnitz, W.
Hulth, P. O.
Hultqvist, K.
Hussain, S.
Ishihara, A.
Jacobi, E.
Jacobsen, J.
Japaridze, G. S.
Jero, K.
Jlelati, O.
Kaminsky, B.
Kappes, A.
Karg, T.
Karle, A.
Kelley, J. L.
Kiryluk, J.
Kislat, F.
Klaes, J.
Klein, S. R.
Koehne, J. -H.
Kohnen, G.
Kolanoski, H.
Koepke, L.
Kopper, C.
Kopper, S.
Koskinen, D. J.
Kowalski, M.
Krasberg, M.
Kroll, G.
Kunnen, J.
Kurahashi, N.
Kuwabara, T.
Labare, M.
Landsman, H.
Larson, M. J.
Lesiak-Bzdak, M.
Leute, J.
Luenemann, J.
Madsen, J.
Maruyama, R.
Mase, K.
Matis, H. S.
McNally, F.
Meagher, K.
Merck, M.
Meszaros, P.
Meures, T.
Miarecki, S.
Middell, E.
Milke, N.
Miller, J.
Mohrmann, L.
Montaruli, T.
Morse, R.
Nahnhauer, R.
Naumann, U.
Niederhausen, H.
Nowicki, S. C.
Nygren, D. R.
Obertacke, A.
Odrowski, S.
Olivas, A.
Olivo, M.
O'Murchadha, A.
Panknin, S.
Paul, L.
Pepper, J. A.
de los Heros, C. Perez
Pfendner, C.
Pieloth, D.
Pirk, N.
Posselt, J.
Price, P. B.
Przybylski, G. T.
Raedel, L.
Rawlins, K.
Redl, P.
Resconi, E.
Rhode, W.
Ribordy, M.
Richman, M.
Riedel, B.
Rodrigues, J. P.
Rott, C.
Ruhe, T.
Ruzybayev, B.
Ryckbosch, D.
Saba, S. M.
Salameh, T.
Sander, H. -G.
Santander, M.
Sarkar, S.
Schatto, K.
Scheel, M.
Scheriau, F.
Schmidt, T.
Schmitz, M.
Schoenen, S.
Schoeneberg, S.
Schoenherr, L.
Schoenwald, A.
Schukraft, A.
Schulte, L.
Schulz, O.
Seckel, D.
Seo, S. H.
Sestayo, Y.
Seunarine, S.
Sheremata, C.
Smith, M. W. E.
Soiron, M.
Soldin, D.
Spiczak, G. M.
Spiering, C.
Stamatikos, M.
Stanev, T.
Stasik, A.
Stezelberger, T.
Stokstad, R. G.
Stoessl, A.
Strahler, E. A.
Stroem, R.
Sullivan, G. W.
Taavola, H.
Taboada, I.
Tamburro, A.
Ter-Antonyan, S.
Tilav, S.
Toale, P. A.
Toscano, S.
Usner, M.
van der Drift, D.
van Eijndhoven, N.
Van Overloop, A.
van Santen, J.
Vehring, M.
Voge, M.
Vraeghe, M.
Walck, C.
Waldenmaier, T.
Wallraff, M.
Wasserman, R.
Weaver, Ch.
Wellons, M.
Wendt, C.
Westerhoff, S.
Whitehorn, N.
Wiebe, K.
Wiebusch, C. H.
Williams, D. R.
Wissing, H.
Wolf, M.
Wood, T. R.
Woschnagg, K.
Xu, C.
Xu, D. L.
Xu, X. W.
Yanez, J. P.
Yodh, G.
Yoshida, S.
Zarzhitsky, P.
Ziemann, J.
Zierke, S.
Zilles, A.
Zoll, M.
CA IceCube Collaboration
TI Measurement of the Atmospheric nu(e) Flux in IceCube
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID NEUTRINO-INDUCED CASCADES; AMANDA; DETECTOR; DEEPCORE; SEARCH
AB We report the first measurement of the atmospheric electron neutrino flux in the energy range between approximately 80 GeV and 6 TeV, using data recorded during the first year of operation of IceCube's DeepCore low-energy extension. Techniques to identify neutrinos interacting within the DeepCore volume and veto muons originating outside the detector are demonstrated. A sample of 1029 events is observed in 281 days of data, of which 496 +/- 66(stat) +/- 88(syst) are estimated to be cascade events, including both electron neutrino and neutral current events. The rest of the sample includes residual backgrounds due to atmospheric muons and charged current interactions of atmospheric muon neutrinos. The flux of the atmospheric electron neutrinos is consistent with models of atmospheric neutrinos in this energy range. This constitutes the first observation of electron neutrinos and neutral current interactions in a very large volume neutrino telescope optimized for the TeV energy range. DOI: 10.1103/PhysRevLett.110.151105
C1 [Bissok, M.; Blumenthal, J.; Boersma, D. J.; Euler, S.; Heimann, P.; Heinen, D.; Paul, L.; Raedel, L.; Scheel, M.; Schoenen, S.; Schoenherr, L.; Schukraft, A.; Soiron, M.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.; Zierke, S.; Zilles, A.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany.
[Aartsen, M. G.; Hill, G. C.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia.
[Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA.
[Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA.
[Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Casey, J.; Daughhetee, J.; Taboada, I.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] Southern Univ, Dept Phys, Baton Rouge, LA 70813 USA.
[Bay, R.; Filimonov, K.; Gerhardt, L.; Ha, C.; Klein, S. R.; Miarecki, S.; Price, P. B.; van der Drift, D.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Beattie, K.; Gerhardt, L.; Goldschmidt, A.; Ha, C.; Klein, S. R.; Matis, H. S.; Miarecki, S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.; van der Drift, D.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Altmann, D.; de With, M.; Kappes, A.; Kolanoski, H.; Waldenmaier, T.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Tjus, J. Becker; Dreyer, J.; Fedynitch, A.; Olivo, M.; Saba, S. M.; Schoeneberg, S.] Ruhr Univ Bochum, Fac Phys & Astron, D-44780 Bochum, Germany.
[Boeser, S.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Panknin, S.; Schulte, L.; Stasik, A.; Usner, M.; Voge, M.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany.
[Bechet, S.; Bertrand, D.; Hanson, K.; Heereman, D.; Meures, T.; O'Murchadha, A.] Univ Libre Brussels, Fac Sci, B-1050 Brussels, Belgium.
[Bose, D.; Brayeur, L.; Buitink, S.; Casier, M.; De Clercq, C.; Golup, G.; Kunnen, J.; Labare, M.; Miller, J.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
[Ishihara, A.; Mase, K.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan.
[Adams, J.; Brown, A. M.; Hickford, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
[Berley, D.; Blaufuss, E.; Christy, B.; Ellsworth, R. W.; Goodman, J. A.; Hellauer, R.; Hoffman, K. D.; Huelsnitz, W.; Meagher, K.; Olivas, A.; Redl, P.; Richman, M.; Schmidt, T.; Sullivan, G. W.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Beatty, J. J.; Davis, J. C.; Pfendner, C.; Rott, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Beatty, J. J.; Davis, J. C.; Pfendner, C.; Rott, C.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Beatty, J. J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Clevermann, F.; Frantzen, K.; Fuchs, T.; Koehne, J. -H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.; Scheriau, F.; Schmitz, M.; Ziemann, J.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany.
[Bohaichuk, S.; Grant, D.; Nowicki, S. C.; Sheremata, C.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada.
[Aguilar, J. A.; Montaruli, T.] Univ Geneva, Dept Phys Nucl & Corpusculaire, CH-1211 Geneva, Switzerland.
[Abdou, Y.; Carson, M.; De Ridder, S.; de Vries-Uiterweerd, G.; Feusels, T.; Ismail, A. Haj; Jlelati, O.; Ryckbosch, D.; Van Overloop, A.; Vraeghe, M.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium.
[Barwick, S. W.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Bruijn, R.; Cohen, S.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland.
[Besson, D. Z.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Abbasi, R.; Ahlers, M.; Auffenberg, J.; Baker, M.; BenZvi, S.; Chirkin, D.; Desiati, P.; Diaz-Velez, J. C.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Jero, K.; Karle, A.; Kelley, J. L.; Koepke, L.; Kopper, C.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; McNally, F.; Merck, M.; Morse, R.; Riedel, B.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wellons, M.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Abbasi, R.; Ahlers, M.; Auffenberg, J.; Baker, M.; BenZvi, S.; Chirkin, D.; Desiati, P.; Diaz-Velez, J. C.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Halzen, F.; Hoshina, K.; Jacobsen, J.; Jero, K.; Karle, A.; Kelley, J. L.; Koepke, L.; Kopper, C.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; McNally, F.; Merck, M.; Morse, R.; Riedel, B.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wellons, M.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Wisconsin IceCube Particle Astrophys Ctr, Madison, WI 53706 USA.
[Baum, V.; Eberhardt, B.; Kroll, G.; Luenemann, J.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany.
[Kohnen, G.] Univ Mons, B-7000 Mons, Belgium.
[Bernhard, A.; Gross, A.; Leute, J.; Odrowski, S.; Resconi, E.; Schulz, O.; Sestayo, Y.] Tech Univ Munich, D-85748 Garching, Germany.
[Bai, X.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.; Xu, C.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Bai, X.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tamburro, A.; Tilav, S.; Xu, C.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England.
[Madsen, J.; Seunarine, S.; Spiczak, G. M.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA.
[Bohm, C.; Danninger, M.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Seo, S. H.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Bohm, C.; Danninger, M.; Finley, C.; Flis, S.; Hulth, P. O.; Hultqvist, K.; Seo, S. H.; Walck, C.; Wolf, M.; Zoll, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Kiryluk, J.; Lesiak-Bzdak, M.; Niederhausen, H.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Larson, M. J.; Pepper, J. A.; Toale, P. A.; Williams, D. R.; Xu, D. L.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Cowen, D. F.; Meszaros, P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Bell, M.; Clark, K.; Cowen, D. F.; DeYoung, T.; Dunkman, M.; Eagan, R.; Koskinen, D. J.; Meszaros, P.; Salameh, T.; Smith, M. W. E.; Wasserman, R.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Boersma, D. J.; Botner, O.; Engdegard, O.; Hallgren, A.; de los Heros, C. Perez; Stroem, R.; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
[Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Gurtner, M.; Helbing, K.; Hoffmann, R.; Klaes, J.; Kopper, S.; Naumann, U.; Obertacke, A.; Posselt, J.; Soldin, D.] Berg Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
[Ackermann, M.; Benabderrahmane, M. L.; Berdermann, J.; Berghaus, P.; Bernardini, E.; Brunner, J.; Silva, A. H. Cruz; Franke, R.; Gluesenkamp, T.; Gora, D.; Jacobi, E.; Kaminsky, B.; Karg, T.; Kislat, F.; Middell, E.; Mohrmann, L.; Nahnhauer, R.; Pirk, N.; Schoenwald, A.; Spiering, C.; Stoessl, A.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany.
[Bai, X.] South Dakota Sch Mines & Technol, Dept Phys, Rapid City, SD 57701 USA.
[Huelsnitz, W.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Montaruli, T.] Dipartimento Fis, Sez INFN, I-70126 Bari, Italy.
[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP DeYoung, T (reprint author), Penn State Univ, Dept Phys, 104 Davey Lab, University Pk, PA 16802 USA.
RI Tjus, Julia/G-8145-2012; Wiebusch, Christopher/G-6490-2012; Auffenberg,
Jan/D-3954-2014; Koskinen, David/G-3236-2014; Brunner,
Juergen/G-3540-2015; Aguilar Sanchez, Juan Antonio/H-4467-2015;
Maruyama, Reina/A-1064-2013; Sarkar, Subir/G-5978-2011; Beatty,
James/D-9310-2011;
OI Schukraft, Anne/0000-0002-9112-5479; Wiebusch,
Christopher/0000-0002-6418-3008; Auffenberg, Jan/0000-0002-1185-9094;
Koskinen, David/0000-0002-0514-5917; Brunner,
Juergen/0000-0002-5052-7236; Aguilar Sanchez, Juan
Antonio/0000-0003-2252-9514; Maruyama, Reina/0000-0003-2794-512X;
Sarkar, Subir/0000-0002-3542-858X; Beatty, James/0000-0003-0481-4952;
Ter-Antonyan, Samvel/0000-0002-5788-1369
FU U.S. National Science Foundation-Office of Polar Programs; U.S. National
Science Foundation-Physics Division; University of Wisconsin Alumni
Research Foundation; Grid Laboratory Of Wisconsin (GLOW) grid
infrastructure at the University of Wisconsin-Madison; Open Science Grid
(OSG) grid infrastructure; U.S. Department of Energy; National Energy
Research Scientific Computing Center; Louisiana Optical Network
Initiative (LONI) grid computing resources; National Science and
Engineering Research Council of Canada; Swedish Research Council;
Swedish Polar Research Secretariat; Swedish National Infrastructure for
Computing (SNIC); Knut and Alice Wallenberg Foundation, Sweden; German
Ministry for Education and Research (BMBF); Deutsche
Forschungsgemeinschaft (DFG); Helmholtz Alliance for Astroparticle
Physics (HAP); Research Department of Plasmas with Complex Interactions
(Bochum), Germany; Fund for Scientific Research (FNRS-FWO); FWO Odysseus
programme; Flanders Institute to encourage scientific and technological
research in industry (IWT); Belgian Federal Science Policy Office
(Belspo); University of Oxford, U.K.; Marsden Fund, New Zealand;
Australian Research Council; Japan Society for Promotion of Science
(JSPS); Swiss National Science Foundation (SNSF), Switzerland
FX We acknowledge the support from the following agencies: U.S. National
Science Foundation-Office of Polar Programs, U.S. National Science
Foundation-Physics Division, University of Wisconsin Alumni Research
Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure
at the University of Wisconsin-Madison, the Open Science Grid (OSG) grid
infrastructure; U.S. Department of Energy, and National Energy Research
Scientific Computing Center, the Louisiana Optical Network Initiative
(LONI) grid computing resources; National Science and Engineering
Research Council of Canada; Swedish Research Council, Swedish Polar
Research Secretariat, Swedish National Infrastructure for Computing
(SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German
Ministry for Education and Research (BMBF), Deutsche
Forschungsgemeinschaft (DFG), Helmholtz Alliance for Astroparticle
Physics (HAP), Research Department of Plasmas with Complex Interactions
(Bochum), Germany; Fund for Scientific Research (FNRS-FWO), FWO Odysseus
programme, Flanders Institute to encourage scientific and technological
research in industry (IWT), Belgian Federal Science Policy Office
(Belspo); University of Oxford, U.K.; Marsden Fund, New Zealand;
Australian Research Council; Japan Society for Promotion of Science
(JSPS); the Swiss National Science Foundation (SNSF), Switzerland.
NR 33
TC 38
Z9 38
U1 0
U2 13
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD APR 10
PY 2013
VL 110
IS 15
AR 151105
DI 10.1103/PhysRevLett.110.151105
PG 7
WC Physics, Multidisciplinary
SC Physics
GA 124JJ
UT WOS:000317459300004
PM 25167245
ER
PT J
AU Metaferia, B
Wei, JS
Song, YK
Evangelista, J
Aschenbach, K
Johansson, P
Wen, XY
Chen, QR
Lee, A
Hempel, H
Gheeya, JS
Getty, S
Gomez, R
Khan, J
AF Metaferia, Belhu
Wei, Jun S.
Song, Young K.
Evangelista, Jennifer
Aschenbach, Konrad
Johansson, Peter
Wen, Xinyu
Chen, Qingrong
Lee, Albert
Hempel, Heidi
Gheeya, Jinesh S.
Getty, Stephanie
Gomez, Romel
Khan, Javed
TI Development of Peptide Nucleic Acid Probes for Detection of the HER2
Oncogene
SO PLOS ONE
LA English
DT Article
ID BREAST-CANCER; HYBRIDIZATION; PNA; DNA; IMMOBILIZATION; RESISTANCE;
STABILITY; PNA/DNA; CELLS; RNA
AB Peptide nucleic acids (PNAs) have gained much interest as molecular recognition tools in biology, medicine and chemistry. This is due to high hybridization efficiency to complimentary oligonucleotides and stability of the duplexes with RNA or DNA. We have synthesized 15/16-mer PNA probes to detect the HER2 mRNA. The performance of these probes to detect the HER2 target was evaluated by fluorescence imaging and fluorescence bead assays. The PNA probes have sufficiently discriminated between the wild type HER2 target and the mutant target with single base mismatches. Furthermore, the probes exhibited excellent linear concentration dependence between 0.4 to 400 fmol for the target gene. The results demonstrate potential application of PNAs as diagnostic probes with high specificity for quantitative measurements of amplifications or over-expressions of oncogenes.
C1 [Metaferia, Belhu; Wei, Jun S.; Song, Young K.; Johansson, Peter; Wen, Xinyu; Chen, Qingrong; Lee, Albert; Hempel, Heidi; Gheeya, Jinesh S.; Khan, Javed] NCI, Pediat Oncol Branch, NIH, Bethesda, MD 20892 USA.
[Wen, Xinyu] NCI, Adv Biomed Comp Ctr, SAIC Frederick Inc, Frederick, MD 21701 USA.
[Evangelista, Jennifer; Aschenbach, Konrad; Gomez, Romel] Univ Maryland, Dept Elect & Comp Engn, College Pk, MD 20742 USA.
[Getty, Stephanie] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Khan, J (reprint author), NCI, Pediat Oncol Branch, NIH, Bethesda, MD 20892 USA.
EM khanjav@mail.nih.gov
RI Getty, Stephanie/D-7037-2012; Khan, Javed/P-9157-2014; Johansson,
Peter/K-1053-2014;
OI Khan, Javed/0000-0002-5858-0488; Johansson, Peter/0000-0001-7015-5452;
Gheeya, Jinesh/0000-0002-5246-6262
FU National Institutes of Health, National Cancer Institute, Center for
Cancer Research
FX This study was supported by the Intramural Research Program of the
National Institutes of Health, National Cancer Institute, Center for
Cancer Research. The funders had no role in study design, data
collection and analysis, decision to publish, or preparation of the
manuscript.
NR 31
TC 1
Z9 1
U1 0
U2 31
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 APR 10
PY 2013
VL 8
IS 4
AR e58870
DI 10.1371/journal.pone.0058870
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 123IQ
UT WOS:000317382000002
PM 23593123
ER
PT J
AU Follette, KB
Tamura, M
Hashimoto, J
Whitney, B
Grady, C
Close, L
Andrews, SM
Kwon, J
Wisniewski, J
Brandt, TD
Mayama, S
Kandori, R
Dong, RB
Abe, L
Brandner, W
Carson, J
Currie, T
Egner, SE
Feldt, M
Goto, M
Guyon, O
Hayano, Y
Hayashi, M
Hayashi, S
Henning, T
Hodapp, K
Ishii, M
Iye, M
Janson, M
Knapp, GR
Kudo, T
Kusakabe, N
Kuzuhara, M
McElwain, MW
Matsuo, T
Miyama, S
Morino, JI
Moro-Martin, A
Nishimura, T
Pyo, TS
Serabyn, E
Suto, H
Suzuki, R
Takami, M
Takato, N
Terada, H
Thalmann, C
Tomono, D
Turner, EL
Watanabe, M
Yamada, T
Takami, H
Usuda, T
AF Follette, Katherine B.
Tamura, Motohide
Hashimoto, Jun
Whitney, Barbara
Grady, Carol
Close, Laird
Andrews, Sean M.
Kwon, Jungmi
Wisniewski, John
Brandt, Timothy D.
Mayama, Satoshi
Kandori, Ryo
Dong, Ruobing
Abe, Lyu
Brandner, Wolfgang
Carson, Joseph
Currie, Thayne
Egner, Sebastian E.
Feldt, Markus
Goto, Miwa
Guyon, Olivier
Hayano, Yutaka
Hayashi, Masahiko
Hayashi, Saeko
Henning, Thomas
Hodapp, Klaus
Ishii, Miki
Iye, Masanori
Janson, Markus
Knapp, Gillian R.
Kudo, Tomoyuki
Kusakabe, Nobuhiko
Kuzuhara, Masayuki
McElwain, Michael W.
Matsuo, Taro
Miyama, Shoken
Morino, Jun-Ichi
Moro-Martin, Amaya
Nishimura, Tetsuo
Pyo, Tae-Soo
Serabyn, Eugene
Suto, Hiroshi
Suzuki, Ryuji
Takami, Michihiro
Takato, Naruhisa
Terada, Hiroshi
Thalmann, Christian
Tomono, Daigo
Turner, Edwin L.
Watanabe, Makoto
Yamada, Toru
Takami, Hideki
Usuda, Tomonori
TI MAPPING H-BAND SCATTERED LIGHT EMISSION IN THE MYSTERIOUS SR21
TRANSITIONAL DISK
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; protoplanetary disks; stars: individual (SR21);
stars: pre-main sequence; techniques: polarimetric
ID MAIN-SEQUENCE STARS; 2-DIMENSIONAL RADIATIVE-TRANSFER; YOUNG STELLAR
OBJECTS; PROTOPLANETARY DISKS; CIRCUMSTELLAR DUST; PROTOSTELLAR
ENVELOPES; SIZE DISTRIBUTION; MOLECULAR CLOUD; FORMING REGION; GIANT
PLANETS
AB We present the first near infrared (NIR) spatially resolved images of the circumstellar transitional disk around SR21. These images were obtained with the Subaru HiCIAO camera, adaptive optics, and the polarized differential imaging technique. We resolve the disk in scattered light at H-band for stellocentric 0 ''.1 <= r <= 0 ''.6 (12 less than or similar to r less than or similar to 75 AU). We compare our results with previously published spatially resolved 880 mu m continuum Submillimeter Array images that show an inner r less than or similar to 36 AU cavity in SR21. Radiative transfer models reveal that the large disk depletion factor invoked to explain SR21's sub-mm cavity cannot be "universal" for all grain sizes. Even significantly more moderate depletions (delta = 0.1, 0.01 relative to an undepleted disk) than those that reproduce the sub-mm cavity (delta similar to 10(-6)) are inconsistent with our H-band images when they are assumed to carry over to small grains, suggesting that surface grains scattering in the NIR either survive or are generated by whatever mechanism is clearing the disk midplane. In fact, the radial polarized intensity profile of our H-band observations is smooth and steeply inwardly-increasing (r(-3)), with no evidence of a break at the 36 AU sub-mm cavity wall. We hypothesize that this profile is dominated by an optically thin disk envelope or atmosphere component. We also discuss the compatibility of our data with the previously postulated existence of a sub-stellar companion to SR21 at r similar to 10-20 AU, and find that we can neither exclude nor verify this scenario. This study demonstrates the power of multiwavelength imaging of transitional disks to inform modeling efforts, including the debate over precisely what physical mechanism is responsible for clearing these disks of their large midplane grains.
C1 [Follette, Katherine B.; Close, Laird] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Tamura, Motohide; Hashimoto, Jun; Kwon, Jungmi; Kandori, Ryo; Iye, Masanori; Kusakabe, Nobuhiko; Kuzuhara, Masayuki; Morino, Jun-Ichi; Suto, Hiroshi] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Tamura, Motohide; Kwon, Jungmi] Grad Univ Adv Studies Sokendai, Dept Astron Sci, Tokyo 1818588, Japan.
[Whitney, Barbara] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Grady, Carol] Eureka Sci, Oakland, CA 96002 USA.
[Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Wisniewski, John] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA.
[Brandt, Timothy D.; Dong, Ruobing; Janson, Markus; Knapp, Gillian R.; Turner, Edwin L.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Mayama, Satoshi] Grad Univ Adv Studies Sokendai, Ctr Promot Integrated Sci, Hayama, Kanagawa 2400193, Japan.
[Abe, Lyu] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR7293, F-06300 Nice, France.
[Brandner, Wolfgang; Feldt, Markus; Henning, Thomas] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Carson, Joseph] Coll Charleston, Dept Phys & Astron, Charleston, SC 29424 USA.
[Currie, Thayne] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Egner, Sebastian E.; Guyon, Olivier; Hayano, Yutaka; Hayashi, Saeko; Ishii, Miki; Kudo, Tomoyuki; Nishimura, Tetsuo; Pyo, Tae-Soo; Takato, Naruhisa; Terada, Hiroshi; Tomono, Daigo; Takami, Hideki; Usuda, Tomonori] Subaru Telescope, Hilo, HI 96720 USA.
[Goto, Miwa] Univ Munich, Univ Sternwarte Munchen, D-81679 Munich, Germany.
[Hayashi, Masahiko] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
[Hodapp, Klaus] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
[McElwain, Michael W.] NASA, Goddard Space Flight Ctr, ExoPlanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Matsuo, Taro] Kyoto Univ, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake, Kyoto 6068502, Japan.
[Miyama, Shoken] Hiroshima Univ, Off President, Higashihiroshima 7398511, Japan.
[Moro-Martin, Amaya] Inst Nacl Tecn Aeroespacial, CAB INTA CSIC, Dept Astrofis, E-28850 Madrid, Spain.
[Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Suzuki, Ryuji] TMT Observ Corp, Pasadena, CA 91105 USA.
[Takami, Michihiro] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
[Thalmann, Christian] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Turner, Edwin L.] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778568, Japan.
[Watanabe, Makoto] Hokkaido Univ, Dept Cosmosci, Sapporo, Hokkaido 0600810, Japan.
[Yamada, Toru] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan.
RP Follette, KB (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA.
EM kfollette@as.arizona.edu
RI MIYAMA, Shoken/A-3598-2015; Watanabe, Makoto/E-3667-2016
OI Watanabe, Makoto/0000-0002-3656-4081
FU National Science Foundation; MEXT; [NSF-AST 1009314]; [NSF-AST
1009203]
FX We gratefully acknowledge funding from the National Science Foundation
East Asian and Pacific Summer Institute Fellowship (Follette), NSF-AST
1009314 (Wisniewski) and NSF-AST 1009203 (Carson). We are grateful to
Collette Salyk, Glenn Schneider, Dean Hines, Don McCarthy, Vanessa
Bailey, and Johanna Teske for their insightful comments. The authors
wish to recognize and acknowledge the very significant cultural role and
reverence that the summit of Mauna Kea has always had within the
indigenous Hawaiian community. We are most fortunate to have the
opportunity to conduct observations from this mountain. Part of this
work was carried out at JPL. This work is partly supported by a
Grant-in-Aid for Science Research in a Priority Area from MEXT.
NR 77
TC 42
Z9 42
U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2013
VL 767
IS 1
AR 10
DI 10.1088/0004-637X/767/1/10
PG 26
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 117IT
UT WOS:000316947500010
ER
PT J
AU Guyon, O
Eisner, JA
Angel, R
Woolf, NJ
Bendek, EA
Milster, TD
Ammons, SM
Shao, M
Shaklan, S
Levine, M
Nemati, B
Martinache, F
Pitman, J
Woodruff, RA
Belikov, R
AF Guyon, Olivier
Eisner, Josh A.
Angel, Roger
Woolf, Neville J.
Bendek, Eduardo A.
Milster, Thomas D.
Ammons, S. Mark
Shao, Michael
Shaklan, Stuart
Levine, Marie
Nemati, Bijan
Martinache, Frantz
Pitman, Joe
Woodruff, Robert A.
Belikov, Ruslan
TI SIMULTANEOUS EXOPLANET CHARACTERIZATION AND DEEP WIDE-FIELD IMAGING WITH
A DIFFRACTIVE PUPIL TELESCOPE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrometry; planets and satellites: detection; techniques: high angular
resolution; telescopes
ID PRECISION ASTROMETRY; RADIAL-VELOCITY; PHOTOMETRY; PLANETS; SYSTEMS
AB High-precision astrometry can identify exoplanets and measure their orbits and masses while coronagraphic imaging enables detailed characterization of their physical properties and atmospheric compositions through spectroscopy. In a previous paper, we showed that a diffractive pupil telescope (DPT) in space can enable sub-mu as accuracy astrometric measurements from wide-field images by creating faint but sharp diffraction spikes around the bright target star. The DPT allows simultaneous astrometric measurement and coronagraphic imaging, and we discuss and quantify in this paper the scientific benefits of this combination for exoplanet science investigations: identification of exoplanets with increased sensitivity and robustness, and ability to measure planetary masses to high accuracy. We show how using both measurements to identify planets and measure their masses offers greater sensitivity and provides more reliable measurements than possible with separate missions, and therefore results in a large gain in mission efficiency. The combined measurements reliably identify potentially habitable planets in multiple systems with a few observations, while astrometry or imaging alone would require many measurements over a long time baseline. In addition, the combined measurement allows direct determination of stellar masses to percent-level accuracy, using planets as test particles. We also show that the DPT maintains the full sensitivity of the telescope for deep wide-field imaging, and is therefore compatible with simultaneous scientific observations unrelated to exoplanets. We conclude that astrometry, coronagraphy, and deep wide-field imaging can be performed simultaneously on a single telescope without significant negative impact on the performance of any of the three techniques.
C1 [Guyon, Olivier; Eisner, Josh A.; Angel, Roger; Woolf, Neville J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Guyon, Olivier; Martinache, Frantz] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Bendek, Eduardo A.; Milster, Thomas D.] Univ Arizona, Coll Opt Sci, Tucson, AZ 85721 USA.
[Ammons, S. Mark] Lawrence Livermore Natl Lab, Phys Div L210, Livermore, CA 94550 USA.
[Shao, Michael; Shaklan, Stuart; Levine, Marie; Nemati, Bijan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Pitman, Joe] Explorat Sci, Pine, CO 80470 USA.
[Woodruff, Robert A.] Lockheed Martin, Boulder, CO 80304 USA.
[Belikov, Ruslan] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Guyon, O (reprint author), Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
EM guyon@naoj.org
FU NASA Astronomy and Physics Research and Analysis (APRA) program; State
of Arizona Technology Research Initiative Fund (TRIF); NASA through
Hubble Fellowship grant by the Space Telescope Science Institute
[HST-HF-51250.01-A]; NASA [NAS 5-26555]
FX This work is funded by the NASA Astronomy and Physics Research and
Analysis (APRA) program and the State of Arizona Technology Research
Initiative Fund (TRIF). Support for this work was also provided by NASA
through Hubble Fellowship grant HST-HF-51250.01-A awarded to S. Mark
Ammons by the Space Telescope Science Institute, which is operated by
the Association of Universities for Research in Astronomy, Inc., for
NASA, under contract NAS 5-26555.
NR 19
TC 4
Z9 4
U1 1
U2 9
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2013
VL 767
IS 1
AR 11
DI 10.1088/0004-637X/767/1/11
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 117IT
UT WOS:000316947500011
ER
PT J
AU Izidoro, A
Torres, KD
Winter, OC
Haghighipour, N
AF Izidoro, A.
de Souza Torres, K.
Winter, O. C.
Haghighipour, N.
TI A COMPOUND MODEL FOR THE ORIGIN OF EARTH'S WATER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrobiology; Earth; planets and satellites: composition; planets and
satellites: formation
ID TERRESTRIAL PLANET FORMATION; INNER SOLAR-SYSTEM; HIGH-RESOLUTION
SIMULATIONS; GIANT PLANETS; DEUTERIUM ENRICHMENT; PROTOPLANETARY DISKS;
DEUTERATED WATER; HABITABLE PLANET; FORMING REGION; UPPER-MANTLE
AB One of the most important subjects of debate in the formation of the solar system is the origin of Earth's water. Comets have long been considered as the most likely source of the delivery of water to Earth. However, elemental and isotopic arguments suggest a very small contribution from these objects. Other sources have also been proposed, among which local adsorption of water vapor onto dust grains in the primordial nebula and delivery through planetesimals and planetary embryos have become more prominent. However, no sole source of water provides a satisfactory explanation for Earth's water as a whole. In view of that, using numerical simulations, we have developed a compound model incorporating both the principal endogenous and exogenous theories, and investigating their implications for terrestrial planet formation and water delivery. Comets are also considered in the final analysis, as it is likely that at least some of Earth's water has cometary origin. We analyze our results comparing two different water distribution models, and complement our study using the D/H ratio, finding possible relative contributions from each source and focusing on planets formed in the habitable zone. We find that the compound model plays an important role by showing greater advantage in the amount and time of water delivery in Earth-like planets.
C1 [Izidoro, A.; Winter, O. C.] Univ Estadual Paulista, UNESP, Grp Dinam Orbital & Planetol, BR-12516410 Sao Paulo, Brazil.
[Haghighipour, N.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA.
[Haghighipour, N.] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA.
RP Izidoro, A (reprint author), Univ Estadual Paulista, UNESP, Grp Dinam Orbital & Planetol, BR-12516410 Sao Paulo, Brazil.
EM ocwinter@pq.cnpq.br
FU CAPES (Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior);
CNPq (Conselho Nacional de Desenvolvimento Cientifico e Tecnologico);
FAPESP (Fundacao de Amparo a Pesquisa do Estado de Sao Paulo); NASA
Astrobiology Institute at the Institute for Astronomy, University of
Hawaii [NNA09DA77A]; NASA EXOB grant [NNX09AN05G]
FX We thank the anonymous referee for constructive comments that greatly
improved our manuscript. This work was funded by CAPES (Coordenacao de
Aperfeicoamento de Pessoal de Nivel Superior), CNPq (Conselho Nacional
de Desenvolvimento Cientifico e Tecnologico), and FAPESP (Fundacao de
Amparo a Pesquisa do Estado de Sao Paulo). N.H. acknowledges support
from the NASA Astrobiology Institute under Cooperative Agreement
NNA09DA77A at the Institute for Astronomy, University of Hawaii, and
NASA EXOB grant NNX09AN05G.
NR 81
TC 20
Z9 20
U1 6
U2 50
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2013
VL 767
IS 1
AR 54
DI 10.1088/0004-637X/767/1/54
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 117IT
UT WOS:000316947500054
ER
PT J
AU Karoff, C
Campante, TL
Ballot, J
Kallinger, T
Gruberbauer, M
Garcia, RA
Caldwell, DA
Christiansen, JL
Kinemuchi, K
AF Karoff, C.
Campante, T. L.
Ballot, J.
Kallinger, T.
Gruberbauer, M.
Garcia, R. A.
Caldwell, D. A.
Christiansen, J. L.
Kinemuchi, K.
TI OBSERVATIONS OF INTENSITY FLUCTUATIONS ATTRIBUTED TO GRANULATION AND
FACULAE ON SUN-LIKE STARS FROM THE KEPLER MISSION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: activity; stars: individual (KIC 6603624, KIC 6933899, KIC
11244118); stars: oscillations; stars: solar-type
ID SOLAR-TYPE STARS; STELLAR OSCILLATIONS; GLOBAL OSCILLATIONS;
MAIN-SEQUENCE; RED GIANTS; P-MODES; FREQUENCY; SPECTRUM;
ASTEROSEISMOLOGY; PERIODICITIES
AB Sun-like stars show intensity fluctuations on a number of timescales due to various physical phenomena on their surfaces. These phenomena can convincingly be studied in the frequency spectra of these stars-while the strongest signatures usually originate from spots, granulation, and p-mode oscillations, it has also been suggested that the frequency spectrum of the Sun contains a signature of faculae. We have analyzed three stars observed for 13 months in short cadence (58.84 s sampling) by the Kepler mission. The frequency spectra of all three stars, as for the Sun, contain signatures that we can attribute to granulation, faculae, and p-mode oscillations. The temporal variability of the signatures attributed to granulation, faculae, and p-mode oscillations was analyzed and the analysis indicates a periodic variability in the granulation and faculae signatures-comparable to what is seen in the Sun.
C1 [Karoff, C.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark.
[Campante, T. L.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Campante, T. L.] Univ Porto, Fac Ciencias, P-4150762 Oporto, Portugal.
[Campante, T. L.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Ballot, J.] CNRS, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France.
[Ballot, J.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Kallinger, T.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Kallinger, T.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Gruberbauer, M.] St Marys Univ, Dept Phys & Astron, Inst Computat Astrophys, Halifax, NS B3H 3C3, Canada.
[Garcia, R. A.] Univ Paris Diderot, IRFU, Ctr Saclay, Lab AIM,CEA,DSM,CNRS,SAp, F-91191 Gif Sur Yvette, France.
[Caldwell, D. A.; Christiansen, J. L.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Kinemuchi, K.] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
RP Karoff, C (reprint author), Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Ny Munkegade 120, DK-8000 Aarhus C, Denmark.
EM karoff@phys.au.dk
RI Caldwell, Douglas/L-7911-2014; Karoff, Christoffer/L-1007-2013;
OI Caldwell, Douglas/0000-0003-1963-9616; Karoff,
Christoffer/0000-0003-2009-7965; Kallinger, Thomas/0000-0003-3627-2561;
Garcia, Rafael/0000-0002-8854-3776
FU NASAs Science Mission Directorate; Carlsberg foundation; FCT/MCTES,
Portugal; UK Science and Technology Facilities Council (STFC);
FWO-Flanders [O6260 - G.0728.11]; Danish National Research Foundation
[DNRF106]; ASTERISK project (ASTERoseismic Investigations with SONG and
Kepler); European Research Council [267864]; [PTDC/CTE-AST/098754/2008]
FX We thank the referee for thoughtful comments, which significantly
improved the paper. Funding for this Discovery mission is provided by
NASAs Science Mission Directorate. The authors wish to thank the entire
Kepler team, without whom these results would not be possible. C. K.
acknowledged support from the Carlsberg foundation. T. L. C.
acknowledges financial support from project PTDC/CTE-AST/098754/2008
funded by FCT/MCTES, Portugal. T. L. C. also acknowledges the support of
the UK Science and Technology Facilities Council (STFC). T. K. is
supported by the FWO-Flanders under project O6260 - G.0728.11. Funding
for the Stellar Astrophysics Centre is provided by The Danish National
Research Foundation (grant agreement No.: DNRF106). The research is
supported by the ASTERISK project (ASTERoseismic Investigations with
SONG and Kepler) funded by the European Research Council (grant
agreement No.: 267864).
NR 58
TC 18
Z9 18
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2013
VL 767
IS 1
AR 34
DI 10.1088/0004-637X/767/1/34
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 117IT
UT WOS:000316947500034
ER
PT J
AU Kataria, T
Showman, AP
Lewis, NK
Fortney, JJ
Marley, MS
Freedman, RS
AF Kataria, T.
Showman, A. P.
Lewis, N. K.
Fortney, J. J.
Marley, M. S.
Freedman, R. S.
TI THREE-DIMENSIONAL ATMOSPHERIC CIRCULATION OF HOT JUPITERS ON HIGHLY
ECCENTRIC ORBITS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE atmospheric effects; methods: numerical; planets and satellites:
atmospheres; planets and satellites: general
ID TIDALLY LOCKED EXOPLANETS; HD 189733B; EXTRASOLAR PLANET; HYDRODYNAMIC
SIMULATIONS; RADIATIVE-TRANSFER; EMISSION-SPECTRUM; GIANT PLANETS;
MODEL; DYNAMICS; 209458B
AB Of the over 800 exoplanets detected to date, over half are on non-circular orbits, with eccentricities as high as 0.93. Such orbits lead to time-variable stellar heating, which has major implications for the planet's atmospheric dynamical regime. However, little is known about the fundamental dynamical regime of such planetary atmospheres, and how it may influence the observations of these planets. Therefore, we present a systematic study of hot Jupiters on highly eccentric orbits using the SPARC/MITgcm, a model which couples a three-dimensional general circulation model (the MITgcm) with a plane-parallel, two-stream, non-gray radiative transfer model. In our study, we vary the eccentricity and orbit-average stellar flux over a wide range. We demonstrate that the eccentric hot Jupiter regime is qualitatively similar to that of planets on circular orbits; the planets possess a superrotating equatorial jet and exhibit large day-night temperature variations. As in Showman & Polvani, we show that the day-night heating variations induce momentum fluxes equatorward to maintain the superrotating jet throughout its orbit. We find that as the eccentricity and/or stellar flux is increased (corresponding to shorter orbital periods), the superrotating jet strengthens and narrows, due to a smaller Rossby deformation radius. For a select number of model integrations, we generate full-orbit light curves and find that the timing of transit and secondary eclipse viewed from Earth with respect to periapse and apoapse can greatly affect what we see in infrared (IR) light curves; the peak in IR flux can lead or lag secondary eclipse depending on the geometry. For those planets that have large temperature differences from dayside to nightside and rapid rotation rates, we find that the light curves can exhibit "ringing" as the planet's hottest region rotates in and out of view from Earth. These results can be used to explain future observations of eccentric transiting exoplanets.
C1 [Kataria, T.; Showman, A. P.; Lewis, N. K.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Kataria, T.; Showman, A. P.; Lewis, N. K.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Lewis, N. K.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Fortney, J. J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Marley, M. S.; Freedman, R. S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Freedman, R. S.] SETI Inst, Mountain View, CA 94043 USA.
RP Kataria, T (reprint author), Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
EM tkataria@lpl.arizona.edu
RI Marley, Mark/I-4704-2013;
OI Fortney, Jonathan/0000-0002-9843-4354; Marley, Mark/0000-0002-5251-2943
FU NASA Origins and Planetary Atmospheres; NASA High-End Computing (HEC)
Program through the NASA Advanced Supercomputing (NAS) Division at Ames
Research Center
FX This work was supported by NASA Origins and Planetary Atmospheres grants
to APS. T.K. also acknowledges support from the Harriet P. Jenkins
Pre-Doctoral Fellowship Program (JPFP). 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. The
authors thank the anonymous referee for their helpful comments and
suggestions.
NR 47
TC 30
Z9 30
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2013
VL 767
IS 1
AR 76
DI 10.1088/0004-637X/767/1/76
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 117IT
UT WOS:000316947500076
ER
PT J
AU Roettenbacher, RM
Monnier, JD
Harmon, RO
Barclay, T
Still, M
AF Roettenbacher, Rachael M.
Monnier, John D.
Harmon, Robert O.
Barclay, Thomas
Still, Martin
TI IMAGING STARSPOT EVOLUTION ON KEPLER TARGET KIC 5110407 USING
LIGHT-CURVE INVERSION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: activity; stars: imaging; stars: variables: general
ID BINARY II-PEGASI; CLUSTER NGC 6819; DIFFERENTIAL ROTATION; SPACE
TELESCOPE; STELLAR ACTIVITY; SPOT ACTIVITY; ACTIVE LONGITUDES;
SIGMA-GEMINORUM; INPUT CATALOG; MASS STARS
AB The Kepler target KIC 5110407, a K-type star, shows strong quasi-periodic light curve fluctuations likely arising from the formation and decay of spots on the stellar surface rotating with a period of 3.4693 days. Using an established light-curve inversion algorithm, we study the evolution of the surface features based on Kepler space telescope light curves over a period of two years (with a gap of .25 years). At virtually all epochs, we detect at least one large spot group on the surface causing a 1%-10% flux modulation in the Kepler passband. By identifying and tracking spot groups over a range of inferred latitudes, we measured the surface differential rotation to be much smaller than that found for the Sun. We also searched for a correlation between the 17 stellar flares that occurred during our observations and the orientation of the dominant surface spot at the time of each flare. No statistically significant correlation was found except perhaps for the very brightest flares, suggesting that most flares are associated with regions devoid of spots or spots too small to be clearly discerned using our reconstruction technique. While we may see hints of long-term changes in the spot characteristics and flare statistics within our current data set, a longer baseline of observation will be needed to detect the existence of a magnetic cycle in KIC 5110407.
C1 [Roettenbacher, Rachael M.; Monnier, John D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Harmon, Robert O.] Ohio Wesleyan Univ, Dept Phys & Astron, Delaware, OH 43015 USA.
[Barclay, Thomas; Still, Martin] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Barclay, Thomas; Still, Martin] Bay Area Environm Res Inst, Sonoma, CA 95476 USA.
RP Roettenbacher, RM (reprint author), Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
EM rmroett@umich.edu
FU NASA Science Mission Directorate; NASA Harriett G. Jenkins Pre-doctoral
Fellowship Program; Cycle 4 Kepler Guest Observer Program (NASA)
[NNX13AC17G]
FX We gratefully acknowledge the helpful and constructive comments from our
referee, Klaus Strassmeier. This paper includes data collected by the
Kepler mission. Funding for the Kepler mission is provided by the NASA
Science Mission Directorate. R. M. R. acknowledges support through the
NASA Harriett G. Jenkins Pre-doctoral Fellowship Program. Additional
support for this project was provided through the Cycle 4 Kepler Guest
Observer Program (NASA grant NNX13AC17G).
NR 47
TC 14
Z9 14
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2013
VL 767
IS 1
AR 60
DI 10.1088/0004-637X/767/1/60
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 117IT
UT WOS:000316947500060
ER
PT J
AU Sehgal, N
Addison, G
Battaglia, N
Battistelli, ES
Bond, JR
Das, S
Devlin, MJ
Dunkley, J
Dunner, R
Gralla, M
Hajian, A
Halpern, M
Hasselfield, M
Hilton, M
Hincks, AD
Hlozek, R
Hughes, JP
Kosowsky, A
Lin, YT
Louis, T
Marriage, TA
Marsden, D
Menanteau, F
Moodley, K
Niemack, MD
Page, LA
Partridge, B
Reese, ED
Sherwin, BD
Sievers, J
Sifon, C
Spergel, DN
Staggs, ST
Swetz, DS
Switzer, ER
Wollack, E
AF Sehgal, Neelima
Addison, Graeme
Battaglia, Nick
Battistelli, Elia S.
Bond, J. Richard
Das, Sudeep
Devlin, Mark J.
Dunkley, Joanna
Duenner, Rolando
Gralla, Megan
Hajian, Amir
Halpern, Mark
Hasselfield, Matthew
Hilton, Matt
Hincks, Adam D.
Hlozek, Renee
Hughes, John P.
Kosowsky, Arthur
Lin, Yen-Ting
Louis, Thibaut
Marriage, Tobias A.
Marsden, Danica
Menanteau, Felipe
Moodley, Kavilan
Niemack, Michael D.
Page, Lyman A.
Partridge, Bruce
Reese, Erik D.
Sherwin, Blake D.
Sievers, Jon
Sifon, Cristobal
Spergel, David N.
Staggs, Suzanne T.
Swetz, Daniel S.
Switzer, Eric R.
Wollack, Ed
TI THE ATACAMA COSMOLOGY TELESCOPE: RELATION BETWEEN GALAXY CLUSTER OPTICAL
RICHNESS AND SUNYAEV-ZEL'DOVICH EFFECT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; galaxies: clusters: general; galaxies:
clusters: intracluster medium
ID SOUTH-POLE TELESCOPE; DIGITAL SKY SURVEY; BACKGROUND POWER SPECTRUM;
SCALING RELATIONS; MAXBCG CLUSTERS; RADIO-SOURCES; 148 GHZ; CONSTRAINTS;
CATALOG; PLANCK
AB We present the measured Sunyaev-Zel'dovich (SZ) flux from 474 optically selected MaxBCG clusters that fall within the Atacama Cosmology Telescope (ACT) Equatorial survey region. The ACT Equatorial region used in this analysis covers 510 deg(2) and overlaps Stripe 82 of the Sloan Digital Sky Survey. We also present the measured SZ flux stacked on 52 X-ray-selected MCXC clusters that fall within the ACT Equatorial region and an ACT Southern survey region covering 455 deg(2). We find that the measured SZ flux from the X-ray-selected clusters is consistent with expectations. However, we find that the measured SZ flux from the optically selected clusters is both significantly lower than expectations and lower than the recovered SZ flux measured by the Planck satellite. Since we find a lower recovered SZ signal than Planck, we investigate the possibility that there is a significant offset between the optically selected brightest cluster galaxies (BCGs) and the SZ centers, to which ACT is more sensitive due to its finer resolution. Such offsets can arise due to either an intrinsic physical separation between the BCG and the center of the gas concentration or from misidentification of the cluster BCG. We find that the entire discrepancy for both ACT and Planck can be explained by assuming that the BCGs are offset from the SZ maxima with a uniform random distribution between 0 and 1.5 Mpc. Such large offsets between gas peaks and BCGs for optically selected cluster samples seem unlikely given that we find the physical separation between BCGs and X-ray peaks for an X-ray-selected subsample of MaxBCG clusters to have a much narrower distribution that peaks within 0.2 Mpc. It is possible that other effects are lowering the ACT and Planck signals by the same amount, with offsets between BCGs and SZ peaks explaining the remaining difference between ACT and Planck measurements. Several effects that can lower the SZ signal equally for both ACT and Planck, but not explain the difference in measured signals, include a larger percentage of false detections in the MaxBCG sample, a lower normalization of the mass-richness relation, radio or infrared galaxy contamination of the SZ flux, and a low intrinsic SZ signal. In the latter two cases, the effects would need to be preferentially more significant in the optically selected MaxBCG sample than in the MCXC X-ray sample.
C1 [Sehgal, Neelima; Hlozek, Renee; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Addison, Graeme; Dunkley, Joanna; Louis, Thibaut] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
[Battaglia, Nick] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA.
[Battistelli, Elia S.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy.
[Battistelli, Elia S.; Halpern, Mark; Hasselfield, Matthew] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada.
[Bond, J. Richard; Hajian, Amir; Hincks, Adam D.; Sievers, Jon; Switzer, Eric R.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Das, Sudeep] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, LBL, Berkeley, CA 94720 USA.
[Das, Sudeep] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Devlin, Mark J.; Reese, Erik D.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Duenner, Rolando; Sifon, Cristobal] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Fac Fis, Santiago 22, Chile.
[Gralla, Megan; Marriage, Tobias A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Hilton, Matt] Univ Nottingham, Ctr Astron & Particle Theory, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Hincks, Adam D.; Page, Lyman A.; Sherwin, Blake D.; Staggs, Suzanne T.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA.
[Hughes, John P.; Menanteau, Felipe] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Lin, Yen-Ting] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan.
[Lin, Yen-Ting] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2778568, Japan.
[Marsden, Danica] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Moodley, Kavilan] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, Sch Math Sci, ZA-4041 Durban, South Africa.
[Niemack, Michael D.; Swetz, Daniel S.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA.
[Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA.
[Wollack, Ed] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Sehgal, N (reprint author), Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA.
RI Spergel, David/A-4410-2011; Hilton, Matthew James/N-5860-2013; Wollack,
Edward/D-4467-2012;
OI Wollack, Edward/0000-0002-7567-4451; Menanteau,
Felipe/0000-0002-1372-2534; Sievers, Jonathan/0000-0001-6903-5074;
Sifon, Cristobal/0000-0002-8149-1352
FU U.S. National Science Foundation [AST-0408698, PHY-0355328, AST-0707731,
PIRE-0507768, OISE-0530095]; Princeton University; University of
Pennsylvania; Canada Foundation for Innovation (CFI); Compute Canada;
Government of Ontario; Ontario Research Fund-Research Excellence;
University of Toronto; National Science Foundation [1102762, 1066293];
U.S. Department of Energy [DE-AC3-76SF00515]
FX This work was supported by the U.S. National Science Foundation through
awards AST-0408698 for the ACT project, and PHY-0355328, AST-0707731,
and PIRE-0507768 (award number OISE-0530095). The PIRE program made
possible exchanges between Chile, South Africa, Spain, and the U. S.
that enabled this research program. Funding was also provided by
Princeton University, the University of Pennsylvania, and a Canada
Foundation for Innovation (CFI) award to UBC. Computations were
performed on the GPC supercomputer at the SciNet HPC Consortium. SciNet
is funded by the Canada Foundation for Innovation under the auspices of
Compute Canada; the Government of Ontario; Ontario Research
Fund-Research Excellence; and the University of Toronto. ACT is on the
Chajnantor Science preserve, which was made possible by the Chilean
Comision Nacional de Investigacion Cientifica y Tecnologica (CONICYT).
N.S. is supported by the National Science Foundation under Award No.
1102762. During the completion of this work, N.S. was also supported by
the U.S. Department of Energy contract to SLAC No. DE-AC3-76SF00515 and
in part by the National Science Foundation under grant No. 1066293 and
the hospitality of the Aspen Center for Physics. The data will be made
public through LAMBDA (http://lambda.gsfc.nasa.gov/) and the ACT Web
site (http://www.physics.princeton.edu/act/).
NR 60
TC 17
Z9 17
U1 0
U2 9
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2013
VL 767
IS 1
AR 38
DI 10.1088/0004-637X/767/1/38
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 117IT
UT WOS:000316947500038
ER
PT J
AU Trott, CM
Tingay, SJ
Wayth, RB
Thompson, DR
Deller, AT
Brisken, WF
Wagstaff, KL
Majid, WA
Burke-Spolaor, S
Macquart, JPR
Palaniswamy, D
AF Trott, Cathryn M.
Tingay, Steven J.
Wayth, Randall B.
Thompson, David R.
Deller, Adam T.
Brisken, Walter F.
Wagstaff, Kiri L.
Majid, Walid A.
Burke-Spolaor, Sarah
Macquart, Jean-Pierre R.
Palaniswamy, Divya
TI A FRAMEWORK FOR INTERPRETING FAST RADIO TRANSIENTS SEARCH EXPERIMENTS:
APPLICATION TO THE V-FASTR EXPERIMENT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE instrumentation: detectors; methods: data analysis; methods:
observational; radio continuum: general; surveys
ID BASE-LINE ARRAY; PULSAR SURVEY
AB We define a framework for determining constraints on the detection rate of fast transient events from a population of underlying sources, with a view to incorporate beam shape, frequency effects, scattering effects, and detection efficiency into the metric. We then demonstrate a method for combining independent data sets into a single event rate constraint diagram, using a probabilistic approach to the limits on parameter space. We apply this new framework to present the latest results from the V-FASTR experiment, a commensal fast transients search using the Very Long Baseline Array (VLBA). In the 20 cm band, V-FASTR now has the ability to probe the regions of parameter space of importance for the observed Lorimer and Keane fast radio transient candidates by combining the information from observations with differing bandwidths, and properly accounting for the source dispersion measure, VLBA antenna beam shape, experiment time sampling, and stochastic nature of events. We then apply the framework to combine the results of the V-FASTR and Allen Telescope Array Fly's Eye experiments, demonstrating their complementarity. Expectations for fast transients experiments for the SKA Phase I dish array are then computed, and the impact of large differential bandwidths is discussed.
C1 [Trott, Cathryn M.; Tingay, Steven J.; Wayth, Randall B.; Macquart, Jean-Pierre R.; Palaniswamy, Divya] Curtin Univ Technol, Int Ctr Radio Astron Res, Perth, WA 6845, Australia.
[Thompson, David R.; Wagstaff, Kiri L.; Majid, Walid A.; Burke-Spolaor, Sarah] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Deller, Adam T.] ASTRON, NL-7991 PD Dwingeloo, Netherlands.
[Brisken, Walter F.] NRAO, Socorro, NM 87801 USA.
EM cathryn.trott@curtin.edu.au
RI Trott, Cathryn/B-5325-2013; Wayth, Randall/B-2444-2013;
OI Trott, Cathryn/0000-0001-6324-1766; Wayth, Randall/0000-0002-6995-4131;
Deller, Adam/0000-0001-9434-3837; Wagstaff, Kiri/0000-0003-4401-5506
FU State Government of Western Australia; Western Australian Centre of
Excellence in Radio Astronomy Science and Engineering; NRAO Jansky
Fellowship; NWO Veni Fellowship; U.S. National Aeronautics and Space
Administration; [CE110001020]
FX The Centre for All-sky Astrophysics is an Australian Research Council
Centre of Excellence, funded by grant CE110001020. The International
Centre for Radio Astronomy Research (ICRAR) is a Joint Venture between
Curtin University and the University of Western Australia, funded by the
State Government of Western Australia and the Joint Venture partners.
S.J.T. is a Western Australian Premiers Research Fellow. R. B. W. is
supported via the Western Australian Centre of Excellence in Radio
Astronomy Science and Engineering. A. T. D. was supported by an NRAO
Jansky Fellowship and an NWO Veni Fellowship. Part of this research was
carried out at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the U.S. National Aeronautics and Space
Administration. 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.
NR 18
TC 6
Z9 6
U1 0
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2013
VL 767
IS 1
AR 4
DI 10.1088/0004-637X/767/1/4
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 117IT
UT WOS:000316947500004
ER
PT J
AU Weiss, A
De Breuck, C
Marrone, DP
Vieira, JD
Aguirre, JE
Aird, KA
Aravena, M
Ashby, MLN
Bayliss, M
Benson, BA
Bethermin, M
Biggs, AD
Bleem, LE
Bock, JJ
Bothwell, M
Bradford, CM
Brodwin, M
Carlstrom, JE
Chang, CL
Chapman, SC
Crawford, TM
Crites, AT
de Haan, T
Dobbs, MA
Downes, TP
Fassnacht, CD
George, EM
Gladders, MD
Gonzalez, AH
Greve, TR
Halverson, NW
Hezaveh, YD
High, FW
Holder, GP
Holzapfel, WL
Hoover, S
Hrubes, JD
Husband, K
Keisler, R
Lee, AT
Leitch, EM
Lueker, M
Luong-Van, D
Malkan, M
McIntyre, V
McMahon, JJ
Mehl, J
Menten, KM
Meyer, SS
Murphy, EJ
Padin, S
Plagge, T
Reichardt, CL
Rest, A
Rosenman, M
Ruel, J
Ruhl, JE
Schaffer, KK
Shirokoff, E
Spilker, JS
Stalder, B
Staniszewski, Z
Stark, AA
Story, K
Vanderlinde, K
Welikala, N
Williamson, R
AF Weiss, A.
De Breuck, C.
Marrone, D. P.
Vieira, J. D.
Aguirre, J. E.
Aird, K. A.
Aravena, M.
Ashby, M. L. N.
Bayliss, M.
Benson, B. A.
Bethermin, M.
Biggs, A. D.
Bleem, L. E.
Bock, J. J.
Bothwell, M.
Bradford, C. M.
Brodwin, M.
Carlstrom, J. E.
Chang, C. L.
Chapman, S. C.
Crawford, T. M.
Crites, A. T.
de Haan, T.
Dobbs, M. A.
Downes, T. P.
Fassnacht, C. D.
George, E. M.
Gladders, M. D.
Gonzalez, A. H.
Greve, T. R.
Halverson, N. W.
Hezaveh, Y. D.
High, F. W.
Holder, G. P.
Holzapfel, W. L.
Hoover, S.
Hrubes, J. D.
Husband, K.
Keisler, R.
Lee, A. T.
Leitch, E. M.
Lueker, M.
Luong-Van, D.
Malkan, M.
McIntyre, V.
McMahon, J. J.
Mehl, J.
Menten, K. M.
Meyer, S. S.
Murphy, E. J.
Padin, S.
Plagge, T.
Reichardt, C. L.
Rest, A.
Rosenman, M.
Ruel, J.
Ruhl, J. E.
Schaffer, K. K.
Shirokoff, E.
Spilker, J. S.
Stalder, B.
Staniszewski, Z.
Stark, A. A.
Story, K.
Vanderlinde, K.
Welikala, N.
Williamson, R.
TI ALMA REDSHIFTS OF MILLIMETER-SELECTED GALAXIES FROM THE SPT SURVEY: THE
REDSHIFT DISTRIBUTION OF DUSTY STAR-FORMING GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; early universe; galaxies: evolution; galaxies:
high-redshift; ISM: molecules
ID HUBBLE-DEEP-FIELD; SOUTH-POLE TELESCOPE; SCUBA SUPER-MAP; DEGREE
EXTRAGALACTIC SURVEY; SUBMILLIMETER GALAXIES; MOLECULAR GAS; FORMATION
HISTORY; NUMBER COUNTS; HERSCHEL ATLAS; LABOCA SURVEY
AB Using the Atacama Large Millimeter/submillimeter Array, we have conducted a blind redshift survey in the 3 mm atmospheric transmission window for 26 strongly lensed dusty star- forming galaxies (DSFGs) selected with the South Pole Telescope. The sources were selected to have S-1.4mm > 20 mJy and a dust- like spectrum and, to remove low- z sources, not have bright radio (S-843MHz < 6 mJy) or far- infrared counterparts (S100 mu m < 1 Jy, S-60 mu m < 200 mJy). We robustly detect 44 line features in our survey, which we identify as redshifted emission lines of (CO)-C-12, (CO)-C-13, CI, H2O, and H2O+. We find one or more spectral features in 23 sources yielding a similar to 90% detection rate for this survey; in 12 of these sources we detect multiple lines, while in 11 sources we detect only a single line. For the sources with only one detected line, we break the redshift degeneracy with additional spectroscopic observations if available, or infer the most likely line identification based on photometric data. This yields secure redshifts for similar to 70% of the sample. The three sources with no lines detected are tentatively placed in the redshift desert between 1.7< z< 2.0. The resulting mean redshift of our sample is z = 3.5. This finding is in contrast to the redshift distribution of radio- identified DSFGs, which have a significantly lower mean redshift of z = 2.3 and for which only 10%- 15% of the population is expected to be at z> 3. We discuss the effect of gravitational lensing on the redshift distribution and compare our measured redshift distribution to that of models in the literature.
C1 [Weiss, A.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[De Breuck, C.; Aravena, M.; Biggs, A. D.] European So Observ, D-85748 Garching, Germany.
[Marrone, D. P.; Bothwell, M.; Spilker, J. S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Vieira, J. D.; Bock, J. J.; Downes, T. P.; Lueker, M.; Padin, S.; Shirokoff, E.; Staniszewski, Z.] CALTECH, Pasadena, CA 91125 USA.
[Aguirre, J. E.; Rosenman, M.] Univ Penn, Philadelphia, PA 19104 USA.
[Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA.
[Ashby, M. L. N.; Bayliss, M.; Stalder, B.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bayliss, M.; Ruel, J.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Hoover, S.; Keisler, R.; Leitch, E. M.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Schaffer, K. K.; Story, K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Hoover, S.; McMahon, J. J.; Meyer, S. S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Bethermin, M.] Univ Paris Diderot, CEA Saclay, CNRS, CEA,DSM,Irfu,Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France.
[Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Story, K.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Bock, J. J.; Bradford, C. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
[Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Chapman, S. C.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada.
[Chapman, S. C.; Husband, K.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[de Haan, T.; Dobbs, M. A.; Hezaveh, Y. D.; Holder, G. P.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Fassnacht, C. D.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[George, E. M.; Holzapfel, W. L.; Lee, A. T.; Reichardt, C. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Greve, T. R.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Lee, A. T.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA.
[Malkan, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[McIntyre, V.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Murphy, E. J.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Ruhl, J. E.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA.
[Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA.
[Welikala, N.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Welikala, N.] CNRS, F-91405 Orsay, France.
RP Weiss, A (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
RI Aravena, Manuel/O-2361-2014; Williamson, Ross/H-1734-2015; Holzapfel,
William/I-4836-2015;
OI Williamson, Ross/0000-0002-6945-2975; Marrone,
Daniel/0000-0002-2367-1080; Aird, Kenneth/0000-0003-1441-9518;
Reichardt, Christian/0000-0003-2226-9169; De Breuck,
Carlos/0000-0002-6637-3315; Bethermin, Matthieu/0000-0002-3915-2015;
Stark, Antony/0000-0002-2718-9996
NR 85
TC 87
Z9 87
U1 1
U2 13
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2013
VL 767
IS 1
AR 88
DI 10.1088/0004-637X/767/1/88
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 117IT
UT WOS:000316947500088
ER
PT J
AU Zhang, YC
Tan, JC
De Buizer, JM
Sandell, G
Beltran, MT
Churchwell, E
McKee, CF
Shuping, R
Staff, JE
Telesco, C
Whitney, B
AF Zhang, Yichen
Tan, Jonathan C.
De Buizer, James M.
Sandell, Goeran
Beltran, Maria T.
Churchwell, Ed
McKee, Christopher F.
Shuping, Ralph
Staff, Jan E.
Telesco, Charles
Whitney, Barbara
TI A MASSIVE PROTOSTAR FORMING BY ORDERED COLLAPSE OF A DENSE, MASSIVE CORE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: formation
ID STAR-FORMATION; MOLECULAR OUTFLOWS; G35.2-0.74N; G35.20-0.74; CLUSTER;
CLUMPS; VIEW; JET
AB We present 30 and 40 mu m imaging of the massive protostar G35.20-0.74 with SOFIA-FORCAST. The high surface density of the natal core around the protostar leads to high extinction, even at these relatively long wavelengths, causing the observed flux to be dominated by that emerging from the near-facing outflow cavity. However, emission from the far-facing cavity is still clearly detected. We combine these results with fluxes from the near-infrared to mm to construct a spectral energy distribution (SED). For isotropic emission the bolometric luminosity would be 3.3 x 10(4) L-circle dot. We perform radiative transfer modeling of a protostar forming by ordered, symmetric collapse from a massive core bounded by a clump with high-mass surface density, Sigma(cl). To fit the SED requires protostellar masses similar to 20-34 M-circle dot depending on the outflow cavity opening angle (35 degrees-50 degrees), and Sigma(cl) similar to 0.4-1 g cm(-2). After accounting for the foreground extinction and the flashlight effect, the true bolometric luminosity is similar to(0.7-2.2) x 10(5) L-circle dot. One of these models also has excellent agreement with the observed intensity profiles along the outflow axis at 10, 18, 31, and 37 mu m. Overall our results support a model of massive star formation involving the relatively ordered, symmetric collapse of a massive, dense core and the launching bipolar outflows that clear low-density cavities. Thus a unified model may apply for the formation of both low- and high-mass stars.
C1 [Zhang, Yichen; Tan, Jonathan C.; Telesco, Charles] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Tan, Jonathan C.] Univ Florida, Dept Phys, Gainesville, FL 32611 USA.
[De Buizer, James M.; Sandell, Goeran; Shuping, Ralph] NASA, SOFIA USRA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Beltran, Maria T.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
[Churchwell, Ed; Whitney, Barbara] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[McKee, Christopher F.] Univ Calif Berkeley, Dept Astron & Astrophys, Berkeley, CA 94720 USA.
[McKee, Christopher F.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Staff, Jan E.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA.
RP Zhang, YC (reprint author), Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
EM yc.zhang@astro.ufl.edu
OI Beltran Sorolla, Maria Teresa/0000-0003-3315-5626
FU NASA [NAS2-97001, NNX09AK31G]; Deutsches SOFIA Institut (DSI) under DLR
[50 OK 0901]; University of Florida; NSF CAREER [AST-0645412];
NASA/USRA; NSF [AST-0908553, AST-1211729]
FX This work is based on observations made with the NASA/DLR Stratospheric
Observatory for Infrared Astronomy (SOFIA). SOFIA is jointly operated by
the Universities Space Research Association, Inc. (USRA), under NASA
contract NAS2-97001, and the Deutsches SOFIA Institut (DSI) under DLR
contract 50 OK 0901 to the University of Stuttgart. Y.Z. acknowledges
support from a Graduate School Fellowship from the University of
Florida. J.C.T. acknowledges support from NSF CAREER grant AST-0645412
and NASA/USRA grant in support of SOFIA Basic Science observations. C.
F. M. acknowledges support from NSF grants AST-0908553 and AST-1211729
and NASA grant NNX09AK31G.
NR 33
TC 13
Z9 13
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2013
VL 767
IS 1
AR 58
DI 10.1088/0004-637X/767/1/58
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 117IT
UT WOS:000316947500058
ER
PT J
AU Kopparapu, RK
AF Kopparapu, Ravi Kumar
TI A REVISED ESTIMATE OF THE OCCURRENCE RATE OF TERRESTRIAL PLANETS IN THE
HABITABLE ZONES AROUND KEPLER M-DWARFS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planets and satellites: atmospheres
ID M-CIRCLE-PLUS; SUPER-EARTH; STARS; CANDIDATES; SYSTEM; EVOLUTION;
DATABASE; SEARCH; MODELS; MARS
AB Because of their large numbers, low-mass stars may be the most abundant planet hosts in our Galaxy. Furthermore, terrestrial planets in the habitable zones (HZs) around M-dwarfs can potentially be characterized in the near future and hence may be the first such planets to be studied. Recently, Dressing & Charbonneau used Kepler data and calculated the frequency of terrestrial planets in the HZ of cool stars to be 0.15(-0.06)(+0.13) per star for Earth-size planets (0.5-1.4 R-circle plus). However, this estimate was derived using the Kasting et al. HZ limits, which were not valid for stars with effective temperatures lower than 3700 K. Here we update their result using new HZ limits from Kopparapu et al. for stars with effective temperatures between 2600 K and 7200 K, which includes the cool M stars in the Kepler target list. The new HZ boundaries increase the number of planet candidates in the HZ. Assuming Earth- size planets as 0.5- 1.4 R-circle plus, when we reanalyze their results, we obtain a terrestrial planet frequency of 0.48(- 0.24)(+0.12) and 0.53(-0.17)(+0.08) planets per M-dwarf star for conservative and optimistic limits of the HZ boundaries, respectively. Assuming Earth- size planets as 0.5-2 R-circle plus, the frequency increases to 0.51(-0.20)(+0.10) per star for the conservative estimate and to 0.61(-0.15)(+0.07) per star for the optimistic estimate. Within uncertainties, our optimistic estimates are in agreement with a similar optimistic estimate from the radial velocity survey of M-dwarfs (0.41(-0.13)(+0.54)). So, the potential for finding Earth- like planets around M stars may be higher than previously reported.
C1 [Kopparapu, Ravi Kumar] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
[Kopparapu, Ravi Kumar] Penn State Astrobiol Res Ctr, University Pk, PA 16802 USA.
[Kopparapu, Ravi Kumar] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
RP Kopparapu, RK (reprint author), NASA, Astrobiol Inst Virtual Planetary Lab, Washington, DC USA.
FU NASA Astrobiology Institute's Virtual Planetary Laboratory lead team;
NASA [NNH05ZDA001C]; Penn State Astrobiology Research Center
FX The author is grateful to Courtney Dressing for discussions leading to
this paper. The author thanks James Kasting, Steinn Sigurdsson, Eric
Feigelson, Suvrath Mahadevan, Jason Wright, Chester Harman, and Ramses
Ramirez for their valuable input and the anonymous referee whose
comments improved the manuscript. R.K. gratefully acknowledges funding
from NASA Astrobiology Institute's Virtual Planetary Laboratory lead
team, supported by NASA under cooperative agreement NNH05ZDA001C, and
the Penn State Astrobiology Research Center.
NR 31
TC 79
Z9 79
U1 1
U2 22
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 10
PY 2013
VL 767
IS 1
AR L8
DI 10.1088/2041-8205/767/1/L8
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 118CB
UT WOS:000316998900008
ER
PT J
AU Nersisyan, SR
Tabiryan, NV
Mawet, D
Serabyn, E
AF Nersisyan, Sarik R.
Tabiryan, Nelson V.
Mawet, Dimitri
Serabyn, Eugene
TI Improving vector vortex waveplates for high-contrast coronagraphy
SO OPTICS EXPRESS
LA English
DT Article
AB Vector vortex waveplates (VVWs) open the door to new techniques in stellar coronagraphy and optical communications, but the performance of currently available liquid-crystal-polymer-based VVWs tends to be limited by defects in the axial region of the vortex pattern. As described here, several steps allow for a reduction in the size of such axial defects, including the use of photoalignment materials with high photosensitivity and reversible response, and a reduction in exposure energy. Moreover, redistributing the writing beam's intensity from the axial region to its periphery (using a VVW) allows the production of large area VVWs with a small defect area. Finally, using VVWs as linear to axial polarization converters allows producing VVWs of higher topological charge, while also reducing the photoalignment time to a few minutes. These steps have allowed the fabrication of VVWs with topological charges of 1 and 2 with central defect sizes below 3 mu m. (C)2013 Optical Society of America
C1 [Nersisyan, Sarik R.; Tabiryan, Nelson V.] BEAM Engn Adv Measurements Co, Winter Pk, FL 32789 USA.
[Mawet, Dimitri] European So Observ, Santiago 19, Chile.
[Serabyn, Eugene] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Nersisyan, SR (reprint author), BEAM Engn Adv Measurements Co, 809 S Orlando Ave,Suite 1, Winter Pk, FL 32789 USA.
EM nelson@beamco.com
FU NASA SBIR Program [NNX11CF39P]
FX The study was supported by NASA SBIR Program (Contract no. NNX11CF39P).
Part of this work was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under contract with NASA.
NR 15
TC 21
Z9 21
U1 2
U2 21
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD APR 8
PY 2013
VL 21
IS 7
BP 8205
EP 8213
DI 10.1364/OE.21.008205
PG 9
WC Optics
SC Optics
GA 126YN
UT WOS:000317659300036
PM 23571910
ER
PT J
AU Kaul, AB
Coles, JB
Eastwood, M
Green, RO
Bandaru, PR
AF Kaul, Anupama B.
Coles, James B.
Eastwood, Michael
Green, Robert O.
Bandaru, Prabhakar R.
TI Ultra-High Optical Absorption Efficiency from the Ultraviolet to the
Infrared Using Multi-Walled Carbon Nanotube Ensembles
SO SMALL
LA English
DT Article
DE optical absorbers; nanoabsorbers; nanomaterials; carbon nanotubes
ID SILICON NANOWIRE; ABSORBER; ARRAYS; DEPOSITION; CATALYST; DENSITY;
GROWTH
AB The optical absorption efficiencies of vertically aligned multi-walled (MW)-carbon nanotube (CNT) ensembles are characterized in the 3507000 nm wavelength range where CNT site densities > 1 x 1011/cm2 are achieved directly on metallic substrates. The site density directly impacts the optical absorption characteristics, and while high-density arrays of CNTs on electrically insulating and non-metallic substrates have been commonly reported, achieving high site-densities on metals has been challenging and remains an area of active research. These absorber ensembles are ultra-thin (<10 m) and yet they still exhibit a reflectance as low as approximate to 0.02%, which is 100 times lower than the reference; these characteristics make them potentially attractive for high-sensitivity and high-speed thermal detectors. In addition, the use of a plasma-enhanced chemical vapor deposition process for the synthesis of the absorbers increases the portfolio of materials that can be integrated with such absorbers due to the potential for reduced synthesis temperatures. The remarkable ruggedness of the absorbers is also demonstrated as they are exposed to high temperatures in an oxidizing ambient environment, making them well-suited for extreme thermal environments encountered in the field, potentially for solar cell applications. Finally, a phenomenological model enables the determinatiom of the extinction coefficients in these nanostructures and the results compare well with experiment.
C1 [Kaul, Anupama B.; Coles, James B.; Eastwood, Michael; Green, Robert O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bandaru, Prabhakar R.] Univ Calif San Diego, Jacobs Sch Engn, La Jolla, CA 92093 USA.
RP Kaul, AB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Anupama.B.Kaul@jpl.nasa.gov
FU internal Research and Technology Development (RTD) program [01STCR,
R.10.021.067]; National Science Foundation
FX We thank K. Megerian, M. Anderson, and R. Kowalczyk for technical
assistance and T. Pagano, P. Goldsmith, J. Hyon, M. Foote, and W. Holmes
for useful discussions. This research was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration and was
funded through the internal Research and Technology Development (R&TD)
program (01STCR, R.10.021.067). ABK also acknowledges support for this
work through the National Science Foundation's IR/D program.
NR 27
TC 13
Z9 13
U1 7
U2 70
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY
SN 1613-6810
J9 SMALL
JI Small
PD APR 8
PY 2013
VL 9
IS 7
BP 1058
EP 1065
DI 10.1002/smll.201202232
PG 8
WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience &
Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied;
Physics, Condensed Matter
SC Chemistry; Science & Technology - Other Topics; Materials Science;
Physics
GA 118IT
UT WOS:000317019800016
PM 23233398
ER
PT J
AU Blake, DR
Simpson, IJ
Meinardi, SJ
Andersen, MJS
Bruhwiler, L
AF Blake, Donald R.
Simpson, Isobel J.
Meinardi, Simone J.
Andersen, Mads J. Sulbaek
Bruhwiler, Lori
TI Award Address (ACS Award for Creative Advances in Environmental Science
and Technology sponsored by ACS Division of Environmental Chemistry and
ACS Publications Divisions). Long-term trends in global concentrations
of atmospheric methane and ethane
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 245th National Spring Meeting of the American-Chemical-Society (ACS)
CY APR 07-11, 2013
CL New Orleans, LA
SP Amer Chem Soc
C1 [Blake, Donald R.; Simpson, Isobel J.; Meinardi, Simone J.] Univ Calif Irvine, Irvine, CA 92617 USA.
[Andersen, Mads J. Sulbaek] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bruhwiler, Lori] NOAA Earth Syst Res Lab ESRL, Boulder, CO 80305 USA.
EM drblake@uci.edu
NR 0
TC 0
Z9 0
U1 0
U2 1
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD APR 7
PY 2013
VL 245
MA 241-ENVR
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 216SF
UT WOS:000324303600089
ER
PT J
AU Chu, SH
Park, C
Lowther, SE
Gibbons, LJ
Sauti, G
Kang, JH
Thibeault, SA
Fay, CC
Bryant, RG
AF Chu, Sang-Hyon
Park, Cheol
Lowther, Sharon E.
Gibbons, Luke J.
Sauti, Godfrey
Kang, Jin Ho
Thibeault, Sheila A.
Fay, Catharine C.
Bryant, Robert G.
TI Porous polyimide nanocomposite films with high neutron absorption
effectiveness
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 245th National Spring Meeting of the American-Chemical-Society (ACS)
CY APR 07-11, 2013
CL New Orleans, LA
SP Amer Chem Soc
C1 [Chu, Sang-Hyon; Park, Cheol; Gibbons, Luke J.; Sauti, Godfrey; Kang, Jin Ho] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Lowther, Sharon E.; Thibeault, Sheila A.; Fay, Catharine C.; Bryant, Robert G.] NASA Langley Res Ctr, Hampton, VA 23681 USA.
EM sang-hyon.chu-1@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 4
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD APR 7
PY 2013
VL 245
MA 488-PMSE
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 216SF
UT WOS:000324303604437
ER
PT J
AU Guo, HQ
Meador, MAB
Bali, S
McCorkle, L
Guo, J
Hamilton, B
Cakmak, M
AF Guo, Haiquan
Meador, Mary Ann B.
Bali, Sheeba
McCorkle, Linda
Guo, Jiao
Hamilton, Bart
Cakmak, Miko
TI Optimization of properties of cross-linked polyimide aerogels for high
temperature aerospace applications
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 245th National Spring Meeting of the American-Chemical-Society (ACS)
CY APR 07-11, 2013
CL New Orleans, LA
SP Amer Chem Soc
C1 [Guo, Haiquan; McCorkle, Linda] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
[Meador, Mary Ann B.; Bali, Sheeba] NASA Glenn Res Ctr, Cleveland, OH 44135 USA.
[Guo, Jiao; Hamilton, Bart; Cakmak, Miko] Univ Akron, Akron, OH 44325 USA.
EM haiquan.n.guo@nasa.gov
NR 0
TC 0
Z9 1
U1 1
U2 3
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD APR 7
PY 2013
VL 245
MA 358-PMSE
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 216SF
UT WOS:000324303604306
ER
PT J
AU Li, J
Klankowski, S
Rojeski, R
Cruden, BA
Liu, JW
Wu, J
AF Li, Jun
Klankowski, Steven
Rojeski, Ronald
Cruden, Brett A.
Liu, Jianwei
Wu, Judy
TI High-performance lithium-ion battery anode based on core-shell
heterostructure of silicon-coated vertically aligned carbon nanofibers
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 245th National Spring Meeting of the American-Chemical-Society (ACS)
CY APR 07-11, 2013
CL New Orleans, LA
SP Amer Chem Soc
C1 [Li, Jun; Klankowski, Steven] Kansas State Univ, Dept Chem, Manhattan, KS 66506 USA.
[Rojeski, Ronald] Catalyst Power Technol, Campbell, CA 95008 USA.
[Cruden, Brett A.] NASA Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
[Liu, Jianwei; Wu, Judy] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
EM junli@ksu.edu
NR 0
TC 0
Z9 0
U1 0
U2 8
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD APR 7
PY 2013
VL 245
MA 30-IEC
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 216SF
UT WOS:000324303600622
ER
PT J
AU Meador, MAB
Miranda, FA
Wright, S
Sandberg, A
Nguyen, BN
Van Keuls, FW
Mueller, CH
Rodriguez, R
AF Meador, Mary Ann B.
Miranda, Felix A.
Wright, Sarah
Sandberg, Anna
Nguyen, Baochau N.
Van Keuls, Frederick W.
Mueller, Carl H.
Rodriguez, Rafael
TI Low dielectric polyimide aerogels as substrates for lightweight patch
antennas
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 245th National Spring Meeting of the American-Chemical-Society (ACS)
CY APR 07-11, 2013
CL New Orleans, LA
SP Amer Chem Soc
C1 [Meador, Mary Ann B.; Miranda, Felix A.; Wright, Sarah; Sandberg, Anna; Van Keuls, Frederick W.; Mueller, Carl H.; Rodriguez, Rafael] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Nguyen, Baochau N.] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
EM maryann.meador@nasa.gov
NR 0
TC 0
Z9 0
U1 5
U2 6
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD APR 7
PY 2013
VL 245
MA 241-PMSE
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 216SF
UT WOS:000324303604182
ER
PT J
AU Vance, S
Christensen, L
AF Vance, Steve
Christensen, Lance
TI In situ characterization of naturally occurring methane and ethane at
sites of active serpentinization by tunable diode laser spectroscopy
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 245th National Spring Meeting of the American-Chemical-Society (ACS)
CY APR 07-11, 2013
CL New Orleans, LA
SP Amer Chem Soc
C1 [Vance, Steve; Christensen, Lance] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
EM svance@jpl.nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 1
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD APR 7
PY 2013
VL 245
MA 93-GEOC
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 216SF
UT WOS:000324303600534
ER
PT J
AU Wojtecki, RJ
Johnson, JC
Meador, MA
Rowan, SJ
AF Wojtecki, Rudy J.
Johnson, J. Casey
Meador, Michael A.
Rowan, Stuart J.
TI Toward the design and synthesis of mechanically interlocked polymers
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 245th National Spring Meeting of the American-Chemical-Society (ACS)
CY APR 07-11, 2013
CL New Orleans, LA
SP Amer Chem Soc
C1 [Wojtecki, Rudy J.; Johnson, J. Casey; Rowan, Stuart J.] Case Western Reserve Univ, Cleveland, OH 44106 USA.
[Meador, Michael A.] NASA, Glenn Res Ctr, Dept Nanotechnol Res, Cleveland, OH 44135 USA.
EM rjw41@case.edu
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD APR 7
PY 2013
VL 245
MA 526-ORGN
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 216SF
UT WOS:000324303603197
ER
PT J
AU Barzen-Hanson, K
Uz-Zaman, A
Oye, M
Meyyapan, M
Koehne, J
AF Barzen-Hanson, Krista
Uz-Zaman, Asma
Oye, Michael
Meyyapan, Meyya
Koehne, Jessica
TI Growth optimization of monolayer graphene films using chemical vapor
deposition
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 245th National Meeting of the American-Chemical-Society (ACS)
CY APR 07-11, 2013
CL New Orleans, LA
SP Amer Chem Soc
C1 [Barzen-Hanson, Krista] Coll St Benedict, Dept Chem, St Joseph, MN 56374 USA.
[Uz-Zaman, Asma] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
[Oye, Michael; Meyyapan, Meyya; Koehne, Jessica] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
EM kabarzenhanson@csbsju.edu
NR 0
TC 0
Z9 0
U1 0
U2 4
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD APR 7
PY 2013
VL 245
MA 844-CHED
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 210RD
UT WOS:000323851302637
ER
PT J
AU Fortenberry, RC
Huang, XC
Lee, TJ
AF Fortenberry, Ryan C.
Huang, Xinchuan
Lee, Timothy J.
TI Quartic force fields and dipole surfaces for accurate computational
rovibrational reference data for interstellar studies
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 245th National Meeting of the American-Chemical-Society (ACS)
CY APR 07-11, 2013
CL New Orleans, LA
SP Amer Chem Soc
C1 [Fortenberry, Ryan C.; Lee, Timothy J.] NASA, Space Sci & Astrobiol Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Huang, Xinchuan] SETI Inst, Mountain View, CA 94043 USA.
EM ryan.c.fortenberry@nasa.gov
RI HUANG, XINCHUAN/A-3266-2013
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD APR 7
PY 2013
VL 245
MA 391-COMP
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 210RD
UT WOS:000323851304396
ER
PT J
AU Holt, B
Jones, CE
Minchew, B
Brekke, C
AF Holt, Benjamin
Jones, Cathleen E.
Minchew, Brent
Brekke, Camilla
TI Deepwater Horizon oil slick characterization with UAVSAR: Continuing
investigations
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 245th National Meeting of the American-Chemical-Society (ACS)
CY APR 07-11, 2013
CL New Orleans, LA
SP Amer Chem Soc
C1 [Holt, Benjamin; Jones, Cathleen E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Minchew, Brent] CALTECH, Pasadena, CA 91125 USA.
[Brekke, Camilla] Univ Tromso, Tromso, Norway.
EM Benjamin.M.Holt@jpl.nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 3
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD APR 7
PY 2013
VL 245
MA 223-ANYL
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 210RD
UT WOS:000323851300440
ER
PT J
AU Rajput, NN
Monk, J
Hung, FR
AF Rajput, Nav N.
Monk, Joshua
Hung, Francisco R.
TI Ionic liquids confined inside model nanoporous carbons: A molecular
simulation study
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 245th National Meeting of the American-Chemical-Society (ACS)
CY APR 07-11, 2013
CL New Orleans, LA
SP Amer Chem Soc
C1 [Rajput, Nav N.; Hung, Francisco R.] Louisiana State Univ, Cain Dept Chem Engn, Baton Rouge, LA 70803 USA.
[Monk, Joshua] NASA, Thermal Protect Mat Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM nrajpu1@tigers.lsu.edu
NR 0
TC 0
Z9 0
U1 0
U2 1
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD APR 7
PY 2013
VL 245
MA 449-COMP
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 210RD
UT WOS:000323851304444
ER
PT J
AU Rajput, NN
Monk, J
Singh, R
Hung, FR
AF Rajput, Nav N.
Monk, Joshua
Singh, Ramesh
Hung, Francisco R.
TI Molecular modeling of the ionic liquid [EMIM+][TFMSI-] confined in model
nanoporous materials
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 245th National Meeting of the American-Chemical-Society (ACS)
CY APR 07-11, 2013
CL New Orleans, LA
SP Amer Chem Soc
C1 [Rajput, Nav N.; Hung, Francisco R.] Louisiana State Univ, Cain Dept Chem Engn, Baton Rouge, LA 70803 USA.
[Monk, Joshua] NASA, Thermal Protect Mat Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Singh, Ramesh] Univ Notre Dame, Dept Chem & Biomol Engn, Notre Dame, IN 46556 USA.
EM nrajpu1@tigers.lsu.edu
NR 0
TC 0
Z9 0
U1 0
U2 1
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD APR 7
PY 2013
VL 245
MA 240-COMP
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 210RD
UT WOS:000323851304267
ER
PT J
AU Sutton, AJ
McKenzie, K
Ware, B
de Vine, G
Spero, RE
Klipstein, W
Shaddock, DA
AF Sutton, Andrew J.
McKenzie, Kirk
Ware, Brent
de Vine, Glenn
Spero, Robert E.
Klipstein, W.
Shaddock, Daniel A.
TI Improved optical ranging for space based gravitational wave detection
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article
ID LISA; LASER; COMMUNICATION
AB The operation of 10(6) km scale laser interferometers in space will permit the detection of gravitational waves at previously unaccessible frequency regions. Multi-spacecraft missions, such as the Laser Interferometer Space Antenna (LISA), will use time delay interferometry to suppress the otherwise dominant laser frequency noise from their measurements. This is accomplished by performing sub-sample interpolation of the optical phase measurements recorded at each spacecraft for synchronization and cancellation of the otherwise dominant laser frequency noise. These sub-sample interpolation time shifts are dependent upon the inter-spacecraft range and will be measured using a pseudo-random noise ranging modulation upon the science laser. One limit to the ranging performance is mutual interference between the outgoing and incoming ranging signals upon each spacecraft. This paper reports on the demonstration of a noise cancellation algorithm which is shown to providing a factor of similar to 8 suppression of the mutual interference noise. Demonstration of the algorithm in an optical test bed showed an rms ranging error of 0.06 m, improved from 0.19 m in previous results, surpassing the 1 m RMS LISA specification and potentially improving the cancellation of laser frequency noise.
C1 [Sutton, Andrew J.; Shaddock, Daniel A.] Australian Natl Univ, Ctr Gravitat Phys, Canberra, ACT 0200, Australia.
[McKenzie, Kirk; Ware, Brent; de Vine, Glenn; Spero, Robert E.; Klipstein, W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Sutton, AJ (reprint author), Australian Natl Univ, Ctr Gravitat Phys, GPO Box 4, Canberra, ACT 0200, Australia.
EM andrew.sutton@anu.edu.au
RI Shaddock, Daniel/A-7534-2011
OI Shaddock, Daniel/0000-0002-6885-3494
NR 25
TC 4
Z9 4
U1 2
U2 12
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0264-9381
J9 CLASSICAL QUANT GRAV
JI Class. Quantum Gravity
PD APR 7
PY 2013
VL 30
IS 7
AR 075008
DI 10.1088/0264-9381/30/7/075008
PG 8
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA 107OK
UT WOS:000316227500008
ER
PT J
AU Aguilar, M
Alberti, G
Alpat, B
Alvino, A
Ambrosi, G
Andeen, K
Anderhub, H
Arruda, L
Azzarello, P
Bachlechner, A
Barao, F
Baret, B
Barrau, A
Barrin, L
Bartoloni, A
Basara, L
Basili, A
Batalha, L
Bates, J
Battiston, R
Bazo, J
Becker, R
Becker, U
Behlmann, M
Beischer, B
Berdugo, J
Berges, P
Bertucci, B
Bigongiari, G
Biland, A
Bindi, V
Bizzaglia, S
Boella, G
de Boer, W
Bollweg, K
Bolmont, J
Borgia, B
Borsini, S
Boschini, MJ
Boudoul, G
Bourquin, M
Brun, P
Buenerd, M
Burger, J
Burger, W
Cadoux, F
Cai, XD
Capell, M
Casadei, D
Casaus, J
Cascioli, V
Castellini, G
Cernuda, I
Cervelli, F
Chae, MJ
Chang, YH
Chen, AI
Chen, CR
Chen, H
Cheng, GM
Chen, HS
Cheng, L
Chernoplyiokov, N
Chikanian, A
Choumilov, E
Choutko, V
Chung, CH
Clark, C
Clavero, R
Coignet, G
Commichau, V
Consolandi, C
Contin, A
Corti, C
Dios, MTC
Coste, B
Crespo, D
Cui, Z
Dai, M
Delgado, C
Della Torre, S
Demirkoz, B
Dennett, P
Derome, L
Di Falco, S
Diao, XH
Diago, A
Djambazov, L
Diaz, C
von Doetinchem, P
Du, WJ
Dubois, JM
Duperay, R
Duranti, M
D'Urso, D
Egorov, A
Eline, A
Eppling, FJ
Eronen, T
van Es, J
Esser, H
Falvard, A
Fiandrini, E
Fiasson, A
Finch, E
Fisher, P
Flood, K
Foglio, R
Fohey, M
Fopp, S
Fouque, N
Galaktionov, Y
Gallilee, M
Gallin-Martel, L
Gallucci, G
Garcia, B
Garcia, J
Garcia-Lopez, R
Garcia-Tabares, L
Gargiulo, C
Gast, H
Gebauer, I
Gentile, S
Gervasi, M
Gillard, W
Giovacchini, F
Girard, L
Goglov, P
Gong, J
Goy-Henningsen, C
Grandi, D
Graziani, M
Grechko, A
Gross, A
Guerri, I
de la Guia, C
Guo, KH
Habiby, M
Haino, S
Hauler, F
He, ZH
Heil, M
Heilig, J
Hermel, R
Hofer, H
Huang, ZC
Hungerford, W
Incagli, M
Ionica, M
Jacholkowska, A
Jang, WY
Jinchi, H
Jongmanns, M
Journet, L
Jungermann, L
Karpinski, W
Kim, GN
Kim, KS
Kirn, T
Kossakowski, R
Koulemzine, A
Kounina, O
Kounine, A
Koutsenko, V
Krafczyk, MS
Laudi, E
Laurenti, G
Lauritzen, C
Lebedev, A
Lee, MW
Lee, SC
Leluc, C
Vargas, HL
Lepareur, V
Li, JQ
Li, Q
Li, TX
Li, W
Li, ZH
Lipari, P
Lin, CH
Liu, D
Liu, H
Lomtadze, T
Lu, YS
Lucidi, S
Lubelsmeyer, K
Luo, JZ
Lustermann, W
Lv, S
Madsen, J
Majka, R
Malinin, A
Mana, C
Marin, J
Martin, T
Martinez, G
Masciocchi, F
Masi, N
Maurin, D
McInturff, A
McIntyre, P
Menchaca-Rocha, A
Meng, Q
Menichelli, M
Mereu, I
Millinger, M
Mo, DC
Molina, M
Mott, P
Mujunen, A
Natale, S
Nemeth, P
Ni, JQ
Nikonov, N
Nozzoli, F
Nunes, P
Obermeier, A
Oh, S
Oliva, A
Palmonari, F
Palomares, C
Paniccia, M
Papi, A
Park, WH
Pauluzzi, M
Pauss, F
Pauw, A
Pedreschi, E
Pensotti, S
Pereira, R
Perrin, E
Pessina, G
Pierschel, G
Pilo, F
Piluso, A
Pizzolotto, C
Plyaskin, V
Pochon, J
Pohl, M
Poireau, V
Porter, S
Pouxe, J
Putze, A
Quadrani, L
Qi, XN
Rancoita, PG
Rapin, D
Ren, ZL
Ricol, JS
Riihonen, E
Rodriguez, I
Roeser, U
Rosier-Lees, S
Rossi, L
Rozhkov, A
Rozza, D
Sabellek, A
Sagdeev, R
Sandweiss, J
Santos, B
Saouter, P
Sarchioni, M
Schael, S
Schinzel, D
Schmanau, M
Schwering, G
von Dratzig, AS
Scolieri, G
Seo, ES
Shan, BS
Shi, JY
Shi, YM
Siedenburg, T
Siedling, R
Son, D
Spada, F
Spinella, F
Steuer, M
Stiff, K
Sun, W
Sun, WH
Sun, XH
Tacconi, M
Tang, CP
Tang, XW
Tang, ZC
Tao, L
Tassan-Viol, J
Ting, SCC
Ting, SM
Titus, C
Tomassetti, N
Toral, F
Torsti, J
Tsai, JR
Tutt, JC
Ulbricht, J
Urban, T
Vagelli, V
Valente, E
Vannini, C
Valtonen, E
Trevino, MV
Vaurynovich, S
Vecchi, M
Vergain, M
Verlaat, B
Vescovi, C
Vialle, JP
Viertel, G
Volpini, G
Wang, D
Wang, NH
Wang, QL
Wang, RS
Wang, X
Wang, ZX
Wallraff, W
Weng, ZL
Willenbrock, M
Wlochal, M
Wu, H
Wu, KY
Wu, ZS
Xiao, WJ
Xie, S
Xiong, RQ
Xin, GM
Xu, NS
Xu, W
Yan, Q
Yang, J
Yang, M
Ye, QH
Yi, H
Yu, YJ
Yu, ZQ
Zeissler, S
Zhang, JG
Zhang, Z
Zhang, MM
Zheng, ZM
Zhuang, HL
Zhukov, V
Zichichi, A
Zuccon, P
Zurbach, C
AF Aguilar, M.
Alberti, G.
Alpat, B.
Alvino, A.
Ambrosi, G.
Andeen, K.
Anderhub, H.
Arruda, L.
Azzarello, P.
Bachlechner, A.
Barao, F.
Baret, B.
Barrau, A.
Barrin, L.
Bartoloni, A.
Basara, L.
Basili, A.
Batalha, L.
Bates, J.
Battiston, R.
Bazo, J.
Becker, R.
Becker, U.
Behlmann, M.
Beischer, B.
Berdugo, J.
Berges, P.
Bertucci, B.
Bigongiari, G.
Biland, A.
Bindi, V.
Bizzaglia, S.
Boella, G.
de Boer, W.
Bollweg, K.
Bolmont, J.
Borgia, B.
Borsini, S.
Boschini, M. J.
Boudoul, G.
Bourquin, M.
Brun, P.
Buenerd, M.
Burger, J.
Burger, W.
Cadoux, F.
Cai, X. D.
Capell, M.
Casadei, D.
Casaus, J.
Cascioli, V.
Castellini, G.
Cernuda, I.
Cervelli, F.
Chae, M. J.
Chang, Y. H.
Chen, A. I.
Chen, C. R.
Chen, H.
Cheng, G. M.
Chen, H. S.
Cheng, L.
Chernoplyiokov, N.
Chikanian, A.
Choumilov, E.
Choutko, V.
Chung, C. H.
Clark, C.
Clavero, R.
Coignet, G.
Commichau, V.
Consolandi, C.
Contin, A.
Corti, C.
Dios, M. T. Costado
Coste, B.
Crespo, D.
Cui, Z.
Dai, M.
Delgado, C.
Della Torre, S.
Demirkoz, B.
Dennett, P.
Derome, L.
Di Falco, S.
Diao, X. H.
Diago, A.
Djambazov, L.
Diaz, C.
von Doetinchem, P.
Du, W. J.
Dubois, J. M.
Duperay, R.
Duranti, M.
D'Urso, D.
Egorov, A.
Eline, A.
Eppling, F. J.
Eronen, T.
van Es, J.
Esser, H.
Falvard, A.
Fiandrini, E.
Fiasson, A.
Finch, E.
Fisher, P.
Flood, K.
Foglio, R.
Fohey, M.
Fopp, S.
Fouque, N.
Galaktionov, Y.
Gallilee, M.
Gallin-Martel, L.
Gallucci, G.
Garcia, B.
Garcia, J.
Garcia-Lopez, R.
Garcia-Tabares, L.
Gargiulo, C.
Gast, H.
Gebauer, I.
Gentile, S.
Gervasi, M.
Gillard, W.
Giovacchini, F.
Girard, L.
Goglov, P.
Gong, J.
Goy-Henningsen, C.
Grandi, D.
Graziani, M.
Grechko, A.
Gross, A.
Guerri, I.
de la Guia, C.
Guo, K. H.
Habiby, M.
Haino, S.
Hauler, F.
He, Z. H.
Heil, M.
Heilig, J.
Hermel, R.
Hofer, H.
Huang, Z. C.
Hungerford, W.
Incagli, M.
Ionica, M.
Jacholkowska, A.
Jang, W. Y.
Jinchi, H.
Jongmanns, M.
Journet, L.
Jungermann, L.
Karpinski, W.
Kim, G. N.
Kim, K. S.
Kirn, Th.
Kossakowski, R.
Koulemzine, A.
Kounina, O.
Kounine, A.
Koutsenko, V.
Krafczyk, M. S.
Laudi, E.
Laurenti, G.
Lauritzen, C.
Lebedev, A.
Lee, M. W.
Lee, S. C.
Leluc, C.
Vargas, H. Leon
Lepareur, V.
Li, J. Q.
Li, Q.
Li, T. X.
Li, W.
Li, Z. H.
Lipari, P.
Lin, C. H.
Liu, D.
Liu, H.
Lomtadze, T.
Lu, Y. S.
Lucidi, S.
Luebelsmeyer, K.
Luo, J. Z.
Lustermann, W.
Lv, S.
Madsen, J.
Majka, R.
Malinin, A.
Mana, C.
Marin, J.
Martin, T.
Martinez, G.
Masciocchi, F.
Masi, N.
Maurin, D.
McInturff, A.
McIntyre, P.
Menchaca-Rocha, A.
Meng, Q.
Menichelli, M.
Mereu, I.
Millinger, M.
Mo, D. C.
Molina, M.
Mott, P.
Mujunen, A.
Natale, S.
Nemeth, P.
Ni, J. Q.
Nikonov, N.
Nozzoli, F.
Nunes, P.
Obermeier, A.
Oh, S.
Oliva, A.
Palmonari, F.
Palomares, C.
Paniccia, M.
Papi, A.
Park, W. H.
Pauluzzi, M.
Pauss, F.
Pauw, A.
Pedreschi, E.
Pensotti, S.
Pereira, R.
Perrin, E.
Pessina, G.
Pierschel, G.
Pilo, F.
Piluso, A.
Pizzolotto, C.
Plyaskin, V.
Pochon, J.
Pohl, M.
Poireau, V.
Porter, S.
Pouxe, J.
Putze, A.
Quadrani, L.
Qi, X. N.
Rancoita, P. G.
Rapin, D.
Ren, Z. L.
Ricol, J. S.
Riihonen, E.
Rodriguez, I.
Roeser, U.
Rosier-Lees, S.
Rossi, L.
Rozhkov, A.
Rozza, D.
Sabellek, A.
Sagdeev, R.
Sandweiss, J.
Santos, B.
Saouter, P.
Sarchioni, M.
Schael, S.
Schinzel, D.
Schmanau, M.
Schwering, G.
von Dratzig, A. Schulz
Scolieri, G.
Seo, E. S.
Shan, B. S.
Shi, J. Y.
Shi, Y. M.
Siedenburg, T.
Siedling, R.
Son, D.
Spada, F.
Spinella, F.
Steuer, M.
Stiff, K.
Sun, W.
Sun, W. H.
Sun, X. H.
Tacconi, M.
Tang, C. P.
Tang, X. W.
Tang, Z. C.
Tao, L.
Tassan-Viol, J.
Ting, Samuel C. C.
Ting, S. M.
Titus, C.
Tomassetti, N.
Toral, F.
Torsti, J.
Tsai, J. R.
Tutt, J. C.
Ulbricht, J.
Urban, T.
Vagelli, V.
Valente, E.
Vannini, C.
Valtonen, E.
Trevino, M. Vargas
Vaurynovich, S.
Vecchi, M.
Vergain, M.
Verlaat, B.
Vescovi, C.
Vialle, J. P.
Viertel, G.
Volpini, G.
Wang, D.
Wang, N. H.
Wang, Q. L.
Wang, R. S.
Wang, X.
Wang, Z. X.
Wallraff, W.
Weng, Z. L.
Willenbrock, M.
Wlochal, M.
Wu, H.
Wu, K. Y.
Wu, Z. S.
Xiao, W. J.
Xie, S.
Xiong, R. Q.
Xin, G. M.
Xu, N. S.
Xu, W.
Yan, Q.
Yang, J.
Yang, M.
Ye, Q. H.
Yi, H.
Yu, Y. J.
Yu, Z. Q.
Zeissler, S.
Zhang, J. G.
Zhang, Z.
Zhang, M. M.
Zheng, Z. M.
Zhuang, H. L.
Zhukov, V.
Zichichi, A.
Zuccon, P.
Zurbach, C.
CA AMS Collaboration
TI First Result from the Alpha Magnetic Spectrometer on the International
Space Station: Precision Measurement of the Positron Fraction in Primary
Cosmic Rays of 0.5-350 GeV
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID AMS RICH DETECTOR; TIME-OF-FLIGHT; FAST TRIGGER; IDENTIFICATION;
PROTOTYPE; ELECTRONS; EARTH; TRD
AB A precision measurement by the Alpha Magnetic Spectrometer on the International Space Station of the positron fraction in primary cosmic rays in the energy range from 0.5 to 350 GeV based on 6.8 x 10(6) positron and electron events is presented. The very accurate data show that the positron fraction is steadily increasing from 10 to similar to 250 GeV, but, from 20 to 250 GeV, the slope decreases by an order of magnitude. The positron fraction spectrum shows no fine structure, and the positron to electron ratio shows no observable anisotropy. Together, these features show the existence of new physical phenomena. DOI: 10.1103/PhysRevLett.110.141102
C1 [Basili, A.; Becker, R.; Becker, U.; Behlmann, M.; Berges, P.; Burger, J.; Cai, X. D.; Capell, M.; Chen, A. I.; Chen, H.; Choumilov, E.; Choutko, V.; Dennett, P.; Egorov, A.; Eline, A.; Eppling, F. J.; Fisher, P.; Flood, K.; Galaktionov, Y.; Gallilee, M.; Gargiulo, C.; Goglov, P.; Hungerford, W.; Incagli, M.; Koulemzine, A.; Kounina, O.; Kounine, A.; Koutsenko, V.; Krafczyk, M. S.; Lebedev, A.; Plyaskin, V.; Rozhkov, A.; Schinzel, D.; Steuer, M.; Sun, W.; Ting, Samuel C. C.; Ting, S. M.; Titus, C.; Vaurynovich, S.; Vergain, M.; Wang, X.; Willenbrock, M.; Zuccon, P.] Rhein Westfal TH Aachen, Phys Inst B, D-52056 Aachen, Germany.
[Madsen, J.] Univ Aarhus, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Verlaat, B.] NIKHEF, Natl Inst Nucl Phys & High Energy Phys, NL-1098 SJ Amsterdam, Netherlands.
[Demirkoz, B.] Middle E Tech Univ, Dept Phys, TR-06800 Ankara, Turkey.
[Basara, L.; Brun, P.; Cadoux, F.; Coignet, G.; Dubois, J. M.; Fiasson, A.; Fouque, N.; Girard, L.; Goy-Henningsen, C.; Hermel, R.; Journet, L.; Kossakowski, R.; Lepareur, V.; Paniccia, M.; Pochon, J.; Poireau, V.; Rosier-Lees, S.; Tao, L.; Tassan-Viol, J.; Vialle, J. P.] CNRS, LAPP, IN2P3, Lab Annecy Le Vieux Phys Particules, F-74941 Annecy Le Vieux, France.
[Basara, L.; Brun, P.; Cadoux, F.; Coignet, G.; Dubois, J. M.; Fiasson, A.; Fouque, N.; Girard, L.; Goy-Henningsen, C.; Hermel, R.; Journet, L.; Kossakowski, R.; Lepareur, V.; Paniccia, M.; Pochon, J.; Poireau, V.; Rosier-Lees, S.; Tao, L.; Tassan-Viol, J.; Vialle, J. P.] Univ Savoie, F-74941 Annecy Le Vieux, France.
[Li, W.; Shan, B. S.; Wu, K. Y.; Zheng, Z. M.] Beihang Univ, BUAA, Beijing 100191, Peoples R China.
[Dai, M.; Wang, Q. L.; Yu, Y. J.] Chinese Acad Sci, Inst Elect Engn, IEE, Beijing 100080, Peoples R China.
[Cheng, G. M.; Chen, H. S.; Li, Z. H.; Lu, Y. S.; Tang, X. W.; Tang, Z. C.; Xu, W.; Yan, Q.; Yang, M.; Yu, Z. Q.; Zhuang, H. L.] Chinese Acad Sci, Inst High Energy Phys, IHEP, Beijing 100039, Peoples R China.
[Casadei, D.; Contin, A.; Laurenti, G.; Masi, N.; Palmonari, F.; Quadrani, L.; Zichichi, A.] INFN Sez Bologna, I-40126 Bologna, Italy.
[Casadei, D.; Contin, A.; Masi, N.; Palmonari, F.; Quadrani, L.; Zichichi, A.] Univ Bologna, I-40126 Bologna, Italy.
[Basili, A.; Becker, R.; Becker, U.; Behlmann, M.; Berges, P.; Burger, J.; Cai, X. D.; Capell, M.; Chen, A. I.; Chen, H.; Choumilov, E.; Choutko, V.; Dennett, P.; Egorov, A.; Eline, A.; Eppling, F. J.; Fisher, P.; Flood, K.; Galaktionov, Y.; Gallilee, M.; Gargiulo, C.; Goglov, P.; Hungerford, W.; Incagli, M.; Koulemzine, A.; Kounina, O.; Kounine, A.; Koutsenko, V.; Krafczyk, M. S.; Lebedev, A.; Plyaskin, V.; Rozhkov, A.; Schinzel, D.; Steuer, M.; Sun, W.; Ting, Samuel C. C.; Ting, S. M.; Titus, C.; Vaurynovich, S.; Vergain, M.; Wang, X.; Willenbrock, M.; Zuccon, P.] MIT, Cambridge, MA 02139 USA.
[Chang, Y. H.; Haino, S.; Vecchi, M.] Natl Cent Univ, Tao Yuan 32054, Taiwan.
[Sagdeev, R.] Univ Maryland, East West Ctr Space Sci, College Pk, MD 20742 USA.
[Malinin, A.; Seo, E. S.] Univ Maryland, IPST, College Pk, MD 20742 USA.
[McInturff, A.; McIntyre, P.; Stiff, K.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA.
[Jang, W. Y.; Kim, G. N.; Kim, K. S.; Lee, M. W.; Park, W. H.; Son, D.] Kyungpook Natl Univ, CHEP, Taegu 702701, South Korea.
[van Es, J.; Pauw, A.] NLR, Natl Aerosp Lab, NL-8300 AD Emmeloord, Netherlands.
[Castellini, G.] CNR IROE, I-50125 Florence, Italy.
[Nozzoli, F.; Pizzolotto, C.] ASDC ESRIN, I-00044 Frascati, Italy.
[Aguilar, M.; Barrin, L.; D'Urso, D.; Rossi, L.; Rozza, D.] CERN, European Org Nucl Res, CH-1211 Geneva 23, Switzerland.
[Azzarello, P.; Bourquin, M.; Cadoux, F.; Habiby, M.; Leluc, C.; Masciocchi, F.; Paniccia, M.; Perrin, E.; Pohl, M.; Rapin, D.; Saouter, P.] Univ Geneva, DPNC, CH-1211 Geneva 4, Switzerland.
[Baret, B.; Barrau, A.; Boudoul, G.; Buenerd, M.; Coste, B.; Derome, L.; Duperay, R.; Foglio, R.; Gallin-Martel, L.; Gillard, W.; Maurin, D.; Pouxe, J.; Ricol, J. S.; Trevino, M. Vargas; Vescovi, C.] CNRS, LPSC, IN2P3, F-38026 St Martin Dheres, France.
[Alvino, A.; Baret, B.; Barrau, A.; Boudoul, G.; Buenerd, M.; Coste, B.; Derome, L.; Duperay, R.; Foglio, R.; Gallin-Martel, L.; Gillard, W.; Maurin, D.; Pouxe, J.; Ricol, J. S.; Trevino, M. Vargas; Vescovi, C.] Univ Grenoble 1, Grenoble INP, F-38026 Grenoble, France.
[Diao, X. H.; Guo, K. H.; He, Z. H.; Huang, Z. C.; Li, T. X.; Lv, S.; Mo, D. C.; Ni, J. Q.; Qi, X. N.; Sun, X. H.; Tang, C. P.; Wang, Z. X.; Weng, Z. L.; Wu, Z. S.; Xiao, W. J.; Xu, N. S.; Zhang, Z.; Zhang, M. M.] Sun Yat Sen Univ, Guangzhou 510275, Peoples R China.
[Bindi, V.; Consolandi, C.; Corti, C.] Univ Hawaii, Dept Phys & Astron, Honolulu, HI 96822 USA.
[Bates, J.; Bollweg, K.; Clark, C.; Fohey, M.; Heilig, J.; Hungerford, W.; Lauritzen, C.; Martin, T.; Mott, P.; Nemeth, P.; Porter, S.; Tutt, J. C.; Urban, T.] NASA, Johnson Space Ctr, JSC, Houston, TX 77058 USA.
[Bates, J.; Bollweg, K.; Clark, C.; Fohey, M.; Heilig, J.; Hungerford, W.; Lauritzen, C.; Martin, T.; Mott, P.; Nemeth, P.; Porter, S.; Tutt, J. C.; Urban, T.] Jacobs Sverdrup, Houston, TX 77058 USA.
[Chen, C. R.; Tsai, J. R.; Wang, D.] Natl Space Org, Hsinchu 300, Taiwan.
[Mujunen, A.] Aalto Univ, Metsahovi Radio Observ, FIN-02540 Kylmala, Finland.
[Andeen, K.; de Boer, W.; Gebauer, I.; Hauler, F.; Heil, M.; Jungermann, L.; Nikonov, N.; Obermeier, A.; Sabellek, A.; Schmanau, M.; Vagelli, V.; Zeissler, S.] Karlsruhe Inst Technol, Inst Expt Kernphys, D-76128 Karlsruhe, Germany.
[Clavero, R.; Dios, M. T. Costado; Diago, A.; Garcia-Lopez, R.; Pochon, J.] Inst Astrofis Canarias, E-38205 Tenerife, Spain.
[Arruda, L.; Barao, F.; Batalha, L.; Nunes, P.; Pereira, R.; Santos, B.] LIP, Lab Instrumentacao & Fis Expt Particulas, P-1000 Lisbon, Portugal.
[Jinchi, H.] Chung Shan Inst Sci & Technol, Tao Yuan 325, Taiwan.
[Aguilar, M.; Berdugo, J.; Casaus, J.; Cernuda, I.; Crespo, D.; Delgado, C.; Diaz, C.; Garcia, B.; Garcia, J.; Garcia-Tabares, L.; Giovacchini, F.; de la Guia, C.; Mana, C.; Marin, J.; Martinez, G.; Oliva, A.; Palomares, C.; Rodriguez, I.; Toral, F.] CIEMAT, Ctr Invest Energet Medioambientales & Tecnol, E-28040 Madrid, Spain.
[Vargas, H. Leon; Menchaca-Rocha, A.] Univ Nacl Autonoma Mexico, Inst Fis, Mexico City 01000, DF, Mexico.
[Volpini, G.] INFN Sez Milano, I-20090 Milan, Italy.
[Rossi, L.; Volpini, G.] Univ Milan, I-20090 Milan, Italy.
[Boella, G.; Boschini, M. J.; Consolandi, C.; Della Torre, S.; Gervasi, M.; Grandi, D.; Pensotti, S.; Pessina, G.; Rancoita, P. G.; Rozza, D.; Tacconi, M.] INFN Sez Milano Bicocca, I-20126 Milan, Italy.
[Boella, G.; Della Torre, S.; Gervasi, M.; Pensotti, S.; Pessina, G.; Rozza, D.; Tacconi, M.] Univ Milano Bicocca, I-20126 Milan, Italy.
[Bolmont, J.; Falvard, A.; Jacholkowska, A.; Zurbach, C.] CNRS, IN2P3, LUPM Ex LPTA, Lab Univ & Particules Montpellier, F-34095 Montpellier, France.
[Bolmont, J.; Falvard, A.; Jacholkowska, A.; Zurbach, C.] Univ Montpellier 2, F-34095 Montpellier, France.
[Chernoplyiokov, N.; Grechko, A.] Russian Res Ctr, Kurchatov Inst, Moscow 123182, Russia.
[Gong, J.; Li, J. Q.; Li, Q.; Liu, H.; Luo, J. Z.; Meng, Q.; Shi, J. Y.; Sun, W. H.; Wu, H.; Xiong, R. Q.; Yi, H.; Zhang, J. G.] Southeast Univ, SEU, Nanjing 210096, Jiangsu, Peoples R China.
[Chikanian, A.; Finch, E.; Majka, R.; Sandweiss, J.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Alberti, G.; Alpat, B.; Alvino, A.; Ambrosi, G.; Azzarello, P.; Battiston, R.; Bazo, J.; Bertucci, B.; Bizzaglia, S.; Borsini, S.; Cascioli, V.; Duranti, M.; D'Urso, D.; Fiandrini, E.; Graziani, M.; Haino, S.; Ionica, M.; Laudi, E.; Lucidi, S.; Menichelli, M.; Mereu, I.; Nozzoli, F.; Oliva, A.; Papi, A.; Pauluzzi, M.; Piluso, A.; Pizzolotto, C.; Sarchioni, M.; Scolieri, G.; Tomassetti, N.; Zuccon, P.] INFN Sez Perugia, I-06100 Perugia, Italy.
[Alberti, G.; Alvino, A.; Battiston, R.; Bertucci, B.; Borsini, S.; Burger, W.; Cascioli, V.; Duranti, M.; Fiandrini, E.; Graziani, M.; Ionica, M.; Laudi, E.; Mereu, I.; Oliva, A.; Pauluzzi, M.; Piluso, A.; Tomassetti, N.] Univ Perugia, I-06100 Perugia, Italy.
[Bigongiari, G.; Cervelli, F.; Di Falco, S.; Gallucci, G.; Guerri, I.; Incagli, M.; Lomtadze, T.; Pedreschi, E.; Pilo, F.; Spinella, F.; Vannini, C.] INFN Sez Pisa, I-56100 Pisa, Italy.
[Bigongiari, G.; Guerri, I.] Univ Pisa, I-56100 Pisa, Italy.
[Battiston, R.] INFN TIFPA, I-38123 Povo, Trento, Italy.
[Battiston, R.] Univ Trent, I-38123 Povo, Trento, Italy.
[Bartoloni, A.; Borgia, B.; Gargiulo, C.; Gentile, S.; Lipari, P.; Spada, F.; Valente, E.] INFN Sez Roma 1, I-00185 Rome, Italy.
[Borgia, B.; Gentile, S.] Univ Roma La Sapienza, I-00185 Rome, Italy.
[Chae, M. J.; Oh, S.; Yang, J.] Ewha Womans Univ, Dept Phys, Seoul 120750, South Korea.
[Cheng, L.; Cui, Z.; Du, W. J.; Wang, N. H.; Xin, G. M.] Shandong Univ, SDU, Jinan 51, Shandong, Peoples R China.
[Shi, Y. M.; Wang, R. S.; Xie, S.; Ye, Q. H.] Shanghai Jiao Tong Univ, SJTU, Shanghai 200030, Peoples R China.
[Lee, S. C.; Lin, C. H.; Liu, D.; Natale, S.; Ren, Z. L.; Weng, Z. L.; Wu, K. Y.] Acad Sinica, Inst Phys, Taipei 11529, Taiwan.
[Eronen, T.; Riihonen, E.; Torsti, J.; Valtonen, E.] Univ Turku, Dept Phys, Space Res Lab, FIN-20014 Turku, Finland.
[Anderhub, H.; Biland, A.; Commichau, V.; Djambazov, L.; Hofer, H.; Jongmanns, M.; Lustermann, W.; Pauss, F.; Roeser, U.; Ulbricht, J.; Viertel, G.] ETH, Inst Particle Phys, CH-8093 Zurich, Switzerland.
RP Aguilar, M (reprint author), CIEMAT, Ctr Invest Energet Medioambientales & Tecnol, E-28040 Madrid, Spain.
RI Zuccon, Paolo/I-7736-2012; Ye, Qinghao/O-5630-2015; Palomares,
Carmen/H-7783-2015; Duranti, Matteo/I-7691-2013; Tomassetti,
Nicola/K-2380-2016; Masi, Nicolo/G-7911-2016; Pizzolotto,
Cecilia/G-5821-2013; Barao, Fernando/O-2357-2016; Paniccia,
Mercedes/A-4519-2017; alpat, ali behcet/G-6290-2013; Delgado,
Carlos/K-7587-2014; Rancoita, Pier Giorgio/J-9896-2015; Fiandrini,
Emanuele/C-4549-2008; bertucci, bruna/J-5237-2012; Casadei,
Diego/I-1785-2013; Zhukov, Valery/K-3615-2013; Arruda,
Luisa/I-2403-2013; Vecchi, Manuela/J-9180-2014; Martinez Botella,
Gustavo/K-8834-2014; Marin, Jesus/K-6991-2014; Berdugo,
Javier/A-2858-2015; Demirkoz, Bilge/C-8179-2014;
OI Zuccon, Paolo/0000-0002-2728-0167; Palomares,
Carmen/0000-0003-4374-9065; Duranti, Matteo/0000-0003-0980-6425;
Tomassetti, Nicola/0000-0002-0856-9299; Masi,
Nicolo/0000-0002-3729-7608; Pizzolotto, Cecilia/0000-0003-0200-2408;
Barao, Fernando/0000-0002-8346-9941; Paniccia,
Mercedes/0000-0001-8482-2703; alpat, ali behcet/0000-0002-0116-1506;
Delgado, Carlos/0000-0002-7014-4101; Rancoita, Pier
Giorgio/0000-0002-1990-4283; Arruda, Luisa/0000-0001-6720-6933; Martinez
Botella, Gustavo/0000-0002-1061-8520; Marin, Jesus/0000-0002-9049-3667;
Berdugo, Javier/0000-0002-7911-8532; Della Torre,
Stefano/0000-0002-7669-0859; Seo, Eun-Suk/0000-0001-8682-805X; Casadei,
Diego/0000-0002-3343-3529; Vagelli, Valerio/0000-0002-4495-9331; Basara,
Laurent/0000-0002-5726-9954; PAPI, ALBERTO/0000-0002-6924-4500; Corti,
Claudio/0000-0001-9127-7133; Bertucci, Bruna/0000-0001-7584-293X;
Graziani, Maura/0000-0001-7570-2048; Pessina, Gianluigi
Ezio/0000-0003-3700-9757; Tacconi, Mauro/0000-0002-9344-6305; Nozzoli,
Francesco/0000-0002-4355-7947; Ambrosi, Giovanni/0000-0001-6977-9559;
Castellini, Guido/0000-0002-0177-0643; Rozza,
Davide/0000-0002-7378-6353; Bigongiari, Gabriele/0000-0003-3691-0826;
GILLARD, William/0000-0003-4744-9748; Quadrani,
Lucio/0000-0003-4830-0259; Gallucci, Giovanni/0000-0003-3554-9733
FU U.S. DOE; CERN; Deutsches Zentrum fur Luft- und Raumfahrt, DLR; National
Natural Science Foundation of China; Italian Space Agency, ASI; SEIDI;
CPAN
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 current and former NASA leadership including Charles
Bolden, Lori Garver, William Gerstenmeier, George Abbey, Franklin
Chang-Diaz, and Mark Sistilli, and we thank the crew of STS-134: Mark
Kelly, Greg Johnson, Greg Chamitoff, Drew Feustel, Mike Fincke, and
Roberto Vittori. AMS is a U.S. DOE sponsored international
collaboration. We are grateful for the support of Jim Siegrist, Michael
Salamon, Dennis Kovar, Robin Staffin, Saul Gonzalez, and John O'Fallon.
We also acknowledge the continuous support from MIT, beginning with
former President Charles M. Vest, and its School of Science, Marc
Kastner, Robert Silbey, Robert Birgeneau, Ernest Moniz, Edmund
Bertschinger, and Richard Milner. We acknowledge support from CAS, NNSF,
MOST, NLAA, and the Provincial Governments of Shandong, Jiangsu, and
Guandong, China; CNRS, IN2P3, CNES, Enigmass, and the ANR, France, and
Bernard Accoyer, former President of the French National Assembly; DLR,
the Julich Supercomputing Center, P. Hintze, J. Trumper, and J. D.
Woerner, Germany; INFN, ASI, E. Iarocci, R. Petronzio, F. Ferroni, S. De
Julio, S. Vetrella, G. Bignami, and E. Saggese, Italy; CIEMAT, CDTI,
SEIDI-MINECO, and CPAN, Spain; the Swiss National Science Foundation
(SNSF), federal and cantonal authorities, Switzerland; and Academia
Sinica and the National Science Council (NSC), former President of
Academia Sinica Yuan-Tseh Lee and former Ministers of NSC Chien-Jen
Chen, Maw-Kuen Wu, and Luo-Chuan Lee, Taiwan. We gratefully acknowledge
the strong support from CERN: Rolf-Dieter Heuer, Robert Aymar, and
Luciano Maiani as well as Steve Meyers and Andrzej Siemko. From ESA, we
thank Jean-Jacques Dordain, Simona DiPippo, and Martin Zell for their
support. We are grateful for important discussions with Barry Barish,
Claude Canizares, James Cronin, Jonathan Ellis, Len Fisk, Sheldon
Glashow, Alan Guth, Neal Lane, Steve Olsen, Alvaro de Rujula, Alexander
Rumyantsev, Reinhard Simon, George Smoot, Jian Song, Evgeny Velikhov,
Steven Weinberg, Frank Wilczek, and Cunhao Zhang. Finally, we
acknowledge with appreciation the United States Congress for their
unanimous approval of HR6063 (2008) restoring AMS to the Space Shuttle
manifest and bringing major science to the ISS, and we are grateful for
the support of Joe Barton, Jeff Bingham, Gabrielle Giffords, John Glenn,
Ralph Hall, Kay Bailey Hutchison, Nick Lampson, Bill Nelson, and David
Vitter.; Supported by the Deutsches Zentrum fur Luft- und Raumfahrt,
DLR.; Supported by the National Natural Science Foundation of China.;
Also supported by the Italian Space Agency, ASI.; Also supported by
SEIDI and CPAN.
NR 53
TC 417
Z9 425
U1 29
U2 210
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD APR 3
PY 2013
VL 110
IS 14
AR 141102
DI 10.1103/PhysRevLett.110.141102
PG 10
WC Physics, Multidisciplinary
SC Physics
GA 119OJ
UT WOS:000317106800003
PM 25166975
ER
PT J
AU Kelly, BJ
Baker, JG
AF Kelly, Bernard J.
Baker, John G.
TI Decoding mode mixing in black-hole merger ringdown
SO PHYSICAL REVIEW D
LA English
DT Article
ID GRAVITATIONAL-WAVES; SPHERICAL-HARMONICS; GENERAL RELATIVITY; INITIAL
DATA; SPIN; PERTURBATIONS; TIME
AB Optimal extraction of information from gravitational-wave observations of binary black-hole coales-cences requires detailed knowledge of the waveforms. Current approaches for representing waveform information are based on spin-weighted spherical harmonic decomposition. Higher-order harmonic modes carrying a few percent of the total power output near merger can supply information critical to determining intrinsic and extrinsic parameters of the binary. One obstacle to constructing a full multimode template of merger waveforms is the apparently complicated behavior of some of these modes; instead of settling down to a simple quasinormal frequency with decaying amplitude, some vertical bar m vertical bar not equal l modes show periodic bumps characteristic of mode mixing. We analyze the strongest of these modes-the anomalous (3, 2) harmonic mode-measured in a set of binary black-hole merger waveform simulations, and show that to leading order, they are due to a mismatch between the spherical harmonic basis used for extraction in 3D numerical relativity simulations, and the spheroidal harmonics adapted to the perturbation theory of Kerr black holes. Other causes of mode mixing arising from gauge ambiguities and physical properties of the quasinormal ringdown modes are also considered and found to be small for the waveforms studied here. DOI:10.1103/PhysRevD.87.084004
C1 [Kelly, Bernard J.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Kelly, Bernard J.; Baker, John G.] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, Greenbelt, MD 20771 USA.
[Kelly, Bernard J.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
RP Kelly, BJ (reprint author), NASA, Goddard Space Flight Ctr, CRESST, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
OI Kelly, Bernard/0000-0002-3326-4454
FU NASA [09-ATP09-0136]
FX The new numerical evolutions performed for this paper were carried out
on the machine Pleiades at NASA's Ames Research Center. The work was
supported by NASA Grant No. 09-ATP09-0136. The authors would like to
thank Enrico Barausse, Emanuele Berti, Alessandra Buonanno, Rafael
Porto, Luciano Rezzolla, Jeremy Schnittman, and James van Meter for
useful comments.
NR 82
TC 6
Z9 6
U1 0
U2 3
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
J9 PHYS REV D
JI Phys. Rev. D
PD APR 2
PY 2013
VL 87
IS 8
AR 084004
DI 10.1103/PhysRevD.87.084004
PG 15
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 117LO
UT WOS:000316955100005
ER
PT J
AU Wu, CC
Gopalswamy, N
Lepping, RP
Yashiro, S
AF Wu, Chin-Chun
Gopalswamy, Natchimuthuk
Lepping, Ronld Paul
Yashiro, Seiji
TI Characteristics of Magnetic Clouds and Interplanetary Coronal Mass
Ejections which Cause Intense Geomagnetic Storms
SO TERRESTRIAL ATMOSPHERIC AND OCEANIC SCIENCES
LA English
DT Article
DE Magnetic cloud; Interplanetary coronal mass ejection; Geomagnetic storm;
Solar flare; Corotating interaction region
ID SOLAR; WIND; GEOEFFECTIVENESS; MAXIMUM; EVENTS; CYCLE; CMES
AB We present the results of a statistical data analysis of the geo-effectiveness of non-magnetic-cloud interplanetary coronal mass ejections (ICMEs) and compare them with those of magnetic-cloud (MC) interplanetary coronal mass ejections observed during solar cycle 23. (The term ICME as used here will refer to a non-MC ICME.) The starting point of this investigation is the set of intense geomagnetic storms (Dst(min) <= -100 nT) of solar cycle 23 between 1996 and 2005. We also compare the solar source locations of the ICMEs with those of the MCs. The source locations of the solar disturbances are, on average, closer to the Sun-Earth line for the MCs than for the ICMEs. There is an anomaly for the location of the related solar sources: no event came from the region between the solar equator plane and 10 degrees S (south) of that plane. The primary results are listed as follows. The average duration of these MCs is slightly longer (similar to 7%) than that of ICMEs. The average geomagnetic storm intensity for the MCs is higher than that for the ICMEs and CIRs formed by high-speed streams from coronal holes, especially for the events associated with X class flares. The relevant average magnetic field component, i.e., vertical bar Bz(min) vertical bar, is more intense within the MCs than within the ICMEs. The average solar wind speed is similar for both MCs and ICMEs. Maximum solar wind speed is higher within ICMEs than within MCs. Maximum solar wind proton density is higher for MCs than for ICMEs.
C1 [Wu, Chin-Chun] Naval Res Lab, Washington, DC USA.
[Gopalswamy, Natchimuthuk; Yashiro, Seiji] NASA GSFC, Solar Syst Explorat Div, Solar Phys Lab, Greenbelt, MD USA.
[Lepping, Ronld Paul] NASA GSFC, Heliosphys Sci Div, Greenbelt, MD USA.
[Yashiro, Seiji] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Wu, CC (reprint author), Naval Res Lab, Washington, DC USA.
EM chin-chun.wu@nrl.navy.mil
FU NASA's LWS program [NNH09AM46I]; NRL 6.1 program
FX We thank the Wind SWE and MFI teams and the National Space Science Data
Center at Goddard Space Flight Center for Wind data management and for
providing the Wind solar wind plasma and magnetic field data, and the
team at Kyoto University, Kyoto, Japan for providing the Dst data. This
study is supported partially by NASA's LWS program via grants NNH09AM46I
(CCW and RPL), and NRL 6.1 program (CCW).
NR 31
TC 7
Z9 7
U1 0
U2 4
PU CHINESE GEOSCIENCE UNION
PI TAIPEI
PA PO BOX 23-59, TAIPEI 10764, TAIWAN
SN 1017-0839
J9 TERR ATMOS OCEAN SCI
JI Terr. Atmos. Ocean. Sci.
PD APR
PY 2013
VL 24
IS 2
SI SI
BP 233
EP 241
DI 10.3319/TAO.2012.09.26.03(SEC)
PG 9
WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences;
Oceanography
SC Geology; Meteorology & Atmospheric Sciences; Oceanography
GA 292IC
UT WOS:000329894400009
ER
PT J
AU Gao, HY
Wang, ZJ
Huynh, HT
AF Gao, Haiyang
Wang, Z. J.
Huynh, H. T.
TI Differential Formulation of Discontinuous Galerkin and Related Methods
for the Navier-Stokes Equations
SO COMMUNICATIONS IN COMPUTATIONAL PHYSICS
LA English
DT Article
DE Discontinuous Galerkin; lifting collocation penalty; flux
reconstruction; Navier-Stokes equations; correction procedure via
reconstruction; unstructured hybrid grids
ID FINITE-ELEMENT-METHOD; ONE-DIMENSIONAL SYSTEMS; CONSERVATION-LAWS;
UNSTRUCTURED GRIDS; VOLUME METHOD; NUMERICAL-SOLUTION; BASIC
FORMULATION; EULER
AB A new approach to high-order accuracy for the numerical solution of conservation laws introduced by Huynh and extended to simplexes by Wang and Gao is renamed CPR (correction procedure or collocation penalty via reconstruction). The CPR approach employs the differential form of the equation and accounts for the jumps in flux values at the cell boundaries by a correction procedure. In addition to being simple and economical, it unifies several existing methods including discontinuous Galerkin, staggered grid, spectral volume, and spectral difference. To discretize the diffusion terms, we use the BR2 (Bassi and Rebay), interior penalty, compact DG (CDG), and I-continuous approaches. The first three of these approaches, originally derived using the integral formulation, were recast here in the CPR framework, whereas the I-continuous scheme, originally derived for a quadrilateral mesh, was extended to a triangular mesh. Fourier stability and accuracy analyses for these schemes on quadrilateral and triangular meshes are carried out. Finally, results for the Navier-Stokes equations are shown to compare the various schemes as well as to demonstrate the capability of the CPR approach.
C1 [Gao, Haiyang; Wang, Z. J.] Iowa State Univ, Dept Aerosp Engn, Ames, IA 50011 USA.
[Gao, Haiyang; Wang, Z. J.] Iowa State Univ, CFD Ctr, Ames, IA 50011 USA.
[Huynh, H. T.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Gao, HY (reprint author), Iowa State Univ, Dept Aerosp Engn, 2271 Howe Hall Ames, Ames, IA 50011 USA.
EM hgao@iastate.edu; zjw@iastate.edu; hung.t.huynh@nasa.gov
RI Wang, Z.J./A-9628-2010
OI Wang, Z.J./0000-0002-6203-6303
FU AFOSR [FA9550-06-1-0146]; NASA's Fundamental Aeronautics Program
FX The first two authors were funded by AFOSR grant FA9550-06-1-0146. The
third author is supported by NASA's Fundamental Aeronautics Program. The
views and conclusions contained herein are those of the authors and
should not be interpreted as necessarily representing the official
policies or endorsements, either expressed or implied, of AFOSR, NASA or
the U.S. Government.
NR 29
TC 8
Z9 8
U1 0
U2 7
PU GLOBAL SCIENCE PRESS
PI WANCHAI
PA ROOM 3208, CENTRAL PLAZA, 18 HARBOUR RD, WANCHAI, HONG KONG 00000,
PEOPLES R CHINA
SN 1815-2406
J9 COMMUN COMPUT PHYS
JI Commun. Comput. Phys.
PD APR
PY 2013
VL 13
IS 4
BP 1013
EP 1044
DI 10.4208/cicp.020611.090312a
PG 32
WC Physics, Mathematical
SC Physics
GA 186SN
UT WOS:000322065200004
ER
PT J
AU Schwalm, CR
Huntinzger, DN
Michalak, AM
Fisher, JB
Kimball, JS
Mueller, B
Zhang, K
Zhang, YQ
AF Schwalm, Christopher R.
Huntinzger, Deborah N.
Michalak, Anna M.
Fisher, Joshua B.
Kimball, John S.
Mueller, Brigitte
Zhang, Ke
Zhang, Yongqiang
TI Sensitivity of inferred climate model skill to evaluation decisions: a
case study using CMIP5 evapotranspiration
SO ENVIRONMENTAL RESEARCH LETTERS
LA English
DT Article
DE climate models; model validation; evapotranspiration; CMIP5
ID LAND-SURFACE MODELS; CARBON; BENCHMARK; WATER; AVHRR
AB Confrontation of climate models with observationally-based reference datasets is widespread and integral to model development. These comparisons yield skill metrics quantifying the mismatch between simulated and reference values and also involve analyst choices, or meta-parameters, in structuring the analysis. Here, we systematically vary five such meta-parameters (reference dataset, spatial resolution, regridding approach, land mask, and time period) in evaluating evapotranspiration (ET) from eight CMIP5 models in a factorial design that yields 68 700 intercomparisons. The results show that while model-data comparisons can provide some feedback on overall model performance, model ranks are ambiguous and inferred model skill and rank are highly sensitive to the choice of meta-parameters for all models. This suggests that model skill and rank are best represented probabilistically rather than as scalar values. For this case study, the choice of reference dataset is found to have a dominant influence on inferred model skill, even larger than the choice of model itself. This is primarily due to large differences between reference datasets, indicating that further work in developing a community-accepted standard ET reference dataset is crucial in order to decrease ambiguity in model skill.
C1 [Schwalm, Christopher R.; Huntinzger, Deborah N.] No Arizona Univ, Sch Earth Sci & Environm Sustainabil, Flagstaff, AZ 86011 USA.
[Huntinzger, Deborah N.] No Arizona Univ, Dept Civil Engn Construct Management & Environm E, Flagstaff, AZ 86011 USA.
[Michalak, Anna M.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA.
[Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kimball, John S.] Univ Montana, Flathead Lake Biol Stn, Div Biol Sci, Polson, MT 59860 USA.
[Mueller, Brigitte] ETH, Inst Atmospher & Climate Sci, CH-8092 Zurich, Switzerland.
[Zhang, Ke] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA.
[Zhang, Yongqiang] CSIRO Land & Water, Canberra, ACT, Australia.
RP Schwalm, CR (reprint author), No Arizona Univ, Sch Earth Sci & Environm Sustainabil, Flagstaff, AZ 86011 USA.
EM christopher.schwalm@nau.edu
RI Zhang, Yongqiang/C-5708-2008; Mueller, Brigitte/E-2594-2011; Zhang,
Ke/B-3227-2012;
OI Zhang, Yongqiang/0000-0002-3562-2323; Mueller,
Brigitte/0000-0003-1876-4722; Zhang, Ke/0000-0001-5288-9372; Fisher,
Joshua/0000-0003-4734-9085
FU National Aeronautics and Space Administration (NASA) [NNX10AG01A,
NNX12AK12G]
FX We acknowledge the World Climate Research Programme's Working Group on
Coupled Modelling, which is responsible for CMIP, and we thank the
climate modeling groups for producing and making available their model
output. For CMIP the US Department of Energy's Program for Climate Model
Diagnosis and Intercomparison provides coordinating support and led
development of software infrastructure in partnership with the Global
Organization for Earth System Science Portals. CRS, DNH, and AMM were
supported by the National Aeronautics and Space Administration (NASA)
under Grant No. NNX10AG01A 'The NACP Multi-Scale Synthesis and
Terrestrial Model Intercomparison Project (MsTMIP)'. CRS was also
supported by NASA Grant No. NNX12AK12G. JBF contributed to this paper at
the Jet Propulsion Laboratory, California Institute of Technology under
a contract with NASA.
NR 25
TC 16
Z9 16
U1 2
U2 20
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 APR-JUN
PY 2013
VL 8
IS 2
AR 024028
DI 10.1088/1748-9326/8/2/024028
PG 9
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 178DU
UT WOS:000321425100032
ER
PT J
AU Murthy, R
Stephanou, HE
Popa, DO
AF Murthy, Rakesh
Stephanou, Harry E.
Popa, Dan O.
TI AFAM: An Articulated Four Axes Microrobot for Nanoscale Applications
SO IEEE TRANSACTIONS ON AUTOMATION SCIENCE AND ENGINEERING
LA English
DT Article
DE Microassembly; microelectromechanical systems (MEMS); microrobot
ID ROBOTICS
AB This paper presents a microassembled robot called the Articulated Four Axes Microrobot (AFAM). Target application areas include micro and nano part manipulation and probing. The robot consists of a cantilever actuated along four axes: in-place X, Y and Y AW; out-of-plane pitch. The microrobot size spans a total volume of 3 mm x 1.5 mm x 1 mm (XYZ), and operates within a workspace envelope of 50 mu m x 50 mu m x 75 mu m (XYZ). This is by far the largest operating envelope of any micropositioner with nonplanar dexterity. As a result it can be classified as a new type of three-dimensional microrobot and a candidate for miniaturizing top-down assembly systems to dimensions under 1 cm(3). A key feature in this design is a cable-like microwire that transforms in-plane actuator displacement into out-of-plane pitch and yaw motion (via flexure joints). Finite-element analysis simulation followed by microfabrication and assembly processes developed to prototype the designs are described. The microrobot is designed to carry an AFM tip as the end effector and accomplish nanoindentation on a polymer surface. The tip attachment technique and nanoindentation experiments have also been described in this paper. Open loop precision has been characterized using a laser interferometer which measured an average resolution of 50 nm along XYZ, repeatability of 100 nm and accuracy of 500 nm. Experiments to determine microrobot reliability are also presented.
Note to Practitioners-Micro/nanosystems research and development incorporates a large variety of tools and processes in order to accomplish high precision fabrication, assembly, testing and characterization. A very common component in these tools is high precision positioning units (robots) that are a combination of linear and rotary subunits (stages). Their role is to position micro or nanocomponents, substrates or wafers in an accurately and repeatable manner. Current state-of-art positioners typically span few inches to many feet in size. Although they are able to deliver the required precision, range of motion, and dexterity, their size inhibits the merger of multiple units under a common platform leading to throughput limitations. This paper presents an attempt to develop a new class of miniaturized robots that span no more than a few cubic millimeters in size, while delivering a subset of the capabilities as traditional macroscale equivalents. The tradeoffs between robot size, stiffness, range of motion, dexterity, and precision is taken to a new level where the robots are no more than two or three orders of magnitude larger than the smallest parts being manufactured.
C1 [Murthy, Rakesh] Jet Prop Lab, Instrument Elect & Sensors Div, Nano & Micro Syst Grp, Passadena, CA 91109 USA.
[Stephanou, Harry E.; Popa, Dan O.] Univ Texas Arlington, Arlington, TX 76011 USA.
RP Murthy, R (reprint author), Jet Prop Lab, Instrument Elect & Sensors Div, Nano & Micro Syst Grp, Passadena, CA 91109 USA.
EM rakesh.murthy@jpl.nasa.gov; popa@arri.uta.edu
FU Office of Naval Research
FX This work was supported by the Office of Naval Research and carried out
at Automation and Robotics Research Institute, the University of Texas
at Arlington.
NR 21
TC 2
Z9 2
U1 5
U2 24
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1545-5955
J9 IEEE T AUTOM SCI ENG
JI IEEE Trans. Autom. Sci. Eng.
PD APR
PY 2013
VL 10
IS 2
BP 276
EP 284
DI 10.1109/TASE.2012.2217740
PG 9
WC Automation & Control Systems
SC Automation & Control Systems
GA 172IF
UT WOS:000320994500006
ER
PT J
AU Ostrikov, K
Neyts, EC
Meyyappan, M
AF Ostrikov, K.
Neyts, E. C.
Meyyappan, M.
TI Plasma nanoscience: from nano-solids in plasmas to nano-plasmas in
solids
SO ADVANCES IN PHYSICS
LA English
DT Review
DE nanoscale solid systems; self-organization; plasma-specific effects;
structural and functional properties; nano-plasmas
ID CHEMICAL-VAPOR-DEPOSITION; WALLED CARBON NANOTUBES; LOW-TEMPERATURE
GROWTH; INDUCTIVELY-COUPLED PLASMA; SURFACE LOSS PROBABILITIES;
METAL-OXIDE NANOWIRES; DIAMOND-LIKE CARBON; WARM DENSE MATTER; GRAPHENE
NANORIBBONS; SOLAR-CELLS
AB The unique plasma-specific features and physical phenomena in the organization of nanoscale soild-state systems in a broad range of elemental composition, structure, and dimensionality are critically reviewed. These effects lead to the possibility to localize and control energy and matter at nanoscales and to produce self-organized nano-solids with highly unusual and superior properties. A unifying conceptual framework based on the control of production, transport, and self-organization of precursor species is introduced and a variety of plasma-specific non-equilibrium and kinetics-driven phenomena across the many temporal and spatial scales is explained. When the plasma is localized to micrometer and nanometer dimensions, new emergent phenomena arise. The examples range from semiconducting quantum dots and nanowires, chirality control of single-walled carbon nanotubes, ultra-fine manipulation of graphenes, nano-diamond, and organic matter to nano-plasma effects and nano-plasmas of different states of matter.
C1 [Ostrikov, K.] CSIRO Mat Sci & Engn, Lindfield, NSW 2070, Australia.
[Neyts, E. C.] Univ Antwerp, Dept Chem, Res Grp PLASMANT, B-2610 Antwerp, Belgium.
[Meyyappan, M.] NASA Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Ostrikov, K (reprint author), CSIRO Mat Sci & Engn, POB 218, Lindfield, NSW 2070, Australia.
EM kostya.ostrikov@csiro.au
RI Neyts, Erik/H-4198-2012;
OI Neyts, Erik/0000-0002-3360-3196; Ostrikov, Kostya
(Ken)/0000-0001-8672-9297
FU Australian Research Council; CSIRO's Science Leadership Program; ARC
Future Fellowship
FX We sincerely thank many our colleagues for fruitful collaborations,
discussions, and critical comments with apologies of not being able to
mention by name due to limited space. We also thank all authors of
original figures for the permissions to reproduce. This work was
partially supported by the Australian Research Council and CSIRO's
Science Leadership Program. K. O. is grateful to the University of
Sydney (Australia) and Nanyang Technological University (Singapore) as
Host Organizations for his ARC Future Fellowship as well as Huazhong
University of Science and Technology (China), the University of
Technology Sydney (Australia), and the University of Wollongong
(Australia) for the visiting, adjunct, and honorary professor support.
We are particularly thankful to the anonymous referee for the insightful
discussion of states of matter and phase transitions at nanoscales. We
also thank every person who has ever contributed to the relevant areas
and apologize for not being able to include all these results, although
would certainly do that if that were physically possible.
NR 393
TC 279
Z9 284
U1 34
U2 284
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 0001-8732
EI 1460-6976
J9 ADV PHYS
JI Adv. Phys.
PD APR 1
PY 2013
VL 62
IS 2
BP 113
EP 224
DI 10.1080/00018732.2013.808047
PG 112
WC Physics, Condensed Matter
SC Physics
GA 171GQ
UT WOS:000320913600001
ER
PT J
AU Stoner, AW
Copeman, LA
Ottmar, ML
AF Stoner, Allan W.
Copeman, Louise A.
Ottmar, Michele L.
TI Molting, growth, and energetics of newly-settled blue king crab: Effects
of temperature and comparisons with red king crab
SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY
LA English
DT Article
DE Bioenergetics; Culture; Fatty acid; Growth; Lipid; Paralithodes
platypus; Temperature
ID PARALITHODES-PLATYPUS BRANDT; MOLECULAR-SPECIES COMPOSITION; FATTY-ACID
COMPOSITION; BERING-SEA; CLIMATE-CHANGE; LIPID-COMPOSITION;
EMBRYONIC-DEVELOPMENT; CALLINECTES-SAPIDUS; LITHODES-SANTOLLA; STOCK
ENHANCEMENT
AB Populations of blue king crab (BKC) (Paralithodes platypus Brandt, 1850) have declined in Alaskan waters over recent decades, and substantial effort is being made to rehabilitate the once important fishery with releases of hatchery-reared juveniles. However, little is known about the species' first year of post-settlement life. This study was conducted to evaluate how temperature mediates growth and energy allocation beginning with the first benthic instar (stage C1). Juvenile BKC were reared in four temperatures (1.5 to 12 degrees C) for a period of 60 days in low-density populations (150 crabs m(-2)) and 120 days in individual cultures. Growth rate increased rapidly up to 8 degrees C, and then leveled off. At 60 days, most of the crabs in 1.5 degrees C remained at stage C1, most in 4.5 degrees C were C2, and most in 8 degrees C were C3, while those in 12 degrees C were highly variable and ranged from C2 to C5. Growth records for individuals revealed an inverse exponential relationship between water temperature and intermolt period (up to 8 degrees C). A small decrease in molt increment at 12 degrees C resulted in crabs 6% smaller than those at 8 degrees C. Total lipid content increased with temperature in C2 BKC, but the response was variable and not significant in later stages. The proportion of storage class lipids (triacylglycerols) increased with an increase in temperature and polar lipids decreased. Concentrations of essential fatty acids were relatively constant over all temperature treatments, indicating that temperature and growth rate did not affect the biochemical condition of juvenile BKC. Survival rates of BKC (>95%) were similar across temperatures and were much higher than rates observed for red king crab (RKC) (Paralithodes camchaticus Tilesius 1815) (65-72%) in identical experiments. Growth rates of the two species were nearly identical up to 8 degrees C, but RKC grew faster than BKC at temperatures greater than 8 degrees C, with more molts resulting in larger individuals. Fatty acid (FA) signatures supported the lipid class data and showed that BKC had higher proportions of FA associated with energy storage while RKC had higher proportions of polyunsaturated FAs associated with membranes. These results indicate that BKC are the hardier species, and it shows little sign of cannibalism in culture (unlike RKC), but RKC grow faster at high temperature and are less vulnerable to warming climate. These data help to model temperature-dependent recruitment processes in the field and assist in the design of diets and hatchery conditions for production of seed stocks intended for field release. Published by Elsevier B.V.
C1 [Stoner, Allan W.; Ottmar, Michele L.] NOAA, Fisheries Behav Ecol Program, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Newport, OR 97365 USA.
[Copeman, Louise A.] Oregon State Univ, Hatfield Marine Sci Ctr, Cooperat Inst Marine Resources Studies, Newport, OR 97365 USA.
RP Stoner, AW (reprint author), NOAA, Fisheries Behav Ecol Program, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, 2030 S,Marine Sci Dr, Newport, OR 97365 USA.
EM allan.stoner@gmail.com
FU NOAA Aquaculture Program; Alaska Sea Grant College Program
FX This study was conducted as part of the AKCRRAB Program (Alaska King
Crab Research, Rehabilitation, and Biology) funded in part by the NOAA
Aquaculture Program and the Alaska Sea Grant College Program. Crabs were
provided by the Alutiiq Pride Shellfish Hatchery, Seward, AK, with
special thanks to B. Daly and J. Swingle who cultured the larvae for
this experiment. Assistance with apparatus and maintenance of the
cultures in Newport was provided by S. Haines, P. Iseri, and C. Danley.
A. Sremba assisted with the lipid and fatty acid analyses. Thanks also
to Drs. B. MacFarlane and S. Sogard for the long-term loan of the
Iatroscan TLC-FID system for lipid class analyses. B. Daly and T. Hurst
provided helpful reviews for the manuscript. [SS]
NR 73
TC 16
Z9 16
U1 3
U2 37
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 APR
PY 2013
VL 442
BP 10
EP 21
DI 10.1016/j.jembe.2013.02.002
PG 12
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 164QW
UT WOS:000320425600002
ER
PT J
AU Frey, A
Dutton, PH
Balazs, GH
AF Frey, Amy
Dutton, Peter H.
Balazs, George H.
TI Insights on the demography of cryptic nesting by green turtles (Chelonia
mydas) in the main Hawaiian Islands from genetic relatedness analysis
SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY
LA English
DT Article
DE Chelonia mydas; Founder event; Kinship; Microsatellite; Relatedness; Sea
turtles
ID MULTILOCUS GENOTYPE DATA; NATURAL-POPULATIONS; PARENTAGE ANALYSIS;
SIBSHIP INFERENCE; MARINE TURTLES; CONSERVATION; RECOVERY;
RECONSTRUCTION; MARKERS; ERRORS
AB Within the Hawaiian archipelago, green turtle nesting has occurred almost exclusively in the northwestern Hawaiian Islands, mainly at French Frigate Shoals (FFS), however an increase in occasional nesting has recently been observed on the main Hawaiian Islands (MHI). Due to logistical constraints, monitoring the nesting activity on the MHI has been limited to nest documentation. Without systematic tagging of the nesting females it is not clear how many are nesting here. We used mitochondrial (mt) DNA sequencing combined with nuclear (n) DNA analysis based on 14 microsatellite markers to infer the number of individual nesters. Genotypes were determined for 181 dead embryos and hatchlings salvaged from 71 nests laid on Maui, Molokai, Kauai, Lanai, and Oahu, along with those of 81 nesting females that were sampled on FFS. MtDNA results showed that 58% of the MHI clutches were laid by females with a relatively rare haplotype only reported in 16% of the FFS nesting population. Nuclear DNA results showed that nesting in the MHI might be attributed to a relatively small number of females that appear to be related to each other. We were able to reconstruct genotypes for nesting females from hatchling profiles and we estimate that 15 different females were responsible for clutches laid on the MHI. Taken together, the mtDNA and nDNA results suggest that the nesting population at the MHI may be the result of a few founders that originated from the FFS breeding population, possibly facilitated by captive rearing and release of FFS juveniles locally from Oahu. We suggest that this regional range expansion may buffer against the loss of current nesting sites at FFS due to sea level rise. Our results demonstrate the potential for genetic tools to be incorporated into population assessment, particularly in areas where access to reproductive females is difficult and population size is unknown. Published by Elsevier B.V.
C1 [Frey, Amy; Dutton, Peter H.] NOAA, Natl Marine Fisheries Serv, SW Fisheries Sci Ctr, Protected Resources Div, La Jolla, CA 92037 USA.
[Balazs, George H.] NOAA, Natl Marine Fisheries Serv, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA.
RP Frey, A (reprint author), NOAA, Natl Marine Fisheries Serv, SW Fisheries Sci Ctr, Protected Resources Div, 8901 La Jolla Shores Dr, La Jolla, CA 92037 USA.
EM Amy.Frey@noaa.gov
FU NOAA-National Marine Fisheries Service
FX Thanks to the Molokai Turtle Trackers, Nature Conservancy community
volunteers who monitored nesting tracks and nests. Samples from the
Hawaiian Islands National Wildlife Refuge were overseen by the USFWS,
Department of the Interior. We'd like to thank Stacy Hargrove, Kelly
Stewart, Erin LaCasella, Amy Jue, Gabriela Serra-Valente, Amanda Bowman,
Michael Jensen, Suzanne Roden, Brad McDonald and Robin LeRoux for their
help at the lab and with the data. This study was funded by
NOAA-National Marine Fisheries Service. [RH]
NR 38
TC 4
Z9 5
U1 3
U2 45
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-0981
J9 J EXP MAR BIOL ECOL
JI J. Exp. Mar. Biol. Ecol.
PD APR
PY 2013
VL 442
BP 80
EP 87
DI 10.1016/j.jembe.2013.01.030
PG 8
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 164QW
UT WOS:000320425600010
ER
PT J
AU Maselko, J
Bishop, G
Murphy, P
AF Maselko, Jacek
Bishop, Gretchen
Murphy, Peter
TI Ghost Fishing in the Southeast Alaska Commercial Dungeness Crab Fishery
SO NORTH AMERICAN JOURNAL OF FISHERIES MANAGEMENT
LA English
DT Article
ID CANCER-MAGISTER; TRAP; ESTUARY; POTS
AB Entrapment of crabs by derelict crab pots (also known as ghost fishing) can be a significant consequence of commercial fishing. The prevalence of lost commercial pots and ghost-fishing entrapments was estimated for the commercial Dungeness crab Cancer magister fishery in southeastern Alaska during the 2009 and 2010 summer closures of the commercial season (16 August through 30 September). Teams of divers retrieved a random subsample of the derelict crab pots located using side-scan sonar. Altogether, we retrieved 123 derelict crab pots containing 215 entrapped Dungeness crabs. The densities of derelict crab pots varied from 1.5 to 10.1/km(2), while the densities of entrapped Dungeness crabs ranged from 0 to 54.5/km(2), depending on the area surveyed. Derelict crab pots were discovered to effectively ghost-fish for at least 7years, indicating that there are long-term cumulative impacts on Dungeness crab populations. The number of derelict crab pots and entrapped Dungeness crabs at each of the surveyed areas was highly correlated with the number of fishermen, the number of pot lifts, and annual harvest in numbers, allowing for extrapolation to a regionwide estimate of crab entrapment and derelict crab pot abundance. Overall, our findings show instantaneous entrapment of less than 1% of the commercial crab harvest with a cumulative annual loss of less than 3% of the regional commercial crab harvest. We challenge the efficacy of the biodegradable escape mechanism currently employed in commercial Dungeness crab pots in southeastern Alaska and present alternatives which may require further in situ or laboratory verification of their effectiveness.
C1 [Maselko, Jacek] Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Auke Bay Labs, Juneau, AK 99801 USA.
[Bishop, Gretchen] Alaska Dept Fish & Game, Div Commercial Fisheries, Juneau, AK 99811 USA.
[Murphy, Peter] NOAA, Marine Debris Program, Off Response & Restorat, Seattle, WA 98115 USA.
RP Maselko, J (reprint author), Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Auke Bay Labs, 17109 Point Lena Loop Rd, Juneau, AK 99801 USA.
EM jacek.maselko@noaa.gov
FU NOAA Marine Debris Division
FX This study was funded by the NOAA Marine Debris Division. Special thanks
to Eric Brown, Andrew Eller, and Haley Poole for help with field work
and data processing and to the divers: Manuel Cruz, Peter Fischel, David
Francksen, Bill Heard, Justin Keese, Pat Malecha, Jennifer Mondragon,
Matthew Nardi, Kalei Shotwell, Elizabeth Siddon, Bob Stone, Ryan Wattam,
Brad Weinlaeder, and Alex Wertheimer. We also thank the reviewers for
their invaluable contribution. Reference to trade names does not imply
endorsement by the U.S. Government. The findings and conclusions in this
report are those of the author(s) and do not necessarily represent the
views of the funding agency.
NR 29
TC 6
Z9 6
U1 1
U2 14
PU TAYLOR & FRANCIS INC
PI PHILADELPHIA
PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA
SN 0275-5947
J9 N AM J FISH MANAGE
JI North Am. J. Fish Manage.
PD APR 1
PY 2013
VL 33
IS 2
BP 422
EP 431
DI 10.1080/02755947.2013.763875
PG 10
WC Fisheries
SC Fisheries
GA 167PD
UT WOS:000320643000020
ER
PT J
AU Liston, DB
Krukowski, AE
Stone, LS
AF Liston, Dorion B.
Krukowski, Anton E.
Stone, Leland S.
TI Saccade detection during smooth tracking
SO DISPLAYS
LA English
DT Article
DE Eye movements; Saccades; Smooth pursuit; Fixation
ID PURSUIT EYE-MOVEMENTS; VESTIBULO-OCULAR REFLEX; MONKEY; PERCEPTION;
FREQUENCIES; EXPANSION; MECHANICS; FIXATION; LATENCY; SEARCH
AB Saccade detection in an eye-movement trace provides a starting point for analyses ranging from the investigation of low-level oculomotor mechanisms to high-level cognitive processes. When the eye tracks the motion of the object of current interest (smooth pursuit), of the visual background (OKN), or of the resultant visual motion from a head movement (tVOR, rVOR), the smooth tracking movement is generally intermixed with rapid-phase saccadic eye movements, which must be excised to analyze the smooth components of tracking behavior properly. We describe a simple method to detect saccades on a background trace of variable velocity, compare our saccade-detection algorithm with the performance of an expert human observer, and present an ideal-observer analysis to benchmark its detection performance. (c) 2012 Elsevier B.V. All rights reserved.
C1 [Liston, Dorion B.; Krukowski, Anton E.; Stone, Leland S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Liston, Dorion B.; Krukowski, Anton E.] San Jose State Univ, San Jose, CA 95192 USA.
RP Liston, DB (reprint author), NASA, Ames Res Ctr, Mail Stop 262-2, Moffett Field, CA 94035 USA.
EM dorion.b.liston@nasa.gov
FU NSF's Program in Perception, Action and Cognition [NSF 0924841];
National Aeronautics and Space Administration (National Space Biomedical
Research Institute Grant) [SA2002]
FX This work was supported by NSF's Program in Perception, Action and
Cognition (NSF 0924841 to DL) and the National Aeronautics and Space
Administration (National Space Biomedical Research Institute Grant
SA2002 to LS). We thank Chad Netzer and Rami Ersheid for technical
assistance and Brent Beutter for helpful suggestions on this manuscript.
NR 40
TC 5
Z9 5
U1 1
U2 6
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0141-9382
J9 DISPLAYS
JI Displays
PD APR
PY 2013
VL 34
IS 2
BP 171
EP 176
DI 10.1016/j.displa.2012.10.002
PG 6
WC Computer Science, Hardware & Architecture; Engineering, Electrical &
Electronic; Instruments & Instrumentation; Optics
SC Computer Science; Engineering; Instruments & Instrumentation; Optics
GA 163PR
UT WOS:000320349900014
ER
PT J
AU Scalo, C
Boegman, L
Piomelli, U
AF Scalo, C.
Boegman, L.
Piomelli, U.
TI Large-eddy simulation and low-order modeling of sediment-oxygen uptake
in a transitional oscillatory flow
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
DE sediment oxygen uptake; seiche dynamics; high Schmidt number; mass
transfer; transitional flow; oscillating boundary layer
ID BOUNDARIES INTERFACIAL FLUX; LAKE-ERIE; BOTTOM-BOUNDARY; WATER
INTERFACE; HEAT-TRANSFER; TURBULENCE; NUMBERS; LAYERS; BED;
PHYTOPLANKTON
AB We have tested a dissolved oxygen (DO) transport model based on large-eddy simulation (LES) of a transitional oscillatory flow observed in the bottom boundary layer of Lake Alpnach, Switzerland. The transition from a quasi-laminar to a fully turbulent state makes this flow difficult to study with a Reynolds-averaged Navier-Stokes equation (RANSE) model. By resolving the full range of governing transport processes, LES provides a reliable prediction of the sediment-oxygen uptake (SOU). The model biogeochemical and flow parameters have been calibrated against DO and velocity measurements from published in situ data at the earliest phase available in the cycle. The fully developed flow thus obtained is used as an initial condition for the imposed oscillatory forcing. Numerical predictions show that transport in the outer layer is in equilibrium with the main current throughout most of the cycle and that nonequilibrium effects are limited to the diffusive sublayer response to the external forcing. During flow deceleration, the concentration boundary layer slowly expands as turbulence decays; later, during re-transition, mixing is restored by rapid and intense turbulent production events enhancing the SOU with a well-defined time lag. An algebraic model for the SOU is proposed for eventual inclusion in RANSE biogeochemical management-type models developed based on parameterizations used in turbulent mass transfer and with the support of published numerical data and the present simulation. The only input parameters required are the sediment oxidation rate, bulk temperature and DO concentration, and friction velocity.
C1 [Scalo, C.; Piomelli, U.] Queens Univ, Dept Mech & Mat Engn, Kingston, ON, Canada.
[Boegman, L.] Queens Univ, Dept Civil Engn, Kingston, ON K7L 3N6, Canada.
RP Scalo, C (reprint author), Stanford Univ, NASA, Ctr Turbulence Res, Bldg 500, Stanford, CA 94305 USA.
EM cscalo.ca@gmail.com
FU Natural Science and Engineering Research Council of Canada; Canada
Research Chair program
FX We acknowledge the financial support of the Natural Science and
Engineering Research Council of Canada under the Discovery Grant Program
and the Canada Research Chair program. The authors also thank the High
Performance Computing Virtual Laboratory (HPCVL), Queen's University
site, for the computational support. The authors thank Damien Bouffard
for the fruitful discussions on the flow physics, field-scale
measurements, on the parametrization of the sediment-oxygen uptake and
for providing us with his field data.
NR 49
TC 7
Z9 7
U1 0
U2 29
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD APR
PY 2013
VL 118
IS 4
BP 1926
EP 1939
DI 10.1002/jgrc.20113
PG 14
WC Oceanography
SC Oceanography
GA 163GN
UT WOS:000320324100020
ER
PT J
AU Qu, TD
Gao, S
Fukumori, I
AF Qu, Tangdong
Gao, Shan
Fukumori, Ichiro
TI Formation of salinity maximum water and its contribution to the
overturning circulation in the North Atlantic as revealed by a global
general circulation model
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
DE salinity maximum; formation; overturning circulation; North Atlantic
ID SEA-SURFACE SALINITY; TROPICAL ATLANTIC; OCEAN; PATHWAYS; PACIFIC;
TRENDS; DEEP; CLIMATOLOGY; VARIABILITY; VENTILATION
AB The formation of salinity maximum water in the North Atlantic is investigated using a simulated passive tracer and its adjoint. The results reveal that most salinity maximum water in the North Atlantic comes from the northwestern part of the subtropical gyre, and direct contribution from the evaporation-precipitation maximum region via the surface Ekman current is minor. Water originating from the evaporation-precipitation maximum region has to recirculate in the subtropical gyre before entering the sea surface salinity maximum region from the northwest. Once subducted, some portion (similar to 10%) of the salinity maximum water enters the equatorial region in the shallow subtropical cell, but most (similar to 70%) of it appears to turn northward to join the North Atlantic Deep Water. The latter pathway involves a three-dimensional circulation. When the warm, fresh surface water flows northward along the western boundary, it turns eastward in the northern subtropical gyre. As a result of the large excess of evaporation over precipitation, this water gradually gains its salinity on the route, until it reaches the sea surface salinity maximum region in the central subtropical gyre. From there, the salinity maximum water is subducted and flows back to the western boundary in the depth range of the thermocline. With its high-salinity nature, a major portion of this water penetrates into the subpolar region and directly contributes to the deep thermohaline circulation.
C1 [Qu, Tangdong; Gao, Shan] Univ Hawaii Manoa, Int Pacific Res Ctr, SOEST, Honolulu, HI 96822 USA.
[Fukumori, Ichiro] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Qu, TD (reprint author), Univ Hawaii Manoa, Int Pacific Res Ctr, SOEST, 1680 East West Rd, Honolulu, HI 96822 USA.
EM tangdong@hawaii.edu
RI Gao, Shan/H-7959-2013
OI Gao, Shan/0000-0003-4510-5028
FU NASA
FX This research was supported by NASA as part of the Aquarius Science Team
investigation. The OAFlux evaporation climatology was downloaded at
ftp://ftp.whoi.edu/pub/science/oaflux/data_v3 and the GPCP precipitation
climatology at ftp://rsd.gsfc.nasa.gov/pub/gpcp-v2.2cl, both through the
Asian Pacific Data Research Center at http://apdrc.soest.hawaii.edu. The
authors thank the three anonymous reviewers for their thoughtful
comments and constructive suggestions on an earlier version of the
manuscript. School of Ocean and Earth Science and Technology
contribution number 8885, and International Pacific Research Center
contribution number IPRC-953.
NR 47
TC 16
Z9 16
U1 1
U2 20
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD APR
PY 2013
VL 118
IS 4
BP 1982
EP 1994
DI 10.1002/jgrc.20152
PG 13
WC Oceanography
SC Oceanography
GA 163GN
UT WOS:000320324100024
ER
PT J
AU Moon, JH
Song, YT
AF Moon, Jae-Hong
Song, Y. Tony
TI Sea level and heat content changes in the western North Pacific
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
DE Sea level rise; oceanic heat content; non-Boussinesq OGCM; ocean mass;
western North Pacific
ID SOUTH CHINA SEA; TROPICAL PACIFIC; SATELLITE ALTIMETRY; OCEAN;
VARIABILITY; TRENDS; BUDGET; RISE; SURFACE; SYSTEM
AB Altimetry-observed sea level rise (SLR) over the western North Pacific (WNP), including the South China Sea, Yellow Sea, East China Sea, and East/Japan Sea, has a rate of 5 mm/year over 1993-2010, which is about 1.5 times the rate of the global mean. Here we have examined sea level changes and related ocean heat content (OHC) in the WNP by comparing results from a non-Boussinesq ocean general circulation model (mass-conserved) with data sets from altimeters, the Gravity Recovery and Climate Experiment (GRACE), and in situ profiles. Our model reproduces the altimetry regional trends as well as their seasonal/interannual variations. Adding a GRACE-estimated mass to the model result further explains the altimetry SLR in a way that mass-induced effect contributes more in the midlatitudes than in the tropical WNP over the GRACE period. In addition, interannual variability and linear trend of regional sea levels are explained mainly by changes in the OHC due to heat convergence and divergence by ocean circulations, while seasonal variability is caused mainly by surface air-sea fluxes. To understand the underline physics, a comparative experiment was carried out, showing that the recent strengthening trends of SLR and OHC in the tropical regions are significantly attributed to the heat and water mass redistribution in the upper ocean caused by the intensified easterly trade wind over the past two decades.
C1 [Moon, Jae-Hong; Song, Y. Tony] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA.
RP Moon, JH (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA.
EM Jae-Hong.Moon@jpl.nasa.gov
NR 42
TC 8
Z9 9
U1 1
U2 24
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9275
EI 2169-9291
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD APR
PY 2013
VL 118
IS 4
BP 2014
EP 2022
DI 10.1002/jgrc.20096
PG 9
WC Oceanography
SC Oceanography
GA 163GN
UT WOS:000320324100026
ER
PT J
AU Kidd, C
Srinivasan, J
Roca, R
AF Kidd, Chris
Srinivasan, J.
Roca, Remy
TI The Megha-Tropiques mission: day 1 algorithms
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Editorial Material
C1 [Kidd, Chris] Univ Maryland, ESSIC, NASA GSFC, Greenbelt, MD USA.
[Srinivasan, J.] Indian Inst Sci, Ctr Atmospher & Ocean Sci, Bangalore 560012, Karnataka, India.
[Roca, Remy] OMP LEGOS, F-31400 Toulouse, France.
RP Roca, R (reprint author), OMP LEGOS, 14 Av Edouard Belin, F-31400 Toulouse, France.
EM Remy.Roca@legos.obs-mip.fr
RI Kidd, Christopher/H-9910-2014
NR 0
TC 2
Z9 2
U1 1
U2 5
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-9009
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD APR
PY 2013
VL 139
IS 673
SI SI
BP 841
EP 841
DI 10.1002/qj.2201
PN B
PG 1
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 164FG
UT WOS:000320393800001
ER
PT J
AU Kacimi, S
Viltard, N
Kirstetter, PE
AF Kacimi, Sahra
Viltard, Nicolas
Kirstetter, Pierre-Emmanuel
TI A new methodology for rain identification from passive microwave data in
the Tropics using neural networks
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE passive microwave; neural networks; Probability of Detection; bias;
Bayesian inversion; rainfall estimation
ID PRECIPITATION ESTIMATION; RETRIEVAL ALGORITHMS; PROFILING ALGORITHM;
TRMM; SENSORS; CLOUDS; RADAR; WATER; LAND
AB The detection of rainfall remains a challenge for the monitoring of precipitation from space. A methodology is presented to identify rain events from spaceborne passive microwave data using neural networks. We focus on BRAIN, the algorithm that provides instantaneous quantitative precipitation estimates at the surface, based on the MADRAS radiometer onboard the Megha-Tropiques satellite. A version of BRAIN using data from the Tropical Rainfall Measuring Mission (TRMM) Microwave Imager (TMI) has been used to compare several multilayer perceptrons (MLP) trained on different combinations of TMI brightness temperatures with the conventional GSCAT-2 algorithm approach used for rainfall detection. These classifiers were compared at a global scale to reference values from the TRMM Precipitation Radar (PR). They were also compared to ground measurements using two 1 degrees x 1 degrees dense rain-gauge networks from different climatic zones in West Africa to assess the inFLuence of rainfall types. At the global scale the MLPs provide better Probability of Detection than the GSCAT-2 decision tree but tend to have a higher False Alarm Rate. While no unique solution exists given the strong regional dependence of the classifiers' performances, the screen based on the 19, 21 and 85 GHz channels provides the best detection results at the instantaneous scales. As to accumulated rainfall, the screen that exhibits the lower bias relative to the PR makes use of the 37 and 85 GHz channels. The evaluation over West Africa using 10 years of TRMM overpasses shows that MLPs are in better agreement with both the PR and the gauges than GSCAT-2. The MLP trained on the 37 and 85 GHz channels increases the Probability of Detection by nearly 35% compared to the former screening over the two studied regions. Better results are obtained in the case of organized systems. Copyright (c) 2013 Royal Meteorological Society
C1 [Kacimi, Sahra] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Viltard, Nicolas] Univ Versailles, CNRS INSU, LATMOS IPSL, Guyancourt, France.
[Kirstetter, Pierre-Emmanuel] NOAA, Natl Severe Storms Lab, Norman, OK 73069 USA.
RP Kacimi, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 300-243, Pasadena, CA 91109 USA.
EM sahra.kacimi@jpl.nasa.gov
RI Kirstetter, Pierre/E-2305-2013; Measurement, Global/C-4698-2015
OI Kirstetter, Pierre/0000-0002-7381-0229;
NR 27
TC 4
Z9 4
U1 0
U2 5
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-9009
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD APR
PY 2013
VL 139
IS 673
SI SI
BP 912
EP 922
DI 10.1002/qj.2114
PN B
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 164FG
UT WOS:000320393800007
ER
PT J
AU Holdaway, D
Thuburn, J
Wood, N
AF Holdaway, D.
Thuburn, J.
Wood, N.
TI Comparison of Lorenz and Charney-Phillips vertical discretisations for
dynamics-boundary layer coupling. Part I: Steady states
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE physics-dynamics coupling; steady-state boundary layer; vertical
staggering; NWP
ID EQUATION ATMOSPHERIC MODELS; OPTIMAL REPRESENTATION; PHYSICAL
PARAMETERIZATIONS; DISCRETIZATIONS; PARAMETRIZATIONS; SENSITIVITY;
PARALLEL; SCHEMES; SPLIT; CORE
AB Accurate coupling between the resolved-scale dynamics and the parametrised physics is essential for accurate modelling of the atmosphere. Previous emphasis has been on the temporal aspects of this so-called physics-dynamics coupling problem, with little attention on the spatial aspects. When designing a model for numerical weather prediction there is a choice for how to vertically arrange the predicted variables, namely the Lorenz and Charney-Phillips grids, and there is ongoing debate as to which is the optimal. The Charney-Phillips grid is considered good for capturing the potential vorticity dynamics and wave propagation, whereas the Lorenz grid is more suitable for conservation. However the Lorenz grid supports a computational mode. It is argued here that the Lorenz grid is preferred for modelling the stably stratified boundary layer. This presents the question: which grid will produce more accurate results when coupling the large-scale dynamics to the stably stratified planetary boundary layer? The question is addressed by examining the ability of both the Lorenz and Charney-Phillips grids to capture the steady state of a set of equations that simultaneously represents both large-scale dynamics and the planetary boundary layer. The results show that the Charney-Phillips grid is able to capture accurately the steady boundary-layer solution provided the Richardson number is calculated without vertically averaging the shear. Averaging the shear suppresses the negative feedback of the shear on the diffusion coefficient; the positive feedback, via the vertical gradient of potential temperature, then leads to the formation of unrealistic step-like features. Copyright (c) 2012 Royal Meteorological Society
C1 [Holdaway, D.; Thuburn, J.] Univ Exeter, Coll Engn Math & Phys Sci, Exeter EX4 4QJ, Devon, England.
[Holdaway, D.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Wood, N.] Met Off, Exeter, Devon, England.
RP Holdaway, D (reprint author), NASA, Goddard Space Flight Ctr, Code 610-1, Greenbelt, MD 20771 USA.
EM dan.holdaway@nasa.gov
RI Holdaway, Daniel/Q-5198-2016
OI Holdaway, Daniel/0000-0002-3672-2588
FU EPSRC; Met Office under Industrial CASE partnership
FX The lead author wishes to thank the EPSRC and the Met Office for funding
this work under an Industrial CASE partnership. Further thanks are due
to the dynamics research group at the Met Office for providing access to
their expertise.
NR 35
TC 0
Z9 1
U1 1
U2 9
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-9009
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD APR
PY 2013
VL 139
IS 673
SI SI
BP 1073
EP 1086
DI 10.1002/qj.2016
PN B
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 164FG
UT WOS:000320393800019
ER
PT J
AU Holdaway, D
Thuburn, J
Wood, N
AF Holdaway, D.
Thuburn, J.
Wood, N.
TI Comparison of Lorenz and Charney-Phillips vertical discretisations for
dynamics-boundary layer coupling. Part II: Transients
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE physics-dynamics coupling; computational mode; eigenmodes; atmospheric
waves
ID OPTIMAL REPRESENTATION; ATMOSPHERIC MODELS; DISCRETIZATIONS
AB A numerical comparison of the Lorenz and Charney-Phillips vertical grids for capturing the steady state of a set of equations that models the large-scale dynamics of the atmosphere and the planetary boundary layer (Part I of this article) has revealed important differences between the grids. Due to suppression of a negative feedback, Charney-Phillips grids that involve averaging of shear in the boundary-layer terms are not able to capture the structure of the boundary layer accurately. The Lorenz grid performs well in terms of capturing the boundary layer on its own, but the Charney-Phillips grids that use averaging of potential temperature gradient are generally preferred once dynamics are included. Any finite-difference approximation of the problem must be capable of accurately representing both the steady-state and time-dependent parts of the solution. In this Part II of the article, the ability of the Lorenz and Charney-Phillips configurations to capture the transient part of the system is considered. The configurations are compared in terms of their ability to capture the eigenmodes of the solution. Full comparison between Lorenz and Charney-Phillips grids is limited by non-normality of the linearised system, associated with the boundary layer. The Lorenz grid computational mode is examined. The structure is modified by the boundary layer but it still exists. For the modes that could be accurately examined, it is found that both grids perform well in terms of capturing spatial and temporal mode structure. Some Lorenz grid modes are identified that have spurious computational mode-like behaviour occurring near the top of the boundary layer. Copyright (c) 2012 Royal Meteorological Society
C1 [Holdaway, D.; Thuburn, J.] Univ Exeter, Coll Engn Math & Phys Sci, Exeter EX4 4QJ, Devon, England.
[Holdaway, D.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Wood, N.] Met Off, Exeter, Devon, England.
RP Holdaway, D (reprint author), NASA, Goddard Space Flight Ctr, Code 610-1, Greenbelt, MD 20771 USA.
EM dan.holdaway@nasa.gov
RI Holdaway, Daniel/Q-5198-2016
OI Holdaway, Daniel/0000-0002-3672-2588
FU EPSRC; Met Office under Industrial CASE partnership
FX The lead author wishes to thank the EPSRC and the Met Office for funding
this work under an Industrial CASE partnership. Further thanks are due
to the dynamics research group at the Met Office for providing access to
their expertise.
NR 20
TC 1
Z9 2
U1 0
U2 5
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-9009
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD APR
PY 2013
VL 139
IS 673
SI SI
BP 1087
EP 1098
DI 10.1002/qj.2017
PN B
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 164FG
UT WOS:000320393800020
ER
PT J
AU Ericson, KL
Cooper, BR
Peels, ME
Deng, Y
Smith, SM
Coburn, SP
AF Ericson, Karen Louise
Cooper, B. R.
Peels, M. E.
Deng, Y.
Smith, S. M.
Coburn, S. P.
TI Application of Urine Metabolomics to Probe the Effects of Long-Term Bed
Rest as a Model for Spaceflight
SO FASEB JOURNAL
LA English
DT Meeting Abstract
CT Joint Annual Meeting of the ASPET/BPS at Experimental Biology (EB)
CY APR 20-24, 2013
CL Boston, MA
SP ASPET, British Pharmacol Soc (BPS)
C1 [Ericson, Karen Louise; Peels, M. E.; Deng, Y.; Coburn, S. P.] Indiana Univ Purdue Univ, Ft Wayne, IN 46805 USA.
[Cooper, B. R.] Purdue Univ, Bindley Biosci, W Lafayette, IN 47907 USA.
[Smith, S. M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
J9 FASEB J
JI Faseb J.
PD APR
PY 2013
VL 27
MA lb311
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA 157GG
UT WOS:000319883505456
ER
PT J
AU Heer, M
Buehlmeier, J
Smith, SM
Baecker, N
Frings-Meuthen, P
AF Heer, Martina
Buehlmeier, Judith
Smith, Scott M.
Baecker, Natalie
Frings-Meuthen, Petra
TI KHCO3 Prevents Increase in Bone Resorption with High Protein in Bed Rest
(MEP Study)
SO FASEB JOURNAL
LA English
DT Meeting Abstract
CT Joint Annual Meeting of the ASPET/BPS at Experimental Biology (EB)
CY APR 20-24, 2013
CL Boston, MA
SP ASPET, British Pharmacol Soc (BPS)
C1 [Heer, Martina] Profil, Nutr Sci, Neuss, Germany.
[Heer, Martina; Buehlmeier, Judith; Baecker, Natalie] Univ Bonn, IEL Nutr Physiol, Bonn, Germany.
[Buehlmeier, Judith; Frings-Meuthen, Petra] DLR, Inst Aerosp Med, Cologne, Germany.
[Smith, Scott M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
J9 FASEB J
JI Faseb J.
PD APR
PY 2013
VL 27
MA 615.15
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA 156YK
UT WOS:000319860505547
ER
PT J
AU Morgan, JLL
Crucian, BE
Sams, CF
Smith, SM
Zwart, SR
AF Morgan, Jennifer L. L.
Crucian, Brian E.
Sams, Clarence F.
Smith, Scott M.
Zwart, Sara R.
TI The Effects of High Dietary Iron and Radiation Exposure on Markers of
Oxidative Stress and Immune Status of Rats
SO FASEB JOURNAL
LA English
DT Meeting Abstract
CT Joint Annual Meeting of the ASPET/BPS at Experimental Biology (EB)
CY APR 20-24, 2013
CL Boston, MA
SP ASPET, British Pharmacol Soc (BPS)
C1 [Morgan, Jennifer L. L.] NASA, ORAU, Houston, TX USA.
[Crucian, Brian E.; Sams, Clarence F.; Smith, Scott M.] NASA, Houston, TX USA.
[Zwart, Sara R.] NASA, USRA, Houston, TX USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
J9 FASEB J
JI Faseb J.
PD APR
PY 2013
VL 27
MA 866.4
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA 156YK
UT WOS:000319860504284
ER
PT J
AU Serrador, JM
Falvo, MJ
Maracaja, L
Blatt, MM
Caine, TL
Stenger, MB
Platts, S
Knapp, CF
Evans, JM
AF Serrador, Jorge M.
Falvo, Michael J.
Maracaja, Luiz
Blatt, Melissa M.
Caine, Timothy L.
Stenger, Michael B.
Platts, Steven
Knapp, Charles F.
Evans, Joyce M.
TI Acute Hypovolemia Does Not Affect Dynamic Cerebral Autoregulation in
Humans
SO FASEB JOURNAL
LA English
DT Meeting Abstract
CT Joint Annual Meeting of the ASPET/BPS at Experimental Biology (EB)
CY APR 20-24, 2013
CL Boston, MA
SP ASPET, British Pharmacol Soc (BPS)
C1 [Serrador, Jorge M.; Falvo, Michael J.; Blatt, Melissa M.] VA New Jersey Healthcare Syst, WRIISC, E Orange, NJ USA.
[Serrador, Jorge M.; Falvo, Michael J.] Univ Med & Dent New Jersey, New Jersey Med Sch, Newark, NJ 07103 USA.
[Maracaja, Luiz] Suny Downstate Med Ctr, Brooklyn, NY 11203 USA.
[Caine, Timothy L.; Stenger, Michael B.; Platts, Steven] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Knapp, Charles F.; Evans, Joyce M.] Univ Kentucky, Lexington, KY USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
J9 FASEB J
JI Faseb J.
PD APR
PY 2013
VL 27
MA 925.12
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA 156YK
UT WOS:000319860506194
ER
PT J
AU Smith, SM
Sceppa, CC
O'Brien, KO
Abrams, SA
Gillman, P
Zwart, SR
Wastney, ME
AF Smith, Scott M.
Sceppa, Carmen Casteneda
O'Brien, Kimberly O.
Abrams, Steven A.
Gillman, Patti
Zwart, Sara R.
Wastney, Meryl E.
TI Calcium Kinetics during Bed Rest with Artificial Gravity and Exercise
Countermeasures
SO FASEB JOURNAL
LA English
DT Meeting Abstract
CT Joint Annual Meeting of the ASPET/BPS at Experimental Biology (EB)
CY APR 20-24, 2013
CL Boston, MA
SP ASPET, British Pharmacol Soc (BPS)
C1 [Smith, Scott M.] NASA, JSC, Houston, TX USA.
[Sceppa, Carmen Casteneda] Northeastern Univ, Boston, MA 02115 USA.
[Sceppa, Carmen Casteneda] Tufts Univ, Boston, MA 02111 USA.
[O'Brien, Kimberly O.] Cornell Univ, Ithaca, NY USA.
[Abrams, Steven A.] Baylor Coll Med, Houston, TX 77030 USA.
[Gillman, Patti] NASA, EASI, Houston, TX USA.
[Zwart, Sara R.] NASA, USRA, Houston, TX USA.
[Wastney, Meryl E.] Metab Modeling, W Lafayette, IN USA.
NR 0
TC 0
Z9 0
U1 1
U2 5
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
J9 FASEB J
JI Faseb J.
PD APR
PY 2013
VL 27
MA 233.6
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA 156YK
UT WOS:000319860500140
ER
PT J
AU Wotring, VE
AF Wotring, Virginia E.
TI Effects of Radiation Exposure and Dietary Iron on Liver Metabolic Gene
Expression
SO FASEB JOURNAL
LA English
DT Meeting Abstract
CT Joint Annual Meeting of the ASPET/BPS at Experimental Biology (EB)
CY APR 20-24, 2013
CL Boston, MA
SP ASPET, British Pharmacol Soc (BPS)
C1 [Wotring, Virginia E.] NASA, Houston, TX USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
J9 FASEB J
JI Faseb J.
PD APR
PY 2013
VL 27
MA 1180.7
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA 156YK
UT WOS:000319860503268
ER
PT J
AU Zwart, SR
Morgan, JLL
Smith, SM
AF Zwart, Sara R.
Morgan, Jennifer L. L.
Smith, Scott M.
TI Risk of Oxidative Damage and Bone Resorption from Increased Iron Stores
during Space Flight
SO FASEB JOURNAL
LA English
DT Meeting Abstract
CT Joint Annual Meeting of the ASPET/BPS at Experimental Biology (EB)
CY APR 20-24, 2013
CL Boston, MA
SP ASPET, British Pharmacol Soc (BPS)
C1 [Zwart, Sara R.] USRA NASA JSC, Houston, TX USA.
[Morgan, Jennifer L. L.] ORAU NASA JSC, Houston, TX USA.
[Smith, Scott M.] NASA, Houston, TX USA.
NR 0
TC 0
Z9 0
U1 1
U2 5
PU FEDERATION AMER SOC EXP BIOL
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814-3998 USA
SN 0892-6638
J9 FASEB J
JI Faseb J.
PD APR
PY 2013
VL 27
MA 634.4
PG 1
WC Biochemistry & Molecular Biology; Biology; Cell Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics; Cell Biology
GA 157GG
UT WOS:000319883500648
ER
PT J
AU Kocsis, MB
Cholewiak, SA
Traylor, RM
Adelstein, BD
Hirleman, ED
Tan, HZ
AF Kocsis, Matthew B.
Cholewiak, Steven A.
Traylor, Ryan M.
Adelstein, Bernard D.
Hirleman, E. Daniel
Tan, Hong Z.
TI Discrimination of Real and Virtual Surfaces with Sinusoidal and
Triangular Gratings Using the Fingertip and Stylus
SO IEEE TRANSACTIONS ON HAPTICS
LA English
DT Article
DE Haptic texture perception; real texture; virtual texture; amplitude
discrimination
ID ADAPTING MECHANORECEPTIVE AFFERENTS; PERCEIVED INSTABILITY; TACTILE
ROUGHNESS; HAPTIC TEXTURE; MONKEY FINGERPAD; PERCEPTION; FORCE;
RESPONSES; GEOMETRY; DISPLAY
AB Two-interval two-alternative forced-choice discrimination experiments were conducted separately for sinusoidal and triangular textured surface gratings from which amplitude (i.e., height) discrimination thresholds were estimated. Participants (group sizes.n = 4 to 7) explored one of these texture types either by fingertip on real gratings (Finger real), by stylus on real gratings (Stylus real), or by stylus on virtual gratings (Stylus virtual). The real gratings were fabricated from stainless steel by an electrical discharge machining process while the virtual gratings were rendered via a programmable force-feedback device. All gratings had a 2.5-mm spatial period. On each trial, participants compared test gratings with 55, 60, 65, or 70 mu m amplitudes against a 50-mu m reference. The results indicate that discrimination thresholds did not differ significantly between sinusoidal and triangular gratings. With sinusoidal and triangular data combined, the average (mean +/- standard error) for the Stylus-real threshold (2.5 +/- 0.2 mu m) was significantly smaller (p < 0.01) than that for the Stylus-virtual condition (4.9 +/- 0.2 mu m). Differences between the Finger-real threshold (3.8 +/- 0.2 mu m) and those from the other two conditions were not statistically significant. Further studies are needed to better understand the differences in perceptual cues resulting from interactions with real and virtual gratings.
C1 [Kocsis, Matthew B.] Aircell, Broomfield, CO 80021 USA.
[Cholewiak, Steven A.] Rutgers State Univ, Dept Psychol, Piscataway, NJ 08854 USA.
[Traylor, Ryan M.] Battelle Huntsville Operat, Battelle Mem Inst, Huntsville, AL 35806 USA.
[Adelstein, Bernard D.] NASA, Ames Res Ctr, Human Syst Integrat Div, Moffett Field, CA 94035 USA.
[Hirleman, E. Daniel] Univ Calif, Sch Engn, Merced, CA 95343 USA.
[Tan, Hong Z.] Purdue Univ, Sch Elect & Comp Engn, Hapt Interface Res Lab, W Lafayette, IN 47907 USA.
RP Kocsis, MB (reprint author), Aircell, 303 S Technol Ct,Bldg A, Broomfield, CO 80021 USA.
EM mattkocsis@alumni.purdue.edu; scholewi@rutgers.edu;
ryantraylor@alumni.purdue.edu; Bernard.D.Adelstein@nasa.gov;
dhirleman@ucmerced.edu; hongtan@purdue.edu
RI Cholewiak, Steven/N-6426-2013
OI Cholewiak, Steven/0000-0003-0605-4395
FU US National Science Foundation [0098443-IIS]; NASA [NCC 2-1363]; School
of Electrical and Computer Engineering at Purdue University
FX This work was supported in part by a US National Science Foundation
Award under Grant No. 0098443-IIS, and in part by NASA under award no.
NCC 2-1363. In addition, Matthew Kocsis was partially supported by a
graduate fellowship from the School of Electrical and Computer
Engineering at Purdue University. The authors thank Drs. Susan Lederman
and Roberta Klatzky for discussions on experimental methods, Mike
Sherwood at Purdue University for his assistance with the fabrication of
the EDM samples with surface gratings, Patrick Kalita for the spectral
analysis of virtual texture gratings shown in Figs. 6 and 7, and Dr.
Michael Seaman at the University of South Carolina for providing the
extended Kruskal-Wallis tables for some of the statistical analyses.
Portions of this paper reprinted with permission from [36] and [35], (c)
2006/2007 IEEE.
NR 49
TC 3
Z9 3
U1 0
U2 5
PU IEEE COMPUTER SOC
PI LOS ALAMITOS
PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1314 USA
SN 1939-1412
EI 2329-4051
J9 IEEE T HAPTICS
JI IEEE Trans. Haptics
PD APR-JUN
PY 2013
VL 6
IS 2
BP 181
EP 192
DI 10.1109/ToH.2012.31
PG 12
WC Computer Science, Cybernetics
SC Computer Science
GA 157EA
UT WOS:000319877500005
PM 24808302
ER
PT J
AU Hellinger, P
Travnicek, PM
Stverak, S
Matteini, L
Velli, M
AF Hellinger, Petr
Travnicek, Pavel M.
Stverak, Stepan
Matteini, Lorenzo
Velli, Marco
TI Proton thermal energetics in the solar wind: Helios reloaded
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE solar wind; proton energetics; turbulent heating
ID VELOCITY DISTRIBUTIONS; ION-BEAMS; EQUATION; PLASMA; WAVE; 1-AU;
INSTABILITIES; ANISOTROPY; TURBULENCE; EVOLUTION
AB The proton thermal energetics in the slow solar wind between 0.3 and 1 AU is reinvestigated using the Helios 1 and 2 data, complementing a similar analysis for the fast solar wind [Hellinger et al., 2011]. The results for slow and fast solar winds are compared and discussed in the context of previous results. Protons need to be heated in the perpendicular direction with respect to the ambient magnetic field from 0.3 to 1 AU. In the parallel direction, protons need to be cooled at 0.3 AU, with a cooling rate comparable to the corresponding perpendicular heating rate; between 0.3 and 1 AU, the required cooling rate decreases until a transition to heating occurs: by 1 AU the protons require parallel heating, with a heating rate comparable to that required to sustain the perpendicular temperature. The heating/cooling rates (per unit volume) in the fast and slow solar winds are proportional to the ratio between the proton kinetic energy and the expansion time. On average, the protons need to be heated and the necessary heating rates are comparable to the energy cascade rate of the magnetohydrodynamic turbulence estimated from the stationary Kolmogorov-Yaglom law at 1 AU; however, in the expanding solar wind, the stationarity assumption for this law is questionable. The turbulent energy cascade may explain the average proton energetics (although the stationarity assumption needs to be justified) but the parallel cooling is likely related to microinstabilities connected with the structure of the proton velocity distribution function. This is supported by linear analysis based on observed data and by results of numerical simulations.
C1 [Hellinger, Petr; Travnicek, Pavel M.; Stverak, Stepan] AS CR, Astron Inst, Prague, Czech Republic.
[Hellinger, Petr; Stverak, Stepan] AS CR, Inst Atmospher Phys, Prague, Czech Republic.
[Travnicek, Pavel M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Matteini, Lorenzo; Velli, Marco] Univ Florence, Dipartimento Fis & Astron, Florence, Italy.
[Matteini, Lorenzo] Univ London Imperial Coll Sci Technol & Med, London, England.
[Velli, Marco] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Hellinger, P (reprint author), AS CR, Astron Inst, Prague, Czech Republic.
EM Petr.Hellinger@asu.cas.cz
RI Hellinger, Petr/F-5267-2014; Stverak, Stepan/F-5282-2014; Travnicek,
Pavel/G-8608-2014
OI Hellinger, Petr/0000-0002-5608-0834;
FU Grant Agency of the Czech Republic [P209/12/2023, P209/12/2041];
European Commission [284515, 263340]; [RVO:67985815]; [RVO:68378289]
FX PH, SS, and PMT acknowledge grants P209/12/2023 and P209/12/2041 of the
Grant Agency of the Czech Republic. The research leading to these
results has received funding from the European Commission's Seventh
Framework Programme (FP7) under the grant agreement SHOCK (project
number 284515, project-shock.eu) and SWIFF (project number 263340,
www.swiff.eu). This work was also supported by the projects RVO:67985815
and RVO:68378289.
NR 48
TC 31
Z9 31
U1 2
U2 20
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 APR
PY 2013
VL 118
IS 4
BP 1351
EP 1365
DI 10.1002/jgra.50107
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 157UJ
UT WOS:000319924400001
ER
PT J
AU Turner, DL
Omidi, N
Sibeck, DG
Angelopoulos, V
AF Turner, D. L.
Omidi, N.
Sibeck, D. G.
Angelopoulos, V.
TI First observations of foreshock bubbles upstream of Earth's bow shock:
Characteristics and comparisons to HFAs
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE Ion foreshock; Particle acceleration; Kinetic phenomena
ID DIAMAGNETIC CAVITIES UPSTREAM; HOT FLOW ANOMALIES; SOLAR-WIND;
ACCELERATION; MAGNETOPAUSE; MODEL
AB Using multipoint in situ observations upstream of Earth's bow shock from the THEMIS mission, we present the first observations of foreshock bubbles (FBs) and compare them to observations of hot flow anomalies (HFAs). FBs are recently conceptualized kinetic phenomena that can form under the commonplace condition of a rotational discontinuity in the interplanetary magnetic field interacting with backstreaming energetic ions in Earth's quasi-parallel foreshock. FBs may have remained elusive until now due to their many observational similarities to HFAs and the lack of coordinated multipoint measurements. Here we introduce identification criteria for distinguishing between HFAs and FBs using in situ observations, and use them to analyze five example events that occurred on Bastille Day (14 July) and 11-12 August 2008. Three of these events satisfy the criteria for FBs and are inconsistent with multiple criteria for HFAs. The remaining two events are consistent with the traditional picture of HFAs. Furthermore, FBs involve two converging shocks, and using these events, we demonstrate their effectiveness at particle acceleration. Considering that their formation conditions are not extraordinary, FBs may be ubiquitous at collisionless, quasi-parallel shocks in a variety of astrophysical settings.
C1 [Turner, D. L.; Angelopoulos, V.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA.
[Turner, D. L.; Angelopoulos, V.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
[Omidi, N.] Solana Sci Inc, Solana Beach, CA USA.
[Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Turner, DL (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
EM drew.lawson.turner@gmail.com
RI Turner, Drew/G-3224-2012
FU NASA [NAS5-02099]; NSF [AGS-1007449]
FX D. L. Turner thanks Ferdinand Plaschke, Michael Hartinger, and Heli
Hietala for invaluable discussions, comments, questions, and
suggestions. The authors would all like to thank the entire THEMIS team
and especially the following people for providing various instrument
data: Karl-Heinz Glassmeier (spacecraft magnetometers), Jim McFadden
(ESA), and Davin Larson (SST). This work was funded under NASA contract
NAS5-02099, and N. Omidi acknowledges NSF grant AGS-1007449.
NR 39
TC 17
Z9 17
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD APR
PY 2013
VL 118
IS 4
BP 1552
EP 1570
DI 10.1002/jgra.50198
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 157UJ
UT WOS:000319924400016
ER
PT J
AU Wendel, DE
Adrian, ML
AF Wendel, D. E.
Adrian, M. L.
TI Current structure and nonideal behavior at magnetic null points in the
turbulent magnetosheath
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE turbulence; magnetosheath; magnetic reconnection; magnetic null points
ID SOLAR-WIND PLASMA; IN-SITU EVIDENCE; KINEMATIC RECONNECTION; ALIGNED
CURRENT; MHD TURBULENCE; NEUTRAL POINTS; CURRENT SHEETS; FIELD LINES;
EVOLUTION; DISCONTINUITIES
AB The Poincare index indicates that the Cluster spacecraft tetrahedron entraps a number of 3-D magnetic nulls during an encounter with the turbulent magnetosheath. Previous researchers have found evidence for reconnection at one of the many filamentary current layers observed by Cluster in this region. We find that many of the entrained nulls are also associated with strong currents. We dissect the current structure of a pair of spiral nulls that may be topologically connected. At both nulls, we find a strong current along the spine, accompanied by a somewhat more modest current perpendicular to the spine that tilts the fan toward the axis of the spine. The current along the fan is comparable to the that along the spine. At least one of the nulls manifests a rotational flow pattern in the fan plane that is consistent with torsional spine reconnection as predicted by theory. These results emphasize the importance of examining the magnetic topology in interpreting the nature of currents and reconnection in 3-D turbulence.
C1 [Wendel, D. E.; Adrian, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Wendel, DE (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
EM deirdre.e.wendel@nasa.gov
RI Wendel, Deirdre/D-4429-2012
OI Wendel, Deirdre/0000-0002-1925-9413
FU NASA
FX The authors wish to thank Melvyn L. Goldstein, Mats Andre, and Adolfo F.
Vi as for helpful discussions. D. E. Wendel wishes to acknowledge the
assistance of Kyoung-Joo Hwang for verification of the MVA. We wish to
acknowledge data provided by the Cluster Active Archive and thank the
FGM PI Elizabeth Lucek and the EFW PI Mats Andre and their teams for
making the data available. This research was supported by NASA funding
for the Cluster mission and for the MMS Interdisciplinary Science grant
to the Goddard Space Flight Center.
NR 73
TC 14
Z9 14
U1 0
U2 8
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 APR
PY 2013
VL 118
IS 4
BP 1571
EP 1588
DI 10.1002/jgra.50234
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 157UJ
UT WOS:000319924400017
ER
PT J
AU Raines, JM
Gershman, DJ
Zurbuchen, TH
Sarantos, M
Slavin, JA
Gilbert, JA
Korth, H
Anderson, BJ
Gloeckler, G
Krimigis, SM
Baker, DN
McNutt, RL
Solomon, SC
AF Raines, Jim M.
Gershman, Daniel J.
Zurbuchen, Thomas H.
Sarantos, Menelaos
Slavin, James A.
Gilbert, Jason A.
Korth, Haje
Anderson, Brian J.
Gloeckler, George
Krimigis, Stamatios M.
Baker, Daniel N.
McNutt, Ralph L., Jr.
Solomon, Sean C.
TI Distribution and compositional variations of plasma ions in Mercury's
space environment: The first three Mercury years of MESSENGER
observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE Mercury; exosphere; magnetosphere; plasma composition
ID SODIUM EXOSPHERE; SPATIAL-DISTRIBUTION; MAGNETIC-FIELD; MAGNETOSPHERE;
ATMOSPHERE; SURFACE; MODEL; ACCELERATION; INSTRUMENT; DEPENDENCE
AB We have analyzed measurements of planetary ions near Mercury made by the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) Fast Imaging Plasma Spectrometer (FIPS) over the first three Mercury years of orbital observations (25 March 2011 through 31 December 2011). We determined the composition and spatial distributions of the most abundant species in the regions sampled by the MESSENGER spacecraft during that period. In particular, we here focus on altitude dependence and relative abundances of species in a variety of spatial domains. We used observed density as a proxy for ambient plasma density, because of limitations to the FIPS field of view. We find that the average observed density is 3.9 x 10-2cm-3 for He2+, 3.4 x 10-4cm-3 for He+, 8.0 x 10-4cm-3 for O+-group ions, and 5.1 x 10-3cm-3 for Na+-group ions. Na+-group ions are particularly enhanced over other planetary ions (He+ and O+ group) in the northern magnetospheric cusp (by a factor of similar to 2.0) and in the premidnight sector on the nightside (by a factor of similar to 1.6). Within 30 degrees of the equator, the average densities of all planetary ions are depressed at the subsolar point relative to the dawn and dusk terminators. The effect is largest for Na+-group ions, which are 49% lower in density at the subsolar point than at the terminators. This depression could be an effect of the FIPS energy threshold. The three planetary ion species considered show distinct dependences on altitude and local time. The Na+ group has the smallest e-folding height at all dayside local times, whereas He+ has the largest. At the subsolar point, the e-folding height for Na+-group ions is 590km, and that for the O+ group and He+ is 1100km. On the nightside and within 750km of the geographic equator, Na+-group ions are enhanced in the premidnight sector. This enhancement is consistent with nonadiabatic motion and may be observational evidence that nonadiabatic effects are important in Mercury's magnetosphere.
C1 [Raines, Jim M.; Gershman, Daniel J.; Zurbuchen, Thomas H.; Slavin, James A.; Gilbert, Jason A.; Gloeckler, George] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Sarantos, Menelaos] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Sarantos, Menelaos] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA.
[Korth, Haje; Anderson, Brian J.; Krimigis, Stamatios M.; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Krimigis, Stamatios M.] Acad Athens, Off Space Res & Technol, Athens, Greece.
[Baker, Daniel N.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA.
[Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA.
RP Raines, JM (reprint author), Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
EM jraines@umich.edu
RI Sarantos, Menelaos/H-8136-2013; Slavin, James/H-3170-2012; McNutt,
Ralph/E-8006-2010; Gilbert, Jason/I-9020-2012
OI Slavin, James/0000-0002-9206-724X; McNutt, Ralph/0000-0002-4722-9166;
Gilbert, Jason/0000-0002-3182-7014
FU NASA's Graduate Student Research Program; MESSENGER mission; NASA
Discovery Program [NAS5-97271, NASW-00002]
FX This work was supported by NASA's Graduate Student Research Program and
the MESSENGER mission. The MESSENGER project is supported by the NASA
Discovery Program under contracts NAS5-97271 to The Johns Hopkins
University Applied Physics Laboratory and NASW-00002 to the Carnegie
Institution of Washington. NASA's Astrophysics Data System has been used
extensively for this work. J.M.R. thanks Jonathan W. Thomas for
designing and programming FIPS software libraries and Mark O. Stakhiv
for suggesting one of the key visualizations used in this work.
NR 64
TC 28
Z9 28
U1 1
U2 16
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD APR
PY 2013
VL 118
IS 4
BP 1604
EP 1619
DI 10.1029/2012JA018073
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 157UJ
UT WOS:000319924400019
ER
PT J
AU Glocer, A
Fok, M
Meng, X
Toth, G
Buzulukova, N
Chen, S
Lin, K
AF Glocer, A.
Fok, M.
Meng, X.
Toth, G.
Buzulukova, N.
Chen, S.
Lin, K.
TI CRCM+BATS-R-US two-way coupling
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
DE magnetosphere; Ring Current; MHD; Modeling; Model Coupling
ID BLOCK-ADAPTIVE GRIDS; RING CURRENT; INNER MAGNETOSPHERE; GEOMAGNETIC
STORMS; NOSE STRUCTURES; FIELD MODEL; MAGNETOHYDRODYNAMICS; SIMULATION;
PROTONS; SHEET
AB We present the coupling methodology and validation of a fully coupled inner and global magnetosphere code using the infrastructure provided by the Space Weather Modeling Framework (SWMF). In this model, the Comprehensive Ring Current Model (CRCM) represents the inner magnetosphere, while the BlockAdaptiveTree SolarWind RoeType Upwind Scheme (BATSRUS) represents the global magnetosphere. The combined model is a global magnetospheric code with a realistic ring current and consistent electric and magnetic fields. The computational performance of the model was improved to surpass realtime execution by the use of the Message Passing Interface (MPI) to parallelize the CRCM. Initial simulations under steady driving found that the coupled model resulted in a higher pressure in the inner magnetosphere and an inflated closed fieldline region as compared to simulations without innermagnetosphere coupling. Our validation effort was split into two studies. The first study examined the ability of the model to reproduce Dst for a range of events from the Geospace Environment Modeling (GEM) Dst Challenge. It also investigated the possibility of a baseline shift and compared two approaches to calculating Dst from the model. We found that the model did a reasonable job predicting Dst and SymH according to our two metrics of prediction efficiency and predicted yield. The second study focused on the specific case of the 22 July 2009 moderate geomagnetic storm. In this study, we directly compare model predictions and observations for Dst, THEMIS energy spectragrams, TWINS ENA images, and GOES 11 and 12 magnetometer data. The model did an adequate job reproducing trends in the data. Moreover, we found that composition can have a large effect on the result.
C1 [Glocer, A.; Fok, M.; Buzulukova, N.; Lin, K.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD USA.
[Meng, X.; Toth, G.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Buzulukova, N.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Buzulukova, N.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Chen, S.] Univ Space Res Assoc, Columbia, MD USA.
RP Glocer, A (reprint author), NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD USA.
EM alex.glocer-1@nasa.gov
RI Glocer, Alex/C-9512-2012; Toth, Gabor/B-7977-2013; feggans,
john/F-5370-2012; Fok, Mei-Ching/D-1626-2012; Meng, Xing/A-1929-2016
OI Glocer, Alex/0000-0001-9843-9094; Toth, Gabor/0000-0002-5654-9823;
FU NASA High-End Computing (HEC) Program through the NASA Advanced
Supercomputing (NAS) Division at Ames Research Center; NASA Center for
Climate Simulation (NCCS) at Goddard Space Flight Center
FX 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 and the NASA Center for Climate
Simulation (NCCS) at Goddard Space Flight Center. This work was carried
out as a part of the TWINS mission, which is part of NASA's Explorer
Program.
NR 52
TC 20
Z9 20
U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD APR
PY 2013
VL 118
IS 4
BP 1635
EP 1650
DI 10.1002/jgra.50221
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 157UJ
UT WOS:000319924400021
ER
PT J
AU Capossela, KM
Fabrizio, MC
Brill, RW
AF Capossela, Karen M.
Fabrizio, Mary C.
Brill, Richard W.
TI Migratory and within-estuary behaviors of adult Summer Flounder
(Paralichthys dentatus) in a lagoon system of the southern mid-Atlantic
Bight
SO FISHERY BULLETIN
LA English
DT Article
ID LOWER CHESAPEAKE BAY; JUVENILE SUMMER; NEW-JERSEY; WINTER FLOUNDER;
PSEUDOPLEURONECTES-AMERICANUS; ULTRASONIC TELEMETRY; ACOUSTIC TELEMETRY;
GROWTH LIMITATION; HABITAT DYNAMICS; 2 TEMPERATURES
AB We monitored the movements of 45 adult Summer Flounder (Paralichthys dentatus) between June 2007 and July 2008 through the use of passive acoustic telemetry to elucidate migratory and within-estuary behaviors in a lagoon system of the southern mid-Atlantic Bight. Between 8 June and 10 October 2007, fish resided primarily in the deeper (>3 m) regions of the system and exhibited low levels of large-scale (100s of meters) activity. Mean residence time within this estuarine lagoon system was conservatively estimated to be 130 days (range: 18-223 days), which is 1.5 times longer than the residence time previously reported for Summer Flounder in a similar estuarine habitat similar to 250 km to the north. The majority of fish remained within the lagoon system until mid-October, although some fish dispersed earlier and some of them appeared to disperse temporarily (i.e., exited the system for at least 14 consecutive days before returning). Larger fish were more likely to disperse before mid-October than smaller fish and may have moved to other estuaries or the inner continental shelf. Fish that dispersed after mid-October were more likely to return to the lagoon system the following spring than were fish that dispersed before mid-October. In 2008, fish returned to the system between 7 February and 7 April. Dispersals and returns most closely followed seasonal changes in mean water temperature, but photoperiod and other factors also may have played a role in large-scale movements of Summer Flounder.
C1 [Capossela, Karen M.; Fabrizio, Mary C.] Virginia Inst Marine Sci, Coll William & Mary, Dept Fisheries Sci, Gloucester Point, VA 23062 USA.
[Brill, Richard W.] NOAA, James J Howard Marine Sci Lab, Northeast Fisheries Sci Ctr, Natl Marine Fisheries Serv, Highlands, NJ 07732 USA.
RP Capossela, KM (reprint author), Maryland Dept Nat Resources, 301 Marine Acad Dr, Stevensville, MD 21666 USA.
EM kcapossela@dnr.state.md.us
OI Fabrizio, Mary/0000-0002-6115-5490
FU Oceanside Conservation Co., Inc.; Eastern Shore Graduate Research Grant
FX We thank the following individuals for their assistance with this study:
P. Bushnell, D. Gauthier, M. Henderson, J. Smith, and L. Smith. We
acknowledge M. Luckenbach, S. Fate, R. Bonniwell, and the support staff
of the Virginia Institute of Marine Science Eastern Shore Laboratory. We
also thank T. Targett for his comments on earlier drafts of this
manuscript and D. Fox for sharing detections from Delaware Bay. Funding
for this project was provided by the Oceanside Conservation Co., Inc.,
Student Research Grant, and the Eastern Shore Graduate Research Grant.
This is contribution 3251 from the Virginia Institute of Marine Science,
College of William & Mary.
NR 55
TC 11
Z9 11
U1 1
U2 22
PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE
PI SEATTLE
PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA
SN 0090-0656
EI 1937-4518
J9 FISH B-NOAA
JI Fish. Bull.
PD APR
PY 2013
VL 111
IS 2
BP 189
EP 201
DI 10.7755/FB.111.2.6
PG 13
WC Fisheries
SC Fisheries
GA 149HQ
UT WOS:000319310000006
ER
PT J
AU Taylor, RG
Scanlon, B
Doll, P
Rodell, M
van Beek, R
Wada, Y
Longuevergne, L
Leblanc, M
Famiglietti, JS
Edmunds, M
Konikow, L
Green, TR
Chen, JY
Taniguchi, M
Bierkens, MFP
MacDonald, A
Fan, Y
Maxwell, RM
Yechieli, Y
Gurdak, JJ
Allen, DM
Shamsudduha, M
Hiscock, K
Yeh, PJF
Holman, I
Treidel, H
AF Taylor, Richard G.
Scanlon, Bridget
Doell, Petra
Rodell, Matt
van Beek, Rens
Wada, Yoshihide
Longuevergne, Laurent
Leblanc, Marc
Famiglietti, James S.
Edmunds, Mike
Konikow, Leonard
Green, Timothy R.
Chen, Jianyao
Taniguchi, Makoto
Bierkens, Marc F. P.
MacDonald, Alan
Fan, Ying
Maxwell, Reed M.
Yechieli, Yossi
Gurdak, Jason J.
Allen, Diana M.
Shamsudduha, Mohammad
Hiscock, Kevin
Yeh, Pat J. -F.
Holman, Ian
Treidel, Holger
TI Ground water and climate change
SO NATURE CLIMATE CHANGE
LA English
DT Review
ID MURRAY-DARLING BASIN; UNITED-STATES; LAND-SURFACE; HIGH-PLAINS;
RECHARGE; IRRIGATION; AUSTRALIA; IMPACT; MODEL; RESOURCES
AB As the world's largest distributed store of fresh water, ground water plays a central part in sustaining ecosystems and enabling human adaptation to climate variability and change. The strategic importance of ground water for global water and food security will probably intensify under climate change as more frequent and intense climate extremes (droughts and floods) increase variability in precipitation, soil moisture and surface water. Here we critically review recent research assessing the impacts of climate on ground water through natural and human-induced processes as well as through groundwater-driven feedbacks on the climate system. Furthermore, we examine the possible opportunities and challenges of using and sustaining groundwater resources in climate adaptation strategies, and highlight the lack of groundwater observations, which, at present, limits our understanding of the dynamic relationship between ground water and climate.
C1 [Taylor, Richard G.] UCL, Dept Geog, London WC1E 6BT, England.
[Scanlon, Bridget] Univ Texas Austin, Jackson Sch Geosci, Bur Econ Geol, Austin, TX 78758 USA.
[Doell, Petra] Goethe Univ Frankfurt, Inst Phys Geog, D-60054 Frankfurt, Germany.
[Rodell, Matt] NASA, Hydrol Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[van Beek, Rens; Wada, Yoshihide; Bierkens, Marc F. P.] Univ Utrecht, Dept Phys Geog, NL-3508 TC Utrecht, Netherlands.
[Longuevergne, Laurent] Univ Rennes 1, Geosci Rennes, F-35042 Rennes, France.
[Leblanc, Marc] James Cook Univ, NCGRT, Sch Earth & Environm Sci, Cairns, Qld 4870, Australia.
[Famiglietti, James S.] Univ Calif Irvine, UC Ctr Hydrol Modelling, Irvine, CA 92617 USA.
[Edmunds, Mike] Univ Oxford, Sch Geog & Environm, Oxford OX1 3QY, England.
[Konikow, Leonard] US Geol Survey, Reston, VA 20192 USA.
[Green, Timothy R.] ARS, Agr Syst Res Unit, USDA, Ft Collins, CO 80526 USA.
[Chen, Jianyao] Sun Yat Sen Univ, Sch Geog & Planning, Guangzhou 510275, Guangdong, Peoples R China.
[Taniguchi, Makoto] Res Inst Humanity & Nat, Kyoto 6308047, Japan.
[MacDonald, Alan] British Geol Survey, Edinburgh EH9 3LA, Midlothian, Scotland.
[Fan, Ying] Rutgers State Univ, Dept Earth & Planetary Sci, New Brunswick, NJ 08901 USA.
[Maxwell, Reed M.] Colorado Sch Mines, Dept Geol & Geol Engn, Golden, CO 80401 USA.
[Yechieli, Yossi] Geol Survey Israel, IL-95501 Jerusalem, Israel.
[Gurdak, Jason J.] San Francisco State Univ, Dept Geosci, San Francisco, CA 94132 USA.
[Allen, Diana M.] Simon Fraser Univ, Dept Earth Sci, Burnaby, BC V5A 1S6, Canada.
[Shamsudduha, Mohammad] UCL, Inst Risk & Disaster Reduct, London WC1E 6BT, England.
[Hiscock, Kevin] Univ E Anglia, Sch Environm Sci, Norwich NR4 7TJ, Norfolk, England.
[Yeh, Pat J. -F.] UNESCO, Int Ctr Water Hazard & Risk Management ICHARM, Tsukuba, Ibaraki 1538505, Japan.
[Holman, Ian] Cranfield Univ, Environm Sci & Technol Dept, Milton Keynes MK43 0AL, Bucks, England.
[Treidel, Holger] UNESCO IHP, Div Water Sci, F-75732 Paris 15, France.
RP Taylor, RG (reprint author), UCL, Dept Geog, Mortimer St, London WC1E 6BT, England.
EM r.taylor@geog.ucl.ac.uk
RI Maxwell, Reed/D-7980-2013; Doll, Petra/A-3784-2009; YEH,
Pat/B-2758-2011; Wada, Yoshihide/F-3595-2012; Rodell,
Matthew/E-4946-2012; James Cook University, TESS/B-8171-2012; TropWATER,
Research ID/P-1401-2014; Allen, Diana/A-4215-2010; Taniguchi,
Makoto/E-3335-2012; Longuevergne, Laurent /F-4641-2010; van Beek,
Rens/B-4904-2014
OI Holman, Ian/0000-0002-5263-7746; Maxwell, Reed/0000-0002-1364-4441;
Doll, Petra/0000-0003-2238-4546; YEH, Pat/0000-0001-7629-3362; Wada,
Yoshihide/0000-0003-4770-2539; Rodell, Matthew/0000-0003-0106-7437;
Allen, Diana/0000-0003-3541-2470; Taniguchi, Makoto/0000-0001-7416-0275;
Longuevergne, Laurent /0000-0003-3169-743X; van Beek,
Rens/0000-0002-4758-108X
NR 98
TC 191
Z9 193
U1 51
U2 417
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1758-678X
J9 NAT CLIM CHANGE
JI Nat. Clim. Chang.
PD APR
PY 2013
VL 3
IS 4
BP 322
EP 329
DI 10.1038/NCLIMATE1744
PG 8
WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric
Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 150OL
UT WOS:000319400400008
ER
PT J
AU Middleton, EM
Ungar, SG
Mandl, DJ
Ong, L
Frye, SW
Campbell, PE
Landis, DR
Young, JP
Pollack, NH
AF Middleton, Elizabeth M.
Ungar, Stephen G.
Mandl, Daniel J.
Ong, Lawrence
Frye, Stuart W.
Campbell, Petya E.
Landis, David R.
Young, Joseph P.
Pollack, Nathan H.
TI The Earth Observing One (EO-1) Satellite Mission: Over a Decade in Space
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Advanced Land Imager; ALI; Earth; EO-1; Hyperion; imaging spectrometer;
remote sensing
ID ADVANCED LAND IMAGER; LEAF-AREA INDEX; AUTONOMOUS SCIENCECRAFT
EXPERIMENT; PEARL RIVER ESTUARY; HYPERION DATA; HYPERSPECTRAL IMAGE;
ATMOSPHERIC CORRECTION; APPALACHIAN MOUNTAINS; CHLOROPHYLL CONTENT;
VEGETATION INDEXES
AB The Earth Observing One (EO-1) satellite was launched in November 2000 as a technology demonstration mission with an estimated 1-year lifespan. It has now successfully completed 12 years of high spatial resolution imaging operations from low Earth orbit. EO-1's two main instruments, Hyperion and the Advanced Land Imager (ALI), have both served as prototypes for new generation satellite missions. ALI, an innovative multispectral instrument, is the forerunner of the Operational Land Imager (OLI) onboard the Landsat Data Continuity Mission's (LDCM) Landsat-8 satellite, recently launched in Feb. 2013. Hyperion, a hyperspectral instrument, serves as the heritage orbital spectrometer for future global platforms, including the proposed NASA Hyperspectral Infrared Imager (HyspIRI) and the forthcoming (in 2017) German satellite, EnMAP.
This JSTARS Special Issue is dedicated to EO-1. This paper serves as an introduction to the Hyperion and ALI instruments, their capabilities, and the important contributions this mission has made to the science and technology communities. This paper also provides an overview of the EO-1 mission, including the several operational phases which have characterized its lifetime. It also briefly describes calibration and validation activities, and gives an overview of the spin-off technologies, including disaster monitoring and new Web-based tools which can be adapted for use in future missions.
C1 [Middleton, Elizabeth M.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Ungar, Stephen G.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Mandl, Daniel J.] NASA, Goddard Space Flight Ctr, Software Syst Engn Branch, Greenbelt, MD 20771 USA.
[Ong, Lawrence; Pollack, Nathan H.] Syst Sci & Applicat Inc, Lanham, MD 20706 USA.
[Frye, Stuart W.; Young, Joseph P.] SGT, Greenbelt, MD 20770 USA.
[Campbell, Petya E.] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA.
[Landis, David R.] Sigma Space Corp Inc, Lanham, MD 20706 USA.
RP Middleton, EM (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Code 618, Greenbelt, MD 20771 USA.
RI Campbell, Petya/G-4931-2013; Campbell, Petya/L-7486-2013
OI Campbell, Petya/0000-0002-0505-4951; Campbell, Petya/0000-0002-0505-4951
NR 101
TC 29
Z9 30
U1 10
U2 61
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD APR
PY 2013
VL 6
IS 2
SI SI
BP 243
EP 256
DI 10.1109/JSTARS.2013.2249496
PN 1
PG 14
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA 148VV
UT WOS:000319277100001
ER
PT J
AU Chien, S
Mclaren, D
Tran, D
Davies, AG
Doubleday, J
Mandl, D
AF Chien, Steve
Mclaren, David
Tran, Daniel
Davies, Ashley Gerard
Doubleday, Joshua
Mandl, Daniel
TI Onboard Product Generation on Earth Observing One: A Pathfinder for the
Proposed Hyspiri Mission Intelligent Payload Module
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Cryosphere; flooding; instrument data processing; onboard processing;
thermal analysis; volcanoes
ID AUTONOMOUS SCIENCECRAFT EXPERIMENT; MERIS; EO-1
AB The proposed HyspIRI mission is evaluating a X-band Direct Broadcast capability that would enable data to be delivered to ground stations virtually as it is acquired. However the HyspIRI VSWIR and TIR instruments are expected to produce over 800 x 10(6) bits per second of data while the Direct Broadcast capability is approximately 10 x 10(6) bits per second for a similar to 80x oversubscription. In order to address this data throughput mismatch a Direct Broadcast concept called the Intelligent Payload Module (IPM) has been developed to determine which data to downlink based on both the type of surface the spacecraft is overlying and onboard processing of the data to detect events. For example, when the spacecraft is overlying polar regions it might downlink a snow/ice product. Additionally the onboard software would search for thermal signatures indicative of a volcanic event or wild fire and downlink summary information (extent, spectra) when detected.
Earth Observing One (EO-1) has served as a test bed and pathfinder for this type of onboard product generation. As part of the Autonomous Sciencecraft (ASE), EO-1 implemented in flight software the ability to analyze and develop products for a limited swath of the Hyperion hyperspectral instrument onboard the spacecraft. In a series of technology demonstrations that became part of the operational EO-1 system over 5000 science products have been generated onboard EO-1 and down linked via engineering S-band contacts, a routine automated process that continues to this day. We describe the onboard products demonstrated in EO-1 operations and show how they have paved the way for the HyspIRI Intelligent Payload Module concept.
C1 [Chien, Steve] CALTECH, Jet Prop Lab, Artificial Intelligence Lab, Pasadena, CA 91125 USA.
[Mclaren, David; Tran, Daniel; Doubleday, Joshua] CALTECH, Jet Prop Lab, Artificial Intelligence Grp, Pasadena, CA USA.
[Davies, Ashley Gerard] CALTECH, Jet Prop Lab, Earth & Space Sci Div, Pasadena, CA USA.
[Mandl, Daniel] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Chien, S (reprint author), CALTECH, Jet Prop Lab, Artificial Intelligence Lab, Pasadena, CA 91125 USA.
FU National Aeronautics and Space Administration
FX Portions of this work were performed by the Jet Propulsion Laboratory,
California Institute of Technology, under contract from the National
Aeronautics and Space Administration.
NR 20
TC 7
Z9 7
U1 0
U2 7
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD APR
PY 2013
VL 6
IS 2
SI SI
BP 257
EP 264
DI 10.1109/JSTARS.2013.2249574
PN 1
PG 8
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA 148VV
UT WOS:000319277100002
ER
PT J
AU Huemmrich, KF
Gamon, JA
Tweedie, CE
Campbell, PKE
Landis, DR
Middleton, EM
AF Huemmrich, Karl Fred
Gamon, John A.
Tweedie, Craig E.
Campbell, Petya K. Entcheva
Landis, David R.
Middleton, Elizabeth M.
TI Arctic Tundra Vegetation Functional Types Based on Photosynthetic
Physiology and Optical Properties
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Environmental factors; ecosystems; geoscience and remote sensing;
hyperspectral imaging; remote sensing; vegetation mapping
ID CLIMATE-CHANGE; REFLECTANCE SPECTRA; GLOBAL CHANGE; CARBON-CYCLE; CO2
FLUX; ECOSYSTEMS; ALASKA; PRODUCTIVITY; RESPONSES; LICHENS
AB Non-vascular plants (lichens and mosses) are significant components of tundra landscapes and may respond to climate change differently from vascular plants affecting ecosystem carbon balance. Remote sensing provides critical tools for monitoring plant cover types, as optical signals provide a way to scale from plot measurements to regional estimates of biophysical properties, for which spatial-temporal patterns may be analyzed. Gas exchange measurements were collected for pure patches of key vegetation functional types (lichens, mosses, and vascular plants) in sedge tundra at Barrow AK. These functional types were found to have three significantly different values of light use efficiency (LUE) with values of 0.013 +/- 0.001, 0.0018 +/- 0.0002, and 0.0012 +/- 0.0001 mol C mol(-1) absorbed quanta for vascular plants, mosses and lichens, respectively. Discriminant analysis of the spectra reflectance of these patches identified five spectral bands that separated each of these vegetation functional types as well as nongreen material (bare soil, standing water, and dead leaves). These results were tested along a 100 m transect where midsummer spectral reflectance and vegetation coverage were measured at one meter intervals.
Along the transect, area-averaged canopy LUE estimated from coverage fractions of the three functional types varied widely, even over short distances. The patch-level statistical discriminant functions applied to in situ hyperspectral reflectance data collected along the transect successfully unmixed cover fractions of the vegetation functional types. The unmixing functions, developed from the transect data, were applied to 30 m spatial resolution Earth Observing-1 Hyperion imaging spectrometer data to examine variability in distribution of the vegetation functional types for an area near Barrow, AK. Spatial variability of LUE was derived from the observed functional type distributions. Across this landscape, a fivefold variation in tundra LUE was observed. LUE calculated from the functional type cover fractions was also correlated to a spectral vegetation index developed to detect vegetation chlorophyll content. The concurrence of these alternate methods suggest that hyperspectral remote sensing can distinguish functionally distinct vegetation types and can be used to develop regional estimates of photosynthetic LUE in tundra landscapes.
C1 [Huemmrich, Karl Fred; Campbell, Petya K. Entcheva] Univ Maryland Baltimore Cty, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gamon, John A.] Univ Alberta, Edmonton, AB T6G 2R3, Canada.
[Tweedie, Craig E.] Univ Texas El Paso, El Paso, TX 79968 USA.
[Landis, David R.] Sigma Space Corp, Lanham, MD 20706 USA.
[Middleton, Elizabeth M.] NASA, Greenbelt, MD 20771 USA.
RP Huemmrich, KF (reprint author), Univ Maryland Baltimore Cty, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM karl.f.huemmrich@nasa.gov
RI Campbell, Petya/G-4931-2013; Campbell, Petya/L-7486-2013; Gamon,
John/A-2641-2014
OI Campbell, Petya/0000-0002-0505-4951; Campbell,
Petya/0000-0002-0505-4951; Gamon, John/0000-0002-8269-7723
FU IARC through the Desert Research Institute, Reno, Nevada, USA
FX Manuscript received February 23, 2012; revised August 03, 2012; accepted
February 27, 2013. Date of publication April 24, 2013; date of current
version May 13, 2013. Funding for the field component of this study was
provided by IARC to J. A. Gamon and K. F. Huemmrich through the Desert
Research Institute, Reno, Nevada, USA.
NR 50
TC 9
Z9 9
U1 4
U2 71
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 APR
PY 2013
VL 6
IS 2
SI SI
BP 265
EP 275
DI 10.1109/JSTARS.2013.2253446
PN 1
PG 11
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA 148VV
UT WOS:000319277100003
ER
PT J
AU Campbell, PKE
Middleton, EM
Thome, KJ
Kokaly, RF
Huemmrich, KF
Lagomasino, D
Novick, KA
Brunsell, NA
AF Campbell, Petya K. Entcheva
Middleton, Elizabeth M.
Thome, Kurt J.
Kokaly, Raymond F.
Huemmrich, Karl Fred
Lagomasino, David
Novick, Kimberly A.
Brunsell, Nathaniel A.
TI EO-1 Hyperion Reflectance Time Series at Calibration and Validation
Sites: Stability and Sensitivity to Seasonal Dynamics
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Earth Observing-1; eddy covariance; flux sites; forest; grassland;
Hyperion; imaging spectroscopy; Pseudo-Invariant Calibration Sites;
reflectance; remote sensing; seasonal carbon dynamics; spectral time
series; vegetation function; woodland
ID RAILROAD VALLEY PLAYA; NET ECOSYSTEM EXCHANGE; ABSORPTION FEATURES;
HYPERSPECTRAL DATA; CARBON; GRADIENT; SENSORS; FLUXES; FOREST;
RESPIRATION
AB This study evaluated Earth Observing 1 (EO-1) Hyperion reflectance time series at established calibration sites to assess the instrument stability and suitability for monitoring vegetation functional parameters. Our analysis using three pseudo-invariant calibration sites in North America indicated that the reflectance time series are devoid of apparent spectral trends and their stability consistently is within 2.5-5 percent throughout most of the spectral range spanning the 12+ year data record. Using three vegetated sites instrumented with eddy covariance towers, the Hyperion reflectance time series were evaluated for their ability to determine important variables of ecosystem function. A number of narrowband and derivative vegetation indices (VI) closely described the seasonal profiles in vegetation function and ecosystem carbon exchange (e.g., net and gross ecosystem productivity) in three very different ecosystems, including a hardwood forest and tallgrass prairie in North America, and a Miombo woodland in Africa. Our results demonstrate the potential for scaling the carbon flux tower measurements to local and regional landscape levels. The VIs with stronger relationships to the CO2 parameters were derived using continuous reflectance spectra and included wavelengths associated with chlorophyll content and/or chlorophyll fluorescence. Since these indices cannot be calculated from broadband multispectral instrument data, the opportunity to exploit these spectrometer-based VIs in the future will depend on the launch of satellites such as EnMAP and HyspIRI. This study highlights the practical utility of space-borne spectrometers for characterization of the spectral stability and uniformity of the calibration sites in support of sensor cross-comparisons, and demonstrates the potential of narrowband VIs to track and spatially extend ecosystem functional status as well as carbon processes measured at flux towers.
C1 [Campbell, Petya K. Entcheva; Huemmrich, Karl Fred] Univ Maryland Baltimore Cty, NASA, GSFC, Greenbelt, MD 20771 USA.
[Middleton, Elizabeth M.] NASA, Goddard Space Flight Ctr, Lab Biospher Sci, Greenbelt, MD 20771 USA.
[Thome, Kurt J.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Kokaly, Raymond F.] USGS, Denver, CO USA.
[Lagomasino, David] Florida Int Univ, Hydrogeol Lab, Miami, FL 33199 USA.
[Novick, Kimberly A.] US Forest Serv, USDA, Coweeta Hydrol Lab, So Res Stn, Otto, NC USA.
[Brunsell, Nathaniel A.] Univ Kansas, Dept Geog, Lawrence, KS 66045 USA.
RP Campbell, PKE (reprint author), Univ Maryland Baltimore Cty, NASA, GSFC, Greenbelt, MD 20771 USA.
EM petya.campbell@nasa.gov
RI Campbell, Petya/G-4931-2013; Thome, Kurtis/D-7251-2012; Campbell,
Petya/L-7486-2013; Lagomasino, David/P-8413-2015; Kokaly,
Raymond/A-6817-2017
OI Campbell, Petya/0000-0002-0505-4951; Campbell,
Petya/0000-0002-0505-4951; Lagomasino, David/0000-0003-4008-5363;
Kokaly, Raymond/0000-0003-0276-7101
FU U.S. Department of Energy (DOE) through the Office of Biological and
Environmental Research (BER) Terrestrial Carbon Processes (TCP) program
[10509-0152, DE-FG02-00ER53015, DE-FG02-95ER62083]
FX Manuscript received March 15, 2012; revised July 20, 2012 and November
02, 2012; accepted November 25, 2012. Date of publication April 24,
2013; date of current version May 13, 2013. This work was supported by
the U.S. Department of Energy (DOE) through the Office of Biological and
Environmental Research (BER) Terrestrial Carbon Processes (TCP) program
(Grants 10509-0152, DE-FG02-00ER53015, and DE-FG02-95ER62083).
NR 53
TC 15
Z9 15
U1 1
U2 35
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD APR
PY 2013
VL 6
IS 2
SI SI
BP 276
EP 290
DI 10.1109/JSTARS.2013.2246139
PN 1
PG 15
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA 148VV
UT WOS:000319277100004
ER
PT J
AU Chien, S
Doubleday, J
Mclaren, D
Tran, D
Tanpipat, V
Chitradon, R
Boonya-aroonnet, S
Thanapakpawin, P
Mandl, D
AF Chien, Steve
Doubleday, Joshua
Mclaren, David
Tran, Daniel
Tanpipat, Veerachai
Chitradon, Royol
Boonya-aroonnet, Surajate
Thanapakpawin, Porranee
Mandl, Daniel
TI Monitoring Flooding in Thailand Using Earth Observing One in a Sensorweb
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Flooding; hydrological modeling; in-situ sensing; space-based remote
sensing
AB The Earth Observing One (EO-1) mission has been a pathfinder in demonstrating autonomous operations paradigms. In 2010-2012 (and continuing), EO-1 has been supporting sensorweb operations to enable autonomous tracking of flooding in Thailand. In this approach, the Moderate Imaging Spectrometer (MODIS) is used to perform broad-scale monitoring to track flooding at the regional level (500 m/pixel) and EO-1 is autonomously tasked in response to alerts to acquire higher resolution (30 m/pixel) Advanced Land Imager (ALI) data. This data is then automatically processed to derive products such as surface water extent and volumetric water estimates. These products are then automatically pushed to relevant authorities in Thailand for use in damage estimation, relief efforts, and damage mitigation.
EO-1 has served as a testbed and pathfinder to this type of sensorweb operations. Beginning with EO-1, these techniques for monitoring are being extended to other space sensors (such as Radarsat-2, Landsat, Worldview-2, TRMM) and integrated with hydrological models, and integration with in-situ sensors.
C1 [Chien, Steve; Doubleday, Joshua; Mclaren, David; Tran, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Tanpipat, Veerachai] Thaiflood Net, Remote Sensing, Bangkok, Thailand.
[Mandl, Daniel] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Chien, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM imatanpipat@hotmail.com
FU National Aeronautics and Space Administration
FX Portions of this work were performed by the Jet Propulsion Laboratory,
California Institute of Technology, under contract from the National
Aeronautics and Space Administration.
NR 22
TC 4
Z9 4
U1 0
U2 15
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 APR
PY 2013
VL 6
IS 2
SI SI
BP 291
EP 297
DI 10.1109/JSTARS.2013.2247974
PN 1
PG 7
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA 148VV
UT WOS:000319277100005
ER
PT J
AU Mandl, D
Frye, S
Cappelaere, P
Handy, M
Policelli, F
Katjizeu, M
Van Langenhove, G
Aube, G
Saulnier, JF
Sohlberg, R
Silva, JA
Kussul, N
Skakun, S
Ungar, SG
Grossman, R
Szarzynski, J
AF Mandl, Daniel
Frye, Stuart
Cappelaere, Pat
Handy, Matthew
Policelli, Fritz
Katjizeu, McCloud
Van Langenhove, Guido
Aube, Guy
Saulnier, Jean-Francois
Sohlberg, Rob
Silva, Julie A.
Kussul, Nataliia
Skakun, Sergii
Ungar, Stephen G.
Grossman, Robert
Szarzynski, Joerg
TI Use of the Earth Observing One (EO-1) Satellite for the Namibia
SensorWeb Flood Early Warning Pilot
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Earth Observing One (EO-1); Flood Early Warning; sensor systems and
applications; SensorWeb
AB The Earth Observing One (EO-1) satellite was launched in November 2000 as a one year technology demonstration mission for a variety of space technologies. After the first year, it was used as a pathfinder for the creation of SensorWebs. A SensorWeb is the integration of a variety of space, airborne and ground sensors into a loosely coupled collaborative sensor system that automatically provides useful data products. Typically, a SensorWeb is comprised of heterogeneous sensors tied together with an open messaging architecture and web services. SensorWebs provide easier access to sensor data, automated data product production and rapid data product delivery. Disasters are the perfect arena to test SensorWeb functionality since emergency workers and managers need easy and rapid access to satellite, airborne and in-situ sensor data as decision support tools. The Namibia Early Flood Warning SensorWeb pilot project was established to experiment with various aspects of sensor interoperability and SensorWeb functionality. The SensorWeb system features EO-1 data along with other data sets from such satellites as Radarsat, Terra and Aqua. Finally, the SensorWeb team began to examine how to measure economic impact of SensorWeb technology infusion. This paper describes the architecture and software components that were developed along with performance improvements that were experienced. Also, problems and challenges that were encountered are described along with a vision for future enhancements to mitigate some of the problems.
C1 [Mandl, Daniel] NASA, Goddard Space Flight Ctr, Software Syst Engn Branch, Greenbelt, MD 20771 USA.
[Frye, Stuart] SGT, Greenbelt, MD 20770 USA.
[Cappelaere, Pat] Vightel Inc, Ellicott City, MD 21043 USA.
[Handy, Matthew] NASA, Goddard Space Flight Ctr, Ground Software Syst Branch, Greenbelt, MD 20771 USA.
[Policelli, Fritz] NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD 20771 USA.
[Katjizeu, McCloud; Van Langenhove, Guido] Minist Agr Water & Forestry, Dept Hydrol, Windhoek, Namibia.
[Aube, Guy; Saulnier, Jean-Francois] Canadian Space Agcy, St Hubert, PQ J3Y 8Y9, Canada.
[Sohlberg, Rob; Silva, Julie A.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Kussul, Nataliia; Skakun, Sergii] NSAU, Space Res Inst NASU, UA-03680 Kiev, Ukraine.
[Ungar, Stephen G.] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Grossman, Robert] Univ Chicago, Computat Inst, Searle Chem Lab, Chicago, IL 60637 USA.
[Szarzynski, Joerg] United Nations Univ, D-53113 Bonn, Germany.
RP Mandl, D (reprint author), NASA, Goddard Space Flight Ctr, Software Syst Engn Branch, Code 581, Greenbelt, MD 20771 USA.
EM daniel.j.mandl@nasa.gov
RI Kussul, Nataliia/N-8649-2014; Skakun, Sergii/E-2769-2012
OI Kussul, Nataliia/0000-0002-9704-9702; Skakun, Sergii/0000-0002-9039-0174
NR 9
TC 8
Z9 8
U1 0
U2 10
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD APR
PY 2013
VL 6
IS 2
SI SI
BP 298
EP 308
DI 10.1109/JSTARS.2013.2255861
PN 1
PG 11
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA 148VV
UT WOS:000319277100006
ER
PT J
AU Abrams, M
Pieri, D
Realmuto, V
Wright, R
AF Abrams, Michael
Pieri, Dave
Realmuto, Vince
Wright, Robert
TI Using EO-1 Hyperion Data as HyspIRI Preparatory Data Sets for
Volcanology Applied to Mt Etna, Italy
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Hyperspectral imaging; infrared image sensors; volcanic activity
ID MOUNT-ETNA; LAVA-FLOW; INFRARED DATA; LASCAR VOLCANO; SPECTRORADIOMETER
MODIS; KILAUEA VOLCANO; FLANK ERUPTION; DOME GROWTH; RADIOMETER;
SATELLITE
AB One of the main goals of the Hyperspectral and Infrared Imager (HyspIRI) mission is to provide global observations of surface attributes at local and landscape spatial scales (tens of meters to hundreds of kilometers) to map volcanic gases and surface temperatures, which are identified as indicators of impending volcanic hazards, as well as plume ejecta which pose risks to aircraft and people and property downwind. Our project has created precursor HyspIRI data sets for volcanological analyses, using existing data over Mt. Etna, Italy. We have identified 28 EO-1 Hyperion data acquisitions, and 12 near-coincident ASTER data acquisitions, covering six eruptive periods between 2001 and 2010. These data sets provide us with 30 m hyperspectral VSWIR data and 90 m multispectral TIR data (satellite). They allowed us to examine temporal sequences of several Etnaean eruptions. We addressed the following critical questions, directly related to understanding eruption hazards: 1) What do changes in SO2 emissions tell us about a volcano's activity? How well do these measurements compare with ground-based COSPEC measurements? 2) How do we use measurements of lava flow temperature and volume to predict advances of the flow front? 3) What do changes in lava lake temperatures and energy emissions tell us about possible eruptive behavior?
C1 [Abrams, Michael; Pieri, Dave; Realmuto, Vince] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wright, Robert] Univ Hawaii, Honolulu, HI 96822 USA.
RP Abrams, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
FU National Aeronautics and Space Administration
FX Manuscript received February 29, 2012; revised May 28, 2012 and July 18,
2012; accepted August 28, 2012. Date of publication March 12, 2013; date
of current version May 13, 2013. Work by Abrams, Realmuto, and Pieri was
done at the California Institute of Technology, Jet Propulsion
Laboratory, under contract with the National Aeronautics and Space
Administration.
NR 49
TC 7
Z9 9
U1 1
U2 22
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD APR
PY 2013
VL 6
IS 2
SI SI
BP 375
EP 385
DI 10.1109/JSTARS.2012.2224095
PN 1
PG 11
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA 148VV
UT WOS:000319277100013
ER
PT J
AU Chander, G
Angal, A
Choi, T
Xiong, XX
AF Chander, Gyanesh
Angal, Amit
Choi, Taeyoung
Xiong, Xiaoxiong
TI Radiometric Cross-Calibration of EO-1 ALI With L7 ETM+ and Terra MODIS
Sensors Using Near-Simultaneous Desert Observations
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Arabia 1; EO-1 ALI and Hyperion; L7 ETM+; Libya 4; Mauritania 2;
radiometric cross-calibration; RSR; SBAF; Sudan 1; Terra MODIS
ID ADVANCED LAND IMAGER; OPTICAL SATELLITE SENSORS; ON-ORBIT; SITES;
PERFORMANCE; SAHARAN; LANDSAT-7-ETM+; SPECTROMETER; HYPERION; DESIGN
AB The Earth Observing-1 (EO-1) satellite was launched on November 21, 2000, as part of a one-year technology demonstration mission. The mission was extended because of the value it continued to add to the scientific community. EO-1 has now been operational for more than a decade, providing both multispectral and hyperspectral measurements. As part of the EO-1 mission, the Advanced Land Imager (ALI) sensor demonstrates a potential technological direction for the next generation of Landsat sensors. To evaluate the ALI sensor capabilities as a precursor to the Operational Land Imager (OLI) onboard the Landsat Data Continuity Mission (LDCM, or Landsat 8 after launch), its measured top-of-atmosphere (TOA) reflectances were compared to the well-calibrated Landsat 7 (L7) Enhanced Thematic Mapper Plus (ETM+) and the Terra Moderate Resolution Imaging Spectroradiometer (MODIS) sensors in the reflective solar bands (RSB). These three satellites operate in a near-polar, sun-synchronous orbit 705 km above the Earth's surface. EO-1 was designed to fly one minute behind L7 and approximately 30 minutes in front of Terra. In this configuration, all the three sensors can view near-identical ground targets with similar atmospheric, solar, and viewing conditions. However, because of the differences in the relative spectral response (RSR), the measured physical quantities can be significantly different while observing the same target. The cross-calibration of ALI with ETM+ and MODIS was performed using near-simultaneous surface observations based on image statistics from areas observed by these sensors over four desert sites (Libya 4, Mauritania 2, Arabia 1, and Sudan 1). The differences in the measured TOA reflectances due to RSR mismatches were compensated by using a spectral band adjustment factor (SBAF), which takes into account the spectral profile of the target and the RSR of each sensor. For this study, the spectral profile of the target comes from the near-simultaneous EO-1 Hyperion data over these sites. The results indicate that the TOA reflectance measurements for ALI agree with those of ETM+ and MODIS to within 5% after the application of SBAF.
C1 [Chander, Gyanesh] US Geol Survey, Earth Resources Observat & Sci EROS Ctr, SGT Inc, Sioux Falls, SD 57198 USA.
[Angal, Amit] Sci Syst & Applicat SSAI Inc, Lanham, MD 20706 USA.
[Choi, Taeyoung] Sigma Space Corp, Lanham, MD 20706 USA.
[Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Chander, G (reprint author), US Geol Survey, Earth Resources Observat & Sci EROS Ctr, SGT Inc, Sioux Falls, SD 57198 USA.
EM gchander@usgs.gov
RI Richards, Amber/K-8203-2015
FU U.S. Geological Survey [G10PC00044]
FX Manuscript received March 09, 2012; revised September 03, 2012, January
23, 2013; accepted March 06, 2013. Date of publication April 04, 2013;
date of current version May 13, 2013. This work was performed under U.S.
Geological Survey contract G10PC00044.
NR 40
TC 5
Z9 5
U1 13
U2 44
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD APR
PY 2013
VL 6
IS 2
SI SI
BP 386
EP 399
DI 10.1109/JSTARS.2013.2251999
PN 1
PG 14
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA 148VV
UT WOS:000319277100014
ER
PT J
AU McCorkel, J
Thome, K
Ong, L
AF McCorkel, Joel
Thome, Kurtis
Ong, Lawrence
TI Vicarious Calibration of EO-1 Hyperion
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Hyperion; imaging spectrometer; lunar calibration; radiometric
calibration; vicarious calibration
ID ABSOLUTE RADIOMETRIC CALIBRATION; REFLECTANCE-BASED METHOD; ON-ORBIT
CALIBRATION; IMAGING SPECTROMETER; MOON; IRRADIANCE; INSTRUMENT;
RADIANCE; AVIRIS; ASTER
AB The Hyperion imaging spectrometer on the Earth Observing-1 satellite is the first high-spatial resolution imaging spectrometer to routinely acquire science-grade data from orbit. Data gathered with this instrument needs to be quantitative and accurate in order to derive meaningful information about ecosystem properties and processes. Also, comprehensive and long-term ecological studies require these data to be comparable over time, between coexisting sensors and between generations of follow-on sensors. One method to assess the radiometric calibration is the reflectance-based approach, a common technique used for several other earth science sensors covering similar spectral regions. This work presents results of radiometric calibration of Hyperion based on the reflectance-based approach of vicarious calibration implemented by University of Arizona during 2001-2005. These results show repeatability to the 2% level and accuracy on the 3-5% level for spectral regions not affected by strong atmospheric absorption. Knowledge of the stability of the Hyperion calibration from moon observations allows for an average absolute calibration based on the reflectance-based results to be determined and applicable for the lifetime of Hyperion.
C1 [McCorkel, Joel; Thome, Kurtis] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
[Ong, Lawrence] NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA.
RP McCorkel, J (reprint author), NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
EM joel.mccorkel@nasa.gov; kurtis.thome@nasa.gov; lawrence.ong@nasa.gov
RI Thome, Kurtis/D-7251-2012; McCorkel, Joel/D-4454-2012
OI McCorkel, Joel/0000-0003-2853-2036
NR 31
TC 12
Z9 12
U1 4
U2 39
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 APR
PY 2013
VL 6
IS 2
SI SI
BP 400
EP 407
DI 10.1109/JSTARS.2012.2225417
PN 1
PG 8
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA 148VV
UT WOS:000319277100015
ER
PT J
AU Cappelaere, P
Sanchez, S
Bernabe, S
Scuri, A
Mandl, D
Plaza, A
AF Cappelaere, Pat
Sanchez, Sergio
Bernabe, Sergio
Scuri, Antonio
Mandl, Daniel
Plaza, Antonio
TI Cloud Implementation of a Full Hyperspectral Unmixing Chain Within the
NASA Web Coverage Processing Service for EO-1
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Earth Observing One (EO-1); hyperion; hyperspectral imaging; NASA
SensorWeb; spectral unmixing; Web Coverage Processing Service (WCPS)
ID IMAGERY
AB The launch of the NASA Earth Observing 1 (EO-1) platform in November 2000 marked the establishment of spaceborne hyperspectral technology for land imaging. The Hyperion sensor onboard EO-1 operates in the 0.4-2.5 micrometer spectral range, with 10 nanometer spectral resolution and 30-meter spatial resolution. Spectral unmixing has been one of the most successful approaches to analyze Hyperion data since its launch. It estimates the abundance of spectrally pure constituents (endmembers) in each observation collected by the sensor. Due to the high spectral dimensionality of Hyperion data, unmixing is a very time-consuming operation. In this paper, we develop a cloud implementation of a full hyperspectral unmixing chain made up of the following steps: 1) dimensionality reduction; 2) automatic endmember identification; and 3) fully constrained abundance estimation. The unmixing chain will be available online within the Web Coverage Processing Service (WCPS), an image processing framework that can run on the cloud, as part of the NASA SensorWeb suite of web services. The proposed implementation has been demonstrated using the EO-1 Hyperion imagery. Our experimental results with a hyperspectral scene collected over the Okavango Basin in Botswana suggest the (present and future) potential of spectral unmixing for improved exploitation of spaceborne hyperspectral data. The integration of the unmixing chain in the WCPS framework as part of the NASA SensorWeb suite of web services is just the start of an international collaboration in which many more processing algorithms will be made available to the community through this service. This paper is not so much focused on the theory and results of unmixing (widely demonstrated in other contributions) but about the process and added value of the proposed contribution for ground processing on the cloud and onboard migration of those algorithms to support the generation of low-latency products for new airborne/spaceborne missions.
C1 [Cappelaere, Pat] Vightel Corp, Ellicott City, MD 21043 USA.
[Sanchez, Sergio; Bernabe, Sergio; Plaza, Antonio] Univ Extremadura, Hyperspectral Comp Lab, Calceres 10003, Spain.
[Scuri, Antonio] Pontificia Univ Catolica Rio de Janeiro PUC Rio, Tecgraf, Rio De Janeiro, Brazil.
[Mandl, Daniel] NASA, Goddard Space Flight Ctr, Software Syst Branch, Greenbelt, MD 20771 USA.
RP Cappelaere, P (reprint author), Vightel Corp, Ellicott City, MD 21043 USA.
RI Plaza, Antonio/C-4455-2008; Bernabe Garcia, Sergio/H-5350-2015
OI Plaza, Antonio/0000-0002-9613-1659; Bernabe Garcia,
Sergio/0000-0001-9916-0634
FU Spanish Ministry of Science and Innovation (CEOS-SPAIN project)
[AYA2011-29334-C02-02]; Spanish Ministry of Science and Innovation
FX Manuscript received February 28, 2012; revised October 01, 2012;
accepted February 20, 2013. Date of publication April 18, 2013; date of
current version May 13, 2013. This work was supported by the Spanish
Ministry of Science and Innovation (CEOS-SPAIN project, reference
AYA2011-29334-C02-02).; The authors thank Prof. Melba Crawford from
Purdue University for graciously providing the EO-1 Hyperion data sets,
along with the references signatures and ground-truth used in
experiments. Funding from the Spanish Ministry of Science and Innovation
is also gratefully acknowledged. The authors also thank the editors and
the two anonymous reviewers for their outstanding comments and
suggestions, which greatly helped to improve the technical quality and
presentation of the manuscript.
NR 28
TC 7
Z9 8
U1 0
U2 7
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD APR
PY 2013
VL 6
IS 2
SI SI
BP 408
EP 418
DI 10.1109/JSTARS.2013.2250256
PN 1
PG 11
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA 148VV
UT WOS:000319277100016
ER
PT J
AU Thenkabail, PS
Mariotto, I
Gumma, MK
Middleton, EM
Landis, DR
Huemmrich, KF
AF Thenkabail, Prasad S.
Mariotto, Isabella
Gumma, Murali Krishna
Middleton, Elizabeth M.
Landis, David R.
Huemmrich, K. Fred
TI Selection of Hyperspectral Narrowbands (HNBs) and Composition of
Hyperspectral Twoband Vegetation Indices (HVIs) for Biophysical
Characterization and Discrimination of Crop Types Using Field
Reflectance and Hyperion/EO-1 Data
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Hyperion; field reflectance; imaging spectroscopy; HyspIRI; biophysical
parameters; hyperspectral vegetation indices; hyperspectral narrowbands;
broadbands
ID WATER PRODUCTIVITY; IRRIGATED WHEAT; ENERGY FLUXES; IMAGERY
AB The overarching goal of this study was to establish optimal hyperspectral vegetation indices (HVIs) and hyperspectral narrowbands (HNBs) that best characterize, classify, model, and map the world's main agricultural crops. The primary objectives were: (1) crop biophysical modeling through HNBs and HVIs, (2) accuracy assessment of crop type discrimination using Wilks' Lambda through a discriminant model, and (3) meta-analysis to select optimal HNBs and HVIs for applications related to agriculture. The study was conducted using two Earth Observing One (EO-1) Hyperion scenes and other surface hyperspectral data for the eight leading worldwide crops (wheat, corn, rice, barley, soybeans, pulses, cotton, and alfalfa) that occupy similar to 70% of all cropland areas globally. This study integrated data collected from multiple study areas in various agroecosystems of Africa, the Middle East, Central Asia, and India. Data were collected for the eight crop types in six distinct growth stages. These included (a) field spectroradiometer measurements (350-2500 nm) sampled at 1-nm discrete bandwidths, and (b) field biophysical variables (e.g., biomass, leaf area index) acquired to correspond with spectroradiometer measurements. The eight crops were described and classified using similar to 20 HNBs. The accuracy of classifying these 8 crops using HNBs was around 95%, which was similar to 25% better than the multi-spectral results possible from Landsat-7's Enhanced Thematic Mapper+ or EO-1's Advanced Land Imager. Further, based on this research and meta-analysis involving over 100 papers, the study established 33 optimal HNBs and an equal number of specific two-band normalized difference HVIs to best model and study specific biophysical and biochemical quantities of major agricultural crops of the world. Redundant bands identified in this study will help overcome the Hughes Phenomenon (or "the curse of high dimensionality") in hyperspectral data for a particular application (e.g., biophysical characterization of crops). The findings of this study will make a significant contribution to future hyperspectral missions such as NASA's HyspIRI.
C1 [Thenkabail, Prasad S.] US Geol Survey, Western Geog Sci Ctr, Flagstaff, AZ 86001 USA.
[Mariotto, Isabella] Univ Texas El Paso, Dept Geol Sci, Environm Sci Program, El Paso, TX 79968 USA.
[Gumma, Murali Krishna] Int Crops Res Inst Semi Arid Trop, South Asia Breeding Hub, IRRI, Patancheru 502324, Andhra Pradesh, India.
[Middleton, Elizabeth M.] NASA, Goddard Space Flight Ctr, Biospher Sci Lab, Greenbelt, MD 20771 USA.
[Landis, David R.] Sigma Space Corp Inc, Lanham, MD 20706 USA.
[Huemmrich, K. Fred] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA.
RP Thenkabail, PS (reprint author), US Geol Survey, Western Geog Sci Ctr, Flagstaff, AZ 86001 USA.
EM pthenkabail@usgs.gov
FU U.S. Geological Survey; NASA Science Mission Directorate's Earth Science
Division [NNH10ZDA001N-HYSPIRI]; USGS John Wesley Powell Center for
Analysis and Synthesis
FX The authors want to thank Dr. Zhuoting Wu for help with Figs. 3 and 8.
The four anonymous reviewers and two internal USGS reviewers (Dr. Dennis
Dye and Dr. Kristin Byrd) were very insightful in their comments and
helped improve the quality of this manuscript. We are grateful to Dr.
Elizabeth Middleton, NASA, Guest Editor of this special issue, for the
encouragement to put this paper together. Dr. David Landis, Sigma Space
Corp. for editing the penultimate version along with Dr. Middleton. The
financial support through Land Remote Sensing (LRS) and Geographic
Analysis and Monitoring (GAM) Programs of the U.S. Geological Survey are
gratefully acknowledged. The authors are thankful to NASA Science
Mission Directorate's Earth Science Division for the research grant in
response to NASA ROSES HyspIRI solicitation (NNH10ZDA001N-HYSPIRI). The
authors are grateful for continued support and encouragement from Susan
Benjamin, Director of the USGS Western Geographic Science Center and
Edwin Pfeifer, USGS Southwest Geographic Team Chief. Finally, the
authors would like to thank USGS John Wesley Powell Center for Analysis
and Synthesis for funding the Working group on Global Croplands (WGGC).
Our special thanks to Powell Center Directors: Jill Baron and Marty
Goldhaber. Inputs from WGGC team members
(http://powellcenter.usgs.gov/currentprojects.php#GlobalCroplandMembers)
are acknowledged. The WGGC web site
(https://powellcenter.usgs.gov/globalcroplandwater/) support provided by
Megan Eberhardt Frank, Gail A. Montgomery, Tim Kern and others is deeply
appreciated.
NR 43
TC 46
Z9 47
U1 3
U2 52
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1939-1404
J9 IEEE J-STARS
JI IEEE J. Sel. Top. Appl. Earth Observ. Remote Sens.
PD APR
PY 2013
VL 6
IS 2
SI SI
BP 427
EP 439
DI 10.1109/JSTARS.2013.2252601
PN 1
PG 13
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA 148VV
UT WOS:000319277100018
ER
PT J
AU Masi, E
Bellan, J
Harstad, KG
Okong'o, NA
AF Masi, Enrica
Bellan, Josette
Harstad, Kenneth G.
Okong'o, Nora A.
TI Multi-species turbulent mixing under supercritical-pressure conditions:
modelling, direct numerical simulation and analysis revealing species
spinodal decomposition
SO JOURNAL OF FLUID MECHANICS
LA English
DT Article
DE mixing; turbulent mixing
ID MASS DIFFUSION-COEFFICIENTS; SHEAR-LAYER; BINARY; TRANSITION; METHANE;
NUMBER; FLAMES; AIR
AB A model is developed for describing mixing of several species under high-pressure conditions. The model includes the Peng-Robinson equation of state, a full mass-diffusion matrix, a full thermal-diffusion-factor matrix necessary to incorporate the Soret and Dufour effects and both thermal conductivity and viscosity computed for the species mixture using mixing rules. Direct numerical simulations (DNSs) are conducted in a temporal mixing layer configuration. The initial mean flow is perturbed using an analytical perturbation which is consistent with the definition of vorticity and is divergence free. Simulations are performed for a set of five species relevant to hydrocarbon combustion and an ensemble of realizations is created to explore the effect of the initial Reynolds number and of the initial pressure. Each simulation reaches a transitional state having turbulent characteristics and most of the data analysis is performed on that state. A mathematical reformulation of the flux terms in the conservation equations allows the definition of effective species-specific Schmidt numbers (Sc) and of an effective Prandtl number (Pr) based on effective species-specific diffusivities and an effective thermal conductivity, respectively. Because these effective species-specific diffusivities and the effective thermal conductivity are not directly computable from the DNS solution, we develop models for both of these quantities that prove very accurate when compared with the DNS database. For two of the five species, values of the effective species-specific diffusivities are negative at some locations indicating that these species experience spinodal decomposition; we determine the necessary and sufficient condition for spinodal decomposition to occur. We also show that flows displaying spinodal decomposition have enhanced vortical characteristics and trace this aspect to the specific features of high-density-gradient magnitude regions formed in the flows. The largest values of the effective species-specific S c numbers can be well in excess of those known for gases but almost two orders of magnitude smaller than those of liquids at atmospheric pressure. The effective thermal conductivity also exhibits negative values at some locations and the effective Pr displays values that can be as high as those of a liquid refrigerant. Examination of the equivalence ratio indicates that the stoichiometric region is thin and coincides with regions where the mixture effective species-specific Lewis number values are well in excess of unity. Very lean and very rich regions coexist in the vicinity of the stoichiometric region. Analysis of the dissipation indicates that it is dominated by mass diffusion, with viscous dissipation being the smallest among the three dissipation modes. The sum of the heat and species (i.e. scalar) dissipation is functionally modelled using the effective species-specific diffusivities and the effective thermal conductivity. Computations of the modelled sum employing the modelled effective species-specific diffusivities and the modelled effective thermal conductivity shows that it accurately replicates the exact equivalent dissipation.
C1 [Masi, Enrica; Bellan, Josette] CALTECH, Pasadena, CA 91125 USA.
[Bellan, Josette; Harstad, Kenneth G.; Okong'o, Nora A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Bellan, J (reprint author), CALTECH, Pasadena, CA 91125 USA.
EM josette.bellan@jpl.nasa.gov
FU Department of Energy (DOE), Basic Energy Sciences (BES); JPL Research
and Technology Development under the Spontaneous Concepts program under
the DOE-BES
FX This work was conducted at the Jet Propulsion Laboratory (JPL) of the
California Institute of Technology (Caltech) and sponsored by the
Department of Energy (DOE), Basic Energy Sciences (BES) under the
direction of Dr W. Sisk and Dr M. Pederson. Sponsorship from the JPL
Research and Technology Development under the Spontaneous Concepts
program permitted the development of some ideas which were fully
explored under the DOE-BES sponsorship. The computational resources were
provided by the JPL Supercomputing Center, by NASA Advanced
Supercomputing at Ames Research Center and by National Energy Research
Supercomputing Center of the Department of Energy.
NR 39
TC 7
Z9 7
U1 0
U2 25
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0022-1120
J9 J FLUID MECH
JI J. Fluid Mech.
PD APR
PY 2013
VL 721
BP 578
EP 626
DI 10.1017/jfm.2013.70
PG 49
WC Mechanics; Physics, Fluids & Plasmas
SC Mechanics; Physics
GA 147IT
UT WOS:000319160800008
ER
PT J
AU Lawrence, SJ
Stopar, JD
Hawke, BR
Greenhagen, BT
Cahill, JTS
Bandfield, JL
Jolliff, BL
Denevi, BW
Robinson, MS
Glotch, TD
Bussey, DBJ
Spudis, PD
Giguere, TA
Garry, WB
AF Lawrence, Samuel J.
Stopar, Julie D.
Hawke, B. Ray
Greenhagen, Benjamin T.
Cahill, Joshua T. S.
Bandfield, Joshua L.
Jolliff, Bradley L.
Denevi, Brett W.
Robinson, Mark S.
Glotch, Timothy D.
Bussey, D. Benjamin J.
Spudis, Paul D.
Giguere, Thomas A.
Garry, W. Brent
TI LRO observations of morphology and surface roughness of volcanic cones
and lobate lava flows in the Marius Hills
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Moon; LROC; Diviner; Mini-RF; volcanism; domes; cones; block abundance;
surface roughness; lava flows
ID DIVINER LUNAR RADIOMETER; THERMAL INFRARED-SPECTRA; PLANETARY SURFACES;
CINDER CONES; MOON; EMPLACEMENT; HAWAII; MARS; INSTRUMENT; TRANSITION
AB The volcanic domes, cones, sinuous rilles, and pyroclastic deposits of the Marius Hills region of the Moon (similar to 13.4 degrees N, 304.6 degrees E) represent a significant episode of magmatic activity at or near the lunar surface that is still poorly understood. Comparisons between LROC NAC block populations, Mini-RF data, and Diviner-derived rock abundances confirm that blocky lava flows comprise the domes of the Marius Hills. 8 mu m features measured by Diviner indicate that the domes are not rich in silica and are not significantly different than surrounding mare materials. LROC observations indicate that some of the dome-building lava flows originated directly from volcanic cones. Many of the cones are C-shaped, while others are irregularly shaped, and local topography and lava eruptions affect cone shape. In general, the cones are morphologically similar to terrestrial cinder and lava cones and are composed of varying amounts of cinder, spatter, and lava. Many of the cones are found in local groupings or alignments. The wide range of volcanic features, from broad low domes to steep cones, represents a range of variable eruption conditions. Complex morphologies and variable layering show that eruption conditions were variable over the plateau.
C1 [Lawrence, Samuel J.; Stopar, Julie D.; Robinson, Mark S.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Hawke, B. Ray; Giguere, Thomas A.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Sch Ocean & Earth Sci & Technol, Honolulu, HI 96822 USA.
[Greenhagen, Benjamin T.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Cahill, Joshua T. S.; Denevi, Brett W.; Bussey, D. Benjamin J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA.
[Bandfield, Joshua L.] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA.
[Jolliff, Bradley L.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
[Glotch, Timothy D.] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA.
[Spudis, Paul D.] Univ Space Res Assoc, Lunar & Planetary Inst, Houston, TX USA.
[Giguere, Thomas A.] Intergraph Corp, Kapolei, HI USA.
[Garry, W. Brent] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
RP Lawrence, SJ (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
EM Samuel.lawrence@asu.edu
RI Garry, Brent/I-5920-2013; Denevi, Brett/I-6502-2012; Cahill,
Joshua/I-3656-2012; Greenhagen, Benjamin/C-3760-2016;
OI Denevi, Brett/0000-0001-7837-6663; Cahill, Joshua/0000-0001-6874-5533;
Stopar, Julie/0000-0003-1578-3688
FU NASA Lunar Reconnaissance Orbiter project
FX The hard work and dedication of the LROC Science Operations Center team
are gratefully acknowledged. This work was funded by the NASA Lunar
Reconnaissance Orbiter project. This work has made use of the NASA/SAO
Astrophysical Data System. This is Lunar and Planetary Institute
contribution 1721 and Hawaii Institute of Geophysics and Planetology
publication 2004.
NR 73
TC 12
Z9 13
U1 1
U2 8
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 APR
PY 2013
VL 118
IS 4
BP 615
EP 634
DI 10.1002/jgre.20060
PG 20
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 147GR
UT WOS:000319155000002
ER
PT J
AU Bishop, JL
Perry, KA
Dyar, MD
Bristow, TF
Blake, DF
Brown, AJ
Peel, SE
AF Bishop, Janice L.
Perry, Kaysea A.
Dyar, M. Darby
Bristow, Thomas F.
Blake, David F.
Brown, Adrian J.
Peel, Samantha E.
TI Coordinated spectral and XRD analyses of magnesite-nontronite-forsterite
mixtures and implications for carbonates on Mars
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Martian mineralogy; carbonates; reflectance spectroscopy; Mossbauer
spectroscopy; XRD
ID THERMAL EMISSION-SPECTRA; COMMON GEOLOGIC MINERALS; PHOENIX LANDING
SITE; REFLECTANCE SPECTROSCOPY; MOSSBAUER-SPECTROSCOPY; SPECTROMETER
EXPERIMENT; GEOCHEMICAL ANALYSES; SPIRIT ROVER; MARTIAN SOIL;
IDENTIFICATION
AB Mineral detection on Mars largely relies on laboratory data of minerals and mineral mixtures. The objective of this study is to provide reflectance spectra in the visible/near-infrared (VNIR) and mid-IR regions, X-ray diffraction (XRD) data and Mossbauer spectra of a suite of carbonate, phyllosilicate and olivine mixtures in order to facilitate identification and characterization of these minerals on Mars. Remote sensing observations indicate that combinations of these minerals are present in ancient rocks on Mars around the Isidis Basin and in Gusev crater. Magnesite, nontronite, and forsterite size fractions <125 mu m were selected for this study. Results of the VNIR reflectance analyses illustrate the complexity of VNIR spectra of mixtures. Analyses of the NIR band depths near 2.3, 2.5, 3.4, and 4 mu m showed clear trends with carbonate abundance, although the data are not linear. Mixtures of magnesite and nontronite exhibited a band near 2.3 mu m much closer to that observed for nontronite than that for magnesite. VNIR analyses of the mixtures indicated that a small amount of forsterite in any of the mixtures contributed a large increase in the broad similar to 1 mu m band and, hence, the red slope characteristic of Fe2+-bearing minerals. Mid-IR mixture spectra were dominated by magnesite and forsterite, and nontronite was much more difficult to detect by mid-IR spectra in the mixtures. This could be related to why phyllosilicates are detected in many locations on Mars using data collected by the Compact Reconnaissance Imaging Spectrometer for Mars, but not detected using data collected by the Thermal Emission Spectrometer. Mossbauer spectroscopy is well suited for analyses of Fe2+- and Fe3+-bearing minerals, and modeling of the peak areas gave well-correlated trends for nontronite and forsterite abundances where abundant Fe was present. XRD full-pattern fitting analyses were performed on the magnesite-forsterite series, giving results within 6 wt % of the actual values, with a mean difference between actual and calculated values of 2.4 wt %. This study provides important laboratory data for characterizing the spectral and XRD properties of mineral mixtures that will facilitate mineral identification on Mars. Carbonates, in particular, have been primarily observed at low abundances and in small outcrops, and they are frequently found mixed with other minerals. Through analyses of mineral mixtures using multiple data sets, this study seeks to provide ground truthing that will enable better coordination of carbonate detections in the dust and rocks of Mars.
C1 [Bishop, Janice L.; Perry, Kaysea A.; Brown, Adrian J.] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
[Bishop, Janice L.; Bristow, Thomas F.; Blake, David F.; Brown, Adrian J.] NASA Ames Res Ctr, Exobiol Branch, Moffett Field, CA USA.
[Dyar, M. Darby; Peel, Samantha E.] Mt Holyoke Coll, Dept Astron, S Hadley, MA USA.
RP Bishop, JL (reprint author), SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA.
EM jbishop@seti.org
OI Peel, Samantha/0000-0002-2285-6446
FU NASA's MFR; PGG; NASA Postdoctoral Program; National Science Foundation;
NASA Astrobiology Institute
FX The authors thank NASA's MFR and PGG programs and MRO and MSL missions
for partial support of this work. Support from the NASA Postdoctoral
Program to T. Bristow and from the National Science Foundation and the
NASA Astrobiology Institute to K. Perry through the Research Experience
for Undergraduates program at the SETI Institute are greatly
appreciated. Thanks are also due to NASA's PGG program and the NASA
Lunar Science Institute for supporting Brown University's RELAB
facility. Helpful comments from an anonymous reviewer and B. Sutter
improved the manuscript.
NR 94
TC 8
Z9 8
U1 3
U2 33
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 APR
PY 2013
VL 118
IS 4
BP 635
EP 650
DI 10.1002/jgre.20066
PG 16
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 147GR
UT WOS:000319155000003
ER
PT J
AU Song, E
Bandfield, JL
Lucey, PG
Greenhagen, BT
Paige, DA
AF Song, Eugenie
Bandfield, Joshua L.
Lucey, Paul G.
Greenhagen, Benjamin T.
Paige, David A.
TI Bulk mineralogy of lunar crater central peaks via thermal infrared
spectra from the Diviner Lunar Radiometer: A study of the Moon's crustal
composition at depth
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE Lunar crust; Thermal Infrared spectroscopy; Lunar bulk composition
ID PLANETARY SURFACES; EMISSION-SPECTRA; COPERNICUS; CLEMENTINE; OLIVINE;
SOILS; MODEL; SPECTROSCOPY; TOPOGRAPHY; SCATTERING
AB The central peaks of lunar impact craters are thought to be composed of uplifted material originating from varying depths of the crustal column. The interpreted crystallization sequence of the early lunar magma ocean resulted in an anorthositic upper crust that may become progressively more mafic as it approaches the olivine-rich mantle. Emissivity spectra from the Lunar Reconnaissance Orbiter (LRO) Diviner Radiometer are used to derive the wavelength location of the Christiansen Feature (CF), which is sensitive to bulk silicate mineralogy. Here a survey of CF values has been performed for the central peaks of 135 complex craters, providing global and regional observations of the heterogeneity of crustal compositions. Crustal thickness models give context to the preimpact depth of the central peak material and its proximity to the crust-mantle boundary. This study has identified six craters with potentially ultramafic compositions within their central peaks. More common occurrences of mafic material, found in a wide variety of crater central peaks, show a silicate composition roughly similar to mare basalt or an olivine-bearing gabbro. The range of central peak CF values is similar to that of the rest of the lunar surface. Bulk mineralogy of the central peak material does not appear to be correlated with its crustal depth of origin, suggesting both lateral and vertical heterogeneity in crustal composition rather than a gradual transition from felsic to mafic composition. It is likely that the Moon's extensive cratering history has continually overturned the original crust, erasing any original systematic dependence of composition on depth or proximity to the mantle.
C1 [Song, Eugenie; Bandfield, Joshua L.] Univ Washington, Seattle, WA 98195 USA.
[Lucey, Paul G.] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Greenhagen, Benjamin T.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Paige, David A.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA.
RP Song, E (reprint author), Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, 1680 East West Rd,POST 602, Honolulu, HI 96822 USA.
EM eugesong@higp.hawaii.edu
RI Greenhagen, Benjamin/C-3760-2016
FU operations teams at UCLA; Jet Propulsion Laboratory
FX We would like to thank the Diviner science and operations teams at UCLA
and Jet Propulsion Laboratory for their support. Thanks also to
Jean-Pierre Williams at UCLA for developing data processing scripts that
were vital for this project, Mark Sullivan at UCLA for technical
support. Many thanks to Alan Gillespie and Bruce Nelson at University of
Washington for feedback and advice. Finally, thanks to Joshua T. Cahill
and an anonymous reviewer for their time and constructive advice that
led to the publication of this manuscript.
NR 76
TC 12
Z9 12
U1 0
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD APR
PY 2013
VL 118
IS 4
BP 689
EP 707
DI 10.1002/jgre.20065
PG 19
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 147GR
UT WOS:000319155000006
ER
PT J
AU Datta, A
Yeo, H
Norman, TR
AF Datta, Anubhav
Yeo, Hyeonsoo
Norman, Thomas R.
TI Experimental Investigation and Fundamental Understanding of a Full-Scale
Slowed Rotor at High Advance Ratios
SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY
LA English
DT Article
ID COMPOUND HELICOPTER; TECHNOLOGY
AB This paper describes and analyzes the measurements from a full-scale, slowed revolutions per minute (rpm), UH-60A rotor tested at the National Full-Scale Aerodynamics Complex 40- by 80-ft wind tunnel up to an advance ratio of 1.0. A comprehensive set of measurements that includes performance, blade loads, hub loads, and pressures/airloads makes this data set unique. The measurements reveal new and rich aeromechanical phenomena that are unique to this exotic regime. These include reverse chord dynamic stall, retreating side impulse in torsion load, large inboard outboard elastic twist differential, diminishing rotor forces and yet a dramatic buildup of blade loads, and high blade loads and yet benign levels of vibratory hub loads. The objective of this research is the fundamental understanding of these unique aeromechanical phenomena. The intent is to provide useful knowledge for the design of high-speed, high-efficiency, slowed rpm rotors of the future and a database for validation of advanced analyses.
C1 [Datta, Anubhav] NASA, Ames Res Ctr, Sci & Technol Corp, USA,Aeroflightdynam Directorate, Moffett Field, CA 94035 USA.
[Yeo, Hyeonsoo] NASA, Ames Res Ctr, Aeroflightdynam Directorate AMRDEC, USA,Res Dev & Engn Command, Moffett Field, CA 94035 USA.
[Norman, Thomas R.] NASA, Ames Res Ctr, Aeromech Branch, Moffett Field, CA 94035 USA.
RP Datta, A (reprint author), NASA, Ames Res Ctr, Sci & Technol Corp, USA,Aeroflightdynam Directorate, Moffett Field, CA 94035 USA.
EM hubloads@gmail.com
NR 39
TC 10
Z9 10
U1 0
U2 7
PU AMER HELICOPTER SOC INC
PI ALEXANDRIA
PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA
SN 0002-8711
J9 J AM HELICOPTER SOC
JI J. Am. Helicopter Soc.
PD APR
PY 2013
VL 58
IS 2
AR 022004
DI 10.4050/JAHS.58.022004
PG 17
WC Engineering, Aerospace
SC Engineering
GA 147NF
UT WOS:000319173600004
ER
PT J
AU Yeo, H
Romander, EA
AF Yeo, Hyeonsoo
Romander, Ethan A.
TI Loads Correlation of a Full-Scale UH-60A Air loads Rotor in a Wind
Tunnel
SO JOURNAL OF THE AMERICAN HELICOPTER SOCIETY
LA English
DT Article
ID COMPREHENSIVE ANALYSIS; HELICOPTER ROTORS; AIRLOADS; PERFORMANCE;
PREDICTION; SYSTEM
AB Wind tunnel measurements of the rotor trim, blade airloads, and structural loads of a full-scale UH-60A Black Hawk main rotor are compared with calculations obtained using the comprehensive rotorcraft analysis CAMRAD II and a coupled CAMRAD II/OVERFLOW 2 analysis. A speed sweep at constant lift up to an advance ratio of 0.4 and a thrust sweep at constant speed into deep stall are investigated. The coupled analysis shows significant improvement over comprehensive analysis. Normal force phase is better captured for all the test conditions examined. Pitching moment is better predicted, including the magnitude and phase of the two stall events in the fourth quadrant at the deeply stalled condition. Structural loads are, in general, improved with the coupled analysis, but the magnitude of chord bending moment is still significantly underpredicted. As there are three modes around 4 and 5/rev frequencies, the structural responses to the 5/rev airloads due to dynamic stall are magnified and thus accurate analysis of the deeply stalled condition is challenging.
C1 [Yeo, Hyeonsoo] NASA, Ames Res Ctr, Aeroflightdynam Directorate AMRDEC, USA,Res Dev & Engn Command, Moffett Field, CA 94035 USA.
[Romander, Ethan A.] NASA, Ames Res Ctr, Flight Vehicle Res & Technol Div, Moffett Field, CA 94035 USA.
RP Yeo, H (reprint author), NASA, Ames Res Ctr, Aeroflightdynam Directorate AMRDEC, USA,Res Dev & Engn Command, Moffett Field, CA 94035 USA.
EM hyeonsoo.yeo.civ@mail.mil
NR 20
TC 1
Z9 1
U1 0
U2 3
PU AMER HELICOPTER SOC INC
PI ALEXANDRIA
PA 217 N WASHINGTON ST, ALEXANDRIA, VA 22314 USA
SN 0002-8711
J9 J AM HELICOPTER SOC
JI J. Am. Helicopter Soc.
PD APR
PY 2013
VL 58
IS 2
DI 10.4050/JAHS.58.022003
PG 18
WC Engineering, Aerospace
SC Engineering
GA 147NF
UT WOS:000319173600003
ER
PT J
AU Dauser, T
Garcia, J
Wilms, J
Bock, M
Brenneman, LW
Falanga, M
Fukumura, K
Reynolds, CS
AF Dauser, T.
Garcia, J.
Wilms, J.
Boeck, M.
Brenneman, L. W.
Falanga, M.
Fukumura, K.
Reynolds, C. S.
TI Irradiation of an accretion disc by a jet: general properties and
implications for spin measurements of black holes
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; black hole physics; lines: profiles;
galaxies: active; galaxies: nuclei
ID X-RAY REFLECTION; ADVECTION-DOMINATED ACCRETION; K-ALPHA LINE;
XMM-NEWTON; IRON LINE; CYGNUS X-1; GX 339-4; ACTIVE GALAXY; 1H 0707-495;
HARD STATE
AB X-ray irradiation of the accretion disc leads to strong reflection features, which are then broadened and distorted by relativistic effects. We present a detailed, general relativistic approach to model this irradiation for different geometries of the primary X-ray source. These geometries include the standard point source on the rotational axis as well as more jet-like sources, which are radially elongated and accelerating. Incorporating this code in the RELLINE model for relativistic line emission, the line shape for any configuration can be predicted. We study how different irradiation geometries affect the determination of the spin of the black hole. Broad emission lines are produced only for compact irradiating sources situated close to the black hole. This is the only case where the black hole spin can be unambiguously determined. In all other cases the line shape is narrower, which could either be explained by a low spin or an elongated source. We conclude that in those cases and independent of the quality of the data no unique solution for the spin exists and therefore only a lower limit of the spin value can be given.
C1 [Dauser, T.; Wilms, J.; Boeck, M.] Dr Karl Remeis Observ, D-96049 Bamberg, Germany.
[Dauser, T.; Wilms, J.; Boeck, M.] Erlangen Ctr Astroparticle Phys, D-96049 Bamberg, Germany.
[Garcia, J.; Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Garcia, J.; Reynolds, C. S.] Univ Maryland, Maryland Astron Ctr Theory & Computat, College Pk, MD 20742 USA.
[Boeck, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Brenneman, L. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Falanga, M.] Int Space Sci Inst, CH-3012 Bern, Switzerland.
[Fukumura, K.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
RP Dauser, T (reprint author), Dr Karl Remeis Observ, Sternwartstr 7, D-96049 Bamberg, Germany.
EM thomas.dauser@sternwarte.uni-erlangen.de
RI Wilms, Joern/C-8116-2013
OI Wilms, Joern/0000-0003-2065-5410
FU European Commission [ITN 215212]; Elitenetzwerk Bayern; Deutsches
Zentrum fur Luft- und Raumfahrt [50 OR 1113]
FX We acknowledge support from the European Commission under contract ITN
215212 'Black Hole Universe' by a fellowship from the Elitenetzwerk
Bayern, and by the Deutsches Zentrum fur Luft- und Raumfahrt under
contract number 50 OR 1113. We thank John E. Davis for the development
of the SLXFIG module used to prepare the figures in this paper, Katja
Pottschmidt and John Tomsick for useful discussions, and the referee,
Andy Fabian, for his constructive comments which helped in improving
this paper.
NR 105
TC 68
Z9 68
U1 0
U2 2
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR
PY 2013
VL 430
IS 3
BP 1694
EP 1708
DI 10.1093/mnras/sts710
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 148QG
UT WOS:000319260500014
ER
PT J
AU Szabados, L
Derekas, A
Kiss, LL
Kovacs, J
Anderson, RI
Kiss, C
Szalai, T
Szekely, P
Christiansen, JL
AF Szabados, L.
Derekas, A.
Kiss, L. L.
Kovacs, J.
Anderson, R. I.
Kiss, Cs.
Szalai, T.
Szekely, P.
Christiansen, J. L.
TI Discovery of the spectroscopic binary nature of six southern Cepheids
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE binaries: spectroscopic; stars: variables: Cepheids
ID RADIAL-VELOCITIES; VARIABLE-STARS; INTERMEDIATE-BAND; PERIOD CEPHEIDS;
HEMISPHERE; SPECTROGRAPH; PHOTOMETRY
AB We present the analysis of photometric and spectroscopic data of six bright Galactic Cepheids: GH Carinae, V419 Centauri, V898 Centauri, AD Puppis, AY Sagittarii and ST Velorum. Based on new radial velocity data (in some cases supplemented with earlier data available in the literature), these Cepheids have been found to be members in spectroscopic binary systems. V898 Cen turned out to have one of the largest orbital radial velocity amplitude (>40 km s(-1)) among the known binary Cepheids. The data are insufficient to determine the orbital periods nor other orbital elements for these new spectroscopic binaries.
These discoveries corroborate the statement on the high frequency of occurrence of binaries among the classical Cepheids, a fact to be taken into account when calibrating the period-luminosity relationship for Cepheids.
We have also compiled all available photometric data that revealed that the pulsation period of AD Pup, the longest period Cepheid in this sample, is continuously increasing with Delta P = 0.004567d century(-1), likely to be caused by stellar evolution. The wave-like pattern superimposed on the parabolic O - C graph of AD Pup may well be caused by the light-time effect in the binary system. ST Vel also pulsates with a continuously increasing period. The other four Cepheids are characterized with stable pulsation periods in the last half century.
C1 [Szabados, L.; Derekas, A.; Kiss, L. L.; Kiss, Cs.] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, H-1121 Budapest, Hungary.
[Derekas, A.; Kiss, L. L.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Kiss, L. L.; Kovacs, J.] ELTE Gothard Lendulet Res Grp, H-9700 Szombathely, Hungary.
[Anderson, R. I.] Univ Geneva, Observ Geneve, CH-1290 Versoix, Switzerland.
[Szalai, T.] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary.
[Szekely, P.] Univ Szeged, Dept Expt Phys, H-6720 Szeged, Hungary.
[Christiansen, J. L.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
RP Szabados, L (reprint author), Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, Konkoly Thege Miklos Ul 15-17, H-1121 Budapest, Hungary.
EM szabados@konkoly.hu
RI Derekas, Aliz/G-2091-2016;
OI Derekas, Aliz/0000-0002-6526-9444; Anderson, Richard
I./0000-0001-8089-4419
FU ESA PECS Project [C98090]; ESTEC [4000106398/12/NL/KML]; Hungarian OTKA
[K76816, K83790, K104607, MB08C 81013]; European Community [269194];
Hungarian Academy of Sciences; Hungarian Eotvos fellowship; Janos Bolyai
Research Scholarship of the Hungarian Academy of Sciences; European
Research Council under the European Community/ERC [227224]
FX This project has been supported by the ESA PECS Project C98090, ESTEC
Contract No. 4000106398/12/NL/KML, the Hungarian OTKA Grants K76816,
K83790, K104607 and MB08C 81013, as well as the European Community's
Seventh Framework Programme (FP7/2007-2013) under grant agreement no.
269194 and the 'Lendulet-2009' Young Researchers Programme of the
Hungarian Academy of Sciences. AD was supported by the Hungarian Eotvos
fellowship. AD has been supported by the Janos Bolyai Research
Scholarship of the Hungarian Academy of Sciences. AD is very thankful to
the staff at The Lodge in Siding Spring Observatory for their
hospitality and the very nice food, making the time spent there lovely
and special. Part of the research leading to these results has received
funding from the European Research Council under the European
Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant
agreement no. 227224 (PROSPERITY). The INTEGRAL photometric data,
pre-processed by ISDC, have been retrieved from the OMC Archive at CAB
(INTA-CSIC). Critical remarks by Dr. Maria Kun and the referee's
suggestions led to a considerable improvement in the presentation of the
results.
NR 46
TC 3
Z9 3
U1 0
U2 2
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR
PY 2013
VL 430
IS 3
BP 2018
EP 2028
DI 10.1093/mnras/stt027
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 148QG
UT WOS:000319260500040
ER
PT J
AU Corsaro, E
Frohlich, HE
Bonanno, A
Huber, D
Bedding, TR
Benomar, O
De Ridder, J
Stello, D
AF Corsaro, E.
Froehlich, H. -E.
Bonanno, A.
Huber, D.
Bedding, T. R.
Benomar, O.
De Ridder, J.
Stello, D.
TI A Bayesian approach to scaling relations for amplitudes of solar-like
oscillations in Kepler stars
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: data analysis; methods: statistical; stars: evolution; stars:
late-type; stars: oscillations
ID RED GIANT BRANCH; STELLAR OSCILLATIONS; MAIN-SEQUENCE; OPEN CLUSTERS;
INITIAL CHARACTERISTICS; INPUT CATALOG; CADENCE DATA; HR DIAGRAM; NGC
6819; ASTEROSEISMOLOGY
AB We investigate different amplitude scaling relations adopted for the asteroseismology of stars that show solar-like oscillations. Amplitudes are among the most challenging asteroseismic quantities to handle because of the large uncertainties that arise in measuring the background level in the star's power spectrum. We present results computed by means of a Bayesian inference on a sample of 1640 stars observed with Kepler, spanning from main sequence to red giant stars, for 12 models used for amplitude predictions and exploiting recently well-calibrated effective temperatures from Sloan Digital Sky Survey photometry. We test the candidate amplitude scaling relations by means of a Bayesian model comparison. We find the model having a separate dependence upon the mass of the stars to be largely the most favoured one. The differences among models and the differences seen in their free parameters from early to late phases of stellar evolution are also highlighted.
C1 [Corsaro, E.] Univ Catania, Dept Phys & Astron, Astrophys Sect, I-95123 Catania, Italy.
[Corsaro, E.; Bonanno, A.] INAF Astrophys Observ Catania, I-95123 Catania, Italy.
[Corsaro, E.; De Ridder, J.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Froehlich, H. -E.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany.
[Huber, D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Bedding, T. R.; Benomar, O.; Stello, D.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
[Bedding, T. R.; Benomar, O.; Stello, D.] Aarhus Univ, Stellar Astrophys Ctr, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
RP Corsaro, E (reprint author), Univ Catania, Dept Phys & Astron, Astrophys Sect, Via S Sofia 78, I-95123 Catania, Italy.
EM eco@oact.inaf.it
OI Bedding, Timothy/0000-0001-5943-1460; Bonanno,
Alfio/0000-0003-3175-9776; Bedding, Tim/0000-0001-5222-4661
FU PRIN-INAF; FWO-Flanders [O6260 - G.0728.11]; Danish National Research
Foundation; ASTERISK project (ASTERoseismic Investigations with SONG and
Kepler); European Research Council [267864]
FX EC acknowledges financial support from the PRIN-INAF 2010
Asteroseismology: looking inside the stars with space-and ground-based
observations. EC and JDR acknowledge the support of the FWO-Flanders
under project O6260 - G.0728.11. Funding for the Stellar Astrophysics
Centre is provided by the Danish National Research Foundation. The
research is supported by the ASTERISK project (ASTERoseismic
Investigations with SONG and Kepler) funded by the European Research
Council (Grant agreement no.: 267864).
NR 67
TC 20
Z9 20
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR
PY 2013
VL 430
IS 3
BP 2313
EP 2326
DI 10.1093/mnras/stt059
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 148QG
UT WOS:000319260500061
ER
PT J
AU Gudipati, MS
Jacovi, R
Couturier-Tamburelli, I
Lignell, A
Allen, M
AF Gudipati, Murthy S.
Jacovi, Ronen
Couturier-Tamburelli, Isabelle
Lignell, Antti
Allen, Mark
TI Photochemical activity of Titan's low-altitude condensed haze
SO NATURE COMMUNICATIONS
LA English
DT Article
ID FAR-INFRARED SPECTRA; HUYGENS LANDING SITE; COUPLING PHOTOCHEMISTRY;
ELECTRONIC-SPECTRUM; EXCITED-STATES; ATMOSPHERE; DICYANOACETYLENE;
AEROSOLS; C4N2; STRATOSPHERE
AB Titan, the largest moon of Saturn and similar to Earth in many aspects, has unique orange-yellow colour that comes from its atmospheric haze, whose formation and dynamics are far from well understood. Present models assume that Titan's tholin-like haze formation occurs high in atmosphere through gas-phase chemical reactions initiated by high-energy solar radiation. Here we address an important question: Is the lower atmosphere of Titan photochemically active or inert? We demonstrate that indeed tholin-like haze formation could occur on condensed aerosols throughout the atmospheric column of Titan. Detected in Titan's atmosphere, dicyanoacetylene (C4N2) is used in our laboratory simulations as a model system for other larger unsaturated condensing compounds. We show that C4N2 ices undergo condensed-phase photopolymerization (tholin formation) at wavelengths as long as 355 nm pertinent to solar radiation reaching a large portion of Titan's atmosphere, almost close to the surface.
C1 [Gudipati, Murthy S.; Jacovi, Ronen; Lignell, Antti; Allen, Mark] CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA 91109 USA.
[Gudipati, Murthy S.] Univ Maryland, IPST, College Pk, MD 20742 USA.
[Couturier-Tamburelli, Isabelle] Aix Marseille Univ, UMR CNRS 7345, Lab Phys Interact Ion & Mol, F-13397 Marseille 20, France.
[Allen, Mark] CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Gudipati, MS (reprint author), CALTECH, Jet Prop Lab, Div Sci, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM murthy.gudipati@jpl.nasa.gov
RI Gudipati, Murthy/F-7575-2011; Lignell, Antti/C-2146-2009
OI Lignell, Antti/0000-0001-7664-5583
FU NASA Astrobiology Institute team 'Titan as a Prebiotic Chemical System';
Jet Propulsion Laboratory; JPL; Titan organic aerosol spectroscopy and
chemistry (TOAST) laboratory at JPL; French national program
Environnements Planetaires et Origines de la Vie (EPOV)
FX The Jet Propulsion Laboratory (JPL) part of the work is partly supported
by several of the following funding sources: NASA Astrobiology Institute
team 'Titan as a Prebiotic Chemical System', the Jet Propulsion
Laboratory Director's Research and Development Fund and the JPL Research
and Technology Development funding for the infrastructure of the Ice
Spectroscopy Laboratory (ISL) and Titan organic aerosol spectroscopy and
chemistry (TOAST) laboratory at JPL. The University of Provence part of
the work was funded by the French national program Environnements
Planetaires et Origines de la Vie (EPOV). This research was carried out
at the Jet Propulsion Laboratory, California Institute of Technology,
under a contract with the National Aeronautics and Space Administration.
NR 50
TC 10
Z9 10
U1 2
U2 57
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 APR
PY 2013
VL 4
AR 1648
DI 10.1038/ncomms2649
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 143MR
UT WOS:000318872100005
PM 23552063
ER
PT J
AU Rios, J
AF Rios, Joseph
TI Algorithm 928: A General, Parallel Implementation of Dantzig-Wolfe
Decomposition
SO ACM TRANSACTIONS ON MATHEMATICAL SOFTWARE
LA English
DT Article
DE Algorithms; Linear programming; optimization; parallel implementations
ID MATRICES; PROGRAMS
AB Dantzig-Wolfe Decomposition is recognized as a powerful, algorithmic tool for solving linear programs of block-angular form. While use of the approach has been reported in a wide variety of domains, there has not been a general implementation of Dantzig-Wolfe decomposition available. This article describes an open-source implementation of the algorithm. It is general in the sense that any properly decomposed linear program can be provided to the software for solving. While the original description of the algorithm was motivated by its reduced memory usage, modern computers can also take advantage of the algorithm's inherent parallelism. This implementation is parallel and built upon the POSIX threads (pthreads) library. Some computational results are provided to motivate use of such parallel solvers, as this implementation outperforms state-of-the-art commercial solvers in terms of wall-clock runtime by an order of magnitude or more on several problem instances.
C1 [Rios, Joseph] NASA, Moffett Field, CA 94035 USA.
RP Rios, J (reprint author), NASA, Ames Res Ctr, Mail Stop 210-15, Moffett Field, CA 94035 USA.
EM joseph.l.rios@nasa.gov
NR 22
TC 0
Z9 0
U1 0
U2 2
PU ASSOC COMPUTING MACHINERY
PI NEW YORK
PA 2 PENN PLAZA, STE 701, NEW YORK, NY 10121-0701 USA
SN 0098-3500
J9 ACM T MATH SOFTWARE
JI ACM Trans. Math. Softw.
PD APR
PY 2013
VL 39
IS 3
AR 21
DI 10.1145/2450153.2450159
PG 10
WC Computer Science, Software Engineering; Mathematics, Applied
SC Computer Science; Mathematics
GA 140BI
UT WOS:000318628800006
ER
PT J
AU Som, SM
Hagadorn, JW
Thelen, WA
Gillespie, AR
Catling, DC
Buick, R
AF Som, Sanjoy M.
Hagadorn, James W.
Thelen, Weston A.
Gillespie, Alan R.
Catling, David C.
Buick, Roger
TI Quantitative discrimination between geological materials with variable
density contrast by high resolution X-ray computed tomography: An
example using amygdule size-distribution in ancient lava flows
SO COMPUTERS & GEOSCIENCES
LA English
DT Article
DE X-ray tomography; Amygdules; Bubble-size distribution; Dynamic
thresholding; Bootstrap resampling; Central limit theorem
ID BASALT FLOWS; BUBBLE; ROCKS; MICROTOMOGRAPHY; COALESCENCE; ERUPTION
AB The bubble-size distribution in 2.7 billion year old lava flows can be used as a proof of concept illustrating a new set of techniques for measuring volumes of geological materials with variable density contrasts using high-resolution X-ray computed tomography. Such studies have been limited in the past to high-contrast situations such as vesicles devoid of secondary fill. We present a new dynamic thresholding method for computationally separating amygdules from their basaltic matrix in X-ray images that is based on a technique used in seismology. The technique is sensitive to the gradient of the gray-scale value, rather than an absolute threshold value often applied to an entire set of X-ray images. Additionally, we present statistical methods for extrapolating the volumetric measurement mean and standard deviation of amygdules in the measured samples to the entire population in the flow. To do so, we create additional amygdule sample sets from the original sample set in the process of 'bootstrap' resampling, and use the Central Limit Theorem to calculate the mean and standard deviation of the amygdule population from these sample sets. This suite of methods allows the extension of bubble-size distribution studies typically done on modern flows to the ancient rock record and potentially has many other uses in geosciences where quantitative discrimination between materials with a range of densities is required. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Som, Sanjoy M.; Thelen, Weston A.; Gillespie, Alan R.; Catling, David C.; Buick, Roger] Univ Washington, Dept Earth & Space Sci, Seattle, WA 98195 USA.
[Som, Sanjoy M.] Blue Marble Space Inst Sci, Seattle, WA 98145 USA.
[Hagadorn, James W.] Denver Museum Nat & Sci, Dept Earth Sci, Denver, CO 80205 USA.
[Thelen, Weston A.] Hawaii Volcano Observ, Volcano, HI 96718 USA.
RP Som, SM (reprint author), NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA.
EM sanjoy@uw.edu
OI Catling, David/0000-0001-5646-120X; Buick, Roger/0000-0003-0139-1659
FU NASA Exobiology/Astrobiology grant [NNX08AP56G]
FX This work was funded by NASA Exobiology/Astrobiology grant NNX08AP56G.
The help of John Perreault is gratefully acknowledged in assisting with
BLOB3D amygdule extraction. Richard Ketcham and Philip Watson at the UT
HRXCT facility are thanked for their helpful feedback during our
implementation of BLOB3D. This manuscript benefited from constructive
reviews by Richard Ketcham and Guilherme Gualda.
NR 28
TC 3
Z9 3
U1 2
U2 12
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0098-3004
J9 COMPUT GEOSCI-UK
JI Comput. Geosci.
PD APR
PY 2013
VL 54
BP 231
EP 238
DI 10.1016/j.cageo.2012.11.019
PG 8
WC Computer Science, Interdisciplinary Applications; Geosciences,
Multidisciplinary
SC Computer Science; Geology
GA 136PW
UT WOS:000318376900027
ER
PT J
AU Ishikawa, ST
Gulick, VC
AF Ishikawa, Sascha T.
Gulick, Virginia C.
TI An automated mineral classifier using Raman spectra
SO COMPUTERS & GEOSCIENCES
LA English
DT Article
DE Mineral classification; Raman spectroscopy; Machine learning; Mars;
Robotic exploration; Igneous rocks
ID PRINCIPAL COMPONENT ANALYSIS; SPECTROSCOPY; IDENTIFICATION
AB We present a robust and autonomous mineral classifier for analyzing igneous rocks. Our study shows that machine learning methods, specifically artificial neural networks, can be trained using spectral data acquired by in situ Raman spectroscopy in order to accurately distinguish among key minerals for characterizing the composition of igneous rocks. These minerals include olivine, quartz, plagioclase, potassium feldspar, mica, and several pyroxenes. On average, our classifier performed with 83 percent accuracy. Quartz and olivine, as well as the pyroxenes, were classified with 100 percent accuracy. In addition to using traditional features such as the location of spectral bands and their shapes, our automated mineral, classifier was able to incorporate fluorescence patterns, which are not as easily perceived by humans, into its classification scheme. The latter was able to improve the classification accuracy and is an example of the robustness of our classifier. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Ishikawa, Sascha T.; Gulick, Virginia C.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Ishikawa, Sascha T.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
[Gulick, Virginia C.] SETI Inst, Mountain View, CA 94043 USA.
RP Ishikawa, ST (reprint author), NASA, Ames Res Ctr, Div Space Sci, Mail Stop 239-20, Moffett Field, CA 94035 USA.
EM Sascha.T.Ishikawa@nasa.gov
FU NASA
FX We thank Shawn Hart for acquiring the Raman spectra of our samples. This
research was supported by a prior grant from NASA's Advanced Cross
Enterprise Technology Development Program.
NR 26
TC 11
Z9 12
U1 4
U2 23
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0098-3004
J9 COMPUT GEOSCI-UK
JI Comput. Geosci.
PD APR
PY 2013
VL 54
BP 259
EP 268
DI 10.1016/j.cageo.2013.01.011
PG 10
WC Computer Science, Interdisciplinary Applications; Geosciences,
Multidisciplinary
SC Computer Science; Geology
GA 136PW
UT WOS:000318376900030
ER
PT J
AU Won, J
Said, MA
Seyam, AFM
AF Won, Jessica
Said, Magdi A.
Seyam, Abdel-Fattah M.
TI Development of UV Protective Sheath for High Performance Fibers for High
Altitude Applications
SO FIBERS AND POLYMERS
LA English
DT Article
DE High performance fibers; Ultraviolet and visible light; Low density
polyethylene; Zylon (R)
AB High performance fibers have distinguished properties such as high tensile strength, good thermal and chemical resistance, dimensional stability, lightweight, and high electrical conductivity. Due to these superior properties, high performance fibers made it to the scene of broad range of applications such as aerospace, automotive, windmill, fiber reinforced composites, high strength tethers, tendons for scientific balloon, tension structures, protective clothing, and marine. Examples of such fibers are Zylon (R), Kevlar (R), and Vectran (R). However, the fibers lose their strength significantly upon exposure to Ultraviolet (UV) and visible light. In this research, UV protective films from extruded low density polyethylene (LDPE) loaded with different content of UV stabilizers (TiO2 nanoparticles and White PE CC (R)) were investigated. To assess the degree of UV blockage of each extruded protective film, their transmittance to UV and visible (UV-VIS) light was measured. Additionally, Zylon (R) braids were sheathed with the protective films and the strength of the braids and yarns raveled from braids was measured before and after UV exposure for different number of days. LDPE loaded with White PE CC (R) and 10 % TiO2 showed the least transmittance to UV-VIS and their yarns and braids exhibited highest strength retention after exposure to artificial UV. Strength retention of braids was higher than that of individual yarns due to weak link effect and braid structure assistant.
C1 [Won, Jessica] Hyosung Corp, Anyang 431080, South Korea.
[Said, Magdi A.] NASA, Wallops Isl, VA USA.
[Seyam, Abdel-Fattah M.] NC State Univ, Coll Text, Raleigh, NC USA.
RP Seyam, AFM (reprint author), NC State Univ, Coll Text, Raleigh, NC USA.
EM aseyam@ncsu.edu
FU NASA Balloon Program Office [NNXlOAE26G]; State of North Carolina
FX This work is funded by NASA Balloon Program Office (Grant Number
NNXlOAE26G) and the State of North Carolina. The authors extend their
appreciation to Dr. Rahul Vallabh of NC State University College of
Textiles for his valuable discussion.
NR 11
TC 5
Z9 5
U1 2
U2 37
PU KOREAN FIBER SOC
PI SEOUL
PA KOREA SCIENCE TECHNOLOGY CTR #501 635-4 YEOGSAM-DONG, KANGNAM-GU, SEOUL
135-703, SOUTH KOREA
SN 1229-9197
J9 FIBER POLYM
JI Fiber. Polym.
PD APR
PY 2013
VL 14
IS 4
BP 647
EP 652
DI 10.1007/s12221-013-0647-9
PG 6
WC Materials Science, Textiles; Polymer Science
SC Materials Science; Polymer Science
GA 141RA
UT WOS:000318743000020
ER
PT J
AU Reinhart, RC
Kacpura, TJ
Johnson, SK
Lux, JP
AF Reinhart, Richard C.
Kacpura, Thomas J.
Johnson, Sandra K.
Lux, James P.
TI NASA's Space Communications and Navigation Test Bed aboard the
International Space Station
SO IEEE AEROSPACE AND ELECTRONIC SYSTEMS MAGAZINE
LA English
DT Article
C1 [Reinhart, Richard C.; Kacpura, Thomas J.; Johnson, Sandra K.] NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA.
[Lux, James P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Reinhart, RC (reprint author), NASA, John H Glenn Res Ctr, 21000 Brookpark Rd,Mail Stop 54-1, Cleveland, OH 44135 USA.
EM richard.c.reinhart@nasa.gov
NR 6
TC 2
Z9 3
U1 0
U2 6
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0885-8985
J9 IEEE AERO EL SYS MAG
JI IEEE Aerosp. Electron. Syst. Mag.
PD APR
PY 2013
VL 28
IS 4
BP 4
EP 15
PG 12
WC Engineering, Aerospace; Engineering, Electrical & Electronic
SC Engineering
GA 138YF
UT WOS:000318547100002
ER
PT J
AU Mayer, JM
Graves, JE
Manini, TM
Nuzzo, JL
Ploutz-Snyder, LL
AF Mayer, John M.
Graves, James E.
Manini, Todd M.
Nuzzo, James L.
Ploutz-Snyder, Lori L.
TI Lumbar Muscle Activity During Common Lifts: A Preliminary Study Using
Magnetic Resonance Imaging
SO JOURNAL OF APPLIED BIOMECHANICS
LA English
DT Article
DE biomechanics; exercise; MRI; muscle; spine
ID LOW-BACK-PAIN; EXERCISE INTENSITY; RELAXATION-TIMES; SKELETAL-MUSCLE;
WORK; ELECTROMYOGRAPHY; MANAGEMENT; IMAGES; T2
AB The purpose of this preliminary study was to assess lumbar multifidus, erector spinae, and quadratus lumborum muscle activity during lifts as measured by changes in transverse relaxation time (T2) from magnetic resonance imaging (MRI). Thirteen healthy adults performed dynamic squat, stoop, and asymmetric stoop lifts at a standard load, with each lift followed by MRI. Increase in T2 for the multifidus and erector spinae was greater for the stoop than squat. No difference in T2 increase was noted between the multifidus and erector spinae for the squat or stoop. Increase in T2 for the contralateral multifidus was less for the asymmetric stoop than stoop. Future research using MRI and other biomechanical techniques is needed to fully characterize lumbar muscle activity during lifts for various populations, settings, postures, and loads.
C1 [Mayer, John M.; Nuzzo, James L.] Univ S Florida, Coll Med, Sch Phys Therapy & Rehabil Sci, Tampa, FL 33620 USA.
[Graves, James E.] Univ Utah, Coll Hlth, Salt Lake City, UT USA.
[Manini, Todd M.] Univ Florida, Coll Med, Dept Aging & Geriatr Res, Gainesville, FL USA.
[Ploutz-Snyder, Lori L.] NASA Johnson Space Ctr, Univ Space Res Assoc, Houston, TX USA.
RP Mayer, JM (reprint author), Univ S Florida, Coll Med, Sch Phys Therapy & Rehabil Sci, Tampa, FL 33620 USA.
NR 32
TC 1
Z9 1
U1 0
U2 3
PU HUMAN KINETICS PUBL INC
PI CHAMPAIGN
PA 1607 N MARKET ST, PO BOX 5076, CHAMPAIGN, IL 61820-2200 USA
SN 1065-8483
J9 J APPL BIOMECH
JI J. Appl. Biomech.
PD APR
PY 2013
VL 29
IS 2
BP 147
EP 154
PG 8
WC Engineering, Biomedical; Sport Sciences
SC Engineering; Sport Sciences
GA 138WP
UT WOS:000318542000004
PM 22814283
ER
PT J
AU Fraisse, AA
Ade, PAR
Amiri, M
Benton, SJ
Bock, JJ
Bond, JR
Bonetti, JA
Bryan, S
Burger, B
Chiang, HC
Clark, CN
Contaldi, CR
Crill, BP
Davis, G
Dore, O
Farhang, M
Filippini, JP
Fissel, LM
Gandilo, NN
Golwala, S
Gudmundsson, JE
Hasselfield, M
Hilton, G
Holmes, W
Hristov, VV
Irwin, K
Jones, WC
Kuo, CL
MacTavish, CJ
Mason, PV
Montroy, TE
Morford, TA
Netterfield, CB
O'Dea, DT
Rahlin, AS
Reintsema, C
Ruhl, JE
Runyan, MC
Schenker, MA
Shariff, JA
Soler, JD
Trangsrud, A
Tucker, C
Tucker, RS
Turner, AD
Wiebe, D
AF Fraisse, A. A.
Ade, P. A. R.
Amiri, M.
Benton, S. J.
Bock, J. J.
Bond, J. R.
Bonetti, J. A.
Bryan, S.
Burger, B.
Chiang, H. C.
Clark, C. N.
Contaldi, C. R.
Crill, B. P.
Davis, G.
Dore, O.
Farhang, M.
Filippini, J. P.
Fissel, L. M.
Gandilo, N. N.
Golwala, S.
Gudmundsson, J. E.
Hasselfield, M.
Hilton, G.
Holmes, W.
Hristov, V. V.
Irwin, K.
Jones, W. C.
Kuo, C. L.
MacTavish, C. J.
Mason, P. V.
Montroy, T. E.
Morford, T. A.
Netterfield, C. B.
O'Dea, D. T.
Rahlin, A. S.
Reintsema, C.
Ruhl, J. E.
Runyan, M. C.
Schenker, M. A.
Shariff, J. A.
Soler, J. D.
Trangsrud, A.
Tucker, C.
Tucker, R. S.
Turner, A. D.
Wiebe, D.
CA SPIDER Collaboration
TI SPIDER: probing the early Universe with a suborbital polarimeter
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE CMBR experiments; CMBR polarisation; inflation; physics of the early
universe
ID MICROWAVE BACKGROUND-RADIATION; GALACTIC DUST EMISSION; POWER SPECTRUM;
WMAP OBSERVATIONS; 2003 FLIGHT; POLARIZATION; ANISOTROPY; TELESCOPE;
TEMPERATURE; BOOMERANG
AB We evaluate the ability of SPIDER, a balloon-borne polarimeter, to detect a divergence-free polarization pattern (B-modes) in the cosmic microwave background (CMB). In the inflationary scenario, the amplitude of this signal is proportional to that of the primordial scalar perturbations through the tensor-to-scalar ratio r. We show that the expected level of systematic error in the SPIDER instrument is significantly below the amplitude of an interesting cosmological signal with r = 0.03. We present a scanning strategy that enables us to minimize uncertainty in the reconstruction of the Stokes parameters used to characterize the CMB, while accessing a relatively wide range of angular scales. Evaluating the amplitude of the polarized Galactic emission in the SPIDER field, we conclude that the polarized emission from interstellar dust is as bright or brighter than the cosmological signal at all SPIDER frequencies (90 GHz, 150 GHz, and 280 GHz), a situation similar to that found in the "Southern Hole." We show that two similar to 20-day flights of the SPIDER instrument can constrain the amplitude of the B-mode signal to r < 0.03 (99% CL) even when foreground contamination is taken into account. In the absence of foregrounds, the same limit can be reached after one 20-day flight.
C1 [Fraisse, A. A.; Chiang, H. C.; Gudmundsson, J. E.; Jones, W. C.; Rahlin, A. S.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
[Tucker, C.; SPIDER Collaboration] Cardiff Univ, Sch Phys & Astron, Cardiff CF10 3AX, S Glam, Wales.
[Amiri, M.; Burger, B.; Davis, G.; Hasselfield, M.; Wiebe, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada.
[Benton, S. J.; Netterfield, C. B.] Univ Toronto, Dept Phys, Toronto, ON, Canada.
[Bock, J. J.; Crill, B. P.; Dore, O.; Filippini, J. P.; Golwala, S.; Hristov, V. V.; Mason, P. V.; Morford, T. A.; Runyan, M. C.; Schenker, M. A.; Trangsrud, A.; Tucker, R. S.] CALTECH, Dept Phys, Pasadena, CA 91125 USA.
[Bock, J. J.; Bonetti, J. A.; Crill, B. P.; Dore, O.; Holmes, W.; Turner, A. D.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Bond, J. R.; Farhang, M.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 1A1, Canada.
[Bryan, S.; Montroy, T. E.; Ruhl, J. E.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA.
[Clark, C. N.; Contaldi, C. R.; O'Dea, D. T.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London, England.
[Farhang, M.; Fissel, L. M.; Gandilo, N. N.; Netterfield, C. B.; Shariff, J. A.; Soler, J. D.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada.
[Hilton, G.; Irwin, K.; Reintsema, C.] NIST, Boulder, CO USA.
[Kuo, C. L.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[MacTavish, C. J.] Univ Cambridge, Kavli Inst Cosmol, Cambridge, England.
RP Fraisse, AA (reprint author), Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
EM afraisse@princeton.edu
FU National Science Foundation [ANT-1043515]; NASA [APRA-NNX07AL64G,
NESSF-NNX10AM55H]; Gordon and Betty Moore Foundation; NSERC; Canadian
Space Agency; CIFAR; Leifur Eiriksson Foundation; NASA Office of Space
Science
FX The SPIDER collaboration gratefully acknowledges the support of the
National Science Foundation (ANT-1043515), NASA (APRA-NNX07AL64G), and
the Gordon and Betty Moore Foundation. Support in Canada is provided by
NSERC, the Canadian Space Agency, and CIFAR. JEG is supported by a grant
from the Leifur Eiriksson Foundation. ASR is supported by NASA
(NESSF-NNX10AM55H). WCJ acknowledges the generous support of the Alfred
P. Sloan Foundation and of the David and Lucile Packard Foundation. Some
of the results in this paper have been derived using the
HEALPix1 [57] package, as well as the FFTW subroutine library
[58]. This research has made use of NASA's Astrophysics Data System. We
acknowledge the use of the Legacy Archive for Microwave Background Data
Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of
Space Science.
NR 59
TC 26
Z9 26
U1 0
U2 4
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 APR
PY 2013
IS 4
AR 047
DI 10.1088/1475-7516/2013/04/047
PG 25
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 139BJ
UT WOS:000318556200047
ER
PT J
AU Rastatter, L
Kuznetsova, MM
Glocer, A
Welling, D
Meng, X
Raeder, J
Wiltberger, M
Jordanova, VK
Yu, Y
Zaharia, S
Weigel, RS
Sazykin, S
Boynton, R
Wei, H
Eccles, V
Horton, W
Mays, ML
Gannon, J
AF Rastaetter, L.
Kuznetsova, M. M.
Glocer, A.
Welling, D.
Meng, X.
Raeder, J.
Wiltberger, M.
Jordanova, V. K.
Yu, Y.
Zaharia, S.
Weigel, R. S.
Sazykin, S.
Boynton, R.
Wei, H.
Eccles, V.
Horton, W.
Mays, M. L.
Gannon, J.
TI Geospace environment modeling 2008-2009 challenge: D-st index
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
DE model validation; GEM 2008 challenge
ID IONOSPHERE-THERMOSPHERE MODEL; OUTPUT PARAMETRIC MODELS; MAGNETIC-FIELD
MODEL; NON-LINEAR SYSTEMS; SOLAR-WIND; ELECTRIC-FIELDS; RING CURRENT;
SIMULATION; MAGNETOSPHERE; SUBSTORM
AB This paper reports the metrics-based results of the Dst index part of the 20082009 GEM Metrics Challenge. The 20082009 GEM Metrics Challenge asked modelers to submit results for four geomagnetic storm events and five different types of observations that can be modeled by statistical, climatological or physics-based models of the magnetosphere-ionosphere system. We present the results of 30 model settings that were run at the Community Coordinated Modeling Center and at the institutions of various modelers for these events. To measure the performance of each of the models against the observations, we use comparisons of 1hour averaged model data with the Dst index issued by the World Data Center for Geomagnetism, Kyoto, Japan, and direct comparison of 1minute model data with the 1minute Dst index calculated by the United States Geological Survey. The latter index can be used to calculate spectral variability of model outputs in comparison to the index. We find that model rankings vary widely by skill score used. None of the models consistently perform best for all events. We find that empirical models perform well in general. Magnetohydrodynamics-based models of the global magnetosphere with inner magnetosphere physics (ring current model) included and stand-alone ring current models with properly defined boundary conditions perform well and are able to match or surpass results from empirical models. Unlike in similar studies, the statistical models used in this study found their challenge in the weakest events rather than the strongest events.
C1 [Rastaetter, L.; Kuznetsova, M. M.] NASA, Goddard Space Flight Ctr, Community Coordinated Modeling Ctr, Greenbelt, MD 20770 USA.
[Glocer, A.; Mays, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
[Welling, D.; Meng, X.] Univ Michigan, Coll Engn, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Raeder, J.] Univ New Hampshire, Inst Study Earth Oceans & Space, Dept Phys, Durham, NH 03824 USA.
[Wiltberger, M.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Jordanova, V. K.; Yu, Y.; Zaharia, S.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Weigel, R. S.] George Mason Univ, Dept Computat & Data Sci, Fairfax, VA 22030 USA.
[Sazykin, S.] Rice Univ, Sch Phys Astron & Computat Sci, Houston, TX USA.
[Boynton, R.; Wei, H.] Univ Sheffield, ACSE, Sheffield, S Yorkshire, England.
[Eccles, V.] Space Environm Corp, Providence, UT USA.
[Horton, W.] Univ Texas Austin, Inst Fus Studies, Austin, TX 78712 USA.
[Gannon, J.] US Geol Survey, Golden, CO USA.
RP Rastatter, L (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Lab, Code 674, Greenbelt, MD 20770 USA.
EM lutz.rastaetter@nasa.gov
RI Glocer, Alex/C-9512-2012; Yu, Yiqun/E-2710-2012; Welling,
Daniel/C-1970-2013; Wiltberger, Michael/B-8781-2008; Rastaetter,
Lutz/D-4715-2012; Sazykin, Stanislav/C-3775-2008; Meng,
Xing/A-1929-2016;
OI Glocer, Alex/0000-0001-9843-9094; Yu, Yiqun/0000-0002-1013-6505;
Jordanova, Vania/0000-0003-0475-8743; Wiltberger,
Michael/0000-0002-4844-3148; Rastaetter, Lutz/0000-0002-7343-4147;
Sazykin, Stanislav/0000-0002-9401-4248; Wei,
Hua-Liang/0000-0002-4704-7346
FU Center for Integrated Space Weather Modeling; Science and Technology
Centers program of the National Science Foundation [ATM-0120950];
National Science Foundation
FX Hourly Dst data were obtained from the World Data Center of
Geomagnetism, Kyoto, Japan and 1 minute data were obtained from the
United States Geological Survey (USGS). Both index values include
magnetic data from the following stations: KAK: Kakioka Magnetic
Observatory, Japan Meteorological Agency, Japan, HON, SJG: Honolulu and
San Juan magnetic observatories, USGS, HER: Hermanus Magnetic
Observatory, South African National Space Agency (SANSA). Solar wind
input data for the models (magnetic field and plasma parameters) were
obtained from OMNI (http://omniweb.gsfc.nasa.gov) and CDAweb
(cdaweb.gsfc.nasa.gov) databases. This work was supported by the Center
for Integrated Space Weather Modeling, which is funded by the Science
and Technology Centers program of the National Science Foundation under
agreement number ATM-0120950. The National Center for Atmospheric
Research is sponsored by the National Science Foundation.
NR 69
TC 15
Z9 15
U1 0
U2 11
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1539-4956
J9 SPACE WEATHER
JI Space Weather
PD APR
PY 2013
VL 11
IS 4
BP 187
EP 205
DI 10.1002/swe.20036
PG 19
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA 140EH
UT WOS:000318636700008
ER
PT J
AU Adams, JH
Ahmad, S
Albert, JN
Allard, D
Ambrosio, M
Anchordoqui, L
Anzalone, A
Arai, Y
Aramo, C
Asano, K
Ave, M
Barrillon, P
Batsch, T
Bayer, J
Belenguer, T
Bellotti, R
Berlind, AA
Bertaina, M
Biermann, PL
Biktemerova, S
Blaksley, C
Biccki, J
Blin-Bondil, S
Blumer, J
Bobik, P
Bogomilov, M
Bonamente, M
Briggs, MS
Briz, S
Bruno, A
Cafagna, F
Campana, D
Capdevielle, JN
Caruso, R
Casolino, M
Cassardo, C
Castellini, G
Catalano, O
Cellino, A
Chikawa, M
Christi, MJ
Connaughton, V
Cortes, JF
Crawford, HJ
Cremonini, R
Csorna, S
D'Olivo, JC
Dagoret-Campagne, S
de Castro, AJ
De Donato, C
de la Taille, C
del Peral, L
Dell'Oro, A
De Pascale, MP
Di Martino, M
Distratis, G
Dupieux, M
Ebersoldt, A
Ebisuzaki, T
Engel, R
Falk, S
Fang, K
Fenu, F
Fernandez-Gomez, I
Ferrarese, S
Franceschi, A
Fujimoto, J
Galeotti, P
Garipov, G
Geary, J
Giaccari, UG
Giraudo, G
Gonchar, M
Alvarado, CG
Gorodetzky, P
Guarino, F
Guzman, A
Hachisu, Y
Harlov, B
Haungs, A
Carretero, JH
Higashide, K
Iguchi, T
Ikeda, H
Inoue, N
Inoue, S
Insolia, A
Isgro, F
Itow, Y
Joven, E
Judd, EG
Jung, A
Kajino, F
Kajino, T
Kaneko, I
Karadzhov, Y
Karczmarczyk, J
Katahira, K
Kawai, K
Kawasaki, Y
Keilhauer, B
Khrenov, BA
Kim, JS
Kim, SW
Kim, SW
Kleifges, M
Klimov, PA
Ko, SH
Kolev, D
Kreykenbohm, I
Kudela, K
Kurihara, Y
Kuznetsov, E
La Rosa, G
Lee, J
Licandro, J
Lim, H
Lopez, F
Maccarone, MC
Mannheim, K
Marcelli, L
Marini, A
Martin-Chassard, G
Martinez, O
Masciantonio, G
Mase, K
Matev, R
Maurissen, A
Medina-Tanco, G
Mernik, T
Miyamoto, H
Miyazaki, Y
Mizumoto, Y
Modestino, G
Monnier-Ragaigne, D
de los Rios, JAM
Mot, B
Murakami, T
Nagano, M
Nagata, M
Nagataki, S
Nakamura, T
Nam, JW
Nam, S
Nam, K
Napolitano, T
Naumov, D
Neronov, A
Nomoto, K
Ogawa, T
Ohmori, H
Olinto, AV
Orleanski, P
Osteria, G
Pacheco, N
Panasyuk, MI
Parizot, E
Park, IH
Pastircak, B
Patzak, T
Paul, T
Pennypacker, C
Peter, T
Picozza, P
Pollini, A
Prieto, H
Reardon, P
Reinabi, M
Reyes, M
Ricci, M
Rodriguez, I
Frias, MDR
Ronga, F
Rothkaehl, H
Roudil, G
Rusinov, I
Rybczynski, M
Sabau, MD
Cano, GS
Saito, A
Sakaki, N
Sakata, M
Salazar, H
Sanchez, S
Santangelo, A
Cruz, LS
Palomino, MS
Saprykin, O
Sarazin, F
Sato, H
Sato, M
Schanz, T
Schieler, H
Scotti, V
Scuderi, M
Segreto, A
Selmane, S
Semikoz, D
Serra, M
Sharakin, S
Shibata, T
Shimizu, HM
Shinozaki, K
Shirahama, T
Siemieniec-Ozigbio, G
Lopez, HHS
Sledd, J
Slomiriska, K
Sobey, A
Sugiyama, T
Supanitsky, D
Suzuki, M
Szabelska, B
Szabelski, J
Tajima, F
Tajima, N
Tajima, T
Takahashi, Y
Takami, H
Takeda, M
Takizawa, Y
Tenzer, C
Tibolla, O
Tkachev, L
Tomida, T
Tone, N
Trillaud, F
Tsenov, R
Tsuno, K
Tymieniecka, T
Uchihori, Y
Vaduvescu, O
Valdes-Galicia, JF
Vallania, P
Valore, L
Vankova, G
Vigorito, C
Villasenor, L
von Ballmoos, P
Wada, S
Watanabe, J
Watanabe, S
Watts, J
Weber, M
Weiler, TJ
Wibig, T
Wiencke, L
Wille, M
Wilms, J
Wlodarczyk, Z
Yamamoto, T
Yamamoto, Y
Yang, J
Yano, H
Yashin, IV
Yonetoku, D
Yoshida, K
Yoshida, S
Young, R
Zamora, A
Marchi, AZ
AF Adams, J. H., Jr.
Ahmad, S.
Albert, J. -N.
Allard, D.
Ambrosio, M.
Anchordoqui, L.
Anzalone, A.
Arai, Y.
Aramo, C.
Asano, K.
Ave, M.
Barrillon, P.
Batsch, T.
Bayer, J.
Belenguer, T.
Bellotti, R.
Berlind, A. A.
Bertaina, M.
Biermann, P. L.
Biktemerova, S.
Blaksley, C.
Biccki, J.
Blin-Bondil, S.
Bluemer, J.
Bobik, P.
Bogomilov, M.
Bonamente, M.
Briggs, M. S.
Briz, S.
Bruno, A.
Cafagna, F.
Campana, D.
Capdevielle, J. -N.
Caruso, R.
Casolino, M.
Cassardo, C.
Castellini, G.
Catalano, O.
Cellino, A.
Chikawa, M.
Christi, M. J.
Connaughton, V.
Cortes, J. F.
Crawford, H. J.
Cremonini, R.
Csorna, S.
D'Olivo, J. C.
Dagoret-Campagne, S.
de Castro, A. J.
De Donato, C.
de la Taille, C.
del Peral, L.
Dell'Oro, A.
De Pascale, M. P.
Di Martino, M.
Distratis, G.
Dupieux, M.
Ebersoldt, A.
Ebisuzaki, T.
Engel, R.
Falk, S.
Fang, K.
Fenu, F.
Fernandez-Gomez, I.
Ferrarese, S.
Franceschi, A.
Fujimoto, J.
Galeotti, P.
Garipov, G.
Geary, J.
Giaccari, U. G.
Giraudo, G.
Gonchar, M.
Gonzalez Alvarado, C.
Gorodetzky, P.
Guarino, F.
Guzman, A.
Hachisu, Y.
Harlov, B.
Haungs, A.
Hernandez Carretero, J.
Higashide, K.
Iguchi, T.
Ikeda, H.
Inoue, N.
Inoue, S.
Insolia, A.
Isgro, F.
Itow, Y.
Joven, E.
Judd, E. G.
Jung, A.
Kajino, F.
Kajino, T.
Kaneko, I.
Karadzhov, Y.
Karczmarczyk, J.
Katahira, K.
Kawai, K.
Kawasaki, Y.
Keilhauer, B.
Khrenov, B. A.
Kim, Jeong-Sook
Kim, Soon-Wook
Kim, Sug-Whan
Kleifges, M.
Klimov, P. A.
Ko, S. H.
Kolev, D.
Kreykenbohm, I.
Kudela, K.
Kurihara, Y.
Kuznetsov, E.
La Rosa, G.
Lee, J.
Licandro, J.
Lim, H.
Lopez, F.
Maccarone, M. C.
Mannheim, K.
Marcelli, L.
Marini, A.
Martin-Chassard, G.
Martinez, O.
Masciantonio, G.
Mase, K.
Matev, R.
Maurissen, A.
Medina-Tanco, G.
Mernik, T.
Miyamoto, H.
Miyazaki, Y.
Mizumoto, Y.
Modestino, G.
Monnier-Ragaigne, D.
Morales de los Rios, J. A.
Mot, B.
Murakami, T.
Nagano, M.
Nagata, M.
Nagataki, S.
Nakamura, T.
Nam, J. W.
Nam, S.
Nam, K.
Napolitano, T.
Naumov, D.
Neronov, A.
Nomoto, K.
Ogawa, T.
Ohmori, H.
Olinto, A. V.
Orleanski, P.
Osteria, G.
Pacheco, N.
Panasyuk, M. I.
Parizot, E.
Park, I. H.
Pastircak, B.
Patzak, T.
Paul, T.
Pennypacker, C.
Peter, T.
Picozza, P.
Pollini, A.
Prieto, H.
Reardon, P.
Reinabi, M.
Reyes, M.
Ricci, M.
Rodriguez, I.
Rodriguez Frias, M. D.
Ronga, F.
Rothkaehl, H.
Roudil, G.
Rusinov, I.
Rybczynski, M.
Sabau, M. D.
Saez Cano, G.
Saito, A.
Sakaki, N.
Sakata, M.
Salazar, H.
Sanchez, S.
Santangelo, A.
Santiago Cruz, L.
Sanz Palomino, M.
Saprykin, O.
Sarazin, F.
Sato, H.
Sato, M.
Schanz, T.
Schieler, H.
Scotti, V.
Scuderi, M.
Segreto, A.
Selmane, S.
Semikoz, D.
Serra, M.
Sharakin, S.
Shibata, T.
Shimizu, H. M.
Shinozaki, K.
Shirahama, T.
Siemieniec-Ozigbio, G.
Silva Lopez, H. H.
Sledd, J.
Slomiriska, K.
Sobey, A.
Sugiyama, T.
Supanitsky, D.
Suzuki, M.
Szabelska, B.
Szabelski, J.
Tajima, F.
Tajima, N.
Tajima, T.
Takahashi, Y.
Takami, H.
Takeda, M.
Takizawa, Y.
Tenzer, C.
Tibolla, O.
Tkachev, L.
Tomida, T.
Tone, N.
Trillaud, F.
Tsenov, R.
Tsuno, K.
Tymieniecka, T.
Uchihori, Y.
Vaduvescu, O.
Valdes-Galicia, J. F.
Vallania, P.
Valore, L.
Vankova, G.
Vigorito, C.
Villasenor, L.
von Ballmoos, P.
Wada, S.
Watanabe, J.
Watanabe, S.
Watts, J., Jr.
Weber, M.
Weiler, T. J.
Wibig, T.
Wiencke, L.
Wille, M.
Wilms, J.
Wlodarczyk, Z.
Yamamoto, T.
Yamamoto, Y.
Yang, J.
Yano, H.
Yashin, I. V.
Yonetoku, D.
Yoshida, K.
Yoshida, S.
Young, R.
Zamora, A.
Marchi, A. Zuccaro
TI An evaluation of the exposure in nadir observation of the JEM-EUSO
mission
SO ASTROPARTICLE PHYSICS
LA English
DT Article
DE Ultra High Energy Cosmic Rays; Space-based experiment; Extensive air
showers; JEM-EUSO mission
ID EXTENSIVE AIR SHOWERS; ENERGY COSMIC-RAYS; SPACE; RADIATION; SPECTRUM;
DETECTOR; CLOUDS; NM
AB We evaluate the exposure during nadir observations with JEM-EUSO, the Extreme Universe Space Observatory, on-board the Japanese Experiment Module of the International Space Station. Designed as a mission to explore the extreme energy Universe from space, JEM-EUSO will monitor the Earth's nighttime atmosphere to record the ultraviolet light from tracks generated by extensive air showers initiated by ultra-high energy cosmic rays. In the present work, we discuss the particularities of space-based observation and we compute the annual exposure in nadir observation. The results are based on studies of the expected trigger aperture and observational duty cycle, as well as, on the investigations of the effects of clouds and different types of background light. We show that the annual exposure is about one order of magnitude higher than those of the presently operating ground-based observatories. (C) 2013 Elsevier B.V. All rights reserved.
C1 [Bogomilov, M.; Karadzhov, Y.; Kolev, D.; Matev, R.; Rusinov, I.; Tsenov, R.; Vankova, G.] Sofia Univ St Kliment Ohridski, Sofia, Bulgaria.
[Ahmad, S.; Albert, J. -N.; Barrillon, P.; Blin-Bondil, S.; de la Taille, C.; Martin-Chassard, G.; Monnier-Ragaigne, D.; Weiler, T. J.] Univ Paris 11, Lab Accelerateur Lineaire, CNES, IN2P3, Orsay, France.
[Allard, D.; Blaksley, C.; Capdevielle, J. -N.; Gorodetzky, P.; Parizot, E.; Patzak, T.; Selmane, S.; Semikoz, D.] Univ Paris Diderot, APC, CNRS, CEA,Irfu,IN2P3, Sorbonne Paris Cite, France.
[Dupieux, M.; Mot, B.; Roudil, G.; von Ballmoos, P.] Univ Toulouse, CNRS, IRAP, Toulouse, France.
[Kreykenbohm, I.; Wille, M.; Wilms, J.] Univ Erlangen Nurnberg, ECAP, Erlangen, Germany.
[Biermann, P. L.; Bluemer, J.; Ebersoldt, A.; Engel, R.; Falk, S.; Haungs, A.; Keilhauer, B.; Kleifges, M.; Sakaki, N.; Schieler, H.; Scuderi, M.; Weber, M.] Karlsruhe Inst Technol KIT, Karlsruhe, Germany.
[Tajima, T.] Univ Munich, Munich, Germany.
[Bayer, J.; Distratis, G.; Fenu, F.; Guzman, A.; Mernik, T.; Santangelo, A.; Schanz, T.; Tenzer, C.] Univ Tubingen, Kepler Ctr, Inst Astron & Astrophys, Tubingen, Germany.
[Mannheim, K.; Tibolla, O.] Univ Wurzburg, Inst Theoret Phys & Astrophys, Wurzburg, Germany.
[Bruno, A.; Cafagna, F.] Ist Nazl Fis Nucl, Sez Bari, Bari, Italy.
[Bellotti, R.] Univ Bari Aldo Moro, Bari, Italy.
[Bellotti, R.] INFN Sez Bari, Bari, Italy.
[Insolia, A.] Univ Catania, Dipartimento Fis & Astron, I-95124 Catania, Italy.
[Castellini, G.] CNR, Ist Nazl Ott Firenze, Florence, Italy.
[Franceschi, A.; Marini, A.; Modestino, G.; Napolitano, T.; Ricci, M.; Ronga, F.] Ist Nazl Fis Nucl, Lab Nazl Frascati, Frascati, Italy.
[Ambrosio, M.; Aramo, C.; Campana, D.; Giaccari, U. G.; Guarino, F.; Isgro, F.; Osteria, G.; Scotti, V.; Valore, L.] Ist Nazl Fis Nucl, Sez Napoli, Naples, Italy.
[Guarino, F.; Isgro, F.; Scotti, V.] Univ Naples Federico II, Dipartimento Sci Fis, Naples, Italy.
[Anzalone, A.; Catalano, O.; La Rosa, G.; Maccarone, M. C.; Segreto, A.] INAF Ist Astrofis Spaziale & Fis Cosm Palermo, Palermo, Italy.
[Casolino, M.; De Donato, C.; De Pascale, M. P.; Marcelli, L.; Masciantonio, G.; Picozza, P.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, Rome, Italy.
[Casolino, M.; De Donato, C.; De Pascale, M. P.; Marcelli, L.; Masciantonio, G.; Picozza, P.] Univ Roma Tor Vergata, Dipartimento Fis, Rome, Italy.
[Bertaina, M.; Cassardo, C.; Cellino, A.; Dell'Oro, A.; Di Martino, M.; Ferrarese, S.; Galeotti, P.; Giraudo, G.; Vallania, P.; Vigorito, C.] Ist Nazl Fis Nucl, Sez Torino, Turin, Italy.
[Bertaina, M.; Cassardo, C.; Cremonini, R.; Ferrarese, S.; Galeotti, P.; Vigorito, C.] Univ Turin, Dipartimento Fis, I-10125 Turin, Italy.
[Cellino, A.; Dell'Oro, A.; Di Martino, M.; Vallania, P.] Osserv Astron Torino, Ist Nazl Astrofis, Turin, Italy.
[Mase, K.; Yoshida, S.] Chiba Univ, Chiba, Japan.
[Uchihori, Y.] Natl Inst Radiol Sci, Chiba 260, Japan.
[Miyazaki, Y.; Nagano, M.] Fukui Univ Technol, Fukui, Japan.
[Chikawa, M.] Kinki Univ, Higashiosaka, Osaka 577, Japan.
[Tajima, F.] Hiroshima Univ, Hiroshima, Japan.
[Murakami, T.; Yonetoku, D.] Kanazawa Univ, Kanazawa, Ishikawa, Japan.
[Takeda, M.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba, Japan.
[Nagata, M.] Kobe Univ, Kobe, Hyogo 657, Japan.
[Iguchi, T.; Kajino, F.; Sakata, M.; Sato, H.; Yamamoto, T.; Yamamoto, Y.; Yoshida, K.] Konan Univ, Kobe, Hyogo, Japan.
[Nakamura, T.; Saito, A.] Kyoto Univ, Kyoto, Japan.
[Nagataki, S.] Kyoto Univ, Yukawa Inst, Kyoto, Japan.
[Kajino, T.; Mizumoto, Y.; Watanabe, J.] Natl Astron Observ, Mitaka, Tokyo 181, Japan.
[Shimizu, H. M.; Sugiyama, T.] Nagoya Univ, Nagoya, Aichi 4648601, Japan.
[Itow, Y.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Ikeda, H.; Suzuki, M.; Yano, H.] Inst Space & Astronaut Sci JAXA, Sagamihara, Kanagawa, Japan.
[Shibata, T.] Aoyama Gakuin Univ, Sagamihara, Kanagawa, Japan.
[Higashide, K.; Inoue, N.; Shirahama, T.] Saitama Univ, Saitama 3388570, Japan.
[Sato, M.; Takahashi, Y.; Watanabe, S.] Hokkaido Univ, Sapporo, Hokkaido, Japan.
[Asano, K.] Tokyo Inst Technol, Interact Res Ctr Sci, Tokyo 152, Japan.
[Inoue, S.; Nomoto, K.] Univ Tokyo, Tokyo, Japan.
[Arai, Y.; Fujimoto, J.; Kurihara, Y.; Takami, H.] High Energy Accelerator Res Org KEK, Tsukuba, Ibaraki, Japan.
[Casolino, M.; Ebisuzaki, T.; Hachisu, Y.; Higashide, K.; Kaneko, I.; Katahira, K.; Kawai, K.; Kawasaki, Y.; Miyamoto, H.; Ogawa, T.; Ohmori, H.; Picozza, P.; Shinozaki, K.; Tajima, N.; Takizawa, Y.; Tomida, T.; Tone, N.; Tsuno, K.; Wada, S.; Marchi, A. Zuccaro] RIKEN Adv Sci Inst, Wako, Saitama, Japan.
[Ko, S. H.] Korea Adv Inst Sci & Technol, Taejon 305701, South Korea.
[Kim, Jeong-Sook; Kim, Soon-Wook] Korea Astron & Space Sci Inst KASI, Taejon, South Korea.
[Jung, A.; Lee, J.; Lim, H.; Nam, J. W.; Nam, S.; Nam, K.; Park, I. H.; Yang, J.] Ewha Womans Univ, Seoul, South Korea.
[Kim, Sug-Whan] Yonsei Univ, Ctr Galaxy Evolut Res, Seoul 120749, South Korea.
[D'Olivo, J. C.; Medina-Tanco, G.; Santiago Cruz, L.; Silva Lopez, H. H.; Supanitsky, D.; Trillaud, F.; Valdes-Galicia, J. F.; Zamora, A.] Univ Nacl Autonoma Mexico, Mexico City, DF, Mexico.
[Villasenor, L.] UMSNH, Morelia, Michoacan, Mexico.
[Martinez, O.; Salazar, H.] BUAP, Mexico City, DF, Mexico.
[Rybczynski, M.; Wlodarczyk, Z.] Jan Kochanowski Univ Humanities & Sci, Inst Phys, Kielce, Poland.
[Siemieniec-Ozigbio, G.] Jagiellonian Univ, Astron Observ, Krakow, Poland.
[Batsch, T.; Karczmarczyk, J.; Szabelska, B.; Szabelski, J.; Wibig, T.] Natl Ctr Nucl Res, Lodz, Poland.
[Tymieniecka, T.] Cardinal Stefan Wyszyriski Univ, Warsaw, Poland.
[Biccki, J.; Orleanski, P.; Rothkaehl, H.; Slomiriska, K.] Polish Acad Sci CBK, Space Res Ctr, Warsaw, Poland.
[Biktemerova, S.; Gonchar, M.; Naumov, D.; Tkachev, L.] Joint Inst Nucl Res, Dubna, Russia.
[Harlov, B.; Saprykin, O.] TsNIIMash, Cent Res Inst Machine Bldg, Korolev, Russia.
[Garipov, G.; Khrenov, B. A.; Klimov, P. A.; Panasyuk, M. I.; Sharakin, S.; Yashin, I. V.] Moscow MV Lomonosov State Univ, Skobeltsyn Inst Nucl Phys, Moscow 117234, Russia.
[Bobik, P.; Kudela, K.; Pastircak, B.] Slovak Acad Sci, Inst Expt Phys, Kosice 04353, Slovakia.
[Prieto, H.] CSIC, Madrid, Spain.
[Belenguer, T.; Gonzalez Alvarado, C.; Reinabi, M.; Sabau, M. D.; Sanz Palomino, M.] INTA, Madrid, Spain.
[Pacheco, N.] Univ Autonoma Madrid, Inst Fis Teor, E-28049 Madrid, Spain.
[del Peral, L.; Hernandez Carretero, J.; Morales de los Rios, J. A.; Prieto, H.; Rodriguez Frias, M. D.; Saez Cano, G.] Univ Alcala UAH, Madrid, Spain.
[Briz, S.; Cortes, J. F.; de Castro, A. J.; Fernandez-Gomez, I.; Lopez, F.; Rodriguez, I.; Sanchez, S.] Univ Carlos III Madrid, E-28903 Getafe, Spain.
[Ave, M.] Univ Santiago de Compostela, Santiago De Compostela, Spain.
[Joven, E.; Licandro, J.; Reyes, M.; Serra, M.; Vaduvescu, O.] IAC, Tenerife, Spain.
[Maurissen, A.; Pollini, A.] Swiss Ctr Elect & Microtechnol CSEM, Neuchatel, Switzerland.
[Neronov, A.] ISDC Data Ctr Astrophys, Versoix, Switzerland.
[Peter, T.] ETH, Inst Atmospher & Climate Sci, Zurich, Switzerland.
[Crawford, H. J.; Judd, E. G.; Pennypacker, C.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Fang, K.; Olinto, A. V.] Univ Chicago, Chicago, IL 60637 USA.
[Sarazin, F.; Wiencke, L.] Colorado Sch Mines, Golden, CO 80401 USA.
[Adams, J. H., Jr.; Bonamente, M.; Briggs, M. S.; Connaughton, V.; Geary, J.; Kuznetsov, E.; Reardon, P.; Watts, J., Jr.] Univ Alabama, Huntsville, AL 35899 USA.
[Anchordoqui, L.; Paul, T.] Univ Wisconsin, Milwaukee, WI 53201 USA.
[Christi, M. J.; Sledd, J.; Sobey, A.; Young, R.] NASA, George C Marshall Space Flight Ctr, Washington, DC USA.
[Berlind, A. A.; Csorna, S.] Vanderbilt Univ, Nashville, TN USA.
RP Bertaina, M (reprint author), Univ Turin, Dipartimento Fis, I-10125 Turin, Italy.
EM bertaina@to.infn.it; kenjikry@riken.jp
RI scuderi, mario/O-7019-2014; Guarino, Fausto/I-3166-2012; marcelli,
laura/K-8860-2016; Rodriguez Frias, Maria /A-7608-2015; Briz,
Susana/G-7732-2015; Ko, Seung Hwan/B-5448-2008; Insolia,
Antonio/M-3447-2015; Cellino, Alberto/N-1570-2015; Kreykenbohm,
Ingo/H-9659-2013; Ko, Seung Hwan/C-2043-2011; Klimov, Pavel/E-2783-2012;
Wilms, Joern/C-8116-2013; Panasyuk, Mikhail/E-2005-2012; Cafagna,
Francesco/A-9299-2010; Ebisuzaki, Toshikazu/N-6998-2014; Ohmori ,
Hitoshi /A-7562-2015; LOPEZ, FERNANDO/H-5071-2015; De Donato,
Cinzia/J-9132-2015
OI Aramo, Carla/0000-0002-8412-3846; Bertaina, Mario
Edoardo/0000-0003-1069-1397; Dell'Oro, Aldo/0000-0003-1561-9685;
Anzalone, Anna/0000-0003-1849-198X; Bellotti,
Roberto/0000-0003-3198-2708; Vallania, Piero/0000-0001-9089-7875; La
Rosa, Giovanni/0000-0002-3931-2269; Modestino,
Giuseppina/0000-0003-1556-3917; Cassardo, Claudio/0000-0001-5212-3211;
casolino, marco/0000-0001-6067-5104; Catalano,
Osvaldo/0000-0002-9554-4128; Segreto, Alberto/0000-0001-7341-6603;
Maccarone, Maria Concetta/0000-0001-8722-0361; Isgro,
Francesco/0000-0001-9342-5291; Castellini, Guido/0000-0002-0177-0643;
Naumov, Dmitry Vadimovich/0000-0002-0966-8803; Picozza,
Piergiorgio/0000-0002-7986-3321; scuderi, mario/0000-0001-9026-5317;
Guarino, Fausto/0000-0003-1427-9885; marcelli,
laura/0000-0002-3180-1228; Rodriguez Frias, Maria /0000-0002-2550-4462;
Briz, Susana/0000-0001-5963-3257; Wibig, Tadeusz/0000-0002-2078-0580;
Weiler, Thomas/0000-0002-0885-1868; Franceschi, Massimo
Alberto/0000-0002-8222-7000; Masciantonio, Giuseppe/0000-0002-8911-1561;
Del Peral, Luis/0000-0003-2580-5668; Ko, Seung Hwan/0000-0002-7477-0820;
Insolia, Antonio/0000-0002-9040-1566; Cellino,
Alberto/0000-0002-6645-334X; Kreykenbohm, Ingo/0000-0001-7335-1803;
Klimov, Pavel/0000-0001-9815-6123; Wilms, Joern/0000-0003-2065-5410;
Cafagna, Francesco/0000-0002-7450-4784; Ebisuzaki,
Toshikazu/0000-0002-3918-1166; LOPEZ, FERNANDO/0000-0003-4723-0535; De
Donato, Cinzia/0000-0002-9725-1281
FU RIKEN; JSPS KAKENHI [22340063, 23340081, 24244042]; Italian Ministry of
Foreign Affairs, General Direction for the Cultural Promotion and
Cooperation; Helmholtz Alliance for Astroparticle Physics HAP; Helmholtz
Association, Germany; Slovak Academy of Sciences MVTS JEM-EUSO; VEGA
grant agency [2/0081/10]; MICINN [AYA2009-06037-E/ESP, AYA-ESP
2010-19082, AYA2011-29489-C03-01, AYA2012-39115-C03-01, CSD2009-00064];
Comunidad de Madrid (CAM) [S2009/ESP-1496]
FX This work was partially supported by Basic Science Interdisciplinary
Research Projects of RIKEN and JSPS KAKENHI Grant (22340063, 23340081,
and 24244042), by the Italian Ministry of Foreign Affairs, General
Direction for the Cultural Promotion and Cooperation, by the 'Helmholtz
Alliance for Astroparticle Physics HAP' funded by the Initiative and
Networking Fund of the Helmholtz Association, Germany, and by Slovak
Academy of Sciences MVTS JEM-EUSO as well as VEGA grant agency project
2/0081/10. The Spanish Consortium involved in the JEM-EUSO Space Mission
is funded by MICINN under projects AYA2009-06037-E/ESP, AYA-ESP
2010-19082, AYA2011-29489-C03-01, AYA2012-39115-C03-01, CSD2009-00064
(Consolider MULTIDARK) and by Comunidad de Madrid (CAM) under project
S2009/ESP-1496.
NR 53
TC 55
Z9 55
U1 2
U2 53
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0927-6505
EI 1873-2852
J9 ASTROPART PHYS
JI Astropart Phys.
PD APR
PY 2013
VL 44
BP 76
EP 90
DI 10.1016/j.astropartphys.2013.01.008
PG 15
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 135WT
UT WOS:000318322100009
ER
PT J
AU Hoffmayer, ER
Franks, JS
Driggers, WB
Howey, PW
AF Hoffmayer, Eric R.
Franks, James S.
Driggers, William B., III
Howey, Paul W.
TI DIEL VERTICAL MOVEMENTS OF A SCALLOPED HAMMERHEAD, SPHYRNA LEWINI, IN
THE NORTHERN GULF OF MEXICO
SO BULLETIN OF MARINE SCIENCE
LA English
DT Article
ID SATELLITE ARCHIVAL TAGS; TUNA THUNNUS-THYNNUS; PACIFIC-OCEAN; SHARKS;
CALIFORNIA; FISH; TEMPERATURE; AUSTRALIA; TRACKING; MOKARRAN
AB Despite the circumglobal distribution of scalloped hammerheads, Sphyrna lewini (Griffith and Smith, 1834), little information is available regarding fine-scale movement and habitat use patterns for this species. Over a 27-d period, data were collected on diel habitat use and environmental preferences of a 240 cm (total length) female S. lewini. The shark exhibited a consistent and repeated diel vertical movement pattern, making more than 76 deep nighttime dives; the maximum depth reached was 964 m, where the temperature was 5.8 degrees C. The purpose of the nightly oscillatory deep diving pattern is unknown but could possibly represent feeding behavior. These findings represent the first detailed account of S. lewini diel vertical behavior and habitat utilization in the western North Atlantic Ocean.
C1 [Hoffmayer, Eric R.; Driggers, William B., III] Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Mississippi Labs, Pascagoula, MS 39567 USA.
[Franks, James S.] Univ So Mississippi, Gulf Coast Res Lab, Ctr Fisheries Res & Dev, Ocean Springs, MS 39564 USA.
[Howey, Paul W.] Microwave Telemetry Inc, Columbia, MD 21045 USA.
RP Hoffmayer, ER (reprint author), Natl Marine Fisheries Serv, Southeast Fisheries Sci Ctr, Mississippi Labs, PO Drawer 1207, Pascagoula, MS 39567 USA.
EM eric.hoffmayer@noaa.gov
RI sebastianovitsch, stepan/G-8507-2013
FU US National Marine Fisheries Service [NA08NMF4540389]
FX We extend our appreciation to B Delabar and BC Bobby of the sport
fishing vessel FRENZY (Venice, Louisiana). We also thank R Berg (BEI,
Inc.) for providing video of the scalloped hammerhead aggregation at
MC582 the day prior to our tagging event. G Parsons provided valuable
comments on an earlier version of the manuscript. This research was
partially supported by US National Marine Fisheries Service, Cooperative
Research Program, Grant #NA08NMF4540389 to E Hoffmayer and J Franks.
This research was conducted in compliance with US law under Scientific
Research Permit HMS-EFP-08-07, issued by the Highly Migratory Species
Division of the Office of Sustainable Fisheries, National Marine
Fisheries Service, Silver Spring, MD 20910, USA, and the Institutional
Animal Care and Use Committee of the University of Southern Mississippi
(protocol 09031204). Mention of commercial products does not imply
endorsement by the University of Southern Mississippi or the National
Marine Fisheries Service.
NR 22
TC 5
Z9 6
U1 3
U2 38
PU ROSENSTIEL SCH MAR ATMOS SCI
PI MIAMI
PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA
SN 0007-4977
J9 B MAR SCI
JI Bull. Mar. Sci.
PD APR
PY 2013
VL 89
IS 2
BP 551
EP 557
DI 10.5343/bms.2012.1048
PG 7
WC Marine & Freshwater Biology; Oceanography
SC Marine & Freshwater Biology; Oceanography
GA 136QM
UT WOS:000318378500009
ER
PT J
AU Angal, A
Xiong, XX
Wu, AS
Chander, G
Choi, T
AF Angal, Amit
Xiong, Xiaoxiong
Wu, Aisheng
Chander, Gyanesh
Choi, Taeyoung
TI Multitemporal Cross-Calibration of the Terra MODIS and Landsat 7 ETM+
Reflective Solar Bands
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Cross-calibration; landsat ETM; Libya-4; MODTRAN; MODIS; water-vapor
ID NEAR-INFRARED CHANNELS; SATELLITE SENSORS; DESERT SITES; WATER-VAPOR;
PERFORMANCE; AVHRR; MODEL
AB In recent years, there has been a significant increase in the use of remotely sensed data to address global issues. With the open data policy, the data from the Moderate Resolution Imaging Spectroradiometer (MODIS) and Enhanced Thematic Mapper Plus (ETM+) sensors have become a critical component of numerous applications. These two sensors have been operational for more than a decade, providing a rich archive of multispectral imagery for analysis of mutitemporal remote sensing data. This paper focuses on evaluating the radiometric calibration agreement between MODIS and ETM+ using the near-simultaneous and cloud-free image pairs over an African pseudo-invariant calibration site, Libya 4. To account for the combined uncertainties in the top-of-atmosphere (TOA) reflectance due to surface and atmospheric bidirectional reflectance distribution function (BRDF), a semiempirical BRDF model was adopted to normalize the TOA reflectance to the same illumination and viewing geometry. In addition, the spectra from the Earth Observing-1 (EO-1) Hyperion were used to compute spectral corrections between the corresponding MODIS and ETM+ spectral bands. As EO-1 Hyperion scenes were not available for all MODIS and ETM+ data pairs, MODerate resolution atmospheric TRANsmission (MODTRAN) 5.0 simulations were also used to adjust for differences due to the presence or lack of absorption features in some of the bands. A MODIS split-window algorithm provides the atmospheric water vapor column abundance during the overpasses for the MODTRAN simulations. Additionally, the column atmospheric water vapor content during the overpass was retrieved using the MODIS precipitable water vapor product. After performing these adjustments, the radiometric cross-calibration of the two sensors was consistent to within 7%. Some drifts in the response of the bands are evident, with MODIS band 3 being the largest of about 6% over 10 years, a change that will be corrected in Collection 6 MODIS processing.
C1 [Angal, Amit] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
[Wu, Aisheng; Choi, Taeyoung] Sigma Space Co, Lanham, MD 20706 USA.
[Chander, Gyanesh] SGT Inc, Greenbelt, MD 20770 USA.
RP Angal, A (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
EM amit.angal@ssaihq.com; Xiaoxiong.Xiong-1@nasa.gov; wu@sigmaspace.com;
gchander@usgs.gov; tchoi@sigmaspace.com
RI Trivedi, Kruti/E-7558-2015; Choi, Taeyoung/E-4437-2016; Richards,
Amber/K-8203-2015
OI Choi, Taeyoung/0000-0002-4596-989X;
FU U.S. Geological Survey [G10PC00044]
FX The authors would like to thank T. Adamson (SGT) for providing helpful
comments in the technical review of this paper. The work performed by G.
Chander is under U.S. Geological Survey contract G10PC00044. The
detailed comments from the anonymous reviewers were extremely helpful in
improving the quality and readability of this paper.
NR 25
TC 14
Z9 14
U1 3
U2 30
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD APR
PY 2013
VL 51
IS 4
SI SI
BP 1870
EP 1882
DI 10.1109/TGRS.2012.2235448
PN 1
PG 13
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 137HN
UT WOS:000318426400002
ER
PT J
AU Zhao, JJ
Wang, YQ
Hashimoto, H
Melton, FS
Hiatt, SH
Zhang, HY
Nemani, RR
AF Zhao, Jianjun
Wang, Yeqiao
Hashimoto, Hirofumi
Melton, Forrest S.
Hiatt, Samuel H.
Zhang, Hongyan
Nemani, Ramakrishna R.
TI The Variation of Land Surface Phenology From 1982 to 2006 Along the
Appalachian Trail
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Appalachian Trail (AT); climatic variation; Global Inventory Modeling
and Mapping Studies (GIMMS); land surface phenology (LSP); Surface
Observation and Gridding System (SOGS)
ID NDVI TIME-SERIES; SATELLITE SENSOR DATA; SPRING PHENOLOGY; PLANT
PHENOLOGY; HIGH-LATITUDES; COVER CHANGE; MODIS; DYNAMICS; SEASONALITY;
FORESTS
AB The gradients of the Appalachian Trail (A.T.) in elevations and latitudes provide a megatransect to study environmental variations in the eastern United States. This paper reveals patterns and trends of land surface phenology (LSP) in association with climatic variables within a corridor area along the A. T. We employed time-series data from Global Inventory Modeling and Mapping Studies and the Surface Observation and Gridding System between 1982 and 2006 to extract spatial and temporal variation patterns of LSP metrics and the correlations with meteorological parameters. The derived trends in LSP metrics indicate that the extended length of season mainly resulted from delayed end of season (EOS) across the study area. More significant change occurred in the northern segment than in the southern segment, which reflects latitudinal effects. We analyzed the relationship between LSP and longitude, latitude, elevation, local climatic variables, and large-scale climate oscillations. Delayed start of season in 1989 and advanced EOS in 1988 were observed responding to the La Nina episode during 1988-1989. This paper provides information about the effects of climate and topography on LSP along the Appalachian Mountain ridges.
C1 [Zhao, Jianjun; Zhang, Hongyan] NE Normal Univ, Sch Urban & Environm Sci, Changchun 130024, Peoples R China.
[Zhao, Jianjun; Wang, Yeqiao] Univ Rhode Isl, Dept Nat Resources Sci, Kingston, RI 02881 USA.
[Hashimoto, Hirofumi; Melton, Forrest S.] Calif State Univ, Div Sci & Environm Policy, Monterey, CA 93955 USA.
[Hashimoto, Hirofumi; Melton, Forrest S.; Hiatt, Samuel H.; Nemani, Ramakrishna R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Zhao, JJ (reprint author), NE Normal Univ, Sch Urban & Environm Sci, Changchun 130024, Peoples R China.
EM zhaojj662@gmail.com; yqwang@mail.uri.edu; hirofumi.hashimoto@gmail.com;
forrest.s.melton@nasa.gov; samhiatt@gmail.com; zhy@nenu.edu.cn;
rama.nemani@nasa.gov
FU NASA Science Mission Directorate (ROSES) [NNX09AV82G]
FX This work was a component of the project titled "A Decision Support
System for Monitoring, Reporting and Forecasting Ecological Conditions
of the Appalachian National Scenic Trail," which was supported by NASA
Science Mission Directorate (ROSES-2008) under Decision Support through
Earth Science Research Results (Grant NNX09AV82G).
NR 53
TC 6
Z9 6
U1 1
U2 25
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD APR
PY 2013
VL 51
IS 4
SI SI
BP 2087
EP 2095
DI 10.1109/TGRS.2012.2217149
PN 1
PG 9
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 137HN
UT WOS:000318426400020
ER
PT J
AU Connor, LN
Farrell, SL
McAdoo, DC
Krabill, WB
Manizade, S
AF Connor, Laurence N.
Farrell, Sinead Louise
McAdoo, David C.
Krabill, William B.
Manizade, Serdar
TI Validating ICESat Over Thick Sea Ice in the Northern Canada Basin
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Altimetry; laser radar; satellite applications; sea ice; snow
ID LASER ALTIMETER MEASUREMENTS; AIRBORNE LASER; RADAR ALTIMETER; SNOW;
FREEBOARD; VARIABILITY; MOTION; OCEAN; COVER; LAND
AB Only in the past eight years has the feasibility of using satellite-borne altimeters to estimate sea ice freeboard and thickness been demonstrated, and these estimates still have uncertainties primarily associated with limited knowledge of snow loading on sea ice. Because accurate estimates of Arctic-wide sea ice thickness and volume are fundamental inputs to global climate models, validation of satellite-derived thickness estimates using independent data is required. A detailed assessment of freeboard retrieved by the Geoscience Laser Altimeter System (GLAS) aboard the Ice, Cloud, and land Elevation Satellite has been carried out using high-resolution laser altimetry from the National Aeronautics and Space Administration's Airborne Topographic Mapper (ATM), the Delay-Doppler radar altimeter, and digital photography collected along a 300-km segment of sea ice in the Canada Basin. Exploiting the repeat coverage of the aircraft flight line, a correction was applied to GLAS footprint geolocations to adjust for sea ice drift that occurred during the time between satellite and aircraft acquisitions. Comparisons of GLAS and ATM measurements over sea ice show excellent agreement (about a 0.00-m mean) with no apparent bias between data sets. Freeboard estimates were examined using data from GLAS and ATM independently, employing measurements over refrozen leads to estimate local sea surface heights (SSHs). The results demonstrate the sensitivity of freeboard and thickness calculations to an accurate estimation of local SSH. Snow depth derived by differencing laser and radar data was combined with the freeboard estimates to yield a mean sea ice thickness of similar to 5.5mover a 250-km subsection of the flight track.
C1 [Connor, Laurence N.; McAdoo, David C.] NOAA, Lab Satellite Altimetry, Natl Environm Satellite Data & Informat Serv, Ctr Satellite Applicat & Res, College Pk, MD 20740 USA.
[Farrell, Sinead Louise] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
[Farrell, Sinead Louise] NOAA, Lab Satellite Altimetry, NESDIS, STAR, College Pk, MD 20740 USA.
[Krabill, William B.] NASA, Sigma Space Inc, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
[Manizade, Serdar] NASA, URS Corp, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
RP Connor, LN (reprint author), NOAA, Lab Satellite Altimetry, Natl Environm Satellite Data & Informat Serv, Ctr Satellite Applicat & Res, College Pk, MD 20740 USA.
EM Laurence.Connor@noaa.gov; Sineadf@umd.edu; Dave.McAdoo@noaa.gov;
William.B.Krabill@nasa.gov; Serdar.Manizade@nasa.gov
RI Farrell, Sinead/F-5586-2010; McAdoo, Dave/F-5612-2010; Connor,
Laurence/E-7930-2011
OI Farrell, Sinead/0000-0003-3222-2751; McAdoo, Dave/0000-0002-7533-5564;
Connor, Laurence/0000-0002-5276-6257
FU National Oceanic and Atmospheric Administration; National Aeronautics
and Space Administration; National Oceanic and Atmospheric
Administration (NOAA)'s Ocean Remote Sensing program; NASA's Cryosphere
Program
FX This work was supported in part by the National Oceanic and Atmospheric
Administration and in part by the National Aeronautics and Space
Administration. The views, opinions, and findings contained in this
report are those of the authors and should not be construed as an
official NOAA or U. S. Government position, policy, or decision.; The
authors would like to thank the National Aeronautics and Space
Administration (NASA) P3 aircrew for their support during the Arctic
Aircraft Altimeter (AAA) 2006 campaign. The March 27, 2006, AAA flight
was supported by the National Oceanic and Atmospheric Administration
(NOAA)'s Ocean Remote Sensing program and NASA's Cryosphere Program. The
authors would also like to thank C. Leuschen for providing the processed
Delay-Doppler data for the AAA flights, the reviewers for their efforts
and insightful suggestions, and NASA's Ice, Cloud, and land Elevation
Satellite (ICESat) Science Project and National Snow and Ice Data Center
for the distribution of the ICESat data (see
http://nsidc.org/data/icesat/). Moderate Resolution Imaging
Spectroradiometer imagery was obtained from NASA's Level 1 and
Atmosphere Archive and Distribution System
(http://ladsweb.nascom.nasa.gov).
NR 46
TC 7
Z9 7
U1 0
U2 15
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 APR
PY 2013
VL 51
IS 4
BP 2188
EP 2200
DI 10.1109/TGRS.2012.2211603
PN 2
PG 13
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 137HY
UT WOS:000318427500004
ER
PT J
AU Tombesi, F
Cappi, M
Reeves, JN
Nemmen, RS
Braito, V
Gaspari, M
Reynolds, CS
AF Tombesi, F.
Cappi, M.
Reeves, J. N.
Nemmen, R. S.
Braito, V.
Gaspari, M.
Reynolds, C. S.
TI Unification of X-ray winds in Seyfert galaxies: from ultra-fast outflows
to warm absorbers
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; black hole physics; galaxies: active;
galaxies: Seyfert; X-rays: galaxies.
ID ACTIVE GALACTIC NUCLEI; XMM-NEWTON OBSERVATION; SUPERMASSIVE
BLACK-HOLES; RADIO-QUIET AGNS; TRANSMISSION GRATING SPECTROMETER;
ACCRETION DISC OUTFLOWS; SHELL ABSORPTION-LINES; DEEP CHANDRA ACIS;
EMISSION-LINE; PHYSICAL CONDITIONS
AB The existence of ionized X-ray absorbing layers of gas along the line of sight to the nuclei of Seyfert galaxies is a well established observational fact. This material is systematically outflowing and shows a large range in parameters. However, its actual nature and dynamics are still not clear. In order to gain insights into these important issues we performed a literature search for papers reporting the parameters of the soft X-ray warm absorbers (WAs) in 35 type 1 Seyferts and compared their properties to those of the ultra-fast outflows (UFOs) detected in the same sample. The fraction of sources with WAs is >60 per cent, consistent with previous studies. The fraction of sources with UFOs is >34 per cent, >67 per cent of which also show WAs. The large dynamic range obtained when considering all the absorbers together, spanning several orders of magnitude in ionization, column, velocity and distance allows us, for the first time, to investigate general relations among them. In particular, we find significant correlations indicating that the closer the absorber is to the central black hole, the higher the ionization, column, outflow velocity and consequently the mechanical power. In all the cases, the absorbers continuously populate the whole parameter space, with the WAs and the UFOs lying always at the two ends of the distribution. These evidence strongly suggest that these absorbers, often considered of different types, could actually represent parts of a single large-scale stratified outflow observed at different locations from the black hole. The UFOs are likely launched from the inner accretion disc and the WAs at larger distances, such as the outer disc and/or torus. We argue that the observed parameters and correlations are, to date, consistent with both radiation pressure through Compton scattering and magnetohydrodynamic processes contributing to the outflow acceleration, the latter playing a major role. Most of the absorbers, especially the UFOs, show a sufficiently high mechanical power (at least similar to 0.5 per cent of the bolometric luminosity) to provide a significant contribution to active galactic nuclei (AGN) feedback and thus to the evolution of the host galaxy. In this regard, we find possible evidence for the interaction of the AGN wind with the surrounding environment on large scales.
C1 [Tombesi, F.; Nemmen, R. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Tombesi, F.; Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Cappi, M.] INAF IASF Bologna, I-40129 Bologna, Italy.
[Reeves, J. N.] Keele Univ, Sch Phys & Geog Sci, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Braito, V.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy.
[Gaspari, M.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
RP Tombesi, F (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM ftombesi@astro.umd.edu
RI Nemmen, Rodrigo/O-6841-2014; Cappi, Massimo/F-4813-2015;
OI Braito, Valentina/0000-0002-2629-4989; Cappi,
Massimo/0000-0001-6966-8920
FU ASI [ASI/INAF/I/009/10/0]; INAF [PRIN-INAF-2011]
FX The authors thank the anonymous referee for the positive and
constructive comments. FT thanks D. Kazanas, K. Fukumura, R. F.
Mushotzky for the useful discussions. MC acknowledges financial support
from ASI (contract ASI/INAF/I/009/10/0) and INAF (contract
PRIN-INAF-2011). RN was supported by an appointment to the NASA
Postdoctoral Program at Goddard Space Flight Center, administered by Oak
Ridge Associated Universities through a contract with NASA. This
research made use of the StatCodes statistical software hosted by Penn
State's Center for Astrostatistics. This research has made use of data
obtained from the High Energy Astrophysics Science Archive Research
Center (HEASARC), provided by NASA's Goddard Space Flight Center. This
research has made use of the NASA/IPAC Extragalactic Database (NED)
which is operated by the Jet Propulsion Laboratory, California Institute
of Technology, under contract with the National Aeronautics and Space
Administration. This research has made use of NASA's Astrophysics Data
System.
NR 128
TC 64
Z9 65
U1 0
U2 1
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR
PY 2013
VL 430
IS 2
BP 1102
EP 1117
DI 10.1093/mnras/sts692
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 135FY
UT WOS:000318275000029
ER
PT J
AU Rostem, K
Chuss, DT
Lourie, NP
Voellmer, GM
Wollack, EJ
AF Rostem, K.
Chuss, D. T.
Lourie, N. P.
Voellmer, G. M.
Wollack, E. J.
TI A waveguide-coupled thermally isolated radiometric source
SO REVIEW OF SCIENTIFIC INSTRUMENTS
LA English
DT Article
ID HEAT; CONDUCTIVITY; NOISE; EPOXY
AB The design and validation of a dual polarization source for waveguide-coupled millimeter and sub-millimeter wave cryogenic sensors is presented. The thermal source is a waveguide mounted absorbing conical dielectric taper. The absorber is thermally isolated with a kinematic suspension that allows the guide to be heat sunk to the lowest bath temperature of the cryogenic system. This approach enables the thermal emission from the metallic waveguide walls to be subdominant to that from the source. The use of low thermal conductivity Kevlar threads for the kinematic mount effectively decouples the absorber from the sensor cold stage. Hence, the absorber can be heated to significantly higher temperatures than the sensor with negligible conductive loading. The kinematic suspension provides high mechanical repeatability and reliability with thermal cycling. A 33-50 GHz blackbody source demonstrates an emissivity of 0.999 over the full waveguide band where the dominant deviation from unity arises from the waveguide ohmic loss. The observed thermal time constant of the source is 40 s when the absorber temperature is 15 K. The specific heat of the lossy dielectric, MF-117, is well approximated by C-v(T) = 0.12 T-2.06 mJ g(-1) K-1 between 3.5 K and 15 K. [http://dx.doi.org/10.1063/1.4795556]
C1 [Rostem, K.; Chuss, D. T.; Lourie, N. P.; Voellmer, G. M.; Wollack, E. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Rostem, K (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
RI Wollack, Edward/D-4467-2012
OI Wollack, Edward/0000-0002-7567-4451
FU NASA ROSES/APRA program
FX We gratefully acknowledge financial support from the NASA ROSES/APRA
program. K. Rostem was supported by an appointment to the NASA
Postdoctoral Program at Goddard Space Flight Center. We thank Paul
Cursey for fabrication and metrology support.
NR 27
TC 2
Z9 2
U1 0
U2 3
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0034-6748
J9 REV SCI INSTRUM
JI Rev. Sci. Instrum.
PD APR
PY 2013
VL 84
IS 4
AR 044701
DI 10.1063/1.4795556
PG 6
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA 134UQ
UT WOS:000318240900041
PM 23635214
ER
PT J
AU Wang, DH
Liu, Y
Zhu, P
Yin, JF
Li, XF
Tao, WK
AF Wang Donghai
Liu Ying
Zhu Ping
Yin Jinfang
Li Xiaofan
Tao Wei-Kuo
TI Cloud microphysical budget associated with torrential rainfall during
the landfall of severe tropical storm Bilis (2006)
SO ACTA METEOROLOGICA SINICA
LA English
DT Article
DE cloud radiation effects; cloud-radiation interaction; ice clouds; cloud
microphysical budget; torrential rainfall
ID MICROSCALE STRUCTURE; STRATIFORM REGIONS; FRONTAL RAINBANDS;
PRECIPITATION; RADIATION; MESOSCALE; RESPONSES; WATER; ORGANIZATION;
CONVECTION
AB Effects of vertical wind shear, radiation, and ice clouds on cloud microphysical budget associated with torrential rainfall during landfall of severe tropical storm Bilis (2006) are investigated by using a series of analysis of two-day grid-scale sensitivity experiment data. When upper-tropospheric upward motions and lower-tropospheric downward motions occur on 15 July 2006, the removal of vertical wind shear and ice clouds increases rainfall contributions from the rainfall type (CM) associated with positive net condensation and hydrometeor loss/convergence, whereas the exclusion of cloud radiative effects and cloud-radiation interaction reduces rainfall contribution from CM. The elimination of vertical wind shear and cloud-radiation interaction increases rainfall contribution from the rainfall type (Cm) associated with positive net condensation and hydrometeor gain/divergence, but the removal of cloud radiative effects and ice clouds decreases rainfall contribution from Cm. The enhancements in rainfall contribution from the rainfall type (cM) associated with negative net condensation and hydrometeor loss/convergence are caused by the exclusion of cloud radiative effects, cloud-radiation interaction and ice clouds, whereas the reduction in rainfall contribution from cM results from the removal of vertical wind shear. When upward motions appear throughout the troposphere on 16 July, the exclusion of all these effects increases rainfall contribution from CM, but generally decreases rainfall contributions from Cm and cM.
C1 [Wang Donghai; Liu Ying; Yin Jinfang] Chinese Acad Meteorol Sci, State Key Lab Severe Weather, Beijing 100081, Peoples R China.
[Wang Donghai] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Zhu Ping] Florida Int Univ, Dept Earth & Environm, Miami, FL 33199 USA.
[Li Xiaofan] NOAA, NESDIS, Ctr Satellite Applicat & Res, Camp Springs, MD 20746 USA.
[Tao Wei-Kuo] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Wang, DH (reprint author), Chinese Acad Meteorol Sci, State Key Lab Severe Weather, Beijing 100081, Peoples R China.
EM d.wang@hotmail.com
RI Li, Xiaofan/F-5605-2010; Li, Xiaofan/G-2094-2014
FU National (Key) Basic Research and Development (973) Program of China
[2012CB417204]; China Meteorological Administration [GYHY200806007,
GYHY201006014, GYHY201206039]; National Natural Science Foundation of
China [40875022, 40633016, 41175064]; State Key Laboratory of Severe
Weather, Chinese Academy of Meteorological Sciences
FX Supported by the National (Key) Basic Research and Development (973)
Program of China (2012CB417204), China Meteorological Administration
Special Public Welfare Research Fund (GYHY200806007, GYHY201006014, and
GYHY201206039), National Natural Science Foundation of China (40875022,
40633016, and 41175064), and Basic Research Project of the State Key
Laboratory of Severe Weather, Chinese Academy of Meteorological
Sciences.
NR 26
TC 0
Z9 0
U1 0
U2 6
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 0894-0525
J9 ACTA METEOROL SIN
JI Acta Meteorol. Sin.
PD APR
PY 2013
VL 27
IS 2
BP 263
EP 272
DI 10.1007/s13351-013-0210-z
PG 10
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 135PW
UT WOS:000318302000010
ER
PT J
AU McKay, CP
Stoker, CR
Glass, BJ
Dave, AI
Davila, AF
Heldmann, JL
Marinova, MM
Fairen, AG
Quinn, RC
Zacny, KA
Paulsen, G
Smith, PH
Parro, V
Andersen, DT
Hecht, MH
Lacelle, D
Pollard, WH
AF McKay, Christopher P.
Stoker, Carol R.
Glass, Brian J.
Dave, Arwen I.
Davila, Alfonso F.
Heldmann, Jennifer L.
Marinova, Margarita M.
Fairen, Alberto G.
Quinn, Richard C.
Zacny, Kris A.
Paulsen, Gale
Smith, Peter H.
Parro, Victor
Andersen, Dale T.
Hecht, Michael H.
Lacelle, Denis
Pollard, Wayne H.
TI The Icebreaker Life Mission to Mars: A Search for Biomolecular Evidence
for Life
SO ASTROBIOLOGY
LA English
DT Article
DE In situ measurement; Life detection; Mars; Planetary protection; Special
region
ID PHOENIX LANDING SITE; MARTIAN SOIL; MERIDIANI-PLANUM; GROUND ICE;
ORGANIC-COMPOUNDS; LIQUID WATER; SURFACE; PERMAFROST; CARBONATE; IRON
AB The search for evidence of life on Mars is the primary motivation for the exploration of that planet. The results from previous missions, and the Phoenix mission in particular, indicate that the ice-cemented ground in the north polar plains is likely to be the most recently habitable place that is currently known on Mars. The near-surface ice likely provided adequate water activity during periods of high obliquity, similar to 5 Myr ago. Carbon dioxide and nitrogen are present in the atmosphere, and nitrates may be present in the soil. Perchlorate in the soil together with iron in basaltic rock provides a possible energy source for life. Furthermore, the presence of organics must once again be considered, as the results of the Viking GCMS are now suspect given the discovery of the thermally reactive perchlorate. Ground ice may provide a way to preserve organic molecules for extended periods of time, especially organic biomarkers. The Mars Icebreaker Life mission focuses on the following science goals: (1) Search for specific biomolecules that would be conclusive evidence of life. (2) Perform a general search for organic molecules in the ground ice. (3) Determine the processes of ground ice formation and the role of liquid water. (4) Understand the mechanical properties of the martian polar ice-cemented soil. (5) Assess the recent habitability of the environment with respect to required elements to support life, energy sources, and possible toxic elements. (6) Compare the elemental composition of the northern plains with midlatitude sites. The Icebreaker Life payload has been designed around the Phoenix spacecraft and is targeted to a site near the Phoenix landing site. However, the Icebreaker payload could be supported on other Mars landing systems. Preliminary studies of the SpaceX Dragon lander show that it could support the Icebreaker payload for a landing either at the Phoenix site or at midlatitudes. Duplicate samples could be cached as a target for possible return by a Mars Sample Return mission. If the samples were shown to contain organic biomarkers, interest in returning them to Earth would be high.
C1 [McKay, Christopher P.; Stoker, Carol R.; Glass, Brian J.; Dave, Arwen I.; Davila, Alfonso F.; Heldmann, Jennifer L.; Marinova, Margarita M.; Fairen, Alberto G.; Quinn, Richard C.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Zacny, Kris A.; Paulsen, Gale] Honeybee Robot, Pasadena, CA USA.
[Smith, Peter H.] Univ Arizona, Tucson, AZ USA.
[Parro, Victor] Ctr Astrobio INTA CSIC, Madrid, Spain.
[Andersen, Dale T.] SETI Inst, Mountain View, CA USA.
[Hecht, Michael H.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Lacelle, Denis] Univ Ottawa, Ottawa, ON, Canada.
[Pollard, Wayne H.] McGill Univ, Montreal, PQ, Canada.
RP McKay, CP (reprint author), NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
EM chris.mckay@nasa.gov
RI sebastianovitsch, stepan/G-8507-2013;
OI Lacelle, Denis/0000-0002-6691-8717
FU NASA ASTEP program; NASA ASTID program
FX This work was supported by the NASA ASTEP and ASTID programs.
NR 122
TC 24
Z9 24
U1 7
U2 106
PU MARY ANN LIEBERT, INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
J9 ASTROBIOLOGY
JI Astrobiology
PD APR
PY 2013
VL 13
IS 4
BP 334
EP 353
DI 10.1089/ast.2012.0878
PG 20
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 130ZX
UT WOS:000317961000003
PM 23560417
ER
PT J
AU Dave, A
Thompson, SJ
McKay, CP
Stoker, CR
Zacny, K
Paulsen, G
Mellerowicz, B
Glass, BJ
Willson, D
Bonaccorsi, R
Rask, J
AF Dave, Arwen
Thompson, Sarah J.
McKay, Christopher P.
Stoker, Carol R.
Zacny, Kris
Paulsen, Gale
Mellerowicz, Bolek
Glass, Brian J.
Willson, David
Bonaccorsi, Rosalba
Rask, Jon
TI The Sample Handling System for the Mars Icebreaker Life Mission: From
Dirt to Data
SO ASTROBIOLOGY
LA English
DT Article
DE Mars; Analogue; Life-detection instruments; Planetary protection;
Spacecraft experiments
ID SITE; ANALOG
AB The Mars Icebreaker Life mission will search for subsurface life on Mars. It consists of three payload elements: a drill to retrieve soil samples from approximately 1 m below the surface, a robotic sample handling system to deliver the sample from the drill to the instruments, and the instruments themselves. This paper will discuss the robotic sample handling system.
Collecting samples from ice-rich soils on Mars in search of life presents two challenges: protection of that icy soil-considered a "special region" with respect to planetary protection-from contamination from Earth, and delivery of the icy, sticky soil to spacecraft instruments. We present a sampling device that meets these challenges. We built a prototype system and tested it at martian pressure, drilling into ice-cemented soil, collecting cuttings, and transferring them to the inlet port of the SOLID2 life-detection instrument. The tests successfully demonstrated that the Icebreaker drill, sample handling system, and life-detection instrument can collectively operate in these conditions and produce science data that can be delivered via telemetry-from dirt to data. Our results also demonstrate the feasibility of using an air gap to prevent forward contamination. We define a set of six analog soils for testing over a range of soil cohesion, from loose sand to basalt soil, with angles of repose of 27 degrees and 39 degrees, respectively. Particle size is a key determinant of jamming of mechanical parts by soil particles. Jamming occurs when the clearance between moving parts is equal in size to the most common particle size or equal to three of these particles together. Three particles acting together tend to form bridges and lead to clogging. Our experiments show that rotary-hammer action of the Icebreaker drill influences the particle size, typically reducing particle size by similar to 100 mu m.
C1 [Dave, Arwen; Thompson, Sarah J.; McKay, Christopher P.; Stoker, Carol R.; Glass, Brian J.; Willson, David; Bonaccorsi, Rosalba] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Dave, Arwen] Lockheed Martin IS&GS, Moffett Field, CA USA.
[Thompson, Sarah J.] Stinger Ghaffarian Technol Inc, Moffett Field, CA USA.
[Zacny, Kris; Paulsen, Gale; Mellerowicz, Bolek] Honeybee Robot, Pasadena, CA USA.
[Willson, David] KISS Inst Pract Robot, Moffett Field, CA USA.
[Bonaccorsi, Rosalba] SETI Inst, Mountain View, CA USA.
[Rask, Jon] NASA, Ames Res Ctr, Space Biosci Div, Dynamac Inc, Mountain View, CA USA.
RP Dave, A (reprint author), NASA, Ames Res Ctr, Planetary Syst Branch, MS N240A-4, Moffett Field, CA 94035 USA.
EM arwen.i.dave@nasa.gov
FU NASA ASTEP program; NASA ASTID program; Lockheed Martin ISGS
FX We'd like to thank the members of the extended team that made this
testing and analysis possible. Thanks to the NASA and Lockheed Martin
staff that supported the ambient testing at Ames Research Center: Roger
Arno for his design work, Emmett Quigley for expert help in fabrication
and modification, Ryan Walker for help with microscopic particle size
analysis, and John Livacich for backhoe and contamination control advice
and help with evaluation criteria. Mike Hecht for providing raw data
from Phoenix soil measurements. This project was supported by the NASA
ASTEP and ASTID programs and Lockheed Martin IS&GS.
NR 27
TC 6
Z9 6
U1 0
U2 16
PU MARY ANN LIEBERT INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
J9 ASTROBIOLOGY
JI Astrobiology
PD APR
PY 2013
VL 13
IS 4
BP 354
EP 369
DI 10.1089/ast.2012.0911
PG 16
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 130ZX
UT WOS:000317961000004
PM 23577818
ER
PT J
AU Kains, N
Street, RA
Choi, JY
Han, C
Udalski, A
Almeida, LA
Jablonski, F
Tristram, PJ
Jorgensen, UG
Szymanski, MK
Kubiak, M
Pietrzynski, G
Soszynski, I
Poleski, R
Kozlowski, S
Pietrukowicz, P
Ulaczyk, K
Wyrzykowski, L
Skowron, J
Alsubai, KA
Bozza, V
Browne, P
Burgdorf, MJ
Novati, SC
Dodds, P
Dominik, M
Dreizler, S
Fang, XS
Grundahl, F
Gu, CH
Hardis, S
Harpsoe, K
Hessman, FV
Hinse, TC
Hornstrup, A
Hundertmark, M
Jessen-Hansen, J
Kerins, E
Liebig, C
Lund, M
Lundkvist, M
Mancini, L
Mathiasen, M
Penny, MT
Rahvar, S
Ricci, D
Sahu, KC
Scarpetta, G
Skottfelt, J
Snodgrass, C
Southworth, J
Surdej, J
Tregloan-Reed, J
Wambsganss, J
Wertz, O
Bajek, D
Bramich, DM
Horne, K
Ipatov, S
Steele, IA
Tsapras, Y
Abe, F
Bennett, DP
Bond, IA
Botzler, CS
Chote, P
Freeman, M
Fukui, A
Furusawa, K
Itow, Y
Ling, CH
Masuda, K
Matsubara, Y
Miyake, N
Muraki, Y
Ohnishi, K
Rattenbury, N
Saito, T
Sullivan, DJ
Sumi, T
Suzuki, D
Suzuki, K
Sweatman, WL
Takino, S
Wada, K
Yock, PCM
Allen, W
Batista, V
Chung, SJ
Christie, G
DePoy, DL
Drummond, J
Gaudi, BS
Gould, A
Henderson, C
Jung, YK
Koo, JR
Lee, CU
McCormick, J
McGregor, D
Munoz, JA
Natusch, T
Ngan, H
Park, H
Pogge, RW
Shin, IG
Yee, J
Albrow, MD
Bachelet, E
Beaulieu, JP
Brillant, S
Caldwell, JAR
Cassan, A
Cole, A
Corrales, E
Coutures, C
Dieters, S
Prester, DD
Donatowicz, J
Fouque, P
Greenhill, J
Kane, SR
Kubas, D
Marquette, JB
Martin, R
Meintjes, P
Menzies, J
Pollard, KR
Williams, A
Wouters, D
Zub, A
AF Kains, N.
Street, R. A.
Choi, J. -Y.
Han, C.
Udalski, A.
Almeida, L. A.
Jablonski, F.
Tristram, P. J.
Jorgensen, U. G.
Szymanski, M. K.
Kubiak, M.
Pietrzynski, G.
Soszynski, I.
Poleski, R.
Kozlowski, S.
Pietrukowicz, P.
Ulaczyk, K.
Wyrzykowski, L.
Skowron, J.
Alsubai, K. A.
Bozza, V.
Browne, P.
Burgdorf, M. J.
Novati, S. Calchi
Dodds, P.
Dominik, M.
Dreizler, S.
Fang, X. -S.
Grundahl, F.
Gu, C-H.
Hardis, S.
Harpsoe, K.
Hessman, F. V.
Hinse, T. C.
Hornstrup, A.
Hundertmark, M.
Jessen-Hansen, J.
Kerins, E.
Liebig, C.
Lund, M.
Lundkvist, M.
Mancini, L.
Mathiasen, M.
Penny, M. T.
Rahvar, S.
Ricci, D.
Sahu, K. C.
Scarpetta, G.
Skottfelt, J.
Snodgrass, C.
Southworth, J.
Surdej, J.
Tregloan-Reed, J.
Wambsganss, J.
Wertz, O.
Bajek, D.
Bramich, D. M.
Horne, K.
Ipatov, S.
Steele, I. A.
Tsapras, Y.
Abe, F.
Bennett, D. P.
Bond, I. A.
Botzler, C. S.
Chote, P.
Freeman, M.
Fukui, A.
Furusawa, K.
Itow, Y.
Ling, C. H.
Masuda, K.
Matsubara, Y.
Miyake, N.
Muraki, Y.
Ohnishi, K.
Rattenbury, N.
Saito, T.
Sullivan, D. J.
Sumi, T.
Suzuki, D.
Suzuki, K.
Sweatman, W. L.
Takino, S.
Wada, K.
Yock, P. C. M.
Allen, W.
Batista, V.
Chung, S. -J.
Christie, G.
DePoy, D. L.
Drummond, J.
Gaudi, B. S.
Gould, A.
Henderson, C.
Jung, Y. -K.
Koo, J. -R.
Lee, C. -U.
McCormick, J.
McGregor, D.
Munoz, J. A.
Natusch, T.
Ngan, H.
Park, H.
Pogge, R. W.
Shin, I. -G.
Yee, J.
Albrow, M. D.
Bachelet, E.
Beaulieu, J. -P.
Brillant, S.
Caldwell, J. A. R.
Cassan, A.
Cole, A.
Corrales, E.
Coutures, Ch.
Dieters, S.
Prester, D. Dominis
Donatowicz, J.
Fouque, P.
Greenhill, J.
Kane, S. R.
Kubas, D.
Marquette, J. -B.
Martin, R.
Meintjes, P.
Menzies, J.
Pollard, K. R.
Williams, A.
Wouters, D.
Zub, Andm.
CA OGLE Collaboration
MiNDSTEp Consortium
RoboNet Collaboration
MOA Collaboration
FUN Collaboration
PLANET Collaboration
TI A giant planet beyond the snow line in microlensing event
OGLE-2011-BLG-0251
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE gravitational lensing: weak; planets and satellites: detection;
planetary systems; Galaxy: bulge
ID BINARY; DWARF; MASS; LENS; STARS; ALGORITHM; DISCOVERY; FREQUENCY;
SYSTEMS; SEARCH
AB Aims. We present the analysis of the gravitational microlensing event OGLE-2011-BLG-0251. This anomalous event was observed by several survey and follow-up collaborations conducting microlensing observations towards the Galactic bulge.
Methods. Based on detailed modelling of the observed light curve, we find that the lens is composed of two masses with a mass ratio q = 1.9 x 10(-3). Thanks to our detection of higher-order effects on the light curve due to the Earth's orbital motion and the finite size of source, we are able to measure the mass and distance to the lens unambiguously.
Results. We find that the lens is made up of a planet of mass 0.53 +/- 0.21 M-J orbiting an M dwarf host star with a mass of 0.26 +/- 0.11 M-circle dot. The planetary system is located at a distance of 2.57 +/- 0.61 kpc towards the Galactic centre. The projected separation of the planet from its host star is d = 1.408 +/- 0.019, in units of the Einstein radius, which corresponds to 2.72 +/- 0.75 AU in physical units. We also identified a competitive model with similar planet and host star masses, but with a smaller orbital radius of 1.50 +/- 0.50 AU. The planet is therefore located beyond the snow line of its host star, which we estimate to be around similar to 1-1.5 AU.
C1 [Kains, N.; Bramich, D. M.] European So Observ, D-85748 Garching, Germany.
[Street, R. A.; Tsapras, Y.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA.
[Choi, J. -Y.; Han, C.; Jung, Y. -K.; Park, H.; Shin, I. -G.] Chungbuk Natl Univ, Inst Astrophys, Dept Phys, Chonju 371763, South Korea.
[Udalski, A.; Szymanski, M. K.; Kubiak, M.; Pietrzynski, G.; Soszynski, I.; Poleski, R.; Kozlowski, S.; Pietrukowicz, P.; Ulaczyk, K.; Wyrzykowski, L.; Skowron, J.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
[Almeida, L. A.; Jablonski, F.] Inst Nacl Pesquisas Espaciais, Div Astrofis, BR-12227010 Sao Jose Dos Campos, SP, Brazil.
[Tristram, P. J.; Chote, P.; Sullivan, D. J.] Victoria Univ, Sch Chem & Phys Sci, Wellington, New Zealand.
[Jorgensen, U. G.; Hardis, S.; Harpsoe, K.; Hinse, T. C.; Mathiasen, M.; Skottfelt, J.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Jorgensen, U. G.; Harpsoe, K.] Geol Museum, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
[Alsubai, K. A.] Qatar Fdn, Doha, Qatar.
[Bozza, V.; Novati, S. Calchi; Scarpetta, G.] Univ Salerno, Dipartimento Fis ER Caianiello, I-84084 Fisciano, Italy.
[Bozza, V.] Ist Nazl Fis Nucl, Sez Napoli, Naples, Italy.
[Browne, P.; Dodds, P.; Dominik, M.; Hundertmark, M.; Liebig, C.; Bajek, D.; Horne, K.] Univ St Andrews, SUPA Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Burgdorf, M. J.] Univ Stuttgart, Deutsch SOFIA Inst, D-70569 Stuttgart, Germany.
[Burgdorf, M. J.] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA.
[Novati, S. Calchi] IIASS, Vietri Sul Mare, SA, Italy.
[Dreizler, S.; Hessman, F. V.; Hundertmark, M.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
[Hinse, T. C.; Chung, S. -J.; Koo, J. -R.; Lee, C. -U.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
[Fang, X. -S.; Gu, C-H.] Chinese Acad Sci, Yunnan Observ, Natl Astron Observ, Joint Lab Opt Astron, Kunming 650011, Peoples R China.
[Grundahl, F.; Jessen-Hansen, J.; Lund, M.; Lundkvist, M.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Hinse, T. C.] Armagh Observ, Armagh BT61 9DG, North Ireland.
Danmarks Tekniske Univ, Inst Rumforskning Og Teknol, DK-2100 Copenhagen, Denmark.
[Hornstrup, A.; Kerins, E.; Penny, M. T.] Univ Manchester, Jodrell Bank Ctr Astrophys, Oxford M13 9PL, England.
[Mancini, L.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Poleski, R.; Skowron, J.; Penny, M. T.; Batista, V.; Gaudi, B. S.; Gould, A.; Henderson, C.; McGregor, D.; Pogge, R. W.; Yee, J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Rahvar, S.] Sharif Univ Technol, Dept Phys, Tehran, Iran.
[Rahvar, S.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada.
[Ricci, D.; Surdej, J.; Wertz, O.] Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[Sahu, K. C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Scarpetta, G.] Ist Nazl Fis Nucl, Grp Collegato Salerno, Sez Napoli, Naples, Italy.
[Brillant, S.; Kubas, D.] ESO, Santiago 19, Chile.
[Snodgrass, C.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Southworth, J.; Tregloan-Reed, J.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Wambsganss, J.; Williams, A.; Zub, Andm.] Univ Heidelberg ZAH, Zentrum Astron, Astron Rechen Inst, D-69120 Heidelberg, Germany.
[Wyrzykowski, L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Ipatov, S.] Alsubais Estab Sci Studies, Doha, Qatar.
[Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Wirral, England.
[Tsapras, Y.] Univ London, Sch Math Sci, London E1 4NS, England.
[Allen, W.] Vintage Lane Observ, Blenheim, New Zealand.
[Christie, G.; Natusch, T.; Ngan, H.] Auckland Observ, Auckland 1023, New Zealand.
[DePoy, D. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
[Drummond, J.] Possum Observ, Patutahi, Gisbourne, New Zealand.
[McCormick, J.] Ctr Backyard Astrophys, Farm Cove Observ, Auckland, New Zealand.
[Natusch, T.] AUT Univ, Inst Radiophys & Space Res, Auckland, New Zealand.
Chungnam Natl Univ, Dept Astron & Space Sci, Oneonta, NY USA.
[Munoz, J. A.] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain.
[Beaulieu, J. -P.; Cassan, A.; Corrales, E.; Coutures, Ch.; Kubas, D.; Marquette, J. -B.; Wouters, D.] UPMC CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France.
[Albrow, M. D.; Pollard, K. R.] Univ Canterbury, Dept Phys & Astron, Christchurch 8020, New Zealand.
[Caldwell, J. A. R.] McDonald Observ, Ft Davis, TX 79734 USA.
[Meintjes, P.] Univ Free State, Fac Nat & Agr Sci, Dept Phys, ZA-9300 Bloemfontein, South Africa.
[Cole, A.; Greenhill, J.] Univ Tasmania, Sch Math & Phys, Gpo Hobart, Tas 7001, Australia.
Lawrence Livermore Natl Lab, IGPP, Livermore, CA 94551 USA.
[Bachelet, E.; Dieters, S.; Fouque, P.] Univ Toulouse, UPS OMP, IRAP, F-31400 Toulouse, France.
[Bachelet, E.; Fouque, P.] CNRS, IRAP, F-31400 Toulouse, France.
[Prester, D. Dominis] Univ Rijeka, Fac Arts & Sci, Dept Phys, Rijeka 51000, Croatia.
[Donatowicz, J.] Vienna Univ Technol, Dept Comp, A-1060 Vienna, Austria.
[Kane, S. R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Martin, R.] Perth Observ, Perth, WA 6076, Australia.
[Menzies, J.] S African Astron Observ, ZA-7935 Observatory, South Africa.
[Abe, F.; Furusawa, K.; Itow, Y.; Masuda, K.; Matsubara, Y.; Miyake, N.; Suzuki, K.; Takino, S.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Bennett, D. P.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
[Bond, I. A.; Ling, C. H.; Sweatman, W. L.] Massey Univ, Inst Informat & Math Sci, North Shore Mail Ctr, Auckland, New Zealand.
[Botzler, C. S.; Freeman, M.; Rattenbury, N.; Yock, P. C. M.] Univ Auckland, Dept Phys, Auckland, New Zealand.
[Fukui, A.] Natl Astron Observ Japan, Okayama Astrophys Observ, Okayama 7190232, Japan.
Mt John Observ, Lake Tekapo 8770, New Zealand.
[Muraki, Y.] Konan Univ, Dept Phys, Kobe, Hyogo 6588501, Japan.
[Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan.
[Saito, T.] Tokyo Metropolitan Coll Ind Technol, Tokyo 1168523, Japan.
[Sumi, T.; Suzuki, D.; Wada, K.] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan.
[Pietrzynski, G.] Univ Concepcion, Dept Astron, Concepcion, Chile.
RP Kains, N (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
EM nkains@eso.org; cheongho@astroph.chungbuk.ac.kr
RI Almeida, L./G-7188-2012; Kozlowski, Szymon/G-4799-2013; Williams,
Andrew/K-2931-2013; Skowron, Jan/M-5186-2014; Hundertmark,
Markus/C-6190-2015; Rahvar, Sohrab/A-9350-2008; Ipatov,
Sergei/O-2302-2014
OI Ricci, Davide/0000-0002-9790-0552; Penny, Matthew/0000-0001-7506-5640;
Snodgrass, Colin/0000-0001-9328-2905; Lund, Mikkel
Norup/0000-0001-9214-5642; Lundkvist, Mia Sloth/0000-0002-8661-2571;
Cole, Andrew/0000-0003-0303-3855; Kozlowski, Szymon/0000-0003-4084-880X;
Williams, Andrew/0000-0001-9080-0105; Skowron, Jan/0000-0002-2335-1730;
Hundertmark, Markus/0000-0003-0961-5231; Rahvar,
Sohrab/0000-0002-7084-5725; Dominik, Martin/0000-0002-3202-0343; Ipatov,
Sergei/0000-0002-1413-9180
FU ESO; European Community [229517, 268421]; European Research Council
under the European Community [246678]; NPRP from the Qatar National
Research Fund (a member of Qatar Foundation) [NPRP-09-476-1-78];
Creative Research Initiative Program of National Research Foundation of
Korea [2009-0081561]; Danish Natural Science Foundation (FNU); German
Research Foundation (DFG); Communaute francaise de Belgique - Actions de
recherche concertees - Academie universitaire Wallonie-Europe; Korea
Research Council for Fundamental Science and Technology (KRCF); KASI
(Korea Astronomy and Space Science Institute) [2012-1-410-02]; National
Science Foundation Graduate Research Fellowship [2009068160]; NSF; NASA
[NNX12AB99G]; JSPS [JSPS23540339, JSPS19340058]; [JSPS22403003];
[JSPS23340064]; [JSPS23340044]
FX N.K. acknowledges an ESO Fellowship. The research leading to these
results has received funding from the European Community's Seventh
Framework Programme (/FP7/2007-2013/) under grant agreements No 229517
and 268421. The OGLE project has received funding from the European
Research Council under the European Community's Seventh Framework
Programme (FP7/2007-2013) / ERC grant agreement No. 246678 to AU. K. A.,
D. B., M. D., K. H., M. H., S. I., C. L., R. S., Y.T. are supported by
NPRP grant NPRP-09-476-1-78 from the Qatar National Research Fund (a
member of Qatar Foundation). Work by C. Han was supported by Creative
Research Initiative Program (2009-0081561) of National Research
Foundation of Korea. This work is based in part on data collected by
MiNDSTEp with the Danish 1.54 m telescope at the ESO La Silla
Observatory. The Danish 1.54 m telescope is operated based on a grant
from the Danish Natural Science Foundation (FNU). The MiNDSTEp
monitoring campaign is powered by ARTEMiS (Automated Terrestrial
Exoplanet Microlensing Search; Dominik et al. 2008). M. H. acknowledges
support by the German Research Foundation (DFG). D. R. (boursier FRIA),
O.W. (aspirant FRS - FNRS) and J. Surdej acknowledge support from the
Communaute francaise de Belgique - Actions de recherche concertees -
Academie universitaire Wallonie-Europe. T. C. H. gratefully acknowledges
financial support from the Korea Research Council for Fundamental
Science and Technology (KRCF) through the Young Research Scientist
Fellowship Program. T. C. H. and C. U. L. acknowledge financial support
from KASI (Korea Astronomy and Space Science Institute) grant number
2012-1-410-02. Work by J. C. Yee is supported by a National Science
Foundation Graduate Research Fellowship under Grant No. 2009068160. A.
Gould and B. S. Gaudi acknowledge support from NSF AST-1103471. B. S.
Gaudi, A. Gould, and R. W. Pogge acknowledge support from NASA grant
NNX12AB99G. The MOA experiment was supported by grants JSPS22403003 and
JSPS23340064. T. S. was supported by the grant JSPS23340044. Y. Muraki
acknowledges support from JSPS grants JSPS23540339 and JSPS19340058.
NR 35
TC 12
Z9 12
U1 0
U2 15
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 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2013
VL 552
AR A70
DI 10.1051/0004-6361/201220626
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 130JW
UT WOS:000317912000070
ER
PT J
AU Kuulkers, E
Kouveliotou, C
Belloni, T
Bel, MC
Chenevez, J
Trigo, MD
Homan, J
Ibarra, A
Kennea, JA
Munoz-Darias, T
Ness, JU
Parmar, AN
Pollock, AMT
van den Heuvel, EPJ
van der Horst, AJ
AF Kuulkers, E.
Kouveliotou, C.
Belloni, T.
Cadolle Bel, M.
Chenevez, J.
Trigo, M. Diaz
Homan, J.
Ibarra, A.
Kennea, J. A.
Munoz-Darias, T.
Ness, J. -U.
Parmar, A. N.
Pollock, A. M. T.
van den Heuvel, E. P. J.
van der Horst, A. J.
TI MAXI J1659-152: the shortest orbital period black-hole transient in
outburst
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE accretion, accretion disks; binaries: close; stars: individual: MAXI
J1659-152; X-rays: binaries
ID X-RAY BINARIES; DRIVEN ECCENTRIC INSTABILITIES; ACCRETING COMPACT
OBJECTS; PHOTON IMAGING CAMERA; BOARD XMM-NEWTON; LOW-MASS; CATACLYSMIC
VARIABLES; SWIFT J1753.5-0127; LIGHT CURVES; CYGNUS X-1
AB MAXI J1659-152 is a bright X-ray transient black-hole candidate binary system discovered in September 2010. We report here on MAXI, RXTE, Swift, and XMM-Newton observations during its 2010/2011 outburst. We find that during the first one and a half week of the outburst the X-ray light curves display drops in intensity at regular intervals, which we interpret as absorption dips. About three weeks into the outbursts, again drops in intensity are seen. These dips have, however, a spectral behaviour opposite to that of the absorption dips, and are related to fast spectral state changes (hence referred to as transition dips). The absorption dips recur with a period of 2.414 +/- 0.005 h, which we interpret as the orbital period of the system. This implies that MAXI J1659-152 is the shortest period black-hole candidate binary known to date. The inclination of the accretion disk with respect to the line of sight is estimated to be 65-80 degrees. We propose the companion to the black-hole candidate to be close to an M5 dwarf star, with a mass and radius of about 0.15-0.25 M-circle dot and 0.2-0.25 R-circle dot, respectively. We derive that the companion had an initial mass of about 1.5 M-circle dot, which evolved to its current mass in about 5-6 billion years. The system is rather compact (orbital separation of greater than or similar to 1.33 R-circle dot), and is located at a distance of 8.6 +/- 3.7 kpc, with a height above the Galactic plane of 2.4 +/- 1.0 kpc. The characteristics of short orbital period and high Galactic scale height are shared with two other transient black-hole candidate X-ray binaries, i.e., XTE J1118+480 and Swift J1735.5-0127. We suggest that all three are kicked out of the Galactic plane into the halo, rather than being formed in a globular cluster.
C1 [Kuulkers, E.; Cadolle Bel, M.; Ibarra, A.; Ness, J. -U.; Parmar, A. N.; Pollock, A. M. T.] European Space Astron Ctr ESA ESAC, Sci Operat Dept, Madrid 28691, Spain.
[Kouveliotou, C.] NASA, Astrophys Off, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Belloni, T.; Munoz-Darias, T.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy.
[Chenevez, J.] Tech Univ Denmark, Natl Space Inst, DK-2800 Lyngby, Denmark.
[Trigo, M. Diaz] ESO, D-85748 Garching, Germany.
[Homan, J.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Kennea, J. A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Munoz-Darias, T.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[van den Heuvel, E. P. J.; van der Horst, A. J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[van der Horst, A. J.] NSSTC, Univ Space Res Assoc, Huntsville, AL 35805 USA.
RP Kuulkers, E (reprint author), European Space Astron Ctr ESA ESAC, Sci Operat Dept, Madrid 28691, Spain.
EM Erik.Kuulkers@esa.int
OI Parmar, Arvind/0000-0002-3307-6517
FU ESA Member States; NASA; European Community's Seventh Framework
Programme [ITN 215212]; EU Marie Curie Intra-European Fellowship
[2011-301355]; ESA-PRODEX [90057]; [I/009/10/0]
FX Partly based on observations obtained with XMM-Newton, an ESA science
mission with instruments and contributions directly funded by ESA Member
States and NASA. This research has made use of data obtained through the
High Energy Astrophysics Science Archive Research Center Online Service,
provided by the NASA/Goddard Space Flight Center. The MAXI/GSC data are
provided by RIKEN, JAXA and the MAXI team, whilst the Swift/BAT
transient monitor results are provided by the Swift/BAT team. We
especially thank the XMM-Newton Science Operations Centre for their
prompt scheduling of the Target of Opportunity observations, 5 h between
trigger and start of observation on September 27! We would also like to
thank the Swift and RXTE teams for their scheduling of the many
monitoring observations. The research leading to these results has
received funding from the European Community's Seventh Framework
Programme (FP7/2007/2013) under grant agreement number ITN 215212 "Black
Hole Universe". TMB acknowledges support to ASI-INAF grant I/009/10/0,
as well as funding via an EU Marie Curie Intra-European Fellowship under
contract no. 2011-301355. EK thanks John Tonry for discussions regarding
the Pan-STARRS 1 optical candidate, Vik Dhillon for supplying the
"PERIOD" analysis package, which we used in our periodicity analysis,
and Kazutaka Yamaoka for providing the estimated 3-200 keV fluxes from
RXTE spectral fits. E.K. and T.M.D. acknowledge Sara Motta for her
comments on the RXTE spectral analysis. E.K. and M.D.T. thank Roberto
Vio for a discussion on the periodograms. J.C. was supported by
ESA-PRODEX contract N: 90057. Last but not least, we thank the referee
for his/her careful reading of the manuscript.
NR 146
TC 25
Z9 25
U1 0
U2 2
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 APR
PY 2013
VL 552
AR A32
DI 10.1051/0004-6361/201219447
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 130JW
UT WOS:000317912000032
ER
PT J
AU Olofsson, J
Benisty, M
Le Bouquin, JB
Berger, JP
Lacour, S
Menard, F
Henning, T
Crida, A
Burtscher, L
Meeus, G
Ratzka, T
Pinte, C
Augereau, JC
Malbet, F
Lazareff, B
Traub, W
AF Olofsson, J.
Benisty, M.
Le Bouquin, J. -B.
Berger, J. -P.
Lacour, S.
Menard, F.
Henning, Th
Crida, A.
Burtscher, L.
Meeus, G.
Ratzka, T.
Pinte, C.
Augereau, J. -C.
Malbet, F.
Lazareff, B.
Traub, W.
TI Sculpting the disk around T Chamaeleontis: an interferometric view
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: individual: T Cha; circumstellar matter; infrared: stars;
techniques: interferometric
ID HERBIG AE/BE STARS; PROTOPLANETARY DISKS; RADIATIVE-TRANSFER;
OPTICAL-PROPERTIES; SCATTERED-LIGHT; YOUNG STARS; HD 142527; TAURI;
MODELS; DUST
AB Context. Circumstellar disks are believed to be the birthplace of planets and are expected to dissipate on a timescale of a few Myr. The processes responsible for the removal of the dust and gas will strongly modify the radial distribution of the circumstellar matter and consequently the spectral energy distribution. In particular, a young planet will open a gap, resulting in an inner disk dominating the near-IR emission and an outer disk emitting mostly in the far-infrared.
Aims. We analyze a full set of data involving new near-infrared data obtained with the 4-telescope combiner (VLTI/PIONIER), new mid-infrared interferometric VLTI/MIDI data, literature photometric and archival data from VLT/NaCo/SAM to constrain the structure of the transition disk around T Cha.
Methods. After a preliminary analysis with a simple geometric model, we used the MCFOST radiative transfer code to simultaneously model the SED and the interferometric observables from raytraced images in the H-, L'-, and N-bands.
Results. We find that the dust responsible for the strong emission in excess in the near-IR must have a narrow temperature distribution with a maximum close to the silicate sublimation temperature. This translates into a narrow inner dusty disk (0.07-0.11 AU), with a significant height (H/r similar to 0.2) to increase the geometric surface illuminated by the central star. We find that the outer disk starts at about 12 AU and is partially resolved by the PIONIER, SAM, and MIDI instruments. We discuss the possibility of a self-shadowed inner disk, which can extend to distances of several AU. Finally, we show that the SAM closure phases, interpreted as the signature of a candidate companion, may actually trace the asymmetry generated by forward scattering by dust grains in the upper layers of the outer disk. These observations help constrain the inclination and position angle of the disk to about +58 degrees and -70 degrees, respectively.
Conclusions. The circumstellar environment of T Cha appears to be best described by two disks spatially separated by a large gap. The presence of matter (dust or gas) inside the gap is, however, difficult to assess with present-day observations. Our model suggests the outer disk contaminates the interferometric signature of any potential companion that could be responsible for the gap opening, and such a companion still has to be unambiguously detected. We stress the difficulty to observe point sources in bright massive disks, and the consequent need to account for disk asymmetries (e.g. anisotropic scattering) in model-dependent search for companions.
C1 [Olofsson, J.; Henning, Th] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Benisty, M.; Le Bouquin, J. -B.; Menard, F.; Pinte, C.; Augereau, J. -C.; Malbet, F.; Lazareff, B.] UJF Grenoble 1 CNRS INSU, Inst Planetol & Astrophys Grenoble IPAG UMR 5274, Grenoble, France.
[Berger, J. -P.] European So Observ, Alonso De Cordova 3107, Vitacura, Chile.
[Lacour, S.] Univ Paris Diderot, Univ Paris 06, CNRS, LESIA Observ Paris, F-92195 Meudon, France.
[Menard, F.] Univ Chile, CNRS INSU France UMI 3386, UMI FCA, Santiago, Chile.
[Menard, F.] Univ Chile, Dept Astron, Santiago, Chile.
[Crida, A.] Univ Nice Sophia Antipolis CNRS Observ Cote dAzur, Lab Lagrange UMR 7293, F-06304 Nice 04, France.
[Burtscher, L.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
[Meeus, G.] Univ Autonoma Madrid, Dpt Fis Teor, E-28049 Madrid, Spain.
[Ratzka, T.] Univ Munich, Univ Sternwarte Munchen, D-81679 Munich, Germany.
[Traub, W.] Jet Prop Lab NASA JPL, Pasadena, CA 91109 USA.
RP Olofsson, J (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
EM olofsson@mpia.de
OI Ratzka, Thorsten/0000-0001-9557-8232
FU European Commission [PERG06-GA-2009-256513]; Agence Nationale pour la
Recherche (ANR) of France [ANR-2010-JCJC-0504-01]; [089.C-0537(A)]
FX The authors are grateful to the anonymous referee for useful advices and
comments that improved the readability of the paper. The authors thank
Bertram Bitsch for valuable discussions. C.P. acknowledges funding from
the European Commission's 7th Framework Program (contract
PERG06-GA-2009-256513) and from Agence Nationale pour la Recherche (ANR)
of France under contract ANR-2010-JCJC-0504-01. CNRS is acknowledged for
having supported this work in the form of Guaranteed Time Observations
(program 089.C-0537(A)).
NR 49
TC 29
Z9 29
U1 0
U2 2
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 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2013
VL 552
AR A4
DI 10.1051/0004-6361/201220675
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 130JW
UT WOS:000317912000004
ER
PT J
AU Sanchez-Monge, A
Cesaroni, R
Beltran, MT
Kumar, MSN
Stanke, T
Zinnecker, H
Etoka, S
Galli, D
Hummel, CA
Moscadelli, L
Preibisch, T
Ratzka, T
van der Tak, FFS
Vig, S
Walmsley, CM
Wang, KS
AF Sanchez-Monge, A.
Cesaroni, R.
Beltran, M. T.
Kumar, M. S. N.
Stanke, T.
Zinnecker, H.
Etoka, S.
Galli, D.
Hummel, C. A.
Moscadelli, L.
Preibisch, T.
Ratzka, T.
van der Tak, F. F. S.
Vig, S.
Walmsley, C. M.
Wang, K. -S.
TI A candidate circumbinary Keplerian disk in G35.20-0.74N: A study with
ALMA
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: formation; ISM: individual objects: G35.20-0.74N; ISM: jets and
outflows
ID YOUNG STELLAR OBJECTS; MOLECULAR OUTFLOWS; IRAS 20126+4104;
STAR-FORMATION; ACCRETION; REGIONS; JET; G35.2-0.74N; AFGL-5142; CLUSTER
AB We report on ALMA observations of continuum and molecular line emission with 0 ''.4 resolution towards the high-mass star-forming region G35.20-0.74 N. Two dense cores are detected in typical hot-core tracers (e. g., CH3CN) that reveal velocity gradients. In one of these cores, the velocity field can be fitted with an almost edge-on Keplerian disk rotating about a central mass of similar to 18 M-circle dot. This finding is consistent with the results of a recent study of the CO first overtone bandhead emission at 2.3 mu m towards G35.20-0.74 N. The disk radius and mass are greater than or similar to 2500 au and similar to 3 M-circle dot. To reconcile the observed bolometric luminosity (similar to 3x10(4) L-circle dot) with the estimated stellar mass of 18 M-circle dot, we propose that the latter is the total mass of a binary system.
C1 [Sanchez-Monge, A.; Cesaroni, R.; Beltran, M. T.; Galli, D.; Moscadelli, L.; Walmsley, C. M.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy.
[Kumar, M. S. N.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Stanke, T.; Hummel, C. A.] ESO, D-85748 Garching, Germany.
[Zinnecker, H.] NASA Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA.
[Etoka, S.] Univ Manchester, Sch Phys & Astron, Ctr Astrophys, Jodrell Bank, Manchester M13 9PL, Lancs, England.
[Etoka, S.] Hamburger Sternwarte, D-21029 Hamburg, Germany.
[Preibisch, T.; Ratzka, T.] Univ Munich, Univ Sternwarte Munchen, D-81679 Munich, Germany.
[van der Tak, F. F. S.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands.
[van der Tak, F. F. S.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands.
[Vig, S.] Indian Inst Space Sci & Technol, Dept Earth & Space Sci, Thiruvananthapuram 695547, Kerala, India.
[Walmsley, C. M.] Dublin Inst Adv Studies DIAS, Dublin 2, Ireland.
[Wang, K. -S.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Sanchez-Monge, A (reprint author), Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy.
EM asanchez@arcetri.astro.it
RI Kumar, Nanda/I-4183-2013;
OI Moscadelli, Luca/0000-0002-8517-8881; Galli,
Daniele/0000-0001-7706-6049; Beltran Sorolla, Maria
Teresa/0000-0003-3315-5626; Ratzka, Thorsten/0000-0001-9557-8232;
Cesaroni, Riccardo/0000-0002-2430-5103
FU European ALMA Regional Center; Italian ARC node; NASA; FCT (Portugal);
POPH/FSE (EC)
FX It is a pleasure to thank Goran Sandell for stimulating discussions of
the G35.20-0.74 N region and the anonymous referee for constructive
criticisms. We also acknowledge the support of the European ALMA
Regional Center and the Italian ARC node. This paper makes use of the
following ALMA data: ADS/JAO. ALMA#2011.0.00275. 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. This work also used observations
made with the Spitzer Space Telescope, which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with NASA. MSNK is supported by a Ciencia 2007 contract, funded
by FCT (Portugal) and POPH/FSE (EC).
NR 32
TC 31
Z9 31
U1 1
U2 2
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 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2013
VL 552
AR L10
DI 10.1051/0004-6361/201321134
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 130JW
UT WOS:000317912000154
ER
PT J
AU Zwintz, K
Fossati, L
Guenther, DB
Ryabchikova, T
Baglin, A
Themessl, N
Barnes, TG
Matthews, JM
Auvergne, M
Bohlender, D
Chaintreuil, S
Kuschnig, R
Moffat, AFJ
Rowe, JF
Rucinski, SM
Sasselov, D
Weiss, WW
AF Zwintz, K.
Fossati, L.
Guenther, D. B.
Ryabchikova, T.
Baglin, A.
Themessl, N.
Barnes, T. G.
Matthews, J. M.
Auvergne, M.
Bohlender, D.
Chaintreuil, S.
Kuschnig, R.
Moffat, A. F. J.
Rowe, J. F.
Rucinski, S. M.
Sasselov, D.
Weiss, W. W.
TI Regular frequency patterns in the young delta Scuti star HD 261711
observed by the CoRoT and MOST satellites
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: variables: delta Scuti; stars: oscillations; stars: individual:
HD261711; techniques: photometric; techniques: spectroscopic
ID PRE-MAIN-SEQUENCE; CLUSTER NGC 2264; LINE-DATA-BASE; DIFFERENTIAL
ROTATION; MODEL ATMOSPHERES; STELLAR EVOLUTION; PRAESEPE CLUSTER;
F-STARS; PHOTOMETRY; SPACE
AB Context. The internal structure of pre-main-sequence (PMS) stars is poorly constrained at present. This could change significantly through high-quality asteroseismological observations of a sample of such stars.
Aims. We concentrate on an asteroseismological study of HD261711, a rather hot delta Scuti-type pulsating member of the young open cluster NGC 2264 located at the blue border of the instability region. HD261711 was discovered to be a PMS delta Scuti star using the time series photometry obtained by the MOST satellite in 2006.
Methods. High-precision, time-series photometry of HD261711 was obtained by the MOST and CoRoT satellites in four separate new observing runs that are put into context with the star's fundamental atmospheric parameters obtained from spectroscopy. Frequency Analysis was performed using Period04. The spectral analysis was performed using equivalent widths and spectral synthesis.
Results. With the new MOST data set from 2011/12 and the two CoRoT light curves from 2008 and 2011/12, the delta Scuti variability was confirmed and regular groups of frequencies were discovered. The two pulsation frequencies identified in the data from the first MOST observing run in 2006 are confirmed and 23 new delta Scuti-type frequencies were discovered using the CoRoT data. Weighted average frequencies for each group were determined and are related to l = 0 and l = 1 p-modes. Evidence for amplitude modulation of the frequencies in two groups is seen. The effective temperature (T-eff) was derived to be 8600 +/- 200K, log g is 4.1 +/- 0.2, and the projected rotational velocity (upsilon sin i) is 53 +/- 1 km s(-1). Using our T-eff value and the radius of 1.8 +/- 0.5 R-circle dot derived from spectral energy distribution (SED) fitting, we get a luminosity log L/L-circle dot of 1.20 +/- 0.14 which agrees well to the seismologically determined values of 1.65 R-circle dot and, hence, a log L/L-circle dot of 1.13. The radial velocity of 14 +/- 2 km s(-1) we derived for HD261711, confirms the star's membership to NGC 2264.
Conclusions. Our asteroseismic models suggest that HD261711 is a delta Scuti-type star close to the zero-age main sequence (ZAMS) with a mass of 1.8 to 1.9 M-circle dot. With an age of about 10 million years derived from asteroseismology, the star is either a young ZAMS star or a late PMS star just before the onset of hydrogen-core burning. The observed splittings about the l = 0 and 1 parent modes may be an artifact of the Fourier derived spectrum of frequencies with varying amplitudes.
C1 [Zwintz, K.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Zwintz, K.; Themessl, N.; Kuschnig, R.; Weiss, W. W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Fossati, L.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Guenther, D. B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada.
[Ryabchikova, T.] Russian Acad Sci, Inst Astron, Moscow 119017, Russia.
[Baglin, A.; Auvergne, M.; Chaintreuil, S.] Observ Paris, LESIA, F-92195 Meudon, France.
[Barnes, T. G.] Univ Texas Austin, McDonald Observ, Austin, TX 79734 USA.
[Matthews, J. M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Bohlender, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada.
[Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Rowe, J. F.] NASA Ames Res Pk, Moffett Field, CA 94035 USA.
[Rucinski, S. M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Zwintz, K (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Louvain, Belgium.
EM konstanze.zwintz@ster.kuleuven.be
OI Zwintz, Konstanze/0000-0001-9229-8315
FU Research Foundation - Flanders (FWO); Austrian Fonds zur Forderung der
wissenschaftlichen Forschung [P 21830-N16, P22691-N16]; Russian Academy
of Sciences "Non-stationary phenomena in the Universe"; Natural Sciences
and Engineering Research Council (NSERC) of Canada; Austrian Research
Promotion Agency-ALR
FX K.Z. receives a Pegasus Marie Curie Fellowship of the Research
Foundation - Flanders (FWO). This investigation has been supported by
the Austrian Fonds zur Forderung der wissenschaftlichen Forschung
through project P 21830-N16 (PI: M. Breger). T.R. acknowledges partial
financial support from Basic Research Program of the Russian Academy of
Sciences "Non-stationary phenomena in the Universe". D.B.G., J.M.,
A.F.J.M. and S.M.R. acknowledge the funding support of the Natural
Sciences and Engineering Research Council (NSERC) of Canada. R.K. and
W.W.W. are supported by the Austrian Fonds zur Forderung der
wissenschaftlichen Forschung (P22691-N16) and by the Austrian Research
Promotion Agency-ALR. Spectroscopic data were obtained with the 2.7-m
telescope at Mc Donald Observatory, Texas, US and at the Dominion
Astrophysical Observatory, Herzberg Institute of Astrophysics, National
Research Council of Canada.
NR 71
TC 5
Z9 5
U1 0
U2 2
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 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2013
VL 552
AR A68
DI 10.1051/0004-6361/201220934
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 130JW
UT WOS:000317912000068
ER
PT J
AU Lucas, N
Doty, M
Taubert, L
Wygnanski, I
AF Lucas, Nathaniel
Doty, Michael
Taubert, Lutz
Wygnanski, Israel
TI Reducing the noise emanating from a twin jet nozzle using flexible
filaments
SO EXPERIMENTS IN FLUIDS
LA English
DT Article
AB A twin jet was tested in anechoic facilities at the University of Arizona and NASA Langley Research Center to determine the effectiveness of flexible filaments in jet noise reduction. Results were strongly dependent on filament diameter and material, the most effective of which was found to be Tex 800 Kevlar. In the best configurations, the filaments consistently eliminated screech tones and reduced overall sound pressure level by 3 dB or more. Additionally, broadband shock noise was diminished by more than 5 dB over certain audible frequency ranges. Larger-scale tests run at NASA showed comparable reductions in overall sound pressure level and broadband shock-associated noise.
C1 [Lucas, Nathaniel; Taubert, Lutz; Wygnanski, Israel] Univ Arizona, Dept Aerosp & Mech Engn, Tucson, AZ 85721 USA.
[Doty, Michael; Wygnanski, Israel] NASA, Aeroacoust Branch, Langley Res Ctr, Hampton, VA 23681 USA.
RP Lucas, N (reprint author), Univ Arizona, Dept Aerosp & Mech Engn, 1130 N Mt Ave, Tucson, AZ 85721 USA.
EM nlucas333@gmail.com
FU NASA Langley Research Directorate Office; Fundamental Aeronautics
Program Supersonics Project
FX We would like to acknowledge the assistance of Dr. Jesse Little, who was
very helpful in making sure the results and background information were
framed in the proper context with respect to other aeroacoustics
research that has been done in the past, and Philipp Tewes, who
contributed to the data processing effort. Many thanks to Harry Haskin,
John Swartzbaugh, and the rest of the NASA JNL crew for the exciting
opportunity to collaborate our research. Funding for the NASA tests from
the NASA Langley Research Directorate Office and the Fundamental
Aeronautics Program Supersonics Project is gratefully acknowledged.
NR 17
TC 0
Z9 0
U1 2
U2 9
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0723-4864
J9 EXP FLUIDS
JI Exp. Fluids
PD APR
PY 2013
VL 54
IS 4
AR 1504
DI 10.1007/s00348-013-1504-8
PG 10
WC Engineering, Mechanical; Mechanics
SC Engineering; Mechanics
GA 133RX
UT WOS:000318158500014
ER
PT J
AU Saxena, R
Fingland, N
Patil, D
Sharma, AK
Crooke, E
AF Saxena, Rahul
Fingland, Nicholas
Patil, Digvijay
Sharma, Anjali K.
Crooke, Elliott
TI Crosstalk between DnaA Protein, the Initiator of Escherichia coli
Chromosomal Replication, and Acidic Phospholipids Present in Bacterial
Membranes
SO INTERNATIONAL JOURNAL OF MOLECULAR SCIENCES
LA English
DT Review
DE acidic phospholipids; DnaA protein; chromosomal replication; Escherichia
coli
ID OSMOSENSORY TRANSPORTER PROP; DIVISION-SITE SELECTION; UNSATURATED
FATTY-ACIDS; AAA PLUS PROTEIN; CARDIOLIPIN SYNTHESIS; FUNCTIONAL
INTERACTION; AMINO-ACIDS; CELL-CYCLE; IN-VITRO; REGULATORY INACTIVATION
AB Anionic (i.e., acidic) phospholipids such as phosphotidylglycerol (PG) and cardiolipin (CL), participate in several cellular functions. Here we review intriguing in vitro and in vivo evidence that suggest emergent roles for acidic phospholipids in regulating DnaA protein-mediated initiation of Escherichia coli chromosomal replication. In vitro acidic phospholipids in a fluid bilayer promote the conversion of inactive ADP-DnaA to replicatively proficient ATP-DnaA, yet both PG and CL also can inhibit the DNA-binding activity of DnaA protein. We discuss how cellular acidic phospholipids may positively and negatively influence the initiation activity of DnaA protein to help assure chromosomal replication occurs once, but only once, per cell-cycle. Fluorescence microscopy has revealed that PG and CL exist in domains located at the cell poles and mid-cell, and several studies link membrane curvature with sub-cellular localization of various integral and peripheral membrane proteins. E. coli DnaA itself is found at the cell membrane and forms helical structures along the longitudinal axis of the cell. We propose that there is cross-talk between acidic phospholipids in the bacterial membrane and DnaA protein as a means to help control the spatial and temporal regulation of chromosomal replication in bacteria.
C1 [Saxena, Rahul; Patil, Digvijay; Sharma, Anjali K.; Crooke, Elliott] Georgetown Univ, Med Ctr, Dept Biochem & Mol & Cellular Biol, Washington, DC 20007 USA.
[Fingland, Nicholas] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Crooke, Elliott] Georgetown Univ, Med Ctr, Lombardi Comprehens Canc Ctr, Washington, DC 20007 USA.
RP Saxena, R (reprint author), Georgetown Univ, Med Ctr, Dept Biochem & Mol & Cellular Biol, Washington, DC 20007 USA.
EM rs426@georgetown.edu; nick.k.fingland@jpl.nasa.gov;
dap89@georgetown.edu; anjali0623@gmail.com; crooke@georgetown.edu
FU Georgetown University Medical Center Office
FX This work was supported in part by the Georgetown University Medical
Center Office for the Dean for Research.
NR 125
TC 14
Z9 14
U1 2
U2 25
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 1422-0067
J9 INT J MOL SCI
JI Int. J. Mol. Sci.
PD APR
PY 2013
VL 14
IS 4
BP 8517
EP 8537
DI 10.3390/ijms14048517
PG 21
WC Biochemistry & Molecular Biology; Chemistry, Multidisciplinary
SC Biochemistry & Molecular Biology; Chemistry
GA 131SU
UT WOS:000318017100108
PM 23595001
ER
PT J
AU Korolev, A
Emery, E
Creelman, K
AF Korolev, Alexei
Emery, Edward
Creelman, Kirk
TI Modification and Tests of Particle Probe Tips to Mitigate Effects of Ice
Shattering
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID OPTICAL ARRAY PROBES; CRYSTALS; BREAKUP; FSSP; SIZE
AB Ice particle shattering may significantly contaminate measurements taken by airborne particle probes in ice clouds. Environment Canada and the NASA Glenn Research Center (GRC) undertook efforts to modify and test probe tips in order to mitigate the effect of shattering on measurements. This work presents an overview of the results obtained during the design work on the particle probe arm tips. Even though this work was focused on the modifications of three of the probes-Particle Measuring Systems Inc. (PMS) Forward Scattering Spectrometer Probe and optical array probe, and Droplet Measurement Technologies (DMT) Cloud Imaging Probe-the outcomes of this work bear a general character and are applicable to other similar instruments. The results of the airflow analysis around the probe's housing and the simulations of particle bouncing from the probe tips are discussed here. The originally designed and modified tips were tested in a high-speed wind tunnel in ice and liquid sprays. The ice particle bouncing processes as well as patterns of water shedding over the surface of the probes arms were studied with the help of a high-speed video camera. It was found that at aircraft speed, after bouncing from a solid surface, ice particles may travel several centimeters across the airflow and bounce forward up to 1 cm. For the first time it has been directly documented with high-speed video recording that the sample volumes of particle probes with the originally designed tips are contaminated by shattered and bounced particles. A set of recommendations on the existing modification and the design of future particle probe housings is presented.
C1 [Korolev, Alexei] Environm Canada, Cloud Phys & Severe Weather Res Sect, Toronto, ON M3H 5T4, Canada.
[Emery, Edward] NASA Glenn Res Ctr, Cleveland, OH USA.
[Creelman, Kirk] Auriga Design Inc, Haliburton, ON, Canada.
RP Korolev, A (reprint author), Environm Canada, 4905 Dufferin St, Toronto, ON M3H 5T4, Canada.
EM alexei.korolev@ec.gc.ca
FU Environment Canada; Federal Aviation Administration; NASA; Transport
Canada
FX This work was funded by Environment Canada, Transport Canada, the
Federal Aviation Administration, and NASA. The authors express their
gratitude to Cox and Company personnel and, in particular, to Adam
Lawrence for such a high level of cooperation and support in operating
the Cox and Company wind tunnel facility. The NASA Glenn Research Center
video group Vince Reich, Chris Lynch, and Quentin Schwinn did an
excellent job capturing highspeed videos during the Cox and Company wind
tunnel tests. It is hard to overestimate the role of Vladimir Torgashev,
who did mechanical drawing and supervised manufacturing of the probe
tips. Special thanks to Alex Shahshkov of Environment Canada for his
help in data analysis. The authors thank Alain Protat and two anonymous
reviewers for their thoughtful comments.
NR 20
TC 31
Z9 31
U1 2
U2 9
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD APR
PY 2013
VL 30
IS 4
BP 690
EP 708
DI 10.1175/JTECH-D-12-00142.1
PG 19
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 130YF
UT WOS:000317955700004
ER
PT J
AU Chepfer, H
Cesana, G
Winker, D
Getzewich, B
Vaughan, M
Liu, Z
AF Chepfer, H.
Cesana, G.
Winker, D.
Getzewich, B.
Vaughan, M.
Liu, Z.
TI Comparison of Two Different Cloud Climatologies Derived from
CALIOP-Attenuated Backscattered Measurements (Level 1): The CALIPSO-ST
and the CALIPSO-GOCCP
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID TROPICAL TROPOPAUSE; LIDAR; ISCCP; PERFORMANCE; VALIDATION; AEROSOLS;
MISSION; CIRRUS; ECMWF; TERRA
AB Two different cloud climatologies have been derived from the same NASA-Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP)-measured attenuated backscattered profile (level 1, version 3 dataset). The first climatology, named Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations-Science Team (CALIPSO-ST), is based on the standard CALIOP cloud mask (level 2 product, version 3), with the aim to document clouds with the highest possible spatiotemporal resolution, taking full advantage of the CALIOP capabilities and sensitivity for a wide range of cloud scientific studies. The second climatology, named GCM-Oriented CALIPSO Cloud Product (CALIPSO-GOCCP), is aimed at a single goal: evaluating GCM prediction of cloudiness. For this specific purpose, it has been designed to be fully consistent with the CALIPSO simulator included in the Cloud Feedback Model Intercomparison Project (CFMIP) Observation Simulator Package (COSP) used within version 2 of the CFMIP (CFMIP-2) experiment and phase 5 of the Coupled Model Intercomparison Project (CMIP5).
The differences between the two datasets in the global cloud cover maps-total, low level (P > 680 hPa), midlevel (680 < P < 440 hPa), and high level (P < 440 hPa)-are frequently larger than 10% and vary with region.
The two climatologies show significant differences in the zonal cloud fraction profile (which differ by a factor of almost 2 in some regions), which are due to the differences in the horizontal and vertical averaging of the measured attenuated backscattered profile CALIOP profile before the cloud detection and to the threshold used to detect clouds (this threshold depends on the resolution and the signal-to-noise ratio).
C1 [Chepfer, H.] Univ Paris 06, LMD, IPSL, Paris, France.
[Cesana, G.] Ecole Polytech, LMD, IPSL, Palaiseau, France.
[Winker, D.; Vaughan, M.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Getzewich, B.; Liu, Z.] SSAI, Hampton, VA USA.
RP Chepfer, H (reprint author), UPMC, Ecole Polytech, LMD, IPSL, F-91128 Palaiseau, France.
EM helene.chepfer@lmd.polytechnique.fr
RI Liu, Zhaoyan/B-1783-2010
OI Liu, Zhaoyan/0000-0003-4996-5738
NR 40
TC 15
Z9 15
U1 1
U2 22
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
EI 1520-0426
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD APR
PY 2013
VL 30
IS 4
BP 725
EP 744
DI 10.1175/JTECH-D-12-00057.1
PG 20
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 130YF
UT WOS:000317955700006
ER
PT J
AU Koskulics, J
Englehardt, S
Long, S
Hu, YX
Ottaviani, M
Stamnes, K
AF Koskulics, Jeffrey
Englehardt, Steven
Long, Steven
Hu, Yongxiang
Ottaviani, Matteo
Stamnes, Knut
TI Water Surface Topography Retrieved from Color Images
SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY
LA English
DT Article
ID ATMOSPHERE-OCEAN SYSTEM; WIND-WAVES; MULTIANGLE; RADIANCES; SLOPES
AB Submerged objects viewed through wavy water surfaces appear distorted by refraction. An imaging system exploiting this effect is implemented using a submerged planar light source designed so that color images reveal features of small-amplitude waves in a wind-wave tank. The system is described by a nonlinear model of image formation based on the geometry of refraction, spectral emission from the light source, radiative transfer through the water and surface, and camera spectral response. Surface normal vector components are retrieved from the color image data using an iterative solution to the nonlinear model. The surface topography is then retrieved using a linear model that combines surface normal data with a priori constraints on elevation and curvature. The high-resolution topographic data reveal small-amplitude waves spanning wavelength scales from capillary through short gravity wave regimes. The system capabilities are demonstrated in the retrieval of test surfaces, and of a case of wind-driven waves, using data collected at high spatial and temporal resolution in a wave tank. The approach of using a physical model of image formation with inverse solution methods provides an example of how surface topography can be retrieved and may be applicable to data from other similar instruments.
C1 [Koskulics, Jeffrey; Englehardt, Steven; Stamnes, Knut] Stevens Inst Technol, Hoboken, NJ 07030 USA.
[Long, Steven] NASA, Goddard Space Flight Ctr, Air Sea Interact Res Facil, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
[Hu, Yongxiang] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Ottaviani, Matteo] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Koskulics, J (reprint author), Stevens Inst Technol, Light & Life Lab, 1 Castle Point Hudson, Hoboken, NJ 07030 USA.
EM jkoskuli@stevens.edu
RI Hu, Yongxiang/K-4426-2012
FU NASA Radiation Sciences Program
FX The authors acknowledge support from the NASA Radiation Sciences Program
and wish to thank the program manager, Dr. Hal Maring. SRL would like to
express his thanks to Dr. Eric Lindstrom of the NASA Science Mission
Directorate for supporting the research efforts of NASIRF during its
final years of operation.
NR 29
TC 0
Z9 0
U1 0
U2 6
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0739-0572
EI 1520-0426
J9 J ATMOS OCEAN TECH
JI J. Atmos. Ocean. Technol.
PD APR
PY 2013
VL 30
IS 4
BP 846
EP 860
DI 10.1175/JTECH-D-12-00047.1
PG 15
WC Engineering, Ocean; Meteorology & Atmospheric Sciences
SC Engineering; Meteorology & Atmospheric Sciences
GA 130YF
UT WOS:000317955700012
ER
PT J
AU Reynolds, RW
Chelton, DB
Roberts-Jones, J
Martin, MJ
Menemenlis, D
Merchant, CJ
AF Reynolds, Richard W.
Chelton, Dudley B.
Roberts-Jones, Jonah
Martin, Matthew J.
Menemenlis, Dimitris
Merchant, Christopher John
TI Objective Determination of Feature Resolution in Two Sea Surface
Temperature Analyses
SO JOURNAL OF CLIMATE
LA English
DT Article
ID OCEAN; MODEL; CLIMATE
AB Considerable effort is presently being devoted to producing high-resolution sea surface temperature (SST) analyses with a goal of spatial grid resolutions as low as 1 km. Because grid resolution is not the same as feature resolution, a method is needed to objectively determine the resolution capability and accuracy of SST analysis products. Ocean model SST fields are used in this study as simulated "true'' SST data and subsampled based on actual infrared and microwave satellite data coverage. The subsampled data are used to simulate sampling errors due to missing data. Two different SST analyses are considered and run using both the full and the subsampled model SST fields, with and without additional noise. The results are compared as a function of spatial scales of variability using wavenumber auto-and cross-spectral analysis.
The spectral variance at high wavenumbers (smallest wavelengths) is shown to be attenuated relative to the true SST because of smoothing that is inherent to both analysis procedures. Comparisons of the two analyses (both having grid sizes of roughly 1/20 degrees) show important differences. One analysis tends to reproduce small-scale features more accurately when the high-resolution data coverage is good but produces more spurious small-scale noise when the high-resolution data coverage is poor. Analysis procedures can thus generate small-scale features with and without data, but the small-scale features in an SST analysis may be just noise when high-resolution data are sparse. Users must therefore be skeptical of high-resolution SST products, especially in regions where high-resolution ( similar to 5 km) infrared satellite data are limited because of cloud cover.
C1 [Reynolds, Richard W.] N Carolina State Univ, Cooperat Inst Climate & Satellites, Asheville, NC USA.
[Reynolds, Richard W.] NOAA, Natl Climat Data Ctr, Asheville, NC 28801 USA.
[Chelton, Dudley B.] Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA.
[Chelton, Dudley B.] Oregon State Univ, Cooperat Inst Oceanog Satellite Studies, Corvallis, OR 97331 USA.
[Roberts-Jones, Jonah; Martin, Matthew J.] Met Off, Exeter, Devon, England.
[Menemenlis, Dimitris] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Merchant, Christopher John] Univ Edinburgh, Edinburgh, Midlothian, Scotland.
RP Reynolds, RW (reprint author), NOAA, Cooperat Inst Climate & Satellites, 151 Patton Ave, Asheville, NC 28801 USA.
EM richard.w.reynolds@noaa.gov
RI Merchant, Christopher/E-1180-2014
OI Merchant, Christopher/0000-0003-4687-9850
FU NOAA's Climate Data Record Program; NCDC; NOAA/Climate Program Office;
NASA Grant through Oregon State University [NS214A]; European Community
[283367]; NASA
FX This work was funded in part by NOAA's Climate Data Record Program,
managed by the National Climatic Data Center. We are grateful to NCDC
and the NOAA/Climate Program Office, which provided partial support for
this work. The graphics for all of the figures were computed using the
Grid Analysis and Display System (GrADS; available online at
http://grads.iges.org/grads) and finalized by the NCDC Graphics
Department. Both DCB and RWR were partially supported by NASA Grant
NS214A funded through Oregon State University. The research of JRJ and
MJM leading to these results has received funding from the European
Community's Seventh Framework Programme FP7/2007-2013 under Grant
Agreement 283367 (MyOcean 2). DM performed this work at the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with NASA.
NR 19
TC 4
Z9 4
U1 1
U2 14
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
J9 J CLIMATE
JI J. Clim.
PD APR
PY 2013
VL 26
IS 8
BP 2514
EP 2533
DI 10.1175/JCLI-D-12-00787.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 130XX
UT WOS:000317954700007
ER
PT J
AU Tatarinova, T
Neely, M
Bartroff, J
van Guilder, M
Yamada, W
Bayard, D
Jelliffe, R
Leary, R
Chubatiuk, A
Schumitzky, A
AF Tatarinova, Tatiana
Neely, Michael
Bartroff, Jay
van Guilder, Michael
Yamada, Walter
Bayard, David
Jelliffe, Roger
Leary, Robert
Chubatiuk, Alyona
Schumitzky, Alan
TI Two general methods for population pharmacokinetic modeling:
non-parametric adaptive grid and non-parametric Bayesian
SO JOURNAL OF PHARMACOKINETICS AND PHARMACODYNAMICS
LA English
DT Article
DE Population pharmacokinetic modeling; Non-parametric; Maximum likelihood;
Bayesian; Stick-breaking; Pmetrics; RJags
ID CHAIN MONTE-CARLO; PARAMETERS; SIMULATION; PRIORS
AB Population pharmacokinetic (PK) modeling methods can be statistically classified as either parametric or nonparametric (NP). Each classification can be divided into maximum likelihood (ML) or Bayesian (B) approaches. In this paper we discuss the nonparametric case using both maximum likelihood and Bayesian approaches. We present two nonparametric methods for estimating the unknown joint population distribution of model parameter values in a pharmacokinetic/pharmacodynamic (PK/PD) dataset. The first method is the NP Adaptive Grid (NPAG). The second is the NP Bayesian (NPB) algorithm with a stick-breaking process to construct a Dirichlet prior. Our objective is to compare the performance of these two methods using a simulated PK/PD dataset. Our results showed excellent performance of NPAG and NPB in a realistically simulated PK study. This simulation allowed us to have benchmarks in the form of the true population parameters to compare with the estimates produced by the two methods, while incorporating challenges like unbalanced sample times and sample numbers as well as the ability to include the covariate of patient weight. We conclude that both NPML and NPB can be used in realistic PK/PD population analysis problems. The advantages of one versus the other are discussed in the paper. NPAG and NPB are implemented in R and freely available for download within the Pmetrics package from www.lapk.org.
C1 [Tatarinova, Tatiana; Neely, Michael; Bartroff, Jay; van Guilder, Michael; Yamada, Walter; Bayard, David; Jelliffe, Roger; Leary, Robert; Schumitzky, Alan] Univ So Calif, Keck Sch Med, Lab Appl Pharmacokinet, Los Angeles, CA 90033 USA.
[Bartroff, Jay; Chubatiuk, Alyona; Schumitzky, Alan] Univ So Calif, Dept Math, Dornsife Coll Letters & Sci, Los Angeles, CA 90089 USA.
[Yamada, Walter] Azusa Pacific Univ, Dept Psychol, Azusa, CA USA.
[Bayard, David] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Leary, Robert] Pharsight Corp, Cary, NC USA.
RP Tatarinova, T (reprint author), Univ So Calif, Keck Sch Med, Lab Appl Pharmacokinet, Los Angeles, CA 90033 USA.
EM tatiana.tatarinova@lapk.org
RI Tatarinova, Tatiana/K-3445-2016
OI Tatarinova, Tatiana/0000-0003-1787-1112
FU NIH [GM068968, EB005803, EB001978]; NIH-NICHD [HD070996]; Royal Society
[TG103083]
FX Support from NIH: GM068968, EB005803, EB001978, NIH-NICHD: HD070996 and
Royal Society: TG103083 is gratefully acknowledged.
NR 43
TC 25
Z9 25
U1 2
U2 8
PU SPRINGER/PLENUM PUBLISHERS
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1567-567X
EI 1573-8744
J9 J PHARMACOKINET PHAR
JI J. Pharmacokinet. Pharmacodyn.
PD APR
PY 2013
VL 40
IS 2
BP 189
EP 199
DI 10.1007/s10928-013-9302-8
PG 11
WC Pharmacology & Pharmacy
SC Pharmacology & Pharmacy
GA 131EC
UT WOS:000317974200005
PM 23404393
ER
PT J
AU Sears, DWG
AF Sears, Derek W. G.
TI Oral Histories in Meteoritics and Planetary Science - XX: Dale
Cruikshank
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID SATELLITES; TRITON; ATMOSPHERE; ASTEROIDS; SURFACE; PLUTO; ICES; IO
AB In this interview, Dale Cruikshank (Fig.1) explains how as an undergraduate at Iowa State University he was a summer student at Yerkes Observatory where he assisted Gerard Kuiper in work on his Photographic Lunar Atlas. Upon completing his degree, Dale went to graduate school at the University of Arizona with Kuiper where he worked on the IR spectroscopy of the lunar surface. After an eventful 1968 trip to Moscow via Prague, during which the Soviets invaded Czechoslovakia, Dale assumed a postdoc position with Vasili Moroz at the Sternberg Astronomical Institute and more observational IR astronomy. Upon returning to the United States and after a year at Arizona, Dale assumed a position at the University of Hawai'i that he held for 17years. During this period Dale worked with others on thermal infrared determinations of the albedos of small bodies beyond the asteroid Main Belt, leading to the recognition that low-albedo material is prevalent in the outer solar system that made the first report of complex organic solids on a planetary body (Saturn's satellite Iapetus). After moving to Ames Research Center, where he works currently, he continued this work and became involved in many outer solar system missions. Dale has served the community through his involvement in developing national policies for science-driven planetary exploration, being chair of the DPS 19901991 and secretary/treasurer for 19821985. He served as president of Commission 16 (Physics of Planets) of the IAU (20012003). He received the Kuiper prize in 2006. 1 Dale P. Cruikshank.
C1 NASA, Ames Res Ctr, Planetary Sci & Astrobiol Div, Mountain View, CA 94035 USA.
RP Sears, DWG (reprint author), NASA, Ames Res Ctr, Planetary Sci & Astrobiol Div, Mountain View, CA 94035 USA.
EM derek.sears@nasa.gov
FU NASA
FX This interview was recorded on March 16, 2011, and edited by the author
and DPC. I am grateful to Klaus Keil for a review and Hazel Sears for
reviewing and proofing this article. A grant from NASA supported the
work.
NR 16
TC 0
Z9 0
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD APR
PY 2013
VL 48
IS 4
BP 700
EP 711
DI 10.1111/j.1945-5100.2012.01414.x
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 131WU
UT WOS:000318029400008
ER
PT J
AU Handler, G
Prinja, RK
Urbaneja, MA
Antoci, V
Twicken, JD
Barclay, T
AF Handler, G.
Prinja, R. K.
Urbaneja, M. A.
Antoci, V.
Twicken, J. D.
Barclay, T.
TI Kepler photometry and optical spectroscopy of the ZZ Lep central star of
the planetary nebula NGC 6826: rotational and wind variability
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: early-type; stars: mass-loss; stars: rotation; stars: winds,
outflows; planetary nebulae: individual: NGC 6826
ID COROTATING INTERACTION REGIONS; O-TYPE STARS; INITIAL CHARACTERISTICS;
CADENCE DATA; ASTEROSEISMOLOGY; ULTRAVIOLET; EVOLUTION; SCIENCE
AB We present three years of long-cadence and over one year of short-cadence photometry of the central star of the planetary nebula NGC 6826 obtained with the Kepler spacecraft, and temporally coinciding optical spectroscopy. The light curves are dominated by incoherent variability on time-scales of several hours, but contain a lower amplitude periodicity of 1.237 99 d. The temporal amplitude and shape changes of this signal are best explicable with a rotational modulation, and are not consistent with a binary interpretation. We argue that we do not observe stellar pulsations within the limitations of our data, and show that a binary central star with an orbital period less than seven days could only have escaped our detection in the case of low orbital inclination. Combining the photometric and spectroscopic evidence, we reason that the hourly variations are due to a variable stellar wind, and are global in nature. The physical cause of the wind variability of NGC 6826 and other ZZ Leporis stars is likely related to the mechanism responsible for wind variations in massive hot stars.
C1 [Handler, G.] Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
[Prinja, R. K.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Urbaneja, M. A.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Antoci, V.] Aarhus Univ, Dept Phys & Astron, SAC, DK-8000 Aarhus C, Denmark.
[Antoci, V.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Twicken, J. D.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Barclay, T.] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
RP Handler, G (reprint author), Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland.
EM gerald@camk.edu.pl
OI Antoci, Victoria/0000-0002-0865-3650
FU NASA's Science Mission Directorate; Danish National Research Foundation;
ASTERISK project; European Research Council [267864]; NCN
[2011/01/B/ST9/05448]
FX Funding for this Discovery mission is provided by NASA's Science Mission
Directorate. The authors thank the Kepler team for their continuous work
that ensures the best possible science output. Funding for the Stellar
Astrophysics Centre (SAC) is provided by The Danish National Research
Foundation. The research is supported by the ASTERISK project
(ASTERoseismic Investigations with SONG and Kepler) funded by the
European Research Council (Grant agreement no.: 267864). The authors
would like to thank S. Simon-Diaz for his assistance with the FIES/NOT
observations. GH acknowledges funding through NCN grant
2011/01/B/ST9/05448, and thanks Nada Jevtic and Andrzej Baran for their
comments on a draft version of this paper. Comments by the anonymous
referee improved part of our argumentation. This paper is partly based
on observations made with the Nordic Optical Telescope operated on the
island of La Palma by the Nordic Optical Telescope Scientific
Association in the Spanish Observatorio del Roque de los Muchachos.
NR 41
TC 5
Z9 5
U1 0
U2 4
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR
PY 2013
VL 430
IS 4
BP 2923
EP 2931
DI 10.1093/mnras/stt092
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 136CZ
UT WOS:000318339700035
ER
PT J
AU Zhou, Y
Isheim, D
Hsieh, G
Noebe, RD
Seidman, DN
AF Zhou, Yang
Isheim, Dieter
Hsieh, Gillian
Noebe, Ronald D.
Seidman, David N.
TI Effects of ruthenium on phase separation in a model NiAlCrRu superalloy
SO PHILOSOPHICAL MAGAZINE
LA English
DT Article
DE NiAlCrRu alloy; effects of Ru; coarseniing kinetics; atom-probe
tomography; transmission electron microscopy
ID NICKEL-BASE SUPERALLOYS; SINGLE-CRYSTAL SUPERALLOYS; NI-CR-AL;
3-DIMENSIONAL ATOM-PROBE; OSTWALD RIPENING THEORIES;
MONTE-CARLO-SIMULATION; TEMPORAL EVOLUTION; GAMMA'-PHASE; MULTICOMPONENT
ALLOYS; KINETIC PATHWAYS
AB The temporal evolution of a Ni10.0Al8.5Cr2.0Ru (at.%) alloy aged at 1073K was investigated using transmission electron microscopy (TEM) and atom-probe tomography. The (L1(2))-precipitate morphology is spheroidal through 256h of ageing as a result of adding Ru, which decreases the lattice parameter misfit between the (L1(2))- and (f.c.c.)-phases. The addition of Ru accelerates the compositional evolution of the (L1(2))- and (f.c.c.)-phases, which achieve their equilibrium compositions after 0.25h. Initially, Ru accelerates the partitioning of Ni and Cr to the (f.c.c.)-phase, and the partitioning of Al to the (L1(2))-phase, but after 0.25h, Ru, which partitions to the (f.c.c.)-phase, decreases the partitioning of Ni and increases the partitioning of Al and Cr. The temporal evolution of the average radius, R(t), number density, volume fraction of the (L1(2))-precipitates, and the supersaturations of Ni, Al, Cr, and Ru in the (f.c.c.)- and (L1(2))-phases are compared in detail with predictions of coarsening models and PrecipiCalc simulations. Based on a spline function fitting procedure of the concentration profiles between the (L1(2))- and (f.c.c.)-phases, it is demonstrated that the temporal evolution of the normalized interfacial width, /R(t) vs.R(t), of each element, decreases with increasing ageing time: is the interfacial width.
C1 [Zhou, Yang; Isheim, Dieter; Hsieh, Gillian; Seidman, David N.] Northwestern Univ, Dept Mat Sci & Engn, Evanston, IL 60208 USA.
[Zhou, Yang] Micron Technol Inc, Surface Anal Lab, Boise, ID 83707 USA.
[Noebe, Ronald D.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
[Isheim, Dieter; Seidman, David N.] Northwestern Univ, Ctr Atom Probe Tomog NUCAPT, Mat Res Sci & Engn Ctr, Evanston, IL 60208 USA.
RP Seidman, DN (reprint author), Northwestern Univ, Dept Mat Sci & Engn, 2220 Campus Dr, Evanston, IL 60208 USA.
EM d-seidman@northwestern.edu
RI Seidman, David/B-6697-2009
FU National Science Foundation (NSF) [DMR-0804610]; NSF-NSEC; NSF-MRSEC;
Keck Foundation; State of Illinois; Northwestern University; NSF-MRI
[DMR-0420, 532]; ONR-DURIP [N00014-0400, 798, N00014-0610539,
NOOO14-0910, 781]
FX This research was sponsored by the National Science Foundation (NSF)
under grant DMR-0804610. The TEM studies were performed in the EPIC
facility of the NUANCE Center at Northwestern University. The NUANCE
Center is supported by NSF-NSEC, NSF-MRSEC, the Keck Foundation, the
State of Illinois and Northwestern University. Atom-probe tomographic
measurements were performed in the Northwestern University Center for
Atom-Probe Tomography (NUCAPT). The LEAP tomograph was purchased and
upgraded with funding from NSF-MRI (DMR-0420,532) and ONR-DURIP
(N00014-0400,798, N00014-0610539, NOOO14-0910,781) grants. Ms. Gillian
Hsieh's contributions to this article constitute portions of her senior
thesis in the Department of Material Science and Engineering: she was
also supported by a NSF REU during one summer. Dr Jou at Questek
Inovations LLC is kindly thanked for help with PrecipiCalc simulations,
Dr Chantal K. Sudbrack is thanked for performing the JMat Pro
calculations and reading the manuscript, Drs Christopher Booth-Morrison
and Yaron Amouyal are thanked for helpful discussions and Dr Carelyn
Campbell (NIST) for diffusivity databases.
NR 113
TC 3
Z9 3
U1 0
U2 20
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 1478-6435
J9 PHILOS MAG
JI Philos. Mag.
PD APR 1
PY 2013
VL 93
IS 10-12
SI SI
BP 1326
EP 1350
DI 10.1080/14786435.2013.765989
PG 25
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering; Physics, Applied; Physics, Condensed Matter
SC Materials Science; Metallurgy & Metallurgical Engineering; Physics
GA 129LO
UT WOS:000317841300014
ER
PT J
AU Aunai, N
Hesse, M
Black, C
Evans, R
Kuznetsova, M
AF Aunai, Nicolas
Hesse, Michael
Black, Carrie
Evans, Rebekah
Kuznetsova, Maria
TI Influence of the dissipation mechanism on collisionless magnetic
reconnection in symmetric and asymmetric current layers
SO PHYSICS OF PLASMAS
LA English
DT Article
ID MAGNETOPAUSE; SIMULATIONS; CHALLENGE; REGION; SHEET
AB Numerical studies implementing different versions of the collisionless Ohm's law have shown a reconnection rate insensitive to the nature of the non-ideal mechanism occurring at the X line, as soon as the Hall effect is operating. Consequently, the dissipation mechanism occurring in the vicinity of the reconnection site in collisionless systems is usually thought not to have a dynamical role beyond the violation of the frozen-in condition. The interpretation of recent studies has, however, led to the opposite conclusion that the electron scale dissipative processes play an important dynamical role in preventing an elongation of the electron layer from throttling the reconnection rate. This work re-visits this topic with a new approach. Instead of focusing on the extensively studied symmetric configuration, we aim to investigate whether the macroscopic properties of collisionless reconnection are affected by the dissipation physics in asymmetric configurations, for which the effect of the Hall physics is substantially modified. Because it includes all the physical scales a priori important for collisionless reconnection (Hall and ion kinetic physics) and also because it allows one to change the nature of the non-ideal electron scale physics, we use a (two dimensional) hybrid model. The effects of numerical, resistive, and hyper-resistive dissipation are studied. In a first part, we perform simulations of symmetric reconnection with different non-ideal electron physics. We show that the model captures the already known properties of collisionless reconnection. In a second part, we focus on an asymmetric configuration where the magnetic field strength and the density are both asymmetric. Our results show that contrary to symmetric reconnection, the asymmetric model evolution strongly depends on the nature of the mechanism which breaks the field line connectivity. The dissipation occurring at the X line plays an important role in preventing the electron current layer from elongating and forming plasmoids. (C) 2013 American Institute of Physics. [http://dx.doi.org/10.1063/1.4795727]
C1 [Aunai, Nicolas; Hesse, Michael; Black, Carrie; Evans, Rebekah; Kuznetsova, Maria] NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Aunai, N (reprint author), NASA, Space Weather Lab, Goddard Space Flight Ctr, Code 674, Greenbelt, MD 20771 USA.
EM nicolas.aunai@nasa.gov
RI feggans, john/F-5370-2012; NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
FU NASA
FX Three of us (N.A., C. B., and R. E.) acknowledge support from the NASA
postdoctoral program. The authors acknowledge Roch Smets for the hybrid
code.
NR 41
TC 7
Z9 7
U1 1
U2 6
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 1070-664X
J9 PHYS PLASMAS
JI Phys. Plasmas
PD APR
PY 2013
VL 20
IS 4
AR 042901
DI 10.1063/1.4795727
PG 13
WC Physics, Fluids & Plasmas
SC Physics
GA 134UY
UT WOS:000318241900051
ER
PT J
AU Denneau, L
Jedicke, R
Grav, T
Granvik, M
Kubica, J
Milani, A
Veres, P
Wainscoat, R
Chang, D
Pierfederici, F
Kaiser, N
Chambers, KC
Heasley, JN
Magnier, EA
Price, PA
Myers, J
Kleyna, J
Hsieh, H
Farnocchia, D
Waters, C
Sweeney, WH
Green, D
Bolin, B
Burgett, WS
Morgan, JS
Tonry, JL
Hodapp, KW
Chastel, S
Chesley, S
Fitzsimmons, A
Holman, M
Spahr, T
Tholen, D
Williams, GV
Abe, S
Armstrong, JD
Bressi, TH
Holmes, R
Lister, T
McMillan, RS
Micheli, M
Ryan, EV
Ryan, WH
Scotti, JV
AF Denneau, Larry
Jedicke, Robert
Grav, Tommy
Granvik, Mikael
Kubica, Jeremy
Milani, Andrea
Veres, Peter
Wainscoat, Richard
Chang, Daniel
Pierfederici, Francesco
Kaiser, N.
Chambers, K. C.
Heasley, J. N.
Magnier, Eugene A.
Price, P. A.
Myers, Jonathan
Kleyna, Jan
Hsieh, Henry
Farnocchia, Davide
Waters, Chris
Sweeney, W. H.
Green, Denver
Bolin, Bryce
Burgett, W. S.
Morgan, J. S.
Tonry, John L.
Hodapp, K. W.
Chastel, Serge
Chesley, Steve
Fitzsimmons, Alan
Holman, Matthew
Spahr, Tim
Tholen, David
Williams, Gareth V.
Abe, Shinsuke
Armstrong, J. D.
Bressi, Terry H.
Holmes, Robert
Lister, Tim
McMillan, Robert S.
Micheli, Marco
Ryan, Eileen V.
Ryan, William H.
Scotti, James V.
TI The Pan-STARRS Moving Object Processing System
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID EARTH-APPROACHING ASTEROIDS; SYNOPTIC SURVEY TELESCOPE; ORBIT
DETERMINATION; SIZE DISTRIBUTION; POPULATION; SPACEWATCH;
IDENTIFICATION; CALIBRATION; PROGRAM; ARRAY
AB We describe the Pan-STARRS Moving Object Processing System (MOPS), a modern software package that produces automatic asteroid discoveries and identifications from catalogs of transient detections from next-generation astronomical survey telescopes. MOPS achieves >99.5% efficiency in producing orbits from a synthetic but realistic population of asteroids whose measurements were simulated for a Pan-STARRS4-class telescope. Additionally, using a nonphysical grid population, we demonstrate that MOPS can detect populations of currently unknown objects such as interstellar asteroids. MOPS has been adapted successfully to the prototype Pan-STARRS1 telescope despite differences in expected false detection rates, fill-factor loss, and relatively sparse observing cadence compared to a hypothetical Pan-STARRS4 telescope and survey. MOPS remains highly efficient at detecting objects but drops to 80% efficiency at producing orbits. This loss is primarily due to configurable MOPS processing limits that are not yet tuned for the Pan-STARRS1 mission. The core MOPS software package is the product of more than 15 person-years of software development and incorporates countless additional years of effort in third-party software to perform lower-level functions such as spatial searching or orbit determination. We describe the high-level design of MOPS and essential subcomponents, the suitability of MOPS for other survey programs, and suggest a road map for future MOPS development.
C1 [Denneau, Larry; Jedicke, Robert; Veres, Peter; Wainscoat, Richard; Chang, Daniel; Kaiser, N.; Chambers, K. C.; Heasley, J. N.; Magnier, Eugene A.; Kleyna, Jan; Hsieh, Henry; Waters, Chris; Sweeney, W. H.; Green, Denver; Bolin, Bryce; Burgett, W. S.; Morgan, J. S.; Tonry, John L.; Hodapp, K. W.; Chastel, Serge; Tholen, David; Armstrong, J. D.; Micheli, Marco] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Grav, Tommy] Johns Hopkins Univ, Baltimore, MD USA.
[Granvik, Mikael] Univ Helsinki, Dept Phys, FIN-00014 Helsinki, Finland.
[Milani, Andrea; Farnocchia, Davide] Univ Pisa, Pisa, Italy.
[Pierfederici, Francesco] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Myers, Jonathan] Univ Arizona, Tucson, AZ USA.
[Farnocchia, Davide; Chesley, Steve] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Fitzsimmons, Alan] Queens Univ Belfast, Astrophys Res Ctr, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland.
[Holman, Matthew] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Spahr, Tim; Williams, Gareth V.] Smithsonian Astrophys Observ, Cambridge, MA USA.
[Abe, Shinsuke] Natl Cent Univ, Inst Astron, Taipei, Taiwan.
[Bressi, Terry H.; McMillan, Robert S.; Scotti, James V.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Holmes, Robert] Astron Res Inst, Charleston, IL 61920 USA.
[Lister, Tim] Las Cumbres Observ Global Telescope Network Inc, Santa Barbara, CA 93117 USA.
[Ryan, Eileen V.; Ryan, William H.] New Mexico Inst Min & Technol, Magdalena Ridge Observ, Socorro, NM 87801 USA.
RP Denneau, L (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
EM denneau@ifa.hawaii.edu
OI Chambers, Kenneth /0000-0001-6965-7789; Granvik,
Mikael/0000-0002-5624-1888; Micheli, Marco/0000-0001-7895-8209
FU National Aeronautics and Space Administration issued through the
Planetary Science Division of the NASA Science Mission Directorate
[NNX08AR22G]; United States Air Force Research Laboratory (AFRL,
Albuquerque, NM) [F29601-02-1-0268]; Large Synoptic Survey Telescope
(LSST) Corporation
FX The Pan-STARRS1 Survey has been made possible through contributions of
the Institute for Astronomy, the University of Hawai'i, the Pan-STARRS
Project Office, the Max-Planck Society and its participating institutes,
the Max Planck Institute for Astronomy, Heidelberg and the Max Planck
Institute for Extraterrestrial Physics, Garching, The Johns Hopkins
University, Durham University, the University of Edinburgh, Queen's
University Belfast, the Harvard-Smithsonian Center for Astrophysics, and
the Las Cumbres Observatory Global Telescope Network, Incorporated, the
National Central University of Taiwan, and the National Aeronautics and
Space Administration under Grant No. NNX08AR22G issued through the
Planetary Science Division of the NASA Science Mission Directorate.; The
design and construction of the Panoramic Survey Telescope and Rapid
Response System by the University of Hawaii Institute for Astronomy was
funded by the United States Air Force Research Laboratory (AFRL,
Albuquerque, NM) through grant number F29601-02-1-0268.; We acknowledge
the financial and technical contributions to this work made by the Large
Synoptic Survey Telescope (LSST) Corporation team, in particular Tim
Axelrod, Lynne Jones and Jeff Kantor. In addition, we acknowledge the
support by Pan-STARRS and LSST management to enable and facilitate this
productive collaborative effort between the two projects.
NR 59
TC 30
Z9 30
U1 0
U2 5
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD APR
PY 2013
VL 125
IS 926
BP 357
EP 395
DI 10.1086/670337
PG 39
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 131BM
UT WOS:000317965800004
ER
PT J
AU Dixon, WV
Blair, WP
Kruk, JW
Romelfanger, ML
AF Dixon, William V.
Blair, William P.
Kruk, Jeffrey W.
Romelfanger, Mary L.
TI The Hopkins Ultraviolet Telescope: The Final Archive
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID CALIBRATION; MISSION; PERFORMANCE; ASTRONOMY; SPECTRUM
AB The Hopkins Ultraviolet Telescope (HUT) was a 0.9 m telescope and moderate-resolution (Delta lambda = 3 angstrom) far-ultraviolet (820-1850 angstrom) spectrograph that flew twice on the space shuttle, in 1990 December (Astro-1, STS-35) and 1995 March (Astro-2, STS-67). The resulting spectra were originally archived in a nonstandard format that lacked important descriptive metadata. To increase their utility, we have modified the original data-reduction software to produce a new and more user-friendly data product, a time-tagged photon list similar in format to the Intermediate Data Files (IDFs) produced by the Far Ultraviolet Spectroscopic Explorer calibration pipeline. We have transferred all relevant pointing and instrument-status information from locally-archived science and engineering databases into new FITS header keywords for each data set. Using this new pipeline, we have reprocessed the entire HUT archive from both missions, producing a new set of calibrated spectral products in a modern FITS format that is fully compliant with Virtual Observatory requirements. For each exposure, we have generated quick-look plots of the fully-calibrated spectrum and associated pointing history information. Finally, we have retrieved from our archives HUT TV guider images, which provide information on aperture positioning relative to guide stars, and converted them into FITS-format image files. All of these new data products are available in the new HUT section of the Mikulski Archive for Space Telescopes (MAST), along with historical and reference documents from both missions. In this article, we document the improved data-processing steps applied to the data and show examples of the new data products.
C1 [Dixon, William V.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Blair, William P.; Romelfanger, Mary L.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Kruk, Jeffrey W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Dixon, WV (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM dixon@stsci.edu; wpb@pha.jhu.edu; Jeffrey.W.Kruk@nasa.gov;
mary@pha.jhu.edu
FU NASA ADP Grant [NNX09AC70G]; Center for Astrophysical Sciences at the
Johns Hopkins University; NASA [NAS5-26555]; NASA Office of Space
Science [NAG5-7584]
FX This work has been supported by NASA ADP Grant #NNX09AC70G to the Johns
Hopkins University and by the Center for Astrophysical Sciences at the
Johns Hopkins University. It has made use of NASA's Astrophysics Data
System Bibliographic Services (ADS) and the Mikulski Archive for Space
Telescopes (MAST), hosted at the Space Telescope Science Institute.
STScI is operated by the Association of Universities for Research in
Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for
non-HST data is provided by the NASA Office of Space Science via grant
NAG5-7584 and by other grants and contracts. IRAF, the Image Reduction
and Analysis Facility, is distributed by the National Optical Astronomy
Observatories, which are operated by the Association of Universities for
Research in Astronomy, Inc., under cooperative agreement with the
National Science Foundation. IDL is a registered trademark of Exelis
Visual Information Solutions, Inc., for its Interactive Data Language
software.
NR 17
TC 2
Z9 2
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD APR
PY 2013
VL 125
IS 926
BP 431
EP 443
DI 10.1086/670227
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 131BM
UT WOS:000317965800008
ER
PT J
AU Sonnett, S
Meech, K
Jedicke, R
Bus, S
Tonry, J
Hainaut, O
AF Sonnett, S.
Meech, K.
Jedicke, R.
Bus, S.
Tonry, J.
Hainaut, O.
TI Testing Accuracy and Precision of Existing Photometry Algorithms on
Moving Targets
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID APERTURE PHOTOMETRY; CCD PHOTOMETRY; FIELDS; SEXTRACTOR; EXTRACTION;
NOISE; TOOL
AB Previous studies determining which astronomical photometry software is best suited for a particular dataset are usually focused on speed, source classification, and/or meeting a sensitivity requirement. For faint objects in particular, the priority is given to maximizing signal-to-noise ratio. Photometry of moving targets offers additional challenges (1) to aperture photometry because background object contamination varies from image to image, and (2) to routines that build a PSF model from point sources in the image because trailed field stars do not perfectly represent the PSF of the untrailed target. Here, we present the results of testing several photometry algorithms (tphot, DAOPHOT, DoPHOT, APT, and multiple techniques within Source Extractor and IRAF's PHOT) on data for a faint, slow-moving solar system object with a known light curve. We find that the newly-developed tphot software most accurately and precisely reproduces the object's true light curve, with particular advantages in centroiding, exclusion of contaminants from the target's flux, and fitting flux in the wings of the point-spread function.
C1 [Sonnett, S.; Meech, K.; Jedicke, R.; Bus, S.; Tonry, J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Sonnett, S.; Meech, K.] Univ Hawaii, NASA, Astrobiol Inst, Honolulu, HI 96822 USA.
[Hainaut, O.] European So Observ, D-85748 Garching, Germany.
RP Sonnett, S (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA.
FU National Aeronautics and Space Administration by NASA [NAG5-4495,
NNX07A044G, NNX07AF79G]; National Science Foundation [AST-1010059,
AST-1009749]
FX This material is based upon work supported by the National Aeronautics
and Space Administration by NASA Grant Nos. NAG5-4495, NNX07A044G,
NNX07AF79G, and from the National Science Foundation through grant
AST-1010059. Partial support for this work was provided by National
Science Foundation grant AST-1009749. Initial image processing in this
article has been performed using the IRAF software. IRAF is distributed
by the National Optical Astronomy Observatories, which is operated by
the Association of Universities for Research in Astronomy, Inc. (AURA)
under cooperative agreement with the National Science Foundation.
NR 25
TC 1
Z9 1
U1 0
U2 0
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD APR
PY 2013
VL 125
IS 926
BP 456
EP 469
DI 10.1086/670593
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 131BM
UT WOS:000317965800010
ER
PT J
AU El Akkraoui, A
Tremolet, Y
Todling, R
AF El Akkraoui, Amal
Tremolet, Yannick
Todling, Ricardo
TI Preconditioning of variational data assimilation and the use of a
bi-conjugate gradient method
SO QUARTERLY JOURNAL OF THE ROYAL METEOROLOGICAL SOCIETY
LA English
DT Article
DE minimization algorithms; Lanczos method; 4D-Var; GSI; preconditioned
Conjugate Gradient methods
ID ECMWF OPERATIONAL IMPLEMENTATION; NONSYMMETRIC LINEAR-SYSTEMS;
METEOROLOGICAL OBSERVATIONS; 4D-VAR; MODEL; CONVERGENCE; SCHEME;
COVARIANCES; ALGORITHMS; EQUATIONS
AB Presently, a preferred minimization for strong-constraint four-dimensional variational (4D-Var) assimilation uses a Lanczos-based conjugate gradient (CG) algorithm. This requires the availability of a square-root of the background-error covariance matrix (B). In the context of weak-constraint 4D-Var, this requirement might be too restrictive for the formulations of the model error term. It might therefore be desirable to avoid a square-root decomposition of the augmented background term. An appealing minimization scheme is the double CG minimization employed, for example, in the grid-point statistical interpolation (GSI) analysis. Realizing the double CG algorithm is a special case of the more general bi-conjugate gradient (BiCG) method for solving non-symmetric problems, the present work introduces a Lanczos-based preconditioning strategy when B, instead of its square-root, is used initially. Implementation of the scheme is done in the context of the GSI analysis system, and preliminary experiments are presented using its 3D-Var version. Comparison of the Lanczos-based CG and the BiCG shows that the algorithms converge at the same rate and to the same solution. Despite the additional computational cost, the importance of the re-orthogonalization step is also shown to be fundamental to any of these CG algorithms. Furthermore, when using the Hessian eigenvectors for preconditioning, the BiCG behaviour is shown to be comparable to that of the Lanczos-CG algorithm. Both schemes construct the same approximation of the Hessian with the same number of eigenvectors, and benefit in the same way from the reduction of the condition number. The efficiency, computational cost, and stability of the three algorithms are discussed. Copyright (c) 2012 Royal Meteorological Society
C1 [El Akkraoui, Amal; Todling, Ricardo] NASA, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[El Akkraoui, Amal] Sci Syst & Applicat Inc, Lanham, MD USA.
[Tremolet, Yannick] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England.
RP El Akkraoui, A (reprint author), NASA, Global Modeling & Assimilat Off, GSFC, Code 610-1, Greenbelt, MD 20771 USA.
EM amal.elakkraoui@nasa.gov
NR 50
TC 5
Z9 5
U1 0
U2 4
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-9009
J9 Q J ROY METEOR SOC
JI Q. J. R. Meteorol. Soc.
PD APR
PY 2013
VL 139
IS 672
BP 731
EP 741
DI 10.1002/qj.1997
PN A
PG 11
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 130QK
UT WOS:000317933600013
ER
PT J
AU Whitehurst, AS
Swatantran, A
Blair, JB
Hofton, MA
Dubayah, R
AF Whitehurst, Amanda S.
Swatantran, Anu
Blair, J. Bryan
Hofton, Michelle A.
Dubayah, Ralph
TI Characterization of Canopy Layering in Forested Ecosystems Using Full
Waveform Lidar
SO REMOTE SENSING
LA English
DT Article
DE lidar; vertical structure; canopy layering; New Hampshire
ID DISCRETE-RETURN LIDAR; SPECIES-DIVERSITY; AIRBORNE LIDAR; TREE GROWTH;
RAIN-FOREST; STRUCTURAL CHARACTERISTICS; LASER ALTIMETER; TROPICAL
FOREST; SMALL-FOOTPRINT; VEGETATION
AB Canopy structure, the vertical distribution of canopy material, is an important element of forest ecosystem dynamics and habitat preference. Although vertical stratification, or "canopy layering," is a basic characterization of canopy structure for research and forest management, it is difficult to quantify at landscape scales. In this paper we describe canopy structure and develop methodologies to map forest vertical stratification in a mixed temperate forest using full-waveform lidar. Two definitions-one categorical and one continuous-are used to map canopy layering over Hubbard Brook Experimental Forest, New Hampshire with lidar data collected in 2009 by NASA's Laser Vegetation Imaging Sensor (LVIS). The two resulting canopy layering datasets describe variation of canopy layering throughout the forest and show that layering varies with terrain elevation and canopy height. This information should provide increased understanding of vertical structure variability and aid habitat characterization and other forest management activities.
C1 [Whitehurst, Amanda S.; Swatantran, Anu; Hofton, Michelle A.; Dubayah, Ralph] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA.
[Blair, J. Bryan] NASA, Goddard Space Flight Ctr, Laser Remote Sensing Lab, Greenbelt, MD 20771 USA.
RP Whitehurst, AS (reprint author), Univ Maryland, Dept Geog Sci, 2181 Samuel J LeFrak Hall, College Pk, MD 20742 USA.
EM awhitehu@umd.edu; aswatan@umd.edu; james.b.blair@nasa.gov;
mhofton@umd.edu; dubayah@umd.edu
RI Blair, James/D-3881-2013; Beckley, Matthew/D-4547-2013; Swatantran,
Anu/B-8786-2016
FU NASA Graduate Student Researchers Program Fellowship [NNX09AL43H]
FX We would like to thank Geoffrey Parker, Sean McMahon, and Eric Kasischke
for their conceptual advice and comments throughout the research
process. Also, we would like to thank Naiara Pinto and Joseph Sexton for
their editorial reviews of this manuscript and Jyoteshwar Nagol for his
technical expertise. This project was funded by the NASA Graduate
Student Researchers Program Fellowship, grant number NNX09AL43H.
NR 60
TC 17
Z9 18
U1 1
U2 50
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD APR
PY 2013
VL 5
IS 4
BP 2014
EP 2036
DI 10.3390/rs5042014
PG 23
WC Remote Sensing
SC Remote Sensing
GA 131TZ
UT WOS:000318020600025
ER
PT J
AU James, JT
Lam, CW
Santana, PA
Scully, RR
AF James, John T.
Lam, Chiu-Wing
Santana, Patricia A.
Scully, Robert R.
TI Estimate of safe human exposure levels for lunar dust based on
comparative benchmark dose modeling
SO INHALATION TOXICOLOGY
LA English
DT Article
DE Benchmark dose; inhalation; lunar dust; mineral dust
ID TOXICITY
AB Brief exposures of Apollo astronauts to lunar dust occasionally elicited upper respiratory irritation; however, no limits were ever set for prolonged exposure to lunar dust. The United States and other space faring nations intend to return to the moon for extensive exploration within a few decades. In the meantime, habitats for that exploration, whether mobile or fixed, must be designed to limit human exposure to lunar dust to safe levels. Herein we estimate safe exposure limits for lunar dust collected during the Apollo 14 mission. We instilled three respirable- sized (similar to 2 mu mass median diameter) lunar dusts (two ground and one unground) and two standard dusts of widely different toxicities (quartz and TiO2) into the respiratory system of rats. Rats in groups of six were given 0, 1, 2.5 or 7.5 mg of the test dust in a saline-Survanta (R) vehicle, and biochemical and cellular biomarkers of toxicity in lung lavage fluid were assayed 1 week and one month after instillation. By comparing the dose-response curves of sensitive biomarkers, we estimated safe exposure levels for astronauts and concluded that unground lunar dust and dust ground by two different methods were not toxicologically distinguishable. The safe exposure estimates were 1.3 +/- 0.4 mg/m(3) (jet-milled dust), 1.0 +/- 0.5 mg/m(3) (ball-milled dust) and 0.9 +/- 0.3 mg/m(3) (unground, natural dust). We estimate that 0.5-1 mg/ m(3) of lunar dust is safe for periodic human exposures during long stays in habitats on the lunar surface.
C1 [James, John T.] NASA, Lyndon B Johnson Space Ctr, Space Toxicol Off, Houston, TX 77058 USA.
[Lam, Chiu-Wing; Scully, Robert R.] Wyle Sci Technol & Engn Grp, Houston, TX USA.
[Santana, Patricia A.] Univ Space Res Assoc, Houston, TX USA.
RP James, JT (reprint author), NASA, Lyndon B Johnson Space Ctr, Space Toxicol Off, Houston, TX 77058 USA.
EM john.t.james@nasa.gov
FU Human Research Program of the NASA
FX This work was supported by the Human Research Program of the NASA. The
estimates provided herein should not be construed as official NASA
standards. The conclusions are those of the authors alone, and we report
no conflicts of interest.
NR 10
TC 4
Z9 4
U1 0
U2 8
PU INFORMA HEALTHCARE
PI LONDON
PA TELEPHONE HOUSE, 69-77 PAUL STREET, LONDON EC2A 4LQ, ENGLAND
SN 0895-8378
J9 INHAL TOXICOL
JI Inhal. Toxicol.
PD APR
PY 2013
VL 25
IS 5
BP 243
EP 256
DI 10.3109/08958378.2013.777821
PG 14
WC Toxicology
SC Toxicology
GA 131YJ
UT WOS:000318034500002
PM 23614726
ER
PT J
AU Chatterjee, A
Plawsky, JL
Wayner, PC
Chao, DF
Sicker, RJ
Lorik, T
Chestney, L
Margie, R
Eustace, J
Zoldak, J
AF Chatterjee, Arya
Plawsky, Joel L.
Wayner, Peter C., Jr.
Chao, David F.
Sicker, Ronald J.
Lorik, Tibor
Chestney, Louis
Margie, Raymond
Eustace, John
Zoldak, John
TI Constrained Vapor Bubble Heat Pipe Experiment Aboard the International
Space Station
SO JOURNAL OF THERMOPHYSICS AND HEAT TRANSFER
LA English
DT Article; Proceedings Paper
CT 49th AIAA Aerospace Sciences Meeting including the New Horizons Forum
and Aerospace Exposition
CY JAN 03-07, 2011
CL Orlando, FL
SP AIAA
ID TRIANGULAR MICROGROOVES; PREDICTION; TRANSPORT; EXCHANGER; GROOVES; FIN
AB A constrained vapor bubble heat pipe experiment was run in the microgravity environment of the International Space Station. Here we present the initial results that demonstrate significant differences in the operation of the constrained vapor bubble heat pipe in the microgravity environment as compared to the Earth's gravity. The temperature profile data along the heat pipe indicate that the heat pipe behavior is affected favorably by increased capillary flow and adversely by the absence of outside convective heat transfer as a heat loss mechanism. The reflectivity pattern viewed through the transparent quartz wall documented complex microflow patterns. Image data of the liquid profile in the grooves of the heat pipe indicate that the curvature gradient giving capillary flow is considerably different from that on Earth. Using experimental data for the temperature and meniscus profiles, a one-dimensional model gives the inside heat transfer coefficient, which was significantly higher in microgravity. An initial discussion of some of the data collected is presented.
C1 [Chatterjee, Arya; Plawsky, Joel L.; Wayner, Peter C., Jr.] Rensselaer Polytech Inst, Troy, NY 12180 USA.
[Chao, David F.; Sicker, Ronald J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Lorik, Tibor; Chestney, Louis; Margie, Raymond; Eustace, John; Zoldak, John] Zin Technol, Cleveland, OH 44130 USA.
RP Plawsky, JL (reprint author), Rensselaer Polytech Inst, Troy, NY 12180 USA.
EM arya.chatterjee@gmail.com; plawsky@rpi.edu; wayner@rpi.edu;
david.f.chao@nasa.gov; ronald.j.sicker@nasa.gov; lorikt@ZIN-TECH.COM;
ChestneyL@ZIN-TECH.COM; margier@Zin-tech.com; eustacej@ZIN-TECH.COM;
zoldakj@ZIN-TECH.COM
NR 23
TC 9
Z9 9
U1 0
U2 19
PU AMER INST AERONAUTICS ASTRONAUTICS
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0887-8722
EI 1533-6808
J9 J THERMOPHYS HEAT TR
JI J. Thermophys. Heat Transf.
PD APR-JUN
PY 2013
VL 27
IS 2
BP 309
EP 319
DI 10.2514/1.T3792
PG 11
WC Thermodynamics; Engineering, Mechanical
SC Thermodynamics; Engineering
GA 129YT
UT WOS:000317880600011
ER
PT J
AU Glaze, LS
Baloga, SM
AF Glaze, Lori S.
Baloga, Stephen M.
TI Simulation of inflated pahoehoe lava flows
SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH
LA English
DT Article
DE Lava flows; Pahoehoe; Modeling; Simulation
ID KILAUEA VOLCANO; INCLINED PLANE; FLOOD LAVAS; RANDOM-WALK; HAWAII;
MODEL; EMPLACEMENT; EXAMPLES; TUMULI; MARS
AB A new stochastic model simulates late-stage pahoehoe lobes where random processes dominate emplacement. The model prescribes probabilistic rules for determining where and when parcels of lava move within the lobe. Unlike a classical Brownian motion random walk, the model allows individual parcels to remain dormant, but fluid, for multiple time steps. The randomness of parcel volume transfers within the lobe interior as well as at the margins qualitatively reflects inflation processes observed in the field. The fraction of inflated volume to total volume increases with the total volume, with greater than 75% of the lobe volume contributed through inflation for typical lobes. The influence on planform shape and topographic cross-sectional profiles of total volume, source area and shape, topographic confinement, and sequential breakouts at the lobe margins, are all explored with the stochastic model. Each of these factors influences the overall lobe thickness and width. The model provides a means for assessing the relative importance of these processes through comparisons with field data. For the first time, Gaussian and parabolic functions are quantitatively fit to field measurements of pahoehoe lobes. Both functional forms provide adequate description of the cross-sectional flow shapes. When comparing simulated lobes to field data, sequential breakouts at the lobe margins are found to be an important process controlling the final topographic distribution of observed pahoehoe lobes. (C) 2013 Published by Elsevier B.V.
C1 [Glaze, Lori S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Baloga, Stephen M.] Proxemy Res, Gaithersburg, MD 20882 USA.
RP Glaze, LS (reprint author), NASA, Goddard Space Flight Ctr, Code 698,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM Lori.S.Glaze@nasa.gov; steve@proxemy.com
RI Glaze, Lori/D-1314-2012
FU NASA [WBS 811073.02.01.04.44, NNX08AF16G, WBS 203959.02.03.17.56,
NNX10AP63G]
FX This work was funded by the NASA Planetary Geology and Geophysics
Program (WBS 811073.02.01.04.44 for L. Glaze, and grant NNX08AF16G for
S. Baloga) and the NASA Mars Data Analysis Program (WBS
203959.02.03.17.56 for L Glaze, and grant NNX10AP63G for S. Baloga). The
authors would like to thank Dr. Scott Rowland for many insightful
discussions in the field over a number of years and Dr. Christopher
Hamilton for helpful comments on this manuscript and discussions of
quantitative field observations. Many others have also contributed over
many years regarding basic behavior of pahoehoe lava flows, including S.
Self, A. Harris, T. Thordarson, J. Bleacher, and R. Wright. L. Kestay
and an anonymous reviewer kindly provided very helpful comments on this
manuscript.
NR 38
TC 4
Z9 4
U1 1
U2 10
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0377-0273
EI 1872-6097
J9 J VOLCANOL GEOTH RES
JI J. Volcanol. Geotherm. Res.
PD APR 1
PY 2013
VL 255
BP 108
EP 123
DI 10.1016/j.jvolgeores.2013.01.018
PG 16
WC Geosciences, Multidisciplinary
SC Geology
GA 126PQ
UT WOS:000317633800009
ER
PT J
AU Liang, ZB
He, ZL
Zhou, XX
Powell, CA
Yang, YG
He, LM
Stoffella, PJ
AF Liang, Zhanbei
He, Zhenli
Zhou, Xuxia
Powell, Charles A.
Yang, Yuangen
He, Li Ming
Stoffella, Peter J.
TI Impact of mixed land-use practices on the microbial water quality in a
subtropical coastal watershed
SO SCIENCE OF THE TOTAL ENVIRONMENT
LA English
DT Article
DE Surface runoff water; Fecal indicator bacteria; Salmonella; Land use;
Host specific marker; Environmental parameters
ID FECAL INDICATOR BACTERIA; ESCHERICHIA-COLI; SOUTH FLORIDA; PCR ASSAY;
POLLUTION; SALMONELLA; CONTAMINATION; STREAM; ASSOCIATIONS; PERSISTENCE
AB Surface runoff water is an important non-point source of fecal pollution to downstream water; however, there is a lack of systematic studies on the microbial quality of surface runoff water from watersheds with mixed land uses. In this study water samples from 12 surface runoff holding water bodies (SRW), which collected runoff from various patterns of land use within the St. Lucie watershed along the southeastern coastline of Florida, were collected monthly for 22 months. The concentration of fecal indicator bacteria (FIB) and frequency of detection of Salmonella and host specific markers (HF183, CF128, CF193, and HS-esp) were determined, and their associations with land use, rainfall, and water physico-chemical parameters were investigated. Higher FIB concentrations were observed from urban land and cattle ranch sites. Within the same primary land use pattern, different sub-patterns did not have the same level of FIB: golf communities contributed less to fecal pollution than residential areas, and plant nursery sites contained relative higher FIB concentrations than other agricultural sites. Salmonella, CF128, and CF193 markers were more frequently detected from the cattle ranch sites. In contrast the frequency of detecting human specific markers (HF183 and HS-esp) was much higher in residential sites. Rainfall positively affected the concentration of FIB and occurrence of Salmonella, possibly by providing more inputs or mobilizing the sources from sediments. Water temperature, dissolved organic carbon (DOC), and nutrient levels were positively correlated with FIB concentrations and occurrence in SRW, possibly by promoting their growth and survival. This study indicated the need for site specific mitigation strategies to improve SRW and downstream water quality. (C) 2013 Elsevier B.V. All rights reserved.
C1 [Liang, Zhanbei; He, Zhenli; Zhou, Xuxia; Powell, Charles A.; Yang, Yuangen; Stoffella, Peter J.] Univ Florida, Inst Food & Agr Sci, Indian River Res & Educ Ctr, Ft Pierce, FL 34945 USA.
[He, Li Ming] NOAA, Natl Marine Fisheries Serv, Sacramento, CA 95814 USA.
RP He, ZL (reprint author), Univ Florida, Inst Food & Agr Sci, Indian River Res & Educ Ctr, Ft Pierce, FL 34945 USA.
EM lzbei001@gmail.com; zhe@ufl.edu; zhouxx1205@163.com; capowell@ufl.edu;
ygyang@ufl.edu; li-ming.he@noaa.gov; pjs@ufl.edu
RI He, Zhenli/R-1494-2016
OI He, Zhenli/0000-0001-7761-2070
FU South Florida Water Management District [4600001774]; GIS
FX This study was in part supported by a grant (contract#4600001774) from
South Florida Water Management District. Authors acknowledge Dr.
Chonggang Xu for GIS support. Special thanks are extended to anonymous
reviewers whose comments improved the manuscript.
NR 52
TC 15
Z9 15
U1 3
U2 45
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0048-9697
J9 SCI TOTAL ENVIRON
JI Sci. Total Environ.
PD APR 1
PY 2013
VL 449
BP 426
EP 433
DI 10.1016/j.scitotenv.2013.01.087
PG 8
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA 125KH
UT WOS:000317538200049
PM 23454704
ER
PT J
AU Liu, YQ
Peters-Lidard, CD
Kumar, S
Foster, JL
Shaw, M
Tian, YD
Fall, GM
AF Liu, Yuqiong
Peters-Lidard, Christa D.
Kumar, Sujay
Foster, James L.
Shaw, Michael
Tian, Yudong
Fall, Gregory M.
TI Assimilating satellite-based snow depth and snow cover products for
improving snow predictions in Alaska
SO ADVANCES IN WATER RESOURCES
LA English
DT Article
DE Data assimilation; Satellite snow products; Snow prediction; Streamflow
prediction
ID ENSEMBLE KALMAN FILTER; LAND INFORMATION-SYSTEM; HYDROLOGY MODEL;
SURFACE MODEL; MODIS; FRAMEWORK; AREA
AB Several satellite-based snow products are assimilated, both separately and jointly, into the Noah land surface model for improving snow prediction in Alaska. These include the standard and interpreted versions of snow cover fraction (SCF) data from the Moderate-Resolution Imaging Spectroradiometer (MODIS) and the snow depth (SD) estimates from the Advanced Microwave Scanning Radiometer for the Earth Observing System (AMSR-E). The satellite-based SD estimates are adjusted against in situ observations via statistical interpolation to reduce the potentially large biases, prior to being assimilated using an ensemble Kalman filter. A customized, rule-based direct insertion approach is developed to assimilate the two SCF datasets. Our results indicate that considerable overall improvement on snow prediction can be achieved via assimilating the bias-adjusted satellite SD estimates; however, the improvement does not always translate into improvements in streamflow prediction. Assimilating the standard MODIS SCF is found to have little impact on snow and streamflow predictions, while assimilating the interpreted SCF estimates, which have reduced cloud coverage and improved snow mapping accuracy, has resulted in the most consistent improvements on snow and streamflow predictions across the study domain. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Liu, Yuqiong; Kumar, Sujay; Tian, Yudong] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Liu, Yuqiong; Peters-Lidard, Christa D.; Foster, James L.; Shaw, Michael; Tian, Yudong] NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Kumar, Sujay; Shaw, Michael] Sci Applicat Int Corp, Beltsville, MD USA.
[Shaw, Michael] AF Weather Agcy, Offutt, NE USA.
[Fall, Gregory M.] Natl Operat Hydrol Remote Sensing Ctr, Chanhassem, MN USA.
RP Liu, YQ (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
EM Yuqiong.Liu@nasa.gov
RI Kumar, Sujay/B-8142-2015; Peters-Lidard, Christa/E-1429-2012
OI Peters-Lidard, Christa/0000-0003-1255-2876
FU NASA [NNX08AU51G]; NASA; NOAA; Air Force Weather Agency (AFWA)
FX Support for this study was provided by NASA under Grant NNX08AU51G and
as part of NASA's contribution to the National Climate Assessment
program. Additional funding comes from NOAA and the Air Force Weather
Agency (AFWA). Comments from Martyn Clark and an anonymous reviewer
helped to improve this manuscript.
NR 65
TC 25
Z9 28
U1 4
U2 37
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0309-1708
J9 ADV WATER RESOUR
JI Adv. Water Resour.
PD APR
PY 2013
VL 54
BP 208
EP 227
DI 10.1016/j.advwatres.2013.02.005
PG 20
WC Water Resources
SC Water Resources
GA 122UT
UT WOS:000317344300015
ER
PT J
AU Arzeno, NM
Stenger, MB
Lee, SMC
Ploutz-Snyder, R
Platts, SH
AF Arzeno, Natalia M.
Stenger, Michael B.
Lee, Stuart M. C.
Ploutz-Snyder, Robert
Platts, Steven H.
TI Sex differences in blood pressure control during 6 degrees head-down
tilt bed rest
SO AMERICAN JOURNAL OF PHYSIOLOGY-HEART AND CIRCULATORY PHYSIOLOGY
LA English
DT Article
DE microgravity; spaceflight; heart rate variability; autonomic control;
baroreflex sensitivity
ID AUTONOMIC CARDIOVASCULAR REGULATION; SYMPATHETIC-NERVE ACTIVITY;
PLASMA-VOLUME RESTORATION; RATE-VARIABILITY; BAROREFLEX SENSITIVITY;
ORTHOSTATIC HYPOTENSION; GENDER-DIFFERENCES; ARTERIAL-PRESSURE;
MENSTRUAL-CYCLE; CARDIAC BAROREFLEX
AB Arzeno NM, Stenger MB, Lee SM, Ploutz-Snyder R, Platts SH. Sex differences in blood pressure control during 6 degrees head-down tilt bed rest. Am J Physiol Heart Circ Physiol 304: H1114-H1123, 2013. First published February 8, 2013; doi: 10.1152/ajpheart.00391.2012.-Spaceflight-induced orthostatic intolerance has been studied for decades. Although similar to 22% of the astronaut corps are women, most mechanistic studies use mostly male subjects, despite known sex differences in autonomic control and postflight orthostatic intolerance. We studied adrenergic, baroreflex, and autonomic indexes during continuous infusions of vasoactive drugs in men and women during a 60-day head-down bed rest. Volunteers were tested before bed rest (20 men and 10 women) and around day 30 (20 men and 10 women) and day 60 (16 men and 8 women) of bed rest. Three increasing doses of phenylephrine (PE) and sodium nitroprusside were infused for 10 min after an infusion of normal saline. A 20-min rest period separated the phenylephrine and sodium nitroprusside infusions. Autonomic activity was approximated by spectral indexes of heart rate and blood pressure variability, and baroreflex sensitivity was measured by the spontaneous baroreflex slope. Parasympathetic modulation and baroreflex sensitivity decreased with bed rest, with women experiencing a larger decrease in baroreflex sensitivity by day 30 than men. The sympathetic activation of men and parasympathetic responsiveness of women in blood pressure control during physiological stress were preserved throughout bed rest. During PE infusions, women experienced saturation of the R-R interval at high frequency, whereas men did not, revealing a sex difference in the parabolic relationship between high-frequency R-R interval, a measurement of respiratory sinus arrhythmia, and R-R interval. These sex differences in blood pressure control during simulated microgravity reveal the need to study sex differences in long-duration spaceflight to ensure the health and safety of the entire astronaut corps.
C1 [Arzeno, Natalia M.; Stenger, Michael B.; Lee, Stuart M. C.] Wyle Sci Technol & Engn Grp, Houston, TX USA.
[Ploutz-Snyder, Robert] Univ Space Res Assoc, Houston, TX USA.
[Platts, Steven H.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Stenger, MB (reprint author), 1290 Hercules Dr, Houston, TX 77058 USA.
EM michael.b.stenger@nasa.gov
FU National Aeronautics and Space Administration (NASA)
[BRC-2003-0000-0543]; NASA Flight Analogs Project; NCRR [M01-RR-0073]
FX This work was funded by National Aeronautics and Space Administration
(NASA) Grant BRC-2003-0000-0543 and sponsored by the NASA Flight Analogs
Project. This work was conducted at the National Center for Research
Resources (NCRR)-funded (NCRR Grant M01-RR-0073) General Clinical
Research Center at the University of Texas Medical Branch (Galveston,
TX).
NR 66
TC 4
Z9 4
U1 1
U2 12
PU AMER PHYSIOLOGICAL SOC
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA
SN 0363-6135
J9 AM J PHYSIOL-HEART C
JI Am. J. Physiol.-Heart Circul. Physiol.
PD APR
PY 2013
VL 304
IS 8
BP H1114
EP H1123
DI 10.1152/ajpheart.00391.2012
PG 10
WC Cardiac & Cardiovascular Systems; Physiology; Peripheral Vascular
Disease
SC Cardiovascular System & Cardiology; Physiology
GA 126GP
UT WOS:000317601600008
PM 23396455
ER
PT J
AU Righter, K
Danielson, LR
Pando, K
Morris, RV
Graff, TG
Agresti, DG
Martin, AM
Sutton, SR
Newville, M
Lanzirotti, A
AF Righter, Kevin
Danielson, Lisa R.
Pando, Kellye
Morris, Richard V.
Graff, Trevor G.
Agresti, David G.
Martin, Audrey M.
Sutton, Stephen R.
Newville, Matt
Lanzirotti, Antonio
TI Redox systematics of martian magmas with implications for magnetite
stability
SO AMERICAN MINERALOGIST
LA English
DT Article
DE Mars; basalt; redox; magnetite
ID NATURAL SILICATE LIQUIDS; MARS MOSSBAUER DATA; OXIDATION-STATE; OXYGEN
FUGACITY; MELT EQUILIBRIA; SNC METEORITES; FREE-ENERGY; IRON;
SHERGOTTITE; CRYSTALLIZATION
AB Magnetite is commonly found at sites on Mars explored by robotic spacecraft, yet is rare in martian meteorites and in experimental studies of martian magma compositions. Iron redox systematics of the high-FeO shergottitic liquids are poorly known, yet have a fundamental control on stability of phases such as magnetite, ilmenite, and pyroxenes. We undertook experiments to constrain the Fe3+/Sigma Fe in high-FeO (15-22 wt%) glasses as a function of f(O2), melt P2O5, temperature and pressure. We also performed a series of sub-liquidus experiments between 1100 and 1000 degrees C and FMQ+0.5 to FMQ-1 to define magnetite stability. Run products were analyzed for Fe3+ and Fe2+ by Mossbauer spectroscopy and micro-X-ray absorption near edge structure (micro-XANES) spectroscopy. One bar liquids equilibrated at FMQ-3 to FMQ+3 show a much lower Fe3+/Sigma Fe than terrestrial basalts at the same conditions. As melt P2O5 contents increase from 0 to 3 wt% (at fixed pressure, temperature, and f(O2)), Fe3+/Sigma Fe decreases from 0.07 to 0.05, but this is within error on the measurements. Temperature increases between 1200 and 1500 degrees C cause little to no variation in Fe3+/Sigma Fe. Pressure increases from 1 to 4 GPa cause a 0.06 decrease in Fe3+/Sigma Fe. The trends with pressure and temperature are in agreement with results of previous studies. Combining our new series of data allows derivation of an expression to calculate Fe3+/Fe2+ for high-FeO melts such as martian magmas.
ln(XFe3+/XFe2+) = a lnf(O2) + b/T + cP/T + dX(FeO) + eX(Al2O3) + fX(CaO) + gX(Na2O) + hX(K2O) + iX(P2O5) + j
This expression can be used to show that decompressed melts become slightly more oxidized at the surface (compared to 4 GPa). Magnetite stability is suppressed by the lower Fe3+/Fe2+ of the high-FeO melts. Magnetite stability is a function of Fe2O3 and temperature and is stable similar to 50 degrees C lower than typical terrestrial basalt. Difficulty in producing magnetite as a liquidus phase in magmatic systems suggests either that many martian basalts are more oxidized than FMQ (but not represented among meteorite collections), that the titano-magnetite only forms upon cooling below similar to 1000 degrees C at FMQ, or that the magnetite has a secondary origin.
C1 [Righter, Kevin; Morris, Richard V.; Martin, Audrey M.] NASA, Lyndon B Johnson Space Ctr, Mailcode KT, 2101 NASA Pkwy, Houston, TX 77058 USA.
[Danielson, Lisa R.; Pando, Kellye; Graff, Trevor G.] NASA, Engn & Sci Contract Grp, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Agresti, David G.] Univ Alabama Birmingham, Dept Phys, Birmingham, AL 35294 USA.
[Sutton, Stephen R.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA.
[Sutton, Stephen R.; Newville, Matt; Lanzirotti, Antonio] Univ Chicago, Ctr Adv Radiat Sources, Chicago, IL 60637 USA.
RP Righter, K (reprint author), NASA, Lyndon B Johnson Space Ctr, Mailcode KT, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM kevin.righter-1@nasa.gov
OI Martin, Audrey/0000-0002-1165-8866
FU NASA-JSC by an RTOP from the NASA Mars Fundamental Research program;
National Science Foundation-Earth Sciences [EAR-1128799]; Department of
Energy-Geosciences [DE-FG02-94ER14466]; U.S. Department of Energy,
Office of Science, Office of Basic Energy Sciences [DE-AC02-06CH11357]
FX We thank M. Toplis and T. McCoy for discussions relating to redox
equilibria in martian magmas, and to T. McCoy for loaning samples from
his experimental study. The journal reviews of J. Karner, G. Moore, and
D. Dyar helped to improve the clarity of the presentation of this
material. Loan Le provided assistance in the gas mixing furnace lab, and
Anne Peslier and Kent Ross provided assistance with the electron
microbeam analysis. This research was supported at NASA-JSC by an RTOP
to K.R. from the NASA Mars Fundamental Research program. 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).
Use of the Advanced Photon Source was supported by the U.S. Department
of Energy, Office of Science, Office of Basic Energy Sciences, under
Contract No. DE-AC02-06CH11357.
NR 71
TC 11
Z9 11
U1 0
U2 39
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 APR
PY 2013
VL 98
IS 4
BP 616
EP 628
DI 10.2138/am.2013.4251
PG 13
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA 123FG
UT WOS:000317373200011
ER
PT J
AU Shen, ZZ
Konishi, H
Brown, PE
Xu, HF
AF Shen, Zhizhang
Konishi, Hiromi
Brown, Philip E.
Xu, Huifang
TI STEM investigation of exsolution lamellae and "c" reflections in Ca-rich
dolomite from the Platteville Formation, western Wisconsin
SO AMERICAN MINERALOGIST
LA English
DT Article
DE Dolomite; Z-contrast imaging; Ca-Mg ordering; TEM; twinning; high
magnesian calcite; c-reflection; exsolution
ID CALCIAN DOLOMITE; MICROSTRUCTURES; SUPERSTRUCTURES; ANKERITE
AB Dolomite crystals in partially dolomitized limestone from the Platteville Formation are both compositionally and microstructurally heterogeneous. A single dolomite crystal usually contains three phases: the host Ca-rich dolomite [Ca1.14Mg0.86(CO3)(2)], an Fe-bearing dolomite [Ca1.06Mg0.80Fe0.14(CO3)(2)], and calcite inclusions. These three phases show similar orientations. The Ca-rich dolomite exhibits modulated microstructures with wavelength ranging from 7 to 30 nm. The modulated microstructures are not evident in Fe-bearing dolomite.
Modulations in the Ca-rich dolomite have three predominant orientation ranges in the studied sample: from (205) to (104), from (001) to ((1) over bar 01), and (110), which are consistent with previous studies. Bright-field (BF) and high-angle annular dark-field (HAADF) images confirm that these modulations are due to chemical variation rather than strain or diffraction contrast. The Ca-rich lamellae are Mg-rich calcite with compositions ranging from Ca0.85Mg0.15CO3 to Ca0.70Mg0.30CO3. The observed results indicate that these Ca-rich exsolution lamellae formed during diagenesis. In this study, three kinds of "c"-reflections, which are weak spots in the halfway position between the principal reflections along the (104)*, ((1) over bar 12)*, and (110)* directions, have been found in the diffraction patterns of some Ca-rich dolomite. Mg-Ca ordering in x-y planes was not observed directly in Z-contrast images. FFT patterns from the Z-contrast images do not show "c"-reflections. STEM images confirm that the "c"-reflections could result from multiple diffraction between the host dolomite and twinned Mg-calcite nano-lamellae under TEM imaging and diffraction modes.
C1 [Shen, Zhizhang; Konishi, Hiromi; Brown, Philip E.; Xu, Huifang] Univ Wisconsin, Dept Geosci, NASA Astrobiol Inst, Madison, WI 53706 USA.
RP Shen, ZZ (reprint author), Univ Wisconsin, Dept Geosci, NASA Astrobiol Inst, Madison, WI 53706 USA.
EM hfxu@geology.wisc.edu
FU NASA Astrobiology Institute [N07-5489]; NSF [EAR-095800]; U.S.
Department of Energy [DE-FG02-09ER16050]
FX This work is supported by NASA Astrobiology Institute (N07-5489), NSF
(EAR-095800), and U.S. Department of Energy (DE-FG02-09ER16050).
NR 20
TC 4
Z9 4
U1 2
U2 16
PU MINERALOGICAL SOC AMER
PI CHANTILLY
PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA
SN 0003-004X
J9 AM MINERAL
JI Am. Miner.
PD APR
PY 2013
VL 98
IS 4
BP 760
EP 766
DI 10.2138/am.2013.4184
PG 7
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA 123FG
UT WOS:000317373200027
ER
PT J
AU Hilker, T
Frazer, GW
Coops, NC
Wulder, MA
Newnham, GJ
Stewart, JD
van Leeuwen, M
Culvenor, DS
AF Hilker, Thomas
Frazer, Gordon W.
Coops, Nicholas C.
Wulder, Michael A.
Newnham, Glenn J.
Stewart, James D.
van Leeuwen, Martin
Culvenor, Darius S.
TI Prediction of Wood Fiber Attributes from LiDAR-Derived Forest Canopy
Indicators
SO FOREST SCIENCE
LA English
DT Article
DE LiDAR; wood fiber; canopy structure; light regime; lodgepole pine
ID AIRBORNE LASER SCANNER; DOUGLAS-FIR; WESTERN HEMLOCK; MICROFIBRIL ANGLE;
PINUS-SYLVESTRIS; LODGEPOLE PINE; BASIC DENSITY; NORWAY SPRUCE; TREE
HEIGHT; SCOTS PINE
AB We investigated the potential use of airborne light detection and ranging (LiDAR) data to predict key wood fiber properties from extrinsic indicators in lodgepole pine leading forest stands located in the foothills of central Alberta, Canada. Six wood fiber attributes (wood density, cell perimeter, cell coarseness, mature fiber length, microfibril angle, and modulus of elasticity) were measured at 21 plots, and with use of data reduction techniques, two components of wood properties were derived: wood strength, stiffness, and fiber yield and fiber strength and smoothness. These wood fiber components were then compared with extrinsic indicators of wood characteristic-derived LiDAR-estimated topographic morphology, tree height, and canopy light metrics. The first principal component indicating wood strength and stiffness was significantly correlated to the depth of different canopy zones (or light regimes; r(2) = 0.55, P < 0.05). The second component, related to fiber strength and smoothness, was significantly correlated to the height of the canopy and canopy thickness (r(2) = 0.65, P < 0.05). The results indicate that airborne LiDAR attributes can explain about half of the observed variance in intrinsic wood fiber attributes, which is approximately 5-10% less than that explained by growth-related field-measured variables such as diameter increment and height. This reduction in explained variance can be balanced by the opportunities for much broader spatial characterizations of wood quantity and quality at the stand and landscape levels. FOR. SCI. 59(2):231-242.
C1 [Hilker, Thomas] Oregon State Univ, Coll Forestry, Corvallis, OR 97331 USA.
[Hilker, Thomas] NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA.
[Frazer, Gordon W.; Wulder, Michael A.] Nat Resources Canada, Canadian Forest Serv, Ottawa, ON, Canada.
[Coops, Nicholas C.; van Leeuwen, Martin] Univ British Columbia, Vancouver, BC V5Z 1M9, Canada.
[Newnham, Glenn J.; Culvenor, Darius S.] CSIRO Land & Water, Black Mountain, ACT, Australia.
[Stewart, James D.] Nat Resources Canada, Canadian Wood Fiber Ctr, Ottawa, ON, Canada.
RP Hilker, T (reprint author), Oregon State Univ, Coll Forestry, Corvallis, OR 97331 USA.
EM thomas.hilker@oregonstate.edu
RI van Leeuwen, Martin/B-3947-2013; Coops, Nicholas/J-1543-2012; Newnham,
Glenn/G-8115-2011; Wulder, Michael/J-5597-2016;
OI van Leeuwen, Martin/0000-0003-2572-2088; Coops,
Nicholas/0000-0002-0151-9037; Wulder, Michael/0000-0002-6942-1896;
Stewart, James/0000-0003-1664-1083
FU Canadian Wood Fiber Centre of the Canadian Forest Service of Natural
Resources Canada; Natural Sciences and Engineering Research Council
FX We thank West Fraser Mills, Hinton Wood Products, for access to the
Integrated Wood Properties Trend Assessment wood quality and forest
inventory data sets. We are also grateful to Alberta Sustainable
Resource Development for access to the LiDAR data set. We thank Jared
Salvail and Prem Gurung (Canadian Wood Fiber Centre) for their
assistance in field plot location and measurements. The Canadian Wood
Fiber Centre of the Canadian Forest Service of Natural Resources Canada
provided funding to support this research with additional support from
an Natural Sciences and Engineering Research Council Discovery grant to
NC Coops.
NR 67
TC 11
Z9 11
U1 2
U2 17
PU SOC AMER FORESTERS
PI BETHESDA
PA 5400 GROSVENOR LANE, BETHESDA, MD 20814 USA
SN 0015-749X
J9 FOREST SCI
JI For. Sci.
PD APR
PY 2013
VL 59
IS 2
BP 231
EP 242
PG 12
WC Forestry
SC Forestry
GA 123FJ
UT WOS:000317373500010
ER
PT J
AU Yi, TH
Zhang, GG
Tsujii, N
Fleurial, JP
Zevalkink, A
Snyder, GJ
Gronbech-Jensen, N
Kauzlarich, SM
AF Yi, Tanghong
Zhang, Gaigong
Tsujii, Naohito
Fleurial, Jean-Pierre
Zevalkink, Alex
Snyder, G. Jeffrey
Gronbech-Jensen, Niels
Kauzlarich, Susan M.
TI Phase Characterization, Thermal Stability, High-Temperature Transport
Properties, and Electronic Structure of Rare-Earth Zintl Phosphides
Eu3M2P4 (M = Ga, In)
SO INORGANIC CHEMISTRY
LA English
DT Article
ID THERMOELECTRIC PROPERTIES; CRYSTAL-STRUCTURE; BORON PHOSPHIDE; COMPOUND;
MAGNETORESISTANCE; EFFICIENCY; EU3IN2P4
AB Two rare-earth-containing ternary phosphides, Eu3Ga2P4 and Eu3In2P4, were synthesized by a two-step solid-state method with stoichiometric amounts of the constitutional elements. Refinements of the powder X-ray diffraction are consistent with the reported single-crystal structure with space group C2/c for Eu3Ga2P4 and Pnnm for Eu3In2P4. Thermal gravimetry and differential scanning calorimetry (TG-DSC) measurements reveal high thermal stability up to 1273 K. Thermal diffusivity measurements from room temperature to 800 K demonstrate thermal conductivity as low as 0.6 W/m.K for both compounds. Seebeck coefficient measurements from room temperature to 800 K indicate that both compounds are small band gap semiconductors. Eu3Ga2P4 shows p-type conductivity and Eu3In2P4 p-type conductivity in the temperature range 300-700 K and n-type conductivity above 700 K. Electronic structure calculations result in band gaps of 0.60 and 0.29 eV for Eu3Ga2P4 and Eu3In2P4, respectively. As expected for a valence precise Zintl phase, electrical resistivity is large, approximately 2600 and 560 m Omega.cm for Eu3Ga2P4 and Eu3In2P4 at room temperature, respectively. Measurements of transport properties suggest that these Zintl phosphides have potential for being good high-temperature thermoelectric materials with optimization of the charge carrier concentration by appropriate extrinsic dopants.
C1 [Yi, Tanghong; Tsujii, Naohito; Kauzlarich, Susan M.] Univ Calif Davis, Dept Chem, Davis, CA 95616 USA.
[Zhang, Gaigong; Gronbech-Jensen, Niels] Univ Calif Davis, Dept Appl Sci, Davis, CA 95616 USA.
[Tsujii, Naohito] Natl Inst Mat Sci, Tsukuba, Ibaraki 3050047, Japan.
[Fleurial, Jean-Pierre] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Zevalkink, Alex; Snyder, G. Jeffrey] CALTECH, Dept Mat Sci, Pasadena, CA 91109 USA.
RP Kauzlarich, SM (reprint author), Univ Calif Davis, Dept Chem, 1 Shields Ave, Davis, CA 95616 USA.
EM smkauzlarich@ucdavis.edu
RI Snyder, G. Jeffrey/E-4453-2011; Snyder, G/I-2263-2015; Tsujii,
Naohito/H-2544-2011
OI Snyder, G. Jeffrey/0000-0003-1414-8682; Tsujii,
Naohito/0000-0002-6181-5911
FU NSF [DMR1100313]; NSF/DOE [CBET-1048799]; NASA Jet Propulsion Laboratory
FX We gratefully acknowledge financial support from NSF DMR1100313, NSF/DOE
Partnership CBET-1048799, and NASA Jet Propulsion Laboratory.
NR 36
TC 4
Z9 4
U1 3
U2 61
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0020-1669
EI 1520-510X
J9 INORG CHEM
JI Inorg. Chem.
PD APR 1
PY 2013
VL 52
IS 7
BP 3787
EP 3794
DI 10.1021/ic302400q
PG 8
WC Chemistry, Inorganic & Nuclear
SC Chemistry
GA 119JT
UT WOS:000317094300041
PM 23517094
ER
PT J
AU Navarrete, JU
Cappelle, IJ
Schnittker, K
Borrok, DM
AF Navarrete, Jesica U.
Cappelle, Ian J.
Schnittker, Kimberlin
Borrok, David M.
TI Bioleaching of ilmenite and basalt in the presence of iron-oxidizing and
iron-scavenging bacteria
SO INTERNATIONAL JOURNAL OF ASTROBIOLOGY
LA English
DT Article
DE Bioleaching; biomining; in situ resource utilization; iron oxidizing
bacteria; biomineral
ID PSEUDOMONAS-MENDOCINA; LEPTOSPIRILLUM-FERROOXIDANS;
THIOBACILLUS-FERROOXIDANS; DISSOLUTION KINETICS; MINERAL DISSOLUTION;
GROWTH; DRAINAGE; MOBILIZATION; METEORITES; SUPPORT
AB Bioleaching has been suggested as an alternative to traditional mining techniques in extraterrestrial environments because it does not require extensive infrastructure and bulky hardware. In situ bioleaching of silicate minerals, such as those found on the moon or Mars, has been proposed as a feasible alternative to traditional extraction techniques that require either extreme heat and/or substantial chemical treatment. In this study, we investigated the biotic and abiotic leaching of basaltic rocks (analogues to those found on the moon and Mars) and the mineral ilmenite (FeTiO3) in aqueous environments under acidic (pH similar to 2.5) and circumneutral pH conditions. The biological leaching experiments were conducted using Acidithiobacillus ferrooxidans, an iron (Fe)-oxidizing bacteria, and Pseudomonas mendocina, an Fe-scavenging bacteria. We found that both strains were able to grow using the Fe(II) derived from the tested basaltic rocks and ilmenite. Although silica leaching rates were the same or slightly less in the bacterial systems with A. ferrooxidans than in the abiotic control systems, the extent of Fe, Al and Ti released (and re-precipitated in new solid phases) was actually greater in the biotic systems. This is likely because the Fe(II) leached from the basalt was immediately oxidized by A. ferrooxidans, and precipitated into Fe(III) phases which causes a change in the equilibrium of the system, i.e. Le Chatelier's principle. Iron(II) in the abiotic experiment was allowed to build up in solution which led to a decrease in its overall release rate. For example, the percentage of Fe, Al and Ti leached (dissolved + reactive mineral precipitates) from the Mars simulant in the A. ferrooxidans experimental system was 34, 41 and 13% of the total Fe, Al and Ti in the basalt, respectively, while the abiotic experimental system released totals of only 11, 25 and 2%. There was, however, no measurable difference in the amounts of Fe and Ti released from ilmenite in the experiments with A. ferrooxidans versus the abiotic controls. P. mendocina scavenged some Fe from the rock/mineral substrates, but the overall amount of leaching was small (<2% of total Fe in rocks) when compared with the acidophilic systems. Although the mineralogy of the tested basaltic rocks was roughly similar, the surface areas of the lunar and Mars simulants varied greatly and thus were possible factors in the overall amount of metals released. Overall, our results indicate that the presence of bacteria does not increase the overall silica leaching rates of basaltic rocks; however, the presence of A. ferrooxidans does lead to enhanced release of Fe, Al and Ti and subsequent sequestration of Fe (and other metals) in Fe(III)-precipitates.
C1 [Navarrete, Jesica U.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
[Navarrete, Jesica U.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Cappelle, Ian J.; Schnittker, Kimberlin; Borrok, David M.] Univ Texas El Paso, Dept Geol Sci, El Paso, TX 79968 USA.
RP Navarrete, JU (reprint author), Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
EM jesica.u.navarrete@nasa.gov
FU NASA [NNX09AV09A]; Center for Space Exploration Research at The
University of Texas at El Paso; National Science Foundation Graduate
Research Fellowship Programme
FX The material is based upon work supported by NASA under award No.
NNX09AV09A and the Center for Space Exploration Research at The
University of Texas at El Paso. Graduate funding for J. Navarrete was
provided through the National Science Foundation Graduate Research
Fellowship Programme. In addition, we would like to thank Jose H. Garcia
of the Department of Geological Sciences at the University of Texas at
El Paso and Bonnie L. Cooper from the Astromaterials Research Group at
NASA Johnson Space Center for their assistance with the analysis of our
samples.
NR 39
TC 2
Z9 2
U1 0
U2 28
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 1473-5504
EI 1475-3006
J9 INT J ASTROBIOL
JI Int. J. Astrobiol.
PD APR
PY 2013
VL 12
IS 2
BP 123
EP 134
DI 10.1017/S1473550412000493
PG 12
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 125FV
UT WOS:000317525900003
ER
PT J
AU Henderson, DS
L'Ecuyer, T
Stephens, G
Partain, P
Sekiguchi, M
AF Henderson, David S.
L'Ecuyer, Tristan
Stephens, Graeme
Partain, Phil
Sekiguchi, Miho
TI A Multisensor Perspective on the Radiative Impacts of Clouds and
Aerosols
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID ENERGY SYSTEM CERES; BUDGET EXPERIMENT; CIRRUS CLOUDS; CLIMATE-RESEARCH;
MODIS; TOP; ATMOSPHERE; ISCCP; DISTRIBUTIONS; VALIDATION
AB The launch of CloudSat and Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) in 2006 provided the first opportunity to incorporate information about the vertical distribution of cloud and aerosols directly into global estimates of atmospheric radiative heating. Vertical profiles of radar and lidar backscatter from CloudSat's Cloud Profiling Radar (CPR) and the Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) aboard CALIPSO naturally complement Moderate Resolution Imaging Spectroradiometer (MODIS) radiance measurements, providing a nearly complete depiction of the cloud and aerosol properties that are essential for deriving high-vertical-resolution profiles of longwave (LW) and shortwave (SW) radiative fluxes and heating rates throughout the atmosphere. This study describes a new approach for combining vertical cloud and aerosol information from CloudSat and CALIPSO with MODIS data to assess impacts of clouds and aerosols on top-of-atmosphere (TOA) and surface radiative fluxes. The resulting multisensor cloud-aerosol product is used to document seasonal and annual mean distributions of cloud and aerosol forcing globally from June 2006 through April 2011. Direct comparisons with Clouds and the Earth's Radiant Energy System (CERES) TOA fluxes exhibit a close correlation, with improved errors relative to CloudSat-only products. Sensitivity studies suggest that remaining uncertainties in SW fluxes are dominated by uncertainties in CloudSat liquid water content estimates and that the largest sources of LW flux uncertainty are prescribed surface temperature and lower-tropospheric humidity. Globally and annually averaged net TOA cloud radiative effect is found to b -18.1 W m(-2). The global, annual mean aerosol direct radiative effect is found to be -1.6 +/- 0.5 W m(-2) (-2.5 +/- 0.8 W m(-2) if only clear skies over the ocean are considered), which, surprisingly, is more consistent with past modeling studies than with observational estimates that were based on passive sensors.
C1 [Henderson, David S.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[L'Ecuyer, Tristan] Univ Wisconsin, Dept Atmospher & Ocean Sci, Madison, WI USA.
[Stephens, Graeme] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Partain, Phil] Colorado State Univ, Cooperat Inst Res Atmosphere, Ft Collins, CO 80523 USA.
[Sekiguchi, Miho] Tokyo Univ Marine Sci & Technol, Tokyo, Japan.
RP Henderson, DS (reprint author), Colorado State Univ, 1371 Campus Delivery, Ft Collins, CO 80523 USA.
EM henderson@atmos.colostate.edu
RI L'Ecuyer, Tristan/C-7040-2013; L'Ecuyer, Tristan/E-5607-2012
OI L'Ecuyer, Tristan/0000-0002-7584-4836
FU NASA CloudSat Mission Grants [NAS5-99237, NASA JPL 1439268]
FX This research was supported by NASA CloudSat Mission Grants NAS5-99237
and NASA JPL 1439268. The authors thank the staff at the CloudSat Data
Processing Center (DPC) for their help in data processing. The authors
also thank Norm Wood and Colette Heald for assisting with CALIPSO data.
All CloudSat data presented here were acquired through the DPC and at
the time of writing could be accessed online
(http://www.cloudsat.cira.colostate.edu). CALIPSO data were obtained
online from the ASDC (http://eosweb.larc.nasa.gov).
NR 58
TC 36
Z9 36
U1 3
U2 47
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1558-8424
J9 J APPL METEOROL CLIM
JI J. Appl. Meteorol. Climatol.
PD APR
PY 2013
VL 52
IS 4
BP 853
EP 871
DI 10.1175/JAMC-D-12-025.1
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 128EX
UT WOS:000317753000008
ER
PT J
AU Yoo, JM
Won, YI
Jeong, MJ
Kim, KM
Shin, DB
Lee, YR
Cho, YJ
AF Yoo, Jung-Moon
Won, Young-In
Jeong, Myeong-Jae
Kim, Kyu-Myong
Shin, Dong-Bin
Lee, Yu-Ri
Cho, Young-Jun
TI Intensity of climate variability derived from the satellite and MERRA
reanalysis temperatures: AO, ENSO, and QBO
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE MERRA; AMSU; Climate indices; AO; ENSO; QBO
ID LAND-SURFACE TEMPERATURE; EL-NINO; ARCTIC OSCILLATION; STRATOSPHERIC
TEMPERATURE; EXTRATROPICAL CIRCULATION; BAROCLINIC INSTABILITY;
SOUTHERN-OSCILLATION; BIENNIAL OSCILLATION; GROUND MEASUREMENTS;
CHANGING CLIMATE
AB Satellite measurements (Atmospheric InfraRed Sounder/Advanced Microwave Sounding Unit-A, MODerate resolution Imaging Spectroradiometer) and the Modern Era Retrospective-analysis for Research and Applications (MERRA) reanalysis have been utilized to analyze the relative influence of the climate variability (AO: Arctic Oscillation, ENSO: El Nino-Southern Oscillation, QBO: Quasi-Biennial Oscillation) on the zonal-mean temperature and wind variations over the globe from September 2002 to August 2011. We also extended the usage of MERRA data for the period of 1979-2011; furthermore, three climate indices of AO, NINO3.4, and QBO were used as the corresponding climate indicators. The correlations between the temperature anomalies and the climate indices indicate that the tropospheric temperature variability in the mid-latitude (30-60N) linked to both AO and ENSO has been more pronounced over ocean than over land. However, the low stratospheric temperature variability in the mid-latitude is mainly associated with ENSO and QBO. The north-south symmetric patterns over the globe are seen in the wind anomaly distributions for ENSO and QBO, but not for AO. The ENSO events are globally vigorous but also localized during the recent 9 years compared with those based on the period of 1979-2011. The tropospheric warming and stratospheric cooling phenomena during this period are more remarkable in the recent 9 years, although according to IPCC (2012). their linkage to the ENSO variability is still uncertain. The ENSO is found to have more significant impact on the tropospheric and low stratosphere temperature variability over the tropics in the recent period, consistent with more active zonal wind meridional circulations. The discrepancies between satellite observations and MERRA are also discussed. The estimated relative impact of the three major concurrent large-scale climate phenomena on regional temperature variability can be of great use in its long-term predictability. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Yoo, Jung-Moon; Lee, Yu-Ri] Ewha Womans Univ, Dept Sci Educ, Seoul 120750, South Korea.
[Won, Young-In] NASA GSFC, Wyle IS, Greenbelt, MD 20771 USA.
[Jeong, Myeong-Jae] Gangneung Wonju Natl Univ, Dept Atmospher & Environm Sci, Gangwondo 210702, South Korea.
[Kim, Kyu-Myong] Morgan State Univ, Baltimore, MD 21251 USA.
[Shin, Dong-Bin; Lee, Yu-Ri; Cho, Young-Jun] Yonsei Univ, Dept Atmospher Sci, Seoul 120749, South Korea.
RP Yoo, JM (reprint author), Ewha Womans Univ, Dept Sci Educ, Seoul 120750, South Korea.
EM yjm@ewha.ac.kr
RI Kim, Kyu-Myong/G-5398-2014
FU National Research Foundation of Korea (NRF); Korea government (MEST)
[20120000858]; Korean Ministry of Environment
FX This work was supported by the National Research Foundation of Korea
(NRF) grant funded by Korea government (MEST) (No. 20120000858) and the
Korean Ministry of Environment as part of the Eco-Innovation Project. We
would like to thank Goddard Earth Sciences Data Information and Services
Center (GES DISC) for providing the AIRS/AMSU and MERRA data. We are
also grateful to NASA Land Process Distributed Active Archive Center (LP
DAAC) for providing the MODIS LST data.
NR 66
TC 2
Z9 2
U1 2
U2 9
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1364-6826
J9 J ATMOS SOL-TERR PHY
JI J. Atmos. Sol.-Terr. Phys.
PD APR
PY 2013
VL 95-96
BP 15
EP 27
DI 10.1016/j.jastp.2013.01.002
PG 13
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA 122OB
UT WOS:000317326300002
ER
PT J
AU Choi, CJ
Seo, M
Choi, WS
Kim, KS
Youn, SA
Lindsey, T
Choi, YJ
Kim, CM
AF Choi, Chang-Jin
Seo, Min
Choi, Whan-Seok
Kim, Kyung-Soo
Youn, Sang-Ah
Lindsey, Tony
Choi, Yun-Jung
Kim, Churl-Min
TI Relationship Between Serum 25-Hydroxyvitamin D and Lung Function Among
Korean Adults in Korea National Health and Nutrition Examination Survey
(KNHANES), 2008-2010
SO JOURNAL OF CLINICAL ENDOCRINOLOGY & METABOLISM
LA English
DT Article
ID VITAMIN-D DEFICIENCY; RISK-FACTOR; DISEASE; TUBERCULOSIS; ASSOCIATION;
SUPPLEMENTATION; METAANALYSIS; INFECTIONS; PREVENTION; GUIDELINE
AB Context: The relationship between vitamin D status and pulmonary function has not been investigated for an East Asian population.
Objective: The aim of the present study was to examine the relationship of serum 25-hydroxyvitamin D [25(OH)D] with lung function in Korean adults.
Design and Setting: The analysis used data from the Korea National Health and Nutrition Examination Survey (KNHANES), a cross-sectional survey of Korean civilians, conducted from 2008 to 2010.
Participants: A total of 10 096 people aged 19 years and older were selected from 16 administrative districts in South Korea.
Main Outcome Measures: Serum 25(OH) D levels with lung function [forced expiratory volume in 1 second (FEV1) and forced vital capacity (FVC)].
Results: Serum 25(OH) D concentration was positively associated with lung function after controlling for age, sex, height, and season. For FEV1 and FVC, the differences between top and bottom quartiles in 25(OH) D were 51 mL (SE, 17 mL, P trend <.001) and 58 mL (SE, 20 mL, P trend <.005) greater volume, respectively. Association of serum 25(OH) D with FEV1 and FVC was only slightly attenuated after adjustment for body mass index, lifestyle and socioeconomic factors, and respiratory illness. The subjects with a history of pulmonary tuberculosis showed a much higher increase in FEV1; the difference between top and bottom quartiles in 25(OH) D was 229 mL (SE, 87 mL, P trend <.01).
Conclusion: Serum 25(OH) D levels have a positive correlation with pulmonary function. This relationship appears prominent in subjects with susceptibility to pulmonary tuberculosis. (J Clin Endocrinol Metab 98: 1703-1710, 2013)
C1 [Choi, Chang-Jin; Choi, Whan-Seok; Kim, Kyung-Soo; Youn, Sang-Ah; Kim, Churl-Min] Catholic Univ Korea, Dept Family Med, Seoul St Marys Hosp, Coll Med, Seoul 137701, South Korea.
[Seo, Min] Dankook Univ, Coll Med, Dept Parasitol, Cheonan 330715, South Korea.
[Lindsey, Tony] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Choi, Yun-Jung] Metabolex Inc, Hayward, CA 94545 USA.
RP Kim, CM (reprint author), Catholic Univ Korea, Dept Family Med, Seoul St Marys Hosp, Coll Med, 222 Banpo Daero, Seoul 137701, South Korea.
EM musofm@catholic.ac.kr
NR 32
TC 17
Z9 18
U1 0
U2 4
PU ENDOCRINE SOC
PI CHEVY CHASE
PA 8401 CONNECTICUT AVE, SUITE 900, CHEVY CHASE, MD 20815-5817 USA
SN 0021-972X
J9 J CLIN ENDOCR METAB
JI J. Clin. Endocrinol. Metab.
PD APR
PY 2013
VL 98
IS 4
BP 1703
EP 1710
DI 10.1210/jc.2012-3901
PG 8
WC Endocrinology & Metabolism
SC Endocrinology & Metabolism
GA 120TJ
UT WOS:000317195600076
PM 23533242
ER
PT J
AU Mallick, K
Jarvis, A
Fisher, JB
Tu, KP
Boegh, E
Niyogi, D
AF Mallick, Kaniska
Jarvis, Andrew
Fisher, Joshua B.
Tu, Kevin P.
Boegh, Eva
Niyogi, Dev
TI Latent Heat Flux and Canopy Conductance Based on Penman-Monteith,
Priestley-Taylor Equation, and Bouchet's Complementary Hypothesis
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID RADIOMETRIC SURFACE-TEMPERATURE; CONVECTIVE BOUNDARY-LAYER;
ENERGY-BALANCE CLOSURE; CARBON-DIOXIDE; SENSIBLE HEAT; WATER-VAPOR;
REGIONAL EVAPOTRANSPIRATION; STOMATAL CONDUCTANCE; BIOSPHERE MODEL; PAN
EVAPORATION
AB A novel method is presented to analytically resolve the terrestrial latent heat flux (lambda E) and conductances (boundary layer g(B) and surface g(S)) using net radiation (R-N), ground heat flux (G), air temperature (T-a), and relative humidity (RH). This method consists of set of equations where the two unknown internal state variables (g(B) and g(S)) were expressed in terms of the known core variables, combining diffusion equations, the Penman-Monteith equation, the Priestley-Taylor equation, and Bouchet's complementary hypothesis. Estimated lambda E is validated with the independent eddy covariance lambda E observations over Soil Moisture Experiment 2002 (SMEX-02); the Global Energy and Water Cycle Experiment (GEWEX) Continental-Scale International Project (GCIP) selected sites from FLUXNET and tropics eddy flux, representing four climate zones (tropics, subtropics, temperate, and cold); and multiple biomes. The authors find a RMSE of 23.8-54.6 W m(-2) for hourly lambda E over SMEX-02 and GCIP and 23.8-29.0 W m(-2) for monthly lambda E over the FLUXNET and tropics. Observational and modeled evidence in the reduction in annual evaporation (E) pattern on the order of 33% from 1999 to 2006 was found in central Amazonia. Retrieved g(S) responded to vapor pressure deficit, measured lambda E, and gross photosynthesis in a theoretically robust behavior. However, the current scheme [Penman-Monteith-Bouchet-Lhomme (PMBL)] showed some overestimation of lambda E in limited soil moisture regimes. PMBL provides similar results when compared with another Priestley-Taylor-based lambda E estimation approach [Priestley-Taylor-Jet Propulsion Laboratory (PT-JPL)] but with the advantage of having the conductances analytically recovered.
C1 [Mallick, Kaniska; Fisher, Joshua B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Jarvis, Andrew] Univ Lancaster, Lancaster Environm Ctr, Lancaster, England.
[Tu, Kevin P.] Pioneer HiBred Int Inc, Woodland, CA USA.
[Boegh, Eva] Roskilde Univ, Dept Environm Social & Spatial Change, Roskilde, Denmark.
[Niyogi, Dev] Purdue Univ, Dept Agron, W Lafayette, IN 47907 USA.
[Niyogi, Dev] Purdue Univ, Dept Earth & Atmospher & Planetary Sci, W Lafayette, IN 47907 USA.
RP Mallick, K (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM kaniska.mallick@gmail.com
OI Fisher, Joshua/0000-0003-4734-9085
FU Jet Propulsion Laboratory's Research and Technology Development Climate
Strategic Initiative; Natural Environment Research Council, United
Kingdom [NEE0191531]
FX We gratefully acknowledge NSIDC and CEOP for making the SMEX-02 and GCIP
data available. K. M. acknowledges the comments from Dr. Bill Kustas,
HRSL, USDA, and Dr. B. K. Bhattacharya, Space Applications Centre,
India. We also acknowledge the site PIs of the tropical forest eddy
covariance network and FLUXNET network for the data permission. We
acknowledge Dr. John Prueger for permitting us to use the SMEX-02. K. M.
also acknowledges Dr. Junhak Lee for his help in map preparation and the
postdoctoral research fellowship from the Jet Propulsion Laboratory's
Research and Technology Development Climate Strategic Initiative. D.N.
benefited in part through NSF CAREER (AGS-0847472, Anjuli Bamzai), USDA
NIFA 2011-68002-30220, and NSF INTEROP OCI 0753116. KM was partly funded
by the Natural Environment Research Council, United Kingdom, Grant
NEE0191531. Three anonymous reviewers are also acknowledged for their
helpful comments. The research was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration.
NR 76
TC 11
Z9 11
U1 1
U2 39
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 APR
PY 2013
VL 14
IS 2
BP 419
EP 442
DI 10.1175/JHM-D-12-0117.1
PG 24
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 125SI
UT WOS:000317561200003
ER
PT J
AU Kirstetter, PE
Hong, Y
Gourley, JJ
Schwaller, M
Petersen, W
Zhang, J
AF Kirstetter, Pierre-Emmanuel
Hong, Y.
Gourley, J. J.
Schwaller, M.
Petersen, W.
Zhang, J.
TI Comparison of TRMM 2A25 Products, Version 6 and Version 7, with
NOAA/NSSL Ground Radar-Based National Mosaic QPE
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID SURFACE REFERENCE TECHNIQUE; RAIN-PROFILING ALGORITHM; PRECIPITATION
RADAR; SATELLITE; VALIDATION
AB Characterization of the error associated with satellite rainfall estimates is a necessary component of deterministic and probabilistic frameworks involving spaceborne passive and active microwave measurements for applications ranging from water budget studies to forecasting natural hazards related to extreme rainfall events. The authors focus here on the relative error structure of Tropical Rainfall Measurement Mission (TRMM) precipitation radar (PR) quantitative precipitation estimation (QPE) at the ground by comparison of 2A25 products with reference values derived from NOAA/NSSL's ground radar-based National Mosaic and QPE system (NMQ/Q2). The primary contribution of this study is to compare the new 2A25, version 7 (V7), products that were recently released as a replacement of version 6 (V6). Moreover, the authors supply uncertainty estimates of the rainfall products so that they may be used in a quantitative manner for applications like hydrologic modeling. This new version is considered superior over land areas and will likely be the final version for TRMM PR rainfall estimates. Several aspects of the two versions are compared and quantified, including rainfall rate distributions, systematic biases, and random errors. All analyses indicate that V7 is in closer agreement with the reference rainfall compared to V6.
C1 [Kirstetter, Pierre-Emmanuel; Hong, Y.] Univ Oklahoma, Sch Civil Engn & Environm Sci, Norman, OK 73019 USA.
[Kirstetter, Pierre-Emmanuel; Gourley, J. J.; Zhang, J.] NOAA, Natl Severe Storms Lab, Norman, OK 73069 USA.
[Kirstetter, Pierre-Emmanuel; Hong, Y.] Natl Weather Ctr, Atmospher Radar Res Ctr, Norman, OK 73072 USA.
[Schwaller, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Petersen, W.] NASA, Wallops Flight Facil, Wallops Isl, VA USA.
RP Hong, Y (reprint author), Natl Weather Ctr, Atmospher Radar Res Ctr, 120 David L Boren Blvd,Suite 4610, Norman, OK 73072 USA.
EM yanghong@ou.edu
RI Kirstetter, Pierre/E-2305-2013; Hong, Yang/D-5132-2009; Gourley,
Jonathan/C-7929-2016; Measurement, Global/C-4698-2015
OI Kirstetter, Pierre/0000-0002-7381-0229; Hong, Yang/0000-0001-8720-242X;
Gourley, Jonathan/0000-0001-7363-3755;
FU NASA Global Precipitation Measurement mission Ground Validation
Management
FX We are very much indebted to the team responsible for the NMQ/Q2
products, especially Carrie Langston. We want to thank two anonymous
reviewers, whose comments were very useful in improving the manuscript.
This work was funded by a postdoctoral grant from the NASA Global
Precipitation Measurement mission Ground Validation Management.
NR 34
TC 30
Z9 32
U1 0
U2 16
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 APR
PY 2013
VL 14
IS 2
BP 661
EP 669
DI 10.1175/JHM-D-12-030.1
PG 9
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 125SI
UT WOS:000317561200017
ER
PT J
AU Sanghavi, S
Natraj, V
AF Sanghavi, Suniti
Natraj, Vijay
TI Using analytic derivatives to assess the impact of phase function
Fourier decomposition technique on the accuracy of a radiative transfer
model
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Fourier decomposition; Legendre expansion; Aerosol phase function;
Interpolation error; Jacobian matrix
ID DISCRETE SPACE THEORY; POLARIZED-LIGHT; SCATTERING; RELEVANT; MATRIX
AB Fourier decomposition of the phase function is essential to decouple the azimuthal component of the radiative transfer equation for multiple scattering calculations. This decomposition can be carried out by means of a direct numerical method based on the definition of the Fourier transform (numFT), or by an expansion of the phase function in terms of spherical Legendre polynomials (sphFT). numFT requires interpolation of the phase function between discrete angles, leading to spurious errors in the final computations. This error is difficult to quantify by means of intensity-only computations, since it is hard to determine the absolute accuracy of any given approach. We show that a linearization (analytic computation of derivatives) of the intensity with respect to parameters governing the phase function can be compared against results using the finite difference method, thereby providing a self-consistency test for characterizing and quantifying the error.
We have applied this approach to two linearized versions of the Matrix Operator Method, which are identical in all respects except that one uses numFT while the other uses sphFT. In both cases, we compute the derivatives of the intensity with respect to aerosol 'parameters governing scattering in the simulated atmosphere. Comparison of the derivatives against their finite difference estimates shows a reduction of error by several orders of magnitude when Legendre polynomials are employed. We have also examined the effect of the angular resolution of the phase function on the error due to the numFT technique. A general reduction of error is seen with increasing angular resolution, indicating that interpolation is indeed the major error source. Also, we have pointed out a related source of error in numFT computations that occurs when Fourier decomposition is carried out on the composite phase function of a layer consisting of more than one scatterer. We conclude that an expansion of the phase function in terms of Legendre polynomials eliminates the need for interpolation, making it the more suitable method for linearization of radiative transfer, especially with respect to aerosol properties. (C) 2013 Elsevier Ltd. All rights reserved.
C1 [Sanghavi, Suniti; Natraj, Vijay] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Sanghavi, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM suniti.sanghavi@gmail.com
NR 18
TC 2
Z9 2
U1 1
U2 3
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD APR
PY 2013
VL 119
BP 137
EP 149
DI 10.1016/j.jqsrt.2012.12.028
PG 13
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 126QK
UT WOS:000317636100013
ER
PT J
AU Marchi, S
Bottke, WF
Cohen, BA
Wunnemann, K
Kring, DA
McSween, HY
De Sanctis, MC
O'Brien, DP
Schenk, P
Raymond, CA
Russell, CT
AF Marchi, S.
Bottke, W. F.
Cohen, B. A.
Wuennemann, K.
Kring, D. A.
McSween, H. Y.
De Sanctis, M. C.
O'Brien, D. P.
Schenk, P.
Raymond, C. A.
Russell, C. T.
TI High-velocity collisions from the lunar cataclysm recorded in asteroidal
meteorites
SO NATURE GEOSCIENCE
LA English
DT Article
ID LATE HEAVY BOMBARDMENT; INNER SOLAR-SYSTEM; PARENT BODY; IMPACT;
CONSTRAINTS; HISTORY; VESTA; AGES; CRATER; BELT
AB The Moon experienced an intense period of impacts about 4 Gyr ago. This cataclysm is thought to have affected the entire inner Solar System and has been constrained by the radiometric dating of lunar samples: Ar-40-Ar-39 ages reflect the heating and degassing of target rocks by large basin-forming impacts on the Moon. Radiometric dating of meteorites from Vesta and the H-chondrite parent body also shows numerous Ar-40-Ar-39 ages between 3.4 and 4.1 Gyr ago, despite a different dynamical context, where impacts typically occur at velocities too low to reset geochronometers. Here we interpret the Ar-40-Ar-39 age record in meteorites to reflect unusually high impact velocities exceeding 10 km s(-1). Compared with typical impact velocities for main-belt asteroids of about 5 km s(-1), these collisions would produce 100-1,000 times more highly heated material by volume. We propose that the Ar-40-Ar-39 ages between 3.4 and 4.1 Gyr ago from Vesta, the H-chondrite parent body and the Moon record impacts from numerous main-belt asteroids that were driven onto high-velocity and highly eccentric orbits by the effects of the late migration of the giant planets. We suggest that the bombardment persisted for many hundreds of millions of years and affected most inner Solar System bodies.
C1 [Marchi, S.; Bottke, W. F.] NASA Lunar Sci Inst, SW Res Inst, Boulder, CO 80302 USA.
[Cohen, B. A.] NASA Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
[Wuennemann, K.] Museum Nat Kunde, D-10115 Berlin, Germany.
[Kring, D. A.] NASA Lunar Sci Inst, USRA Lunar & Planetary Inst, Houston, TX 77058 USA.
[McSween, H. Y.] Univ Tennessee, Knoxville, TN 37996 USA.
[De Sanctis, M. C.] Ist Nazl Astrofis, I-00133 Rome, Italy.
[O'Brien, D. P.] Planetary Sci Inst, Tucson, AZ 85719 USA.
[Schenk, P.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Russell, C. T.] Univ Calif Los Angeles, Los Angeles, CA 90024 USA.
RP Marchi, S (reprint author), NASA Lunar Sci Inst, SW Res Inst, Boulder, CO 80302 USA.
EM marchi@boulder.swri.edu
RI De Sanctis, Maria Cristina/G-5232-2013
OI De Sanctis, Maria Cristina/0000-0002-3463-4437
FU NASA Lunar Science Institute (Center for Lunar Origin and Evolution at
the Southwest Research Institute in Boulder, Colorado- NASA)
[NNA09DB32A]; NASA Lunar Science Institute (Center for Lunar Science and
Exploration at the Lunar and Planetary Institute in Houston, Texas);
Helmholtz-Alliance 'Planetary Evolution and Life'; Agenzia Spaziale
Italiana; NASA High-End Computing (HEC) Program through the NASA
Advanced Supercomputing (NAS) Division at Ames Research Center
FX We thank D. Bogard, B. Ivanov, A. Morbidelli, D. Nesvorny, T. Swindle
and the Dawn Science Team for helpful discussions and insightful
comments. The contributions of S. M., W. F. B., B. A. C. and D. A. K.
were supported by the NASA Lunar Science Institute (Center for Lunar
Origin and Evolution at the Southwest Research Institute in Boulder,
Colorado- NASA Grant NNA09DB32A; Center for Lunar Science and
Exploration at the Lunar and Planetary Institute in Houston, Texas). The
contribution of K. W. was funded by the Helmholtz-Alliance 'Planetary
Evolution and Life'. D.P.O'B. and P. S. thank the NASA Dawn at Vesta
Participating Scientist Program. The contribution of M. C. D. S. was
partially supported by Agenzia Spaziale Italiana. 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 47
TC 44
Z9 44
U1 2
U2 30
PU NATURE PUBLISHING GROUP
PI NEW YORK
PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA
SN 1752-0894
J9 NAT GEOSCI
JI Nat. Geosci.
PD APR
PY 2013
VL 6
IS 4
BP 303
EP 307
DI 10.1038/NGEO1769
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 117IJ
UT WOS:000316946500020
ER
PT J
AU Larsson, R
McKay, CP
AF Larsson, Richard
McKay, Christopher P.
TI Timescale for oceans in the past of Titan
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Titan; Surface; Methane ocean; Planetary evolution
ID ATMOSPHERE; LAKES; CYCLE
AB We estimate the past extent of liquid on the surface of Titan as a function of time assuming the current rate of destruction of methane and no sources or subsurface sinks. As methane increases for increasing past time the polar lakes expand equatorward. We use a spherical harmonics model for the surface topography to compute the fraction of the surface covered as the methane inventory increases. We find that substantial parts of the equator would have been flooded by a polar ocean 300 million years ago and that the equator would have been connected to a global ocean 600 million years ago. This provides one possible explanation for the fluvial features seen at the equator on Titan. (C) 2012 Elsevier Ltd. All rights reserved.
C1 [Larsson, Richard] Lulea Univ Technol, Dept Comp Sci Elect & Space Engn, SE-98128 Kiruna, Sweden.
[McKay, Christopher P.] NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Moffett Field, CA 94035 USA.
RP Larsson, R (reprint author), Lulea Univ Technol, Dept Comp Sci Elect & Space Engn, Space Campus 1, SE-98128 Kiruna, Sweden.
EM ric.larsson@gmail.com
OI Larsson, Richard/0000-0001-6719-723X
NR 29
TC 6
Z9 6
U1 0
U2 9
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 APR
PY 2013
VL 78
BP 22
EP 24
DI 10.1016/j.pss.2012.12.001
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 128YX
UT WOS:000317806700002
ER
PT J
AU Scott, JM
Koelwyn, GJ
Hornsby, WE
Khouri, M
Peppercorn, J
Douglas, PS
Jones, LW
AF Scott, Jessica M.
Koelwyn, Graeme J.
Hornsby, Whitney E.
Khouri, Michel
Peppercorn, Jeffrey
Douglas, Pamela S.
Jones, Lee W.
TI Exercise Therapy as Treatment for Cardiovascular and Oncologic Disease
After a Diagnosis of Early-Stage Cancer
SO SEMINARS IN ONCOLOGY
LA English
DT Review
ID ANDROGEN DEPRIVATION THERAPY; RANDOMIZED CONTROLLED-TRIAL; C-REACTIVE
PROTEIN; ADVANCED PROSTATE-CANCER; EARLY BREAST-CANCER; CELL
LUNG-CANCER; PHYSICAL-ACTIVITY; POSTMENOPAUSAL WOMEN; OXIDATIVE STRESS;
METABOLIC SYNDROME
C1 [Scott, Jessica M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Scott, Jessica M.] Univ Space Res Assoc, Houston, TX USA.
[Koelwyn, Graeme J.] Univ British Columbia, Sch Hlth & Exercise Sci, Kelowna, BC, Canada.
[Hornsby, Whitney E.; Khouri, Michel; Peppercorn, Jeffrey; Douglas, Pamela S.; Jones, Lee W.] Duke Univ, Med Ctr, Durham, NC USA.
RP Jones, LW (reprint author), Duke Canc Inst, Box 3085, Durham, NC 27710 USA.
EM lee.w.jones@duke.edu
FU National Institutes of Health [CA143254, CA142566, CA138634, CA133895]
FX L.W.J. was supported by National Institutes of Health grants no.
CA143254, CA142566, CA138634, and CA133895 and with funds from George
and Susan Beischer. The other authors report no potential conflicts of
interest.
NR 118
TC 16
Z9 16
U1 2
U2 11
PU W B SAUNDERS CO-ELSEVIER INC
PI PHILADELPHIA
PA 1600 JOHN F KENNEDY BOULEVARD, STE 1800, PHILADELPHIA, PA 19103-2899 USA
SN 0093-7754
J9 SEMIN ONCOL
JI Semin. Oncol.
PD APR
PY 2013
VL 40
IS 2
BP 218
EP 228
DI 10.1053/j.seminoncol.2013.01.001
PG 11
WC Oncology
SC Oncology
GA 129VA
UT WOS:000317870900010
PM 23540747
ER
PT J
AU Wiens, RC
Maurice, S
Lasue, J
Forni, O
Anderson, RB
Clegg, S
Bender, S
Blaney, D
Barraclough, BL
Cousin, A
Deflores, L
Delapp, D
Dyar, MD
Fabre, C
Gasnault, O
Lanza, N
Mazoyer, J
Melikechi, N
Meslin, PY
Newsom, H
Ollila, A
Perez, R
Tokar, RL
Vaniman, D
AF Wiens, R. C.
Maurice, S.
Lasue, J.
Forni, O.
Anderson, R. B.
Clegg, S.
Bender, S.
Blaney, D.
Barraclough, B. L.
Cousin, A.
Deflores, L.
Delapp, D.
Dyar, M. D.
Fabre, C.
Gasnault, O.
Lanza, N.
Mazoyer, J.
Melikechi, N.
Meslin, P. -Y.
Newsom, H.
Ollila, A.
Perez, R.
Tokar, R. L.
Vaniman, D.
TI Pre-flight calibration and initial data processing for the Chem Cam
laser-induced breakdown spectroscopy instrument on the Mars Science
Laboratory rover
SO SPECTROCHIMICA ACTA PART B-ATOMIC SPECTROSCOPY
LA English
DT Article
DE Laser-induced breakdown spectroscopy; LIBS; Mars; Curiosity rover;
ChemCam
ID PLIOCENE MACUSANI VOLCANICS; SE PERU; PLASMA; SULFUR; EXPLORATION;
ATMOSPHERE; MINERALOGY; CHEMISTRY; EMISSION; OUTCROPS
AB The ChemCam instrument package on the Mars Science Laboratory rover, Curiosity, is the first planetary science instrument to employ laser-induced breakdown spectroscopy (LIBS) to determine the compositions of geological samples on another planet. Pre-processing of the spectra involves subtracting the ambient light background, removing noise, removing the electron continuum, calibrating for the wavelength, correcting for the variable distance to the target, and applying a wavelength-dependent correction for the instrument response. Further processing of the data uses multivariate and univariate comparisons with a LIBS spectral library developed prior to launch as well as comparisons with several on-board standards post-landing. The level-2 data products include semi-quantitative abundances derived from partial least squares regression.
A LIBS spectral library was developed using 69 rock standards in the form of pressed powder disks, glasses, and ceramics to minimize heterogeneity on the scale of the observation (350-550 mu m dia.). The standards covered typical compositional ranges of igneous materials and also included sulfates, carbonates, and phyllosilicates. The provenance and elemental and mineralogical compositions of these standards are described. Spectral characteristics of this data set are presented, including the size distribution and integrated irradiances of the plasmas, and a proxy for plasma temperature as a function of distance from the instrument. Two laboratory-based clones of ChemCam reside in Los Alamos and Toulouse for the purpose of adding new spectra to the database as the need arises. Sensitivity to differences in wavelength correlation to spectral channels and spectral resolution has been investigated, indicating that spectral registration needs to be within half a pixel and resolution needs to match within 1.5 to 2.6 pixels. Absolute errors are tabulated for derived compositions of each major element in each standard using PLS regression. Sources of errors are investigated and discussed, and methods for improving the analytical accuracy of compositions derived from ChemCam spectra are discussed. Published by Elsevier B.V.
C1 [Wiens, R. C.; Clegg, S.; Cousin, A.; Delapp, D.; Lanza, N.] Los Alamos Natl Lab, Los Alamos, NM 87544 USA.
[Maurice, S.; Lasue, J.; Forni, O.; Cousin, A.; Gasnault, O.; Meslin, P. -Y.] Inst Rech Astrophys & Planetol, Toulouse, France.
[Anderson, R. B.] US Geol Survey, Flagstaff, AZ 86001 USA.
[Bender, S.; Barraclough, B. L.; Tokar, R. L.; Vaniman, D.] Planetary Sci Inst, Tucson, AZ USA.
[Blaney, D.; Deflores, L.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Dyar, M. D.] Mt Holyoke Coll, S Hadley, MA 01075 USA.
[Fabre, C.] Georessources, Nancy, France.
[Mazoyer, J.] Observ Paris, LESIA, Meudon, France.
[Melikechi, N.] Delaware State Univ, Dover, DE USA.
[Newsom, H.; Ollila, A.] Univ New Mexico, Albuquerque, NM 87131 USA.
[Perez, R.] Ctr Natl Etud Spatiale, Toulouse, France.
RP Wiens, RC (reprint author), Los Alamos Natl Lab, POB 1663, Los Alamos, NM 87544 USA.
EM rwiens@lanl.gov
RI Gasnault, Olivier/F-4327-2010;
OI Gasnault, Olivier/0000-0002-6979-9012; Forni,
Olivier/0000-0001-6772-9689; Clegg, Sam/0000-0002-0338-0948
FU NASA Mars Program Office for ChemCam; CNES
FX The ChemCam team is grateful for support from the NASA Mars Program
Office for ChemCam, and from CNES. We also gratefully acknowledge the
Los Alamos National Laboratory's laboratory-directed research and
development exploratory research (LDRD-ER) program for supporting early
MVA studies. Many people supported the ChemCam instrument that was used
to carry out these studies, and we are particularly grateful to other
ChemCam team members who supported this work B. Banisadr is thanked for
his contributions to the total emission studies.
NR 52
TC 74
Z9 76
U1 7
U2 67
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0584-8547
J9 SPECTROCHIM ACTA B
JI Spectroc. Acta Pt. B-Atom. Spectr.
PD APR 1
PY 2013
VL 82
BP 1
EP 27
DI 10.1016/j.sab.2013.02.003
PG 27
WC Spectroscopy
SC Spectroscopy
GA 124DG
UT WOS:000317443400001
ER
PT J
AU Lock, JA
Ball, DW
AF Lock, James A.
Ball, David W.
TI Why Is the Sky Blue?
SO SPECTROSCOPY
LA English
DT Article
AB There are many ways in which spectroscopy is relevant to matters celestial. Here, we'll tackle one of the classic ones, one to which many know the simple explanation, but few know the details. In this column, we'll go over the details.
C1 [Lock, James A.; Ball, David W.] Cleveland State Univ, Cleveland, OH 44115 USA.
[Lock, James A.] NASA, Glenn Res Ctr, Cleveland, OH USA.
RP Lock, JA (reprint author), Cleveland State Univ, Cleveland, OH 44115 USA.
EM d.ball@csuohio.edu
NR 2
TC 0
Z9 0
U1 2
U2 12
PU ADVANSTAR COMMUNICATIONS INC
PI DULUTH
PA 131 W 1ST STREET, DULUTH, MN 55802 USA
SN 0887-6703
J9 SPECTROSCOPY-US
JI Spectroscopy
PD APR
PY 2013
VL 28
IS 4
BP 12
EP 17
PG 6
WC Spectroscopy
SC Spectroscopy
GA 125RQ
UT WOS:000317559400003
ER
PT J
AU Griffith, P
Williamson, R
AF Griffith, Peter
Williamson, Ruth
TI Interview with Dr Peter Griffith
SO CARBON MANAGEMENT
LA English
DT Editorial Material
AB Dr Peter Griffith received his PhD in Ecology from the University of Georgia (GA, USA), his MSc in Marine, Estuarine and Environmental Science from the University of Maryland (MD, USA) and a BSc with Honors in Botany and Zoology from Duke University (NC, USA). Dr Griffith is now the founding director of the National Aeronautics and Space Administration (NASA) Carbon Cycle and Ecosystems Office, supporting the North American Carbon Program, a component of the US Global Change Research Program designed to quantify continental-scale carbon sources and sinks in North America, NASA's Arctic Boreal Vulnerability Experiment, and the NASA Carbon Cycle and Ecosystems Focus Area. As a distinguished expert in carbon cycles, Dr Griffith speaks to Ruth Williamson, Commissioning Editor of Carbon Management, about the changes in carbon cycle research throughout his career, important advances in our understanding of climate science, and important obstacles and future directions for carbon cycle scientists.
C1 [Griffith, Peter] NASA, Goddard Space Flight Ctr, Sigma Space Corp, Greenbelt, MD 20771 USA.
RP Griffith, P (reprint author), NASA, Goddard Space Flight Ctr, Sigma Space Corp, Code 618, Greenbelt, MD 20771 USA.
RI Griffith, Peter/I-1392-2016
OI Griffith, Peter/0000-0002-4267-7429
NR 7
TC 0
Z9 0
U1 0
U2 0
PU FUTURE SCI LTD
PI LONDON
PA UNITED HOUSE, 2 ALBERT PL, LONDON, N3 1QB, ENGLAND
SN 1758-3004
J9 CARBON MANAG
JI Carbon Manag.
PD APR
PY 2013
VL 4
IS 2
BP 119
EP 123
DI 10.4155/CMT.13.7
PG 5
WC Environmental Sciences; Environmental Studies
SC Environmental Sciences & Ecology
GA 114XT
UT WOS:000316777000008
ER
PT J
AU Walker, RT
Bergman, EA
Elliott, JR
Fielding, EJ
Ghods, AR
Ghoraishi, M
Jackson, J
Nazari, H
Nemati, M
Oveisi, B
Talebian, M
Walters, RJ
AF Walker, R. T.
Bergman, E. A.
Elliott, J. R.
Fielding, E. J.
Ghods, A. -R.
Ghoraishi, M.
Jackson, J.
Nazari, H.
Nemati, M.
Oveisi, B.
Talebian, M.
Walters, R. J.
TI The 2010-2011 South Rigan (Baluchestan) earthquake sequence and its
implications for distributed deformation and earthquake hazard in
southeast Iran
SO GEOPHYSICAL JOURNAL INTERNATIONAL
LA English
DT Article
DE Radar interferometry; Seismicity and tectonics; Body waves; Continental
neotectonics; Asia
ID DASHT-E-BAYAZ; EASTERN IRAN; FAULT SLIP; SURFACE DEFORMATION; ACTIVE
TECTONICS; GPS MEASUREMENTS; SATELLITE RADAR; MIDDLE-EAST; INSAR;
RELOCATION
AB We investigate the source processes and tectonic significance of two earthquakes that occurred on 2010 December 20 (M-w 6.5) and 2011 January 27 (M-w 6.2) within a desert region south of the town of Rigan, SE Iran. The two earthquakes, which we refer to as the South Rigan events, occurred close to one another at the northern margin of the Shahsavaran mountains: a mainly volcanic chain in which the potential for active faulting has not previously been considered in detail. Surface displacements mapped using SAR interferometry, multiple-event relocation analysis of epicentres, body-waveform modelling and field measurements of surface rupture together reveal that the 2010 December 20 earthquake involved an average of similar to 1.3 m right-lateral slip on a vertical fault trending similar to 210 degrees whereas the 2011 January 27 resulted from similar to 0.6 m of slip on a conjugate left-lateral fault striking similar to 310 degrees, parallel to the trend of the Shahsavaran mountains and confined within a zone of increased Coulomb stress from the earlier main shock. The main slip for the 2010 and 2011 main shocks failed to reach the surface though minor cracks and en-echelon fissures were mapped following both events. Some of the surface cracks may have been enhanced during a period of minor afterslip in the days following the 2010 main shock. Using the insights gained from our investigation of the two South Rigan earthquakes we perform a regional reconnaissance of the active faulting using SPOTS (2.5 m) satellite imagery. We show that distributed similar to N-S right-lateral faulting is widely distributed north of the Shahsavaran mountains. We also show evidence for left-lateral strike-slip faulting parallel to the Shahsavaran mountains, with a component of extension in the east and shortening in the west, which is likely to accommodate regional N-S right-lateral shearing by clockwise rotation about a vertical axis. The distributed strike-slip faulting is closely associated with the distribution of towns and villages and constitutes a continuing hazard to local populations.
C1 [Walker, R. T.; Elliott, J. R.; Walters, R. J.] Univ Oxford, Dept Earth Sci, Oxford OX1 3AN, England.
[Bergman, E. A.] Univ Colorado, Dept Phys, Ctr Imaging Earths Interior, Boulder, CO 80309 USA.
[Fielding, E. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ghods, A. -R.] IASBS, Dept Earth Sci, Zanjan, Iran.
[Ghoraishi, M.; Nazari, H.; Talebian, M.] Geol Survey Iran, Res Inst Earth Sci, Tehran, Iran.
[Jackson, J.] Univ Cambridge, Bullard Labs, Cambridge CB1 3EZ, England.
[Nemati, M.] Bahonar Univ Kerman, Fac Sci, Dept Geol, Kerman, Iran.
[Nemati, M.; Oveisi, B.] Geol Survey Iran, Seismotecton Dept, Tehran, Iran.
RP Walker, RT (reprint author), Univ Oxford, Dept Earth Sci, S Parks Rd, Oxford OX1 3AN, England.
EM Richard.Walker@earth.ox.ac.uk
RI Elliott, John/B-8200-2011; Walker, Richard/D-9908-2011; Walters,
Richard/G-7114-2012; Fielding, Eric/A-1288-2007
OI Elliott, John/0000-0003-2957-4596; Walters, Richard/0000-0002-1704-8727;
Fielding, Eric/0000-0002-6648-8067
FU Geological Survey of Iran; NASA Earth Surface and Interior Focus Area;
ESA [AOALO.3598]; AO PI project [LAN0190, 2214]; NERC; Royal Society of
London; OSUG (Observatoire des Sciences de l'Univers de Grenoble)
Visiting Fellowship
FX We thank the Geological Survey of Iran for their support of our work in
Iran and for enabling field visits to the epicentral region. We also
thank the IIEES (International Institute of Earthquake Engineering and
Seismology), IRSC (Iranian Seismological Centre), and BHRC (Building and
Housing research Centre) for access to instrumental records. Part of the
research described in this paper was supported by the NASA Earth Surface
and Interior Focus Area and performed at the Jet Propulsion Laboratory,
California Institute of Technology under contract with NASA. E K Nissen
helped with the initial body-waveform analysis. We thank Sylvain Barbot
and Manuel Berberian for detailed and constructive review comments.
SPOTS satellite imagery was provided by the European Space Agency
through project allocation No. C1P.6462. ALOS PALSAR data is copyright
JAXA, METI and was provided by ESA under project AOALO.3598. TerraSAR-X
data is copyright 2010, 2011 DLR and was provided under AO PI project
LAN0190. COSMO-SkyMed data is copyright 2010, 2011 ASI and was provided
under AO PI project 2214. We also thank the NERC-ESRC Earthquakes
without Frontiers (EwF) program and the NERC-funded NCEO/COMET+ centre
in the UK. RTW is supported by a University Research Fellowship from the
Royal Society of London and wrote the manuscript at Universite Joseph
Fourier in Grenoble, France, whereas supported by an OSUG (Observatoire
des Sciences de l'Univers de Grenoble) Visiting Fellowship.
NR 49
TC 24
Z9 24
U1 1
U2 22
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0956-540X
EI 1365-246X
J9 GEOPHYS J INT
JI Geophys. J. Int.
PD APR
PY 2013
VL 193
IS 1
BP 349
EP 374
DI 10.1093/gji/ggs109
PG 26
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 120KW
UT WOS:000317170200026
ER
PT J
AU Janches, D
Hormaechea, JL
Brunini, C
Hocking, W
Fritts, DC
AF Janches, D.
Hormaechea, J. L.
Brunini, C.
Hocking, W.
Fritts, D. C.
TI An initial meteoroid stream survey in the southern hemisphere using the
Southern Argentina Agile Meteor Radar (SAAMER)
SO ICARUS
LA English
DT Article
ID ORBIT-RADAR; METHODOLOGY; RADIANTS; ORIGIN; DISKS
AB We present in this manuscript a 4 year survey of meteor shower radiants utilizing the Southern Argentina Agile Meteor Radar (SAAMER). SAAMER, which operates at the southern most region of South America, is a new generation SKiYMET system designed with significant differences from typical meteor radars including high transmitted power and an 8-antenna transmitting array enabling large detected rates at low zenith angles. We applied the statistical methodology developed by Jones and Jones (Jones, J., Jones, W. [2006]. Month. Not. R. Astron. Soc. 367, 1050-1056) to the data collected each day and compiled the results into 1 composite representative year at 1 degrees resolution in Solar Longitude. We then search for enhancements in the activity which last for at least 3 days and evolve temporally as is expected from a meteor shower. Using this methodology, we have identified in our data 32 shower radiants, two of which were not part of the IAU commission 22 meteor shower working list. Recently, SAAMER's capabilities were enhanced by adding two remote stations to receive meteor forward scatter signals from meteor trails and thus enable the determination of meteoroid orbital parameters. SAAMER started recording orbits in January 2012 and future surveys will focus on the search for unknown meteor streams, in particular in the southern ecliptic sky. Published by Elsevier Inc.
C1 [Janches, D.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA.
[Hormaechea, J. L.] Estn Astron Rio Grande, Rio Grande, Tierra del Fueg, Argentina.
[Brunini, C.] Univ Nacl La Plata, Dept Ciencias Astron & Geofis, La Plata, Buenos Aires, Argentina.
[Hocking, W.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Fritts, D. C.] Gats Inc, Boulder, CO 80302 USA.
RP Janches, D (reprint author), NASA, Goddard Space Flight Ctr, Space Weather Lab, Mail Code 674, Greenbelt, MD 20771 USA.
EM diego.janches@nasa.gov; jlhor@earg.gov.ar; claudiobrunini@yahoo.com;
whocking@uwo.ca; dave@gats-inc.com
RI Janches, Diego/D-4674-2012;
OI Janches, Diego/0000-0001-8615-5166; Hormaechea, Jose
Luis/0000-0003-4533-3282
FU NSF [AGS - 0634650, AGS - 0944104, AST - 0908118]
FX This work was supported by NSF Awards AGS - 0634650, AGS - 0944104 and
AST - 0908118. We wish to thank the EARG personnel for their invaluable
help with the operation of SAAMER and D. Moser, P. Brown and M.
Campbell-Brown for useful discussions.
NR 24
TC 3
Z9 3
U1 0
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 APR
PY 2013
VL 223
IS 2
BP 677
EP 683
DI 10.1016/j.icarus.2012.12.018
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 116ZZ
UT WOS:000316923200004
ER
PT J
AU Tice, DS
Irwin, PGJ
Fletcher, LN
Teanby, NA
Hurley, J
Orton, GS
Davis, GR
AF Tice, Dane S.
Irwin, Patrick G. J.
Fletcher, Leigh N.
Teanby, Nick A.
Hurley, Jane
Orton, Glenn S.
Davis, Gary R.
TI Uranus' cloud particle properties and latitudinal methane variation from
IRTF SpeX observations
SO ICARUS
LA English
DT Article
DE Uranus, Atmosphere; Atmospheres, Composition; Atmospheres, Structure;
Data reduction techniques
ID INFRARED-ABSORPTION SPECTRA; OVERTONE BAND; TEMPERATURES; HYDROGEN; CH4;
SPECTROGRAPH; ATMOSPHERE; PLANETS; CM(-1); UKIRT
AB The Uranian atmosphere was observed in August 2009 from 0.8 to 1.8 mu m using the near-infrared spectrometer, SpeX, at NASA's Infrared Telescope Facility. The observations had a spectral resolution of R=1200 and an average seeing of between 0.5" in the H-Band (1.4-1.8 mu m) and 0.6" in the I-Band (0.8-0.9 mu m). The reduced data were analyzed with a multiple-scattering retrieval code. We were able to reproduce observations when using a vertically-compact cloud in the upper troposphere and a vertically-extended, optically-thin haze above the 1-bar level. The existence of these two clouds is consistent with previous studies.
The sub-micron portion of the data are most sensitive to very small scattering particles, allowing more insight into particle size than other portions of the infrared spectrum. This portion of the spectrum was therefore of particular interest and was not available in most previous studies of the planet. We assumed the particles in both clouds to be relatively strong forward scatterers (with a Henyey-Greenstein asymmetry factor of g = 0.7). Given this assumption, we found single-scattering albedos in the tropospheric cloud particles to be (omega) over bar = 0.7 at wavelengths above 1.4 mu m and to gradually increase to (omega) over bar = 1.0 at wavelengths shortward of 1.0 mu m. In the upper haze, we found single-scattering albedos to be (omega) over bar = 1.0 with the exception of a narrow drop at 1.0 mu m to (omega) over bar = 0.6. We found a preference for upper haze particle radii at r = 0.10 mu m. Retrievals of base pressure, fractional scale height, and optical depth in both cloud layers showed the best agreement with data when the base pressure of the upper haze was fixed just above the tropospheric clouds, rather than at or above the tropopausal cold trap. We found that these same retrievals strongly preferred tropospheric cloud particles of 1.35-mu m radii, and observed cloud top height to increase away from the equator in the case of latitudinally invariant methane abundance.
Latitudinal methane variability was also considered, both through a reflectivity study at the 825-nm collision-induced hydrogen absorption feature, as well as through radiative transfer analysis, using forward modeling and retrievals of cloud properties and methane abundance. The data suggested that methane abundance above the tropospheric clouds increased when moving from the midlatitudes towards the equator by at least 9%. The peak of this equatorial methane enrichment was determined to be at 4 +/- 2 degrees S latitude, having moved nearly 15 degrees northward since a reflectance study of 2002 data (Karkoschka and Tomasko, 2009). (C) 2013 Elsevier Inc. All rights reserved.
C1 [Tice, Dane S.; Irwin, Patrick G. J.; Fletcher, Leigh N.; Hurley, Jane] Univ Oxford, Dept Phys, Clarendon Lab, Oxford OX1 3PU, England.
[Teanby, Nick A.] Univ Bristol, Sch Earth Sci, Bristol BS8 1RJ, Avon, England.
[Orton, Glenn S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Davis, Gary R.] Joint Astron Ctr, Hilo, HI 96720 USA.
RP Tice, DS (reprint author), Univ Oxford, Dept Phys, Clarendon Lab, Parks Rd, Oxford OX1 3PU, England.
EM tice@atm.ox.ac.uk
RI Fletcher, Leigh/D-6093-2011;
OI Fletcher, Leigh/0000-0001-5834-9588; Teanby,
Nicholas/0000-0003-3108-5775; Irwin, Patrick/0000-0002-6772-384X
FU United Kingdom Science and Technologies Facilities Council; University
of Oxford Glasstone Fellowship; Leverhulme Trust; NASA
FX We are grateful for project funding from the United Kingdom Science and
Technologies Facilities Council, the University of Oxford Glasstone
Fellowship (Fletcher), the Leverhulme Trust (Teanby), and a grant from
NASA to the Jet Propulsion Laboratory, California Institute of
Technology (Orton). We would like to thank our IRTF support astronomer,
Bobby Bus, and all the staff at the Infrared Telescope Facility. IRTF is
operated by the University of Hawaii under Cooperative Agreement No.
NNX-08AE38A with the National Aeronautics and Space Administration,
Science Mission Directorate, Planetary Astronomy Program.
NR 30
TC 7
Z9 7
U1 0
U2 7
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD APR
PY 2013
VL 223
IS 2
BP 684
EP 698
DI 10.1016/j.icarus.2013.01.006
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 116ZZ
UT WOS:000316923200005
ER
PT J
AU Bottke, WF
Vokrouhlicky, D
Nesvorny, D
Moore, JM
AF Bottke, William F.
Vokrouhlicky, David
Nesvorny, David
Moore, Jeffrey M.
TI Black rain: The burial of the Galilean satellites in irregular satellite
debris
SO ICARUS
LA English
DT Article
DE Ganymede; Jupiter, Satellites; Irregular satellites; Callisto; Europa
ID INFRARED MAPPING SPECTROMETER; OUTER SOLAR-SYSTEM; MAIN ASTEROID BELT;
TERRESTRIAL PLANETS; SUBSURFACE OCEAN; GIANT PLANETS; COLLISIONAL
EVOLUTION; CIRCUMPLANETARY DUST; URANIAN SATELLITES; NATURAL SATELLITES
AB Irregular satellites are dormant comet-like bodies that reside on distant prograde and retrograde orbits around the giant planets. They are likely to be captured objects. Dynamical modeling work indicates they may have been caught during a violent reshuffling of the giant planets similar to 4 Gy ago (Ga) as described by the so-called Nice model. According to this scenario, giant planet migration scattered tens of Earth masses of comet-like bodies throughout the Solar System, with some comets finding themselves near giant planets experiencing mutual encounters. In these cases, gravitational perturbations between the giant planets were often sufficient to capture the comet-like bodies onto irregular satellite-like orbits via three-body reactions. Modeling work suggests these events led to the capture of on the order of similar to 0.001 lunar masses of comet-like objects on isotropic orbits around the giant planets. Roughly half of the population was readily lost by interactions with the Kozai resonance. The remaining half found themselves on orbits consistent with the known irregular satellites. From there, the bodies experienced substantial collisional evolution, enough to grind themselves down to their current low-mass states.
Here we explore the fate of the putative irregular satellite debris in the Jupiter system. Pulverized by collisions, we hypothesize that the carbonaceous chondrite-like material was beaten into small enough particles that it could be driven toward Jupiter by Poynting-Robertson (P-R) drag forces. Assuming its mass distribution was dominated by D > 50 mu m particles, we find that >40% ended up striking the Galilean satellites. The majority were swept up by Callisto, with a factor of 3-4 and 20-30 fewer particles reaching Ganymede and Europa/b, respectively. Collision evolution models indicate most of this material arrived about 4 Ga, but some is still arriving today. We predict that Callisto, Ganymede, Europa, and Io were buried about 4 Ga by similar to 120-140 m, 25-30 m, 7-15 m, and 7-8 m of dark debris, respectively. The first two values are consistent with observations of the deepest dark lag deposits found on the most ancient terrains of Callisto and Ganymede. The rest of the debris was likely worked into the crusts of these worlds by geologic and impact processes. This suggests the debris is a plausible source of the dark lag material found in Europa's low-lying crevices. More speculatively, it is conceivable that the accreted dark particles were a significant source of organic material to Europa's subsurface ocean. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Bottke, William F.; Nesvorny, David] SW Res Inst, Boulder, CO 80302 USA.
[Bottke, William F.; Nesvorny, David] NASA, Lunar Sci Inst, Boulder, CO 80302 USA.
[Vokrouhlicky, David] Charles Univ Prague, Inst Astron, CR-18000 Prague 8, Czech Republic.
[Moore, Jeffrey M.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
RP Bottke, WF (reprint author), SW Res Inst, 1050 Walnut St,Suite 300, Boulder, CO 80302 USA.
EM bottke@boulder.swri.edu
FU NSF's Planetary Astronomy Program; Czech Grant Agency [205/08/0064];
Czech Ministry of Education [MSM0021620860]
FX We thank Mark Buie, Carly Howett, Simone Marchi, Louise Prockter, and
John Spencer for helpful discussions that improved this paper. We also
thank referee Dan Tamayo and an anonymous referee for their constructive
and highly useful comments. Research funds for William Bottke and David
Nesvorny on this work were provided by NSF's Planetary Astronomy
Program. The work of David Vokrouhlicky was partially supported by
research Grant 205/08/0064 of the Czech Grant Agency and the Research
Program MSM0021620860 of the Czech Ministry of Education.
NR 110
TC 9
Z9 9
U1 0
U2 12
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
EI 1090-2643
J9 ICARUS
JI Icarus
PD APR
PY 2013
VL 223
IS 2
BP 775
EP 795
DI 10.1016/j.icarus.2013.01.008
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 116ZZ
UT WOS:000316923200013
ER
PT J
AU Choi, DS
Showman, AP
Vasavada, AR
Simon-Miller, AA
AF Choi, David S.
Showman, Adam P.
Vasavada, Ashwin R.
Simon-Miller, Amy A.
TI Meteorology of Jupiter's equatorial hot spots and plumes from Cassini
SO ICARUS
LA English
DT Article
DE Jupiter; Jupiter, Atmosphere; Atmospheres, Dynamics; Meteorology
ID GREAT RED SPOT; GALILEO PROBE; DYNAMICAL IMPLICATIONS; VERTICAL
STRUCTURE; MOIST CONVECTION; WHITE OVALS; ZONAL WINDS; ATMOSPHERE;
AMMONIA; CLOUDS
AB We present an updated analysis of Jupiter's equatorial meteorology from Cassini observations. For two months preceding the spacecraft's closest approach, the Imaging Science Subsystem (ISS) onboard regularly imaged the atmosphere. We created time-lapse movies from this period in order to analyze the dynamics of equatorial hot spots and their interactions with adjacent latitudes. Hot spots are relatively cloud-free regions that emit strongly at 5 mu m; improved knowledge of these features is crucial for fully understanding Galileo probe measurements taken during its descent through one. Hot spots are quasi-stable, rectangular dark areas on visible-wavelength images, with defined eastern edges that sharply contrast with surrounding clouds, but diffuse western edges serving as nebulous boundaries with adjacent equatorial plumes. Hot spots exhibit significant variations in size and shape over timescales of days and weeks. Some of these changes correspond with passing vortex systems from adjacent latitudes interacting with hot spots. Strong anticyclonic gyres present to the south and southeast of the dark areas appear to circulate into hot spots. Impressive, bright white plumes occupy spaces in between hot spots. Compact cirrus-like 'scooter' clouds flow rapidly through the plumes before disappearing within the dark areas. These clouds travel at 150-200 m s(-1), much faster than the 100 m s(-1) hot spot and plume drift speed. This raises the possibility that the scooter clouds may be more illustrative of the actual jet stream speed at these latitudes. Most previously published zonal wind profiles represent the drift speed of the hot spots at their latitude from pattern matching of the entire longitudinal image strip. If a downward branch of an equatorially-trapped Rossby wave controls the overall appearance of hot spots, however, the westward phase velocity of the wave leads to underestimates of the true jet stream speed. (C) 2013 Elsevier Inc. All rights reserved.
C1 [Choi, David S.] NASA, Goddard Space Flight Ctr, ORAU, Greenbelt, MD 20771 USA.
[Showman, Adam P.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Vasavada, Ashwin R.] CALTECH, Jet Prop Lab, Pasadena, CA 91011 USA.
[Simon-Miller, Amy A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Choi, DS (reprint author), NASA, Goddard Space Flight Ctr, ORAU, Greenbelt, MD 20771 USA.
EM david.s.choi@nasa.gov
RI Simon, Amy/C-8020-2012
OI Simon, Amy/0000-0003-4641-6186
FU NASA Jupiter Data Analysis Program [NNX09AD98G]; NASA Postdoctoral
Program at Goddard Space Flight Center; Oak Ridge Associated
Universities; NASA
FX We thank two anonymous reviewers for their comments that strengthened
this manuscript. This research was supported by a NASA Jupiter Data
Analysis Program Grant, #NNX09AD98G, and by an appointment to the NASA
Postdoctoral Program at Goddard Space Flight Center, administered by Oak
Ridge Associated Universities through a contract with NASA.
NR 36
TC 6
Z9 6
U1 2
U2 12
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD APR
PY 2013
VL 223
IS 2
BP 832
EP 843
DI 10.1016/j.icarus.2013.02.001
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 116ZZ
UT WOS:000316923200017
ER
PT J
AU Polzin, KA
Adwar, JE
Hallock, AK
AF Polzin, Kurt A.
Adwar, Jake E.
Hallock, Ashley K.
TI Optimization of Electrodynamic Energy Transfer in Coilguns With
Multiple, Uncoupled Stages
SO IEEE TRANSACTIONS ON MAGNETICS
LA English
DT Article
DE Coilgun; inductive accelerators; modeling; optimization
ID INDUCTIVE THRUSTER; PERFORMANCE; DESIGN; ACCELERATION
AB A 1-D model for inductive electromagnetic acceleration of projectiles using a coilgun has been nondimensionalized to find relevant scaling parameters. The dynamic impedance parameter, representing the ratio of the resonant period of the unloaded electrical circuit to the time the projectile is electromagnetically coupled to the coil, is the scaling term that can be adjusted to optimize the electromagnetic energy transfer process. The mutual inductance profile, which represents the ability to convert potential electromagnetic energy into projectile kinetic energy, was modeled for a specific geometry using a semi-empirical function previously found suitable for cylindrical pulsed inductive plasma accelerators. Contour plots representing coilgun efficiency were generated for varying initial projectile velocity across a range of dynamic impedances. The contour plots show that below a given initial velocity a dynamic impedance parameter can be selected to maximize energy transfer to the projectile. This optimum varies as a function of the initial velocity a projectile possessed when it enters the coilgun stage. Once the contour plot is generated for a geometry it can be used to optimize the acceleration process for any stage in a coilgun if the individual coils comprising the stages are electromagnetically uncoupled from each other and the velocity of the projectile as it exits the previous stage is known.
C1 [Polzin, Kurt A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Adwar, Jake E.] SUNY Stony Brook, Stony Brook, NY 11790 USA.
[Hallock, Ashley K.] NASA, Yetispace Inc, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Polzin, KA (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM kurt.a.polzin@nasa.gov
NR 23
TC 3
Z9 4
U1 0
U2 9
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9464
EI 1941-0069
J9 IEEE T MAGN
JI IEEE Trans. Magn.
PD APR
PY 2013
VL 49
IS 4
BP 1453
EP 1460
DI 10.1109/TMAG.2012.2230271
PG 8
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA 115II
UT WOS:000316805400023
ER
PT J
AU Lei, JF
Goldberg, RK
AF Lei, Jih-Fen
Goldberg, Robert K.
TI Special Issue on Seventy Years of Aerospace Research and Technology
Excellence at NASA Glenn Research Center Introduction
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Editorial Material
C1 [Lei, Jih-Fen] NASA, Res & Technol Directorate, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Goldberg, Robert K.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Goldberg, RK (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM jih-fen.lei@nasa.gov; Robert.K.Goldberg@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 6
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 197
EP 201
DI 10.1061/(ASCE)AS.1943-5525.0000320
PG 5
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900001
ER
PT J
AU Reddy, DR
AF Reddy, Dhanireddy R.
TI Seventy Years of Aeropropulsion Research at NASA Glenn Research Center
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Air-breathing propulsion; Gas turbine engines; Turbojet; Turbofan;
Turboprop; Energy efficiency; Environmental impact; High-speed
propulsion; Fundamental research; Technology development
AB This paper presents a brief overview of air-breathing propulsion research conducted at the National Aeronautics and Space Administration (NASA) Glenn Research Center (GRC) over the last 70 years. It includes a historical perspective of the center and its various stages of propulsion research in response to the country's different periods of crises and growth opportunities. The GRC's research and technology development covered a broad spectrum, from a short-term focus on improving the energy efficiency of aircraft engines to advancing the frontier technologies of high-speed aviation in the supersonic and hypersonic speed regimes. This paper highlights major research programs, showing their impact on industry and aircraft propulsion, and briefly discusses current research programs and future aeropropulsion technology trends in related areas. DOI: 10.1061/(ASCE)AS.1943-5525.0000312. (C) 2013 American Society of Civil Engineers.
C1 NASA, Aeropropuls Div, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Reddy, DR (reprint author), NASA, Aeropropuls Div, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM dhanireddy.r.reddy@nasa.gov
NR 29
TC 0
Z9 0
U1 2
U2 18
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 202
EP 217
DI 10.1061/(ASCE)AS.1943-5525.0000312
PG 16
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900002
ER
PT J
AU Huff, DL
AF Huff, Dennis L.
TI NASA Glenn's Contributions to Aircraft Engine Noise Research
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Turbofan; Turbojet; Aircraft engine noise; Acoustics; Aeroacoustics;
Fans; Jets; Turbomachinery; Noise reduction
AB This paper reviews all engine noise research conducted at the National Aeronautics and Space Administration (NASA) Glenn Research Center over the last 70 years. The review includes a historical perspective of the center and the facilities used to conduct the research. Major NASA noise research programs are highlighted, showing their impact on the industry and on the development of aircraft noise reduction technology. Noise reduction trends are discussed, and future aircraft concepts are presented. Results show that, since the 1960s, the average perceived noise level has been reduced by about 20 dB. Studies show that, depending on the size of the airport, the aircraft fleet mix, and the actual growth in air travel, another 15-17 dB is required to achieve NASA's long-term goal of providing technologies to limit objectionable noise to the boundaries of an average airport. DOI: 10.1061/(ASCE)AS.1943-5525.0000283. (C) 2013 American Society of Civil Engineers.
C1 NASA, Aeropropuls Div, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Huff, DL (reprint author), NASA, Aeropropuls Div, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM dennis.l.huff@nasa.gov
NR 93
TC 1
Z9 1
U1 0
U2 13
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 218
EP 250
DI 10.1061/(ASCE)AS.1943-5525.0000283
PG 33
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900003
ER
PT J
AU Chang, CT
Tacina, K
Lee, C
Bulzan, D
Hicks, Y
Liu, NS
Lee, J
AF Chang, C. T.
Tacina, K.
Lee, C.
Bulzan, D.
Hicks, Y.
Liu, N. -S.
Lee, J.
TI NASA Glenn Combustion Research for Aeronautical Propulsion
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Combustion; Combustor concept; Fuel injection; Alternate fuel; Optical
diagnostic; CFD; Hypersonic propulsion
ID SUBSONIC CROSS-FLOW; MULTIPLE JETS; PRESSURE
AB NASA Glenn Research Center (GRC) has been involved in a wide range of combustion research topics in combustor concept research, component technology development, and enabling technology development to provide enabling technologies for flight regimes from subsonic to hypersonic. These research efforts were carried out by NASA and industrial and academic partners through a range of NASA fundamental research and focused programs. These synergistic efforts in fuel injection, flame stabilization, combustion physics, and ignition studies have resulted in combustor concept changes that resulted in much cleaner-burning modern jet engines. New computational tools, optical diagnostics, fuels, and fuel conditioning technology are being currently used to develop a better understanding of the complex processes occurring in combustion systems for a range of future propulsion systems. DOI: 10.1061/(ASCE)AS.1943-5525.0000289. (C) 2013 American Society of Civil Engineers.
C1 [Chang, C. T.; Tacina, K.; Bulzan, D.; Hicks, Y.; Liu, N. -S.; Lee, J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Lee, C.] NASA, Combust Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Chang, CT (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM Clarence.T.Chang@nasa.gov; Kathleen.M.Tacina@nasa.gov;
Chi-ming.Lee-1@nasa.gov; Dan.L.Bulzan@nasa.gov;
Yolanda.R.Hicks@nasa.gov; Nan-suey.Liu-1@nasa.gov; Jinho.Lee-1@nasa.gov
NR 104
TC 1
Z9 1
U1 2
U2 8
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 251
EP 259
DI 10.1061/(ASCE)AS.1943-5525.0000289
PG 9
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900004
ER
PT J
AU Potapczuk, MG
AF Potapczuk, Mark G.
TI Aircraft Icing Research at NASA Glenn Research Center
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Aircraft icing
AB The National Aeronautics and Space Administration Glenn Research Center (GRC; and its predecessor organizations) has been and continues to be a focal point for research in the field of aircraft icing. This paper provides a historical perspective on the contributions that GRC research has made to the field, as well as a synopsis of the current research being conducted at the center. The GRC's icing research has been comprehensive, covering the characterization of the icing environment, investigations into the physics of ice accretion on aircraft surfaces, studies of the impact of icing on aircraft aerodynamics and engine performance, icing instrumentation development, and simulation of ice growth on aircraft using wind tunnels and computational methods. This research has led to improved safety for flight in icing conditions through contributions to the development of icing regulations; a greater understanding of the effects of ice accretion; and the development of experimental and computational methods to aid in the design of aircraft and aircraft subsystems (including ice protection systems) that can operate safely in an icing environment. DOI: 10.1061/(ASCE)AS.1943-5525.0000322. (C) 2013 American Society of Civil Engineers.
C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Potapczuk, MG (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM Mark.G.Potapczuk@nasa.gov
NR 102
TC 5
Z9 6
U1 3
U2 17
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 260
EP 276
DI 10.1061/(ASCE)AS.1943-5525.0000322
PG 17
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900005
ER
PT J
AU Liou, MS
Povinelli, LA
AF Liou, Meng-Sing
Povinelli, Louis A.
TI Computational Fluid Dynamics: NASA Glenn Research Center's Legacy and
Contributions
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Numerical methods; Turbulence modeling; Inlet and nozzle; Aeroacoustics;
Combustion; Compressor; Turbine heat transfer; Engine system simulation;
Validation; CFD codes; Multidisciplinary analysis; Design optimization
ID TIME CONSERVATION ELEMENT; DIFFERENCE-SCHEMES; SPLITTING SCHEME;
NAVIER-STOKES; JET FLOW; ACCURATE; ROTOR; AUSM(+)-UP; EQUATIONS; SYSTEMS
AB Development and contributions to computational fluid dynamics (CFD) at the National Aeronautics and Space Administration (NASA) Glenn Research Center (GRC) during the period from 1947 to the present are reviewed in five categories: numerical methods, physical modeling, CFD codes development, CFD validation and engineering applications, and multidisciplinary design optimization. Some representative results in applications to aero and propulsion systems are included to illustrate the developed capabilities. GRC has a long history of investing resources to develop these key subject matters, with an interest in a wide range of applications, primarily focusing on propulsion-related technologies and concepts. The evolved CFD capabilities have enabled simulations of complex three-dimensional flow fields for engine components and integrated configurations, as illustrated in this article. This article is intended to give a useful, albeit noncomplete, overview into GRC's work in CFD. DOI: 10.1061/(ASCE)AS.1943-5525.0000295. (C) 2013 American Society of Civil Engineers.
C1 [Liou, Meng-Sing; Povinelli, Louis A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Liou, MS (reprint author), NASA, Glenn Res Ctr, MS 5-11, Cleveland, OH 44135 USA.
EM meng-sing.liou@nasa.gov
NR 97
TC 1
Z9 1
U1 0
U2 24
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 277
EP 287
DI 10.1061/(ASCE)AS.1943-5525.0000295
PG 11
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900006
ER
PT J
AU Lyons, VJ
AF Lyons, Valerie J.
TI Power and Propulsion at NASA Glenn Research Center: Historic Perspective
of Major Accomplishments
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Power; Propulsion; Space power; NASA history; Lewis Research Center;
Alternative energy; Solar power; Nuclear space power; Electric
propulsion; Stirling convertors
ID SYSTEM
AB Propulsion and power have long been core competencies of the National Aeronautics and Space Administration (NASA) Glenn Research Center (GRC). At the dawn of the space era, the center brought key propulsion and power technology to support spacecraft development. This paper serves as an introduction to a series of papers describing the highlights of the GRC's power and propulsion research and development efforts. The power papers cover solar and nuclear power generation and energy conversion, energy storage (focusing on batteries, flywheels, and fuel cells), power systems, and power management and distribution. The propulsion papers cover chemical propulsion, cryogenic propellant systems, electric propulsion, and nuclear thermal rocket propulsion. Each paper addresses some history, current efforts, and future plans for each of the technology areas. DOI: 10.1061/(ASCE)AS.1943-5525.0000315. (C) 2013 American Society of Civil Engineers.
C1 NASA, Power & In Space Prop Div, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Lyons, VJ (reprint author), NASA, Power & In Space Prop Div, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM Valerie.J.Lyons@nasa.gov
NR 39
TC 0
Z9 0
U1 5
U2 49
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 288
EP 299
DI 10.1061/(ASCE)AS.1943-5525.0000315
PG 12
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900007
ER
PT J
AU Patterson, MJ
Sovey, JS
AF Patterson, Michael J.
Sovey, James S.
TI History of Electric Propulsion at NASA Glenn Research Center: 1956 to
Present
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Electric propulsion; Arcjets; Hall effect thrusters; Ion thrusters;
Glenn Research Center; Lewis Research Center
ID ION PROPULSION; THRUSTER; SPACECRAFT
AB This paper provides a brief overview of the history of electric propulsion (EP) at the National Aeronautics and Space Administration (NASA) Glenn Research Center (GRC). Since the inception of EP technology, GRC has played a pivotal role in developing the technology and transitioning it to flight. Research and development efforts by GRC's employees, grantees, and contractors brought operational EP systems to commercial satellites in the early 1990s and to NASA and other government agency missions starting in the late 1990s. GRC's early construction of unique EP test infrastructure and NASA's and GRC's sustained investments in EP research and development over several decades were strategic in the creation of technologies that continue to greatly benefit the competitiveness and capabilities of U. S. space systems and missions. DOI: 10.1061/(ASCE)AS.1943-5525.0000304. (C) 2013 American Society of Civil Engineers.
C1 [Patterson, Michael J.] NASA, In Space Prop, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Sovey, James S.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Patterson, MJ (reprint author), NASA, In Space Prop, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM michael.j.patterson@nasa.gov
NR 67
TC 5
Z9 6
U1 2
U2 33
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 300
EP 316
DI 10.1061/(ASCE)AS.1943-5525.0000304
PG 17
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900008
ER
PT J
AU Linne, DL
Aukerman, CA
Palaszewski, BA
AF Linne, Diane L.
Aukerman, Carl A.
Palaszewski, Bryan A.
TI Chemical Propulsion: Greater than 60 Years of Leadership and Innovation
at NASA Glenn Research Center
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Aerospace engineering; Engines; Experimentation; History; Research
AB The National Aeronautics and Space Administration (NASA) Glenn Research Center (GRC) was built during World War II with the primary objective of catching up with the Germans in jet engine technology. A decade later, it seemed only natural that these same aeropropulsion engineers would progress into the largely unexplored field of space chemical propulsion. Starting before the launch of Sputnik set off the great space race, researchers at the GRC were testing and flying cryogenic hydrogen-fueled engines that were an eventual key to the success of the Apollo manned missions to the moon. In the 60 years since this first foray into chemical propulsion, engineers at the GRC have made countless innovations and contributions to every component of rocket engine technology. From energetic propellants to green fuels, from innovative metallic alloys to ceramic composites, from seals and bearings to igniters and injectors, and from upper stages and satellites to launch vehicles and planetary landers, the dedicated and creative people at the GRC have propelled the United States to the forefront of space exploration and continue to work toward an even more exciting future. Some of the highlights of this illustrious and ongoing journey are explored in this paper. DOI: 10.1061/(ASCE)AS.1943-5525.0000303. (C) 2013 American Society of Civil Engineers.
C1 [Linne, Diane L.; Aukerman, Carl A.; Palaszewski, Bryan A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Linne, DL (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM diane.l.linne@nasa.gov; auk4@aol.com; bryan.a.palaszewski@nasa.gov
NR 74
TC 2
Z9 2
U1 3
U2 26
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 317
EP 333
DI 10.1061/(ASCE)AS.1943-5525.0000303
PG 17
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900009
ER
PT J
AU Borowski, SK
AF Borowski, Stanley K.
TI Nuclear Thermal Propulsion: Past Accomplishments, Present Efforts, and a
Look Ahead
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Nuclear thermal rocket; NTR; Rover/Nuclear Engine for Rocket Vehicle
Applications (NERVA); Spacecraft; Human Moon Mars exploration
AB The National Aeronautics and Space Administration (NASA) Glenn Research Center (GRC) has been actively involved in nuclear thermal propulsion (NTP) technology development, mission, engine, and vehicle design dating back to the Rover and Nuclear Engine for Rocket Vehicle Applications programs. This technology was successfully developed in over 20 rocket/reactor tests, which demonstrated a wide range of thrust levels, high-temperature fuel, sustained engine operation, accumulated time at full power, and restart capability-everything required for a human mission to Mars. Furthermore, NTP requires no large technology scale-up. The smallest engine tested during the Rover program-the Pewee Engine-is sufficient for this when used in a clustered engine arrangement. The GRC has led every major study involving NTP since the late 1980s and has helped quantify the evolution and growth potential of the nuclear thermal rocket (NTR), which includes the bimodal and liquid-oxygen- (LOX-) augmented NTR concepts. In NASA's recent Mars Design Reference Architecture (DRA) study, NTP reduced total mission mass over 400 t compared with chemical propulsion. Human missions to the Moon and near-Earth asteroids are also enhanced using NTP. In 2011, NASA restarted an NTP technology demonstration effort that is continuing under the Nuclear Cryogenic Propulsion Stage project, which began in 2012. Ground demonstrations of a small, scalable NTR by 2020 are envisioned, with a flight demonstration shortly thereafter. DOI: 10.1061/(ASCE)AS.1943-5525.0000313. (C) 2013 American Society of Civil Engineers.
C1 NASA, Prop & Control Syst Anal Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Borowski, SK (reprint author), NASA, Prop & Control Syst Anal Branch, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM stanley.k.borowski@nasa.gov
NR 34
TC 1
Z9 1
U1 2
U2 41
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 334
EP 342
DI 10.1061/(ASCE)AS.1943-5525.0000313
PG 9
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900010
ER
PT J
AU Meyer, ML
Chato, DJ
Plachta, DW
Zimmerli, GA
Barsi, SJ
Van Dresar, NT
Moder, JP
AF Meyer, Michael L.
Chato, David J.
Plachta, David W.
Zimmerli, Gregory A.
Barsi, Stephen J.
Van Dresar, Neil T.
Moder, Jeffrey P.
TI Mastering Cryogenic Propellants
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Space exploration; Spacecraft; Aerospace engineering; Research; Fluid
dynamics; Thermodynamics; Tanks
AB The National Aeronautics and Space Administration (NASA) Glenn Research Center (GRC) began experimentation with cryogenic propellants in the early 1950s to understand the potential of these high-performance propellants for use in liquid propellant rocket engines. Supporting these tests required learning how to both design cryogenic systems and develop procedures to safely and reliably work with cryogenic fuels and oxidizers. This early work led to the development of a skill set that has been core to the center ever since. When NASA was formed and the exploration missions were defined, it became clear that the ability to use cryogenic propellants in the thermal and microgravity environment of space was critical to mission success, and the agency was tasked with enabling this capability. To support development of the Centaur upper stage and the Saturn S-IVB stage, GRC researchers and engineers initiated extensive technology development for the in-space application of cryogenic fluid management (CFM). These initial efforts addressed basic requirements of propellant slosh, settling, and short-term storage/pressure control. Over the ensuing years, the NASA GRC has advanced CFM technologies to enable more reliable and capable upper stages. Today, these CFM technologies are on the brink of enabling long-duration in-space cryogenic propulsion stages and cryogenic propellant depots. DOI: 10.1061/(ASCE)AS.1943-5525.0000297. (C) 2013 American Society of Civil Engineers.
C1 [Meyer, Michael L.] NASA, Power & In Space Prop Div, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Chato, David J.; Plachta, David W.; Zimmerli, Gregory A.; Barsi, Stephen J.; Van Dresar, Neil T.; Moder, Jeffrey P.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Meyer, ML (reprint author), NASA, Power & In Space Prop Div, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM michael.l.meyer@nasa.gov; david.j.chato@nasa.gov;
david.w.plachta@nasa.gov; greg.zimmerli@nasa.gov;
stephen.j.barsi@nasa.gov; neil.t.vandresar@nasa.gov;
jeffrey.p.moder@nasa.gov
RI Chato, David/B-2698-2013
OI Chato, David/0000-0003-2990-0646
NR 69
TC 3
Z9 3
U1 1
U2 19
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 343
EP 351
DI 10.1061/(ASCE)AS.1943-5525.0000297
PG 9
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900011
ER
PT J
AU Mason, LS
AF Mason, Lee S.
TI Dynamic Energy Conversion: Vital Technology for Space Nuclear Power
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Space; Nuclear power; Energy conversion; Brayton; Stirling
AB The National Aeronautics and Space Administration Glenn Research Center (GRC) has an extensive history in dynamic energy conversion dating back to the early 1960s. This legacy puts the GRC at the forefront of nuclear power systems using thermodynamic power cycles such as Stirling and Brayton. The advantages of dynamic energy conversion include high efficiency, long life, and scalability to high power. These attributes make Brayton and Stirling power cycles an ideal solution for nuclear energy conversion. DOI: 10.1061/(ASCE)AS.1943-5525.0000318. (C) 2013 American Society of Civil Engineers.
C1 NASA, Thermal Energy Convers Branch, Glenn Res Ctr, Cleveland, OH USA.
RP Mason, LS (reprint author), NASA, Thermal Energy Convers Branch, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH USA.
EM lee.s.mason@nasa.gov
NR 48
TC 2
Z9 4
U1 0
U2 8
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 352
EP 360
DI 10.1061/(ASCE)AS.1943-5525.0000318
PG 9
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900012
ER
PT J
AU Reid, CM
Miller, TB
Hoberecht, MA
Loyselle, PL
Taylor, LM
Farmer, SC
Jansen, RH
AF Reid, Concha M.
Miller, Thomas B.
Hoberecht, Mark A.
Loyselle, Patricia L.
Taylor, Linda M.
Farmer, Serene C.
Jansen, Ralph H.
TI History of Electrochemical and Energy Storage Technology Development at
NASA Glenn Research Center
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Energy storage; Electric power; Mechanical systems; Spacecraft; Space
stations; Energy; Satellites; Energy sources
AB The National Aeronautics and Space Administration Glenn Research Center (GRC) has a rich heritage of developing electrochemical technologies and energy storage systems for aerospace. Primary and rechargeable batteries, fuel cells, flywheels, and regenerative fuel cells are among the GRC's portfolio of energy storage devices and primary power systems. These technologies have been developed for missions and applications such as low Earth orbit and geosynchronous Earth orbit satellites, space shuttle, astronaut spacesuit, International Space Station, landers and rovers, and lunar and planetary habitats. The desire for lower mass, lower volume, higher efficiency, and more reliable power systems has most often been the driving force behind the development of these technologies. Often, as with fuel cells for the early Gemini and Apollo missions, development of the technology has been mission enabling. Although many of these technologies were initially developed for applications in space, the existence of such capabilities or development successes at GRC has led to their adoption for terrestrial uses or further research and development for terrestrial applications, including electric vehicles, unmanned aerial and underwater vehicles, and all-electric aircraft. This paper discusses the history of and the current research and development at the GRC in electrochemical and energy storage technologies. The future outlook for each of these technologies is also addressed. DOI: 10.1061/(ASCE)AS.1943-5525.0000323. (C) 2013 American Society of Civil Engineers.
C1 [Reid, Concha M.; Miller, Thomas B.; Hoberecht, Mark A.; Loyselle, Patricia L.; Taylor, Linda M.; Farmer, Serene C.; Jansen, Ralph H.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Reid, CM (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM concha.m.reid@nasa.gov; thomas.b.miller@nasa.gov;
mark.a.hoberecht@nasa.gov; patricia.l.loyselle@nasa.gov;
linda.m.taylor@nasa.gov; serene.c.farmer@nasa.gov;
ralph.h.jansen@nasa.gov
NR 58
TC 3
Z9 3
U1 2
U2 49
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 361
EP 371
DI 10.1061/(ASCE)AS.1943-5525.0000323
PG 11
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900013
ER
PT J
AU Seng, GT
Zeller, MV
Ramos, CT
AF Seng, Gary T.
Zeller, Mary V.
Ramos, Calvin T.
TI Introduction to the Communications, Instrumentation, and Controls
Division
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Instrumentation; Harsh environment sensors; High-temperature
electronics; Turbine engine controls; Engine system dynamics;
Aerocommunications; Space communications technology; RF and optical
communications; Digital communications; Networking
AB This paper explores the organizational history of the three core discipline areas currently residing within the Communications, Instrumentation, and Controls Division, which are harsh environment instrumentation/sensors/electronics, turbine engine controls and systems dynamics, and aerospace communications technology. Division and selected branch management will be identified by discipline in chronological order. In the second section, current division research areas will be listed by branch. Finally, future progress in the key disciplines is discussed by describing near-term future work and projecting a long-term future state beyond the horizon. DOI: 10.1061/(ASCE)AS.1943-5525.0000311. (C) 2013 American Society of Civil Engineers.
C1 [Seng, Gary T.] NASA, Commun Instrumentat & Controls Div, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Zeller, Mary V.; Ramos, Calvin T.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Seng, GT (reprint author), NASA, Commun Instrumentat & Controls Div, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM gary.t.seng@nasa.gov; mary.v.zeller@nasa.gov; calvin.t.ramos@nasa.gov
NR 12
TC 0
Z9 0
U1 0
U2 2
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 372
EP 376
DI 10.1061/(ASCE)AS.1943-5525.0000311
PG 5
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900014
ER
PT J
AU Ramos, C
Fujikawa, G
Jordan, J
Miranda, FA
Ponchak, D
Pouch, JJ
Wallett, TM
AF Ramos, Calvin
Fujikawa, Gene
Jordan, Jennifer
Miranda, Felix A.
Ponchak, Denise
Pouch, John J.
Wallett, Thomas M.
TI Communications Research and Development at NASA Glenn Research Center
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Radiofrequency (RF) communications; Optical communications; Digital
communications; Antennas and propagation; Navigation; Networking
protocols; Traveling-wave tube amplifiers; Communications architectures
ID TRAVELING-WAVE TUBES
AB Over the last several decades, the National Aeronautics and Space Administration (NASA) Glenn Research Center (GRC), formerly Lewis Research Center (LeRC) has performed research and technology development of aeronautic- and space-based communications in support of NASA and the nation. In the 1970s, GRC partnered with the Canadian Department of Communications through the Communications Technology Satellite (CTS) Project, in which GRC researchers were responsible for the development of critical technology components, such as the high-power, traveling-wave tube amplifier (TWTA), thereby pioneering the surge of television channels via satellite. For its efforts, LeRC was awarded an Emmy by the television industry. The decade of the 1980s served as a period for technology development that culminated in the launch of the Advanced Communications Technology Satellite (ACTS) in 1993. The ACTS demonstration of spot beam antenna technology resulted in an overall increase of efficiency in satellite communications. In the latter part of the 1990s and until today, GRC research engineers have continued to conduct research and technology development in multiple domains. The primary focus of this article is to introduce the reader to the long heritage at GRC in communications research and development through the CTS and ACTS projects and delve into specific technology areas following the ACTS Project to today in support of high-data rate communications. DOI: 10.1061/(ASCE)AS.19435525.0000316. (C) 2013 American Society of Civil Engineers.
C1 [Ramos, Calvin; Fujikawa, Gene; Ponchak, Denise] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Jordan, Jennifer] NASA, Electron & Optoelect Devices Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Miranda, Felix A.; Pouch, John J.; Wallett, Thomas M.] NASA, Antenna & Opt Syst Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Ramos, C (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM Calvin.T.Ramos@grc.nasa.gov; Gene.Fujikawa@nasa.gov;
Jennifer.L.Jordan@nasa.gov; Felix.A.Miranda@nasa.gov;
Denise.S.Ponchak@nasa.gov; John.J.Pouch@nasa.gov;
Thomas.M.Wallett@nasa.gov
NR 52
TC 0
Z9 0
U1 0
U2 8
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 377
EP 394
DI 10.1061/(ASCE)AS.1943-5525.0000316
PG 18
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900015
ER
PT J
AU Baaklini, GY
AF Baaklini, George Y.
TI Optical Instrumentation and Nondestructive Evaluation Branch Research
and Technology Advances at NASA Glenn Research Center since 1941
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Optical instrumentation; Nondestructive evaluation; Laser diagnostics;
Flight electronics; Health monitoring; Rayleigh scattering; Particle
imaging velocimetry; Fiber optics; Luminescent coatings; Tomography;
Ultrasonics; Remote sensing; Engine icing
ID RAYLEIGH-SCATTERING; COMPUTED-TOMOGRAPHY; ACOUSTO-ULTRASONICS;
COMPOSITES; VELOCIMETRY; SYSTEM; DAMAGE; MARS
AB This paper is a transitory decadal overview capturing the current research and technology accomplishments that are being developed by the Optical Instrumentation and Nondestructive Evaluation (NDE) Branch at the National Aeronautics and Space Administration (NASA) Glenn Research Center (GRC). The emphasis is on the latest GRC research and technology advances with a brief discussion of the history and technical background of optical instrumentation since the 1940s, NDE sciences and methods since the 1970s, fiber optics since the 1980s, space-qualified instrumentation since the 1990s, and propulsion health monitoring since the beginning of the current century. This paper also identifies and describes recent and future technical directions based on/guided by current NASA strategic and GRC and NASA project implementation plans. DOI: 10.1061/(ASCE)AS.1943-5525.0000305. (C) 2013 American Society of Civil Engineers.
C1 NASA, Opt Instrumentat & NDE Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Baaklini, GY (reprint author), NASA, Opt Instrumentat & NDE Branch, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM george.y.baaklini@nasa.gov
NR 79
TC 0
Z9 0
U1 1
U2 18
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 APR
PY 2013
VL 26
IS 2
SI SI
BP 395
EP 408
DI 10.1061/(ASCE)AS.1943-5525.0000305
PG 14
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900016
ER
PT J
AU Matus, LG
AF Matus, Lawrence G.
TI Instrumentation for Aerospace Applications: Electronic-Based
Technologies
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Instrumentation; Sensors; Electronic devices; Microfabrication; High
temperature
ID DEGREES-C; TEMPERATURE
AB Throughout the 70-year history of the National Aeronautics and Space Administration (NASA) Glenn Research Center (GRC), instrumentation engineers have provided measurement methods and devices necessary to support ongoing and future aeropropulsion research and development efforts. On occasion, routine instrumentation approaches are perfectly suited for the task at hand. However, as propulsion components and systems become more complex through the incorporation of new materials and higher temperature operation, modifications to traditional instrumentation methods or entirely new methods are necessary. This paper provides a glimpse of the core electronic-based instrumentation methods developed throughout the years to measure temperature, strain, pressure, heat flux, and chemical gas species and describes how these methods are evolving to meet the instrumentation challenges of high-performance propulsion systems. It is clear that future aeropropulsion systems will operate at higher temperatures and require more onboard electronics for health monitoring and control functions. For this reason, a significant effort in high-temperature electronics based on the wide-bandgap semiconductor silicon carbide was initiated and has demonstrated several world's first electronic sensors and devices operating at 600 degrees C. It is concluded that electronic-based sensors and devices will continuously be pushed to meet the needs of increasingly harsher environment measurements. DOI: 10.1061/(ASCE)AS.1943-5525.0000302. (C) 2013 American Society of Civil Engineers.
C1 NASA, Sensors & Elect Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Matus, LG (reprint author), NASA, Sensors & Elect Branch, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM Lawrence.G.Matus@nasa.gov
NR 65
TC 0
Z9 0
U1 0
U2 15
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 409
EP 421
DI 10.1061/(ASCE)AS.1943-5525.0000302
PG 13
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900017
ER
PT J
AU Garg, S
AF Garg, Sanjay
TI Aircraft Turbine Engine Control Research at NASA Glenn Research Center
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Gas turbine engines; Engine control; Engine performance; Robust control;
Fault detection control; Diagnostics; Dynamic modeling
ID COMPRESSOR; STALL
AB This paper provides an overview of the aircraft turbine engine control research at NASA Glenn Research Center (GRC). A brief introduction to the engine control problem is first provided with a description of the state-of-the-art control law structure. A historical aspect of engine control development since the 1940s is then provided with a special emphasis on the contributions of GRC. With the increased emphasis on aircraft safety, enhanced performance, and affordability, as well as the need to reduce the environmental impact of aircraft, there are many new challenges being faced by the designers of aircraft propulsion systems. The Controls and Dynamics Branch (CDB) at the GRC is leading and participating in various projects to develop advanced propulsion controls and diagnostics technologies that will help meet the challenging goals of NASA Aeronautics Research Mission programs. The rest of the paper provides an overview of the various CDB technology development activities in aircraft engine control and diagnostics, both current and some accomplished in the recent past. The motivation for each of the research efforts, the research approach, technical challenges, and the key progress to date are summarized. DOI: 10.1061/(ASCE)AS.1943-5525.0000296. (C) 2013 American Society of Civil Engineers.
C1 NASA, Controls & Dynam Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Garg, S (reprint author), NASA, Controls & Dynam Branch, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM sanjay.garg@nasa.gov
NR 47
TC 5
Z9 5
U1 2
U2 28
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 422
EP 438
DI 10.1061/(ASCE)AS.1943-5525.0000296
PG 17
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900018
ER
PT J
AU Sharp, LM
Dietrich, DL
Motil, BJ
AF Sharp, Lauren M.
Dietrich, Daniel L.
Motil, Brian J.
TI Microgravity Fluids and Combustion Research at NASA Glenn Research
Center
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Microgravity; Fluid physics; Combustion science
ID JET DIFFUSION FLAMES; REDUCED GRAVITY; BEHAVIOR; SPREAD
AB At the dawn of the Space Age, the design of early rocket and spacecraft systems presented significant challenges because of the low-gravity environment of space. Motivated by these challenges, the National Aeronautics and Space Administration (NASA) Glenn Research Center (GRC) pioneered the development of low-gravity facilities-including drop towers, sounding rockets, zero-gravity (zero-g) aircraft, and most importantly, space-based facilities-to advance microgravity research to further the nation's space exploration efforts. These efforts resulted in improved spacecraft system designs and practices in areas as diverse as fluid handling and spacecraft fire safety. At the same time, researchers realized that the microgravity environment allows the study of fundamental combustion and fluid physics problems, without the complication of buoyancy-induced convection. Microgravity testing enabled advancements in areas of technological and ecological importance in terrestrial applications such as global atmospheric change, combustor design, groundwater pollution, oil production, and advanced materials manufacturing, which often rely on advances in fluid physics and chemically reacting flows. GRC has been a leader in microgravity fluid physics and combustion research for more than 50 years. This paper highlights the facilities and some of the many accomplishments. DOI: 10.1061/(ASCE)AS.1943-5525.0000293. (C) 2013 American Society of Civil Engineers.
C1 [Sharp, Lauren M.; Dietrich, Daniel L.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Motil, Brian J.] NASA, Fluid Phys & Transport Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Sharp, LM (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM Lauren.M.Sharp@nasa.gov; Daniel.L.Dietrich@nasa.gov;
Brian.J.Motil@nasa.gov
NR 34
TC 0
Z9 1
U1 3
U2 23
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 439
EP 450
DI 10.1061/(ASCE)AS.1943-5525.0000293
PG 12
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900019
ER
PT J
AU Myers, J
Stauber, L
Weaver, A
McKay, T
Harrivel, A
Hepp, A
AF Myers, Jerry
Stauber, Laurel
Weaver, Aaron
McKay, Terri
Harrivel, Angela
Hepp, Aloysius
TI Bioscience and Medical Technology: From the Earth to Space and Back
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Aerospace engineering; Aerospace medicine; Bioengineering; Biosciences;
Computer models; Community relations; Data communication; Data analysis;
Space exploration; Space life support systems
ID NANOTUBES; FORCES; CARBON
AB Throughout the 70-year history of NASA Glenn Research Center (GRC), technology development efforts that promoted advancement in aeronautics technologies, aerospace sciences, materials for hostile environments, and microgravity physics have also enabled the maturation of technologies that have affected medical practice on Earth, in the air, and in space. GRC's unique skill mix, required for aeronautics research and space exploration, ultimately also advanced the development of a wide array of capabilities applicable to biomedical engineering. This paper presents a historical review of notable biomedical endeavors at GRC that have addressed common and uncommon medical conditions afflicting both astronauts and non-astronauts. It also highlights the unique physiological stressors associated with residing in space. The physiological changes associated with these stimuli present evolving challenges for researchers to devise new and innovative medical interventions and technologies. DOI: 10.1061/(ASCE)AS.1943-5525.0000279. (C) 2013 American Society of Civil Engineers.
C1 [Myers, Jerry] NASA, Bio Sci & Technol Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Stauber, Laurel] NASA, Technol Collaborat, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Weaver, Aaron; McKay, Terri; Harrivel, Angela; Hepp, Aloysius] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Myers, J (reprint author), NASA, Bio Sci & Technol Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM jerry.g.myers@nasa.gov
NR 48
TC 0
Z9 0
U1 3
U2 15
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 451
EP 458
DI 10.1061/(ASCE)AS.1943-5525.0000279
PG 8
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900020
ER
PT J
AU Misra, AK
Greenbauer-Seng, LA
AF Misra, Ajay K.
Greenbauer-Seng, Leslie A.
TI Aerospace Propulsion and Power Materials and Structures Research at NASA
Glenn Research Center
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE High-temperature materials and structures; Composite materials; Smart
materials; Nanomaterials; Impact dynamics; Active structures; Rotating
and dynamic structures; Multiscale modeling; Energy storage; Composite
mechanics
ID POLYMER MATRIX COMPOSITES; MECHANICAL-PROPERTIES; PROGRESSIVE DAMAGE;
BARRIER COATINGS; SILICON-CARBIDE; BEHAVIOR; PERFORMANCE; OXIDATION;
POLYIMIDE; CERAMICS
AB The National Aeronautics and Space Administration (NASA) Glenn Research Center (GRC) is well recognized for its contributions toward development of advanced materials and structures for aerospace propulsion and power systems. The Structures and Materials Division conducts research across a broad range of technical areas relevant to the agency's future aeronautics and space mission requirements. This paper will introduce the technical areas of strategic importance in the Structures and Materials Division today and briefly address some of the specific research activities within these areas. A broad look at how the research areas of emphasis have evolved over time, beginning in the early 1940s when the GRC was first formed, will be discussed. Examples of some of the more notable research accomplishments and their impact on the aerospace industry over this time period will be included. A discussion of the division's planned technical directions believed to be required to meet the longer-term national aeronautics and space exploration goals will also be addressed. DOI: 10.1061/(ASCE)AS.1943-5525.0000325. (C) 2013 American Society of Civil Engineers.
C1 [Misra, Ajay K.; Greenbauer-Seng, Leslie A.] NASA, Struct & Mat Div, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Greenbauer-Seng, LA (reprint author), NASA, Struct & Mat Div, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM Ajay.K.Misra@nasa.gov; Leslie.A.Greenbauer-Seng@nasa.gov
NR 142
TC 2
Z9 2
U1 8
U2 31
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 459
EP 490
DI 10.1061/(ASCE)AS.1943-5525.0000325
PG 32
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900021
ER
PT J
AU Nathal, MV
Stefko, GL
AF Nathal, Michael V.
Stefko, George L.
TI Smart Materials and Active Structures
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Shape memory alloys; Morphing structures; Forced vibration response
analysis; High-temperature piezoelectric materials; Rotating blade
vibration damping; Shunted piezoelectric damping; Blade spin rig;
Composite materials; Fan blade
ID MORPHOTROPIC PHASE-BOUNDARY; CERAMICS; NITI
AB Research in smart materials and active structures has grown significantly at the National Aeronautics and Space Administration (NASA) Glenn Research Center (GRC) in the last 10 years. The GRC has achieved several promising results in both new material development and component applications for concepts using both shape memory alloys and piezoelectric ceramics. Progress in understanding and modeling of shape memory alloys has allowed for improved design and control methodologies. New high-temperature alloys with attractive work output have extended the capability from room temperature to similar to 350 degrees C. Finally, the list of successful prototype demonstrations continues to grow for both commercially available alloys and the newer high-temperature alloys. Analytical and experimental methods on piezoelectric blade vibration damping have produced the first successful demonstration of vibration damping on a rotating component. The damping levels achieved lead to reduced dynamic stresses, hence increased engine life and enhanced damage tolerance. In addition, new compositions have been developed to extend the temperature capability of high-performance piezoelectrics to near 400 degrees C. These new materials are just now showing laboratory-scale feasibility and are targeted for continued development. DOI: 10.1061/(ASCE)AS.1943-5525.0000319. (C) 2013 American Society of Civil Engineers.
C1 [Nathal, Michael V.] NASA, Adv Metall Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Stefko, George L.] NASA, Struct & Dynam Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Nathal, MV (reprint author), NASA, Adv Metall Branch, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM michael.v.nathal@nasa.gov; george.l.stefko@nasa.gov
FU NASA; Air Force Office of Scientific Research [FA9550-06-1-0260]
FX The work presented in this paper was the result of the efforts of the
following researchers: M. A. Bakhle, B. B. Choi, K. P. Duffy, J. B. Min,
C. R. Morrison, and A. J. Provenza (piezoelectric damping team); F.
Dynys, A. Sayir, and A. Sehirlioglu (high-temperature piezoelectric
material team); and G. S. Bigelow, O. Benafan, A. Garg, D. J. Gaydosh,
R. D. Noebe, and S. A. Padula (shape memory alloy team). Funding from
NASA's Subsonics Fixed Wing and Supersonics projects and Air Force
Office of Scientific Research Grant No. FA9550-06-1-0260 is appreciated.
NR 31
TC 1
Z9 1
U1 4
U2 85
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 491
EP 499
DI 10.1061/(ASCE)AS.1943-5525.0000319
PG 9
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900022
ER
PT J
AU Dever, JA
Nathal, MV
DiCarlo, JA
AF Dever, Joyce A.
Nathal, Michael V.
DiCarlo, James A.
TI Research on High-Temperature Aerospace Materials at NASA Glenn Research
Center
SO JOURNAL OF AEROSPACE ENGINEERING
LA English
DT Article
DE Metallic materials; Ceramic materials; Ceramic matrix composites;
Thermal barrier coatings; Environmental barrier coatings; Oxidation; Hot
corrosion
ID THERMAL BARRIER COATINGS; SIO2 SCALE VOLATILITY; CYCLIC-OXIDATION
BEHAVIOR; SILICON-CARBIDE; THERMOMECHANICAL PROPERTIES; COMBUSTION
CONDITIONS; MATRIX COMPOSITES; SIC FIBERS; CERAMICS; MODEL
AB Within the Structures and Materials Division at the National Aeronautics and Space Administration Glenn Research Center (GRC), research is being conducted to develop durable high-temperature materials for the most challenging aerospace applications. Research is advancing material and coating technologies for applications including turbine engine hot section components, rocket engine combustion chamber liners, high-temperature components of advanced space power systems, and atmospheric reentry vehicle surfaces. As part of the volume of papers recognizing 70 years of research at the GRC, this paper summarizes key research contributions that GRC has made to the field of high-temperature aerospace materials. DOI: 10.1061/(ASCE)AS.1943-5525.0000321. (C) 2013 American Society of Civil Engineers.
C1 [Dever, Joyce A.] NASA, Durabil & Protect Coatings Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Nathal, Michael V.] NASA, Adv Metall Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
[DiCarlo, James A.] NASA, Struct & Mat Div, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Dever, JA (reprint author), NASA, Durabil & Protect Coatings Branch, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM Joyce.A.Dever@nasa.gov; Michael.V.Nathal@nasa.gov;
James.A.DiCarlo@nasa.gov
NR 102
TC 4
Z9 5
U1 2
U2 61
PU ASCE-AMER SOC CIVIL ENGINEERS
PI RESTON
PA 1801 ALEXANDER BELL DR, RESTON, VA 20191-4400 USA
SN 0893-1321
J9 J AEROSPACE ENG
JI J. Aerosp. Eng.
PD APR
PY 2013
VL 26
IS 2
SI SI
BP 500
EP 514
DI 10.1061/(ASCE)AS.1943-5525.0000321
PG 15
WC Engineering, Aerospace; Engineering, Civil
SC Engineering
GA 118YR
UT WOS:000317063900023
ER
PT J
AU Kaufman, I
Luchinsky, DG
Tindjong, R
McClintock, PVE
Eisenberg, RS
AF Kaufman, I.
Luchinsky, D. G.
Tindjong, R.
McClintock, P. V. E.
Eisenberg, R. S.
TI Multi-ion conduction bands in a simple model of calcium ion channels
SO PHYSICAL BIOLOGY
LA English
DT Article
ID GATED SODIUM-CHANNEL; SELECTIVITY; PERMEATION; MECHANISM; SIMULATION;
MUTATIONS; MEMBRANE
AB We report self-consistent Brownian dynamics simulations of a simple electrostatic model of the selectivity filters (SF) of calcium ion channels. They reveal regular structure in the conductance and selectivity as functions of the fixed negative charge Q(f) at the SF. With increasing Q(f), there are distinct regions of high conductance (conduction bands) M0, M1, M2 separated by regions of almost zero-conductance (stop-bands). Two of these conduction bands, M1 and M2, are related to the saturated calcium occupancies of P = 1 and P = 2, respectively and demonstrate self-sustained conductivity. Despite the model's limitations, its M1 and M2 bands show high calcium selectivity and prominent anomalous mole fraction effects and can be identified with the L-type and RyR calcium channels. The non-selective band M0 can be identified with a non-selective cation channel, or with OmpF porin.
C1 [Kaufman, I.; Luchinsky, D. G.; Tindjong, R.; McClintock, P. V. E.] Univ Lancaster, Dept Phys, Lancaster LA1 4YB, England.
[Luchinsky, D. G.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Eisenberg, R. S.] Rush Med Coll, Dept Physiol & Mol Biophys, Chicago, IL 60612 USA.
RP Kaufman, I (reprint author), Univ Lancaster, Dept Phys, Lancaster LA1 4YB, England.
EM p.v.e.mcclintock@lancaster.ac.uk
FU Engineering and Physical Sciences Research Council (EPSRC)
[EP/G070660/1]
FX This work was supported by Engineering and Physical Sciences Research
Council (EPSRC) (grant no EP/G070660/1).
NR 36
TC 12
Z9 12
U1 1
U2 17
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1478-3967
EI 1478-3975
J9 PHYS BIOL
JI Phys. Biol.
PD APR
PY 2013
VL 10
IS 2
AR 026007
DI 10.1088/1478-3975/10/2/026007
PG 8
WC Biochemistry & Molecular Biology; Biophysics
SC Biochemistry & Molecular Biology; Biophysics
GA 119NE
UT WOS:000317103500013
PM 23481350
ER
PT J
AU Cutler, AD
Harding, GC
Diskin, GS
AF Cutler, A. D.
Harding, G. C.
Diskin, G. S.
TI High Frequency Pulsed Injection into a Supersonic Duct Flow
SO AIAA JOURNAL
LA English
DT Article
ID CROSS-FLOW; JETS; PENETRATION
AB A study is presented of the effect of pulsation (100% modulation) of a sonic jet of helium into a supersonic (ducted) crossflow on its mixing. An injector was developed to provide a high-speed high-frequency (up to 13 kHz) pulsed jet. The injector nozzle is formed between fixed internal passages and a three- or four-sided wheel embedded within the device that rotates due to the flow in the nozzle. For a given geometry the pulsation frequency is repeatable, constant above a certain pressure ratio, and scales with the speed of sound of the gas. The pulsed jet in the crossflow was visualized in a side view by schlieren photography. The plume of injected helium was visualized in a cross section, 69 effective jet diameters downstream of injection, by seeding the helium with a small amount of ethanol, which condensed as tiny particles and illuminated with a laser light sheet. Results indicate a modest reduction in mean plume cross-sectional size (and, therefore, reduction of mixing) with pulsation and an increase in mean helium penetration. The visualization results are consistent with a transitional state between the turbulent puffs and vortex rings previously observed in low-speed experiments on subsonic pulsed jets in crossflow.
C1 [Cutler, A. D.; Harding, G. C.] George Washington Univ, Newport News, VA 23602 USA.
[Diskin, G. S.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Cutler, AD (reprint author), George Washington Univ, Newport News, VA 23602 USA.
NR 27
TC 2
Z9 2
U1 1
U2 18
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 APR
PY 2013
VL 51
IS 4
BP 809
EP 818
DI 10.2514/1.J051620
PG 10
WC Engineering, Aerospace
SC Engineering
GA 115QP
UT WOS:000316827300005
ER
PT J
AU Erkmen, BI
Barber, ZW
Dahl, J
AF Erkmen, Baris I.
Barber, Zeb W.
Dahl, Jason
TI Maximum-likelihood estimation for frequency-modulated continuous-wave
laser ranging using photon-counting detectors
SO APPLIED OPTICS
LA English
DT Article
ID HETERODYNE-DETECTION; PERFORMANCE; RADAR; LADAR
AB We analyze the minimum achievable mean-square error in frequency-modulated continuous-wave range estimation of a single stationary target when photon-counting detectors are employed. Starting from the probability density function for the photon-arrival times in photodetectors with subunity quantum efficiency, dark counts, and dead time, we derive the Cramer-Rao bound and highlight three important asymptotic regimes. We then derive the maximum-likelihood (ML) estimator for arbitrary frequency modulation. Simulation of the ML estimator shows that its performance approaches the standard quantum limit only when the mean received photons are between two thresholds. We provide analytic approximations to these thresholds for linear frequency modulation. We also compare the ML estimator's performance to conventional Fourier transform (FT) frequency estimation, showing that they are equivalent if the reference arm is much stronger than the target return, but that when the reference field is weak the FT estimator is suboptimal by approximately a factor of root 2 in root-mean-square error. Finally, we report on a proof-of-concept experiment in which the ML estimator achieves this theoretically predicted improvement over the FT estimator. (C) 2013 Optical Society of America
C1 [Erkmen, Baris I.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Barber, Zeb W.; Dahl, Jason] Montana State Univ, Spectrum Lab, Bozeman, MT 59717 USA.
RP Erkmen, BI (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM baris.i.erkmen@jpl.nasa.gov
FU DARPA InPho [PROP. 81-17433]; National Aeronautics and Space
Administration; DARPA InPho, Army Research Office [W911NF-11-1-0540]
FX The authors thank the anonymous reviewers for their detailed feedback,
which has greatly improved the manuscript. BIE's contributions to the
research described in this paper were supported by the DARPA InPho,
contract PROP. 81-17433, and were carried out by the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration. ZWB's and JD's
contributions were supported by DARPA InPho, Army Research Office Grant
W911NF-11-1-0540.
NR 21
TC 1
Z9 1
U1 1
U2 8
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 APR 1
PY 2013
VL 52
IS 10
BP 2008
EP 2018
DI 10.1364/AO.52.002008
PG 11
WC Optics
SC Optics
GA 117YB
UT WOS:000316988100016
PM 23545955
ER
PT J
AU Werdell, PJ
Franz, BA
Bailey, SW
Feldman, GC
Boss, E
Brando, VE
Dowell, M
Hirata, T
Lavender, SJ
Lee, ZP
Loisel, H
Maritorena, S
Melin, F
Moore, TS
Smyth, TJ
Antoine, D
Devred, E
d'Andon, OHF
Mangin, A
AF Werdell, P. Jeremy
Franz, Bryan A.
Bailey, Sean W.
Feldman, Gene C.
Boss, Emmanuel
Brando, Vittorio E.
Dowell, Mark
Hirata, Takafumi
Lavender, Samantha J.
Lee, ZhongPing
Loisel, Hubert
Maritorena, Stephane
Melin, Frederic
Moore, Timothy S.
Smyth, Timothy J.
Antoine, David
Devred, Emmanuel
d'Andon, Odile Hembise Fanton
Mangin, Antoine
TI Generalized ocean color inversion model for retrieving marine inherent
optical properties
SO APPLIED OPTICS
LA English
DT Article
ID WATER-LEAVING RADIANCES; PHYTOPLANKTON ABSORPTION; CHLOROPHYLL-A;
SEMIANALYTICAL MODEL; LIGHT ATTENUATION; BIOOPTICAL MODEL; COASTAL
WATERS; CHESAPEAKE BAY; DATA PRODUCTS; TIME-SERIES
AB Ocean color measured from satellites provides daily, global estimates of marine inherent optical properties (IOPs). Semi-analytical algorithms (SAAs) provide one mechanism for inverting the color of the water observed by the satellite into IOPs. While numerous SAAs exist, most are similarly constructed and few are appropriately parameterized for all water masses for all seasons. To initiate community-wide discussion of these limitations, NASA organized two workshops that deconstructed SAAs to identify similarities and uniqueness and to progress toward consensus on a unified SAA. This effort resulted in the development of the generalized IOP (GIOP) model software that allows for the construction of different SAAs at runtime by selection from an assortment of model parameterizations. As such, GIOP permits isolation and evaluation of specific modeling assumptions, construction of SAAs, development of regionally tuned SAAs, and execution of ensemble inversion modeling. Working groups associated with the workshops proposed a preliminary default configuration for GIOP (GIOP-DC), with alternative model parameterizations and features defined for subsequent evaluation. In this paper, we: (1) describe the theoretical basis of GIOP; (2) present GIOP-DC and verify its comparable performance to other popular SAAs using both in situ and synthetic data sets; and, (3) quantify the sensitivities of their output to their parameterization. We use the latter to develop a hierarchical sensitivity of SAAs to various model parameterizations, to identify components of SAAs that merit focus in future research, and to provide material for discussion on algorithm uncertainties and future emsemble applications. (C) 2013 Optical Society of America
C1 [Werdell, P. Jeremy; Franz, Bryan A.; Bailey, Sean W.; Feldman, Gene C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Werdell, P. Jeremy; Boss, Emmanuel] Univ Maine, Sch Marine Sci, Orono, ME 04401 USA.
[Bailey, Sean W.] Futuretech Corp, Greenbelt, MD 20770 USA.
[Brando, Vittorio E.] CSIRO Land & Water, Environm Earth Observat Program, Canberra, ACT, Australia.
[Dowell, Mark; Melin, Frederic] Commiss European Communities, Joint Res Ctr, I-21027 Ispra, Italy.
[Hirata, Takafumi] Hokkaido Univ, Fac Environm Earth Sci, Sapporo, Hokkaido 0600810, Japan.
[Lavender, Samantha J.] Pixalytics Ltd, Plymouth PL6 8BX, Devon, England.
[Lee, ZhongPing] Univ Massachusetts, Boston, MA 02125 USA.
[Loisel, Hubert] Univ Littoral Cote dOpale, Lab Oceanol & Geosci, F-62930 Wimereux, France.
[Maritorena, Stephane] Univ Calif Santa Barbara, Earth Res Inst, Santa Barbara, CA 93106 USA.
[Moore, Timothy S.] Univ New Hampshire, Ocean Proc Anal Lab, Durham, NH 03824 USA.
[Smyth, Timothy J.] Plymouth Marine Lab, Plymouth PL1 3DH, Devon, England.
[Antoine, David] CNRS, Lab Oceanog Villefranche, F-06238 Villefranche Sur Mer, France.
[Devred, Emmanuel] Univ Laval, Joint Int Lab, Unite Mixte Int Takuv, Quebec City, PQ GV1 0AG, Canada.
[d'Andon, Odile Hembise Fanton; Mangin, Antoine] ACRI ST, F-06904 Sophia Antipolis, France.
RP Werdell, PJ (reprint author), NASA, Goddard Space Flight Ctr, Code 616, Greenbelt, MD 20771 USA.
EM jeremy.werdell@nasa.gov
RI Antoine, David/C-3817-2013; Werdell, Jeremy/D-8265-2012; Boss,
Emmanuel/C-5765-2009; Franz, Bryan/D-6284-2012; Brando,
Vittorio/A-1321-2008; Hirata, Takafumi/F-7854-2012; Bailey,
Sean/D-3077-2017
OI Antoine, David/0000-0002-9082-2395; Boss, Emmanuel/0000-0002-8334-9595;
Franz, Bryan/0000-0003-0293-2082; Brando, Vittorio/0000-0002-2193-5695;
Hirata, Takafumi/0000-0003-1258-1837; Bailey, Sean/0000-0001-8339-9763
FU NASA MODIS Science Team; CSIRO Wealth from Oceans Flagship
FX We thank Mike Behrenfeld, Paula Bontempi, Catherine Brown, Yannick Huot,
Paul Lyon, Constant Mazeran, and Jill Schwarz for their helpful advice
and participation in the NASA GIOP workshops. We also thank an anonymous
reviewer for useful comments that improved this manuscript. Support for
this work was provided through the NASA MODIS Science Team (P.J.W., B.
A. F., S. W. B.) and the CSIRO Wealth from Oceans Flagship (V.B.).
NR 60
TC 51
Z9 52
U1 7
U2 49
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 APR 1
PY 2013
VL 52
IS 10
BP 2019
EP 2037
DI 10.1364/AO.52.002019
PG 19
WC Optics
SC Optics
GA 117YB
UT WOS:000316988100017
PM 23545956
ER
PT J
AU Chaplin, WJ
Sanchis-Ojeda, R
Campante, TL
Handberg, R
Stello, D
Winn, JN
Basu, S
Christensen-Dalsgaard, J
Davies, GR
Metcalfe, TS
Buchhave, LA
Fischer, DA
Bedding, TR
Cochran, WD
Elsworth, Y
Gilliland, RL
Hekker, S
Huber, D
Isaacson, H
Karoff, C
Kawaler, SD
Kjeldsen, H
Latham, DW
Lund, MN
Lundkvist, M
Marcy, GW
Miglio, A
Barclay, T
Lissauer, JJ
AF Chaplin, W. J.
Sanchis-Ojeda, R.
Campante, T. L.
Handberg, R.
Stello, D.
Winn, J. N.
Basu, S.
Christensen-Dalsgaard, J.
Davies, G. R.
Metcalfe, T. S.
Buchhave, L. A.
Fischer, D. A.
Bedding, T. R.
Cochran, W. D.
Elsworth, Y.
Gilliland, R. L.
Hekker, S.
Huber, D.
Isaacson, H.
Karoff, C.
Kawaler, S. D.
Kjeldsen, H.
Latham, D. W.
Lund, M. N.
Lundkvist, M.
Marcy, G. W.
Miglio, A.
Barclay, T.
Lissauer, J. J.
TI ASTEROSEISMIC DETERMINATION OF OBLIQUITIES OF THE EXOPLANET SYSTEMS
KEPLER-50 AND KEPLER-65
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE asteroseismology; planets and satellites: formation; planets and
satellites: general; stars: rotation
ID SPIN-ORBIT MISALIGNMENT; SOLAR-TYPE STARS; TRANSIT TIMING OBSERVATIONS;
RAPIDLY ROTATING STARS; OF-STATE TABLES; SUN-LIKE STAR; PLANET
CANDIDATES; LIGHT CURVES; PHOTOMETRIC VARIABILITY; INITIAL
CHARACTERISTICS
AB Results on the obliquity of exoplanet host stars-the angle between the stellar spin axis and the planetary orbital axis-provide important diagnostic information for theories describing planetary formation. Here we present the first application of asteroseismology to the problem of stellar obliquity determination in systems with transiting planets and Sun-like host stars. We consider two systems observed by the NASA Kepler mission which have multiple transiting small (super-Earth sized) planets: the previously reported Kepler-50 and a new system, Kepler-65, whose planets we validate in this paper. Both stars show rich spectra of solar-like oscillations. From the asteroseismic analysis we find that each host has its rotation axis nearly perpendicular to the line of sight with the sines of the angles constrained at the 1 sigma level to lie above 0.97 and 0.91, respectively. We use statistical arguments to show that coplanar orbits are favored in both systems, and that the orientations of the planetary orbits and the stellar rotation axis are correlated.
C1 [Chaplin, W. J.; Campante, T. L.; Davies, G. R.; Elsworth, Y.; Hekker, S.; Miglio, A.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Sanchis-Ojeda, R.; Winn, J. N.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Handberg, R.; Christensen-Dalsgaard, J.; Karoff, C.; Kjeldsen, H.; Lund, M. N.; Lundkvist, M.] Aarhus Univ, Dept Phys & Astron, SAC, DK-8000 Aarhus C, Denmark.
[Stello, D.; Bedding, T. R.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Basu, S.; Fischer, D. A.] Yale Univ, New Haven, CT 06520 USA.
[Metcalfe, T. S.] White Dwarf Res Corp, Boulder, CO 80301 USA.
[Buchhave, L. A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Buchhave, L. A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1530 Copenhagen, Denmark.
[Cochran, W. D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Gilliland, R. L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Hekker, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Huber, D.; Barclay, T.; Lissauer, J. J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Isaacson, H.; Marcy, G. W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Kawaler, S. D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Latham, D. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Barclay, T.] Environm Res Inst, Bay Area, Sonoma, CA 95476 USA.
RP Chaplin, WJ (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
OI Kawaler, Steven/0000-0002-6536-6367; Bedding,
Timothy/0000-0001-5943-1460; Davies, Guy/0000-0002-4290-7351; Buchhave,
Lars A./0000-0003-1605-5666; Metcalfe, Travis/0000-0003-4034-0416;
Karoff, Christoffer/0000-0003-2009-7965; Bedding,
Tim/0000-0001-5222-4661; Basu, Sarbani/0000-0002-6163-3472; Lund, Mikkel
Norup/0000-0001-9214-5642; Lundkvist, Mia Sloth/0000-0002-8661-2571;
Fischer, Debra/0000-0003-2221-0861; Handberg, Rasmus/0000-0001-8725-4502
FU NASA's Science Mission Directorate; UK Science and Technology Facilities
Council (STFC); NASA Kepler Participating Scientist program
[NNX12AC76G]; NSF [AST 1105930]; Danish National Research Foundation;
ASTERISK project (ASTERoseismic Investigations with SONG and Kepler);
European Research Council [267864]; Netherlands Organisation for
Scientific Research (NWO); International Space Science Institute (ISSI)
FX Funding for this Discovery mission is provided by NASA's Science Mission
Directorate. The authors wish to thank the entire Kepler team, without
whom these results would not be possible. W.J.C., T.L.C., G.R. D., Y.E.,
and A. M. acknowledge the support of the UK Science and Technology
Facilities Council (STFC). J.N.W. was supported by the NASA Kepler
Participating Scientist program through grant NNX12AC76G. S.B.
acknowledges NSF grant AST 1105930. Funding for the Stellar Astrophysics
Centre (SAC) is provided by The Danish National Research Foundation. The
research is supported by the ASTERISK project (ASTERoseismic
Investigations with SONG and Kepler) funded by the European Research
Council (grant agreement no.:267864). S.H. acknowledges financial
support from the Netherlands Organisation for Scientific Research (NWO).
Computational time on Kraken at the National Institute of Computational
Sciences was provided through NSF TeraGrid allocation TG-AST090107. We
acknowledge the Pale Blue Dot Project, hosted by White Dwarf Research
Corporation (whitedwarf.org/palebluedot), and we are also grateful for
support from the International Space Science Institute (ISSI).
NR 124
TC 68
Z9 68
U1 1
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2013
VL 766
IS 2
AR 101
DI 10.1088/0004-637X/766/2/101
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 108UE
UT WOS:000316320900035
ER
PT J
AU Filacchione, G
Capaccioni, F
Clark, RN
Nicholson, PD
Cruikshank, DP
Cuzzi, JN
Lunine, JI
Brown, RH
Cerroni, P
Tosi, F
Ciarniello, M
Buratti, BJ
Hedman, MM
Flamini, E
AF Filacchione, G.
Capaccioni, F.
Clark, R. N.
Nicholson, P. D.
Cruikshank, D. P.
Cuzzi, J. N.
Lunine, J. I.
Brown, R. H.
Cerroni, P.
Tosi, F.
Ciarniello, M.
Buratti, B. J.
Hedman, M. M.
Flamini, E.
TI THE RADIAL DISTRIBUTION OF WATER ICE AND CHROMOPHORES ACROSS SATURN'S
SYSTEM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites: composition; planets and satellites: rings
ID CASSINI-VIMS; SURFACE-COMPOSITION; DARK MATERIAL; RINGS; SATELLITES;
SPECTRA; IAPETUS; ENCELADUS; PHOEBE; DISK
AB Over the past eight years, the Visual and Infrared Mapping Spectrometer (VIMS) on board the Cassini orbiter has returned hyperspectral images in the 0.35-5.1 mu m range of the icy satellites and rings of Saturn. These very different objects show significant variations in surface composition, roughness, and regolith grain size as a result of their evolutionary histories, endogenic processes, and interactions with exogenic particles. The distributions of surface water ice and chromophores, i.e., organic and non-icy materials, across the Saturnian system, are traced using specific spectral indicators (spectral slopes and absorption band depths) obtained from rings mosaics and disk-integrated satellites observations by VIMS. Moving from the inner C ring to Iapetus, we found a marking uniformity in the distribution of abundance of water ice. On the other hand, the distribution of chromophores is much more concentrated in the rings particles and on the outermost satellites (Rhea, Hyperion, and Iapetus). A reduction of red material is observed on the satellites' surfaces orbiting within the E ring environment likely due to fine particles from Enceladus' plumes. Once the exogenous dark material covering the Iapetus' leading hemisphere is removed, the texture of the water ice-rich surfaces, inferred through the 2 mu m band depth, appears remarkably uniform across the entire system.
C1 [Filacchione, G.; Capaccioni, F.; Cerroni, P.; Tosi, F.; Ciarniello, M.] Area Ric Tor Vergata, Ist Astrofis & Planetol Spaziali, INAF IAPS, I-00133 Rome, Italy.
[Clark, R. N.] US Geol Survey, Fed Ctr, Denver, CO 80228 USA.
[Nicholson, P. D.; Lunine, J. I.; Hedman, M. M.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Cruikshank, D. P.; Cuzzi, J. N.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Brown, R. H.] Univ Arizona, Lunar Planetary Lab, Tucson, AZ 85721 USA.
[Buratti, B. J.] CALTECH, NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
[Flamini, E.] Italian Space Agcy, ASI, I-00198 Rome, Italy.
RP Filacchione, G (reprint author), Area Ric Tor Vergata, Ist Astrofis & Planetol Spaziali, INAF IAPS, Via Fosso Cavaliere 100, I-00133 Rome, Italy.
EM gianrico.filacchione@iaps.inaf.it
OI Ciarniello, Mauro/0000-0002-7498-5207; Cerroni,
Priscilla/0000-0003-0239-2741; Capaccioni, Fabrizio/0000-0003-1631-4314;
Filacchione, Gianrico/0000-0001-9567-0055; Tosi,
Federico/0000-0003-4002-2434
FU Italian Space Agency [I/015/09/0]; NASA through the Cassini project
FX This research has made use of NASA's Astrophysics Data System and was
completed thanks to the financial support of the Italian Space Agency
(grant I/015/09/0) and NASA through the Cassini project.
NR 30
TC 6
Z9 6
U1 0
U2 12
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2013
VL 766
IS 2
AR 76
DI 10.1088/0004-637X/766/2/76
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 108UE
UT WOS:000316320900010
ER
PT J
AU Fressin, F
Torres, G
Charbonneau, D
Bryson, ST
Christiansen, J
Dressing, CD
Jenkins, JM
Walkowicz, LM
Batalha, NM
AF Fressin, Francois
Torres, Guillermo
Charbonneau, David
Bryson, Stephen T.
Christiansen, Jessie
Dressing, Courtney D.
Jenkins, Jon M.
Walkowicz, Lucianne M.
Batalha, Natalie M.
TI THE FALSE POSITIVE RATE OF KEPLER AND THE OCCURRENCE OF PLANETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; methods: data analysis; methods: statistical;
planetary systems
ID TRANSIT TIMING VARIATIONS; SOLAR-TYPE STARS; SUN-LIKE STARS; ECLIPSING
BINARIES; BLEND SCENARIOS; MULTIPLE SYSTEM; HABITABLE-ZONE; INPUT
CATALOG; DATA RELEASE; CANDIDATES
AB The Kepler mission is uniquely suited to study the frequencies of extrasolar planets. This goal requires knowledge of the incidence of false positives such as eclipsing binaries in the background of the targets, or physically bound to them, which can mimic the photometric signal of a transiting planet. We perform numerical simulations of the Kepler targets and of physical companions or stars in the background to predict the occurrence of astrophysical false positives detectable by the mission. Using real noise level estimates, we compute the number and characteristics of detectable eclipsing pairs involving main-sequence stars and non-main-sequence stars or planets, and we quantify the fraction of those that would pass the Kepler candidate vetting procedure. By comparing their distribution with that of the Kepler Objects of Interest (KOIs) detected during the first six quarters of operation of the spacecraft, we infer the false positive rate of Kepler and study its dependence on spectral type, candidate planet size, and orbital period. We find that the global false positive rate of Kepler is 9.4%, peaking for giant planets (6-22 R-circle plus) at 17.7%, reaching a low of 6.7% for small Neptunes (2-4 R-circle plus), and increasing again for Earth-size planets (0.8-1.25 R-circle plus) to 12.3%. Most importantly, we also quantify and characterize the distribution and rate of occurrence of planets down to Earth size with no prior assumptions on their frequency, by subtracting from the population of actual Kepler candidates our simulated population of astrophysical false positives. We find that 16.5% +/- 3.6% of main-sequence FGK stars have at least one planet between 0.8 and 1.25 R-circle plus with orbital periods up to 85 days. This result is a significant step toward the determination of eta-earth, the occurrence of Earth-like planets in the habitable zone of their parent stars. There is no significant dependence of the rates of planet occurrence between 0.8 and 4 Earth radii with spectral type. In the process, we also derive a prescription for the signal recovery rate of Kepler that enables a good match to both the KOI size and orbital period distribution, as well as their signal-to-noise distribution.
C1 [Fressin, Francois; Torres, Guillermo; Charbonneau, David; Dressing, Courtney D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bryson, Stephen T.; Christiansen, Jessie; Jenkins, Jon M.; Batalha, Natalie M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Walkowicz, Lucianne M.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
RP Fressin, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ffressin@cfa.harvard.edu
OI Charbonneau, David/0000-0002-9003-484X
FU NASA [NNX12AC75G]
FX We thank the anonymous referee for helpful suggestions on the original
manuscript. G.T. acknowledges partial support for this work from NASA
Grant NNX12AC75G (Kepler Participating Scientist Program).
NR 46
TC 329
Z9 331
U1 10
U2 51
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2013
VL 766
IS 2
AR 81
DI 10.1088/0004-637X/766/2/81
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 108UE
UT WOS:000316320900015
ER
PT J
AU Hunana, P
Goldstein, ML
Passot, T
Sulem, PL
Laveder, D
Zank, GP
AF Hunana, P.
Goldstein, M. L.
Passot, T.
Sulem, P. L.
Laveder, D.
Zank, G. P.
TI POLARIZATION AND COMPRESSIBILITY OF OBLIQUE KINETIC ALFVEN WAVES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetohydrodynamics (MHD); solar wind; turbulence; waves
ID WEAKLY COLLISIONAL PLASMAS; LOW-FREQUENCY WAVES; SOLAR-WIND;
MAGNETOHYDRODYNAMIC TURBULENCE; ASTROPHYSICAL GYROKINETICS; HALL-MHD;
FLUID; MODEL; FLUCTUATIONS; EQUATIONS
AB It is well known that a complete description of the solar wind requires a kinetic description and that, particularly at sub-proton scales, kinetic effects cannot be ignored. It is nevertheless usually assumed that at scales significantly larger than the proton gyroscale r(L), magnetohydrodynamics or its extensions, such as Hall-MHD and two-fluid models with isotropic pressures, provide a satisfactory description of the solar wind. Here we calculate the polarization and magnetic compressibility of oblique kinetic Alfven waves and show that, compared with linear kinetic theory, the isotropic two-fluid description is very compressible, with the largest discrepancy occurring at scales larger than the proton gyroscale. In contrast, introducing anisotropic pressure fluctuations with the usual double-adiabatic (or CGL) equations of state yields compressibility values which are unrealistically low. We also show that both of these classes of fluid models incorrectly describe the electric field polarization. To incorporate linear kinetic effects, we use two versions of the Landau fluid model that include linear Landau damping and finite Larmor radius (FLR) corrections. We show that Landau damping is crucial for correct modeling of magnetic compressibility, and that the anisotropy of pressure fluctuations should not be introduced without taking into account the Landau damping through appropriate heat flux equations. We also show that FLR corrections to all the retained fluid moments appear to be necessary to yield the correct polarization. We conclude that kinetic effects cannot be ignored even for kr(L) << 1.
C1 [Hunana, P.; Goldstein, M. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Passot, T.; Sulem, P. L.; Laveder, D.] Univ Nice Sophia Antipolis, CNRS, Lab JL Lagrange, Observ Cote Azur, F-06304 Nice 4, France.
[Zank, G. P.] Univ Alabama, CSPAR, Huntsville, AL 35805 USA.
[Zank, G. P.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
RP Hunana, P (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
FU Magnetospheric Multiscale mission at the Goddard Space Flight Center;
European Commission's Seventh Framework Programme [284515]; INSU-CNRS
"Programme Soleil-Terre"; NASA [NNX08AJ33G, Subaward 37102-2,
NNX09AG70G, NNX09AG63G, NNX09AJ79G, NNG05EC85C, Subcontract A991132BT,
NNX09AP74A]
FX P.H. was supported by NASA Postdoctoral Program, which is administered
by Oak Ridge Associated Universities (ORAU). M.L.G. was supported, in
part, by the Interdisciplinary Science program of the Magnetospheric
Multiscale mission at the Goddard Space Flight Center. The research
leading to these results has received funding from the European
Commission's Seventh Framework Programme (FP7/2007-2013) under the grant
agreement SHOCK (Project No. 284515). The support of INSU-CNRS
"Programme Soleil-Terre" is also acknowledged. We acknowledge the
partial support of NASA grants NNX08AJ33G, Subaward 37102-2, NNX09AG70G,
NNX09AG63G, NNX09AJ79G, NNG05EC85C, Subcontract A991132BT, NNX09AP74A,
NNX10AE46G, NNX09AW45G, and NSF grant ATM-0904007.
NR 45
TC 15
Z9 15
U1 1
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2013
VL 766
IS 2
AR 93
DI 10.1088/0004-637X/766/2/93
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 108UE
UT WOS:000316320900027
ER
PT J
AU Paganini, L
Mumma, MJ
Boehnhardt, H
DiSanti, MA
Villanueva, GL
Bonev, BP
Lippi, M
Kaufl, HU
Blake, GA
AF Paganini, Lucas
Mumma, Michael J.
Boehnhardt, Hermann
DiSanti, Michael A.
Villanueva, Geronimo L.
Bonev, Boncho P.
Lippi, Manuela
Kaeufl, Hans U.
Blake, Geoffrey A.
TI GROUND-BASED INFRARED DETECTIONS OF CO IN THE CENTAUR-COMET
29P/SCHWASSMANN-WACHMANN 1 AT 6.26 AU FROM THE SUN
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; comets: general; comets: individual
(29P/Schwassmann-Wachmann 1); Kuiper belt: general; molecular processes;
planets and satellites: formation
ID JUPITER-FAMILY COMETS; KUIPER-BELT OBJECTS; C/2009 P1 GARRADD; O1
HALE-BOPP; CARBON-MONOXIDE; CHEMICAL-COMPOSITION; OUTBURST ACTIVITY;
MODEL; BAND; ATMOSPHERES
AB We observed Comet 29P/Schwassmann-Wachmann 1 (hereafter, 29P) in 2012 February and May with CRIRES/VLT and NIRSPEC/Keck-II, when the comet was at 6.26 AU from the Sun and about 5.50 AU from Earth. With CRIRES, we detected five CO emission lines on several nights in each epoch, confirming the ubiquitous content and release of carbon monoxide from the nucleus. This is the first simultaneous detection of multiple lines from any (neutral) gaseous species in comet 29P at infrared wavelengths. It is also the first extraction of a rotational temperature based on the intensities of simultaneously measured spectral lines in 29P, and the retrieved rotational temperature is the lowest obtained in our infrared survey to date. We present the retrieved production rates (similar to 3 x 10(28) molecules s(-1)) and remarkably low (similar to 5 K) rotational temperatures for CO, and compare them with results from previous observations at radio wavelengths. Along with CO, we pursued detections of other volatiles, namely H2O, C2H6, C2H2, CH4, HCN, NH3, and CH3OH. Although they were not detected, we present sensitive upper limits. These results establish a new record for detections by infrared spectroscopy of parent volatiles in comets at large heliocentric distances. Until now considered to be a somewhat impossible task with IR ground-based facilities, these discoveries demonstrate new opportunities for targeting volatile species in distant comets.
C1 [Paganini, Lucas; Mumma, Michael J.; DiSanti, Michael A.; Villanueva, Geronimo L.; Bonev, Boncho P.] NASA GSFC, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA.
[Boehnhardt, Hermann; Lippi, Manuela] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Villanueva, Geronimo L.; Bonev, Boncho P.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Kaeufl, Hans U.] ESO, D-85748 Garching, Germany.
[Blake, Geoffrey A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Paganini, L (reprint author), NASA GSFC, Goddard Ctr Astrobiol, MS 690, Greenbelt, MD 20771 USA.
EM lucas.paganini@nasa.gov
RI mumma, michael/I-2764-2013
FU NASA; NSF; Max-Planck-Gesellschaft; German-Israeli Foundation for
Scientific Research and Development
FX We thank the VLT science operations team of the European Southern
Observatory and the W.M. Keck Observatory for efficient operations of
the observatories. L.P. acknowledges Retha Pretorius, Jonathan Smoker
and Carla Aubel for their great assistance, and thanks Michael A'Hearn
and Martin Cordiner for helpful discussions. We are also grateful to
Zhong-Yi Lin and Josep Trigo-Rodriguez for providing magnitude
estimations, and to the anonymous referee for helpful comments. This
work was supported by NASA's Postdoctoral (L.P.), Planetary Astronomy
(PI:M.J.M. and PI:M.A.D.), and Astrobiology Programs (PI:M.J.M.), NSF
(PI:B.P.B.), the Max-Planck-Gesellschaft (H.B.), and the German-Israeli
Foundation for Scientific Research and Development (H.B. and M.L.).
NR 72
TC 9
Z9 9
U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2013
VL 766
IS 2
AR 100
DI 10.1088/0004-637X/766/2/100
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 108UE
UT WOS:000316320900034
ER
PT J
AU Reynolds, MT
Loi, ST
Murphy, T
Miller, JM
Maitra, D
Gultekin, K
Gehrels, N
Kennea, JA
Siegel, MH
Gelbord, J
Kuin, P
Moss, V
Reeves, S
Robbins, WJ
Gaensler, BM
Reis, RC
Petre, R
AF Reynolds, Mark T.
Loi, Shyeh T.
Murphy, Tara
Miller, Jon M.
Maitra, Dipankar
Gueltekin, Kayhan
Gehrels, Neil
Kennea, Jamie A.
Siegel, Michael H.
Gelbord, Jonathan
Kuin, Paul
Moss, Vanessa
Reeves, Sarah
Robbins, William J.
Gaensler, B. M.
Reis, Rubens C.
Petre, Robert
TI G306.3-0.9: A NEWLY DISCOVERED YOUNG GALACTIC SUPERNOVA REMNANT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: individual objects: (G306.3-0.9); ISM: supernova remnants
ID LARGE-MAGELLANIC-CLOUD; X-RAY SPECTROSCOPY; SOURCE CATALOG; EXPLOSION;
ABUNDANCES; EMISSION; PULSARS; MODELS; PLANE; N132D
AB We present X-ray and radio observations of the new Galactic supernova remnant (SNR) G306.3-0.9, recently discovered by Swift. Chandra imaging reveals a complex morphology, dominated by a bright shock. The X-ray spectrum is broadly consistent with a young SNR in the Sedov phase, implying an age of 2500 yr for a distance of 8 kpc, plausibly identifying this as one of the 20 youngest Galactic SNRs. Australia Telescope Compact Array imaging reveals a prominent ridge of radio emission that correlates with the X-ray emission. We find a flux density of similar to 160 mJy at 1 GHz, which is the lowest radio flux recorded for a Galactic SNR to date. The remnant is also detected at 24 mu m, indicating the presence of irradiated warm dust. The data reveal no compelling evidence for the presence of a compact stellar remnant.
C1 [Reynolds, Mark T.; Miller, Jon M.; Maitra, Dipankar; Gueltekin, Kayhan; Reis, Rubens C.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Loi, Shyeh T.; Murphy, Tara; Moss, Vanessa; Reeves, Sarah; Robbins, William J.; Gaensler, B. M.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
[Murphy, Tara] Univ Sydney, Sch Informat Technol, Sydney, NSW 2006, Australia.
[Gehrels, Neil; Petre, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kennea, Jamie A.; Siegel, Michael H.; Gelbord, Jonathan] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Kuin, Paul] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
RP Reynolds, MT (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA.
EM markrey@umich.edu
RI Gaensler, Bryan/F-8655-2010;
OI Loi, Shyeh Tjing/0000-0002-6528-4548; Murphy, Tara/0000-0002-2686-438X;
Moss, Vanessa/0000-0002-3005-9738; reis, rubens/0000-0002-6618-2412;
Gaensler, Bryan/0000-0002-3382-9558; Gultekin,
Kayhan/0000-0002-1146-0198
FU Commonwealth of Australia; Chandra guest investigator program
FX We acknowledge the use of public data from the Swift data archive. We
thank CXC director Harvey Tananbaum for his allocation of Director's
time. The ATCA is part of the ATNF which is funded by the Commonwealth
of Australia for operation as a National Facility managed by CSIRO.
J.M.M. acknowledges support through the Chandra guest investigator
program.
NR 37
TC 5
Z9 5
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2013
VL 766
IS 2
AR 112
DI 10.1088/0004-637X/766/2/112
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 108UE
UT WOS:000316320900046
ER
PT J
AU Setvak, M
Bedka, K
Lindsey, DT
Sokol, A
Charvat, Z
St'astka, J
Wang, PK
AF Setvak, Martin
Bedka, Kristopher
Lindsey, Daniel T.
Sokol, Alois
Charvat, Zdenek
St'astka, Jindrich
Wang, Pao K.
TI A-Train observations of deep convective storm tops
SO ATMOSPHERIC RESEARCH
LA English
DT Article
DE Convective storm; Storm-top; Overshooting top; Cold-ring shape; Cold-U
shape; Enhanced-V feature; Lower stratosphere; A-Train, CloudSat;
CALIPSO; MODIS
ID 3-DIMENSIONAL NUMERICAL-SIMULATION; OKLAHOMA TORNADIC STORMS;
UPPER-LEVEL STRUCTURE; SATELLITE-OBSERVATIONS; BRIGHTNESS TEMPERATURES;
WATER-VAPOR; THUNDERSTORM; CLOUDS; STRATOSPHERE; DYNAMICS
AB The paper highlights simultaneous observations of tops of deep convective clouds from several space-borne instruments including the Moderate Resolution Imaging Spectroradiometer (MODIS) of the Aqua satellite, Cloud Profiling Radar (CPR) of the CloudSat satellite, and Cloud-Aerosol Lidar with Orthogonal Polarization (CALIOP) flown on the CALIPSO satellite. These satellites share very close orbits, thus together with several other satellites they are referred to as the "A-Train" constellation. Though the primary responsibility of these satellites and their instrumentation is much broader than observations of fine-scale processes atop convective storms, in this study we document how data from the A-Train can contribute to a better understanding and interpretation of various storm-top features, such as overshooting tops, cold-U/V and cold ring features with their coupled embedded warm areas, above anvil ice plumes and jumping cirrus. The relationships between MODIS multi-spectral brightness temperature difference (BTD) fields and cloud top signatures observed by the CPR and CALIOP are also examined in detail to highlight the variability in BTD signals across convective storm events. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Setvak, Martin; Charvat, Zdenek; St'astka, Jindrich] Czech Hydrometeorol Inst, Prague, Czech Republic.
[Bedka, Kristopher] NASA, Langley Res Ctr, Sci Syst & Applicat Inc, Hampton, VA 23665 USA.
[Lindsey, Daniel T.] NOAA, NESDIS, RAMMB, CIRA,CSU, Ft Collins, CO USA.
[Sokol, Alois] Comenius Univ, Fac Math Phys & Informat, Bratislava, Slovakia.
[St'astka, Jindrich] Charles Univ Prague, Fac Math & Phys, Prague, Czech Republic.
[Wang, Pao K.] Univ Wisconsin Madison, Madison, WI USA.
RP Setvak, M (reprint author), CHMI, Sabatce 17, CZ-14306 Prague 4, Czech Republic.
EM setvak@chmi.cz
RI Lindsey, Dan/F-5607-2010
OI Lindsey, Dan/0000-0002-0967-5683
FU Grant Agency of the Czech Republic [205/07/0905]; Faculty of Mathematics
and Physics of the Charles University, Prague, Czech Republic
[SW-2011-263308]; Grant C/SSAI/ASAP Program [2626-08-021 Task 1-020CY4];
[NSF ATM-0729898]
FX The authors wish to acknowledge Mike Fromm (Naval Research Laboratory,
Washington, D.C.) and Louie Grasso (Cooperative Institute for Research
in the Atmosphere, Ft. Collins, CO) for their valuable comments,
suggestions and/or long-term support of this study, as well as NASA,
NOAA and EUMETSAT for their data used in this study. Parts of this
research were carried out under support of the Grant Agency of the Czech
Republic, project 205/07/0905; Grant SW-2011-263308 of the Faculty of
Mathematics and Physics of the Charles University, Prague, Czech
Republic; Grant NSF ATM-0729898; and Grant C/SSAI/ASAP 2010 Program,
Contract # 2626-08-021 Task 1-020CY4.
NR 43
TC 17
Z9 17
U1 0
U2 23
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0169-8095
J9 ATMOS RES
JI Atmos. Res.
PD APR 1
PY 2013
VL 123
SI SI
BP 229
EP 248
DI 10.1016/j.atmosres.2012.06.020
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 112GL
UT WOS:000316580600019
ER
PT J
AU Bala, G
Krishna, S
Narayanappa, D
Cao, L
Caldeira, K
Nemani, R
AF Bala, G.
Krishna, Sujith
Narayanappa, Devaraju
Cao, Long
Caldeira, Ken
Nemani, Ramakrishna
TI An estimate of equilibrium sensitivity of global terrestrial carbon
cycle using NCAR CCSM4
SO CLIMATE DYNAMICS
LA English
DT Article
DE Climate change; Terrestrial carbon cycle; CO2-physiological effect;
CO2-fertilization; Carbon cycle feedback
ID FUTURE CLIMATE-CHANGE; COUPLED CLIMATE; ATMOSPHERIC CO2; VEGETATION
MODELS; SOIL RESPIRATION; DIOXIDE; FEEDBACKS; ECOSYSTEM; FERTILIZATION;
DYNAMICS
AB Increasing concentrations of atmospheric CO2 influence climate, terrestrial biosphere productivity and ecosystem carbon storage through its radiative, physiological and fertilization effects. In this paper, we quantify these effects for a doubling of CO2 using a low resolution configuration of the coupled model NCAR CCSM4. In contrast to previous coupled climate-carbon modeling studies, we focus on the near-equilibrium response of the terrestrial carbon cycle. For a doubling of CO2, the radiative effect on the physical climate system causes global mean surface air temperature to increase by 2.14 K, whereas the physiological and fertilization on the land biosphere effects cause a warming of 0.22 K, suggesting that these later effects increase global warming by about 10 % as found in many recent studies. The CO2-fertilization leads to total ecosystem carbon gain of 371 Gt-C (28 %) while the radiative effect causes a loss of 131 Gt-C (10 %) indicating that climate warming damps the fertilization-induced carbon uptake over land. Our model-based estimate for the maximum potential terrestrial carbon uptake resulting from a doubling of atmospheric CO2 concentration (285-570 ppm) is only 242 Gt-C. This highlights the limited storage capacity of the terrestrial carbon reservoir. We also find that the terrestrial carbon storage sensitivity to changes in CO2 and temperature have been estimated to be lower in previous transient simulations because of lags in the climate-carbon system. Our model simulations indicate that the time scale of terrestrial carbon cycle response is greater than 500 years for CO2-fertilization and about 200 years for temperature perturbations. We also find that dynamic changes in vegetation amplify the terrestrial carbon storage sensitivity relative to a static vegetation case: because of changes in tree cover, changes in total ecosystem carbon for CO2-direct and climate effects are amplified by 88 and 72 %, respectively, in simulations with dynamic vegetation when compared to static vegetation simulations.
C1 [Bala, G.; Krishna, Sujith; Narayanappa, Devaraju] Indian Inst Sci, Divecha Ctr Climate Change, Ctr Atmospher & Ocean Sci, Bangalore 560012, Karnataka, India.
[Cao, Long] Zhejiang Univ, Dept Earth Sci, Hangzhou 310027, Peoples R China.
[Caldeira, Ken] Carnegie Inst, Dept Global Ecol, Stanford, CA 94305 USA.
[Nemani, Ramakrishna] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Bala, G (reprint author), Indian Inst Sci, Divecha Ctr Climate Change, Ctr Atmospher & Ocean Sci, Bangalore 560012, Karnataka, India.
EM bala.gov@gmail.com
RI Caldeira, Ken/E-7914-2011;
OI krishnakumar, sujith/0000-0001-7429-2809
FU Department of Science and Technology [DST 0948]; Divecha Center for
Climate Change
FX We thank Drs. Chris Jones and Sam Levis for their critical comments and
suggestions which helped us to improve the original manuscript
substantially. Financial support from Department of Science and
Technology under the grant DST 0948 is gratefully acknowledged. Dr.
Devaraju and Mr. Krishna are supported by the Divecha Center for Climate
Change.
NR 57
TC 6
Z9 6
U1 1
U2 29
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
J9 CLIM DYNAM
JI Clim. Dyn.
PD APR
PY 2013
VL 40
IS 7-8
BP 1671
EP 1686
DI 10.1007/s00382-012-1495-9
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 119CV
UT WOS:000317075700007
ER
PT J
AU Redfern, JV
Mckenna, MF
Moore, TJ
Calambokidis, J
Deangelis, ML
Becker, EA
Barlow, J
Forney, KA
Fiedler, PC
Chivers, SJ
AF Redfern, J. V.
Mckenna, M. F.
Moore, T. J.
Calambokidis, J.
Deangelis, M. L.
Becker, E. A.
Barlow, J.
Forney, K. A.
Fiedler, P. C.
Chivers, S. J.
TI Assessing the Risk of Ships Striking Large Whales in Marine Spatial
Planning
SO CONSERVATION BIOLOGY
LA English
DT Article
DE commercial shipping; generalized additive models; habitat modeling; risk
analysis
ID EASTERN NORTH PACIFIC; ATLANTIC RIGHT WHALES; CALIFORNIA CURRENT; BLUE;
ABUNDANCE; AUTOCORRELATION; HUMPBACK; ECOLOGY; HABITAT; MODEL
AB Marine spatial planning provides a comprehensive framework for managing multiple uses of the marine environment and has the potential to minimize environmental impacts and reduce conflicts among users. Spatially explicit assessments of the risks to key marine species from human activities are a requirement of marine spatial planning. We assessed the risk of ships striking humpback (Megaptera novaeangliae), blue (Balaenoptera musculus), and fin (Balaenoptera physalus) whales in alternative shipping routes derived from patterns of shipping traffic off Southern California (U.S.A.). Specifically, we developed whale-habitat models and assumed ship-strike risk for the alternative shipping routes was proportional to the number of whales predicted by the models to occur within each route. This definition of risk assumes all ships travel within a single route. We also calculated risk assuming ships travel via multiple routes. We estimated the potential for conflict between shipping and other uses (military training and fishing) due to overlap with the routes. We also estimated the overlap between shipping routes and protected areas. The route with the lowest risk for humpback whales had the highest risk for fin whales and vice versa. Risk to both species may be ameliorated by creating a new route south of the northern Channel Islands and spreading traffic between this new route and the existing route in the Santa Barbara Channel. Creating a longer route may reduce the overlap between shipping and other uses by concentrating shipping traffic. Blue whales are distributed more evenly across our study area than humpback and fin whales; thus, risk could not be ameliorated by concentrating shipping traffic in any of the routes we considered. Reducing ship-strike risk for blue whales may be necessary because our estimate of the potential number of strikes suggests that they are likely to exceed allowable levels of anthropogenic impacts established under U.S. laws.
C1 [Redfern, J. V.; Moore, T. J.; Barlow, J.; Fiedler, P. C.; Chivers, S. J.] Natl Ocean & Atmospher Adm, Protected Resources Div, SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, La Jolla, CA 92037 USA.
[Mckenna, M. F.] Marine Mammal Commiss, Bethesda, MD 20814 USA.
[Calambokidis, J.] Cascadia Res, Olympia, WA 98501 USA.
[Deangelis, M. L.] Natl Ocean & Atmospher Adm, Protected Resources Div, Southwest Reg Off, Natl Marine Fisheries Serv, Long Beach, CA 90802 USA.
[Becker, E. A.; Forney, K. A.] Natl Ocean & Atmospher Adm, Protected Resources Div, SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Santa Cruz, CA 95060 USA.
RP Redfern, JV (reprint author), Natl Ocean & Atmospher Adm, Protected Resources Div, SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, 8901 La Jolla Shores Dr, La Jolla, CA 92037 USA.
EM jessica.redfern@noaa.gov
OI Moore, Thomas/0000-0002-0243-6049
NR 33
TC 32
Z9 34
U1 2
U2 123
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0888-8892
EI 1523-1739
J9 CONSERV BIOL
JI Conserv. Biol.
PD APR
PY 2013
VL 27
IS 2
BP 292
EP 302
DI 10.1111/cobi.12029
PG 11
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 113UN
UT WOS:000316694600008
PM 23521668
ER
PT J
AU Schimel, DS
Asner, GP
Moorcroft, P
AF Schimel, David S.
Asner, Gregory P.
Moorcroft, Paul
TI Observing changing ecological diversity in the Anthropocene
SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT
LA English
DT Review
ID REMOTE-SENSING DATA; CLIMATE-CHANGE; EVOLUTIONARY RESPONSES; NICHE;
FOREST; ECOSYSTEMS; BIOGEOCHEMISTRY; TEMPERATURE; SENSITIVITY;
TRANSITIONS
AB As the world enters the Anthropocene - a new geologic period, defined by humanity's massive impact on the planet - the Earth's rapidly changing environment is putting critical ecosystem services at risk. To understand and forecast how ecosystems will change over the coming decades, scientists will require an understanding of the sensitivity of species to environmental change. The current distribution of species and functional groups provides valuable information about the performance of various species in different environments. However, when the rate of environmental change is high, information inherent in the ranges of many species will disappear, since that information exists only under more or less steady-state conditions. The amount of information about species' relationships to climate declines as their distributions move farther from steady state. New remote-sensing technologies can map the chemical and structural traits of plant canopies and will allow for the inference of traits and, in many cases, species' ranges. Current satellite remote-sensing data can only produce relatively simple classifications, but new techniques will produce data with dramatically higher biological information content. Front Ecol Environ 2013;11(3):129-137, doi: 10.1890/120111 (published online 18 Jan 2013)
C1 [Schimel, David S.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Asner, Gregory P.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA USA.
[Moorcroft, Paul] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA.
RP Schimel, DS (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM david.schimel@jpl.nasa.gov
RI Asner, Gregory/G-9268-2013
OI Asner, Gregory/0000-0001-7893-6421
FU NASA; Gordon and Betty Moore Foundation; John D and Catherine T
MacArthur Foundation; WM Keck Foundation; Margaret A Cargill Foundation;
Grantham Foundation for the Protection of the Environment; Mary Anne
Nyburg Baker and G Leonard Baker Jr; William R Hearst III; NEON; NEON
airborne science team; NSF
FX This paper emerged from a workshop convened at the Carnegie Institution
for Science (Stanford, California) in 2010, and was supported by NASA.
The Carnegie Airborne Observatory is supported by the Gordon and Betty
Moore Foundation, the John D and Catherine T MacArthur Foundation, the
WM Keck Foundation, the Margaret A Cargill Foundation, the Grantham
Foundation for the Protection of the Environment, Mary Anne Nyburg Baker
and G Leonard Baker Jr, and William R Hearst III. DSS acknowledges
financial support from NEON and contributions from the NEON airborne
science team. NEON is sponsored by the NSF. Part of this work was
performed at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA.
NR 54
TC 39
Z9 39
U1 6
U2 134
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1540-9295
EI 1540-9309
J9 FRONT ECOL ENVIRON
JI Front. Ecol. Environ.
PD APR
PY 2013
VL 11
IS 3
BP 129
EP 137
DI 10.1890/120111
PG 9
WC Ecology; Environmental Sciences
SC Environmental Sciences & Ecology
GA 117DL
UT WOS:000316932200015
ER
PT J
AU Holt, AL
Gagnon, Y
Vahidinia, S
Morse, DE
Sweeney, AM
AF Holt, A. L.
Gagnon, Y.
Vahidinia, S.
Morse, D. E.
Sweeney, A. M.
TI Photonic enhancement of symbiotic photosynthesis in giant clams
SO INTEGRATIVE AND COMPARATIVE BIOLOGY
LA English
DT Meeting Abstract
CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology
(SICB)
CY JAN 03-07, 2013
CL San Francisco, CA
SP Soc Integrat & Comparat Biol (SICB)
C1 Duke Univ, Durham, NC 27706 USA.
NASA Ames, Ames, IA USA.
Univ Penn, Philadelphia, PA 19104 USA.
EM holt@lifesci.ucsb.edu
RI Gagnon, Yakir/C-2665-2008
OI Gagnon, Yakir/0000-0003-2512-4520
NR 0
TC 0
Z9 0
U1 0
U2 7
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 1540-7063
J9 INTEGR COMP BIOL
JI Integr. Comp. Biol.
PD APR
PY 2013
VL 53
SU 1
BP E95
EP E95
PG 1
WC Zoology
SC Zoology
GA 117ZG
UT WOS:000316991400381
ER
PT J
AU Burow, LC
Woebken, D
Marshall, IPG
Lindquist, EA
Bebout, BM
Prufert-Bebout, L
Hoehler, TM
Tringe, SG
Pett-Ridge, J
Weber, PK
Spormann, AM
Singer, SW
AF Burow, Luke C.
Woebken, Dagmar
Marshall, Ian P. G.
Lindquist, Erika A.
Bebout, Brad M.
Prufert-Bebout, Leslie
Hoehler, Tori M.
Tringe, Susannah G.
Pett-Ridge, Jennifer
Weber, Peter K.
Spormann, Alfred M.
Singer, Steven W.
TI Anoxic carbon flux in photosynthetic microbial mats as revealed by
metatranscriptomics
SO ISME JOURNAL
LA English
DT Article
DE metatranscriptomics; NanoSIMS; anoxic carbon flux; fermentation;
glycogen
ID YELLOWSTONE-NATIONAL-PARK; COMMUNITY STRUCTURE; COASTAL
BACTERIOPLANKTON; CYANOBACTERIAL MATS; HYDROGEN-PRODUCTION;
BAJA-CALIFORNIA; GUERRERO NEGRO; BACTERIA; SEQUENCES; REMOVAL
AB Photosynthetic microbial mats possess extraordinary phylogenetic and functional diversity that makes linking specific pathways with individual microbial populations a daunting task. Close metabolic and spatial relationships between Cyanobacteria and Chloroflexi have previously been observed in diverse microbial mats. Here, we report that an expressed metabolic pathway for the anoxic catabolism of photosynthate involving Cyanobacteria and Chloroflexi in microbial mats can be reconstructed through metatranscriptomic sequencing of mats collected at Elkhorn Slough, Monterey Bay, CA, USA. In this reconstruction, Microcoleus spp., the most abundant cyanobacterial group in the mats, ferment photosynthate to organic acids, CO2 and H-2 through multiple pathways, and an uncultivated lineage of the Chloroflexi take up these organic acids to store carbon as polyhydroxyalkanoates. The metabolic reconstruction is consistent with metabolite measurements and single cell microbial imaging with fluorescence in situ hybridization and NanoSIMS. The ISME Journal (2013) 7, 817-829; doi:10.1038/ismej.2012.150; published online 29 November 2012
C1 [Burow, Luke C.; Woebken, Dagmar; Marshall, Ian P. G.; Spormann, Alfred M.] Stanford Univ, Dept Chem Engn, Stanford, CA 94305 USA.
[Burow, Luke C.; Woebken, Dagmar; Marshall, Ian P. G.; Spormann, Alfred M.] Stanford Univ, Dept Civil & Environm Engn, Stanford, CA 94305 USA.
[Burow, Luke C.; Woebken, Dagmar; Bebout, Brad M.; Prufert-Bebout, Leslie; Hoehler, Tori M.] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA.
[Lindquist, Erika A.; Tringe, Susannah G.] Joint Genome Inst, Walnut Creek, CA USA.
[Pett-Ridge, Jennifer; Weber, Peter K.] Lawrence Livermore Natl Lab, Phys & Life Sci Directorate, Livermore, CA USA.
[Singer, Steven W.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Earth Sci, Berkeley, CA 94720 USA.
RP Singer, SW (reprint author), Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Earth Sci, 1 Cyclotron Rd,Mail Stop 74-316C, Berkeley, CA 94720 USA.
EM SWSinger@lbl.gov
RI Woebken, Dagmar/A-4447-2013;
OI Tringe, Susannah/0000-0001-6479-8427; Woebken,
Dagmar/0000-0002-1314-9926
FU US Department of Energy (DOE) Genomic Science Program [SCW1039]; US
Department of Energy at Lawrence Livermore National Laboratory
[DE-AC52-07NA27344]; US Department of Energy at Lawrence Berkeley
National Laboratory [DE-AC02-05CH11231]; Office of Science of the US
Department of Energy [DE-AC02-05CH11231]; German Research Foundation
(Deutsche Forschungsgemeinschaft)
FX Funding was provided by the US Department of Energy (DOE) Genomic
Science Program under contract SCW1039. Work at LLNL was performed under
the auspices of the US Department of Energy at Lawrence Livermore
National Laboratory under Contract DE-AC52-07NA27344. Work at LBNL was
performed under the auspices of the US Department of Energy at Lawrence
Berkeley National Laboratory under Contract DE-AC02-05CH11231. Pyrotag
and metatranscriptomic sequencing were conducted by the Joint Genome
Institute, which is supported by the Office of Science of the US
Department of Energy under Contract No. DE-AC02-05CH11231. DW was funded
by the German Research Foundation (Deutsche Forschungsgemeinschaft). We
thank Jeff Cann, Associate Wildlife Biologist, Central Region,
California Department of Fish and Game for coordinating our access to
the Moss Landing Wildlife Area.
NR 57
TC 17
Z9 17
U1 6
U2 57
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1751-7362
J9 ISME J
JI ISME J.
PD APR
PY 2013
VL 7
IS 4
BP 817
EP 829
DI 10.1038/ismej.2012.150
PG 13
WC Ecology; Microbiology
SC Environmental Sciences & Ecology; Microbiology
GA 114FZ
UT WOS:000316727800012
PM 23190731
ER
PT J
AU Taylor, PC
Loeb, NG
AF Taylor, Patrick C.
Loeb, Norman G.
TI Impact of Sun-Synchronous Diurnal Sampling on Tropical TOA Flux
Interannual Variability and Trends
SO JOURNAL OF CLIMATE
LA English
DT Article
ID OUTGOING LONGWAVE RADIATION; HYDROLOGIC-CYCLE; CLOUD; BUDGET
AB Satellite observations of the earth's radiation budget (ERB) are a critical component of the climate observing system. Recent observations have been made from sun-synchronous orbits, which provide excellent spatial coverage with global measurements twice daily but do not resolve the full diurnal cycle. Previous investigations show that significant errors can occur in time-averaged energy budgets from sun-synchronous orbits if diurnal variations are ignored. However, the impact of incomplete diurnal sampling on top-of-atmosphere (TOA) flux variability and trends has received less attention. A total of 68 months of 3-hourly tropical outgoing longwave radiation (OLR) and reflected shortwave radiation (RSW) fluxes from the Clouds and the Earth's Radiant Energy System (CERES) synoptic (SYN) data product is used to examine the impact of incomplete diurnal sampling on TOA flux variability. Tropical OLR and RSW interannual variability and trends derived from sun-synchronous time sampling consistent with the Terra satellite from 2000 to 2005 show no statistically significant differences at the 95% confidence level with those obtained at 3-hourly time sampling at both 1 degrees x 1 degrees and 10 degrees x 10 degrees regional scales, as well as for tropical means. Monthly, 3-hourly OLR composite anomalies are decomposed into diurnally uniform and diurnal cycle shape change contributions to explain the impact of sampling on observed TOA flux variability. Diurnally uniform contributions to OLR variability account for more than 80% of interannual OLR variability at 1 degrees x 1 degrees spatial scales. Diurnal cycle shape variations are most important in equatorial land regions, contributing up to 50% to OLR variability over Africa. At spatial scales of 10 degrees x 10 degrees or larger, OLR variance contributions from diurnal cycle shape changes remain smaller than 20%.
C1 [Taylor, Patrick C.; Loeb, Norman G.] NASA, Climate Sci Branch, Langley Res Ctr, Hampton, VA 23681 USA.
RP Taylor, PC (reprint author), NASA, Langley Res Ctr, 21 Langley Blvd,Mail Stop 420, Hampton, VA 23681 USA.
EM patrick.c.taylor@nasa.gov
RI Taylor, Patrick/D-8696-2015
OI Taylor, Patrick/0000-0002-8098-8447
NR 27
TC 8
Z9 8
U1 0
U2 12
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
J9 J CLIMATE
JI J. Clim.
PD APR
PY 2013
VL 26
IS 7
BP 2184
EP 2191
DI 10.1175/JCLI-D-12-00416.1
PG 8
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 117GL
UT WOS:000316941400003
ER
PT J
AU Van Weverberg, K
Vogelmann, AM
Lin, W
Luke, EP
Cialella, A
Minnis, P
Khaiyer, M
Boer, ER
Jensen, MP
AF Van Weverberg, K.
Vogelmann, A. M.
Lin, W.
Luke, E. P.
Cialella, A.
Minnis, P.
Khaiyer, M.
Boer, E. R.
Jensen, M. P.
TI The Role of Cloud Microphysics Parameterization in the Simulation of
Mesoscale Convective System Clouds and Precipitation in the Tropical
Western Pacific
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID RESOLVING MODEL SIMULATIONS; CLIMATOLOGY PROJECT GPCP; MEASURING MISSION
TRMM; BULK ICE SCHEME; SATELLITE-OBSERVATIONS; OCEANIC CONVECTION; SIZE
DISTRIBUTIONS; PART II; EXPLICIT FORECASTS; RADIATIVE-TRANSFER
AB This paper presents a detailed analysis of convection-permitting cloud simulations, aimed at increasing the understanding of the role of parameterized cloud microphysics in the simulation of mesoscale convective systems (MCSs) in the tropical western Pacific (TWP). Simulations with three commonly used bulk microphysics parameterizations with varying complexity have been compared against satellite-retrieved cloud properties. An MCS identification and tracking algorithm was applied to the observations and the simulations to evaluate the number, spatial extent, and microphysical properties of individual cloud systems. Different from many previous studies, these individual cloud systems could be tracked over larger distances because of the large TWP domain studied.
The analysis demonstrates that the simulation of MCSs is very sensitive to the parameterization of microphysical processes. The most crucial element was found to be the fall velocity of frozen condensate. Differences in this fall velocity between the experiments were more related to differences in particle number concentrations than to fall speed parameterization. Microphysics schemes that exhibit slow sedimentation rates for ice aloft experience a larger buildup of condensate in the upper troposphere. This leads to more numerous and/or larger MCSs with larger anvils. Mean surface precipitation was found to be overestimated and insensitive to the microphysical schemes employed in this study. In terms of the investigated properties, the performances of complex two-moment schemes were not superior to the simpler one-moment schemes, since explicit prediction of number concentration does not necessarily improve processes such as ice nucleation, the aggregation of ice crystals into snowflakes, and their sedimentation characteristics.
C1 [Van Weverberg, K.; Vogelmann, A. M.; Lin, W.; Luke, E. P.; Cialella, A.; Jensen, M. P.] Brookhaven Natl Lab, Upton, NY 11973 USA.
[Van Weverberg, K.] Catholic Univ Louvain, Georges Lemaitre Ctr Earth & Climate Res TECLIM, BE-1348 Louvain, Belgium.
[Minnis, P.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Khaiyer, M.] Sci Syst & Applicat Inc, Hampton, VA USA.
[Boer, E. R.] Entropy Control Inc, La Jolla, CA USA.
RP Van Weverberg, K (reprint author), Catholic Univ Louvain, Georges Lemaitre Ctr Earth & Climate Res, Pl Louis Pasteur 3,SC10-L4-03-08, BE-1348 Louvain, Belgium.
EM kwinten.vanweverberg@uclouvain.be
RI Vogelmann, Andrew/M-8779-2014; Minnis, Patrick/G-1902-2010
OI Vogelmann, Andrew/0000-0003-1918-5423; Minnis,
Patrick/0000-0002-4733-6148
FU Laboratory Directed Research and Development Program at Brookhaven
National Laboratory; U.S. Department of Energy's Atmospheric Science
Program Atmospheric System Research (ASR); Office of Science Office of
Biological and Environmental Research program [DE-AC02-98CH10886]; Earth
System Modeling Program via the FASTER project; ASR [DE-SC0000991/003]
FX Research by Van Weverberg, Vogelmann, Lin, Luke, Cialella, and Jensen
was supported by the Laboratory Directed Research and Development
Program at Brookhaven National Laboratory, the U.S. Department of
Energy's Atmospheric Science Program Atmospheric System Research (ASR),
an Office of Science Office of Biological and Environmental Research
program, under Contract DE-AC02-98CH10886, and by the Earth System
Modeling Program via the FASTER project (www.bnl.gov/esm). M. Khaiyer
and P. Minnis were also supported by the ASR under Interagency Agreement
DE-SC0000991/003. We kindly acknowledge the use of the NY Blue: a Blue
Gene/L supercomputer that was used for the WRF simulations. We thank
three anonymous reviewers for their suggestions that led to major
improvements to the paper.
NR 82
TC 23
Z9 23
U1 2
U2 37
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 APR
PY 2013
VL 70
IS 4
BP 1104
EP 1128
DI 10.1175/JAS-D-12-0104.1
PG 25
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 118AC
UT WOS:000316993700008
ER
PT J
AU Odom, B
AF Odom, Brian
TI Great Lives from History: Scientists and Science
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 [Odom, Brian] NASA, Marshall Space & Flight Ctr, Huntsville, AL 35811 USA.
RP Odom, B (reprint author), NASA, Marshall Space & Flight Ctr, Huntsville, AL 35811 USA.
NR 1
TC 0
Z9 0
U1 1
U2 1
PU REED BUSINESS INFORMATION
PI NEW YORK
PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD APR 1
PY 2013
VL 138
IS 6
BP 102
EP 103
PG 2
WC Information Science & Library Science
SC Information Science & Library Science
GA 115XY
UT WOS:000316846400113
ER
PT J
AU Dobrokhodov, V
Xargay, E
Hovakimyan, N
Kaminer, I
Cao, CY
Gregory, IM
AF Dobrokhodov, Vladimir
Xargay, Enric
Hovakimyan, Naira
Kaminer, Isaac
Cao, Chengyu
Gregory, Irene M.
TI Multicriteria analysis of an L-1 adaptive flight control system
SO PROCEEDINGS OF THE INSTITUTION OF MECHANICAL ENGINEERS PART I-JOURNAL OF
SYSTEMS AND CONTROL ENGINEERING
LA English
DT Article
DE L-1 adaptive control; flying qualities; multicriteria optimization;
Pareto optimality; quasi-random sequences
AB This article presents an overview of the application of the Parameter Space Investigation method for the multicriteria design optimization of the L-1 adaptive flight control system implemented on the two turbine-powered dynamically-scaled generic transport model Airborne Subscale Transport Aircraft Research aircraft. In particular, this study addresses the improvement of a nominal prototype solution, obtained using basic design guidelines of L-1 adaptive control theory. The results validate the theoretical claims of L-1 adaptive control in terms of closed-loop performance and robustness and illustrate the systematic character of its design procedure. Furthermore, this article shows the suitability of the Parameter Space Investigation method for the multicriteria design optimization over a multidimensional design variable space of a flight control system subject to desired control specifications. The use of this particular method is of special interest, as it provides invaluable information about the behavior of the closed-loop system in an extended space of design parameters and performance criteria. The results and conclusions of this article have led to a deeper understanding of the characteristics of the closed-loop adaptive system and have contributed to the improvement of the flying qualities and the robustness margins of the adaptive L-1-augmented aircraft, which has been recently flight tested by National Aeronautics and Space Administration.
C1 [Dobrokhodov, Vladimir; Kaminer, Isaac] USN, Postgrad Sch, Dept Mech & Aerosp Engn, Monterey, CA 93943 USA.
[Xargay, Enric; Hovakimyan, Naira] Univ Illinois, Coordinated Sci Lab, Urbana, IL USA.
[Cao, Chengyu] Univ Connecticut, Dept Mech Engn, Storrs, CT USA.
[Gregory, Irene M.] NASA, Langley Res Ctr, Dynam Syst & Control Branch, Hampton, VA 23665 USA.
RP Dobrokhodov, V (reprint author), USN, Postgrad Sch, Dept Mech & Aerosp Engn, Monterey, CA 93943 USA.
EM vldobr@nps.edu
FU Air Force Office of Scientific Research; NASA
FX This study was supported by Air Force Office of Scientific Research and
NASA.
NR 22
TC 2
Z9 2
U1 0
U2 15
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0959-6518
J9 P I MECH ENG I-J SYS
JI Proc. Inst. Mech. Eng. Part I-J Syst Control Eng.
PD APR
PY 2013
VL 227
IS I4
BP 413
EP 427
DI 10.1177/0959651812468545
PG 15
WC Automation & Control Systems
SC Automation & Control Systems
GA 121IC
UT WOS:000317235500004
ER
PT J
AU Liu, Y
Schuck, PW
AF Liu, Yang
Schuck, P. W.
TI A Note on Computation of Relative Magnetic-Helicity Flux Across the
Photosphere
SO SOLAR PHYSICS
LA English
DT Article
DE Solar magnetic field; Magnetic helicity; Helicity flux density
ID DYNAMICS-OBSERVATORY SDO; ACTIVE REGIONS; SOLAR CORONA; EVOLUTION;
ENERGY; INJECTION; IMAGER; TUBES; FIELD
AB A number of investigations of the rate of relative magnetic-helicity transport across the photosphere [] have reported differences in the estimates computed from two different formulations of the relative-helicity flux-density proxy G (A) and G (theta) . There have been suggestions that G (theta) is a more robust helicity-flux density proxy and that the differences in the estimates of are caused by biases in G (A), noise, and/or the boundary conditions. In this note, we prove that the differences are caused by the inconsistent choice of boundary conditions in the explicit or implicit Green's function [] used for computing G (A) and G (theta) when comparing the helicity-flux estimates based on G (A) and G (theta) . When the boundary conditions in are chosen consistently, the two helicity-flux density proxies, [G (A) and G (theta) ] produce essentially identical results for the rate of helicity transport across the photosphere. They also yield essentially identical results for the rate of helicity transport of the shearing and advection terms separately. Using MHD simulation, HMI observational data, and Monte Carlo simulations of noise we show that this result is robust. Neither the shape of the active region, nor the shape of the boundary, nor data noise causes any difference in the rate of helicity transport computed via G (A) and G (theta) .
C1 [Liu, Yang] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Schuck, P. W.] NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Liu, Y (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
EM yliu@sun.stanford.edu; peter.schuck@nasa.gov
FU NASA [NAS5-02139 (HMI)]; NASA LWS grant; NASA HGI grant
FX We wish to thank P. Demoulin, E. Pariat, and K. Dalmasse for valuable
comments and suggestions. P. Demoulin suggested examining the size of
the padding area and the helicity density computed from the FFT. YL was
supported by NASA Contract NAS5-02139 (HMI) to Stanford University, and
PWS was supported by NASA LWS and HGI grants. The data have been used by
courtesy of NASA/SDO and the HMI science team.
NR 27
TC 4
Z9 4
U1 0
U2 5
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
J9 SOL PHYS
JI Sol. Phys.
PD APR
PY 2013
VL 283
IS 2
BP 283
EP 294
DI 10.1007/s11207-012-0219-y
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 108BF
UT WOS:000316265100004
ER
PT J
AU Brown, ME
Hand, KP
AF Brown, M. E.
Hand, K. P.
TI SALTS AND RADIATION PRODUCTS ON THE SURFACE OF EUROPA
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE planets and satellites: composition; planets and satellites: individual
(Europa); planets and satellites: surfaces
ID INFRARED MAPPING SPECTROMETER; SULFURIC-ACID; WATER ICE; SUBSURFACE
OCEAN; GALILEO; SATELLITES; ATMOSPHERE; MINERALS; CHLORINE; IMPLANTATION
AB The surface of Europa could contain the compositional imprint of an underlying interior ocean, but competing hypotheses differ over whether spectral observations from the Galileo spacecraft show the signature of ocean evaporates or simply surface radiation products unrelated to the interior. Using adaptive optics at the W. M. Keck Observatory, we have obtained spatially resolved spectra of most of the disk of Europa at a spectral resolution similar to 40 times higher than seen by the Galileo spacecraft. These spectra show a previously undetected distinct signature of magnesium sulfate salts on Europa, but the magnesium sulfate is confined to the trailing hemisphere and spatially correlated with the presence of radiation products like sulfuric acid and SO2. On the leading, less irradiated, hemisphere, our observations rule out the presence of many of the proposed sulfate salts, but do show the presence of distorted water ice bands. Based on the association of the potential MgSO4 detection on the trailing side with other radiation products, we conclude that MgSO4 is also a radiation product, rather than a constituent of a Europa ocean brine. Based on ocean chemistry models, we hypothesize that, prior to irradiation, magnesium is primarily in the form of MgCl2, and we predict that NaCl and KCl are even more abundant, and, in fact, dominate the non-ice component of the leading hemisphere. We propose observational tests of this new hypothesis.
C1 [Brown, M. E.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Hand, K. P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Brown, ME (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
EM mbrown@caltech.edu
FU Jet Propulsion Laboratory, California Institute of Technology under
National Aeronautics and Space Administration; internal Research and
Technology Development program; NASA Astrobiology Institute; Richard and
Barbara Rosenberg Professorship at the California Institute of
Technology
FX K.P.H. acknowledges support from the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration and funded in part through the
internal Research and Technology Development program. and from the NASA
Astrobiology Institute, through the "Astrobiology of Icy Worlds" node at
JPL. M. E. B. is supported by the Richard and Barbara Rosenberg
Professorship at the California Institute of Technology.
NR 47
TC 29
Z9 31
U1 5
U2 65
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD APR
PY 2013
VL 145
IS 4
AR 110
DI 10.1088/0004-6256/145/4/110
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 107UW
UT WOS:000316247300024
ER
PT J
AU Grazier, KR
Newman, WI
Sharp, PW
AF Grazier, K. R.
Newman, W. I.
Sharp, P. W.
TI A MULTIRATE STORMER ALGORITHM FOR CLOSE ENCOUNTERS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE celestial mechanics; methods: numerical; minor planets, asteroids:
general
ID N-BODY PROBLEM; SOLAR-SYSTEM; TIME-STEPS; INTEGRATIONS; EVOLUTION;
ORBITS
AB We present, analyze, and test a multirate Stormer-based algorithm for integrating close encounters when performing N-body simulations of the Sun, planets, and a large number of test particles. The algorithm is intended primarily for accurate simulations of the outer solar system. The algorithm uses stepsizes H and h(i), i = 1, ..., N-p, where h(i) << H and N-p is the number of planets. The stepsize H is used for the integration of the orbital motion of the Sun and planets at all times. H is also used as the stepsize for the integration of the orbital motion of test particles when they are not undergoing a close encounter. The stepsize h(i) is used to integrate the orbital motion of test particles during a close encounter with the ith planet. The position of the Sun and planets during a close encounter is calculated using Hermite interpolation. We tested the algorithm on two contrasting problems, and compared its performance with the existing method which uses the same stepsize for all bodies (this stepsize must be significantly smaller than H to ensure the close encounters are integrated accurately). Our tests show that the integration error for the new and existing methods are comparable when the stepsizes are chosen to minimize the error, and that for this choice of stepsizes the new method requires considerably less CPU time than the existing method.
C1 [Grazier, K. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Newman, W. I.] Univ Calif Los Angeles, Los Angeles, CA USA.
[Sharp, P. W.] Univ Auckland, Dept Math, Auckland, New Zealand.
RP Sharp, PW (reprint author), Univ Auckland, Dept Math, Private Bag 92019, Auckland, New Zealand.
EM kevin_grazier@yahoo.com; win@ucla.edu; sharp@math.auckland.ac.nz
OI Sharp, Philip/0000-0001-9550-0910
FU National Aeronautics and Space Administration; NeSI; Ministry of
Business, Innovation and Employment's Infrastructure programme
FX This work has been conducted in part at the Jet Propulsion Laboratory,
California Institute of Technology under a contract with the National
Aeronautics and Space Administration. Government sponsorship
acknowledged.; The authors thank the referee for the detailed report.
The referee's comments about the new method relative to the existing
method were especially invaluable. The authors wish to acknowledge the
contribution of the NeSI high-performance computing facilities and the
staff at the Centre for eResearch at the University of Auckland. New
Zealand's national facilities are provided by the New Zealand eScience
Infrastructure (NeSI) and funded jointly by NeSI's collaborator
institutions and through the Ministry of Business, Innovation and
Employment's Infrastructure programme (http://www.nesi.org.nz).
NR 18
TC 2
Z9 2
U1 1
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD APR
PY 2013
VL 145
IS 4
AR 112
DI 10.1088/0004-6256/145/4/112
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 107UW
UT WOS:000316247300026
ER
PT J
AU Howell, SB
Everett, ME
Seebode, SA
Szkody, P
Still, M
Wood, M
Ramsay, G
Cannizzo, J
Smale, A
AF Howell, Steve B.
Everett, Mark E.
Seebode, Sally A.
Szkody, Paula
Still, Martin
Wood, Matt
Ramsay, Gavin
Cannizzo, John
Smale, Alan
TI SPECTROSCOPY OF NEW AND POORLY KNOWN CATACLYSMIC VARIABLES IN THE KEPLER
FIELD
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE novae, cataclysmic variables
ID SU UMA-TYPE; V344 LYRAE; DWARF NOVAE; CATALOG; SUPERHUMPS; DISCOVERY;
ATLAS
AB The NASA Kepler mission has been in science operation since 2009 May and is providing high precision, high cadence light curves of over 150,000 targets. Prior to launch, nine cataclysmic variables were known to lie within Kepler's field of view. We present spectroscopy for seven systems, four of which were newly discovered since launch. All of the stars presented herein have been observed by, or are currently being observed by, the Kepler space telescope. Three historic systems and one new candidate could not be detected at their sky position and two candidates are called into question as to their true identity.
C1 [Howell, Steve B.; Still, Martin] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Everett, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Seebode, Sally A.] San Mateo High Sch, San Mateo, CA 94401 USA.
[Szkody, Paula] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Still, Martin] Bay Area Environm Res Inst Inc, West Sonoma, CA 95476 USA.
[Wood, Matt] Texas A&M Univ, Dept Phys & Astron, Commerce, TX 75429 USA.
[Ramsay, Gavin] Armagh Observ, Armagh BT61 9DG, North Ireland.
[Cannizzo, John] CRESST, Greenbelt, MD 20771 USA.
[Cannizzo, John] NASA GSFC, Astroparticle Phys Lab, Greenbelt, MD 20771 USA.
[Cannizzo, John] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA.
[Smale, Alan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Howell, SB (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
FU NSF [AST-1008734, AST-1109332]
FX We wish to thank the observatory staffs of Kitt Peak and Mount Palomar
for their help in carrying out the observations presented here. P. S.
acknowledges support from NSF grant AST-1008734. M. W. acknowledges
support from NSF grant AST-1109332. Kepler was competitively selected as
the 10th NASA Discovery mission.
NR 22
TC 12
Z9 12
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD APR
PY 2013
VL 145
IS 4
AR 109
DI 10.1088/0004-6256/145/4/109
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 107UW
UT WOS:000316247300023
ER
PT J
AU Hand, KP
Brown, ME
AF Hand, K. P.
Brown, M. E.
TI KECK II OBSERVATIONS OF HEMISPHERICAL DIFFERENCES IN H2O2 ON EUROPA
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE astrochemistry; infrared: planetary systems; planets and satellites:
composition; planets and satellites: surfaces
ID ICY GALILEAN SATELLITES; HYDROGEN-PEROXIDE; WATER ICE; O-2; SURFACE;
ENERGY; LIFE; ION; TEMPERATURE; IRRADIATION
AB We present results from Keck II observations of Europa over four consecutive nights using the near-infrared spectrograph. Spectra were collected in the 3.14-4.0 mu m range, enabling detection and monitoring of the 3.5 mu m feature due to hydrogen peroxide. Galileo Near-Infrared Mapping Spectrometer results first revealed hydrogen peroxide on Europa in the anti-Jovian region of the leading hemisphere at a percent by number abundance of 0.13% +/- 0.07% relative to water. We find comparable results for the two nights over which we observed the leading hemisphere. Significantly, we observed a small amount of hydrogen peroxide (similar to 0.04%) during observations of Europa's anti-Jovian and sub-Jovian hemispheres. Almost no hydrogen peroxide was detected during observations of just the trailing hemisphere. We conclude that the Galileo observations likely represent the maximum hydrogen peroxide concentration, the exception potentially being the cold water ice regions of the poles, which are not readily observable from the ground. Our mapping of the peroxide abundance across Europa requires revisions to previous estimates for Europa's global surface abundance of oxidants and leads to a reduction in the total oxidant delivery expected for the subsurface ocean if an exchange of surface material with the ocean occurs.
C1 [Hand, K. P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Brown, M. E.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91109 USA.
RP Hand, KP (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM khand@jpl.nasa.gov
FU NASA Planetary Astronomy program [NNX09AB49G]; NASA Astrobiology
Institute "Icy Worlds" node at JPL/Caltech
FX This research has been supported by grant NNX09AB49G from the NASA
Planetary Astronomy program and by the NASA Astrobiology Institute "Icy
Worlds" node at JPL/Caltech. The authors thank Robert W. Carlson for
helpful discussions.
NR 30
TC 9
Z9 9
U1 2
U2 30
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD APR 1
PY 2013
VL 766
IS 2
AR L21
DI 10.1088/2041-8205/766/2/L21
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 108UR
UT WOS:000316322200007
ER
PT J
AU Ryder, JW
Buxton, RE
Goetchius, E
Scott-Pandorf, M
Hackney, KJ
Fiedler, J
Ploutz-Snyder, RJ
Bloomberg, JJ
Ploutz-Snyder, LL
AF Ryder, Jeffrey W.
Buxton, Roxanne E.
Goetchius, Elizabeth
Scott-Pandorf, Melissa
Hackney, Kyle J.
Fiedler, James
Ploutz-Snyder, Robert J.
Bloomberg, Jacob J.
Ploutz-Snyder, Lori L.
TI Influence of muscle strength to weight ratio on functional task
performance
SO EUROPEAN JOURNAL OF APPLIED PHYSIOLOGY
LA English
DT Article
DE Muscle; Strength; Power; Work; Task performance
ID HUMAN SKELETAL-MUSCLE; PHYSICAL PERFORMANCE; SPACE; SPACEFLIGHT;
EXERCISE; MOBILITY; ADULTS; VOLUME; WOMEN; CHAIR
AB Existing models of muscle deconditioning such as bed rest are expensive and time-consuming. We propose a new model utilizing a weighted suit to manipulate muscle strength, power, or endurance relative to body weight. The aims of the study were to determine as to which muscle measures best predict functional task performance and to determine muscle performance thresholds below which task performance is impaired. Twenty subjects performed seven occupational astronaut tasks (supine and upright seat egress and walk, rise from fall, hatch opening, ladder climb, object carry, and construction board activity), while wearing a suit weighted with 0-120 % of body weight. Models of the relationship between muscle function/body weight and task completion time were developed using fractional polynomial regression and verified with pre- and post-flight astronaut performance data. Spline regression was used to identify muscle function thresholds for each task. Upright seat egress and walk was the most difficult task according to the spline regression analysis thresholds. Thresholds normalized to body weight were 17.8 N/kg for leg press isometric force, 17.6 W/kg for leg press power, 78.8 J/kg for leg press work, 5.9 N/kg isometric knee extension and 1.9 Nm/kg isokinetic knee extension torque. Leg press maximal isometric force/body weight was the most reliable measure for modeling performance of ambulatory tasks. Laboratory-based manipulation of relative strength has promise as an analog for spaceflight-induced loss of muscle function. Muscle performance values normalized to body weight can be used to predict occupational task performance and to establish relevant strength thresholds.
C1 [Ryder, Jeffrey W.; Fiedler, James; Ploutz-Snyder, Robert J.; Ploutz-Snyder, Lori L.] Univ Space Res Assoc, Houston, TX 77058 USA.
[Buxton, Roxanne E.; Goetchius, Elizabeth] Univ Houston, Houston, TX 77004 USA.
[Scott-Pandorf, Melissa; Hackney, Kyle J.] Wyle Integrated Sci & Engn, Houston, TX 77058 USA.
[Bloomberg, Jacob J.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Ryder, JW (reprint author), Univ Space Res Assoc, Houston, TX 77058 USA.
EM jeffrey.ryder-1@nasa.gov
FU National Aeronautics and Space Administration Human Research Program
FX This work was supported by funding from the National Aeronautics and
Space Administration Human Research Program.
NR 21
TC 5
Z9 6
U1 2
U2 8
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1439-6319
J9 EUR J APPL PHYSIOL
JI Eur. J. Appl. Physiol.
PD APR
PY 2013
VL 113
IS 4
BP 911
EP 921
DI 10.1007/s00421-012-2500-z
PG 11
WC Physiology; Sport Sciences
SC Physiology; Sport Sciences
GA 106EI
UT WOS:000316124900012
PM 23011123
ER
PT J
AU Morrison, KD
Bristow, TF
Kennedy, MJ
AF Morrison, Keith D.
Bristow, Thomas F.
Kennedy, Martin J.
TI The reduction of structural iron in ferruginous smectite via the amino
acid cysteine: Implications for an electron shuttling compound
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID COASTAL MARINE-SEDIMENTS; DIOCTAHEDRAL SMECTITES; CLAY-MINERALS;
QUANTITATIVE ASSAY; GEOBACTER-SULFURREDUCENS; FE(III) REDUCTION;
CRYSTAL-CHEMISTRY; HUMIC SUBSTANCES; METAL REDUCTION; OXIDATION
AB Microbes can reduce the structural iron (Fe(III)(str)) in clay minerals thus providing a potentially important terminal electron acceptor in the oxidation of organic matter. Many of these microorganisms participate in dissimilatory metal reduction with Fe(III) serving as the terminal electron acceptor either through direct contact with mineral surfaces or by way of electron shuttling compounds. Here we provide evidence for the electron shuttling capability of the amino acid cysteine with a ferruginous dioctahedral smectite (SWa-1) using infrared spectroscopy, X-ray diffraction and quantitative assay of ferric and ferrous iron. Reactions to determine the electron exchange between cysteine and SWa-1 were performed in pH 8 adjusted oxygen free solutions. Fourier transform infrared spectroscopy (FTIR) performed on self-supporting clay films reveals that cysteine has the ability to reduce Fe(III)(str), as shown by the decrease in the intensity of the AlFeOH and FeFeOH deformation and stretching bands resulting from decreased hydroxyl vibrations in the octahedral sheets. X-ray diffraction of the c-oriented SWa-1 reveals that cysteine intercalated into the d00l interlayer spaces. Quantitative iron assay indicates that the SWa-1 retains its structural iron upon reduction by cysteine and reoxidation. The increased interlayer spacing due to the intercalation of cysteine implies that this electron exchange is occurring from the basal surfaces of the smectite, as opposed to edge sites. When the SWa-1 was rinsed in dialysis tubing, the AlFeOH and FeFeOH vibrations reappear in FTIR spectra and the XRD patterns reveal that the cysteine no longer occupies interlayer sites. These results are consistent with partially reversible changes in clay mineral structure resulting from the reduction of Fe(III)(str). They support the hypothesis that cysteine could serve as an electron shuttling compound used by microorganisms to gain access to structural iron in clay minerals and extends the range of microbially mediated Fe redox reactions from iron oxides and oxyhydroxides to the largest pool of Fe in aquatic sediments, Fe-bearing clay minerals. (C) 2013 Published by Elsevier Ltd.
C1 [Morrison, Keith D.] Univ Calif Riverside, Dept Earth Sci, Riverside, CA 92521 USA.
[Bristow, Thomas F.] NASA, Exobiol Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kennedy, Martin J.] Univ Adelaide, Sch Earth & Environm Sci, Sprigg Geobiol Ctr, Adelaide, SA 5005, Australia.
RP Morrison, KD (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
EM keith.morrison@asu.edu
FU NSF Marine Sciences; ARC [DP110104367]
FX We would like to thank Eric Chronister and the University of California
Riverside, Department of Chemistry for help with the FTIR analysis and
interpretation. We thank Lynda Williams and Hilairy Hartnett for their
thorough evaluation of the manuscript and helpful discussions. This
research was supported by NSF Marine Sciences and ARC DP110104367.
NR 61
TC 5
Z9 5
U1 2
U2 58
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 APR 1
PY 2013
VL 106
BP 152
EP 163
DI 10.1016/j.gca.2012.12.006
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 100PP
UT WOS:000315713500010
ER
PT J
AU Benafan, O
Noebe, RD
Padula, SA
Gaydosh, DJ
Lerch, BA
Garg, A
Bigelow, GS
An, K
Vaidyanathan, R
AF Benafan, O.
Noebe, R. D.
Padula, S. A., II
Gaydosh, D. J.
Lerch, B. A.
Garg, A.
Bigelow, G. S.
An, K.
Vaidyanathan, R.
TI Temperature-dependent behavior of a polycrystalline NiTi shape memory
alloy around the transformation regime
SO SCRIPTA MATERIALIA
LA English
DT Article
DE Shape memory alloys; NiTi; Martensite reorientation; Dynamic modulus;
Neutron diffraction
ID MODULI
AB The mechanical and microstructural behavior of a polycrystalline Ni49.9Ti50.1 (at.%) shape memory alloy was investigated as a function of temperature around the transformation regime. The bulk macroscopic responses, measured using ex situ tensile deformation and impulse excitation tests, were compared to the microstructural evolution captured using in situ neutron diffraction. The onset stress for inelastic deformation and dynamic Young's modulus were found to decrease with temperature in the martensite regime followed by an increase starting near the austenite start temperature, attributed to the reverse transformation. Published by Elsevier Ltd. on behalf of Acta Materialia Inc.
C1 [Benafan, O.; Noebe, R. D.; Padula, S. A., II; Gaydosh, D. J.; Lerch, B. A.; Garg, A.; Bigelow, G. S.] NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
[Gaydosh, D. J.] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
[Garg, A.] Univ Toledo, Toledo, OH 43606 USA.
[An, K.] Oak Ridge Natl Lab, Spallat Neutron Source, Oak Ridge, TN 37831 USA.
[Vaidyanathan, R.] Univ Cent Florida, Mat Sci & Engn Dept, Adv Mat Proc & Anal Ctr, Orlando, FL 32816 USA.
RP Benafan, O (reprint author), NASA, Glenn Res Ctr, Struct & Mat Div, Cleveland, OH 44135 USA.
EM othmane.benafan@nasa.gov
RI An, Ke/G-5226-2011
OI An, Ke/0000-0002-6093-429X
FU NASA Fundamental Aeronautics Program, Aeronautical Sciences and Fixed
Wing Projects; Division of Scientific User Facilities, Office of Basic
Energy Sciences, US Department of Energy [DE-AC05- 00OR22725]
FX Funding from the NASA Fundamental Aeronautics Program, Aeronautical
Sciences and Fixed Wing Projects is gratefully acknowledged. The authors
thank D.E. Nicholson and H.D. Skorpenske for technical support and
helpful discussions. This work has benefited from the use of the
Spallation Neutron Source at Oak Ridge National Laboratory, which is
funded by the Division of Scientific User Facilities, Office of Basic
Energy Sciences, US Department of Energy under Contract DE-AC05-
00OR22725 with UT-Battelle, LLC.
NR 11
TC 20
Z9 20
U1 2
U2 31
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1359-6462
J9 SCRIPTA MATER
JI Scr. Mater.
PD APR
PY 2013
VL 68
IS 8
BP 571
EP 574
DI 10.1016/j.scriptamat.2012.11.042
PG 4
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Metallurgy & Metallurgical Engineering
SC Science & Technology - Other Topics; Materials Science; Metallurgy &
Metallurgical Engineering
GA 105CB
UT WOS:000316042100007
ER
PT J
AU Salim, WWAW
Zeitchek, MA
Hermann, AC
Ricco, AJ
Tan, M
Selch, F
Fleming, E
Bebout, BM
Bader, MM
ul Haque, A
Porterfield, DM
AF Salim, Wan W. Amani Wan
Zeitchek, Michael A.
Hermann, Andrew C.
Ricco, Antonio J.
Tan, Ming
Selch, Florian
Fleming, Erich
Bebout, Brad M.
Bader, Mamoun M.
ul Haque, Aeraj
Porterfield, D. Marshall
TI Multi-analyte Biochip (MAB) Based on All-solid-state Ion-selective
Electrodes (ASSISE) for Physiological Research
SO JOVE-JOURNAL OF VISUALIZED EXPERIMENTS
LA English
DT Article
DE Bioengineering; Issue 74; Medicine; Biomedical Engineering; Chemical
Engineering; Electrical Engineering; Mechanical Engineering; Chemistry;
Biochemistry; Anatomy; Physiology; Miniaturization; Microtechnology;
Electrochemical Techniques; electrochemical processes; astrobiology;
Analytical; Diagnostic and Therapeutic Techniques and Equipment;
Investigative Techniques; Technology; Industry; Agriculture;
electrochemical sensor; all-solid-state ion-selective electrode
(ASSISE); conductive polymer transducer;
poly(3,4-ethylenedioxythiophene) (PEDOT); lab-on-a-chip; Chlorella
vulgaris; photosynthesis; microfluidics
AB Lab-on-a-chip (LOC) applications in environmental, biomedical, agricultural, biological, and spaceflight research require an ion-selective electrode (ISE) that can withstand prolonged storage in complex biological media (1-4). An all-solid-state ion-selective-electrode (ASSISE) is especially attractive for the aforementioned applications. The electrode should have the following favorable characteristics: easy construction, low maintenance, and (potential for) miniaturization, allowing for batch processing. A microfabricated ASSISE intended for quantifying H+, Ca2+, and CO32- ions was constructed. It consists of a noble-metal electrode layer (i.e. Pt), a transduction layer, and an ion-selective membrane (ISM) layer. The transduction layer functions to transduce the concentration-dependent chemical potential of the ion-selective membrane into a measurable electrical signal.
The lifetime of an ASSISE is found to depend on maintaining the potential at the conductive layer/membrane interface 5-7. To extend the ASSISE working lifetime and thereby maintain stable potentials at the interfacial layers, we utilized the conductive polymer (CP) poly(3,4ethylenedioxythiophene) (PEDOT) 7-9 in place of silver/silver chloride (Ag/AgCl) as the transducer layer. We constructed the ASSISE in a lab-ona- chip format, which we called the multi-analyte biochip (MAB) (Figure 1).
Calibrations in test solutions demonstrated that the MAB can monitor pH (operational range pH 4-9), CO32-(measured range 0.01 mM (-1) mM), and Ca2+ (log-linear range 0.01 mM to 1 mM). The MAB for pH provides a near-Nernstian slope response after almost one month storage in algal medium. The carbonate biochips show a potentiometric profile similar to that of a conventional ion-selective electrode. Physiological measurements were employed to monitor biological activity of the model system, the microalga Chlorella vulgaris.
The MAB conveys an advantage in size, versatility, and multiplexed analyte sensing capability, making it applicable to many confined monitoring situations, on Earth or in space.
Biochip Design and Experimental Methods
The biochip is 10 x 11 mm in dimension and has 9 ASSISEs designated as working electrodes (WEs) and 5 Ag/AgCl reference electrodes (REs). Each working electrode (WE) is 240 mu m in diameter and is equally spaced at 1.4 mm from the REs, which are 480 mu m in diameter. These electrodes are connected to electrical contact pads with a dimension of 0.5 mm x 0.5 mm. The schematic is shown in Figure 2.
Cyclic voltammetry (CV) and galvanostatic deposition methods are used to electropolymerize the PEDOT films using a Bioanalytical Systems Inc. (BASI) C3 cell stand (Figure 3). The counter-ion for the PEDOT film is tailored to suit the analyte ion of interest. A PEDOT with poly(styrenesulfonate) counter ion (PEDOT/PSS) is utilized for H+ and CO32-, while one with sulphate (added to the solution as CaSO4) is utilized for Ca2+. The electrochemical properties of the PEDOT-coated WE is analyzed using CVs in redox-active solution (i.e. 2 mM potassium ferricyanide (K3Fe(CN)6)). Based on the CV profile, Randles-Sevcik analysis was used to determine the effective surface area (10). Spin-coating at 1,500 rpm is used to cast similar to 2 mu m thick ion-selective membranes (ISMs) on the MAB working electrodes (WEs).
The MAB is contained in a microfluidic flow-cell chamber filled with a 150 mu l volume of algal medium; the contact pads are electrically connected to the BASI system (Figure 4). The photosynthetic activity of Chlorella vulgaris is monitored in ambient light and dark conditions.
C1 [Salim, Wan W. Amani Wan; Zeitchek, Michael A.; Hermann, Andrew C.] Purdue Univ, Birck Bindley Physiol Sensing Facil, Dept Agr & Biol Engn, W Lafayette, IN 47907 USA.
[Ricco, Antonio J.; Tan, Ming; Selch, Florian; Fleming, Erich; Bebout, Brad M.] NASA Ames Res Ctr, Mountain View, CA USA.
[Bader, Mamoun M.] Penn State Univ Hazleton, Dept Chem, Hazleton, PA USA.
[ul Haque, Aeraj] Cooley LLP, Palo Alto, CA USA.
[Porterfield, D. Marshall] NASA Headquarters, NASA Life & Phys Sci, Human Explorat & Operat Miss Directorate, Washington, DC USA.
RP Salim, WWAW (reprint author), Purdue Univ, Birck Bindley Physiol Sensing Facil, Dept Agr & Biol Engn, W Lafayette, IN 47907 USA.
EM asalim@purdue.edu
FU NASA Astrobiology Science and Technology Instrument Development (ASTID)
[103498, 103692]; Birck Nantechnology Center at Purdue University for
wirebonding of the MAB devices; oon Hyeong Park for the CAD drawing of
the flow-cell chamber
FX We would like to thank NASA Astrobiology Science and Technology
Instrument Development (ASTID) Program for funding support (grant
numbers 103498 and 103692), Gale Lockwood of the Birck Nantechnology
Center at Purdue University for wirebonding of the MAB devices, and Joon
Hyeong Park for the CAD drawing of the flow-cell chamber.
NR 14
TC 0
Z9 0
U1 7
U2 26
PU JOURNAL OF VISUALIZED EXPERIMENTS
PI CAMBRIDGE
PA 1 ALEWIFE CENTER, STE 200, CAMBRIDGE, MA 02140 USA
SN 1940-087X
J9 JOVE-J VIS EXP
JI J. Vis. Exp.
PD APR
PY 2013
IS 74
AR UNSP e50020
DI 10.3791/50020
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA V36QY
UT WOS:000209227100010
ER
PT J
AU Coggins, SB
Coops, NC
Hilker, T
Wulder, MA
AF Coggins, Sam B.
Coops, Nicholas C.
Hilker, Thomas
Wulder, Michael A.
TI Augmenting forest inventory attributes with geometric optical modelling
in support of regional susceptibility assessments to bark beetle
infestations
SO INTERNATIONAL JOURNAL OF APPLIED EARTH OBSERVATION AND GEOINFORMATION
LA English
DT Article
DE Landsat; Forest inventory; Mountain pine beetle; Susceptibility;
Geometric optical modelling; Western Canada; Lodgepole pine; Forest
health
ID MOUNTAIN PINE-BEETLE; RANGE EXPANSION; BOREAL FOREST; IMAGERY
AB Assessment of the susceptibility of forests to mountain pine beetle (Dendroctonus ponderosae Hopkins) infestation is based upon an understanding of the characteristics that predispose the stands to attack. These assessments are typically derived from conventional forest inventory data; however, this information often represents only managed forest areas. It does not cover areas such as forest parks or conservation regions and is often not regularly updated resulting in an inability to assess forest susceptibility. To address these shortcomings, we demonstrate how a geometric optical model (GOM) can be applied to Landsat-5 Thematic Mapper (TM) imagery (30 m spatial resolution) to estimate stand-level susceptibility to mountain pine beetle attack. Spectral mixture analysis was used to determine the proportion of sunlit canopy and background, and shadow of each Landsat pixel enabling per pixel estimates of attributes required for model inversion. Stand structural attributes were then derived from inversion of the geometric optical model and used as basis for susceptibility mapping. Mean stand density estimated by the geometric optical model was 2753 (standard deviation +/- 308) stems per hectare and mean horizontal crown radius was 2.09 (standard deviation +/- 0.11) metres. When compared to equivalent forest inventory attributes, model predictions of stems per hectare and crown radius were shown to be reasonably estimated using a Kruskal-Wallis ANOVA (p < 0.001). These predictions were then used to create a large area map that provided an assessment of the forest area susceptible to mountain pine beetle damage. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Coggins, Sam B.; Coops, Nicholas C.] Univ British Columbia, Dept Forest Resources Management, Vancouver, BC V6T 1Z4, Canada.
[Hilker, Thomas] NASA, Goddard Space Flight Ctr, Biospher Sci Branch Code 618, Greenbelt, MD 20771 USA.
[Wulder, Michael A.] Nat Resources Canada, Canadian Forest Serv, Pacific Forestry Ctr, Victoria, BC, Canada.
RP Coops, NC (reprint author), Univ British Columbia, Dept Forest Resources Management, 2424 Main Mall, Vancouver, BC V6T 1Z4, Canada.
EM nicholas.coops@ubc.ca
RI Coops, Nicholas/J-1543-2012; Wulder, Michael/J-5597-2016
OI Coops, Nicholas/0000-0002-0151-9037; Wulder, Michael/0000-0002-6942-1896
FU Government of Canada; Pacific Forestry Centre; Natural Sciences and
Engineering Research Council (NSERC)
FX We acknowledge funding for this research from the following funding
agencies: (1) the Government of Canada, through the Mountain Pine Beetle
Program, a 6-year, $40 million program administered by Natural Resources
Canada - Canadian Forest Service; (2) the Pacific Forestry Centre
Graduate Student Award to Sam Coggins, administered by Natural Resources
Canada - Canadian Forest Service; and (3) a Natural Sciences and
Engineering Research Council (NSERC) grant to Nicholas Coops, supported
by the Government of Canada. Finally, we thank Peter Scarth for help at
the initial stages of the study in supplying code for the geometric
optical modelling.
NR 35
TC 3
Z9 3
U1 0
U2 32
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0303-2434
J9 INT J APPL EARTH OBS
JI Int. J. Appl. Earth Obs. Geoinf.
PD APR
PY 2013
VL 21
BP 444
EP 452
DI 10.1016/j.jag.2012.06.007
PG 9
WC Remote Sensing
SC Remote Sensing
GA 065IX
UT WOS:000313143100041
ER
PT J
AU Creamean, JM
Suski, KJ
Rosenfeld, D
Cazorla, A
DeMott, PJ
Sullivan, RC
White, AB
Ralph, FM
Minnis, P
Comstock, JM
Tomlinson, JM
Prather, KA
AF Creamean, Jessie M.
Suski, Kaitlyn J.
Rosenfeld, Daniel
Cazorla, Alberto
DeMott, Paul J.
Sullivan, Ryan C.
White, Allen B.
Ralph, F. Martin
Minnis, Patrick
Comstock, Jennifer M.
Tomlinson, Jason M.
Prather, Kimberly A.
TI Dust and Biological Aerosols from the Sahara and Asia Influence
Precipitation in the Western U.S.
SO SCIENCE
LA English
DT Article
ID ATMOSPHERIC ICE NUCLEI; OROGRAPHIC ENHANCEMENT; AIR-POLLUTION; LIQUID
WATER; MIXED-PHASE; CLOUD; PARTICLES; CLIMATE; SPECTROMETER; SUPPRESSION
AB Winter storms in California's Sierra Nevada increase seasonal snowpack and provide critical water resources and hydropower for the state. Thus, the mechanisms influencing precipitation in this region have been the subject of research for decades. Previous studies suggest Asian dust enhances cloud ice and precipitation, whereas few studies consider biological aerosols as an important global source of ice nuclei (IN). Here, we show that dust and biological aerosols transported from as far as the Sahara were present in glaciated high-altitude clouds coincident with elevated IN concentrations and ice-induced precipitation. This study presents the first direct cloud and precipitation measurements showing that Saharan and Asian dust and biological aerosols probably serve as IN and play an important role in orographic precipitation processes over the western United States.
C1 [Creamean, Jessie M.; Suski, Kaitlyn J.; Cazorla, Alberto; Prather, Kimberly A.] Univ Calif San Diego, Dept Chem & Biochem, La Jolla, CA 92093 USA.
[Rosenfeld, Daniel] Hebrew Univ Jerusalem, Inst Earth Sci, IL-91904 Jerusalem, Israel.
[DeMott, Paul J.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Sullivan, Ryan C.] Carnegie Mellon Univ, Ctr Atmospher Particle Studies, Pittsburgh, PA 15213 USA.
[White, Allen B.; Ralph, F. Martin] NOAA, PSD, ESRL, Boulder, CO 80305 USA.
[Ralph, F. Martin; Prather, Kimberly A.] Univ Calif San Diego, SIO, La Jolla, CA 92093 USA.
[Minnis, Patrick] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Comstock, Jennifer M.; Tomlinson, Jason M.] Pacific NW Natl Lab, Atmospher Sci & Global Change Div, Richland, WA 99352 USA.
RP Prather, KA (reprint author), Univ Calif San Diego, Dept Chem & Biochem, La Jolla, CA 92093 USA.
EM kprather@ucsd.edu
RI Sullivan, Ryan/B-4674-2008; DeMott, Paul/C-4389-2011; Tomlinson,
Jason/C-6566-2009; Rosenfeld, Daniel/F-6077-2016; Minnis,
Patrick/G-1902-2010;
OI Sullivan, Ryan/0000-0003-0701-7158; DeMott, Paul/0000-0002-3719-1889;
Rosenfeld, Daniel/0000-0002-0784-7656; Minnis,
Patrick/0000-0002-4733-6148; Creamean, Jessie/0000-0003-3819-5600
FU California Energy Commission [CEC 500-09-043]; Atmospheric System
Research (ASR)/U.S. Department of Energy (DOE) program; ASR/DOE program
[DE-SC0000991/003]; NASA MAPS Program
FX Funding was provided by the California Energy Commission under contract
CEC 500-09-043. D. R. was funded under the Atmospheric System Research
(ASR)/U.S. Department of Energy (DOE) program. P. M. was supported by
the ASR/DOE program under DE-SC0000991/003 and the NASA MAPS Program. J.
Mayer, E. Fitzgerald, D. Collins, and J. Cahill provided assistance with
UCSD/SIO equipment setup. The authors gratefully acknowledge the NOAA
Air Resources Laboratory (ARL) for the provision of the HYSPLIT
transport and dispersion model and READY website
(www.arl.noaa.gov/ready.php) used in this publication and the Office of
Naval Research for provision of NAAPS data. J. Ayers and R. Palikonda
(Science Systems and Applications) provided GOES-11 cloud top heights
used for HYSPLIT back trajectory analysis and %Ice in cloud. The
deployment of the NOAA and UCSD/SIO equipment at the Sugar Pine site
involved many field staff, particularly C. King (NOAA/ESRL/PSD). The
deployment of the DOE Gulfstream-1 involved many PNNL/Atmospheric
Radiation Measurement field staff, particularly E. Dukes, J. Hubbe, C.
Kluzek, H. Jonsson, M. Pekour, and B. Schmid. M. Hubbell and B. Svancara
flew the G-1 for the CalWater flight campaign. D. Collins and R.
Spackman provided insightful discussions during the editing stages of
this manuscript. T. Lersch of R. J. Lee provided TEM analyses of
collected IN. Data available in this paper are available in the
supplementary materials.
NR 44
TC 140
Z9 142
U1 15
U2 250
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD MAR 29
PY 2013
VL 339
IS 6127
BP 1572
EP 1578
DI 10.1126/science.1227279
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 114HL
UT WOS:000316731600040
PM 23449996
ER
PT J
AU Pearse, J
Lundgren, P
AF Pearse, Jill
Lundgren, Paul
TI Source model of deformation at Lazufre volcanic center, central Andes,
constrained by InSAR time series
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID LONG VALLEY CALDERA; CAMPI-FLEGREI CALDERA; EASTERN CALIFORNIA; MAGMA
BODY; NEW-MEXICO; UPLIFT; INFLATION; SOCORRO; AREA
AB Recent interferometric synthetic aperture radar (InSAR) observations of the Lazufre region, central Andes, show large-scale uplift at a rate of about 3 cm/yr, beginning between 1998 and 2002. The initiation of this activity during the ERS satellite mission and its proximity to active volcanoes have made Lazufre the focus of several studies aimed at understanding its source geometry, its relation to nearby volcanoes, and whether or not the source area is expanding. There now exists a longer time series from multiple ERS/ENVISAT satellite tracks that allows a more comprehensive examination of the source geometry and its temporal and spatial variation, if any. We processed 15 years of InSAR data from three separate tracks; modeling the different look geometries provided greater resolution of source depth and geometry. We conclude that the source is a shallowly dipping sill at a depth of about 8 km, with no evidence of lateral expansion.
C1 [Pearse, Jill; Lundgren, Paul] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Pearse, Jill] Alberta Geol Survey, Edmonton, AB T6B 2X3, Canada.
RP Pearse, J (reprint author), Alberta Geol Survey, 4999 98 Ave NW, Edmonton, AB T6B 2X3, Canada.
EM jillpearse@gmail.com
FU National Aeronautics and Space Administration at the Jet Propulsion
Laboratory, California Institute of Technology
FX ERS and Envisat SAR data were provided courtesy of the European Space
Agency through M. Pritchard. The manuscript benefited from thoughtful
reviews by M. Shirzaei and M. Poland. The research described in this
paper was supported under contract with the National Aeronautics and
Space Administration at the Jet Propulsion Laboratory, California
Institute of Technology.
NR 25
TC 7
Z9 7
U1 1
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 28
PY 2013
VL 40
IS 6
BP 1059
EP 1064
DI 10.1002/grl.50276
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 148AY
UT WOS:000319215700007
ER
PT J
AU Zhang, CD
Gottschalck, J
Maloney, ED
Moncrieff, MW
Vitart, F
Waliser, DE
Wang, B
Wheeler, MC
AF Zhang, Chidong
Gottschalck, Jon
Maloney, Eric D.
Moncrieff, Mitchell W.
Vitart, Frederic
Waliser, Duane E.
Wang, Bin
Wheeler, Matthew C.
TI Cracking the MJO nut
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID MADDEN-JULIAN OSCILLATION; TROPICAL INTRASEASONAL OSCILLATION; ORGANIZED
CONVECTIVE SYSTEMS; GENERAL-CIRCULATION MODELS; CLOUD-RESOLVING MODEL;
SIMULATION DIAGNOSTICS; EQUATORIAL WAVES; WESTERN PACIFIC; FORECAST
SKILL; CLIMATE MODELS
AB The Madden-Julian oscillation poses great challenges to our understanding and prediction of tropical convection and the large-scale circulation. Several internationally coordinated activities were recently formed to meet the challenges from the perspectives of numerical simulations, prediction, diagnostics, and virtual and actual field campaigns. This article provides a brief description of these activities and their connections, with the motivation in part to encourage the next generation of physical scientists to help solve the grand challenging problem of the Madden-Julian oscillation.
C1 [Zhang, Chidong] Univ Miami, Miami, FL USA.
[Gottschalck, Jon] NOAA NCEP CPC, College Pk, MD USA.
[Maloney, Eric D.] Colorado State Univ, Ft Collins, CO 80523 USA.
[Moncrieff, Mitchell W.] NCAR, Boulder, CO USA.
[Vitart, Frederic] ECMWF, Reading, Berks, England.
[Waliser, Duane E.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Wang, Bin] Univ Hawaii, Honolulu, HI 96822 USA.
[Wheeler, Matthew C.] CAWCR, Melbourne, Vic, Australia.
RP Zhang, CD (reprint author), 4600 Rickenbacker Causeway, Miami, FL 33149 USA.
EM czhang@rsmas.miami.edu
RI Wheeler, Matthew/C-9038-2011; Maloney, Eric/A-9327-2008
OI Wheeler, Matthew/0000-0002-9769-1973; Maloney, Eric/0000-0002-2660-2611
FU NSF; NOAA; DOE; ONR; NASA; Bureau of Meteorology; CSIRO; National
Science Foundation
FX The authors thank George Kiladis for his constructive comments on an
earlier version of the manuscript. The writing of this article was
supported by grants and contracts from NSF, NOAA, DOE, ONR, and NASA.
DW's contribution was carried out on behalf of the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
NASA. The Centre for Australian Weather and Climate Research is a
partnership between the Bureau of Meteorology and CSIRO. The National
Center for Atmospheric Research is sponsored by the National Science
Foundation.
NR 75
TC 63
Z9 64
U1 2
U2 30
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD MAR 28
PY 2013
VL 40
IS 6
BP 1223
EP 1230
DI 10.1002/grl.50244
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA 148AY
UT WOS:000319215700037
ER
PT J
AU Baasandorj, M
Fleming, EL
Jackman, CH
Burkholder, JB
AF Baasandorj, Munkhbayar
Fleming, Eric L.
Jackman, Charles H.
Burkholder, James B.
TI O(D-1) Kinetic Study of Key Ozone Depleting Substances and Greenhouse
Gases
SO JOURNAL OF PHYSICAL CHEMISTRY A
LA English
DT Article
ID RATE COEFFICIENTS; ATMOSPHERIC CHEMISTRY; OH; HALOCARBONS; LIFETIMES
AB A key stratospheric loss process for ozone depleting substances (ODSs) and greenhouse gases (GHGs) is reaction with the O(D-1) atom. In this study, rate coefficients, k, for the O(D-1) atom reaction were measured for the following key halocarbons: chlorofluorocarbons (CFCs) CFCl3 (CFC-11), CF2Cl2 (CFC-12), CFCl2 center dot CF2Cl (CFC-113), CF2ClCF2Cl (CFC-114), CF3CF2Cl (CFC-115); hydrochlorofluorocarbons (HCFCs) CHF2Cl (HCFC-22), CH3CClF2 (HCFC-142b); and hydrofluorocarbons (HFCs) CHF3 (HFC-23), CHF2CF3 (HFC-125), CH3CF3 (HFC-143a), and CF3CHFCF3 (HFC-227ea). Total rate coefficients, k(T), corresponding to the loss of the O(D-1) atom, were measured over the temperature range 217-373 K using a competitive reactive technique. k(T) values for the CFC and HCFC reactions were >1 x 10(-10) cm(3) molecule(-1) s(-1), except for CFC-115, and the rate coefficients for the HFCs were in the range (0.095-0.72) x 10(-10) cm(3) molecule(-1) s(-1). Rate coefficients for the CFC-12, CFC-114, CFC-115, HFC-23, HFC-125, HFC-143a, and HFC-227ea reactions were observed to have a weak negative temperature dependence, E/R approximate to -25 K. Reactive rate coefficients, k(R), corresponding to the loss of the halocarbon, were measured for CFC-11, CFC-115, HCFC-22, HCFC-142b, HFC-23, HFC-125, HFC-143a, and HFC-227ea using a relative rate technique. The reactive branching ratio obtained was dependent on the composition of the halocarbon and the trend in O(D-1) reactivity with the extent of hydrogen and chlorine substitution is discussed. The present results are critically compared with previously reported kinetic data and the discrepancies are discussed. 2D atmospheric model calculations were used to evaluate the local and global annually averaged atmospheric lifetimes of the halocarbons and the contribution of O(D-1) chemistry to their atmospheric loss. The O(D-1) reaction was found to be a major global loss process for CFC-114 and CFC-115 and a secondary global loss process for the other molecules included in this study.
C1 [Baasandorj, Munkhbayar; Burkholder, James B.] NOAA, Earth Syst Res Lab, Div Chem Sci, Boulder, CO 80305 USA.
[Baasandorj, Munkhbayar] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80309 USA.
[Fleming, Eric L.; Jackman, Charles H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fleming, Eric L.] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
RP Burkholder, JB (reprint author), NOAA, Earth Syst Res Lab, Div Chem Sci, Boulder, CO 80305 USA.
EM James.B.Burkholder@noaa.gov
RI Burkholder, James/H-4914-2013; Jackman, Charles/D-4699-2012; Manager,
CSD Publications/B-2789-2015
FU NOAA's Climate Goal Program; NASA's Atmospheric Composition: Laboratory
Studies and Modeling and Analysis Program
FX This work was supported in part by NOAA's Climate Goal and NASA's
Atmospheric Composition: Laboratory Studies and Modeling and Analysis
Programs.
NR 20
TC 4
Z9 4
U1 3
U2 26
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1089-5639
J9 J PHYS CHEM A
JI J. Phys. Chem. A
PD MAR 28
PY 2013
VL 117
IS 12
BP 2434
EP 2445
DI 10.1021/jp312781c
PG 12
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 118NO
UT WOS:000317032400004
PM 23441917
ER
PT J
AU Norris, RP
Afonso, J
Bacon, D
Beck, R
Bell, M
Beswick, RJ
Best, P
Bhatnagar, S
Bonafede, A
Brunetti, G
Budavari, T
Cassano, R
Condon, JJ
Cress, C
Dabbech, A
Feain, I
Fender, R
Ferrari, C
Gaensler, BM
Giovannini, G
Haverkorn, M
Heald, G
Van der Heyden, K
Hopkins, AM
Jarvis, M
Johnston-Hollitt, M
Kothes, R
Van Langevelde, H
Lazio, J
Mao, MY
Martinez-Sansigre, A
Mary, D
Mcalpine, K
Middelberg, E
Murphy, E
Padovani, P
Paragi, Z
Prandoni, I
Raccanelli, A
Rigby, E
Roseboom, IG
Rottgering, H
Sabater, J
Salvato, M
Scaife, AMM
Schilizzi, R
Seymour, N
Smith, DJB
Umana, G
Zhao, GB
Zinn, PC
AF Norris, Ray P.
Afonso, J.
Bacon, D.
Beck, Rainer
Bell, Martin
Beswick, R. J.
Best, Philip
Bhatnagar, Sanjay
Bonafede, Annalisa
Brunetti, Gianfranco
Budavari, Tamas
Cassano, Rossella
Condon, J. J.
Cress, Catherine
Dabbech, Arwa
Feain, I.
Fender, Rob
Ferrari, Chiara
Gaensler, B. M.
Giovannini, G.
Haverkorn, Marijke
Heald, George
Van der Heyden, Kurt
Hopkins, A. M.
Jarvis, M.
Johnston-Hollitt, Melanie
Kothes, Roland
Van Langevelde, Huib
Lazio, Joseph
Mao, Minnie Y.
Martinez-Sansigre, Alejo
Mary, David
Mcalpine, Kim
Middelberg, E.
Murphy, Eric
Padovani, P.
Paragi, Zsolt
Prandoni, I.
Raccanelli, A.
Rigby, Emma
Roseboom, I. G.
Rottgering, H.
Sabater, Jose
Salvato, Mara
Scaife, Anna M. M.
Schilizzi, Richard
Seymour, N.
Smith, Dan J. B.
Umana, Grazia
Zhao, G. -B.
Zinn, Peter-Christian
TI Radio Continuum Surveys with Square Kilometre Array Pathfinders
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA
LA English
DT Article
DE radiotelescopes; surveys; galaxy evolution; cosmology
ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; DEEP-FIELD-SOUTH;
STAR-FORMATION HISTORY; K-Z RELATION; PROBABILISTIC
CROSS-IDENTIFICATION; SPECTRAL ENERGY-DISTRIBUTIONS; INFRARED
EXTRAGALACTIC FIELD; BASE-LINE INTERFEROMETRY; SPITZER-SPACE-TELESCOPE
AB In the lead-up to the Square Kilometre Array (SKA) project, several next-generation radio telescopes and upgrades are already being built around the world. These include APERTIF (The Netherlands), ASKAP (Australia), e-MERLIN (UK), VLA (USA), e-EVN (based in Europe), LOFAR (The Netherlands), MeerKAT (South Africa), and the Murchison Widefield Array. Each of these new instruments has different strengths, and coordination of surveys between them can help maximise the science from each of them. A radio continuum survey is being planned on each of them with the primary science objective of understanding the formation and evolution of galaxies over cosmic time, and the cosmological parameters and large-scale structures which drive it. In pursuit of this objective, the different teams are developing a variety of new techniques, and refining existing ones. To achieve these exciting scientific goals, many technical challenges must be addressed by the survey instruments. Given the limited resources of the global radio-astronomical community, it is essential that we pool our skills and knowledge. We do not have sufficient resources to enjoy the luxury of re-inventing wheels. We face significant challenges in calibration, imaging, source extraction and measurement, classification and cross-identification, redshift determination, stacking, and data-intensive research. As these instruments extend the observational parameters, we will face further unexpected challenges in calibration, imaging, and interpretation. If we are to realise the full scientific potential of these expensive instruments, it is essential that we devote enough resources and careful study to understanding the instrumental effects and how they will affect the data. We have established an SKA Radio Continuum Survey working group, whose prime role is to maximise science from these instruments by ensuring we share resources and expertise across the projects. Here we describe these projects, their science goals, and the technical challenges which are being addressed to maximise the science return.
C1 [Norris, Ray P.; Feain, I.; Mao, Minnie Y.; Seymour, N.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Afonso, J.; Bell, Martin; Gaensler, B. M.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW 2016, Australia.
[Afonso, J.] Univ Lisbon, Observ Astron Lisboa, Ctr Astron & Astrofis, P-1349018 Lisbon, Portugal.
[Bacon, D.; Martinez-Sansigre, Alejo; Raccanelli, A.; Zhao, G. -B.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Beck, Rainer] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Bell, Martin; Fender, Rob; Scaife, Anna M. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Bell, Martin; Feain, I.; Gaensler, B. M.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Beswick, R. J.; Schilizzi, Richard] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Best, Philip; Sabater, Jose] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Bhatnagar, Sanjay; Condon, J. J.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Bonafede, Annalisa; Salvato, Mara] Max Planck Inst Plasma Phys, D-85748 Garching, Germany.
[Brunetti, Gianfranco; Cassano, Rossella; Giovannini, G.; Prandoni, I.] INAF IRA, I-40129 Bologna, Italy.
[Budavari, Tamas] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Cress, Catherine; Jarvis, M.] Univ Western Cape, Dept Phys, ZA-7535 Cape Town, South Africa.
[Dabbech, Arwa; Ferrari, Chiara; Mary, David] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR 7293, F-06300 Nice, France.
[Haverkorn, Marijke; Van Langevelde, Huib; Rottgering, H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Haverkorn, Marijke] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Heald, George] ASTRON, NL-7990 AA Dwingeloo, Netherlands.
[Van der Heyden, Kurt] Univ Cape Town, Dept Astron, Astrophys Cosmol & Grav Ctr, ZA-7701 Rondebosch, South Africa.
[Hopkins, A. M.; Mao, Minnie Y.] Australian Astron Observ, Epping, NSW 1710, Australia.
[Jarvis, M.; Mcalpine, Kim; Smith, Dan J. B.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Jarvis, M.] Univ Oxford, Oxford OX1 3RH, England.
[Johnston-Hollitt, Melanie] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand.
[Kothes, Roland] Natl Res Council Canada, Natl Sci Infrastruct, Domin Radio Astrophys Observ, Penticton, BC V2A 6J9, Canada.
[Van Langevelde, Huib] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands.
[Lazio, Joseph; Raccanelli, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mao, Minnie Y.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Mao, Minnie Y.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia.
[Mcalpine, Kim] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa.
[Middelberg, E.; Zinn, Peter-Christian] Ruhr Univ Bochum, Astron Inst, D-44801 Bochum, Germany.
[Murphy, Eric] Carnegie Observ, Pasadena, CA 91101 USA.
[Padovani, P.] European So Observ, D-85748 Garching, Germany.
[Raccanelli, A.] CALTECH, Pasadena, CA 91125 USA.
[Rigby, Emma] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Umana, Grazia] INAF Catania Astrophys Observ, I-95123 Catania, Italy.
RP Norris, RP (reprint author), CSIRO Astron & Space Sci, POB 76, Epping, NSW 1710, Australia.
EM Ray.Norris@csiro.au
RI Norris, Ray/A-1316-2008; Afonso, Jose/B-5185-2013;
OI Norris, Ray/0000-0002-4597-1906; Afonso, Jose/0000-0002-9149-2973;
Raccanelli, Alvise/0000-0001-6726-0438; Prandoni,
Isabella/0000-0001-9680-7092; Umana, Grazia/0000-0002-6972-8388;
Cassano, Rossella/0000-0003-4046-0637; Brunetti,
Gianfranco/0000-0003-4195-8613; Giovannini,
Gabriele/0000-0003-4916-6362; Seymour, Nicholas/0000-0003-3506-5536; van
Langevelde, Huib Jan/0000-0002-0230-5946; Padovani,
Paolo/0000-0002-4707-6841; Paragi, Zsolt/0000-0002-5195-335X; Gaensler,
Bryan/0000-0002-3382-9558; Sabater, Jose/0000-0003-1149-6294
FU Australian Research Council Centre of Excellence for All-sky
Astrophysics (CAASTRO) [CE110001020]; Science and Technology Foundation
(FCT, Portugal) [PTDC/FIS/100170/2008, PTDC/CTE-AST/105287/2008,
PEst-OE/FIS/UI2751/2011]; Agence Nationale de la Recherche
[ANR-09-JCJC-0001-01]; Observatoire de la Cote d'Azur; Conseil regional
Provence-Alpes-Cote d'Azur
FX We are indebted to the Lorentz Center in Leiden for hosting and funding
the workshop in 2011 February, which gave rise to this paper. Parts of
this research were supported by the Australian Research Council Centre
of Excellence for All-sky Astrophysics (CAASTRO), through project number
CE110001020. Part of the research described in this paper was carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration. JA gratefully acknowledges support from the Science and
Technology Foundation (FCT, Portugal) through the research grants
PTDC/FIS/100170/2008, PTDC/CTE-AST/105287/2008, and
PEst-OE/FIS/UI2751/2011. CF and AD acknowledge financial support by the
Agence Nationale de la Recherche through grant ANR-09-JCJC-0001-01. AD
acknowledges financial support from the joint PhD program of
Observatoire de la Cote d'Azur and Conseil regional Provence-Alpes-Cote
d'Azur.
NR 465
TC 17
Z9 17
U1 1
U2 16
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 1323-3580
EI 1448-6083
J9 PUBL ASTRON SOC AUST
JI Publ. Astron. Soc. Aust.
PD MAR 27
PY 2013
VL 30
AR UNSP e020
DI 10.1017/pas.2012.020
PG 54
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 161ZZ
UT WOS:000320235100001
ER
PT J
AU Charlton-Perez, AJ
Baldwin, MP
Birner, T
Black, RX
Butler, AH
Calvo, N
Davis, NA
Gerber, EP
Gillett, N
Hardiman, S
Kim, J
Kruger, K
Lee, YY
Manzini, E
McDaniel, BA
Polvani, L
Reichler, T
Shaw, TA
Sigmond, M
Son, SW
Toohey, M
Wilcox, L
Yoden, S
Christiansen, B
Lott, F
Shindell, D
Yukimoto, S
Watanabe, S
AF Charlton-Perez, Andrew J.
Baldwin, Mark P.
Birner, Thomas
Black, Robert X.
Butler, Amy H.
Calvo, Natalia
Davis, Nicholas A.
Gerber, Edwin P.
Gillett, Nathan
Hardiman, Steven
Kim, Junsu
Krueger, Kirstin
Lee, Yun-Young
Manzini, Elisa
McDaniel, Brent A.
Polvani, Lorenzo
Reichler, Thomas
Shaw, Tiffany A.
Sigmond, Michael
Son, Seok-Woo
Toohey, Matthew
Wilcox, Laura
Yoden, Shigeo
Christiansen, Bo
Lott, Franois
Shindell, Drew
Yukimoto, Seiji
Watanabe, Shingo
TI On the lack of stratospheric dynamical variability in low-top versions
of the CMIP5 models
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID TEMPERATURE TRENDS; CLIMATE-CHANGE; PART I; WINTER; CIRCULATION; OZONE;
CONFIGURATION; SIMULATIONS; IMPACT; WELL
AB We describe the main differences in simulations of stratospheric climate and variability by models within the fifth Coupled Model Intercomparison Project (CMIP5) that have a model top above the stratopause and relatively fine stratospheric vertical resolution (high-top), and those that have a model top below the stratopause (low-top). Although the simulation of mean stratospheric climate by the two model ensembles is similar, the low-top model ensemble has very weak stratospheric variability on daily and interannual time scales. The frequency of major sudden stratospheric warming events is strongly underestimated by the low-top models with less than half the frequency of events observed in the reanalysis data and high-top models. The lack of stratospheric variability in the low-top models affects their stratosphere-troposphere coupling, resulting in short-lived anomalies in the Northern Annular Mode, which do not produce long-lasting tropospheric impacts, as seen in observations. The lack of stratospheric variability, however, does not appear to have any impact on the ability of the low-top models to reproduce past stratospheric temperature trends. We find little improvement in the simulation of decadal variability for the high-top models compared to the low-top, which is likely related to the fact that neither ensemble produces a realistic dynamical response to volcanic eruptions. Citation: Charlton-Perez, A. J., et al. (2013), On the lack of stratospheric dynamical variability in low-top versions of the CMIP5 models, J. Geophys. Res. Atmos., 118, 2494-2505, doi:10.1002/jgrd.50125.
C1 [Charlton-Perez, Andrew J.] Univ Reading, Dept Meteorol, Reading, Berks, England.
[Baldwin, Mark P.] Univ Exeter, Coll Engn Math & Phys Sci, Exeter, Devon, England.
[Birner, Thomas; Davis, Nicholas A.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Black, Robert X.; Lee, Yun-Young] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA.
[Butler, Amy H.] Climate Predict Ctr, College Pk, MD USA.
[Calvo, Natalia] Univ Complutense Madrid, Dept Fis Tierra 2, Madrid, Spain.
[Gerber, Edwin P.] NYU, New York, NY USA.
[Gillett, Nathan] Canadian Ctr Climate Modelling & Anal, Victoria, BC, Canada.
[Hardiman, Steven] Met Off, Exeter, Devon, England.
[Kim, Junsu; Reichler, Thomas] Univ Utah, Dept Atmospher Sci, Salt Lake City, UT 84112 USA.
[Manzini, Elisa] Max Planck Inst Meteorol, D-20146 Hamburg, Germany.
[McDaniel, Brent A.] Kennesaw State Univ, Dept Biol & Phys, Kennesaw, GA USA.
[Polvani, Lorenzo; Shaw, Tiffany A.] Columbia Univ, Dept Appl Math & Appl Phys, New York, NY USA.
[Sigmond, Michael] Univ Toronto, Dept Phys, Toronto, ON, Canada.
[Son, Seok-Woo] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul 151, South Korea.
[Krueger, Kirstin; Toohey, Matthew] GEOMAR Helmholtz Ctr Ocean Res Kiel, Kiel, Germany.
[Wilcox, Laura] Univ Reading, Natl Ctr Atmospher Sci, Reading, Berks, England.
[Yoden, Shigeo] Kyoto Univ, Kyoto, Japan.
[Christiansen, Bo] Danish Meteorol Inst, Copenhagen, Denmark.
[Lott, Franois] Ecole Normale Super, Lab Meteorol Dynam, F-75231 Paris, France.
[Shindell, Drew] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Yukimoto, Seiji] Met Res Inst, Tsukuba, Ibaraki, Japan.
[Watanabe, Shingo] JAMSTEC, Res Inst Global Change, Tokyo, Japan.
RP Charlton-Perez, AJ (reprint author), Univ Reading, Dept Meteorol, Reading, Berks, England.
EM a.j.charlton@reading.ac.uk
RI Sigmond, Michael /K-3169-2012; Wilcox, Laura/F-3394-2013; Toohey,
Matthew/G-3129-2010; Butler, Amy/K-6190-2012; Birner,
Thomas/A-2108-2008; Shindell, Drew/D-4636-2012; Son, Seok-Woo
/A-8797-2013; YODEN, SHIGEO/P-9065-2014; Black, Robert/L-8522-2014;
Watanabe, Shingo/L-9689-2014;
OI Christiansen, Bo/0000-0003-2792-4724; Charlton-Perez,
Andrew/0000-0001-8179-6220; Sigmond, Michael /0000-0003-2191-9756;
Wilcox, Laura/0000-0001-5691-1493; Toohey, Matthew/0000-0002-7070-405X;
Butler, Amy/0000-0002-3632-0925; Birner, Thomas/0000-0002-2966-3428;
Watanabe, Shingo/0000-0002-2228-0088; CALVO FERNANDEZ,
NATALIA/0000-0001-6213-1864
FU National Centre for Atmospheric Science [CMIP5]; NSF under the US CLIVAR
program; NSF under Office of Polar Program; U.S. National Science
Foundation; U.S. Department of Energy, Office of Biological and
Environmental Research [DE-FOA000024]; National Science Foundation
[ARC-1107384]; Spanish Ministry of Science and Innovation (MCINN)
[CGL2008-05968-C02-01]; National Science Foundation; BMBF [01LP1130B];
Joint DECC/Defra Met Office Hadley Centre Climate Programme [GA01101];
European Commission [226520]
FX We acknowledge the World Climate Research Programme's Working Group on
Coupled Modelling, which is responsible for CMIP, and we thank the
climate modeling groups for producing and making available the model
output listed in Table 1. For CMIP the U.S. Department of Energy's
Program for Climate Model Diagnosis and Intercomparison provides
coordinating support and led development of software infrastructure in
partnership with the Global Organization for Earth System Science
Portals. A. J. C.-P. and L. J. W. were supported by an National Centre
for Atmospheric Science CMIP5 grant. M. P. B. was funded by NSF under
the US CLIVAR program and the Office of Polar Programs. T. B. and N. A.
D. acknowledge support by the U.S. National Science Foundation. The
research efforts of R. X. B., B. A. M. & Y.-Y. L. were conducted under
support by the U.S. Department of Energy, Office of Biological and
Environmental Research, Award No. DE-FOA000024 and by the National
Science Foundation Grant, ARC-1107384. N. C. was supported by the
Spanish Ministry of Science and Innovation (MCINN) through the
CGL2008-05968-C02-01 project. E. P. G. was supported by the National
Science Foundation. The work of M. T. and K. K. contributes to the BMBF
joint research project MiKlip within the project ALARM through the grant
01LP1130B. The work of S. C. H. was supported by the Joint DECC/Defra
Met Office Hadley Centre Climate Programme (GA01101). We also
acknowledge the European Commission's 7th Framework Programme, under
Grant Agreement number 226520, COMBINE project which supplied some data
not available from the CMIP5 archive. We also thank Gerard Devine
(NCAS-CMS) for help with accessing and parsing meta-data information
from the models.
NR 40
TC 86
Z9 87
U1 3
U2 67
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 MAR 27
PY 2013
VL 118
IS 6
BP 2494
EP 2505
DI 10.1002/jgrd.50125
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 129MB
UT WOS:000317843200003
ER
PT J
AU Bergman, JW
Fierli, F
Jensen, EJ
Honomichl, S
Pan, LL
AF Bergman, John W.
Fierli, Federico
Jensen, Eric J.
Honomichl, Shawn
Pan, Laura L.
TI Boundary layer sources for the Asian anticyclone: Regional contributions
to a vertical conduit
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID TROPICAL TROPOPAUSE LAYER; LOWER STRATOSPHERE; SUMMER MONSOON;
WATER-VAPOR; SEASONAL-VARIATION; TRANSPORT; MODEL; AIR; TRAJECTORIES;
CIRCULATION
AB The transport of air from the planetary boundary layer (PBL) into the Asian Summer Monsoon anticyclone is investigated using backward trajectories initiated within the anti-cyclone at 100 mb and 200 mb during August 2011. Transport occurs through a well-defined conduit centered over the southern Tibetan plateau, where convection lofts air parcels into the anticyclone. The conduit, as a dynamical feature, is distinct from the anticyclone. Thus, while the anticyclone influences transport through the upper troposphere and lower stratosphere, it does not by itself define a transport pipeline through that region. To quantify model sensitivities, parcel trajectories are calculated using wind fields from multiple analysis data sets (European Centre for Medium-Range Weather Forecasts, National Center for Environmental Prediction's Global Forecasting System, and NASA's Modern-Era Retrospective Analysis for Research and Applications [MERRA]) and from synthetically modified data sets that explore the roles of vertical motion and horizontal resolution for discrepancies among these calculations. All calculations agree on the relative contributions to PBL sources for the anticyclone from large-scale regions with Tibetan Plateau and India/SE Asia being the most important. However, they disagree on the total fraction of air within the anticyclone that was recently in the PBL. At 200 mbar, calculations using MERRA are clear outliers due to problematic vertical motion in those data. Large differences among the different data sets at 100 mbar are more closely related to horizontal resolution. It is speculated that this reflects the importance of deep, small-scale convective updrafts for transport to 100 mbar. Citation: Bergman, J. W., F. Fierli, E. J. Jensen, S. Honomichl, and L. L. Pan (2013), Boundary layer sources for the Asian anticyclone: Regional contributions to a vertical conduit, J. Geophys. Res. Atmos., 118, 2560-2575, doi:10.1002/jgrd.50142.
C1 [Bergman, John W.] Bay Area Environm Res Inst, Sonoma, CA USA.
[Bergman, John W.; Honomichl, Shawn; Pan, Laura L.] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA.
[Fierli, Federico] CNR, Inst Atmospher Sci & Climate, Rome, Italy.
[Jensen, Eric J.] NASA, Ames Res Ctr, Div Earth Sci, Moffett Field, CA 94035 USA.
RP Bergman, JW (reprint author), Natl Ctr Atmospher Res, Div Atmospher Chem, POB 3000, Boulder, CO 80307 USA.
EM bergman@ucar.edu
RI Pan, Laura/A-9296-2008;
OI Pan, Laura/0000-0001-7377-2114; Fierli, Federico/0000-0001-9975-2883
FU National Science Foundation
FX This work benefitted from helpful conversations with and comments on
early versions of the manuscript from C. Homeyer, S. Fueglistaler, H.
Garny, M. Park, L. Pfister, W. Randel, and two anonymous reviewers. J.
Bergman. F. Fierli, and E. Jensen were visitors at the Atmospheric
Chemistry Division of NCAR during the execution of this study. The
National Center for Atmospheric Research is operated by the University
Corporation for Atmospheric Research, under sponsorship of the National
Science Foundation.
NR 44
TC 23
Z9 23
U1 0
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 MAR 27
PY 2013
VL 118
IS 6
BP 2560
EP 2575
DI 10.1002/jgrd.50142
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 129MB
UT WOS:000317843200008
ER
PT J
AU Allen, DR
Douglass, AR
Strahan, SE
AF Allen, Douglas R.
Douglass, Anne R.
Strahan, Susan E.
TI The large-scale frozen-in anticyclone in the 2011 Arctic summer
stratosphere
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID NORTHERN-HEMISPHERE; TRANSPORT MODEL; GMI CHEMISTRY; OZONE LOSS;
CLIMATOLOGY; VORTEX
AB The 2011 Arctic stratospheric final warming was characterized by a large-scale frozen-in anticyclone (FrIAC) that rapidly displaced the winter polar vortex, establishing unusually strong polar easterlies. A comprehensive overview of the 2011 FrIAC is provided using meteorological analyses, Microwave Limb Sounder (MLS) N2O observations, and N2O simulations from the Global Modeling Initiative (GMI) 3-D chemistry and transport model and the Van Leer Icosahedral Triangular Advection (VITA) 2-D (latitude x longitude) isentropic transport model. A vortex edge diagnostic is used to determine the FrIAC boundary, allowing quantification of several FrIAC properties. The 2011 FrIAC originated over North Africa in late March and traveled eastward and poleward over 2 weeks, forming a strong anticyclone that extended from similar to 580-2100 K potential temperature (similar to 25-50 km). Low potential vorticity (PV) was transported to the pole with the FrIAC in early April; during May, most of the PV signature decayed due to diabatic processes. A small remnant negative PV anomaly persisted near the pole until mid-June. Tracer equivalent latitude was low initially and remained low throughout the summer. GMI, VITA, and MLS showed elevated N2O in the FrIAC, although the peak value was smaller in GMI due to a subtropical low bias. The high-resolution (similar to 20 km) VITA filamentary structure quantitatively matched most of the features observed by MLS when smoothed to match the MLS resolution. The high-N2O anomaly persisted in the middle stratosphere over 4 months until late August, when it was destroyed by horizontal and vertical shearing, combined with photochemical processes. Citation: Allen, D. R., A. R. Douglass, and S. E. Strahan (2013), The large-scale frozen-in anticyclone in the 2011 Arctic summer stratosphere, J. Geophys. Res. Atmos., 118, 2656-2672, doi:10.1002/jgrd.50256.
C1 [Allen, Douglas R.] USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA.
[Douglass, Anne R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Strahan, Susan E.] Univ Space Res Assoc, Columbia, MD USA.
RP Allen, DR (reprint author), USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA.
EM Douglas.Allen@nrl.navy.mil
RI Douglass, Anne/D-4655-2012
FU NASA Atmospheric Composition: Modeling and Analysis Program
[NNHH09ZDA001N]; Office of Naval Research
FX This work was supported by a subcontract from the NASA Atmospheric
Composition: Modeling and Analysis Program, NNHH09ZDA001N. Work at the
Naval Research Laboratory is sponsored by the Office of Naval Research.
We would like to thank Gloria Manney for providing the gridded MLS data
used to initialize the VITA simulations. We also acknowledge the Global
Modeling and Assimilation Office and the Goddard Earth Science Data and
Information Services Center for the dissemination of MERRA products.
NR 41
TC 3
Z9 3
U1 0
U2 20
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAR 27
PY 2013
VL 118
IS 6
BP 2656
EP 2672
DI 10.1002/jgrd.50256
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 129MB
UT WOS:000317843200016
ER
PT J
AU Brakebusch, M
Randall, CE
Kinnison, DE
Tilmes, S
Santee, ML
Manney, GL
AF Brakebusch, M.
Randall, C. E.
Kinnison, D. E.
Tilmes, S.
Santee, M. L.
Manney, G. L.
TI Evaluation of Whole Atmosphere Community Climate Model simulations of
ozone during Arctic winter 2004-2005
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID POLAR STRATOSPHERIC CLOUD; CHEMICAL-TRANSPORT MODEL; GENERAL-CIRCULATION
MODEL; CHLORINE ACTIVATION; SATELLITE-OBSERVATIONS; 3-DIMENSIONAL MODEL;
DEPLETION; TRACERS; DENITRIFICATION; LATITUDES
AB The work presented here evaluates polar stratospheric ozone simulations from the Whole Atmosphere Community Climate Model (WACCM) for the Arctic winter of 2004-2005. We use the Specified Dynamics version of WACCM (SD-WACCM), in which temperatures and winds are nudged to meteorological assimilation analysis results. Model simulations of ozone and related constituents generally compare well to observations from the Earth Observing System Microwave Limb Sounder (MLS). At most times, modeled ozone agrees with MLS data to within similar to 10%. However, a systematic high bias in ozone in the model of similar to 18% is found in the lowermost stratosphere in March. We attribute most of this ozone bias to too little heterogeneous processing of halogens late in the winter. We suggest that the model under-predicts ClONO2 early in the winter, which leads to less heterogeneous processing and too little activated chlorine. Model HCl could also be overestimated due to an underestimation of HCl uptake into supercooled ternary solution (STS) particles. In late winter, the model overestimates gas-phase HNO3, and thus NOy, which leads to an over-prediction of ClONO2 (under-prediction of activated chlorine). A sensitivity study, in which temperatures for heterogeneous chemistry reactions were reduced by 1.5 K, shows significant improvement of modeled ozone. Chemical ozone loss is inferred from the MLS observations using the pseudo-passive subtraction approach. The inferred ozone loss using this method is in agreement with or less than previous independent results for the Arctic winter of 2004-2005, reaching 1.0 ppmv on average and up to 1.6 ppmv locally in the polar vortex. Citation: Brakebusch, M., C. E. Randall, D. E. Kinnison, S. Tilmes, M. L. Santee, and G. L. Manney (2013), Evaluation of Whole Atmosphere Community Climate Model simulations of ozone during Arctic winter 2004-2005, J. Geophys. Res. Atmos., 118, 2673-2688, doi:10.1002/jgrd.50226.
C1 [Brakebusch, M.; Randall, C. E.] Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
[Brakebusch, M.; Randall, C. E.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Kinnison, D. E.; Tilmes, S.] Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80307 USA.
[Santee, M. L.; Manney, G. L.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Manney, G. L.] New Mexico Inst Min & Technol, Socorro, NM 87801 USA.
RP Brakebusch, M (reprint author), Univ Colorado, Dept Atmospher & Ocean Sci, Boulder, CO 80309 USA.
EM brakebusch@colorado.edu
RI Randall, Cora/L-8760-2014
OI Randall, Cora/0000-0002-4313-4397
FU JPL/NASA grant [1350080]; NSF [AGS 1135432]; National Science
Foundation; National Aeronautics and Space Administration
FX We thank C. S. Singleton for helpful discussions. M. B. and C. E. R.
were funded by JPL/NASA grant 1350080 and NSF award AGS 1135432. The
SD-WACCM simulations were carried out at NCAR. NCAR is sponsored by the
National Science Foundation. Work at the Jet Propulsion Laboratory,
California Institute of Technology, was done under contract with the
National Aeronautics and Space Administration.
NR 67
TC 19
Z9 20
U1 2
U2 30
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 MAR 27
PY 2013
VL 118
IS 6
BP 2673
EP 2688
DI 10.1002/jgrd.50226
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 129MB
UT WOS:000317843200017
ER
PT J
AU Ting, DZY
Soibel, A
Khoshakhlagh, A
Nguyen, J
Hoglund, L
Keo, SA
Mumolo, JM
Gunapala, SD
AF Ting, David Z. -Y.
Soibel, Alexander
Khoshakhlagh, Arezou
Nguyen, Jean
Hoeglund, Linda
Keo, Sam A.
Mumolo, Jason M.
Gunapala, Sarath D.
TI Exclusion, extraction, and junction placement effects in the
complementary barrier infrared detector
SO APPLIED PHYSICS LETTERS
LA English
DT Article
ID SUPERLATTICE; DEVICES; PERFORMANCE; HGCDTE
AB We demonstrate a long wavelength type-II superlattice (T2SL) complementary barrier infrared detector (CBIRD) with a double broken-gap junction bottom contact structure designed to reduce material growth demands without diminishing performance. Simulation suggests generation-recombination dark current suppression is the result of placing the electrical junction in the wide-gap hole barrier region, away from the metallurgical hole-barrier/ absorber heterojunction. The lower turn-on bias of the modified CBIRD is explained in terms of junction properties. We suggest that minority carrier exclusion and extraction effects are partially responsible for the observed low diffusion-limited CBIRD dark current despite short T2SL minority carrier lifetimes. (C) 2013 American Institute of Physics. [http://dx.doi.org/10.1063/1.4798551]
C1 [Ting, David Z. -Y.; Soibel, Alexander; Khoshakhlagh, Arezou; Nguyen, Jean; Hoeglund, Linda; Keo, Sam A.; Mumolo, Jason M.; Gunapala, Sarath D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ting, DZY (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM David.Z.Ting@jpl.nasa.gov
RI Soibel, Alexander/A-1313-2007
FU National Aeronautics and Space Administration
FX The authors thank S. Bandara, E.S. Daniel, E.R. Blazejewski, T.J.
Cunningham, D.R. Rhiger, R.E. de Wames, and J.N. Schulman for helpful
discussions and R. Liang, M. Herman, E. Kolawa, and M. Tidrow for
encouragement and support. The research described in this publication
was carried out at the Jet Propulsion Laboratory, California Institute
of Technology, under a contract with the National Aeronautics and Space
Administration.
NR 18
TC 12
Z9 12
U1 0
U2 18
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0003-6951
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD MAR 25
PY 2013
VL 102
IS 12
AR 121109
DI 10.1063/1.4798551
PG 4
WC Physics, Applied
SC Physics
GA 117QB
UT WOS:000316967100009
ER
PT J
AU Dietz, A
Fotopoulos, N
Singer, L
Cutler, C
AF Dietz, Alexander
Fotopoulos, Nickolas
Singer, Leo
Cutler, Curt
TI Outlook for detection of GW inspirals by GRB-triggered searches in the
advanced detector era
SO PHYSICAL REVIEW D
LA English
DT Article
ID GAMMA-RAY BURSTS; GRAVITATIONAL-WAVES; LIGO OBSERVATIONS; COMPACT
BINARIES; SCIENCE RUN; JET BREAKS; TELESCOPE; AFTERGLOW; DURATION;
ORIGIN
AB Short, hard gamma-ray bursts (GRBs) are believed to originate from the coalescence of two neutron stars (NSs) or a NS and a black hole (BH). If this scenario is correct, then short GRBs will be accompanied by the emission of strong gravitational waves (GWs), detectable by GW observatories such as LIGO, Virgo, KAGRA, and LIGO-India. As compared with blind, all-sky, all-time GW searches, externally triggered searches for GW counterparts to short GRBs have the advantages of both significantly reduced detection threshold due to known time and sky location and enhanced GW amplitude because of face-on orientation. Based on the distribution of signal-to-noise ratios in candidate compact binary coalescence events in the most recent joint LIGO-Virgo data, our analytic estimates, and our Monte Carlo simulations, we find an effective sensitive volume for GRB-triggered searches that is approximate to 2 times greater than for an all-sky, all-time search. For NS-NS systems, a jet angle theta(j) = 20 degrees, a gamma-ray satellite field of view of 10% of the sky, and priors with generally precessing spin, this doubles the number of NS-NS short-GRB and NS-BH short-GRB associations, to similar to 3-4% of all detections of NS-NSs and NS-BHs. We also investigate the power of tests for statistical excesses in lists of subthreshold events, and show that these are unlikely to reveal a subthreshold population until finding GW associations to short GRBs is already routine. Finally, we provide useful formulas for calculating the prior distribution of GW amplitudes from a compact binary coalescence, for a given GW detector network and given sky location. DOI: 10.1103/PhysRevD.87.064033
C1 [Dietz, Alexander] Univ Mississippi, Dept Phys & Astron, University, MS 38677 USA.
[Fotopoulos, Nickolas; Singer, Leo] CALTECH, LIGO Lab, Pasadena, CA 91125 USA.
[Cutler, Curt] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Dietz, A (reprint author), Univ Mississippi, Dept Phys & Astron, University, MS 38677 USA.
FU National Science Foundation (NSF) [PHY-0107417]; NSF; NSF [PHY-1067985,
PHY-0757937, PHY1068881]; National Aeronautics and Space Administration
FX The authors thank Alan Weinstein and Michal Was for comments on the
manuscript, and Neil Gehrels for updating us on GRB missions. LIGO was
constructed by the California Institute of Technology and Massachusetts
Institute of Technology with funding from the National Science
Foundation (NSF) and operates under cooperative agreement No.
PHY-0107417. L. S. is supported by the NSF through a Graduate Research
Fellowship, while A. D. is supported by NSF Grants No. PHY-1067985 and
No. PHY-0757937. C. C.'s work was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under contract to the
National Aeronautics and Space Administration. C. C. also gratefully
acknowledges support from NSF Grant No. PHY1068881. This paper has LIGO
Document No. LIGO-P1200113- v7.
NR 55
TC 9
Z9 9
U1 0
U2 7
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
J9 PHYS REV D
JI Phys. Rev. D
PD MAR 22
PY 2013
VL 87
IS 6
AR 064033
DI 10.1103/PhysRevD.87.064033
PG 13
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 113NZ
UT WOS:000316676000006
ER
PT J
AU Marley, MS
AF Marley, Mark S.
TI Probing an Extrasolar Planet
SO SCIENCE
LA English
DT Editorial Material
ID ORBITING HR 8799; MU-M; ATMOSPHERE; SPECTRUM; ABSORPTION; JUPITER;
CARBON; MASSES; WATER
C1 NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
RP Marley, MS (reprint author), NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
EM mark.s.marley@nasa.gov
RI Marley, Mark/I-4704-2013;
OI Marley, Mark/0000-0002-5251-2943
NR 15
TC 2
Z9 2
U1 0
U2 5
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD MAR 22
PY 2013
VL 339
IS 6126
BP 1393
EP 1394
DI 10.1126/science.1235078
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 114KU
UT WOS:000316740700030
PM 23520101
ER
PT J
AU Maphutha, S
Moothi, K
Meyyappan, M
Iyuke, SE
AF Maphutha, Selby
Moothi, Kapil
Meyyappan, M.
Iyuke, Sunny E.
TI A carbon nanotube-infused polysulfone membrane with polyvinyl alcohol
layer for treating oil-containing waste water
SO SCIENTIFIC REPORTS
LA English
DT Article
ID POLY(VINYL ALCOHOL); MECHANICAL-PROPERTIES; POLYMER COMPOSITES;
CROSS-LINKING; ULTRAFILTRATION; MICROFILTRATION; NANOFILTRATION;
PERFORMANCE; EMULSION; REINFORCEMENT
AB A carbon nanotube (CNT) integrated polymer composite membrane with a polyvinyl alcohol barrier layer has been prepared to separate oil from water for treatment of oil-containing waste water. The CNTs were synthesised using chemical vapour deposition, and a phase inversion method was employed for the blending of the CNTs in the polymer composite solution for casting of the membrane. Relative to the baseline polymer, an increase of 119% in the tensile strength, 77% in the Young's modulus and 258% in the toughness is seen for a concentration of 7.5% CNTs in the polymer composite. The permeate through the membrane shows oil concentrations below the acceptable 10 mg/L limit with an excellent throughput and oil rejection of over 95%.
C1 [Maphutha, Selby; Moothi, Kapil; Iyuke, Sunny E.] Univ Witwatersrand, Sch Chem & Met Engn, ZA-2050 Wits, South Africa.
[Maphutha, Selby; Moothi, Kapil; Iyuke, Sunny E.] DST NRF Ctr Excellence Strong Mat, ZA-2050 Wits 2050, South Africa.
[Meyyappan, M.] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA.
[Meyyappan, M.] POSTECH, Div IT Convergence Engn, Pohang, South Korea.
RP Iyuke, SE (reprint author), Univ Witwatersrand, Sch Chem & Met Engn, P Bag 3, ZA-2050 Wits, South Africa.
EM Sunny.Iyuke@wits.ac.za
OI Moothi, Kapil/0000-0001-7755-5125; Maphutha, Selby/0000-0003-3105-9016
FU National Research Foundation (NRF) under South Africa Focus Area; NRF
Nanotechnology flagship programme; Department of Science and Technology
(DST)/NRF Centre of Excellence; World Class University program through
the National Research Foundation of Korea; Ministry of Education,
Science and Technology [R31-10100]
FX The authors acknowledge the financial support from the National Research
Foundation (NRF) under South Africa Focus Area, NRF Nanotechnology
flagship programme, Department of Science and Technology (DST)/NRF
Centre of Excellence. The student bursaries provided by the University
of the Witwatersrand are acknowledged. The work in Korea was supported
by the World Class University program through the National Research
Foundation of Korea funded by the Ministry of Education, Science and
Technology under Project R31-10100.
NR 40
TC 24
Z9 25
U1 6
U2 74
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2045-2322
J9 SCI REP-UK
JI Sci Rep
PD MAR 22
PY 2013
VL 3
AR 1509
DI 10.1038/srep01509
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 111TO
UT WOS:000316543800001
PM 23518875
ER
PT J
AU Vieira, JD
Marrone, DP
Chapman, SC
De Breuck, C
Hezaveh, YD
Weiss, A
Aguirre, JE
Aird, KA
Aravena, M
Ashby, MLN
Bayliss, M
Benson, BA
Biggs, AD
Bleem, LE
Bock, JJ
Bothwell, M
Bradford, CM
Brodwin, M
Carlstrom, JE
Chang, CL
Crawford, TM
Crites, AT
de Haan, T
Dobbs, MA
Fomalont, EB
Fassnacht, CD
George, EM
Gladders, MD
Gonzalez, AH
Greve, TR
Gullberg, B
Halverson, NW
High, FW
Holder, GP
Holzapfel, WL
Hoover, S
Hrubes, JD
Hunter, TR
Keisler, R
Lee, AT
Leitch, EM
Lueker, M
Luong-Van, D
Malkan, M
McIntyre, V
McMahon, JJ
Mehl, J
Menten, KM
Meyer, SS
Mocanu, LM
Murphy, EJ
Natoli, T
Padin, S
Plagge, T
Reichardt, CL
Rest, A
Ruel, J
Ruhl, JE
Sharon, K
Schaffer, KK
Shaw, L
Shirokoff, E
Spilker, JS
Stalder, B
Staniszewski, Z
Stark, AA
Story, K
Vanderlinde, K
Welikala, N
Williamson, R
AF Vieira, J. D.
Marrone, D. P.
Chapman, S. C.
De Breuck, C.
Hezaveh, Y. D.
Weiss, A.
Aguirre, J. E.
Aird, K. A.
Aravena, M.
Ashby, M. L. N.
Bayliss, M.
Benson, B. A.
Biggs, A. D.
Bleem, L. E.
Bock, J. J.
Bothwell, M.
Bradford, C. M.
Brodwin, M.
Carlstrom, J. E.
Chang, C. L.
Crawford, T. M.
Crites, A. T.
de Haan, T.
Dobbs, M. A.
Fomalont, E. B.
Fassnacht, C. D.
George, E. M.
Gladders, M. D.
Gonzalez, A. H.
Greve, T. R.
Gullberg, B.
Halverson, N. W.
High, F. W.
Holder, G. P.
Holzapfel, W. L.
Hoover, S.
Hrubes, J. D.
Hunter, T. R.
Keisler, R.
Lee, A. T.
Leitch, E. M.
Lueker, M.
Luong-Van, D.
Malkan, M.
McIntyre, V.
McMahon, J. J.
Mehl, J.
Menten, K. M.
Meyer, S. S.
Mocanu, L. M.
Murphy, E. J.
Natoli, T.
Padin, S.
Plagge, T.
Reichardt, C. L.
Rest, A.
Ruel, J.
Ruhl, J. E.
Sharon, K.
Schaffer, K. K.
Shaw, L.
Shirokoff, E.
Spilker, J. S.
Stalder, B.
Staniszewski, Z.
Stark, A. A.
Story, K.
Vanderlinde, K.
Welikala, N.
Williamson, R.
TI Dusty starburst galaxies in the early Universe as revealed by
gravitational lensing
SO NATURE
LA English
DT Article
ID SOUTH-POLE TELESCOPE; SUBMILLIMETER GALAXY; MOLECULAR GAS; DEEP-FIELD;
REDSHIFT; COUNTS; MODEL
AB In the past decade, our understanding of galaxy evolution has been revolutionized by the discovery that luminous, dusty starburst galaxies were 1,000 times more abundant in the early Universe than at present(1,2). It has, however, been difficult to measure the complete redshift distribution of these objects, especially at the highest redshifts (z>4). Here we report a redshift survey at a wavelength of three millimetres, targeting carbon monoxide line emission from the star-forming molecular gas in the direction of extraordinarily bright millimetre-wave-selected sources. High-resolution imaging demonstrates that these sources are strongly gravitationally lensed by foreground galaxies. We detect spectral lines in 23 out of 26 sources and multiple lines in 12 of those 23 sources, from which we obtain robust, unambiguous redshifts. At least 10 of the sources are found to lie at z > 4, indicating that the fraction of dusty starburst galaxies at high redshifts is greater than previously thought. Models of lens geometries in the sample indicate that the background objects are ultra-luminous infrared galaxies, powered by extreme bursts of star formation.
C1 [Vieira, J. D.; Bock, J. J.; Lueker, M.; Padin, S.; Shirokoff, E.; Staniszewski, Z.] CALTECH, Pasadena, CA 91125 USA.
[Marrone, D. P.; Bothwell, M.; Spilker, J. S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Chapman, S. C.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada.
[Chapman, S. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[De Breuck, C.; Aravena, M.; Biggs, A. D.; Gullberg, B.] European So Observ, D-85748 Garching, Germany.
[Hezaveh, Y. D.; de Haan, T.; Dobbs, M. A.; Holder, G. P.; Shaw, L.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Weiss, A.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Aguirre, J. E.] Univ Penn, Philadelphia, PA 19104 USA.
[Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA.
[Ashby, M. L. N.; Stalder, B.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bayliss, M.; Ruel, J.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Hoover, S.; Keisler, R.; Leitch, E. M.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Mocanu, L. M.; Natoli, T.; Padin, S.; Plagge, T.; Sharon, K.; Schaffer, K. K.; Story, K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Hoover, S.; McMahon, J. J.; Meyer, S. S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Natoli, T.; Story, K.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Bock, J. J.; Bradford, C. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA.
[Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Mocanu, L. M.; Padin, S.; Plagge, T.; Sharon, K.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Fomalont, E. B.; Hunter, T. R.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Fassnacht, C. D.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[George, E. M.; Holzapfel, W. L.; Lee, A. T.; Reichardt, C. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Greve, T. R.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Lee, A. T.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Dept Phys, Berkeley, CA 94720 USA.
[Malkan, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[McIntyre, V.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Murphy, E. J.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Ruhl, J. E.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA.
[Sharon, K.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA.
[Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Welikala, N.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Welikala, N.] CNRS, F-91405 Orsay, France.
RP Vieira, JD (reprint author), CALTECH, 1200 East Calif Blvd, Pasadena, CA 91125 USA.
EM vieira@caltech.edu
RI Holzapfel, William/I-4836-2015; Williamson, Ross/H-1734-2015;
OI Williamson, Ross/0000-0002-6945-2975; Marrone,
Daniel/0000-0002-2367-1080; Aird, Kenneth/0000-0003-1441-9518;
Reichardt, Christian/0000-0003-2226-9169; De Breuck,
Carlos/0000-0002-6637-3315; Hunter, Todd/0000-0001-6492-0090; Stark,
Antony/0000-0002-2718-9996
FU National Science Foundation; Kavli Foundation; Gordon and Betty Moore
Foundation; NASA from the Space Telescope Science Institute; NSERC; CRC;
ClfAR
FX The SPT is supported by the National Science Foundation, the Kavli
Foundation and the Gordon and Betty Moore Foundation. 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 Chile. The Joint ALMA Observatory is operated by ESO,
AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a
facility of the NSF operated under cooperative agreement by Associated
Universities, Inc. Partial support for this work was provided by NASA
from the Space Telescope Science Institute. This work is based in part
on observations made with Herschel, a European Space Agency Cornerstone
Mission with significant participation by NASA. Work at McGill
University is supported by NSERC, the CRC programme and ClfAR.
NR 27
TC 109
Z9 109
U1 1
U2 16
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 MAR 21
PY 2013
VL 495
IS 7441
BP 344
EP 347
DI 10.1038/nature12001
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 113EY
UT WOS:000316650500037
PM 23485967
ER
PT J
AU Nowicki, SF
Hunter, SD
Parsons, AM
AF Nowicki, Suzanne F.
Hunter, Stanley D.
Parsons, Ann M.
TI Development of a quasi-monoenergetic 6 MeV Gamma Facility at NASA
Goddard Space Flight Center
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS
SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT
LA English
DT Article
DE 6.129 MeV; Monoenergetic; Facility; Characterization; Calibration;
Gamma-ray; Neutron; Pulsed neutron generator
ID NEUTRON
AB The 6 MeV Gamma Facility has been developed at NASA Goddard Space Flight Center (GSFC) to allow in-house characterization and testing of a wide range of gamma-ray instruments such as pixelated CdZnTe detectors for planetary science and Compton and pair-production imaging telescopes for astrophysics. The 6 MeV Gamma Facility utilizes a circulating flow of water irradiated by 14 MeV neutrons to produce gamma rays via neutron capture on oxygen (O-16(n,p)N-16 -> O-16*-> O-16+gamma) The facility provides a low cost, in-house source of 2.742, 6.129 and 7.117 MeV gamma rays, near the lower energy range of most accelerators and well above the 2.614 MeV line from the Th-228 decay chain, the highest energy gamma ray available from a natural radionuclide. The 7.13 s half-life of the N-16 decay allows the water to be irradiated on one side of a large granite block and pumped to the opposite side to decay. Separating the irradiation and decay regions allows for shielding material, the granite block, to be placed between them, thus reducing the low-energy gamma-ray continuum. Comparison between high purity germanium (HPGe) spectra from the facility and a manufactured source, Pu-238/C-13, shows that the low-energy continuum from the facility is reduced by a factor similar to 30 and the gamma-ray rate is similar to 100 times higher at 6.129 MeV. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Nowicki, Suzanne F.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Nowicki, Suzanne F.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Nowicki, Suzanne F.; Hunter, Stanley D.; Parsons, Ann M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Nowicki, SF (reprint author), NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd,Bldg 34,Room W271, Greenbelt, MD 20771 USA.
EM suzanne.f.nowicki@nasa.gov
FU NASA GSFC Internal Research and Development (IRAD); NASA GSFC
neutron/gamma-ray group
FX This work was supported by NASA GSFC Internal Research and Development
(IRAD). The authors would like to thank Bert Nahory for assembling the
facility, Julia Bodnarik and Robert Forsythe for their help during
operations, and Jeffrey Schweitzer and the NASA GSFC neutron/gamma-ray
group for their support throughout this work.
NR 13
TC 2
Z9 2
U1 0
U2 7
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-9002
J9 NUCL INSTRUM METH A
JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc.
Equip.
PD MAR 21
PY 2013
VL 705
BP 111
EP 116
DI 10.1016/j.nima.2012.12.066
PG 6
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Nuclear; Physics, Particles & Fields
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 088HX
UT WOS:000314826000016
ER
PT J
AU Edelson, R
Mushotzky, R
Vaughan, S
Scargle, J
Gandhi, P
Malkan, M
Baumgartner, W
AF Edelson, R.
Mushotzky, R.
Vaughan, S.
Scargle, J.
Gandhi, P.
Malkan, M.
Baumgartner, W.
TI KEPLER OBSERVATIONS OF RAPID OPTICAL VARIABILITY IN THE BL LACERTAE
OBJECT W2R1926+42
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE BL Lacertae objects: general; BL Lacertae objects: individual
(W2R1926+42); galaxies: active
ID X-RAY BINARIES; ACTIVE GALACTIC NUCLEI; BLACK-HOLE; GALAXIES; JET;
NOISE; CONNECTION; CATALOG; BLAZARS; LONG
AB We present the first Kepler monitoring of a strongly variable BL Lac, W2R1926+42. The light curve covers 181 days with similar to 0.2% errors, 30 minute sampling and >90% duty cycle, showing numerous delta I/I>25% flares over timescales as short as a day. The flux distribution is highly skewed and non-Gaussian. The variability shows a strong rms-flux correlation with the clearest evidence to date for nonlinearity in this relation. We introduce a method to measure periodograms from the discrete autocorrelation function, an approach that may be well-suited to a wide range of Kepler data. The periodogram is not consistent with a simple power-law, but shows a flattening at frequencies below 7 x 10(-5) Hz. Simple models of the power spectrum, such as a broken power law, do not produce acceptable fits, indicating that the Kepler blazar light curve requires more sophisticated mathematical and physical descriptions than currently in use.
C1 [Edelson, R.; Mushotzky, R.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Mushotzky, R.; Baumgartner, W.] NASA, High Energy Astrophys Lab, GSFC, Greenbelt, MD 20771 USA.
[Vaughan, S.] Univ Leicester, Dept Phys & Astron, Xray & Observat Astron Grp, Leicester LE1 7RH, Leics, England.
[Scargle, J.] NASA, Astrobiol & Space Sci Div, Ames Res Ctr, Stanford, CA 94305 USA.
[Gandhi, P.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Malkan, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
RP Edelson, R (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM redelson@astro.umd.edu
FU Kepler GO program through NASA [NNX11AC81G, NNX12AC93G, NNX13AC26G];
NASA Applied Information Systems Research Program
FX The authors appreciate the helpful assistance of the Kepler GO office in
scheduling and understanding these observations, as well as the editor
and anonymous referee for a timely and useful review. This research
utilized data from the HEASARC, IRSA, NED, and MAST data archives, and
the NASA Astrophysics Data System Bibliographic Service. R.E. and R.M.
acknowledge support by the Kepler GO program through NASA grants
NNX11AC81G, NNX12AC93G, and NNX13AC26G. J.S. acknowledges Joe Bredekamp
and the NASA Applied Information Systems Research Program for support.
NR 38
TC 20
Z9 20
U1 2
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2013
VL 766
IS 1
AR 16
DI 10.1088/0004-637X/766/1/16
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 105GH
UT WOS:000316054000016
ER
PT J
AU Gezari, S
Martin, DC
Forster, K
Neill, JD
Huber, M
Heckman, T
Bianchi, L
Morrissey, P
Neff, SG
Seibert, M
Schiminovich, D
Wyder, TK
Burgett, WS
Chambers, KC
Kaiser, N
Magnier, EA
Price, PA
Tonry, JL
AF Gezari, S.
Martin, D. C.
Forster, K.
Neill, J. D.
Huber, M.
Heckman, T.
Bianchi, L.
Morrissey, P.
Neff, S. G.
Seibert, M.
Schiminovich, D.
Wyder, T. K.
Burgett, W. S.
Chambers, K. C.
Kaiser, N.
Magnier, E. A.
Price, P. A.
Tonry, J. L.
TI THE GALEX TIME DOMAIN SURVEY. I. SELECTION AND CLASSIFICATION OF OVER A
THOUSAND ULTRAVIOLET VARIABLE SOURCES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE surveys; ultraviolet: general
ID DIGITAL SKY SURVEY; DEEP FIELD-SOUTH; POINT-SOURCE CATALOG; SURVEY
STRIPE 82; SHOCK BREAKOUT; LIGHT CURVES; TIDAL DISRUPTION; COSMOS FIELD;
OPTICAL VARIABILITY; RED SUPERGIANT
AB We present the selection and classification of over a thousand ultraviolet (UV) variable sources discovered in similar to 40 deg(2) of GALEX Time Domain Survey (TDS) NUV images observed with a cadence of 2 days and a baseline of observations of similar to 3 years. The GALEX TDS fields were designed to be in spatial and temporal coordination with the Pan-STARRS1 Medium Deep Survey, which provides deep optical imaging and simultaneous optical transient detections via image differencing. We characterize the GALEX photometric errors empirically as a function of mean magnitude, and select sources that vary at the 5 sigma level in at least one epoch. We measure the statistical properties of the UV variability, including the structure function on timescales of days and years. We report classifications for the GALEX TDS sample using a combination of optical host colors and morphology, UV light curve characteristics, and matches to archival X-ray, and spectroscopy catalogs. We classify 62% of the sources as active galaxies (358 quasars and 305 active galactic nuclei), and 10% as variable stars (including 37 RR Lyrae, 53 M dwarf flare stars, and 2 cataclysmic variables). We detect a large-amplitude tail in the UV variability distribution for M-dwarf flare stars and RR Lyrae, reaching up to vertical bar Delta m vertical bar = 4.6 mag and 2.9 mag, respectively. The mean amplitude of the structure function for quasars on year timescales is five times larger than observed at optical wavelengths. The remaining unclassified sources include UV-bright extragalactic transients, two of which have been spectroscopically confirmed to be a young core-collapse supernova and a flare from the tidal disruption of a star by dormant supermassive black hole. We calculate a surface density for variable sources in the UV with NUV < 23 mag and vertical bar Delta m vertical bar > 0.2 mag of similar to 8.0, 7.7, and 1.8 deg(-2) for quasars, active galactic nuclei, and RR Lyrae stars, respectively. We also calculate a surface density rate in the UV for transient sources, using the effective survey time at the cadence appropriate to each class, of similar to 15 and 52 deg(-2) yr(-1) for M dwarfs and extragalactic transients, respectively.
C1 [Gezari, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Martin, D. C.; Forster, K.; Neill, J. D.; Morrissey, P.; Wyder, T. K.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Huber, M.; Burgett, W. S.; Chambers, K. C.; Kaiser, N.; Magnier, E. A.; Tonry, J. L.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Heckman, T.; Bianchi, L.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Neff, S. G.] NASA, Lab Astron & Solar Phys, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Seibert, M.] Observ Carnegie Inst Washington, Pasadena, CA 90095 USA.
[Schiminovich, D.] Columbia Univ, Dept Astron, New York, NY 10027 USA.
[Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
RP Gezari, S (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM suvi@astro.umd.edu
OI Chambers, Kenneth /0000-0001-6965-7789
FU National Aeronautics and Space Administration through the Planetary
Science Division of the NASA Science Mission Directorate [NNX08AR22G]
FX We thank the anonymous referee for their constructive comments which
improved the paper. GALEX (Galaxy Evolution Explorer) is a NASA Small
Explorer, launched in 2003 April. We gratefully acknowledge NASA's
support for construction, operation, and science analysis for the GALEX
mission, developed in cooperation with the Centre National d'Etudes
Spatiales of France and the Korean Ministry of Science and Technology.
The Pan-STARRS1 survey has been made possible through contributions of
the Institute for Astronomy, the University of Hawaii, the Pan-STARRS
Project Office, the Max Planck Society and its participating institutes,
the Max Planck Institute for Astronomy, Heidelberg and the Max Planck
Institute for Extraterrestrial Physics, Garching, The Johns Hopkins
University, Durham University, the University of Edinburgh, Queen's
University Belfast, the Harvard-Smithsonian Center for Astro-physics,
and the Las Cumbres Observatory Global Telescope Network, Incorporated,
the National Central University of Taiwan, and the National Aeronautics
and Space Administration under grant No. NNX08AR22G issued through the
Planetary Science Division of the NASA Science Mission Directorate.
NR 76
TC 22
Z9 22
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2013
VL 766
IS 1
AR 60
DI 10.1088/0004-637X/766/1/60
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 105GH
UT WOS:000316054000060
ER
PT J
AU Giacintucci, S
Kale, R
Wik, DR
Venturi, T
Markevitch, M
AF Giacintucci, Simona
Kale, Ruta
Wik, Daniel R.
Venturi, Tiziana
Markevitch, Maxim
TI DISCOVERY OF A GIANT RADIO HALO IN A NEW PLANCK GALAXY CLUSTER
PLCKG171.9-40.7
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: general; galaxies: clusters: individual
(PLCKG171.9-40.7); intergalactic medium; radio continuum: general;
X-rays: galaxies: clusters
ID X-RAY LUMINOSITY; VLA SKY SURVEY; DEEP 1.4 GHZ; XMM-NEWTON;
SUNYAEV-ZELDOVICH; COSMIC-RAYS; PARTICLE-ACCELERATION; RELIC CANDIDATES;
HADRONIC MODELS; SHOCK-WAVES
AB We report the discovery of a giant radio halo in a new, hot, X-ray luminous galaxy cluster recently found by Planck, PLCKG171.9-40.7. The radio halo was found using Giant Metrewave Radio Telescope observations at 235 MHz and 610 MHz, and in the 1.4 GHz data from an NRAO Very Large Array Sky Survey pointing that we have reanalyzed. The diffuse radio emission is coincident with the cluster X-ray emission, and has an extent of similar to 1 Mpc and a radio power of similar to 5 x 10(24) W Hz(-1) at 1.4 GHz. Its integrated radio spectrum has a slope of alpha approximate to 1.8 between 235 MHz and 1.4 GHz, steeper than that of a typical giant halo. The analysis of the archival XMM-Newton X-ray data shows that the cluster is hot (similar to 10 keV) and disturbed, consistent with X-ray-selected clusters hosting radio halos. This is the first giant radio halo discovered in one of the new clusters found by Planck.
C1 [Giacintucci, Simona] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Giacintucci, Simona] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA.
[Kale, Ruta; Venturi, Tiziana] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Kale, Ruta] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy.
[Wik, Daniel R.; Markevitch, Maxim] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Giacintucci, S (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM simona@astro.umd.edu
OI Venturi, Tiziana/0000-0002-8476-6307
FU NASA [PF0-110071]; Chandra X-ray Center (CXC)
FX We are deeply grateful to Rossella Cassano for useful comments and
suggestions, and for providing Figure 6. We thank Kaustuv Basu for
kindly providing Figure 7. We thank the staff of the GMRT for help
during the observations. GMRT is run by the National Centre for Radio
Astrophysics of the Tata Institute of Fundamental Research. The National
Radio Astronomy Observatory is a facility of the National Science
Foundation operated under cooperative agreement by Associated
Universities, Inc. S.G. acknowledges the support of NASA through
Einstein Postdoctoral Fellowship PF0-110071 awarded by the Chandra X-ray
Center (CXC), which is operated by SAO. This research was supported by
an appointment to the NASA Postdoctoral Program at the Goddard Space
Flight Center, administered by Oak Ridge Associated Universities through
a contract with NASA.
NR 62
TC 10
Z9 10
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2013
VL 766
IS 1
AR 18
DI 10.1088/0004-637X/766/1/18
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 105GH
UT WOS:000316054000018
ER
PT J
AU Gilliland, RL
Marcy, GW
Rowe, JF
Rogers, L
Torres, G
Fressin, F
Lopez, ED
Buchhave, LA
Christensen-Dalsgaard, J
Desert, JM
Henze, CE
Isaacson, H
Jenkins, J
Lissauer, JJ
Chaplin, WJ
Basu, S
Metcalfe, TS
Elsworth, Y
Handberg, R
Hekker, S
Huber, D
Karoff, C
Kjeldsen, H
Lund, MN
Lundkvist, M
Miglio, A
Charbonneau, D
Ford, EB
Fortney, JJ
Haas, MR
Howard, AW
Howell, SB
Ragozzine, D
Thompson, SE
AF Gilliland, Ronald L.
Marcy, Geoffrey W.
Rowe, Jason F.
Rogers, Leslie
Torres, Guillermo
Fressin, Francois
Lopez, Eric D.
Buchhave, Lars A.
Christensen-Dalsgaard, Jorgen
Desert, Jean-Michel
Henze, Christopher E.
Isaacson, Howard
Jenkins, Jonm.
Lissauer, Jack J.
Chaplin, William J.
Basu, Sarbani
Metcalfe, Travis S.
Elsworth, Yvonne
Handberg, Rasmus
Hekker, Saskia
Huber, Daniel
Karoff, Christoffer
Kjeldsen, Hans
Lund, Mikkel N.
Lundkvist, Mia
Miglio, Andrea
Charbonneau, David
Ford, Eric B.
Fortney, Jonathan J.
Haas, Michael R.
Howard, Andrew W.
Howell, Steve B.
Ragozzine, Darin
Thompson, Susan E.
TI KEPLER-68: THREE PLANETS, ONE WITH A DENSITY BETWEEN THAT OF EARTH AND
ICE GIANTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: fundamental parameters; stars: individual
(Kepler-68, KIC 11295426, 2MASS J19240775+4902249)
ID SOLAR-TYPE STARS; TESTING BLEND SCENARIOS; SPITZER-SPACE-TELESCOPE;
EXOPLANET HD 189733B; FINE GUIDANCE SENSOR; SUN-LIKE STAR; TRANSITING
PLANET; INITIAL CHARACTERISTICS; EXTRASOLAR PLANETS; ASTEROSEISMIC DATA
AB NASA's Kepler Mission has revealed two transiting planets orbiting Kepler-68. Follow-up Doppler measurements have established the mass of the innermost planet and revealed a third Jovian-mass planet orbiting beyond the two transiting planets. Kepler-68b, in a 5.4 day orbit, has M-P = 8.3(-2.4)(+2.2) M-circle plus, R-P = 2.31(-0.09)(+0.06) R-circle plus, and rho(P) = 3.32(-0.98)(+0.86) g cm(-3), giving Kepler-68b a density intermediate between that of the ice giants and Earth. Kepler-68c is Earth-sized, with a radius R-P = 0.953(-0.042)(+0.037) R-circle plus and transits on a 9.6 day orbit; validation of Kepler-68c posed unique challenges. Kepler-68d has an orbital period of 580 +/- 15 days and a minimum mass of M-P sin i = 0.947 +/- 0.035M(J). Power spectra of the Kepler photometry at one minute cadence exhibit a rich and strong set of asteroseismic pulsation modes enabling detailed analysis of the stellar interior. Spectroscopy of the star coupled with asteroseismic modeling of the multiple pulsation modes yield precise measurements of stellar properties, notably T-eff = 5793 +/- 74 K, M-star = 1.079 +/- 0.051 M-circle dot, R-star = 1.243 +/- 0.019 R-circle dot, and rho(star) = 0.7903 +/- 0.0054 g cm(-3), all measured with fractional uncertainties of only a few percent. Models of Kepler-68b suggest that it is likely composed of rock and water, or has a H and He envelope to yield its density similar to 3 g cm(-3).
C1 [Gilliland, Ronald L.] Penn State Univ, Dept Astron, University Pk, PA 16802 USA.
[Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Marcy, Geoffrey W.; Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Rowe, Jason F.; Henze, Christopher E.; Lissauer, Jack J.; Huber, Daniel; Haas, Michael R.; Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rogers, Leslie] CALTECH, Pasadena, CA 91125 USA.
[Torres, Guillermo; Fressin, Francois; Desert, Jean-Michel; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lopez, Eric D.; Fortney, Jonathan J.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA.
[Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Christensen-Dalsgaard, Jorgen; Handberg, Rasmus; Karoff, Christoffer; Kjeldsen, Hans; Lund, Mikkel N.; Lundkvist, Mia] Stellar Astrophys Ctr, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Christensen-Dalsgaard, Jorgen] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Jenkins, Jonm.; Thompson, Susan E.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Chaplin, William J.; Elsworth, Yvonne; Miglio, Andrea] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Metcalfe, Travis S.] White Dwarf Res Corp, Boulder, CO 80301 USA.
[Hekker, Saskia] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Ford, Eric B.; Ragozzine, Darin] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
RP Gilliland, RL (reprint author), Penn State Univ, Dept Astron, 525 Davey Lab, University Pk, PA 16802 USA.
EM gillil@stsci.edu
RI Howard, Andrew/D-4148-2015;
OI Howard, Andrew/0000-0001-8638-0320; Charbonneau,
David/0000-0002-9003-484X; Fortney, Jonathan/0000-0002-9843-4354;
Buchhave, Lars A./0000-0003-1605-5666; Metcalfe,
Travis/0000-0003-4034-0416; Karoff, Christoffer/0000-0003-2009-7965;
Basu, Sarbani/0000-0002-6163-3472; /0000-0001-6545-639X; Lund, Mikkel
Norup/0000-0001-9214-5642; Lundkvist, Mia Sloth/0000-0002-8661-2571;
Handberg, Rasmus/0000-0001-8725-4502
FU NASA's Science Mission Directorate; W.M. Keck Foundation; NASA,
JPL/Caltech; Space Telescope Science Institute [HF-51313.01-A]; NASA
[NAS 5-26555, NNX12AC75G, AST-1105930, NNX09AG09A]; Danish National
Research Foundation; ASTERISK project (ASTERoseismic Investigations with
SONG and Kepler); European Research Council [267864]; NSF [AST-1105930]
FX Funding for this tenth Discovery mission is provided by NASA's Science
Mission Directorate. The many people contributing to the development of
this mission are gratefully acknowledged. We thank Elizabeth Adams, Eric
Agol, Natalie Batalha, William Borucki, Stephen Bryson, William Cochran,
Andrea Dupree, Debra Fischer, and David Monet for discussion and
contributions. The anonymous referee made comments serving to improve
the paper. Some of the data used here were obtained at the W.M. Keck
Observatory, which is operated as a scientific partnership among the
California Institute of Technology, the University of California, and
NASA. The W.M. Keck Foundation provided generous financial support to
the Keck Observatory. This work is also based in part on observations
made with the Spitzer Space Telescope, which is operated by the Jet
Propulsion Laboratory, California Institute of Technology under a
contract with NASA. Partial support for this work was provided by NASA
through an award issued by JPL/Caltech. Support for L.A.R. was provided
through Hubble Fellowship grant No. HF-51313.01-A awarded by the Space
Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., for NASA under contract
NAS 5-26555. G.T. acknowledges partial support for this work from NASA
grant NNX12AC75G (Kepler Participating Scientist Program). Funding for
the Stellar Astrophysics Centre is provided by The Danish National
Research Foundation. The research is supported by the ASTERISK project
(ASTERoseismic Investigations with SONG and Kepler) funded by the
European Research Council (grant agreement No. 267864). Asteroseismic
analysis was supported in part by White Dwarf Research Corporation
through the Pale Blue Dot project (http://whitedwarf.org/palebluedot).
S.B. acknowledges support from NSF grant AST-1105930. R.L.G. has been
partially supported by NASA co-operative agreement NNX09AG09A.
NR 107
TC 58
Z9 58
U1 0
U2 18
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2013
VL 766
IS 1
AR 40
DI 10.1088/0004-637X/766/1/40
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 105GH
UT WOS:000316054000040
ER
PT J
AU Hermes, JJ
Montgomery, MH
Mullally, F
Winget, DE
Bischoff-Kim, A
AF Hermes, J. J.
Montgomery, M. H.
Mullally, Fergal
Winget, D. E.
Bischoff-Kim, A.
TI A NEW TIMESCALE FOR PERIOD CHANGE IN THE PULSATING DA WHITE DWARF WD
0111+0018
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: individual (WD0111+0018); stars: oscillations (including
pulsations); stars: variables: general; white dwarfs
ID CETI INSTABILITY STRIP; WHOLE EARTH TELESCOPE; DIGITAL SKY SURVEY;
ZZ-CETI; EMPIRICAL DETERMINATION; STARS; ASTEROSEISMOLOGY; G117-B15A;
EVOLUTIONARY; CONVECTION
AB We report the most rapid rate of period change measured to date for a pulsating DA (hydrogen atmosphere) white dwarf (WD), observed in the 292.9 s mode of WD0111+0018. The observed period change, faster than 10(-12) s s(-1), exceeds by more than two orders of magnitude the expected rate from cooling alone for this class of slow and simply evolving pulsating WDs. This result indicates the presence of an additional timescale for period evolution in these pulsating objects. We also measure the rates of period change of nonlinear combination frequencies and show that they share the evolutionary characteristics of their parent modes, confirming that these combination frequencies are not independent modes but rather artifacts of some nonlinear distortion in the outer layers of the star.
C1 [Hermes, J. J.; Montgomery, M. H.; Winget, D. E.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Hermes, J. J.; Montgomery, M. H.; Winget, D. E.] McDonald Observ, Ft Davis, TX 79734 USA.
[Mullally, Fergal] SETI Inst, Mountain View, CA 94043 USA.
[Mullally, Fergal] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Bischoff-Kim, A.] Georgia Coll & State Univ, Chem Phys & Astron Dept, Milledgeville, GA 31061 USA.
RP Hermes, JJ (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA.
EM jjhermes@astro.as.utexas.edu
FU Norman Hackerman Advanced Research Program [003658-0255-2007,
003658-0252-2009]; NASA Origins Program [NAG5-13094]; National Science
Foundation [AST-0909107]
FX We are especially grateful to all those whose time in West Texas made
this result possible: S. E. Thompson, C. M. Yeates, K. I. Winget, Davis
Winget, R. E. Nather, Elizabeth J. Jeffery, Ross E. Falcon, and G. F.
Miller. We thank E. L. Robinson, Anjum S. Mukadam, Denis Sullivan, and
Ross E. Falcon for helpful discussions, and acknowledge the McDonald
Observatory staff for tireless support, especially Dave Doss and John
Kuehne. This work is supported by the Norman Hackerman Advanced Research
Program, under grants 003658-0255-2007 and 003658-0252-2009, by a grant
from the NASA Origins Program, NAG5-13094, and by the National Science
Foundation, under grant AST-0909107.
NR 50
TC 5
Z9 5
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2013
VL 766
IS 1
AR 42
DI 10.1088/0004-637X/766/1/42
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 105GH
UT WOS:000316054000042
ER
PT J
AU Houde, M
Fletcher, A
Beck, R
Hildebrand, RH
Vaillancourt, JE
Stil, JM
AF Houde, Martin
Fletcher, Andrew
Beck, Rainer
Hildebrand, Roger H.
Vaillancourt, John E.
Stil, Jeroen M.
TI CHARACTERIZING MAGNETIZED TURBULENCE IN M51
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (M51); galaxies: ISM; galaxies: magnetic fields;
galaxies: spiral
ID COMPRESSIBLE MAGNETOHYDRODYNAMIC TURBULENCE; FIELDS; POLARIZATION;
DISPERSION; ANISOTROPY; GALAXY
AB We use previously published high-resolution synchrotron polarization data to perform an angular dispersion analysis with the aim of characterizing magnetized turbulence in M51. We first analyze three distinct regions (the center of the galaxy, and the northwest and southwest spiral arms) and can clearly discern the turbulent correlation length scale from the width of the magnetized turbulent correlation function for two regions and detect the imprint of anisotropy in the turbulence for all three. Furthermore, analyzing the galaxy as a whole allows us to determine a two-dimensional Gaussian model for the magnetized turbulence in M51. We measure the turbulent correlation scales parallel and perpendicular to the local mean magnetic field to be, respectively, delta(parallel to) = 98 +/- 5 pc and delta(perpendicular to) = 54 +/- 3 pc, while the turbulent-to-ordered magnetic field strength ratio is found to be B-t/B-0 = 1.01 +/- 0.04. These results are consistent with those of Fletcher et al., who performed a Faraday rotation dispersion analysis of the same data, and our detection of anisotropy is consistent with current magnetized turbulence theories.
C1 [Houde, Martin] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Houde, Martin] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
[Fletcher, Andrew] Newcastle Univ, Sch Math & Stat, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England.
[Beck, Rainer] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Hildebrand, Roger H.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Hildebrand, Roger H.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Hildebrand, Roger H.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Vaillancourt, John E.] NASA, Ames Res Ctr, Stratospher Observ Infrared Astron, Univ Space Res Assoc, Moffett Field, CA 94035 USA.
[Stil, Jeroen M.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada.
RP Houde, M