FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Edwards, JR
Boles, JA
Baurle, RA
AF Edwards, Jack R.
Boles, John A.
Baurle, Robert A.
TI Large-eddy/Reynolds-averaged Navier-Stokes simulation of a supersonic
reacting wall jet
SO COMBUSTION AND FLAME
LA English
DT Article
DE Supersonic combustion; Large-eddy simulation
ID LARGE-EDDY SIMULATION; COMBUSTION; MODELS; FLOWS; FORMULATION
AB This work presents results from large-eddy/Reynolds-averaged Navier-Stokes (LES/RANS) simulations of the well-known Burrows-Kurkov supersonic reacting wall-jet experiment. Generally good agreement with experimental mole fraction, stagnation temperature, and Pitot pressure profiles is obtained for non-reactive mixing of the hydrogen jet with a non-vitiated air stream. A lifted flame, stabilized between 15 and 20 cm downstream of the hydrogen jet, is formed for hydrogen injected into a vitiated air stream. Flame stabilization occurs closer to the hydrogen injection location when a three-dimensional combustor geometry (with boundary layer development resolved on all walls) is considered. Volumetric expansion of the reactive shear layer is accompanied by the formation of large eddies which interact strongly with the reaction zone. Time averaged predictions of the reaction zone structure show an under-prediction of the peak water concentration and stagnation temperature, relative to experimental data, but display generally good agreement with the extent of the reaction zone. Reactive scalar scatter plots indicate that the flame exhibits a transition from a partially-premixed flame structure, characterized by intermittent heat release, to a diffusion-flame structure that could probably be described by a strained laminar flamelet model. (C) 2011 Published by Elsevier Inc. on behalf of The Combustion Institute.
C1 [Edwards, Jack R.] N Carolina State Univ, Dept Mech & Aerosp Engn, Raleigh, NC 27695 USA.
[Boles, John A.] Taitech Inc, Wright Patterson AFB, OH 45433 USA.
[Baurle, Robert A.] NASA Langley Res Ctr, Hyperson Air Breathing Prop Branch, Hampton, VA 23681 USA.
RP Edwards, JR (reprint author), N Carolina State Univ, Dept Mech & Aerosp Engn, Campus Box 7910, Raleigh, NC 27695 USA.
EM jredward@ncsu.edu
FU NASA [NNX07AC27A-S01]; National Center for Hypersonic Combined-Cycle
Propulsion; AFOSR
FX This work is supported by NASA under Cooperative Agreement
NNX07AC27A-S01 and by the National Center for Hypersonic Combined-Cycle
Propulsion, funded jointly by AFOSR and NASA. Computer resources have
been provided by the NASA Advanced Supercomputing (NAS) division.
NR 45
TC 6
Z9 8
U1 0
U2 24
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0010-2180
J9 COMBUST FLAME
JI Combust. Flame
PD MAR
PY 2012
VL 159
IS 3
BP 1127
EP 1138
DI 10.1016/j.combustflame.2011.10.009
PG 12
WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary;
Engineering, Chemical; Engineering, Mechanical
SC Thermodynamics; Energy & Fuels; Engineering
GA 886LH
UT WOS:000299855400019
ER
PT J
AU Keeton, KE
Schmidt, LL
Slack, KJ
Malka, AA
AF Keeton, Kathryn E.
Schmidt, Lacey L.
Slack, Kelley J.
Malka, Ari A.
TI The Rocket Science of Teams
SO INDUSTRIAL AND ORGANIZATIONAL PSYCHOLOGY-PERSPECTIVES ON SCIENCE AND
PRACTICE
LA English
DT Editorial Material
C1 [Keeton, Kathryn E.] NASA, Lyndon B Johnson Space Ctr, BHP Program Element, EASI, Houston, TX 77058 USA.
[Slack, Kelley J.] NASA, Lyndon B Johnson Space Ctr, LZ Technol, Houston, TX 77058 USA.
[Malka, Ari A.] Univ Houston, Houston, TX 77004 USA.
RP Keeton, KE (reprint author), NASA, Lyndon B Johnson Space Ctr, BHP Program Element, EASI, 1290 Hercules, Houston, TX 77058 USA.
EM kathryn.keeton@nasa.gov
NR 1
TC 1
Z9 1
U1 0
U2 0
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1754-9426
J9 IND ORGAN PSYCHOL-US
JI Ind. Organ. Psychol.
PD MAR
PY 2012
VL 5
IS 1
BP 32
EP 35
DI 10.1111/j.1754-9434.2011.01399.x
PG 4
WC Psychology, Applied
SC Psychology
GA 886CT
UT WOS:000299829700005
ER
PT J
AU Draper, SL
Isheim, D
AF Draper, S. L.
Isheim, D.
TI Environmental embrittlement of a third generation gamma TiAl alloy
SO INTERMETALLICS
LA English
DT Article
DE Titanium aluminides; based on TiAl; Environmental embrittlement;
Diffusion; Surface properties; Microprobe; Atom probe
ID TEMPERATURE EXPOSURE; THERMAL EXPOSURE; MET PX; BEHAVIOR
AB Exposure of a Ti-45Al-5Nb alloy to elevated temperatures has been shown to result in a loss of ductility resulting from a near surface effect involving diffusion of oxygen into the alloy. Local electrode atom probe analysis was conducted at 2, 13, and 25 gm distance from the oxide/base-metal interface. Oxygen was preferentially located in the alpha(2) phase with concentrations up to 14.8 at.% and diminishing with increasing distance from the surface. Near surface microstructural changes were only visible up to 10 mu m from the surface but the oxygen diffusion significantly exceeded that distance. The diffusion coefficient of oxygen into the alpha(2) phase was estimated based on the oxygen concentrations obtained from local electrode atom probe analysis. Fluorine ion implantation on the surface was investigated as a possible solution to the embrittlement. Published by Elsevier Ltd.
C1 [Draper, S. L.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Isheim, D.] Northwestern Univ, Dept Mat Sci & Engn, Evanston, IL 60208 USA.
[Isheim, D.] Northwestern Univ, Ctr Atom Probe Tomog NUCAPT, Evanston, IL 60208 USA.
RP Draper, SL (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,MS 49-1, Cleveland, OH 44135 USA.
EM Susan.L.Draper@nasa.gov; isheim@northwestern.edu
FU NSF-MRI [DMR-0420532]; ONR-DURIP [N00014-0400798, N00014-0610539,
N00014-0910781]
FX The authors are grateful to David Hull, NASA Glenn Research Center, for
the electron microprobe analysis and A. Donchev,
Karl-Winnacker-Institut, of the DECHEMA e.V., for the F ion
implantation. The Atom-probe tomographic measurements were performed at
the Northwestern University Center for Atom-Probe Tomography (NUCAPT).
The LEAP tomograph was purchased and upgraded with funding from NSF-MRI
(DMR-0420532) and ONR-DURIP (N00014-0400798, N00014-0610539,
N00014-0910781) grants. The authors are thankful to Stephan Gerstl at
Imago Scientific Instruments for LEAP analysis of bulk alloy.
NR 15
TC 9
Z9 9
U1 0
U2 10
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0966-9795
J9 INTERMETALLICS
JI Intermetallics
PD MAR
PY 2012
VL 22
BP 77
EP 83
DI 10.1016/j.intermet.2011.10.006
PG 7
WC Chemistry, Physical; Materials Science, Multidisciplinary; Metallurgy &
Metallurgical Engineering
SC Chemistry; Materials Science; Metallurgy & Metallurgical Engineering
GA 888DD
UT WOS:000299983100012
ER
PT J
AU Gonzalez, P
Tucker, CJ
Sy, H
AF Gonzalez, P.
Tucker, C. J.
Sy, H.
TI Tree density and species decline in the African Sahel attributable to
climate
SO JOURNAL OF ARID ENVIRONMENTS
LA English
DT Article
DE Climate change; Climate variability; Desertification; Tree cover;
Vegetation shifts
ID WEST-AFRICA; WOODY VEGETATION; BURKINA-FASO; NDVI DATA; DROUGHT;
DESERTIFICATION; DYNAMICS; MORTALITY; PATTERNS; DATABASE
AB Increased aridity and human population have reduced tree cover in parts of the African Sahel and degraded resources for local people. Yet, tree cover trends and the relative importance of climate and population remain unresolved. From field measurements, aerial photos, and Ikonos satellite images, we detected significant 1954-2002 tree density declines in the western Sahel of 18 +/- 14% (P = 0.014, n = 204) and 17 +/- 13% (P = 0.0009, n = 187). From field observations, we detected a significant 1960 2000 species richness decline of 21 +/- 11% (P = 0.0028, n = 14) across the Sahel and a southward shift of the Sahel, Sudan, and Guinea zones. Multivariate analyses of climate, soil, and population showed that temperature most significantly (P < 0.001) explained tree cover changes. Multivariate and bivariate tests and field observations indicated the dominance of temperature and precipitation, supporting attribution of tree cover changes to climate variability. Climate change forcing of Sahel climate variability, particularly the significant (P < 0.05) 1901-2002 temperature increases and precipitation decreases in the research areas, connects Sahel tree cover changes to global climate change. This suggests roles for global action and local adaptation to address ecological change in the Sahel. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Gonzalez, P.] Univ Calif Berkeley, Ctr Forestry, Berkeley, CA 94720 USA.
[Tucker, C. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sy, H.] Famine Early Warning Syst Network, Nouakchott, Mauritania.
RP Gonzalez, P (reprint author), Univ Calif Berkeley, Ctr Forestry, 163 Mulford, Berkeley, CA 94720 USA.
EM pgonzalez@cal.berkeley.edu
RI Gonzalez, Patrick/B-9479-2013
OI Gonzalez, Patrick/0000-0002-7105-0561
FU NASA; U.S. Geological Survey
FX We gratefully acknowledge field work assistance by Alkhalil Adoum,
Elaine Carlson, Issa Khalil, Joseph Sedgo, and Salif Sow, comments from
Paul R. Ehrlich, support from Christine A. Rose, allocation of Ikonos
images from the NASA Scientific Data Purchase, research funding from
NASA and the U.S. Geological Survey, and assistance from the residents
of Akar, Aten, Banizumbi, Buurtey Ganuun, Dan Tsuntsu, Fabugu, Fete Ole,
Guidimouni, Juude Waalo, Kardofal, Kaylaroom, Marchuut, Nampabuum,
Ningelin, Njoobeen Mbataar, Tamaka, and Wolum.
NR 50
TC 50
Z9 52
U1 2
U2 42
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0140-1963
EI 1095-922X
J9 J ARID ENVIRON
JI J. Arid. Environ.
PD MAR
PY 2012
VL 78
BP 55
EP 64
DI 10.1016/j.jaridenv.2011.11.001
PG 10
WC Ecology; Environmental Sciences
SC Environmental Sciences & Ecology
GA 889LA
UT WOS:000300074000007
ER
PT J
AU Alonso-Perez, S
Cuevas, E
Querol, X
Guerra, JC
Perez, C
AF Alonso-Perez, S.
Cuevas, E.
Querol, X.
Guerra, J. C.
Perez, C.
TI African dust source regions for observed dust outbreaks over the
Subtropical Eastern North Atlantic region, above 25 degrees N
SO JOURNAL OF ARID ENVIRONMENTS
LA English
DT Article
DE Aerosols; African dust; Marine Boundary Layer; Dust sources; Residence
time; HYSPLIT
ID LONG-RANGE TRANSPORT; SOUTHEASTERN UNITED-STATES; SAHARAN DUST;
CANARY-ISLANDS; MINERAL-DUST; AIR-QUALITY; ELEMENTAL COMPOSITION;
CHEMICAL-COMPOSITION; SURFACE OBSERVATIONS; SUSPENDED PARTICLES
AB High mineral dust-laden air mass potential source regions affecting the Marine Boundary Layer (MBL) of the Subtropical Eastern North Atlantic Region above 25 degrees N (SENAR), directly or by means of gravitational settlement, were objectively identified. We introduced a new hybrid Lagrangian-Eulerian receptor model, in which air mass residence time probability maps in the geographical domain latitude = [5 degrees N, 60 degrees N], longitude = [70 degrees W, 30 degrees E] were combined with TOMS-AI data (TAPI Index), and with simulated Total Suspended Particles (TSP) with the BSC/DREAM model (SDPI Index). Both approaches show a good agreement. For dust gravitational settlement episodes within the MBL, the dust sources are located in southernmost latitudes compared to those associated with lower air mass transport. A seasonal variability in potential dust sources is found with both approaches, TAPI and SDPI. In winter, most dust sources are located within the Sahara in an area bounded by latitude = [18 degrees N, 35 degrees N], longitude = [15 degrees W, 15 degrees E]. In summer, a high dust-laden air mass reservoir above the Atlantic Ocean has been found during episodes for low altitudes, and dust source regions in the Sahara have been identified for middle and upper altitudes. The Bodele depression was found to have a minor impact on dust outbreaks affecting the SENAR. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Alonso-Perez, S.; Cuevas, E.] Izana Atmospher Res Ctr AEMET, Santa Cruz De Tenerife 38071, Spain.
[Alonso-Perez, S.; Querol, X.] Inst Environm Assessment & Water Res CSIC, Barcelona 08028, Spain.
[Guerra, J. C.] Univ La Laguna, Atmospher Phys Lab, Tenerife 38200, Spain.
[Perez, C.] Columbia Univ, Earth Inst, NASA Goddard Inst Space Studies, New York, NY 10025 USA.
[Perez, C.] Int Res Inst Climate & Soc, New York, NY 10025 USA.
RP Alonso-Perez, S (reprint author), Izana Atmospher Res Ctr AEMET, C La Marina 20,6 Planta, Santa Cruz De Tenerife 38071, Spain.
EM salonsop@aemet.es
RI Querol, Xavier/E-2800-2014; Alonso Perez, Silvia/M-1035-2014; Cuevas,
Emilio/L-2109-2013
OI Querol, Xavier/0000-0002-6549-9899; Alonso Perez,
Silvia/0000-0003-0572-6081; Cuevas, Emilio/0000-0003-1843-8302
FU G.D. of Environmental Quality and Assessment from the Spanish Ministry
of Environment, Rural and Marine Affairs
FX This study was supported by the G.D. of Environmental Quality and
Assessment from the Spanish Ministry of Environment, Rural and Marine
Affairs.
NR 86
TC 13
Z9 13
U1 0
U2 15
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0140-1963
J9 J ARID ENVIRON
JI J. Arid. Environ.
PD MAR
PY 2012
VL 78
BP 100
EP 109
DI 10.1016/j.jaridenv.2011.11.013
PG 10
WC Ecology; Environmental Sciences
SC Environmental Sciences & Ecology
GA 889LA
UT WOS:000300074000011
ER
PT J
AU Jain, A
AF Jain, Abhinandan
TI Multibody graph transformations and analysis
SO NONLINEAR DYNAMICS
LA English
DT Article
DE Multibody systems; Graph theory; Algorithms
ID QUASI-VELOCITIES; DYNAMICS; FORMULATION; SYSTEMS; EQUATIONS; DESIGN
AB This two-part paper uses graph transformation methods to develop methods for partitioning, aggregating, and constraint embedding for multibody systems. This first part focuses on tree-topology systems and reviews the key notion of spatial kernel operator (SKO) models for such systems. It develops systematic and rigorous techniques for partitioning SKO models in terms of the SKO models of the component subsystems based on the path-induced property of the component subgraphs. It shows that the sparsity structure of key matrix operators and the mass matrix for the multibody system can be described using partitioning transformations. Subsequently, the notions of node contractions and subgraph aggregation and their role in coarsening graphs are discussed. It is shown that the tree property of a graph is preserved after subgraph aggregation if and only if the subgraph satisfies an aggregation condition. These graph theory ideas are used to develop SKO models for the aggregated tree multibody systems.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Jain, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Abhi.Jain@jpl.nasa.gov
FU National Aeronautics and Space Administration; National Institute of
Health [RO1GM082896-01A2]
FX The research described in this paper was performed at the Jet Propulsion
Laboratory (JPL), California Institute of Technology, under contract
with the National Aeronautics and Space Administration.7 This
project was also supported in part by Grant Number RO1GM082896-01A2 from
the National Institute of Health.
NR 30
TC 4
Z9 4
U1 0
U2 4
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0924-090X
J9 NONLINEAR DYNAM
JI Nonlinear Dyn.
PD MAR
PY 2012
VL 67
IS 4
BP 2779
EP 2797
DI 10.1007/s11071-011-0188-y
PG 19
WC Engineering, Mechanical; Mechanics
SC Engineering; Mechanics
GA 891AC
UT WOS:000300187500037
ER
PT J
AU Adamovsky, G
Lyuksyutov, SF
Mackey, JR
Floyd, BM
Abeywickrema, U
Fedin, I
Rackaitis, M
AF Adamovsky, Grigory
Lyuksyutov, Sergei F.
Mackey, Jeffrey R.
Floyd, Bertram M.
Abeywickrema, Ujitha
Fedin, Igor
Rackaitis, Mindaugas
TI Peculiarities of thermo-optic coefficient under different temperature
regimes in optical fibers containing fiber Bragg gratings
SO OPTICS COMMUNICATIONS
LA English
DT Article
DE Optical materials; Optical fibers; Bragg gratings; Thermodynamic
properties; High temperature tests
ID THERMAL-STABILITY; SENSOR
AB Direct experimental measurements of the thermo-optic for fixed temperature intervals (20-200 degrees C, 200-500 degrees C C, 500-660 degrees C, 660-780 degrees C) in fused silica fiber containing fiber Bragg gratings (FBGs) were conducted. The diffraction efficiency of a FBG fluctuated with temperature between 2.01 x 10(-4) and 0.17 x 10(-4) while the temperature shift of the Bragg's peak was monitored between 1300 and 1311 nm with sub-Angstrom precision. Numerical simulations were focused on FBG's diffraction efficiency calculations accounting for the temperature drift of the gratings, and found to be in excellent agreement with obtained experimental data.
It was found that the first-order thermo-optic coefficient changes between 1.29 and 1.85 x 10(-5) K-1 for the linear fit and at T=0 degrees C its value was found to be close to 2.37 x 10(-5) K-1 for the polynomial fit of experimental data. The average thermo-optic coefficient undergoes a minimum in the vicinity of 440 degrees C. Additional observation indicates a negative sign of the second-order thermo-optic coefficient. The value of thermal expansion coefficient was much less (0.5 x 10(-6) K-1) than that for the average thermo-optic coefficient. Based on the energy dispersive spectroscopy it was determined that thermal erasing of the FBGs at a temperature around 780 degrees C corresponds to germanium monoxide diffusion out of core in silica-based fibers. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Lyuksyutov, Sergei F.; Abeywickrema, Ujitha; Fedin, Igor] Univ Akron, Dept Phys, Akron, OH 44325 USA.
[Rackaitis, Mindaugas] Bridgestone Amer, Ctr Res & Technol, Akron, OH 44317 USA.
[Floyd, Bertram M.] Sierra Lobo Inc, Cleveland, OH 44135 USA.
[Mackey, Jeffrey R.] ASRC Aerosp Corp, Cleveland, OH 44135 USA.
[Adamovsky, Grigory] NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Lyuksyutov, SF (reprint author), Univ Akron, Dept Phys, Akron, OH 44325 USA.
EM sfl@uakron.edu
FU NASA
FX The authors acknowledge support from the Hypersonic Project of the NASA
Fundamental Aeronautics Program. One of the co-authors, SFL, a NASA
Glenn Research Center 2010 Summer Fellow, also appreciates the support
of the NASA Summer Faculty Program.
NR 16
TC 11
Z9 12
U1 3
U2 18
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0030-4018
J9 OPT COMMUN
JI Opt. Commun.
PD MAR 1
PY 2012
VL 285
IS 5
BP 766
EP 773
DI 10.1016/j.optcom.2011.10.084
PG 8
WC Optics
SC Optics
GA 891EO
UT WOS:000300200200048
ER
PT J
AU Roberts, S
Zachrisson, C
Kozachkov, H
Ullah, A
Shapiro, AA
Johnson, WL
Hofmann, DC
AF Roberts, Scott
Zachrisson, Carl
Kozachkov, Henry
Ullah, Adam
Shapiro, Andrew A.
Johnson, William L.
Hofmann, Douglas C.
TI Cryogenic Charpy impact testing of metallic glass matrix composites
SO SCRIPTA MATERIALIA
LA English
DT Article
DE Bulk metallic glass matrix composites; Charpy; Cryogenic; Toughness
ID DUCTILITY; TEMPERATURES; PLASTICITY; TENSILE
AB Compact Charpy impact testing was employed to investigate the effect of low temperatures on the impact toughness of bulk metallic glass matrix composites (BMGMCs). Samples were fabricated via suction casting and impacted from room temperature down to liquid nitrogen temperature. Unlike monolithic glasses, BMGMCs do exhibit a steep decrease in toughness as the temperature is reduced from the ambient, caused by embrittlement in the ductile reinforcing phase. However, at cryogenic temperatures, BMGMCs have a toughness equivalent to their glassy matrix. (C) 2011 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved.
C1 [Shapiro, Andrew A.; Hofmann, Douglas C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Roberts, Scott; Zachrisson, Carl; Kozachkov, Henry; Ullah, Adam; Shapiro, Andrew A.; Johnson, William L.; Hofmann, Douglas C.] CALTECH, Pasadena, CA 91126 USA.
RP Hofmann, DC (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM dch@jpl.nasa.gov
FU Exploration Systems Mission Directorate (ESMD) Advanced Capabilities
Division at the National Aeronautics and Space Administration (NASA)
[NNH10ZTT001N]; NASA
FX This work was supported by the Exploration Systems Mission Directorate
(ESMD) Advanced Capabilities Division at the National Aeronautics and
Space Administration (NASA) under contract number NNH10ZTT001N. C.F.Z.
acknowledges financial support from AAAS Entry Point's ACCESS, a program
sponsored by NASA. Part of this research was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
NR 18
TC 8
Z9 9
U1 1
U2 44
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 MAR
PY 2012
VL 66
IS 5
BP 284
EP 287
DI 10.1016/j.scriptamat.2011.11.011
PG 4
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Metallurgy & Metallurgical Engineering
SC Science & Technology - Other Topics; Materials Science; Metallurgy &
Metallurgical Engineering
GA 890EZ
UT WOS:000300129200022
ER
PT J
AU Durden, SL
AF Durden, Stephen L.
TI Trends in Intense Typhoon Minimum Sea Level Pressure
SO ATMOSPHERE
LA English
DT Article
DE typhoon; tropical cyclone; intensity; climate change
ID QUANTILE REGRESSION; TROPICAL CYCLONES; ENSO; PACIFIC
AB A number of recent publications have examined trends in the maximum wind speed of tropical cyclones in various basins. In this communication, the author focuses on typhoons in the western North Pacific. Rather than maximum wind speed, the intensity of the storms is measured by their lifetime minimum sea level pressure (MSLP). Quantile regression is used to test for trends in storms of extreme intensity. The results indicate that there is a trend of decreasing intensity in the most intense storms as measured by MSLP over the period 1951-2010. However, when the data are broken into intervals 1951-1987 and 1987-2010, neither interval has a significant trend, but the intensity quantiles for the two periods differ. Reasons for this are discussed, including the cessation of aircraft reconnaissance in 1987. The author also finds that the average typhoon intensity is greater in El Nino years, while the intensity of the strongest typhoons shows no significant relation to El Nino Southern Oscillation.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Durden, SL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM sdurden@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX 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.
NR 22
TC 1
Z9 1
U1 0
U2 1
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 2073-4433
J9 ATMOSPHERE-BASEL
JI Atmosphere
PD MAR
PY 2012
VL 3
IS 1
BP 124
EP 131
DI 10.3390/atmos3010124
PG 8
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 175QS
UT WOS:000321247100006
ER
PT J
AU Fleischer, I
Klingelhofer, G
Morris, RV
Schroder, C
Rodionov, D
de Souza, PA
AF Fleischer, Iris
Klingelhoefer, Goestar
Morris, Richard V.
Schroeder, Christian
Rodionov, Daniel
de Souza, Paulo A.
CA MIMOS II Team
TI In-situ Mossbauer spectroscopy with MIMOS II
SO HYPERFINE INTERACTIONS
LA English
DT Proceedings Paper
CT 65th Yamada Conference / 31st International Conference on the
Applications of the Mossbauer Effect (ICAME)
CY SEP 25-30, 2011
CL Kobe, JAPAN
DE Miniaturized Mossbauer spectrometer; MIMOS II; Mars Exploration Rover
mission; In-situ Mossbauer spectroscopy; Non-destructive analysis
ID GUSEV CRATER; MERIDIANI-PLANUM; SPIRIT ROVER; HEMATITE SPHERULES; BURNS
FORMATION; HOME PLATE; MARS; SPECTROMETER; EXPLORATION; DIAGENESIS
AB The miniaturized Mossbauer spectrometer MIMOS II was developed for the exploration of planetary surfaces. Two MIMOS II instruments were successfully deployed on the martian surface as payload elements of the NASA Mars Exploration Rover (MER) mission and have returned data since landing in January 2004. Mossbauer spectroscopy has made significant contributions to the success of the MER mission, in particular identification of iron-bearing minerals formed through aqueous weathering processes. As a field-portable instrument and with backscattering geometry, MIMOS II provides an opportunity for non-destructive in-situ investigations for a range of applications. For example, the instrument has been used for analyses of archaeological artifacts, for air pollution studies and for in-field monitoring of green rust formation. AMER-type MIMOS II instrument is part of the payload of the Russian Phobos-Grunt mission, scheduled for launch in November 2011, with the aim of exploring the composition of the martian moon Phobos. An advanced version of the instrument, MIMOS IIA, that incorporates capability for elemental analyses, is currently under development.
C1 [Fleischer, Iris; Klingelhoefer, Goestar; Rodionov, Daniel] Johannes Gutenberg Univ Mainz, Inst Inorgan & Analyt Chem, D-55122 Mainz, Germany.
[Morris, Richard V.] NASA, Johnson Space Ctr, Houston, TX USA.
[Schroeder, Christian] Univ Bayreuth, Tubingen, Germany.
[Schroeder, Christian] Univ Tubingen, Tubingen, Germany.
[Rodionov, Daniel] Space Res Inst IKI, Moscow, Russia.
[de Souza, Paulo A.] Tasmanian ICT Ctr, Hobart, Tas, Australia.
RP Fleischer, I (reprint author), Johannes Gutenberg Univ Mainz, Inst Inorgan & Analyt Chem, D-55122 Mainz, Germany.
EM fleischi@uni-mainz.de
RI de Souza, Paulo/B-8961-2008; Schroder, Christian/B-3870-2009
OI de Souza, Paulo/0000-0002-0091-8925; Schroder,
Christian/0000-0002-7935-6039
NR 46
TC 1
Z9 1
U1 2
U2 6
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0304-3843
J9 HYPERFINE INTERACT
JI Hyperfine Interact.
PD MAR
PY 2012
VL 207
IS 1-3
BP 97
EP 105
DI 10.1007/s10751-011-0437-y
PG 9
WC Physics, Atomic, Molecular & Chemical; Physics, Condensed Matter;
Physics, Nuclear
SC Physics
GA 070JM
UT WOS:000313502400018
ER
PT J
AU Siegel, PH
AF Siegel, Peter H.
TI Untitled
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Editorial Material
C1 [Siegel, Peter H.] CALTECH, Pasadena, CA 91125 USA.
[Siegel, Peter H.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Siegel, PH (reprint author), CALTECH, Pasadena, CA 91125 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD MAR
PY 2012
VL 2
IS 2
BP 157
EP 160
DI 10.1109/TTHZ.2012.2186714
PG 4
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 142AA
UT WOS:000318766700001
ER
PT J
AU Siegel, PH
AF Siegel, Peter H.
TI Terahertz Pioneers A Series of Interviews With Significant Contributors
to Terahertz Science and Technology
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Editorial Material
C1 [Siegel, Peter H.] CALTECH, Dept Biol, Pasadena, CA 91109 USA.
[Siegel, Peter H.] CALTECH, Dept Elect Engn, Pasadena, CA 91109 USA.
[Siegel, Peter H.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Siegel, PH (reprint author), CALTECH, Dept Biol, Pasadena, CA 91109 USA.
NR 0
TC 3
Z9 3
U1 0
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD MAR
PY 2012
VL 2
IS 2
BP 161
EP 161
DI 10.1109/TTHZ.2011.2182389
PG 1
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 142AA
UT WOS:000318766700002
ER
PT J
AU Siegel, PH
AF Siegel, Peter H.
TI Terahertz Pioneer: Robert W. Wilson
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Biographical-Item
C1 [Siegel, Peter H.] CALTECH, Dept Biol, Pasadena, CA 91109 USA.
[Siegel, Peter H.] CALTECH, Dept Elect Engn, Pasadena, CA 91109 USA.
[Siegel, Peter H.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Siegel, PH (reprint author), CALTECH, Dept Biol, Pasadena, CA 91109 USA.
EM phs@caltech.edu
NR 1
TC 1
Z9 1
U1 0
U2 0
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD MAR
PY 2012
VL 2
IS 2
BP 162
EP 166
DI 10.1109/TTHZ.2011.2182390
PG 5
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 142AA
UT WOS:000318766700003
ER
PT J
AU Maestrini, A
Mehdi, I
Siles, JV
Ward, JS
Lin, R
Thomas, B
Lee, C
Gill, J
Chattopadhyay, G
Schlecht, E
Pearson, J
Siegel, P
AF Maestrini, Alain
Mehdi, Imran
Siles, Jose V.
Ward, John S.
Lin, Robert
Thomas, Bertrand
Lee, Choonsup
Gill, John
Chattopadhyay, Goutam
Schlecht, Erich
Pearson, John
Siegel, Peter
TI Design and Characterization of a Room Temperature All-Solid-State
Electronic Source Tunable From 2.48 to 2.75 THz
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Broadband terahertz (THz) source; frequency multiplier; frequency
tripler; local oscillator; planar diode; power-combining; Schottky
diode; THz; varactor
ID SCHOTTKY DIODES; FREQUENCY; POWER; BAND
AB We report on the design, fabrication and test of an all-solid-state, frequency agile source that produces over 1 mu W (-30 dBm) across the 2.48-2.75 THz band at room temperature. This frequency-multiplied source is driven by a W-band synthesizer followed by a power amplifier that delivers 350-450 mW (25.5-26.5 dBm) and a cascade of three balanced frequency triplers. The first stage tripler is based on four power-combined six-anode GaAs Schottky diode devices, and the second stage tripler is based on two four-anode GaAs devices. The output tripler uses a single unbiased device featuring two anodes monolithically integrated onto a thin GaAs membrane. The source delivers a record 18 mu W (-17.5 dBm) at 2.58 THz at room temperature. This frequency multiplied source is analyzed with a Fourier transform spectrometer (FTS) and the unwanted harmonics are found to be at least 29 dB below the desired signal. This source, when used as the local oscillator for a hot-electron bolometer mixer, will enable heterodyne instruments for future space missions to map the cosmologically-important 2.675 THz HD molecular line.
C1 [Maestrini, Alain] Univ Paris 06, Paris, France.
[Maestrini, Alain] LERMA, Observatoire Paris, Paris, France.
[Mehdi, Imran; Siles, Jose V.; Ward, John S.; Lin, Robert; Thomas, Bertrand; Lee, Choonsup; Gill, John; Chattopadhyay, Goutam; Schlecht, Erich; Pearson, John; Siegel, Peter] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Maestrini, A (reprint author), Univ Paris 06, Paris, France.
EM alain.maestrini@obspm.fr; Imran.mehdi@jpl.nasa.gov; goutam@jpl.nasa.gov
FU National Aeronautics and Space Administration under a contract, at the
Universite Pierre et Marie Curie-Paris 6; National Aeronautics and Space
Administration at the Observatoire de Paris, France; NASA Astrophysics
Research and Analysis Program (APRA), Universite Pierre et Marie Curie;
Centre National d'Etudes Spatiales
FX This work was supported by National Aeronautics and Space Administration
under a contract, at the Universite Pierre et Marie Curie-Paris 6, and
at the Observatoire de Paris, France. Funding from NASA Astrophysics
Research and Analysis Program (APRA), Universite Pierre et Marie Curie
and Centre National d'Etudes Spatiales.
NR 33
TC 29
Z9 29
U1 1
U2 11
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD MAR
PY 2012
VL 2
IS 2
BP 177
EP 185
DI 10.1109/TTHZ.2012.2183740
PG 9
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 142AA
UT WOS:000318766700005
ER
PT J
AU Fung, A
Samoska, L
Pukala, D
Dawson, D
Kangaslahti, P
Varonen, M
Gaier, T
Lawrence, C
Boll, G
Lai, R
Mei, XB
AF Fung, Andy
Samoska, Lorene
Pukala, David
Dawson, Douglas
Kangaslahti, Pekka
Varonen, Mikko
Gaier, Todd
Lawrence, Charles
Boll, Greg
Lai, Richard
Mei, X. B.
TI On-Wafer S-Parameter Measurements in the 325-508 GHz Band
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Article
DE Millimeter wave; monolithic microwave integrated circuits (MMIC);
on-wafer; S-parameters; submillimeter wave; terahertz (THz)
ID NETWORK ANALYZER MEASUREMENTS; TECHNOLOGY; CIRCUITS; THZ
AB We report on two-port on-wafer vector network analyzer measurements in the 325-508 GHz frequency band. Measurements are made with prototype GGB Industries Inc. WR2.2 (325-500 GHz) coplanar waveguide probes and OML Inc. WR2.2 frequency extenders. New probe performance data and characteristics of probe tip calibration using a Thru-Reflect-Line procedure are discussed. Probe S-parameter measurements indicate insertion loss per probe of 5.0 to 9.1 dB in the WR2.2 band. Calibrated dynamic range of about 30 dB or better for insertion and return loss measurement across the band is achieved. These new results for the prototype WR2.2 probes, the calibration procedure, observed errors, and results of on-wafer amplifier measurements are presented.
C1 [Fung, Andy; Samoska, Lorene; Pukala, David; Dawson, Douglas; Kangaslahti, Pekka; Varonen, Mikko; Gaier, Todd; Lawrence, Charles] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Boll, Greg] GGB Ind Inc, Naples, FL 34101 USA.
[Lai, Richard; Mei, X. B.] Northrop Grumman Corp, Redondo Beach, CA 90278 USA.
RP Fung, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM andy.fung@jpl.nasa.gov
FU NASA ESTO Advanced Component Technologies program [ACT-05]; NASA
Innovative Partners Program [IPP-06]; National Aeronautics and Space
Administration
FX This work was supported in part by the NASA ESTO Advanced Component
Technologies ACT-05 program and by the NASA Innovative Partners Program
IPP-06. This work was carried out in part at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration.
NR 26
TC 9
Z9 9
U1 2
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD MAR
PY 2012
VL 2
IS 2
BP 186
EP 192
DI 10.1109/TTHZ.2011.2182369
PG 7
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 142AA
UT WOS:000318766700006
ER
PT J
AU Bar-Cohen, Y
AF Bar-Cohen, Yoseph
TI 5 Nature as a Model for Mimicking and Inspiration of New Technologies
SO INTERNATIONAL JOURNAL OF AERONAUTICAL AND SPACE SCIENCES
LA English
DT Review
DE Biologically inspired technologies; biomimetics; robotics; actuators;
sensors; humanlike robots
AB Over 3.8 billion years, through evolution nature came up with many effective continually improving solutions to its challenges. Humans have always been inspired by nature capabilities in problems solving and innovation. These efforts have been intensified in recent years where systematic studies are being made towards better understanding and applying more sophisticated capabilities in this field that is increasingly being titled biomimetics. The ultimate challenge to this field is the development of humanlike robots that talk, interpret speech, walk, as well as make eye-contact and facial expressions with some capabilities that are exceeding the original model from nature. This includes flight where there is no creature that is as large, can fly as high, carry so heavy weight, fly so fast, and able to operate in extreme conditions as the aircraft and other aerospace systems. However, there are many capabilities of biological systems that are not feasible to mimic using the available technology. In this paper, the state-of-the-art of some of the developed biomimetic capabilities, potentials and challenges will be reviewed.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Bar-Cohen, Y (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM yosi@jpl.nasa.gov
FU National Aeronautics and Space Administration (NASA)
FX Some of the research reported in this paper was conducted at the Jet
Propulsion Laboratory (JPL), California Institute of Technology, under a
contract with National Aeronautics and Space Administration (NASA).
NR 53
TC 9
Z9 9
U1 3
U2 10
PU KOREAN SOC AERONAUTICAL & SPACE SCIENCES
PI SEOULD
PA 635-4, YEOGSAM-DONG, KANGNAM-KU, SEOULD, 135-703, SOUTH KOREA
SN 2093-274X
EI 2093-2480
J9 INT J AERONAUT SPACE
JI Int. J. Aeronaut. Space Sci.
PD MAR
PY 2012
VL 13
IS 1
BP 1
EP 13
DI 10.5139/IJASS.2012.13.1.1
PG 13
WC Engineering, Aerospace
SC Engineering
GA V35WU
UT WOS:000209176800001
ER
PT J
AU Wu, MLC
Reale, O
Schubert, SD
Suarez, MJ
Thorncroft, CD
AF Wu, Man-Li C.
Reale, Oreste
Schubert, Siegfried D.
Suarez, Max J.
Thorncroft, Chris D.
TI African Easterly Jet: Barotropic Instability, Waves, and Cyclogenesis
SO JOURNAL OF CLIMATE
LA English
DT Article
ID 3-DIMENSIONAL STRUCTURE; TROPICAL ATLANTIC; HILBERT SPECTRUM;
WEST-AFRICA; SUMMER 1981; PART III; DYNAMICS; REANALYSIS; VIEW;
OSCILLATION
AB This study investigates the structure of the African easterly jet, focusing on instability processes on a seasonal and subseasonal scale, with the goal of identifying features that could provide increased predictability of Atlantic tropical cyclogenesis. The Modern-Era Retrospective Analysis for Research and Applications (MERRA) is used as the main investigating tool. MERRA is compared with other reanalyses datasets from major operational centers around the world and was found to describe very effectively the circulation over the African monsoon region. In particular, a comparison with precipitation datasets from the Global Precipitation Climatology Project shows that MERRA realistically reproduces seasonal precipitation over that region. The verification of the generalized Kuo barotropic instability condition computed from seasonal means is found to have the interesting property of defining well the location where observed tropical storms are detected. This property does not appear to be an artifact of MERRA and is present also in the other adopted reanalysis datasets. Therefore, the fact that the areas where the mean flow is unstable seems to provide a more favorable environment for wave intensification, could be another factor to include in addition to sea surface temperature, vertical shear, precipitation, the role of Saharan air, and others among large-scale forcings affecting development and tropical cyclone frequency. In addition, two prominent modes of variability are found based on a spectral analysis that uses the Hilbert-Huang transform: a 2.5-6-day mode that corresponds well to the African easterly waves and also a 6-9-day mode that seems to be associated with tropicalextratropical interaction.
C1 [Wu, Man-Li C.; Schubert, Siegfried D.; Suarez, Max J.] NASA, GMAO, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Reale, Oreste] NASA, Atmospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Thorncroft, Chris D.] SUNY Albany, Dept Earth & Atmospher Sci, Albany, NY 12222 USA.
[Reale, Oreste] Univ Space Res Assoc, Columbia, MD USA.
RP Wu, MLC (reprint author), NASA, GMAO, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM man-li.c.wu@nasa.gov
FU NASA Earth Science Enterprise
FX This work was supported by the NASA Earth Science Enterprise's Global
Modeling and Analysis Program. We thank the two anonymous reviewers for
their helpful comments.
NR 56
TC 8
Z9 8
U1 1
U2 8
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD MAR 1
PY 2012
VL 25
IS 5
BP 1489
EP 1510
DI 10.1175/2011JCLI4241.1
PG 22
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 905ZR
UT WOS:000301315200007
ER
PT J
AU Morik, K
Bhaduri, K
Kargupta, H
AF Morik, Katharina
Bhaduri, Kanishka
Kargupta, Hillol
TI Introduction to data mining for sustainability
SO DATA MINING AND KNOWLEDGE DISCOVERY
LA English
DT Editorial Material
ID GRASSLAND
C1 [Morik, Katharina] TU Dortmund Univ, Fac Comp Sci, Artificial Intelligence Grp, Dortmund, Germany.
[Bhaduri, Kanishka] NASA, Ames Res Ctr, Mission Crit Technol Inc, Moffett Field, CA 94035 USA.
[Kargupta, Hillol] Univ Maryland Baltimore Cty, Dept Comp Sci & Elect Engn, Baltimore, MD 21228 USA.
RP Morik, K (reprint author), TU Dortmund Univ, Fac Comp Sci, Artificial Intelligence Grp, Dortmund, Germany.
EM katharina.morik@tu-dortmund.de; Kanishka.Bhaduri-1@nasa.gov;
hillol@cs.umbc.edu
NR 35
TC 4
Z9 4
U1 7
U2 15
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1384-5810
J9 DATA MIN KNOWL DISC
JI Data Min. Knowl. Discov.
PD MAR
PY 2012
VL 24
IS 2
SI SI
BP 311
EP 324
DI 10.1007/s10618-011-0239-5
PG 14
WC Computer Science, Artificial Intelligence; Computer Science, Information
Systems
SC Computer Science
GA 875TD
UT WOS:000299057000001
ER
PT J
AU Srivastava, AN
AF Srivastava, Ashok N.
TI Greener aviation with virtual sensors: a case study
SO DATA MINING AND KNOWLEDGE DISCOVERY
LA English
DT Article
DE Ensemble learning; Gaussian process; Aviation; Environmental systems;
Anomaly detection
AB The environmental impact of aviation is enormous given the fact that in the US alone there are nearly 6 million flights per year of commercial aircraft. This situation has driven numerous policy and procedural measures to help develop environmentally friendly technologies which are safe and affordable and reduce the environmental impact of aviation. However, many of these technologies require significant initial investment in newer aircraft fleets and modifications to existing regulations which are both long and costly enterprises. We propose to use an anomaly detection method based on Virtual Sensors to help detect overconsumption of fuel in aircraft which relies only on the data recorded during flight of most existing commercial aircraft, thus significantly reducing the cost and complexity of implementing this method. The Virtual Sensors developed here are ensemble-learning regression models for detecting the overconsumption of fuel based on instantaneous measurements of the aircraft state. This approach requires no additional information about standard operating procedures or other encoded domain knowledge. We present experimental results on three data sets and compare five different Virtual Sensors algorithms. The first two data sets are publicly available and consist of a simulated data set from a flight simulator and a real-world turbine disk. We show the ability to detect anomalies with high accuracy on these data sets. These sets contain seeded faults, meaning that they have been deliberately injected into the system. The second data set is from real-world fleet of 84 jet aircraft where we show the ability to detect fuel overconsumption which can have a significant environmental and economic impact. To the best of our knowledge, this is the first study of its kind in the aviation domain.
C1 NASA, Ames Res Ctr, Intelligent Data Understanding Grp, Intelligent Syst Div, Moffett Field, CA 94035 USA.
RP Srivastava, AN (reprint author), NASA, Ames Res Ctr, Intelligent Data Understanding Grp, Intelligent Syst Div, Moffett Field, CA 94035 USA.
EM ashok.n.srivastava@nasa.gov
FU NASA
FX The author would like to thank Irving Statler for extremely thoughtful
and useful discussions throughout this project. The author also thanks
Timothy Woodbury for valuable discussions and Don Simon of NASA Glenn
Research Center for providing key references and analytical advice. He
would also like to acknowledge Nikunj Oza for valuable discussions and
the reviewers for their constructive feedback. The author also thanks
our airline partner in providing access to their flight operational data
to enable this study. This research was conducted with the support of
the NASA Aviation Safety Program's System-Wide Safety and Assurance
project. The code used for many of the algorithms in this paper is
available as opensource and can be found on DASHlink at
https://c3.nasa.gov/dashlink/projects/7/.
NR 29
TC 2
Z9 2
U1 1
U2 2
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1384-5810
J9 DATA MIN KNOWL DISC
JI Data Min. Knowl. Discov.
PD MAR
PY 2012
VL 24
IS 2
SI SI
BP 443
EP 471
DI 10.1007/s10618-011-0240-z
PG 29
WC Computer Science, Artificial Intelligence; Computer Science, Information
Systems
SC Computer Science
GA 875TD
UT WOS:000299057000006
ER
PT J
AU Yeom, K
Park, JH
AF Yeom, Kiwon
Park, Ji-Hyung
TI Morphological approach for autonomous and adaptive systems based on
self-reconfigurable modular agents
SO FUTURE GENERATION COMPUTER SYSTEMS-THE INTERNATIONAL JOURNAL OF ESCIENCE
LA English
DT Article
DE Morphogenesis; Self-organization; Modular agents; Federation of agents
ID ENVIRONMENTS
AB This paper describes a novel approach for managing self-organizing, distributed modular components in dynamically changing environments. The main concept is to fabricate a system which is composed of dynamically associated modular agents, that can migrate and reorganize by itself while the system is being executed. Association between modular agents can be varied and transmuted according to components' own migration schemes including deployment based on biological processes. This paper presents a self-organizable architecture, which can reorganize and reconfigure a system based on modular agents. It is contrived through observation of biological phenomena, and implements a platform to host the architecture in dynamically changing environments. We draw several key features of the modular agents, describe the principles of the modular agent based self-organizable framework, and depict how the proposed framework satisfies the functional requirements of network applications, which are made of several agents. We also demonstrate the efficiency and scalability of the framework through examining some simulation results. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Yeom, Kiwon] NASA, Human Syst Integrat Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Yeom, Kiwon; Park, Ji-Hyung] Korea Inst Sci & Technol, Ctr Intelligence & Interact, Seoul, South Korea.
RP Yeom, K (reprint author), NASA, Human Syst Integrat Div, Ames Res Ctr, Mail Stop 262-4,Bldg 262,Rm 155,POB 1, Moffett Field, CA 94035 USA.
EM kiwon.yeom@nasa.gov
FU University of Science and Technology
FX This work was supported by University of Science and Technology through
UST Post-Doc Research Program.
NR 48
TC 3
Z9 4
U1 0
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0167-739X
EI 1872-7115
J9 FUTURE GENER COMP SY
JI Futur. Gener. Comp. Syst.
PD MAR
PY 2012
VL 28
IS 3
BP 533
EP 543
DI 10.1016/j.future.2011.03.002
PG 11
WC Computer Science, Theory & Methods
SC Computer Science
GA 871YS
UT WOS:000298774200006
ER
PT J
AU Slegers, NJ
Kadish, RT
Payton, GE
Thomas, J
Griffin, MD
Dumbacher, D
AF Slegers, Nathan J.
Kadish, Ronald T.
Payton, Gary E.
Thomas, John
Griffin, Michael D.
Dumbacher, Dan
TI Learning from failure in systems engineering: A panel discussion
SO SYSTEMS ENGINEERING
LA English
DT Article
DE failure; product success; risk; lessons from failure; process
AB This paper summarizes the discussion of the Learning from Failure in Systems Engineering panel that was held in Huntsville, AL on November 8, 2010. The panel objective was to discuss how systems engineers respond to and learn from failure and identify future directions important to the community. The panel consisted of four representatives with experience in government, industry, and academia: (1) Ronald Kadish from Booz Allen Hamilton and former director of the Missile Defense Agency, (2) Gary Payton, retired Deputy Under Secretary of the Air Force for Space Programs, (3) John Thomas from Booz Allen Hamilton and President-elect of INCOSE, and (4) Michael Griffin from the University of Alabama, Huntsville and former NASA Administrator. Each panelist was asked to (i) provide an opening statement and elaborate on their experience with failure, (ii) describe when failure is appropriate, (iii) describe how we learn and react to failure, and (iv) identify and discuss techniques to improve how systems engineers react to failure. Several common themes arose from the discussion including: failure is an option, the importance of failure to allow reassessment, and more process is not the solution. Each of these is discussed in turn along with future directions identified for reacting to and learning from failure. (C) 2011 Wiley Periodicals, Inc. Syst Eng
C1 [Slegers, Nathan J.] Univ Alabama, Dept Mech & Aerosp Engn, Huntsville, AL 35899 USA.
[Kadish, Ronald T.] Booz Allen Hamilton, Ctr Excellence Acquisit & Program Management, Mclean, VA 22102 USA.
[Payton, Gary E.] SCI Aerosp Inc, Fairfax Stn, VA 22039 USA.
[Thomas, John] Booz Allen Hamilton, Herndon, VA 20171 USA.
[Griffin, Michael D.] Univ Alabama, Ctr Syst Studies, Huntsville, AL 35899 USA.
[Dumbacher, Dan] NASA, MSFC, Huntsville, AL 35812 USA.
RP Slegers, NJ (reprint author), Univ Alabama, Dept Mech & Aerosp Engn, N274 Technol Hall, Huntsville, AL 35899 USA.
EM slegers@mae.uah.edu; kadish_ronald@bah.com; gary.payton@sci-aero.com;
thomas_john@bah.com; mdg0007@uah.edu; daniel.l.dumbacher@nasa.gov
RI 李, 涵/B-4995-2012
NR 20
TC 5
Z9 5
U1 2
U2 8
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1098-1241
J9 SYSTEMS ENG
JI Syst. Eng.
PD SPR
PY 2012
VL 15
IS 1
BP 74
EP 82
DI 10.1002/sys.20195
PG 9
WC Engineering, Industrial; Operations Research & Management Science
SC Engineering; Operations Research & Management Science
GA 873JB
UT WOS:000298877400006
ER
PT J
AU Bonamente, M
Hasler, N
Bulbul, E
Carlstrom, JE
Culverhouse, TL
Gralla, M
Greer, C
Hawkins, D
Hennessy, R
Joy, M
Kolodziejczak, J
Lamb, JW
Landry, D
Leitch, EM
Marrone, DP
Miller, A
Mroczkowski, T
Muchovej, S
Plagge, T
Pryke, C
Sharp, M
Woody, D
AF Bonamente, Massimiliano
Hasler, Nicole
Bulbul, Esra
Carlstrom, John E.
Culverhouse, Thomas L.
Gralla, Megan
Greer, Christopher
Hawkins, David
Hennessy, Ryan
Joy, Marshall
Kolodziejczak, Jeffery
Lamb, James W.
Landry, David
Leitch, Erik M.
Marrone, Daniel P.
Miller, Amber
Mroczkowski, Tony
Muchovej, Stephen
Plagge, Thomas
Pryke, Clem
Sharp, Matthew
Woody, David
TI Comparison of pressure profiles of massive relaxed galaxy clusters using
the Sunyaev-Zel'dovich and x-ray data
SO NEW JOURNAL OF PHYSICS
LA English
DT Article
ID COSMIC DISTANCE SCALE; HUBBLE CONSTANT; WMAP DATA; SAMPLE; CHANDRA; GHZ;
SIMULATIONS; COSMOLOGY; FRACTION
AB We present the Sunyaev-Zel'dovich (SZ) effect observations of a sample of 25 massive relaxed galaxy clusters observed with the Sunyaev-Zel'dovich array (SZA), an eight-element interferometer that is part of the Combined Array for Research in Millimeter-wave Astronomy (CARMA). We performed an analysis of new SZA data and archival Chandra observations of this sample to investigate the integrated pressure-a proxy for cluster mass-determined from x-ray and SZ observations, two independent probes of the intra-cluster medium (ICM). This analysis makes use of a model for the ICM introduced by Bulbul (2010 Astrophys. J. 720 1038) which can be applied simultaneously to the SZ and x-ray data. With this model, we estimated the pressure profile for each cluster using a joint analysis of the SZ and x-ray data, and using the SZ data alone. We found that the integrated pressures measured from the x-ray and SZ data are consistent. This conclusion is in agreement with recent results obtained using WMAP and Planck data, confirming that SZ and x-ray observations of massive clusters detect the same amount of thermal pressure from the ICM. To test for possible biases introduced by our choice of model, we also fitted the SZ data using the universal pressure profile proposed by Arnaud (2010 Astron. Astrophys. 517 A92) and found consistency between the two models out to r(500) in the pressure profiles and integrated pressures.
C1 [Bonamente, Massimiliano; Hasler, Nicole; Bulbul, Esra; Landry, David] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
[Bonamente, Massimiliano; Joy, Marshall; Kolodziejczak, Jeffery] NASA, George C Marshall Space Flight Ctr, Space Sci VP62, Huntsville, AL 35812 USA.
[Carlstrom, John E.; Culverhouse, Thomas L.; Gralla, Megan; Greer, Christopher; Hennessy, Ryan; Leitch, Erik M.; Plagge, Thomas; Pryke, Clem; Sharp, Matthew] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Carlstrom, John E.; Culverhouse, Thomas L.; Gralla, Megan; Greer, Christopher; Hennessy, Ryan; Leitch, Erik M.; Plagge, Thomas; Pryke, Clem; Sharp, Matthew] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Carlstrom, John E.; Pryke, Clem] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Carlstrom, John E.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Hawkins, David; Lamb, James W.; Muchovej, Stephen; Woody, David] CALTECH, Owens Valley Radio Observ, Big Pine, CA 93513 USA.
NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Marrone, Daniel P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Miller, Amber] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Miller, Amber] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Mroczkowski, Tony] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
RP Bonamente, M (reprint author), Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
EM bonamem@uah.edu
OI Marrone, Daniel/0000-0002-2367-1080; Mroczkowski,
Tony/0000-0003-3816-5372
FU NSF [AST-0604982, AST-0838187, AST-0507545, AST-05-07161]; University of
Chicago [PHY-0114422]; NASA [PF0-110077]; Chandra X-ray Center;
Smithsonian Astrophysical Observatory for NASA [NAS8-03060]
FX The operation of the SZA is supported by the NSF through grants
AST-0604982 and AST-0838187. Partial support was also provided by grant
PHY-0114422 of the University of Chicago and by NSF grants AST-0507545
and AST-05-07161 to Columbia University. The CARMA operations are
supported by the NSF under a cooperative agreement and by the CARMA
partner universities. Support for TM was provided by the NASA through
Einstein Postdoctoral Fellowship grant number PF0-110077 awarded by the
Chandra X-ray Center, which is operated by the Smithsonian Astrophysical
Observatory for NASA under contract NAS8-03060.
NR 38
TC 28
Z9 28
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1367-2630
J9 NEW J PHYS
JI New J. Phys.
PD FEB 29
PY 2012
VL 14
AR 025010
DI 10.1088/1367-2630/14/2/025010
PG 18
WC Physics, Multidisciplinary
SC Physics
GA 919GO
UT WOS:000302310900001
ER
PT J
AU Choukroun, M
Sotin, C
AF Choukroun, M.
Sotin, C.
TI Is Titan's shape caused by its meteorology and carbon cycle?
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID ETHANE; ATMOSPHERE; METHANE; GAS; PHOTOCHEMISTRY; DIFFUSION; MODEL
AB Titan's shape is characterized by a difference between the long equatorial radius and the polar radius that is several hundred meters larger than that predicted by the flattening due to its spin rate. The North polar region is covered by large mare filled with hydrocarbons, including ethane. Moreover global circulation models predict ethane precipitation on the polar areas. This study shows that the shape of Titan can be explained by the subsidence associated with the substitution of methane with ethane-rich liquids percolating into the crust which, as suggested by evolution models, may be composed of methane clathrate hydrates. Such substitutions have been observed in laboratory experiments. This process would provide an additional methane source as required for sustaining the presence of this constituent in Titan's atmosphere through its history. A 270 m subsidence of the polar caps is explained by the circulation of 1.5 to 6 x 10(18) kg of ethane in the top three kilometers of an initially methane-clathrate crust. This process would have operated during the last 300-1200 Myr at the present ethane production rate. Citation: Choukroun, M., and C. Sotin (2012), Is Titan's shape caused by its meteorology and carbon cycle?, Geophys. Res. Lett., 39, L04201, doi:10.1029/2011GL050747.
C1 [Choukroun, M.; Sotin, C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Choukroun, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 79-24, Pasadena, CA 91109 USA.
EM mathieu.choukroun@jpl.nasa.gov
RI Choukroun, Mathieu/F-3146-2017
OI Choukroun, Mathieu/0000-0001-7447-9139
FU NASA Astrobiology Institute; California Institute of Technology
FX The authors thank M. Janssen and A. Le Gall for useful discussions, and
K. Lawrence for comments that helped improve the English writing. The
authors are grateful to Oded Aharonson and Francis Nimmo for
constructive reviews, which helped improve on this article. This work
has been conducted at the Jet Propulsion Laboratory, California
Institute of Technology, under contract to NASA. Support by the NASA
Astrobiology Institute is acknowledged. Government sponsorship
acknowledged.
NR 35
TC 30
Z9 30
U1 1
U2 17
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 FEB 29
PY 2012
VL 39
AR L04201
DI 10.1029/2011GL050747,2012
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 903OS
UT WOS:000301128200003
ER
PT J
AU Nichols, JE
Huang, YS
AF Nichols, Jonathan E.
Huang, Yongsong
TI Hydroclimate of the northeastern United States is highly sensitive to
solar forcing
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID HOLOCENE CLIMATE; RECORD; VARIABILITY; BOGS; PEAT; RECONSTRUCTION;
NETHERLANDS; POND; SUN
AB Dramatic hydrological fluctuations strongly impact human society, but the driving mechanisms for these changes are unclear. One suggested driver is solar variability, but supporting paleoclimate evidence is lacking. Therefore, long, continuous, high-resolution records from strategic locations are crucial for resolving the scientific debate regarding sensitivity of climate to solar forcing. We present a 6800-year, decadally-resolved biomarker and multidecadally-resolved hydrogen isotope record of hydroclimate from a coastal Maine peatland, The Great Heath (TGH). Regional moisture balance responds strongly and consistently to solar forcing at centennial to millennial timescales, with solar minima concurrent with wet conditions. We propose that the Arctic/North Atlantic Oscillation (AO/NAO) can amplify small solar fluctuations, producing the reconstructed hydrological variations. The Sun may be entering a weak phase, analogous to the Maunder minimum, which could lead to more frequent flooding in the northeastern US at this multidecadal timescale. Citation: Nichols, J. E., and Y. Huang (2012), Hydroclimate of the northeastern United States is highly sensitive to solar forcing, Geophys. Res. Lett., 39, L04707, doi:10.1029/2011GL050720.
C1 [Nichols, Jonathan E.] Columbia Univ, Earth Inst, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
[Nichols, Jonathan E.; Huang, Yongsong] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Nichols, Jonathan E.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
RP Nichols, JE (reprint author), Columbia Univ, Earth Inst, Lamont Doherty Earth Observ, 61 Rte 9W, Palisades, NY 10964 USA.
EM jnichols@ldeo.columbia.edu
FU National Science Foundation [0402383, 0816739, 1024144]; NASA
FX We thank J.M. Russell and M.J. Previdi for critical discussion and
reading of the manuscript. The research is supported by grants from
National Science Foundation (0402383, 0816739, 1024144) to YH. JEN is
currently supported by the NASA Postdoctoral Program.
NR 29
TC 11
Z9 11
U1 2
U2 18
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 FEB 29
PY 2012
VL 39
AR L04707
DI 10.1029/2011GL050720
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 903OS
UT WOS:000301128200002
ER
PT J
AU Lu, GP
Cummer, SA
Blakeslee, RJ
Weiss, S
Beasley, WH
AF Lu, Gaopeng
Cummer, Steven A.
Blakeslee, Richard J.
Weiss, Stephanie
Beasley, William H.
TI Lightning morphology and impulse charge moment change of high peak
current negative strokes
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID TIBETAN PLATEAU; MAPPING ARRAY; HIGH-PLAINS; DISCHARGES; FLASHES;
THUNDERSTORMS; FIELDS; SPRITES; PROPAGATION; INITIATION
AB We have analyzed very high frequency lightning mapping observations and remote magnetic field measurements to investigate connections between lightning morphology and impulse charge moment change (iCMC) of negative cloud-to-ground (CG) strokes with high estimated peak currents. Four lightning morphologies are identified for a total of 2126 strokes within optimum detection range of the North Alabama Lightning Mapping Array, and statistical iCMC distributions are given for each of these types. Almost all (>90%) of the largest impulse charge moments (greater than -200 C km in this data set) are not produced by strokes in ordinary negative CG flashes. Instead, negative strokes with the largest iCMCs are almost exclusively associated with two unusual flash types that both initially develop as positive (normal) intracloud lightning. In the first type the negative stroke with high iCMCs results from a negative leader that descends from the midlevel negative charge region after the upper level negative leader ceases propagating. In the second type, the upper level negative leader of the intracloud lightning progresses toward ground as a so-called bolt from the blue to generate the negative stroke. Measurements of strokes associated with four negative polarity sprites suggest that all four were most likely produced in the first unusual lightning type. Our results highlight that estimated peak current and impulse charge transfer are not always well correlated and that the in-cloud lightning structure strongly influences charge transfer on short time scales in negative CG strokes.
C1 [Lu, Gaopeng; Cummer, Steven A.] Duke Univ, Dept Elect & Comp Engn, Durham, NC 27708 USA.
[Blakeslee, Richard J.] NASA, Earth Sci Off, Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
[Weiss, Stephanie; Beasley, William H.] Univ Oklahoma, Sch Meteorol, Norman, OK 73019 USA.
RP Lu, GP (reprint author), Duke Univ, Dept Elect & Comp Engn, Box 90291,Hudson Hall 05C, Durham, NC 27708 USA.
EM gaopeng.lu@duke.edu; cummer@ee.duke.edu; rich.blakeslee@nasa.gov;
stepha.weiss@gmail.com; whb@ou.edu
RI Lu, Gaopeng/D-9011-2012; Cummer, Steven/A-6118-2008
OI Cummer, Steven/0000-0002-0002-0613
FU National Science Foundation; Defense Advanced Research Projects Agency
FX This work was supported by the Physical and Dynamic Meteorology Program
of the National Science Foundation and the NIMBUS Program of the Defense
Advanced Research Projects Agency. Lucian Zigoneanu is acknowledged for
routinely operating the low light level video camera in Duke Forest.
NR 60
TC 27
Z9 29
U1 2
U2 13
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 FEB 28
PY 2012
VL 117
AR D04212
DI 10.1029/2011JD016890
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 903PG
UT WOS:000301129700002
ER
PT J
AU Holmes, TRH
Jackson, TJ
Reichle, RH
Basara, JB
AF Holmes, Thomas R. H.
Jackson, Thomas J.
Reichle, Rolf H.
Basara, Jeffrey B.
TI An assessment of surface soil temperature products from numerical
weather prediction models using ground-based measurements
SO WATER RESOURCES RESEARCH
LA English
DT Article
ID MICROWAVE EMISSION; MOISTURE RETRIEVAL; PARAMETERIZATION; SALINITY;
NETWORK; MISSION; SPACE
AB Surface soil temperature estimates at approximately 0.05 m depth are needed to retrieve soil moisture from the planned Soil Moisture Active Passive (SMAP) L-band (1.4 GHz) satellite. Numerical weather prediction (NWP) systems as operated by various weather centers produce global estimates of soil temperature. In this study in situ data collected over the state of Oklahoma are used to assess surface (soil) temperature from three NWP systems: (1) the integrated forecast system from the European Center for Medium range Weather Forecasts (ECMWF), (2) the modern-era retrospective analysis for research and applications (MERRA) from the NASA Global Modeling and Assimilation Office, and (3) the global data assimilation system used by the National Center for Environmental Prediction (NCEP). The results are presented by hour of day with specific attention directed to the SMAP early morning overpass time at around 6 A. M. local time, and the period of 1 April to 1 October 2009. It was found that the NWP systems estimate the 0.05 m soil temperature at this time of day with an overall root mean square error of 1.9 to 2.0 K. It is shown that this error can be reduced to 1.6 to 1.8 K when differences between the modeling and measurement depth are accounted for by synchronizing each NWP set to match the mean phase of the in situ data and adjusting the amplitude in accordance with heat flow principles. These results indicate that with little calibration all products meet the SMAP error budget criteria over Oklahoma.
C1 [Holmes, Thomas R. H.; Jackson, Thomas J.] USDA ARS, Hydrol & Remote Sensing Lab, Beltsville, MD 20705 USA.
[Basara, Jeffrey B.] Univ Oklahoma, Oklahoma Climatol Survey, Norman, OK 73072 USA.
[Reichle, Rolf H.] NASA GSFC, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
RP Holmes, TRH (reprint author), USDA ARS, Hydrol & Remote Sensing Lab, 10300 Baltimore Ave,Rm 104,Bldg 007,BARC W, Beltsville, MD 20705 USA.
EM thomas.holmes@ars.usda.gov
RI Reichle, Rolf/E-1419-2012; Basara, Jeffrey/A-4907-2008; Holmes,
Thomas/F-4512-2010
OI Basara, Jeffrey/0000-0002-2096-6844; Holmes, Thomas/0000-0002-4651-0079
FU State of OK through the OK State Regents for Higher Education; State of
OK through the OK Department of Public Safety; NASA SMAP Science
Definition Team
FX The authors would like to thank the Global Modeling and Assimilation
Office (GMAO) and the GES DISC (both at NASA Goddard Space Flight
Center) for the dissemination of MERRA; the taxpayers of the State of OK
for funding the OK mesonet through the OK State Regents for Higher
Education and the OK Department of Public Safety; the European Centre
for Medium range Weather Forecasting (ECMWF) for the dissemination of
their data (by way of the SMAP Test bed), and the National Centers for
Environmental Prediction for dissemination of GDAS data (by way of
Hiroko Beaudoing of NASA's Hydrological Science Branch). Rolf Reichle
was funded by the NASA SMAP Science Definition Team. The USDA is an
equal opportunity provider and employer.
NR 35
TC 18
Z9 19
U1 0
U2 19
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0043-1397
EI 1944-7973
J9 WATER RESOUR RES
JI Water Resour. Res.
PD FEB 28
PY 2012
VL 48
AR W02531
DI 10.1029/2011WR010538
PG 14
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA 903QJ
UT WOS:000301133200001
ER
PT J
AU Barge, LM
Doloboff, IJ
White, LM
Stucky, GD
Russell, MJ
Kanik, I
AF Barge, Laura M.
Doloboff, Ivria J.
White, Lauren M.
Stucky, Galen D.
Russell, Michael J.
Kanik, Isik
TI Characterization of Iron-Phosphate-Silicate Chemical Garden Structures
SO LANGMUIR
LA English
DT Article
ID CITY HYDROTHERMAL FIELD; PRECIPITATION TUBES; LIFE; ORIGIN; GROWTH
AB Chemical gardens form when ferrous chloride hydrate seed crystals are added or concentrated solutions are injected into solutions of sodium silicate and potassium phosphate. Various precipitation morphologies are observed depending on silicate and phosphate concentrations, including hollow plumes, bulbs, and tubes. The growth of precipitates is controlled by the internal osmotic pressure, fluid buoyancy, and membrane strength. Additionally, rapid bubble-led growth is observed when silicate concentrations are high. ESEM/EDX analysis confirms compositional gradients within the membranes, and voltage measurements across the membranes during growth show a final potential of around 150-200 mV, indicating that electrochemical gradients are maintained across the membranes as growth proceeds. The characterization of chemical gardens formed with iron, silicate, and phosphate, three important components of an early earth prebiotic hydrothermal system, can help us understand the properties of analogous structures that likely formed at submarine alkaline hydrothermal vents in the Hadean-structures offering themselves as the hatchery of life.
C1 [Barge, Laura M.; Doloboff, Ivria J.; White, Lauren M.; Russell, Michael J.; Kanik, Isik] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[White, Lauren M.; Stucky, Galen D.] Univ Calif Santa Barbara, Dept Chem & Biochem, Santa Barbara, CA 93106 USA.
[Stucky, Galen D.] Univ Calif Santa Barbara, Dept Mat, Santa Barbara, CA 93106 USA.
RP Barge, LM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM laura.m.barge@jpl.nasa.gov
FU ConvEne IGERT Program [NSF-DGE 0801627]; JPL; National Aeronautics and
Space Administration with support by the NASA Astrobiology Institute
(Icy Worlds); NAI
FX L.M.W. was supported by the ConvEne IGERT Program (NSF-DGE 0801627).
M.J.R. was supported by the Research and Technology Development Program
of the JPL. 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
with support by the NASA Astrobiology Institute (Icy Worlds). We
acknowledge useful discussions with members attending the first and
second meetings of the NAI-sponsored Thermodynamics Disequilibrium and
Evolution Focus Group.
NR 34
TC 28
Z9 29
U1 3
U2 30
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0743-7463
J9 LANGMUIR
JI Langmuir
PD FEB 28
PY 2012
VL 28
IS 8
BP 3714
EP 3721
DI 10.1021/la203727g
PG 8
WC Chemistry, Multidisciplinary; Chemistry, Physical; Materials Science,
Multidisciplinary
SC Chemistry; Materials Science
GA 898QU
UT WOS:000300757700007
PM 22035594
ER
PT J
AU Marcus, SL
Dickey, JO
Fukumori, I
de Viron, O
AF Marcus, S. L.
Dickey, J. O.
Fukumori, I.
de Viron, O.
TI Detection of the Earth rotation response to a rapid fluctuation of
Southern Ocean circulation in November 2009
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID OF-DAY VARIATIONS; LENGTH; VARIABILITY; SIGNALS
AB At seasonal and shorter periods the solid Earth and its overlying geophysical fluids form a closed dynamical system, which (except for tidal forcing) conserves its total angular momentum. While atmospheric effects dominate changes in the Earth's rate of rotation and hence length-of-day (LOD) on these time scales, the addition of oceanic angular momentum (OAM) estimates has been shown to improve closure of the LOD budget in a statistical sense. Here we demonstrate, for the first time, the signature of a specific, sub-monthly ocean current fluctuation on the Earth's rotation rate, coinciding with recently-reported anomalies which developed in southeast Pacific surface temperature and bottom pressure fields during late 2009. Our results show that concurrent variations in the Antarctic Circumpolar Current (ACC), which saw a sharp drop and recovery in zonal transport during a two-week period in November, were strong enough to cause a detectable change in LOD following the removal of atmospheric angular momentum (AAM) computed from the Modern Era Retrospective Analysis for Research and Applications (MERRA) database. The strong OAM variations driving the LOD-AAM changes were diagnosed from ocean state estimates of the Consortium for Estimating the Circulation and Climate of the Ocean (ECCO) and involved roughly equal contributions from the current and pressure terms, with in situ confirmation for the latter provided by tide-corrected bottom pressure recorder data from the South Drake Passage site of the Antarctic Circumpolar Current Levels by Altimetry and Island Measurements (ACCLAIM) network. Citation: Marcus, S. L., J. O. Dickey, I. Fukumori, and O. de Viron (2012), Detection of the Earth rotation response to a rapid fluctuation of Southern Ocean circulation in November 2009, Geophys. Res. Lett., 39, L04605, doi:10.1029/2011GL050671.
C1 [Marcus, S. L.; Dickey, J. O.; Fukumori, I.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[de Viron, O.] Univ Paris Diderot, IPGP, PRES Sorbonne Paris Cite, F-75005 Paris, France.
RP Marcus, SL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM steven.marcus@jpl.nasa.gov
RI de Viron, Olivier/N-6647-2014
OI de Viron, Olivier/0000-0003-3112-9686
FU NASA
FX MERRA data used in this study have been provided by the Global Modeling
and Assimilation Office (GMAO) at NASA Goddard Space Flight Center
through the NASA GES DISC online archive. We thank Chris Hughes of the
U.K. National Oceanography Centre and University of Liverpool for
assistance in acquiring and processing the ACCLAIM bottom pressure
recorder data, and three anonymous reviewers whose comments helped to
improve the manuscript. The contribution of OdV to this study is IPGP
contribution 3269. The work of S. L. M., J.O.D. and I. F. described in
this paper was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with NASA. J.O.D. would like to
thank Universite Paris Diderot and Institut de Physique du Globe de
Paris for their gracious hospitality during her May and June 2011 visit.
NR 23
TC 1
Z9 1
U1 1
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD FEB 28
PY 2012
VL 39
AR L04605
DI 10.1029/2011GL050671
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 903OQ
UT WOS:000301127800003
ER
PT J
AU Knudsen, DJ
Kabirzadeh, R
Burchill, JK
Pfaff, RF
Wallis, DD
Bounds, SR
Clemmons, JH
Pincon, JL
AF Knudsen, D. J.
Kabirzadeh, R.
Burchill, J. K.
Pfaff, R. F.
Wallis, D. D.
Bounds, S. R.
Clemmons, J. H.
Pincon, J. -L.
TI Strong magnetic field fluctuations within filamentary auroral density
cavities interpreted as VLF saucer sources
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID TRANSVERSE ION-ACCELERATION; HYBRID SOLITARY STRUCTURES; IONOSPHERE;
WAVES; PLASMA; DEPLETIONS; MAGNETOSPHERE; EIGENMODES; FREJA; GRADIENTS
AB The Geoelectrodynamics and Electro-Optical Detection of Electron and Suprathermal Ion Currents (GEODESIC) sounding rocket encountered more than 100 filamentary density cavities associated with enhanced plasma waves at ELF (< 3 kHz) and VLF (3-10 kHz) frequencies and at altitudes of 800-990 km during an auroral substorm. These cavities were similar in size (similar to 20 m diameter in most cases) to so-called lower-hybrid cavities (LHCs) observed by previous sounding rockets and satellites; however, in contrast, many of the GEODESIC cavities exhibited up to tenfold enhancements in magnetic wave power throughout the VLF band. GEODESIC also observed enhancements of ELF and VLF electric fields both parallel and perpendicular to the geomagnetic field B-0 within cavities, though the VLF E field increases were often not as large proportionally as seen in the magnetic fields. This behavior is opposite to that predicted by previously published theories of LHCs based on passive scattering of externally incident auroral hiss. We argue that the GEODESIC cavities are active wave generation sites capable of radiating VLF waves into the surrounding plasma and producing VLF saucers, with energy supplied by cold, upward flowing electron beams composing the auroral return current. This interpretation is supported by the observation that the most intense waves, both inside and outside cavities, occurred in regions where energetic electron precipitation was largely inhibited or absent altogether. We suggest that the wave-enhanced cavities encountered by GEODESIC were qualitatively different from those observed by earlier spacecraft because of the fortuitous timing of the GEODESIC launch, which placed the payload at apogee within a substorm-related return current during its most intense phase, lasting only a few minutes.
C1 [Knudsen, D. J.; Kabirzadeh, R.; Burchill, J. K.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada.
[Knudsen, D. J.; Pfaff, R. F.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kabirzadeh, R.] Stanford Univ, Dept Elect Engn, Stanford, CA 94305 USA.
[Wallis, D. D.] Nat Resources Canada, Ottawa, ON K1A 0Y3, Canada.
[Bounds, S. R.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Clemmons, J. H.] Aerosp Corp, Los Angeles, CA 90009 USA.
[Pincon, J. -L.] CNRS, LPCE, F-45071 Orleans, France.
RP Knudsen, DJ (reprint author), Univ Calgary, Dept Phys & Astron, 2500 Univ Dr NW, Calgary, AB T2N 1N4, Canada.
EM knudsen@ucalgary.ca; burchill@phys.ucalgary.ca
RI Pfaff, Robert/F-5703-2012;
OI Pfaff, Robert/0000-0002-4881-9715; Clemmons, James/0000-0002-5298-5222
FU Canadian Space Agency; NASA [NAG5-5201]; Natural Sciences and
Engineering Research Council of Canada
FX Funding for the GEODESIC project was provided by the Canadian Space
Agency and NASA. The GEODESIC payload was built by Bristol Aerospace,
Ltd. Magnetometer data in Figure 3 were provided by the Geophysical
Institute at the University of Alaska, Fairbanks. This study was
supported by the Natural Sciences and Engineering Research Council of
Canada, and by NASA grant NAG5-5201. Thanks to Richard Denton and Susan
Swartz of Dartmouth College for providing a Java-based user interface
for WHAMP, and to John Bonnell, Anders Eriksson and Mats Andre for
helpful discussions. D.J.K. wishes to thank H. deFeraudy for hosting his
visit to CETP-IPSL/CNRS, Velizy, France, during which part of this work
was carried out.
NR 37
TC 1
Z9 2
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 FEB 25
PY 2012
VL 117
AR A02217
DI 10.1029/2011JA017316
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 899NT
UT WOS:000300823500003
ER
PT J
AU Mitsuishi, I
Gupta, A
Yamasaki, NY
Takei, Y
Ohashi, T
Sato, K
Galeazzi, M
Henry, JP
Kelley, RL
AF Mitsuishi, Ikuyuki
Gupta, Anjali
Yamasaki, Noriko Y.
Takei, Yoh
Ohashi, Takaya
Sato, Kosuke
Galeazzi, Massimiliano
Henry, J. Patrick
Kelley, Richard L.
TI Search for X-Ray Emission Associated with the Shapley Supercluster with
Suzaku
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE intergalactic medium; supercluster; X-rays: galaxies: clusters
ID HOT INTERGALACTIC MEDIUM; WIND CHARGE-EXCHANGE; VIRIAL RADIUS; DIFFUSE
EMISSION; GALAXY CLUSTERS; MISSING BARYONS; SCULPTOR WALL; COMA CLUSTER;
H I; CORE
AB Suzaku performed observations of 3 regions in and around the Shapley supercluster, a region located between A 3558 and A 3556, at similar to 0.9 times the virial radii of both clusters, and two other regions at 1 degrees and 4 degrees away from the first pointing. The 4 degrees-offset observation was used to evaluate the Galactic foreground emission. We did not detect significant redshifted Oxygen emission lines (O VII and O VIII) in the spectra of all three pointings, after subtracting the contribution of foreground and background emission. The upper limit for the redshifted O VIII K alpha line intensity of the warm-hot intergalactic medium (WHIM) is 1.5 x 10(-7) photons s(-1) cm(-2) arcmin-2, which corresponds to an overdensity of similar to 380 (Z/0.1 Z(circle dot))(-1/2) (L/3 Mpc)(-1/2), assuming T = 3 x 10(6) K. We found excess continuum emission in the 1 degrees-offset and on-filament regions, represented by thermal models with k T similar to 1 keV and similar to 2 keV, respectively. The redshifts of both 0 and that of the supercluster (0.048) are consistent with the observed spectra. The similar to 1 keV emission can also be fitted with Ne-rich Galactic (zero redshift) thin thermal emission. The radial intensity profile of the 2 keV component suggests contributions from A 3558 and A 3556, but with significant steepening of the intensity slope in the outer region of A 3558. Finally, we summarized the previous Suzaku search for the WHIM, and discussed the feasibility of constraining the WHIM. An overdensity of <400 could be detectable using O VII and 0 VIII emission lines in a range of 1.4 x 10(6) K < T < 5 x 10(6) K or a continuum emission in a relatively high-temperature range of T > 5 x 10(6) K with the Suzaku XIS. The non-detection with Suzaku suggests that a typical line-of-sight average overdensity is <400.
C1 [Mitsuishi, Ikuyuki; Yamasaki, Noriko Y.; Takei, Yoh] Japan Aerosp Explorat Agcy ISAS JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Gupta, Anjali; Galeazzi, Massimiliano] Univ Miami, Dept Phys, Coral Gables, FL 33146 USA.
[Ohashi, Takaya] Tokyo Metropolitan Univ, Dept Phys, Hachioji, Tokyo 1920397, Japan.
[Sato, Kosuke] Tokyo Univ Sci, Dept Phys, Shinjyuku Ku, Tokyo 1628601, Japan.
[Henry, J. Patrick] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Kelley, Richard L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Mitsuishi, I (reprint author), Japan Aerosp Explorat Agcy ISAS JAXA, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan.
EM mitsuisi@astro.isas.jaxa.jp
RI Yamasaki, Noriko/C-2252-2008; Kelley, Richard/K-4474-2012; XRAY,
SUZAKU/A-1808-2009
FU Ministry of Education, Culture, Sports, Science and Technology
[10J07487, 15340088, 20340041, 21224003, 22111513]
FX I. M. is grateful to Kentaro Someya, Hiroshi Yoshitake, Kazuhiro Sakai
and Prof. Kazuhisa Mitsuda for useful advice and discussion. Part of
this work was financially supported by the Ministry of Education,
Culture, Sports, Science and Technology, Grant-in Aid for Scientific
Research 10J07487, 15340088, 20340041, 21224003, and 22111513.
NR 67
TC 6
Z9 6
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0004-6264
EI 2053-051X
J9 PUBL ASTRON SOC JPN
JI Publ. Astron. Soc. Jpn.
PD FEB 25
PY 2012
VL 64
IS 1
AR 18
DI 10.1093/pasj/64.1.18
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 905WS
UT WOS:000301307500018
ER
PT J
AU Sun, AY
Green, R
Swenson, S
Rodell, M
AF Sun, Alexander Y.
Green, Ronald
Swenson, Sean
Rodell, Matthew
TI Toward calibration of regional groundwater models using GRACE data
SO JOURNAL OF HYDROLOGY
LA English
DT Article
DE Groundwater modeling; GRACE; Multiobjective optimization; Water budget
analysis
ID GENETIC ALGORITHM; FLOW; METHODOLOGY; RECHARGE; SYSTEM
AB Regional groundwater models are increasingly used for short- and long-term water resources planning, in anticipation of greater climate variability and population growth. However, many of these models are subject to structural and parametric uncertainties because of the lack of field measurements. In recent years, the Gravity Recovery and Climate Experiment (GRACE) satellite mission has shown great potential for tracking total water storage changes over large regions. The pattern of groundwater storage changes inferred from GRACE may be incorporated as an additional regularization mechanism for calibrating regional groundwater models. Motivated by the demonstrated success of GRACE for monitoring groundwater storage changes, this study explores the combined use of in situ water level measurements and GRACE-derived groundwater storage changes for calibrating regional groundwater models. The resulting optimization problem is solved using an evolutionary optimization algorithm. We demonstrate the proposed calibration strategy for the hydraulically connected Edwards-Trinity Plateau and Pecos Valley aquifers (total area 115,000 km(2)) in west Texas. Monthly GRACE data from 2002 to 2007 were used to recalibrate a regional groundwater model developed for the area. Our results indicate that (i) calibration using in situ data alone may yield multiple plausible solutions, a phenomenon well known to hydrologists; and (ii) GRACE data helped further constrain model parameters over the study period and, thus, may be continuously assimilated, among other sources of data, for enhancing existing regional groundwater models. (C) 2011 Published by Elsevier B.V.
C1 [Sun, Alexander Y.; Green, Ronald] SW Res Inst, Geosci & Engn Div, San Antonio, TX USA.
[Swenson, Sean] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Rodell, Matthew] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA.
RP Sun, AY (reprint author), Univ Texas Austin, Bur Econ Geol, Jackson Sch Geosci, Austin, TX 78712 USA.
EM asun@swri.org
RI Rodell, Matthew/E-4946-2012; Sun, Alexander/A-9959-2011
OI Rodell, Matthew/0000-0003-0106-7437;
FU Southwest Research Institute [R8501]; NASA [NNX09AR63G]
FX The authors are grateful to J.L. Awange and two other anonymous
reviewers for their constructive comments. A. Sun is in debt to Dr. Ian
Jones for providing the original ETPV GAM model and for engaging in
numerous discussions. A. Sun and R. Green were partly supported by
Southwest Research Institute R&D Project R8501 and NASA Grant
NNX09AR63G.
NR 42
TC 22
Z9 23
U1 1
U2 26
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-1694
J9 J HYDROL
JI J. Hydrol.
PD FEB 23
PY 2012
VL 422
BP 1
EP 9
DI 10.1016/j.jhydrol.2011.10.025
PG 9
WC Engineering, Civil; Geosciences, Multidisciplinary; Water Resources
SC Engineering; Geology; Water Resources
GA 904OP
UT WOS:000301208100001
ER
PT J
AU Huang, CS
Retterer, JM
de La Beaujardiere, O
Roddy, PA
Hunton, DE
Ballenthin, JO
Pfaff, RF
AF Huang, Chao-Song
Retterer, J. M.
de La Beaujardiere, O.
Roddy, P. A.
Hunton, D. E.
Ballenthin, J. O.
Pfaff, R. F.
TI Observations and simulations of formation of broad plasma depletions
through merging process
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID EQUATORIAL SPREAD-F; NONLINEAR EVOLUTION; BACKSCATTER PLUMES; DRIFTS;
CLIMATOLOGY; GENERATION; JICAMARCA; BUBBLES; GROWTH
AB Broad plasma depletions in the equatorial ionosphere near dawn are region in which the plasma density is reduced by 1-3 orders of magnitude over thousands of kilometers in longitude. This phenomenon is observed repeatedly by the Communication/Navigation Outage Forecasting System (C/NOFS) satellite during deep solar minimum. The plasma flow inside the depletion region can be strongly upward. The possible causal mechanism for the formation of broad plasma depletions is that the broad depletions result from merging of multiple equatorial plasma bubbles. The purpose of this study is to demonstrate the feasibility of the merging mechanism with new observations and simulations. We present C/NOFS observations for two cases. A series of plasma bubbles is first detected by C/NOFS over a longitudinal range of 3300-3800 km around midnight. Each of the individual bubbles has a typical width of similar to 100 km in longitude, and the upward ion drift velocity inside the bubbles is 200-400 m s(-1). The plasma bubbles rotate with the Earth to the dawn sector and become broad plasma depletions. The observations clearly show the evolution from multiple plasma bubbles to broad depletions. Large upward plasma flow occurs inside the depletion region over 3800 km in longitude and exists for similar to 5 h. We also present the numerical simulations of bubble merging with the physics-based low-latitude ionospheric model. It is found that two separate plasma bubbles join together and form a single, wider bubble. The simulations show that the merging process of plasma bubbles can indeed occur in incompressible ionospheric plasma. The simulation results support the merging mechanism for the formation of broad plasma depletions.
C1 [Huang, Chao-Song; de La Beaujardiere, O.; Roddy, P. A.; Hunton, D. E.; Ballenthin, J. O.] USAF, Space Vehicles Directorate, Res Lab, Kirtland AFB, NM 87117 USA.
[Retterer, J. M.] Boston Coll, Inst Sci Res, Chestnut Hill, MA 02467 USA.
[Pfaff, R. F.] NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Huang, CS (reprint author), USAF, Space Vehicles Directorate, Res Lab, 3550 Aberdeen Ave SE, Kirtland AFB, NM 87117 USA.
EM chaosong.huang@kirtland.af.mil
RI Pfaff, Robert/F-5703-2012
OI Pfaff, Robert/0000-0002-4881-9715
FU Air Force Office of Scientific Research (AFOSR) [FA9550-09-1-0321]; Air
Force Research Laboratory; Department of Defense; National Aeronautics
and Space Administration (NASA); Naval Research Laboratory; Aerospace
Corporation
FX Work by C.S.H. was supported by the Air Force Office of Scientific
Research (AFOSR) award FA9550-09-1-0321. The C/NOFS mission is supported
by the Air Force Research Laboratory, the Department of Defense Space
Test Program, the National Aeronautics and Space Administration (NASA),
the Naval Research Laboratory, and the Aerospace Corporation.
NR 39
TC 13
Z9 13
U1 1
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 FEB 23
PY 2012
VL 117
AR A02314
DI 10.1029/2011JA017084
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 899NR
UT WOS:000300823200001
ER
PT J
AU Jepsen, SM
Molotch, NP
Williams, MW
Rittger, KE
Sickman, JO
AF Jepsen, Steven M.
Molotch, Noah P.
Williams, Mark W.
Rittger, Karl E.
Sickman, James O.
TI Interannual variability of snowmelt in the Sierra Nevada and Rocky
Mountains, United States: Examples from two alpine watersheds
SO WATER RESOURCES RESEARCH
LA English
DT Article
ID COLORADO FRONT RANGE; HIGH-ELEVATION CATCHMENTS; LANDSAT THEMATIC
MAPPER; SPATIAL-DISTRIBUTION; ENERGY EXCHANGE; COVER DATA; CLIMATE;
MODEL; EQUIVALENT; SURFACE
AB The distribution of snow and the energy flux components of snowmelt are intrinsic characteristics of the alpine water cycle controlling the location of source waters and the effect of climate on streamflow. Interannual variability of these characteristics is relevant to the effect of climate change on alpine hydrology. Our objective is to characterize the interannual variability in the spatial distribution of snow and energy fluxes of snowmelt in watersheds of a maritime setting, Tokopah Basin (TOK) in California's southern Sierra Nevada, and a continental setting, Green Lake 4 Valley (GLV4) in Colorado's Front Range, using a 12 year database (1996-2007) of hydrometeorological observations and satellite-derived snow cover. Snowpacks observed in GLV4 exhibit substantially greater spatial variability than in TOK (0.75 versus 0.28 spatial coefficient of variation). In addition, modeling results indicate that the net turbulent energy flux contribution to snowmelt in GLV4 is, on average, 3 times greater in magnitude (mean 29% versus 10%) and interannual variability (standard deviation 17% versus 6%) than in TOK. These energy flux values exhibit strong seasonality, increasing as the melt season progresses to times later in the year (R-2 = 0.54-0.77). This seasonality of energy flux appears to be associated with snowmelt rates that generally increase with onset date of melt (0.02 cm d(-2)). This seasonality in snowmelt rate, coupled to differences in hydrogeology, may account for the observed differences in correspondence between the timing of snowmelt and timing of streamflow in these watersheds.
C1 [Jepsen, Steven M.] US Geol Survey, Denver Fed Ctr, Denver, CO 80225 USA.
[Molotch, Noah P.; Williams, Mark W.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80303 USA.
[Molotch, Noah P.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Rittger, Karl E.] Univ Calif Santa Barbara, Donald Bren Sch Environm Sci & Management, Santa Barbara, CA 93106 USA.
[Sickman, James O.] Univ Calif Riverside, Dept Environm Sci, Riverside, CA 92521 USA.
[Molotch, Noah P.; Williams, Mark W.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA.
RP Jepsen, SM (reprint author), US Geol Survey, Denver Fed Ctr, Box 25046, Denver, CO 80225 USA.
EM noah.molotch@colorado.edu
RI Molotch, Noah/C-8576-2009
FU NSF [EAR 1032308, 1032295, 0614207, 0724960, 0738780, 0738930]; NASA
[NNX08AH18G]; USGS; Niwot Ridge LTER program; NSF's Boulder Creek
Critical Zone Observatory
FX Technical support was provided by the following individuals : S. Burns,
N. Caine, T. Erickson, M. Colee, J. M. Melack, K. Musselman, T. H.
Painter, and K. Skeen. Helpful commentary on the manuscript was provided
by D. W. Clow, D. I. Stannard, and 3 anonymous reviewers. Financial
support was provided by NSF grants EAR 1032308, 1032295, 0614207,
0724960, 0738780, 0738930, NASA Grant NNX08AH18G, The NASA Postdoctoral
Program, The USGS Mendenhall Research Fellowship Program, the Niwot
Ridge LTER program, and NSF's Boulder Creek Critical Zone Observatory.
Any use of trade, firm, or product names is for descriptive purposes
only and does not imply endorsement by the U. S. Government.
NR 71
TC 30
Z9 30
U1 2
U2 42
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0043-1397
J9 WATER RESOUR RES
JI Water Resour. Res.
PD FEB 23
PY 2012
VL 48
AR W02529
DI 10.1029/2011WR011006
PG 15
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA 899NZ
UT WOS:000300824300002
ER
PT J
AU Archidiacono, M
De Bernardis, F
Cooray, A
Melchiorri, A
Amblard, A
Pagano, L
Serra, P
AF Archidiacono, Maria
De Bernardis, Francesco
Cooray, Asantha
Melchiorri, Alessandro
Amblard, Alexandre
Pagano, Luca
Serra, Paolo
TI Amplitudes of thermal and kinetic Sunyaev-Zel'dovich signals from
small-scale CMB anisotropies
SO PHYSICAL REVIEW D
LA English
DT Article
ID ATACAMA COSMOLOGY TELESCOPE; SOUTH-POLE TELESCOPE; POWER SPECTRUM;
BACKGROUND ANISOTROPIES; GALAXIES; FLUCTUATIONS; SIMULATIONS;
PREDICTIONS; SKY
AB While the arcminute-scale cosmic microwave background (CMB) anisotropies are due to secondary effects, point sources dominate the total anisotropy power spectrum. At high frequencies the point sources are primarily in the form of dusty, star-forming galaxies. Both Herschel and Planck have recently measured the anisotropy power spectrum of cosmic infrared background (CIB) generated by dusty, star-forming galaxies from degree to subarcminute angular scales, including the nonlinear clustering of these galaxies at multipoles of 3000 to 6000 relevant to CMB secondary anisotropy studies. We scale the CIB angular power spectra to CMB frequencies and interpret the combined WMAP-7 year and arcminute-scale Atacama Cosmology Telescope and South Pole Telescope CMB power spectra measurements to constrain the Sunyaev-Zel'dovich (SZ) effects. Allowing the CIB clustering amplitude to vary, we constrain the amplitudes of thermal and kinetic SZ power spectra at 150 GHz.
C1 [Archidiacono, Maria; Melchiorri, Alessandro; Pagano, Luca] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy.
[Archidiacono, Maria; Melchiorri, Alessandro; Pagano, Luca] Univ Roma La Sapienza, INFN, I-00185 Rome, Italy.
[De Bernardis, Francesco; Cooray, Asantha] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Amblard, Alexandre; Serra, Paolo] NASA Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA.
RP Archidiacono, M (reprint author), Univ Roma La Sapienza, Dept Phys, Piazzale Aldo Moro 2, I-00185 Rome, Italy.
RI Serra, Paolo/G-9678-2014; amblard, alexandre/L-7694-2014;
OI Serra, Paolo/0000-0002-7609-3931; amblard,
alexandre/0000-0002-2212-5395; Melchiorri,
Alessandro/0000-0001-5326-6003
FU NSF [AST-0645427]; NASA [NNX10AD42G]
FX It is a pleasure to thank Erminia Calabrese for useful suggestions and
comments. M. A. thanks the group at UCI for hospitality while this
research was conducted. We thank NSF AST-0645427 and NASA NNX10AD42G for
support.
NR 30
TC 1
Z9 1
U1 0
U2 1
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2470-0010
EI 2470-0029
J9 PHYS REV D
JI Phys. Rev. D
PD FEB 22
PY 2012
VL 85
IS 4
AR 043015
DI 10.1103/PhysRevD.85.043015
PG 7
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 896MQ
UT WOS:000300571500003
ER
PT J
AU McLinden, CA
Fioletov, V
Boersma, KF
Krotkov, N
Sioris, CE
Veefkind, JP
Yang, K
AF McLinden, C. A.
Fioletov, V.
Boersma, K. F.
Krotkov, N.
Sioris, C. E.
Veefkind, J. P.
Yang, K.
TI Air quality over the Canadian oil sands: A first assessment using
satellite observations
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID OZONE MONITORING INSTRUMENT; TROPOSPHERIC NO2; RETRIEVAL; SPACE;
EMISSIONS; ALGORITHM; SO2; OMI
AB Results from the first assessment of air quality over the Canadian oil sands-one of the largest industrial undertakings in human history-using satellite remote sensing observations of two pollutants, nitrogen dioxide (NO2) and sulfur dioxide (SO2), are presented. High-resolution maps were created that revealed distinct enhancements in both species over an area (roughly 30 km x 50 km) of intensive surface mining at scales of a few kilometers. The magnitude of these enhancements, quantified in terms of total mass, are comparable to the largest seen in Canada from individual sources. The rate of increase in NO2 between 2005 and 2010 was assessed at 10.4 +/- 3.5%/year and resulted from increases both in local values as well as the spatial extent of the enhancement. This is broadly consistent with both surface-measurement trends and increases in annual bitumen production. An increase in SO2 was also found, but given larger uncertainties, it is not statistically significant. Citation: McLinden, C. A., V. Fioletov, K. F. Boersma, N. Krotkov, C. E. Sioris, J. P. Veefkind, and K. Yang (2012), Air quality over the Canadian oil sands: A first assessment using satellite observations, Geophys. Res. Lett., 39, L04804, doi: 10.1029/2011GL050273.
C1 [McLinden, C. A.; Fioletov, V.; Sioris, C. E.] Environm Canada, Toronto, ON M3H 5T4, Canada.
[Boersma, K. F.; Veefkind, J. P.] Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands.
[Krotkov, N.; Yang, K.] NASA, Goddard Space Flight Ctr, Lab Atmospher Chem & Dynam, Greenbelt, MD 20771 USA.
[Boersma, K. F.] Eindhoven Univ Technol, Fluid Dynam Lab, NL-5600 MB Eindhoven, Netherlands.
[Veefkind, J. P.] Delft Univ Technol, Delft, Netherlands.
[Yang, K.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
RP McLinden, CA (reprint author), Environm Canada, 4905 Dufferin St, Toronto, ON M3H 5T4, Canada.
EM chris.mclinden@ec.gc.ca
RI Krotkov, Nickolay/E-1541-2012; Boersma, Klaas/H-4559-2012;
OI Krotkov, Nickolay/0000-0001-6170-6750; Boersma,
Klaas/0000-0002-4591-7635; Fioletov, Vitali/0000-0002-2731-5956; Sioris,
Christopher/0000-0003-1168-8755
FU NASA Earth Science Division
FX The authors thank the Wood Buffalo Environmental Association (WBEA) for
the provision of their in-situ data. In particular, CM thanks Kevin
Percy of WBEA for helpful discussions. We acknowledge the free use of
tropospheric NO2 column data from the GOME, SCIAMACHY, OMI,
and GOME-2 sensors from www.temis.nl. We also acknowledge the NASA Earth
Science Division for funding of OMI NO2 and SO2
products development and analysis.
NR 14
TC 48
Z9 49
U1 1
U2 48
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 FEB 22
PY 2012
VL 39
AR L04804
DI 10.1029/2011GL050273
PG 8
WC Geosciences, Multidisciplinary
SC Geology
GA 899DJ
UT WOS:000300794800001
ER
PT J
AU Renault, L
Dewitte, B
Marchesiello, P
Illig, S
Echevin, V
Cambon, G
Ramos, M
Astudillo, O
Minnis, P
Ayers, JK
AF Renault, Lionel
Dewitte, Boris
Marchesiello, Patrick
Illig, Serena
Echevin, Vincent
Cambon, Gildas
Ramos, Marcel
Astudillo, Orlando
Minnis, Patrick
Ayers, J. Kirk
TI Upwelling response to atmospheric coastal jets off central Chile: A
modeling study of the October 2000 event
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID SEA-SURFACE TEMPERATURE; SUBTROPICAL SOUTH-AMERICA; CALIFORNIA CURRENT
SYSTEM; LOW-LEVEL JET; WIND STRESS; WEST-COAST; EL-NINO; EKMAN
TRANSPORT; BOUNDARY-LAYER; VARIABILITY
AB The spatial and temporal variability of nearshore winds in eastern boundary current systems affect the oceanic heat balance that drives sea surface temperature changes. In this study, regional atmospheric and oceanic simulations are used to document such processes during an atmospheric coastal jet event off central Chile. The event is well reproduced by the atmospheric model and is associated with the migration of an anomalous anticyclone in the southeastern Pacific region during October 2000. A robust feature of the simulation is a sharp coastal wind dropoff, which is insensitive to model resolution. As expected, the simulated oceanic response is a significant sea surface cooling. A surface heat budget analysis shows that vertical mixing is a major contributor to the cooling tendency both in the jet core area and in the nearshore zone where the magnitude of this term is comparable to the magnitude of vertical advection. Sensitivity experiments show that the oceanic response in the coastal area is sensitive to wind dropoff representation. This is because total upwelling, i.e., the sum of coastal upwelling and Ekman pumping, depends on the scale of wind dropoff. Because the latter is much larger than the upwelling scale, coastal wind dropoff has only a weak positive effect on vertical velocities driven by Ekman pumping but has a strong negative effect on coastal upwelling. Interestingly though, the weakening of coastal winds in the dropoff zone has a larger effect on vertical mixing than on vertical advection, with both effects contributing to a reduction of cooling.
C1 [Renault, Lionel] Sistema Observ & Prediccio Costaner Illes Balears, Palma De Mallorca, Spain.
[Ramos, Marcel; Astudillo, Orlando] Univ Catolica Norte, Fac Ciencias Mar, CEAZA, Coquimbo, Chile.
[Ayers, J. Kirk] SSAI, Hampton, VA 23681 USA.
[Dewitte, Boris; Marchesiello, Patrick; Illig, Serena; Cambon, Gildas] IRD, Lab Etud Geophys & Oceanog Spatiale, F-31400 Toulouse 9, France.
[Echevin, Vincent] IRD, Lab Oceanog & Climat Expt & Approches Numer, F-31400 Toulouse 9, France.
[Minnis, Patrick] NASA, Climate Sci Branch, Sci Directorate, Langley Res Ctr, Hampton, VA 23681 USA.
RP Renault, L (reprint author), SOCIB, Parc Bit,Bloc A 2p Pta 3, E-07121 Palma De Mallorca, Spain.
EM lrenault@imedea.uib-csic.es
RI Cambon, Gildas/A-1882-2016; Minnis, Patrick/G-1902-2010;
OI Cambon, Gildas/0000-0002-3899-1204; Minnis, Patrick/0000-0002-4733-6148;
Renault, Lionel/0000-0002-3001-2091; ECHEVIN,
Vincent/0000-0003-3859-840X
FU CNES; NASA; NOAA PACS [NA00AANRG0330]; FONDECYT [1080606]; INNOVA-CHILE
[07CN13 IXM-150]
FX The altimeter products were produced by SSALTO-DUACS and distributed by
AVISO with support from CNES. TMI data are produced by Remote Sensing
Systems and sponsored by the NASA Earth Science REASoN DISCOVER Project.
The QuikSCAT winds were obtained from CERSAT at IFREMER (Plouzane,
France) and Distributed Active Archive Center (PO. DAAC) at the NASA Jet
Propulsion Laboratory. We wish to thank Rene Garreaud and Mark Falvey
for their support in the early stages of this study, Xavier Capet for
helpful discussions, and three anonymous reviewers for their
constructive comments that helped to improve the manuscript. Patrick
Minnis and Kirk Ayers were supported by the NOAA PACS Program under NOAA
agreement NA00AANRG0330 and the NASA Modeling and Analysis Program.
Lionel Renault would like to extend his thanks to Joaquin Tintore and
Guillermo Vizoso as well as the "Sistema d'observacio i
predicciocostaner de les Illes Balears" (SOCIB) for their support during
this study. M. Ramos is grateful for support from FONDECYT grant 1080606
and INNOVA-CHILE (project 07CN13 IXM-150).
NR 76
TC 16
Z9 16
U1 0
U2 11
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 FEB 21
PY 2012
VL 117
AR C02030
DI 10.1029/2011JC007446
PG 21
WC Oceanography
SC Oceanography
GA 899NA
UT WOS:000300821500002
ER
PT J
AU Carter, LM
Neish, CD
Bussey, DBJ
Spudis, PD
Patterson, GW
Cahill, JT
Raney, RK
AF Carter, Lynn M.
Neish, Catherine D.
Bussey, D. B. J.
Spudis, Paul D.
Patterson, G. Wesley
Cahill, Joshua T.
Raney, R. Keith
TI Initial observations of lunar impact melts and ejecta flows with the
Mini-RF radar
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID VENUS; MAGELLAN; CRATERS; STRATIGRAPHY; EMPLACEMENT; MORPHOLOGY;
OUTFLOWS; FLUID
AB The Mini-RF radar on the Lunar Reconnaissance Orbiter spacecraft has revealed a great variety of crater ejecta flow and impact melt deposits, some of which were not observed in prior radar imaging. The craters Tycho and Glushko have long melt flows that exhibit variations in radar backscatter and circular polarization ratio along the flow. Comparison with optical imaging reveals that these changes are caused by features commonly seen in terrestrial lava flows, such as rafted plates, pressure ridges, and ponding. Small (<20 km) sized craters also show a large variety of deposits, including melt flows and ponds. Two craters have flow features that may be ejecta flows caused by entrained debris flowing across the surface rather than by melted rock. The circular polarization ratios (CPRs) of the impact melt flows are typically very high; even ponded areas have CPR values between 0.7 and 1.0. This high CPR suggests that deposits that appear smooth in optical imagery may be rough at centimeter- and decimeter-scales. In some places, ponds and flows are visible with no easily discernable source crater. These melt deposits may have come from oblique impacts that are capable of ejecting melted material farther downrange. They may also be associated with older, nearby craters that no longer have a radar-bright proximal ejecta blanket. The observed morphology of the lunar crater flows has implications for similar features observed on Venus. In particular, changes in backscatter along many of the ejecta flows are probably caused by features typical of lava flows.
C1 [Carter, Lynn M.] NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Neish, Catherine D.; Bussey, D. B. J.; Patterson, G. Wesley; Cahill, Joshua T.; Raney, R. Keith] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Spudis, Paul D.] Lunar & Planetary Inst, Houston, TX 77058 USA.
RP Carter, LM (reprint author), NASA, Planetary Geodynam Lab, Goddard Space Flight Ctr, Code 698, Greenbelt, MD 20771 USA.
EM lynn.m.carter@nasa.gov
RI Carter, Lynn/D-2937-2012; Neish, Catherine/G-6321-2012; Cahill,
Joshua/I-3656-2012
OI Cahill, Joshua/0000-0001-6874-5533
FU NASA LRO [NNX08AM80G]
FX We thank the Mini-RF engineering and operations teams for their work in
building the instrument and acquiring the data. We also thank the LRO
LROC and Kaguya (SELENE) Terrain Camera teams for their efforts to
provide the publicly available data sets used in this work. Thanks to
Veronica Bray and Wenzhe Fa who provided detailed and helpful reviews.
This project was supported through a NASA LRO Participating Scientist
grant (NNX08AM80G) to L. Carter.
NR 30
TC 22
Z9 23
U1 0
U2 6
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 FEB 21
PY 2012
VL 117
AR E00H09
DI 10.1029/2011JE003911
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 899NP
UT WOS:000300823000001
ER
PT J
AU Bahadori, AA
Van Baalen, M
Shavers, MR
Semones, EJ
Bolch, WE
AF Bahadori, Amir A.
Van Baalen, Mary
Shavers, Mark R.
Semones, Edward J.
Bolch, Wesley E.
TI Dosimetric impacts of microgravity: an analysis of 5th, 50th and 95th
percentile male and female astronauts
SO PHYSICS IN MEDICINE AND BIOLOGY
LA English
DT Article
ID RADIATION PROTECTION DOSIMETRY; ADULT VOXEL PHANTOM; BODY-MASS CHANGES;
HUMAN PHYSIOLOGY; SPACE-FLIGHT; BONE; SPACEFLIGHT
AB Computational phantoms serve an important role in organ dosimetry and risk assessment performed at the National Aeronautics and Space Administration (NASA). A previous study investigated the impact on organ dose equivalents and effective doses from the use of the University of Florida hybrid adult male (UFHADM) and adult female (UFHADF) phantoms at differing height and weight percentiles versus those given by the two existing NASA phantoms, the computerized anatomical man (CAM) and female (CAF) (Bahadori et al 2011 Phys. Med. Biol. 56 1671-94). In the present study, the UFHADM and UFHADF phantoms of different body sizes were further altered to incorporate the effects of microgravity. Body self-shielding distributions are generated using the voxel-based ray tracer (VoBRaT), and the results are combined with depth dose data from the NASA codes BRYNTRN and HZETRN to yield organ dose equivalents and their rates for a variety of space radiation environments. It is found that while organ dose equivalents are indeed altered by the physiological effects of microgravity, the magnitude of the change in overall risk (indicated by the effective dose) is minimal for the spectra and simplified shielding configurations considered. The results also indicate, however, that UFHADMand UFHADF could be useful in designing dose reduction strategies through optimized positioning of an astronaut during encounters with solar particle events.
C1 [Bahadori, Amir A.; Bolch, Wesley E.] Univ Florida, Gainesville, FL 32611 USA.
[Bahadori, Amir A.] Univ Houston Downtown, Houston, TX 77002 USA.
[Van Baalen, Mary; Semones, Edward J.] NASA, Johnson Space Ctr, Houston, TX 77058 USA.
[Shavers, Mark R.] Wyle Integrated Sci & Engn, Houston, TX 77058 USA.
RP Bolch, WE (reprint author), Univ Florida, Gainesville, FL 32611 USA.
EM wbolch@ufl.edu
FU NASA GSRP [NNX09AK14H]; NASA Bioastronautics [NAS9-02078]
FX This work was supported by NASA GSRP grant NNX09AK14H and NASA
Bioastronautics Contract NAS9-02078.
NR 32
TC 1
Z9 2
U1 1
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0031-9155
J9 PHYS MED BIOL
JI Phys. Med. Biol.
PD FEB 21
PY 2012
VL 57
IS 4
BP 1047
EP 1070
DI 10.1088/0031-9155/57/4/1047
PG 24
WC Engineering, Biomedical; Radiology, Nuclear Medicine & Medical Imaging
SC Engineering; Radiology, Nuclear Medicine & Medical Imaging
GA 895IV
UT WOS:000300490700013
PM 22298248
ER
PT J
AU Abramowski, A
Acero, F
Aharonian, F
Akhperjanian, AG
Anton, G
Balzer, A
Barnacka, A
de Almeida, UB
Becherini, Y
Becker, J
Behera, B
Bernlohr, K
Birsin, E
Biteau, J
Bochow, A
Boisson, C
Bolmont, J
Bordas, P
Brucker, J
Brun, F
Brun, P
Bulik, T
Busching, I
Carrigan, S
Casanova, S
Cerruti, M
Chadwick, PM
Charbonnier, A
Chaves, RCG
Cheesebrough, A
Clapson, AC
Coignet, G
Cologna, G
Conrad, J
Dalton, M
Daniel, MK
Davids, ID
Degrange, B
Deil, C
Dickinson, HJ
Djannati-Atai, A
Domainko, W
Drury, LO
Dubus, G
Dutson, K
Dyks, J
Dyrda, M
Egberts, K
Eger, P
Espigat, P
Fallon, L
Farnier, C
Fegan, S
Feinstein, F
Fernandes, MV
Fiasson, A
Fontaine, G
Forster, A
Fussling, M
Gallant, YA
Gast, H
Gerard, L
Gerbig, D
Giebels, B
Glicenstein, JF
Gluck, B
Goret, P
Goring, D
Haffner, S
Hague, JD
Hampf, D
Hauser, M
Heinz, S
Heinzelmann, G
Henri, G
Hermann, G
Hinton, JA
Hoffmann, A
Hofmann, W
Hofverberg, P
Holler, M
Horns, D
Jacholkowska, A
de Jager, OC
Jahn, C
Jamrozy, M
Jung, I
Kastendieck, MA
Katarzynski, K
Katz, U
Kaufmann, S
Keogh, D
Khangulyan, D
Khelifi, B
Klochkov, D
Kluzniak, W
Kneiske, T
Komin, N
Kosack, K
Kossakowski, R
Laffon, H
Lamanna, G
Lennarz, D
Lohse, T
Lopatin, A
Lu, CC
Marandon, V
Marcowith, A
Masbou, J
Maurin, D
Maxted, N
Mayer, M
McComb, TJL
Medina, MC
Mehault, J
Moderski, R
Moulin, E
Naumann, CL
Naumann-Godo, M
de Naurois, M
Nedbal, D
Nekrassov, D
Nguyen, N
Nicholas, B
Niemiec, J
Nolan, SJ
Ohm, S
Wilhelmi, ED
Opitz, B
Ostrowski, M
Oya, I
Panter, M
Arribas, MP
Pedaletti, G
Pelletier, G
Petrucci, PO
Pita, S
Puhlhofer, G
Punch, M
Quirrenbach, A
Raue, M
Rayner, SM
Reimer, A
Reimer, O
Renaud, M
de los Reyes, R
Rieger, F
Ripken, J
Rob, L
Rosier-Lees, S
Rowell, G
Rudak, B
Rulten, CB
Ruppel, J
Sahakian, V
Sanchez, DA
Santangelo, A
Schlickeiser, R
Schock, FM
Schulz, A
Schwanke, U
Schwarzburg, S
Schwemmer, S
Sheidaei, F
Skilton, JL
Sol, H
Spengler, G
Stawarz, L
Steenkamp, R
Stegmann, C
Stinzing, F
Stycz, K
Sushch, I
Szostek, A
Tavernet, JP
Terrier, R
Tluczykont, M
Valerius, K
van Eldik, C
Vasileiadis, G
Venter, C
Vialle, JP
Viana, A
Vincent, P
Volk, HJ
Volpe, F
Vorobiov, S
Vorster, M
Wagner, SJ
Ward, M
White, R
Wierzcholska, A
Zacharias, M
Zajczyk, A
Zdziarski, AA
Zech, A
Zechlin, HS
Aleksic, J
Antonelli, LA
Antoranz, P
Backes, M
Barrio, JA
Bastieri, D
Gonzalez, JB
Bednarek, W
Berdyugin, A
Berger, K
Bernardini, E
Biland, A
Blanch, O
Bock, RK
Boller, A
Bonnoli, G
Tridon, DB
Braun, I
Bretz, T
Canellas, A
Carmona, E
Carosi, A
Colin, P
Colombo, E
Contreras, JL
Cortina, J
Cossio, L
Covino, S
Dazzi, F
De Angelis, A
del Pozo, ED
De Lotto, B
Mendez, CD
Ortega, AD
Doert, M
Dominguez, A
Prester, DD
Dorner, D
Doro, M
Elsaesser, D
Ferenc, D
Fonseca, MV
Font, L
Fruck, C
Lopez, RJG
Garczarczyk, M
Garrido, D
Giavitto, G
Godinovic, N
Hadasch, D
Hafner, D
Herrero, A
Hildebrand, D
Hohne-Monch, D
Hose, J
Hrupec, D
Huber, B
Jogler, T
Klepser, S
Krahenbuhl, T
Krause, J
La Barbera, A
Lelas, D
Leonardo, E
Lindfors, E
Lombardi, S
Lopez, M
Lorenz, E
Makariev, M
Maneva, G
Mankuzhiyil, N
Mannheim, K
Maraschi, L
Mariotti, M
Martinez, M
Mazin, D
Meucci, M
Miranda, JM
Mirzoyan, R
Miyamoto, H
Moldon, J
Moralejo, A
Munar, P
Nieto, D
Nilsson, K
Orito, R
Oya, I
Paneque, D
Paoletti, R
Pardo, S
Paredes, JM
Partini, S
Pasanen, M
Pauss, F
Perez-Torres, MA
Persic, M
Peruzzo, L
Pilia, M
Pochon, J
Prada, F
Moroni, PGP
Prandini, E
Puljak, I
Reichardt, I
Reinthal, R
Rhode, W
Ribo, M
Rico, J
Rugamer, S
Saggion, A
Saito, K
Saito, TY
Salvati, M
Satalecka, K
Scalzotto, V
Scapin, V
Schultz, C
Schweizer, T
Shayduk, M
Shore, SN
Sillanpaa, A
Sitarek, J
Sobczynska, D
Spanier, F
Spiro, S
Stamerra, A
Steinke, B
Storz, J
Strah, N
Suric, T
Takalo, L
Takami, H
Tavecchio, F
Temnikov, P
Terzic, T
Tescaro, D
Teshima, M
Thom, M
Tibolla, O
Torres, DF
Treves, A
Vankov, H
Vogler, P
Wagner, RM
Weitzel, Q
Zabalza, V
Zandanel, F
Zanin, R
Arlen, T
Aune, T
Beilicke, M
Benbow, W
Bouvier, A
Bradbury, SM
Buckley, JH
Bugaev, V
Byrum, K
Cannon, A
Cesarini, A
Ciupik, L
Connolly, MP
Cui, W
Dickherber, R
Duke, C
Errando, M
Falcone, A
Finley, JP
Finnegan, G
Fortson, L
Furniss, A
Galante, N
Gall, D
Godambe, S
Griffin, S
Grube, J
Gyuk, G
Hanna, D
Holder, J
Huan, H
Hui, CM
Kaaret, P
Karlsson, N
Kertzman, M
Khassen, Y
Kieda, D
Krawczynski, H
Krennrich, F
Lang, MJ
LeBohec, S
Maier, G
McArthur, S
McCann, A
Moriarty, P
Mukherjee, R
Nunez, PD
Ong, RA
Orr, M
Otte, AN
Park, N
Perkins, JS
Pichel, A
Pohl, M
Prokoph, H
Ragan, K
Reyes, LC
Reynolds, PT
Roache, E
Rose, HJ
Ruppel, J
Schroedter, M
Sembroski, GH
Senturk, GD
Telezhinsky, I
Tesic, G
Theiling, M
Thibadeau, S
Varlotta, A
Vassiliev, VV
Vivier, M
Wakely, SP
Weekes, TC
Williams, DA
Zitzer, B
de Almeida, UB
Cara, M
Casadio, C
Cheung, CC
McConville, W
Davies, F
Doi, A
Giovannini, G
Giroletti, M
Hada, K
Hardee, P
Harris, DE
Junor, W
Kino, M
Lee, NP
Ly, C
Madrid, J
Massaro, F
Mundell, CG
Nagai, H
Perlman, ES
Steele, IA
Walker, RC
Wood, DL
AF Abramowski, A.
Acero, F.
Aharonian, F.
Akhperjanian, A. G.
Anton, G.
Balzer, A.
Barnacka, A.
de Almeida, U. Barres
Becherini, Y.
Becker, J.
Behera, B.
Bernloehr, K.
Birsin, E.
Biteau, J.
Bochow, A.
Boisson, C.
Bolmont, J.
Bordas, P.
Brucker, J.
Brun, F.
Brun, P.
Bulik, T.
Buesching, I.
Carrigan, S.
Casanova, S.
Cerruti, M.
Chadwick, P. M.
Charbonnier, A.
Chaves, R. C. G.
Cheesebrough, A.
Clapson, A. C.
Coignet, G.
Cologna, G.
Conrad, J.
Dalton, M.
Daniel, M. K.
Davids, I. D.
Degrange, B.
Deil, C.
Dickinson, H. J.
Djannati-Atai, A.
Domainko, W.
Drury, L. O'C.
Dubus, G.
Dutson, K.
Dyks, J.
Dyrda, M.
Egberts, K.
Eger, P.
Espigat, P.
Fallon, L.
Farnier, C.
Fegan, S.
Feinstein, F.
Fernandes, M. V.
Fiasson, A.
Fontaine, G.
Foerster, A.
Fuessling, M.
Gallant, Y. A.
Gast, H.
Gerard, L.
Gerbig, D.
Giebels, B.
Glicenstein, J. F.
Glueck, B.
Goret, P.
Goering, D.
Haeffner, S.
Hague, J. D.
Hampf, D.
Hauser, M.
Heinz, S.
Heinzelmann, G.
Henri, G.
Hermann, G.
Hinton, J. A.
Hoffmann, A.
Hofmann, W.
Hofverberg, P.
Holler, M.
Horns, D.
Jacholkowska, A.
de Jager, O. C.
Jahn, C.
Jamrozy, M.
Jung, I.
Kastendieck, M. A.
Katarzynski, K.
Katz, U.
Kaufmann, S.
Keogh, D.
Khangulyan, D.
Khelifi, B.
Klochkov, D.
Kluzniak, W.
Kneiske, T.
Komin, Nu.
Kosack, K.
Kossakowski, R.
Laffon, H.
Lamanna, G.
Lennarz, D.
Lohse, T.
Lopatin, A.
Lu, C. -C.
Marandon, V.
Marcowith, A.
Masbou, J.
Maurin, D.
Maxted, N.
Mayer, M.
McComb, T. J. L.
Medina, M. C.
Mehault, J.
Moderski, R.
Moulin, E.
Naumann, C. L.
Naumann-Godo, M.
de Naurois, M.
Nedbal, D.
Nekrassov, D.
Nguyen, N.
Nicholas, B.
Niemiec, J.
Nolan, S. J.
Ohm, S.
Wilhelmi, E. de Ona
Opitz, B.
Ostrowski, M.
Oya, I.
Panter, M.
Arribas, M. Paz
Pedaletti, G.
Pelletier, G.
Petrucci, P. -O.
Pita, S.
Puehlhofer, G.
Punch, M.
Quirrenbach, A.
Raue, M.
Rayner, S. M.
Reimer, A.
Reimer, O.
Renaud, M.
de los Reyes, R.
Rieger, F.
Ripken, J.
Rob, L.
Rosier-Lees, S.
Rowell, G.
Rudak, B.
Rulten, C. B.
Ruppel, J.
Sahakian, V.
Sanchez, D. A.
Santangelo, A.
Schlickeiser, R.
Schoeck, F. M.
Schulz, A.
Schwanke, U.
Schwarzburg, S.
Schwemmer, S.
Sheidaei, F.
Skilton, J. L.
Sol, H.
Spengler, G.
Stawarz, L.
Steenkamp, R.
Stegmann, C.
Stinzing, F.
Stycz, K.
Sushch, I.
Szostek, A.
Tavernet, J. -P.
Terrier, R.
Tluczykont, M.
Valerius, K.
van Eldik, C.
Vasileiadis, G.
Venter, C.
Vialle, J. P.
Viana, A.
Vincent, P.
Voelk, H. J.
Volpe, F.
Vorobiov, S.
Vorster, M.
Wagner, S. J.
Ward, M.
White, R.
Wierzcholska, A.
Zacharias, M.
Zajczyk, A.
Zdziarski, A. A.
Zech, A.
Zechlin, H. -S.
Aleksic, J.
Antonelli, L. A.
Antoranz, P.
Backes, M.
Barrio, J. A.
Bastieri, D.
Becerra Gonzalez, J.
Bednarek, W.
Berdyugin, A.
Berger, K.
Bernardini, E.
Biland, A.
Blanch, O.
Bock, R. K.
Boller, A.
Bonnoli, G.
Tridon, D. Borla
Braun, I.
Bretz, T.
Canellas, A.
Carmona, E.
Carosi, A.
Colin, P.
Colombo, E.
Contreras, J. L.
Cortina, J.
Cossio, L.
Covino, S.
Dazzi, F.
De Angelis, A.
De Cea del Pozo, E.
De Lotto, B.
Delgado Mendez, C.
Diago Ortega, A.
Doert, M.
Dominguez, A.
Prester, D. Dominis
Dorner, D.
Doro, M.
Elsaesser, D.
Ferenc, D.
Fonseca, M. V.
Font, L.
Fruck, C.
Garcia Lopez, R. J.
Garczarczyk, M.
Garrido, D.
Giavitto, G.
Godinovic, N.
Hadasch, D.
Haefner, D.
Herrero, A.
Hildebrand, D.
Hoehne-Moench, D.
Hose, J.
Hrupec, D.
Huber, B.
Jogler, T.
Klepser, S.
Kraehenbuehl, T.
Krause, J.
La Barbera, A.
Lelas, D.
Leonardo, E.
Lindfors, E.
Lombardi, S.
Lopez, M.
Lorenz, E.
Makariev, M.
Maneva, G.
Mankuzhiyil, N.
Mannheim, K.
Maraschi, L.
Mariotti, M.
Martinez, M.
Mazin, D.
Meucci, M.
Miranda, J. M.
Mirzoyan, R.
Miyamoto, H.
Moldon, J.
Moralejo, A.
Munar, P.
Nieto, D.
Nilsson, K.
Orito, R.
Oya, I.
Paneque, D.
Paoletti, R.
Pardo, S.
Paredes, J. M.
Partini, S.
Pasanen, M.
Pauss, F.
Perez-Torres, M. A.
Persic, M.
Peruzzo, L.
Pilia, M.
Pochon, J.
Prada, F.
Moroni, P. G. Prada
Prandini, E.
Puljak, I.
Reichardt, I.
Reinthal, R.
Rhode, W.
Ribo, M.
Rico, J.
Ruegamer, S.
Saggion, A.
Saito, K.
Saito, T. Y.
Salvati, M.
Satalecka, K.
Scalzotto, V.
Scapin, V.
Schultz, C.
Schweizer, T.
Shayduk, M.
Shore, S. N.
Sillanpaa, A.
Sitarek, J.
Sobczynska, D.
Spanier, F.
Spiro, S.
Stamerra, A.
Steinke, B.
Storz, J.
Strah, N.
Suric, T.
Takalo, L.
Takami, H.
Tavecchio, F.
Temnikov, P.
Terzic, T.
Tescaro, D.
Teshima, M.
Thom, M.
Tibolla, O.
Torres, D. F.
Treves, A.
Vankov, H.
Vogler, P.
Wagner, R. M.
Weitzel, Q.
Zabalza, V.
Zandanel, F.
Zanin, R.
Arlen, T.
Aune, T.
Beilicke, M.
Benbow, W.
Bouvier, A.
Bradbury, S. M.
Buckley, J. H.
Bugaev, V.
Byrum, K.
Cannon, A.
Cesarini, A.
Ciupik, L.
Connolly, M. P.
Cui, W.
Dickherber, R.
Duke, C.
Errando, M.
Falcone, A.
Finley, J. P.
Finnegan, G.
Fortson, L.
Furniss, A.
Galante, N.
Gall, D.
Godambe, S.
Griffin, S.
Grube, J.
Gyuk, G.
Hanna, D.
Holder, J.
Huan, H.
Hui, C. M.
Kaaret, P.
Karlsson, N.
Kertzman, M.
Khassen, Y.
Kieda, D.
Krawczynski, H.
Krennrich, F.
Lang, M. J.
LeBohec, S.
Maier, G.
McArthur, S.
McCann, A.
Moriarty, P.
Mukherjee, R.
Nunez, P. D.
Ong, R. A.
Orr, M.
Otte, A. N.
Park, N.
Perkins, J. S.
Pichel, A.
Pohl, M.
Prokoph, H.
Ragan, K.
Reyes, L. C.
Reynolds, P. T.
Roache, E.
Rose, H. J.
Ruppel, J.
Schroedter, M.
Sembroski, G. H.
Sentuerk, G. D.
Telezhinsky, I.
Tesic, G.
Theiling, M.
Thibadeau, S.
Varlotta, A.
Vassiliev, V. V.
Vivier, M.
Wakely, S. P.
Weekes, T. C.
Williams, D. A.
Zitzer, B.
de Almeida, U. Barres
Cara, M.
Casadio, C.
Cheung, C. C.
McConville, W.
Davies, F.
Doi, A.
Giovannini, G.
Giroletti, M.
Hada, K.
Hardee, P.
Harris, D. E.
Junor, W.
Kino, M.
Lee, N. P.
Ly, C.
Madrid, J.
Massaro, F.
Mundell, C. G.
Nagai, H.
Perlman, E. S.
Steele, I. A.
Walker, R. C.
Wood, D. L.
CA HESS Collaboration
MAGIC Collaboration
VERITAS Collaboration
TI THE 2010 VERY HIGH ENERGY gamma-RAY FLARE AND 10 YEARS OF
MULTI-WAVELENGTH OBSERVATIONS OF M 87
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (M 87); galaxies: jets; galaxies:
nuclei; gamma rays: galaxies; radiation mechanisms: non-thermal
ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; SUPERMASSIVE BLACK-HOLE;
RADIO GALAXY M87; BASE-LINE ARRAY; TEV EMISSION; CRAB-NEBULA; UNIFIED
SCHEMES; SCALE JETS; INNER JET
AB The giant radio galaxy M 87 with its proximity (16 Mpc), famous jet, and very massive black hole ((3-6) x 10(9) M-circle dot) provides a unique opportunity to investigate the origin of very high energy (VHE; E > 100 GeV) gamma-ray emission generated in relativistic outflows and the surroundings of supermassive black holes. M 87 has been established as a VHE gamma-ray emitter since 2006. The VHE gamma-ray emission displays strong variability on timescales as short as a day. In this paper, results from a joint VHE monitoring campaign on M 87 by the MAGIC and VERITAS instruments in 2010 are reported. During the campaign, a flare at VHE was detected triggering further observations at VHE (H.E.S.S.), X-rays (Chandra), and radio (43 GHz Very Long Baseline Array, VLBA). The excellent sampling of the VHE gamma-ray light curve enables one to derive a precise temporal characterization of the flare: the single, isolated flare is well described by a two-sided exponential function with significantly different flux rise and decay times of tau(rise)(d) = (1.69 +/- 0.30) days and tau(decay)(d) = (0.611 +/- 0.080) days, respectively. While the overall variability pattern of the 2010 flare appears somewhat different from that of previous VHE flares in 2005 and 2008, they share very similar timescales (similar to day), peak fluxes (Phi(>0.35 TeV) similar or equal to (1-3) x 10(-11) photons cm(-2) s(-1)), and VHE spectra. VLBA radio observations of 43 GHz of the inner jet regions indicate no enhanced flux in 2010 in contrast to observations in 2008, where an increase of the radio flux of the innermost core regions coincided with a VHE flare. On the other hand, Chandra X-ray observations taken similar to 3 days after the peak of the VHE gamma-ray emission reveal an enhanced flux from the core (flux increased by factor similar to 2; variability timescale <2 days). The long-term (2001-2010) multi-wavelength (MWL) light curve of M 87, spanning from radio to VHE and including data from Hubble Space Telescope, Liverpool Telescope, Very Large Array, and European VLBI Network, is used to further investigate the origin of the VHE gamma-ray emission. No unique, common MWL signature of the three VHE flares has been identified. In the outer kiloparsec jet region, in particular in HST-1, no enhanced MWL activity was detected in 2008 and 2010, disfavoring it as the origin of the VHE flares during these years. Shortly after two of the three flares (2008 and 2010), the X-ray core was observed to be at a higher flux level than its characteristic range (determined from more than 60 monitoring observations: 2002-2009). In 2005, the strong flux dominance of HST-1 could have suppressed the detection of such a feature. Published models for VHE gamma-ray emission from M 87 are reviewed in the light of the new data.
C1 [Abramowski, A.; Fernandes, M. V.; Hampf, D.; Heinzelmann, G.; Horns, D.; Kastendieck, M. A.; Kneiske, T.; Nguyen, N.; Opitz, B.; Raue, M.; Tluczykont, M.; Zechlin, H. -S.] Univ Hamburg, Inst Expt Phys, D-22761 Hamburg, Germany.
[Acero, F.; Farnier, C.; Feinstein, F.; Gallant, Y. A.; Marcowith, A.; Mehault, J.; Renaud, M.; Vasileiadis, G.; Vorobiov, S.; Zajczyk, A.] Univ Montpellier 2, Lab Univers & Particules Montpellier, CNRS IN2P3, CC 72, F-34095 Montpellier 5, France.
[Aharonian, F.; Bernloehr, K.; Bochow, A.; Carrigan, S.; Chaves, R. C. G.; Clapson, A. C.; Deil, C.; Domainko, W.; Foerster, A.; Gast, H.; Hague, J. D.; Hermann, G.; Hofmann, W.; Hofverberg, P.; Khangulyan, D.; Lennarz, D.; Lu, C. -C.; Nekrassov, D.; Ohm, S.; Wilhelmi, E. de Ona; Panter, M.; de los Reyes, R.; Rieger, F.; Sanchez, D. A.; Skilton, J. L.; van Eldik, C.; Voelk, H. J.; Volpe, F.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany.
[Aharonian, F.; Drury, L. O'C.; Fallon, L.] Dublin Inst Adv Studies, Dublin 2, Ireland.
[Aharonian, F.; Akhperjanian, A. G.; Sahakian, V.] Natl Acad Sci Republ Armenia, Yerevan 0019, Armenia.
[Akhperjanian, A. G.; Sahakian, V.] Yerevan Phys Inst, Yerevan 375036, Armenia.
[Anton, G.; Balzer, A.; Brucker, J.; Eger, P.; Glueck, B.; Goering, D.; Haeffner, S.; Heinz, S.; Holler, M.; Jahn, C.; Jung, I.; Katz, U.; Lopatin, A.; Mayer, M.; Schoeck, F. M.; Schulz, A.; Stegmann, C.; Stinzing, F.; Stycz, K.; Valerius, K.] Univ Erlangen Nurnberg, Inst Phys, D-91058 Erlangen, Germany.
[Barnacka, A.; Dyks, J.; Kluzniak, W.; Moderski, R.; Rudak, B.; Zajczyk, A.; Zdziarski, A. A.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
[Barnacka, A.; Brun, P.; Glicenstein, J. F.; Goret, P.; Kosack, K.; Medina, M. C.; Moulin, E.; Naumann-Godo, M.; Viana, A.] CEA Saclay, DSM IRFU, F-91191 Gif Sur Yvette, France.
[de Almeida, U. Barres; Chadwick, P. M.; Cheesebrough, A.; Daniel, M. K.; Keogh, D.; McComb, T. J. L.; Nolan, S. J.; Rayner, S. M.; Rulten, C. B.; Ward, M.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Becherini, Y.; Djannati-Atai, A.; Espigat, P.; Gerard, L.; Marandon, V.; Pita, S.; Punch, M.; Sheidaei, F.; Terrier, R.] Univ Paris 07, CNRS, F-75205 Paris 13, France.
[Becherini, Y.; Biteau, J.; Brun, F.; Degrange, B.; Fegan, S.; Fontaine, G.; Giebels, B.; Khelifi, B.; Laffon, H.; de Naurois, M.] Ecole Polytech, CNRS IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Becker, J.; Buesching, I.; Casanova, S.; Gerbig, D.; Ruppel, J.; Schlickeiser, R.; Zacharias, M.] Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophy 4, D-44780 Bochum, Germany.
[Behera, B.; Cologna, G.; Hauser, M.; Kaufmann, S.; Pedaletti, G.; Quirrenbach, A.; Schwemmer, S.; Wagner, S. J.] Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany.
[Bernloehr, K.; Birsin, E.; Dalton, M.; Fuessling, M.; Lohse, T.; Oya, I.; Arribas, M. Paz; Schwanke, U.; Spengler, G.; Sushch, I.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Boisson, C.; Cerruti, M.; Sol, H.; Zech, A.] Univ Paris Diderot, CNRS, Observ Paris, LUTH, F-92190 Meudon, France.
[Bolmont, J.; Charbonnier, A.; Jacholkowska, A.; Maurin, D.; Naumann, C. L.; Tavernet, J. -P.; Vincent, P.] Univ Paris 07, CNRS IN2P3, Univ Paris 06, LPNHE, F-75252 Paris 5, France.
[Bordas, P.; Hoffmann, A.; Klochkov, D.; Puehlhofer, G.; Santangelo, A.; Schwarzburg, S.] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany.
[Bulik, T.] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland.
[Abramowski, A.; Buesching, I.; de Jager, O. C.; Sheidaei, F.; Venter, C.; Vorster, M.] North West Univ, Unit Space Phys, ZA-2520 Potchefstroom, South Africa.
[Coignet, G.; Fiasson, A.; Komin, Nu.; Kossakowski, R.; Lamanna, G.; Masbou, J.; Rosier-Lees, S.; Vialle, J. P.] Univ Savoie, CNRS IN2P3, Lab Annecy Le Vieux Phys Particules, F-74941 Annecy Le Vieux, France.
[Conrad, J.; Dickinson, H. J.; Ripken, J.] Stockholm Univ, Dept Phys, Oskar Klein Ctr, Albanova Univ Ctr, SE-10691 Stockholm, Sweden.
[Davids, I. D.; Steenkamp, R.] Univ Namibia, Dept Phys, Windhoek, Namibia.
[Dubus, G.; Henri, G.; Pelletier, G.; Petrucci, P. -O.] Univ Grenoble 1, INSU CNRS, Lab Astrophys Grenoble, F-38041 Grenoble 9, France.
[Dutson, K.; Hinton, J. A.; Ohm, S.; White, R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Dyrda, M.; Niemiec, J.] Inst Fizyki Jadrowej PAN, PL-31342 Krakow, Poland.
[Egberts, K.; Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Jamrozy, M.; Ostrowski, M.; Stawarz, L.; Szostek, A.; Wierzcholska, A.] Uniwersytet Jagiellonski, Obserwatorium Astronomiczne, PL-30244 Krakow, Poland.
[Katarzynski, K.] Nicholas Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland.
[Maxted, N.; Nicholas, B.; Rowell, G.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia.
[Nedbal, D.; Rob, L.] Charles Univ Prague, Fac Math & Phys, Inst Particle & Nucl Phys, CR-18000 Prague 8, Czech Republic.
[Ohm, S.; Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Aleksic, J.; Blanch, O.; Cortina, J.; Giavitto, G.; Klepser, S.; Martinez, M.; Mazin, D.; Moralejo, A.; Perez-Torres, M. A.; Reichardt, I.; Zanin, R.] IFAE, E-08193 Bellaterra, Spain.
[Antonelli, L. A.; Bonnoli, G.; Carosi, A.; Covino, S.; La Barbera, A.; Maraschi, L.; Salvati, M.; Spiro, S.; Tavecchio, F.] INAF Natl Inst Astrophys, I-00136 Rome, Italy.
[Antoranz, P.; Leonardo, E.; Meucci, M.; Miranda, J. M.; Paoletti, R.; Partini, S.; Stamerra, A.] Univ Siena, Dipartimento Fis, I-53100 Siena, Italy.
[Antoranz, P.; Leonardo, E.; Meucci, M.; Miranda, J. M.; Paoletti, R.; Partini, S.; Stamerra, A.] INFN Pisa, I-53100 Siena, Italy.
[Backes, M.; Doert, M.; Rhode, W.; Strah, N.; Thom, M.] Tech Univ Dortmund, Fak Phys, D-44221 Dortmund, Germany.
[Barrio, J. A.; Contreras, J. L.; Fonseca, M. V.; Lopez, M.; Nieto, D.; Oya, I.; Pardo, S.; Scapin, V.] Univ Complutense, Grp Fis Altas Energias, E-28040 Madrid, Spain.
[Bastieri, D.; Lombardi, S.; Mariotti, M.; Peruzzo, L.; Prandini, E.; Saggion, A.; Scalzotto, V.; Schultz, C.] Univ Padua, Dipartimento Fis, I-35131 Padua, Italy.
[Bastieri, D.; Lombardi, S.; Mariotti, M.; Peruzzo, L.; Prandini, E.; Saggion, A.; Scalzotto, V.; Schultz, C.] INFN, I-35131 Padua, Italy.
[Becerra Gonzalez, J.; Berger, K.; Colombo, E.; Delgado Mendez, C.; Diago Ortega, A.; Garcia Lopez, R. J.; Garczarczyk, M.; Herrero, A.; Pochon, J.] Inst Astrofis Canarias, E-38200 Tenerife, Spain.
[Bednarek, W.; Sitarek, J.; Sobczynska, D.] Univ Lodz, Dept Astrophys, PL-90236 Lodz, Poland.
[Berdyugin, A.; Lindfors, E.; Nilsson, K.; Pasanen, M.; Reinthal, R.; Sillanpaa, A.; Takalo, L.] Univ Turku, Tuorla Observ, FI-21500 Piikkio, Finland.
[Bernardini, E.; Satalecka, K.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Biland, A.; Boller, A.; Braun, I.; Dorner, D.; Hildebrand, D.; Huber, B.; Kraehenbuehl, T.; Lorenz, E.; Pauss, F.; Vogler, P.; Weitzel, Q.] Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland.
[Bock, R. K.; Tridon, D. Borla; Carmona, E.; Colin, P.; Fruck, C.; Haefner, D.; Hose, J.; Jogler, T.; Krause, J.; Mirzoyan, R.; Miyamoto, H.; Orito, R.; Paneque, D.; Saito, K.; Saito, T. Y.; Schweizer, T.; Shayduk, M.; Steinke, B.; Takami, H.; Teshima, M.; Wagner, R. M.; de Almeida, U. Barres] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Bretz, T.; Elsaesser, D.; Hoehne-Moench, D.; Mannheim, K.; Ruegamer, S.; Spanier, F.; Storz, J.; Tibolla, O.] Univ Wurzburg, Fak Phys & Astron, D-97074 Wurzburg, Germany.
[Canellas, A.; Moldon, J.; Munar, P.; Paredes, J. M.; Ribo, M.; Zabalza, V.] Univ Barcelona ICC IEEC, Fac Fis, E-08028 Barcelona, Spain.
[Cossio, L.; Dazzi, F.; De Angelis, A.; De Lotto, B.; Mankuzhiyil, N.; Persic, M.] Univ Udine, Dipartimento Fis Sperimentale, I-33100 Udine, Italy.
[Cossio, L.; Dazzi, F.; De Angelis, A.; De Lotto, B.; Mankuzhiyil, N.; Persic, M.] INFN Trieste, I-33100 Udine, Italy.
[De Cea del Pozo, E.; Hadasch, D.] Inst Ciencies Espai IEEC CSIC, E-08193 Barcelona, Spain.
[Dominguez, A.; Prada, F.; Zandanel, F.; Casadio, C.] Inst Astrofis Andalucia CSIC, E-18080 Granada, Spain.
[Prester, D. Dominis; Ferenc, D.; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Suric, T.; Terzic, T.] Univ Rijeka, Inst R Boskovic, Croatian MAGIC Consortium, HR-10000 Zagreb, Croatia.
[Prester, D. Dominis; Ferenc, D.; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Suric, T.; Terzic, T.] Univ Split, HR-10000 Zagreb, Croatia.
[Doro, M.; Font, L.; Garrido, D.] Univ Autonoma Barcelona, Fac Fis, E-08193 Bellaterra, Spain.
[Makariev, M.; Maneva, G.; Temnikov, P.; Vankov, H.] Inst Nucl Energy Res, BG-1784 Sofia, Bulgaria.
[Pilia, M.; Treves, A.] Univ Insubria, Dipartimento Fis, I-22100 Como, Italy.
[Moroni, P. G. Prada; Shore, S. N.; Tescaro, D.] Univ Pisa, Dipartimento Fis, I-56126 Pisa, Italy.
[Moroni, P. G. Prada; Shore, S. N.; Tescaro, D.] INFN Pisa, I-56126 Pisa, Italy.
[Rico, J.; Torres, D. F.] ICREA, E-08010 Barcelona, Spain.
[Ong, R. A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Aune, T.; Bouvier, A.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Aune, T.; Bouvier, A.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Benbow, W.; Galante, N.; Roache, E.; Schroedter, M.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Byrum, K.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Cannon, A.; Khassen, Y.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Cesarini, A.; Connolly, M. P.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland.
[Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Cui, W.; Finley, J. P.; Sembroski, G. H.; Varlotta, A.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA.
[Errando, M.; Mukherjee, R.; Sentuerk, G. D.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Finnegan, G.; Godambe, S.; Hui, C. M.; Kieda, D.; LeBohec, S.; Nunez, P. D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Fortson, L.; Karlsson, N.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Gall, D.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Griffin, S.; Hanna, D.; McCann, A.; Ragan, K.; Tesic, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Holder, J.; Vivier, M.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Holder, J.; Vivier, M.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Huan, H.; Park, N.; Reyes, L. C.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Kertzman, M.] DePauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[Krennrich, F.; Orr, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Maier, G.; Pohl, M.; Prokoph, H.; Ruppel, J.; Telezhinsky, I.] DESY, D-15738 Zeuthen, Germany.
[Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland.
[Perkins, J. S.] CRESST, Greenbelt, MD 20771 USA.
[Perkins, J. S.] Astroparticle Phys Lab NASA GSFC, Greenbelt, MD 20771 USA.
[Perkins, J. S.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA.
[Pichel, A.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina.
[Pohl, M.; Ruppel, J.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland.
[Cara, M.; Perlman, E. S.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA.
[Casadio, C.; Giovannini, G.; Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Cheung, C. C.] Natl Acad Sci, Washington, DC 20001 USA.
[McConville, W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[McConville, W.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McConville, W.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Davies, F.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Doi, A.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan.
[Giovannini, G.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Hada, K.] Grad Univ Adv Studies SOKENDAI, Mitaka, Tokyo 1818588, Japan.
[Hada, K.; Kino, M.; Nagai, H.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Hardee, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Harris, D. E.; Lee, N. P.; Massaro, F.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Junor, W.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Ly, C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Madrid, J.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Mundell, C. G.; Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5UX, Merseyside, England.
[Walker, R. C.] Natl Radio Astron Observ NRAO, Socorro, NM 87801 USA.
[Wood, D. L.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
RP Abramowski, A (reprint author), Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany.
EM martin.raue@desy.de; stawarz@astro.isas.jaxa.jp; colin@mppmu.mpg.de;
mazin@ifae.es; beilicke@physics.wustl.edu; cmhui@physics.utah.edu
RI Font, Lluis/L-4197-2014; Contreras Gonzalez, Jose Luis/K-7255-2014;
Maneva, Galina/L-7120-2016; Temnikov, Petar/L-6999-2016; Massaro,
Francesco/L-9102-2016; Makariev, Martin/M-2122-2016; Torres,
Diego/O-9422-2016; Drury, Luke/B-1916-2017; Barrio, Juan/L-3227-2014;
Moulin, Emmanuel/B-5959-2017; Martinez Rodriguez, Manel/C-2539-2017;
Cortina, Juan/C-2783-2017; Lopez Moya, Marcos/L-2304-2014; Moralejo
Olaizola, Abelardo/M-2916-2014; Ribo, Marc/B-3579-2015; Katarzynski,
Krzysztof/G-4528-2014; Jamrozy, Marek/F-4507-2015; Casanova,
Sabrina/J-8935-2013; Antoranz, Pedro/H-5095-2015; Anton,
Gisela/C-4840-2013; Khassen, Yerbol/I-3806-2015; Delgado,
Carlos/K-7587-2014; Nieto, Daniel/J-7250-2015; Miranda, Jose
Miguel/F-2913-2013; Daniel, Michael/A-2903-2010; Braun,
Isabel/C-9373-2012; Prada Moroni, Pier Giorgio/G-5565-2011; Mannheim,
Karl/F-6705-2012; Reimer, Olaf/A-3117-2013; van Eldik,
Christopher/C-3901-2013; Katz, Uli/E-1925-2013; Cara, Mihai/G-1023-2013;
Tjus, Julia/G-8145-2012; Fontaine, Gerard/D-6420-2014; Venter,
Christo/E-6884-2011; Rico, Javier/K-8004-2014; Fernandez,
Ester/K-9734-2014; Komin, Nukri/J-6781-2015; Fonseca Gonzalez, Maria
Victoria/I-2004-2015; Backes, Michael/N-5126-2016; Reichardt,
Ignasi/P-7478-2016
OI Giovannini, Gabriele/0000-0003-4916-6362; Prada Moroni, Pier
Giorgio/0000-0001-9712-9916; Chadwick, Paula/0000-0002-1468-2685;
Kneiske, Tanja M./0000-0002-3210-6200; LA BARBERA,
ANTONINO/0000-0002-5880-8913; Font, Lluis/0000-0003-2109-5961; Contreras
Gonzalez, Jose Luis/0000-0001-7282-2394; Temnikov,
Petar/0000-0002-9559-3384; Massaro, Francesco/0000-0002-1704-9850;
Torres, Diego/0000-0002-1522-9065; Drury, Luke/0000-0002-9257-2270;
Barrio, Juan/0000-0002-0965-0259; Moulin, Emmanuel/0000-0003-4007-0145;
Cortina, Juan/0000-0003-4576-0452; Cui, Wei/0000-0002-6324-5772; Lopez
Moya, Marcos/0000-0002-8791-7908; Moralejo Olaizola,
Abelardo/0000-0002-1344-9080; Casanova, Sabrina/0000-0002-6144-9122;
Antoranz, Pedro/0000-0002-3015-3601; Anton, Gisela/0000-0003-2039-4724;
Khassen, Yerbol/0000-0002-7296-3100; Delgado,
Carlos/0000-0002-7014-4101; Nieto, Daniel/0000-0003-3343-0755; Miranda,
Jose Miguel/0000-0002-1472-9690; Daniel, Michael/0000-0002-8053-7910;
Braun, Isabel/0000-0002-9389-0502; Reimer, Olaf/0000-0001-6953-1385; van
Eldik, Christopher/0000-0001-9669-645X; Katz, Uli/0000-0002-7063-4418;
Venter, Christo/0000-0002-2666-4812; Rico, Javier/0000-0003-4137-1134;
Cesarini, Andrea/0000-0002-8611-8610; leonardo,
elvira/0000-0003-0271-7673; de los Reyes Lopez,
Raquel/0000-0003-0485-9552; Komin, Nukri/0000-0003-3280-0582; De Lotto,
Barbara/0000-0003-3624-4480; Fonseca Gonzalez, Maria
Victoria/0000-0003-2235-0725; Backes, Michael/0000-0002-9326-6400;
Reichardt, Ignasi/0000-0003-3694-3820
FU Namibian authorities; German Ministry for Education and Research (BMBF);
Max Planck Society; French Ministry for Research; CNRS-IN2P3; CNRS; U.K.
Science and Technology Facilities Council (STFC); IPNP of the Charles
University; Polish Ministry of Science and Higher Education; South
African Department of Science and Technology; National Research
Foundation; University of Namibia; German BMBF; German MPG; Italian
INFN; Swiss National Fund SNF; Spanish MICINN; Bulgarian NSF
[CSD2007-00042, CSD2009-00064, DO02-353]; Academy of Finland [127740];
YIP of the Helmholtz Gemeinschaft; DFG Cluster of Excellence "Origin and
Structure of the Universe,"; DFG Collaborative Research Centers
[SFB823/C4, SFB876/C3]; Polish MNiSzW [745/N-HESS-MAGIC/2010/0]; US
Department of Energy Office of Science; US National Science Foundation;
Smithsonian Institution; NSERC in Canada; Science Foundation Ireland
(SFI) [10/RFP/AST2748]; STFC in the UK; Istituto Nazionale di
Astrofisica in Italy; Centre National d'Etudes Spatiales in France; NASA
[GO0-11120X]; Associated Universities, Inc.; European Community [227290]
FX The H.E.S.S. Collaboration acknowledges support of the Namibian
authorities and of the University of Namibia in facilitating the
construction and operation of H.E.S.S., as is the support by the German
Ministry for Education and Research (BMBF), the Max Planck Society, the
French Ministry for Research, the CNRS-IN2P3 and the Astroparticle
Interdisciplinary Programme of the CNRS, the U.K. Science and Technology
Facilities Council (STFC), the IPNP of the Charles University, the
Polish Ministry of Science and Higher Education, the South African
Department of Science and Technology and National Research Foundation,
and by the University of Namibia. We appreciate the excellent work of
the technical support staff in Berlin, Durham, Hamburg, Heidelberg,
Palaiseau, Paris, Saclay, and in Namibia in the construction and
operation of the equipment.; The MAGIC Collaboration thank the Instituto
de Astrofisica de Canarias for the excellent working conditions at the
Observatorio del Roque de los Muchachos in La Palma. The support of the
German BMBF and MPG, the Italian INFN, the Swiss National Fund SNF, and
the Spanish MICINN is gratefully acknowledged. This work was also
supported by the Marie Curie program, by the CPAN CSD2007-00042 and
MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010
programme, by grant DO02-353 of the Bulgarian NSF, by grant 127740 of
the Academy of Finland, by the YIP of the Helmholtz Gemeinschaft, by the
DFG Cluster of Excellence "Origin and Structure of the Universe," by the
DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the
Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0.; The VERITAS Collaboration
acknowledges support from the US Department of Energy Office of Science,
the US National Science Foundation, and the Smithsonian Institution,
from NSERC in Canada, from Science Foundation Ireland (SFI
10/RFP/AST2748), and from STFC in the UK. We acknowledge the excellent
work of the technical support staff at the FLWO and at the collaborating
institutions in the construction and operation of the instrument.; The
Fermi LAT Collaboration acknowledges generous ongoing support from a
number of agencies and institutes that have supported both the
development and the operation of the LAT as well as scientific data
analysis. These include the National Aeronautics and Space
Administration and the Department of Energy in the United States, the
Commissariat a l'Energie Atomique and the Centre National de la
Recherche Scientifique/Institut National de Physique Nucleaire et de
Physique des Particules in France, the Agenzia Spaziale Italiana and the
Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of
Education, Culture, Sports, Science and Technology (MEXT), High Energy
Accelerator Research Organization (KEK) and Japan Aerospace Exploration
Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish
Research Council and the Swedish National Space Board in Sweden.
Additional support for science analysis during the operations phase is
gratefully acknowledged from the Istituto Nazionale di Astrofisica in
Italy and the Centre National d'Etudes Spatiales in France.; Analysis of
the Chandra data was supported by NASA grant GO0-11120X.; The Very Long
Baseline Array is operated by the National Radio Astronomy Observatory,
a facility of the NSF, operated under cooperative agreement by
Associated Universities, Inc.; The European VLBI Network is a joint
facility of European, Chinese, South African, and other radio astronomy
institutes funded by their national research councils. This effort is
supported by the European Community Framework Programme 7, Advanced
Radio Astronomy in Europe, grant agreement no. 227290.
NR 107
TC 59
Z9 61
U1 3
U2 42
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 FEB 20
PY 2012
VL 746
IS 2
AR 151
DI 10.1088/0004-637X/746/2/151
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 894DD
UT WOS:000300406300037
ER
PT J
AU Howell, SB
Rowe, JF
Bryson, ST
Quinn, SN
Marcy, GW
Isaacson, H
Ciardi, DR
Chaplin, WJ
Metcalfe, TS
Monteiro, MJPFG
Appourchaux, T
Basu, S
Creevey, OL
Gilliland, RL
Quirion, PO
Stello, D
Kjeldsen, H
Christensen-Dalsgaard, J
Elsworth, Y
Garcia, RA
Houdek, G
Karoff, C
Molenda-Zakowicz, J
Thompson, MJ
Verner, GA
Torres, G
Fressin, F
Crepp, JR
Adams, E
Dupree, A
Sasselov, DD
Dressing, CD
Borucki, WJ
Koch, DG
Lissauer, JJ
Latham, DW
Buchhave, LA
Gautier, TN
Everett, M
Horch, E
Batalha, NM
Dunham, EW
Szkody, P
Silva, DR
Mighell, K
Holberg, J
Ballot, J
Bedding, TR
Bruntt, H
Campante, TL
Handberg, R
Hekker, S
Huber, D
Mathur, S
Mosser, B
Regulo, C
White, TR
Christiansen, JL
Middour, CK
Haas, MR
Hall, JR
Jenkins, JM
McCaulif, S
Fanelli, MN
Kulesa, C
McCarthy, D
Henze, CE
AF Howell, Steve B.
Rowe, Jason F.
Bryson, Stephen T.
Quinn, Samuel N.
Marcy, Geoffrey W.
Isaacson, Howard
Ciardi, David R.
Chaplin, William J.
Metcalfe, Travis S.
Monteiro, Mario J. P. F. G.
Appourchaux, Thierry
Basu, Sarbani
Creevey, Orlagh L.
Gilliland, Ronald L.
Quirion, Pierre-Olivier
Stello, Denis
Kjeldsen, Hans
Christensen-Dalsgaard, Jorgen
Elsworth, Yvonne
Garcia, Rafael A.
Houdek, Guenter
Karoff, Christoffer
Molenda-Zakowicz, Joanna
Thompson, Michael J.
Verner, Graham A.
Torres, Guillermo
Fressin, Francois
Crepp, Justin R.
Adams, Elisabeth
Dupree, Andrea
Sasselov, Dimitar D.
Dressing, Courtney D.
Borucki, William J.
Koch, David G.
Lissauer, Jack J.
Latham, David W.
Buchhave, Lars A.
Gautier, Thomas N., III
Everett, Mark
Horch, Elliott
Batalha, Natalie M.
Dunham, Edward W.
Szkody, Paula
Silva, David R.
Mighell, Ken
Holberg, Jay
Ballot, Jerome
Bedding, Timothy R.
Bruntt, Hans
Campante, Tiago L.
Handberg, Rasmus
Hekker, Saskia
Huber, Daniel
Mathur, Savita
Mosser, Benoit
Regulo, Clara
White, Timothy R.
Christiansen, Jessie L.
Middour, Christopher K.
Haas, Michael R.
Hall, Jennifer R.
Jenkins, Jon M.
McCaulif, Sean
Fanelli, Michael N.
Kulesa, Craig
McCarthy, Don
Henze, Christopher E.
TI KEPLER-21b: A 1.6 R-Earth PLANET TRANSITING THE BRIGHT OSCILLATING F
SUBGIANT STAR HD 179070
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: activity; stars: individual (HD 179070: KIC
3632418); stars: interiors; stars: late-type; stars: magnetic field;
stars: oscillations (including pulsations); techniques: photometric
ID SOLAR-TYPE STARS; SUN-LIKE STAR; TIMING VARIATIONS; INITIAL
CHARACTERISTICS; ASTEROSEISMIC DATA; BLEND SCENARIOS; MULTIPLE SYSTEM;
LIGHT CURVES; SUPER-EARTHS; CADENCE DATA
AB We present Kepler observations of the bright (V = 8.3), oscillating star HD 179070. The observations show transit-like events which reveal that the star is orbited every 2.8 days by a small, 1.6 R-Earth object. Seismic studies of HD 179070 using short cadence Kepler observations show that HD 179070 has a frequency-power spectrum consistent with solar-like oscillations that are acoustic p-modes. Asteroseismic analysis provides robust values for the mass and radius of HD 179070, 1.34 +/- 0.06 M-circle dot and 1.86 +/- 0.04 R-circle dot, respectively, as well as yielding an age of 2.84 +/- 0.34 Gyr for this F5 subgiant. Together with ground-based follow-up observations, analysis of the Kepler light curves and image data, and blend scenario models, we conservatively show at the >99.7% confidence level (3 sigma) that the transit event is caused by a 1.64 +/- 0.04 R-Earth exoplanet in a 2.785755 +/- 0.000032 day orbit. The exoplanet is only 0.04 AU away from the star and our spectroscopic observations provide an upper limit to its mass of similar to 10 M-Earth (2 sigma). HD 179070 is the brightest exoplanet host star yet discovered by Kepler.
C1 [Howell, Steve B.; Everett, Mark; Silva, David R.; Mighell, Ken] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Middour, Christopher K.; Hall, Jennifer R.; McCaulif, Sean] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
[Fanelli, Michael N.] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
[Rowe, Jason F.; Christiansen, Jessie L.; Jenkins, Jon M.] SETI Inst, Mountain View, CA 94043 USA.
[Quinn, Samuel N.; Torres, Guillermo; Fressin, Francois; Adams, Elisabeth; Dupree, Andrea; Sasselov, Dimitar D.; Dressing, Courtney D.; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Marcy, Geoffrey W.; Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Chaplin, William J.; Elsworth, Yvonne; Karoff, Christoffer; Verner, Graham A.; Hekker, Saskia] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Metcalfe, Travis S.; Thompson, Michael J.; Mathur, Savita] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Metcalfe, Travis S.; Thompson, Michael J.; Mathur, Savita] Natl Ctr Atmospher Res, Div Comp Sci, Boulder, CO 80307 USA.
[Monteiro, Mario J. P. F. G.; Campante, Tiago L.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Appourchaux, Thierry] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR8617, F-91405 Orsay, France.
[Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Creevey, Orlagh L.; Bruntt, Hans; Regulo, Clara] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Creevey, Orlagh L.; Regulo, Clara] Inst Astrofis Canarias, E-38200 Tenerife, Spain.
[Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Quirion, Pierre-Olivier] Canadian Space Agcy, St Hubert, PQ J3Y 8Y9, Canada.
[Stello, Denis; Bedding, Timothy R.; Huber, Daniel; White, Timothy R.] Univ Sydney, Sydney Inst Astron SIfA, Sch Phys, Sydney, NSW 2006, Australia.
[Kjeldsen, Hans; Christensen-Dalsgaard, Jorgen; Campante, Tiago L.; Handberg, Rasmus] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Garcia, Rafael A.] Univ Paris Diderot, Lab AIM, CEA, DSM,CNRS,IRFU,SAp, F-91191 Gif Sur Yvette, France.
[Houdek, Guenter] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Molenda-Zakowicz, Joanna] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland.
[Verner, Graham A.] Univ London, Astron Unit, London E1 4NS, England.
[Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Crepp, Justin R.] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA.
[Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Horch, Elliott] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA.
[Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
[Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Szkody, Paula] Univ Washington, Dept Astron, Seattle, WA USA.
[Holberg, Jay] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85726 USA.
[Ballot, Jerome] Univ Toulouse, Lab Astrophys Toulouse Tarbes, CNRS, F-31400 Toulouse, France.
[Mosser, Benoit] Univ Paris 07, Univ Paris 06, LESIA, CNRS,Observ Paris, F-92195 Meudon, France.
[Kulesa, Craig; McCarthy, Don] Univ Arizona, Steward Observ, Tucson, AZ 85726 USA.
[Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark.
RP Howell, SB (reprint author), Natl Opt Astron Observ, Tucson, AZ 85719 USA.
RI Ballot, Jerome/G-1019-2010; Monteiro, Mario J.P.F.G./B-4715-2008;
Karoff, Christoffer/L-1007-2013;
OI Monteiro, Mario J.P.F.G./0000-0003-0513-8116; Karoff,
Christoffer/0000-0003-2009-7965; Buchhave, Lars A./0000-0003-1605-5666;
Bedding, Timothy/0000-0001-5943-1460; Basu, Sarbani/0000-0002-6163-3472
FU National Aeronautics and Space Administration
FX We thank John Johnson for use of some of his Keck Time. This research
has made use of the NASA/IPAC/NExScI Star and Exoplanet Database, which
is operated by the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration. The authors thank the Kepler Science Office and the
Science Operations Center personal for their dedicated effort to the
mission and for providing us access to the science office data products.
The ground-based observations reported on herein were obtained at Kitt
Peak National Observatory, National Optical Astronomy Observatory, which
is operated by the Association of Universities for Research in Astronomy
(AURA) under cooperative agreement with the National Science Foundation.
Kepler was selected as the 10th mission of the Discovery Program.
Funding for this mission is provided by NASA.
NR 90
TC 73
Z9 73
U1 1
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 FEB 20
PY 2012
VL 746
IS 2
AR 123
DI 10.1088/0004-637X/746/2/123
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 894DD
UT WOS:000300406300009
ER
PT J
AU Hwang, U
Laming, JM
AF Hwang, Una
Laming, J. Martin
TI A CHANDRA X-RAY SURVEY OF EJECTA IN THE CASSIOPEIA A SUPERNOVA REMNANT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE hydrodynamics; ISM: individual objects (Cassiopeia A); ISM: supernova
remnants; X-rays: ISM
ID CORE-COLLAPSE SUPERNOVAE; ISOLATED RADIO PULSARS; A SUPERNOVA;
NEUTRON-STAR; 3-DIMENSIONAL STRUCTURE; ACCELERATED ELECTRONS; GAMMA-RAY;
CAS-A; INTERSTELLAR-MEDIUM; DRIVEN SUPERNOVA
AB We present a survey of the X-ray-emitting ejecta in the Cassiopeia A supernova remnant (SNR) based on an extensive analysis of over 6000 spectral regions extracted on 2.'' 5-10 '' angular scales using the Chandra 1 Ms observation. We interpret these results in the context of hydrodynamical models for the evolution of the remnant. The distributions of fitted temperature and ionization age, and the implied mass coordinates, are highly peaked and suggest that the ejecta were subjected to multiple secondary shocks following reverse shock interaction with ejecta inhomogeneities. Based on the fitted emission measure and element abundances, and an estimate of the emitting volume, we derive masses for the X-ray-emitting ejecta and also show the distribution of the mass of various elements over the remnant. An upper limit to the total shocked Fe mass visible in X-rays appears to be roughly 0.13 M-circle dot, which accounts for nearly all of the mass expected in Fe ejecta. We find two populations of Fe ejecta, that associated with normal Si burning and that possibly associated with alpha-rich freezeout, with a mass ratio of approximately 2:1. Essentially all of the observed Fe (both components) lies well outside the central regions of the SNR, possibly having been ejected by hydrodynamic instabilities during the explosion. We discuss this and its implications for the neutron star kick.
C1 [Hwang, Una] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hwang, Una] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21210 USA.
[Laming, J. Martin] USN, Res Lab, Washington, DC 20375 USA.
RP Hwang, U (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Una.Hwang-1@gsfc.nasa.gov; laming@nrl.navy.mil
FU NASA [NNH04ZSS001N]; Office of Naval Research
FX We thank Roger Chevalier, Elisabetta Micelotta, Rob Petre, and the
referee for helpful comments on the paper. We gratefully acknowledge
support through NASA grants to the Chandra Guest Observer Program and
NNH04ZSS001N to the Long Term Space Astrophysics Program. J.M.L. was
also supported by basic research funds of the Office of Naval Research.
NR 109
TC 68
Z9 68
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 FEB 20
PY 2012
VL 746
IS 2
AR 130
DI 10.1088/0004-637X/746/2/130
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 894DD
UT WOS:000300406300016
ER
PT J
AU Kim, RS
Gopalswamy, N
Moon, YJ
Cho, KS
Yashiro, S
AF Kim, R. -S.
Gopalswamy, N.
Moon, Y. -J.
Cho, K. -S.
Yashiro, S.
TI MAGNETIC FIELD STRENGTH IN THE UPPER SOLAR CORONA USING WHITE-LIGHT
SHOCK STRUCTURES SURROUNDING CORONAL MASS EJECTIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetic fields; methods: statistical; shock waves; Sun: corona; Sun:
coronal mass ejections
ID FARADAY-ROTATION MEASUREMENTS; STANDOFF DISTANCE; ELECTRON-DENSITY;
DRIVEN SHOCK; RADIO-BURSTS; LARGE-ANGLE; II BURSTS; WAVES; SDO/AIA;
ORIGIN
AB To measure the magnetic field strength in the solar corona, we examined 10 fast (>= 1000 km s(-1)) limb coronal mass ejections(CMEs) that show clear shock structures in Solar and Heliospheric Observatory/Large Angle and Spectrometric Coronagraph images. By applying the piston-shock relationship to the observed CME's standoff distance and electron density compression ratio, we estimated the Mach number, Alfven speed, and magnetic field strength in the height range 3-15 solar radii (R-s). The main results from this study are as follows: (1) the standoff distance observed in the solar corona is consistent with those from a magnetohydrodynamic model and near-Earth observations; (2) the Mach number as a shock strength is in the range 1.49-3.43 from the standoff distance ratio, but when we use the density compression ratio, the Mach number is in the range 1.47-1.90, implying that the measured density compression ratio is likely to be underestimated owing to observational limits; (3) the Alfven speed ranges from 259 to 982 km s(-1) and the magnetic field strength is in the range 6-105 mG when the standoff distance is used; (4) if we multiply the density compression ratio by a factor of two, the Alfven speeds and the magnetic field strengths are consistent in both methods; and (5) the magnetic field strengths derived from the shock parameters are similar to those of empirical models and previous estimates.
C1 [Kim, R. -S.; Gopalswamy, N.; Cho, K. -S.; Yashiro, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Moon, Y. -J.] Kyung Hee Univ, Sch Space Res, Yongin 446701, South Korea.
RP Kim, RS (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
EM rok-soon.kim@nasa.gov
RI Gopalswamy, Nat/D-3659-2012; Moon, Yong-Jae/E-1711-2013;
OI Gopalswamy, Nat/0000-0001-5894-9954
FU WCU [R31-10016]; National Research Foundation of Korea [20090071744,
20100014501]; Ministry of Education, Science and Technology; Development
of Korean Space Weather Center; KASI
FX Y.-J.M. has been supported by the WCU program (No. R31-10016) and Basic
Research Promotion Fund (20090071744 and 20100014501) through the
National Research Foundation of Korea funded by the Ministry of
Education, Science and Technology. K.-S.C. is supported by the
Development of Korean Space Weather Center, a project of KASI, and the
KASI basic research fund.
NR 53
TC 24
Z9 24
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 FEB 20
PY 2012
VL 746
IS 2
AR 118
DI 10.1088/0004-637X/746/2/118
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 894DD
UT WOS:000300406300004
ER
PT J
AU Ragland, S
Ohnaka, K
Hillenbrand, L
Ridgway, ST
Colavita, MM
Akeson, RL
Cotton, W
Danchi, WC
Hrynevich, M
Millan-Gabet, R
Traub, WA
AF Ragland, S.
Ohnaka, K.
Hillenbrand, L.
Ridgway, S. T.
Colavita, M. M.
Akeson, R. L.
Cotton, W.
Danchi, W. C.
Hrynevich, M.
Millan-Gabet, R.
Traub, W. A.
TI FIRST KECK NULLING OBSERVATIONS OF A YOUNG STELLAR OBJECT: PROBING THE
CIRCUMSTELLAR ENVIRONMENT OF THE HERBIG Ae STAR MWC325
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; radiative transfer; stars: individual (MWC325);
stars: pre-main sequence; stars: variables: T Tauri, Herbig Ae/Be;
techniques: interferometric
ID BAND INTERFEROMETRIC OBSERVATIONS; NEAR-INFRARED EMISSION; AE/BE STARS;
AB-AURIGAE; INNER DISK; PROTOPLANETARY DISKS; VEGA-TYPE; T TAURI; HR
5999; N-BAND
AB We present the first N-band nulling plus K-and L-band V-2 observations of a young stellar object, MWC325, taken with the 85 m baseline Keck Interferometer. The Keck nuller was designed for the study of faint dust signatures associated with debris disks, but it also has a unique capability for studying the temperature and density distribution of denser disks found around young stellar objects. Interferometric observations of MWC325 at K, L, and N encompass a factor of five in spectral range and thus, especially when spectrally dispersed within each band, enable characterization of the structure of the inner disk regions where planets form. Fitting our observations with geometric models such as a uniform disk or a Gaussian disk show that the apparent size increases monotonically with wavelength in the 2-12 mu m wavelength region, confirming the widely held assumption based on radiative transfer models, now with spatially resolved measurements over a broad wavelength range, that disks are extended with a temperature gradient. The effective size is a factor of about 1.4 and 2.2 larger in the L band and N band, respectively, compared to that in the K band. The existing interferometric measurements and the spectral energy distribution can be reproduced by a flat disk or a weakly shadowed nearly flat disk model, with only slight flaring in the outer regions of the disk, consisting of representative "sub-micron" (0.1 mu m) and "micron" (2 mu m) grains of a 50: 50 ratio of silicate and graphite. This is in marked contrast to the disks previously found in other Herbig Ae/Be stars, suggesting a wide variety in the disk properties among Herbig Ae/Be stars.
C1 [Ragland, S.; Hrynevich, M.] WM Keck Observ, Kamuela, HI 96743 USA.
[Ohnaka, K.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Hillenbrand, L.] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA.
[Ridgway, S. T.] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Colavita, M. M.; Traub, W. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Akeson, R. L.; Millan-Gabet, R.] CALTECH, NExScI, Pasadena, CA 91125 USA.
[Cotton, W.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Danchi, W. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Ragland, S (reprint author), WM Keck Observ, Kamuela, HI 96743 USA.
EM sragland@keck.hawaii.edu
FU National Aeronautics and Space Administration (NASA) [NNH09AK731]; W. M.
Keck Foundation
FX The Keck Interferometer is funded by the National Aeronautics and Space
Administration (NASA). Observations presented were obtained at the W. M.
Keck Observatory, which is operated as a scientific partnership among
the California Institute of Technology, the University of California,
and NASA. The Observatory was made possible by the generous financial
support of the W. M. Keck Foundation. KI observations were taken through
Keck Director's time. We thank E. Appleby, A. Cooper, C. Felizardo, J.
Herstein, D. Medeiros, D. Morrison, T. Panteleeva, B. Parvin, B. Smith,
K. Summers, K. Tsubota, C. Tyau, E. Wetherell, P. Wizinowich, and J.
Woillez for their contributions to KI operations. CHARA observations
were taken through NOAO TAC time. We thank Gail Schaefer, P. J.
Goldfinger, Chris Farrington, and Theo ten Brummelaar for support of the
CHARA observing program and Tabetha Boyajian for advice on data
reductions. S. T. R. acknowledges partial support from NASA grant
NNH09AK731.
NR 65
TC 12
Z9 12
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 FEB 20
PY 2012
VL 746
IS 2
AR 126
DI 10.1088/0004-637X/746/2/126
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 894DD
UT WOS:000300406300012
ER
PT J
AU Reeves, KK
Gibson, SE
Kucera, TA
Hudson, HS
Kano, R
AF Reeves, Katharine K.
Gibson, Sarah E.
Kucera, Therese A.
Hudson, Hugh S.
Kano, Ryouhei
TI THERMAL PROPERTIES OF A SOLAR CORONAL CAVITY OBSERVED WITH THE X-RAY
TELESCOPE ON HINODE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona; Sun: filaments, prominences
ID WHOLE SUN MONTH; PROMINENCES; DENSITIES; XRT; SPECTROMETER;
TEMPERATURES; TOMOGRAPHY; MISSION; CORE
AB Coronal cavities are voids in coronal emission often observed above high latitude filament channels. Sometimes, these cavities have areas of bright X-ray emission in their centers. In this study, we use data from the X-ray Telescope (XRT) on the Hinode satellite to examine the thermal emission properties of a cavity observed during 2008 July that contains bright X-ray emission in its center. Using ratios of XRT filters, we find evidence for elevated temperatures in the cavity center. The area of elevated temperature evolves from a ring-shaped structure at the beginning of the observation, to an elongated structure two days later, finally appearing as a compact round source four days after the initial observation. We use a morphological model to fit the cavity emission, and find that a uniform structure running through the cavity does not fit the observations well. Instead, the observations are reproduced by modeling several short cylindrical cavity "cores" with different parameters on different days. These changing core parameters may be due to some observed activity heating different parts of the cavity core at different times. We find that core temperatures of 1.75 MK, 1.7 MK, and 2.0 MK (for July 19, July 21, and July 23, respectively) in the model lead to structures that are consistent with the data, and that line-of-sight effects serve to lower the effective temperature derived from the filter ratio.
C1 [Reeves, Katharine K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Gibson, Sarah E.] HAO NCAR, Boulder, CO 80307 USA.
[Kucera, Therese A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Hudson, Hugh S.] Univ Calif Berkeley, Space Sci Labs, Berkeley, CA 94720 USA.
[Hudson, Hugh S.] Univ Glasgow, Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland.
[Kano, Ryouhei] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
RP Reeves, KK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 58, Cambridge, MA 02138 USA.
EM kreeves@cfa.harvard.edu
RI Kucera, Therese/C-9558-2012; Reeves, Katharine/P-9163-2014;
OI Kucera, Therese/0000-0001-9632-447X
FU International Space Science Institute (ISSI); NASA [NNM07AB07C];
National Science Foundation
FX The authors thank the anonymous referee, whose insightful comments
helped improve the paper, and Yuhong Fan for useful discussions. The
authors also thank the International Space Science Institute (ISSI) for
funding a Working Group on Coronal Cavities, where this work began. K.
K. Reeves is supported under contract NNM07AB07C from NASA to SAO. T.
Kucera is supported by an award from the NASA SHP Program. The National
Center for Atmospheric Research is sponsored by the National Science
Foundation. Hinode is a Japanese mission developed and launched by
ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as
international partners. It is operated by these agencies in cooperation
with ESA and NSC (Norway). SoHO is a project of international
collaboration between ESA and NASA. The STEREO/SECCHI data used here are
produced by an international consortium of the Naval Research Laboratory
(USA), Lockheed Martin Solar and Astrophysics Lab (USA), NASA Goddard
Space Flight Center (USA) Rutherford Appleton Laboratory (UK),
University of Birmingham (UK), Max-Planck-Institut fur
Sonnensystemforschung (Germany), Centre Spatiale de Liege (Belgium),
Institut d'Optique Theorique et Appliquee (France), and Institut
d'Astrophysique Spatiale (France).
NR 31
TC 19
Z9 19
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 FEB 20
PY 2012
VL 746
IS 2
AR 146
DI 10.1088/0004-637X/746/2/146
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 894DD
UT WOS:000300406300032
ER
PT J
AU Sharon, K
Gladders, MD
Rigby, JR
Wuyts, E
Koester, BP
Bayliss, MB
Barrientos, LF
AF Sharon, Keren
Gladders, Michael D.
Rigby, Jane R.
Wuyts, Eva
Koester, Benjamin P.
Bayliss, Matthew B.
Barrientos, L. Felipe
TI SOURCE-PLANE RECONSTRUCTION OF THE BRIGHT LENSED GALAXY RCSGA
032727-132609
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: individual: RCS2 032727-13262; gravitational
lensing: strong
ID HIGH-REDSHIFT; CLUSTER; Z=1.7
AB We present new Hubble Space Telescope/Wide Field Camera 3 imaging data of RCSGA 032727-132609, a bright lensed galaxy at z = 1.7 that is magnified and stretched by the lensing cluster RCS2 032727-132623. Using this new high-resolution imaging, we modify our previous lens model (which was based on ground-based data) to fully understand the lensing geometry, and use it to reconstruct the lensed galaxy in the source plane. This giant arc represents a unique opportunity to peer into 100 pc scale structures in a high-redshift galaxy. This new source reconstruction will be crucial for a future analysis of the spatially resolved rest-UV and rest-optical spectra of the brightest parts of the arc.
C1 [Sharon, Keren; Gladders, Michael D.; Wuyts, Eva; Bayliss, Matthew B.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Gladders, Michael D.; Wuyts, Eva; Koester, Benjamin P.; Bayliss, Matthew B.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Rigby, Jane R.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Wuyts, Eva] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Barrientos, L. Felipe] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
RP Sharon, K (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
EM kerens@kicp.uchicago.edu
RI Rigby, Jane/D-4588-2012
OI Rigby, Jane/0000-0002-7627-6551
FU NASA through Space Telescope Science Institute [12267]; NASA [NAS
5-26555]; Research Corporation; Carnegie Institute for Science; FONDECYT
[1085286]
FX Support for program 12267 was provided by NASA through a grant from the
Space Telescope Science Institute, which is operated by the Association
of Universities for Research in Astronomy, Inc., under NASA contract NAS
5-26555. M.D.G. thanks the Research Corporation for support of this work
through a Cottrell Scholars award. J.R.R. was supported in part by a
Carnegie Fellowship from the Carnegie Institute for Science. L.F.B. is
supported by FONDECYT under project 1085286. We thank the referee, M.
Limousin, for useful comments.
NR 15
TC 23
Z9 23
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 FEB 20
PY 2012
VL 746
IS 2
AR 161
DI 10.1088/0004-637X/746/2/161
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 894DD
UT WOS:000300406300047
ER
PT J
AU Shin, IG
Choi, JY
Park, SY
Han, C
Gould, A
Sumi, T
Udalski, A
Beaulieu, JP
Dominik, M
Allen, W
Bos, M
Christie, GW
Depoy, DL
Dong, S
Drummond, J
Gal-Yam, A
Gaudi, BS
Hung, LW
Janczak, J
Kaspi, S
Lee, CU
Mallia, F
Maoz, D
Maury, A
McCormick, J
Monard, LAG
Moorhouse, D
Munoz, JA
Natusch, T
Nelson, C
Park, BG
Pogge, RW
Polishook, D
Shvartzvald, Y
Shporer, A
Thornley, G
Yee, JC
Abe, F
Bennett, DP
Bond, IA
Botzler, CS
Fukui, A
Furusawa, K
Hayashi, F
Hearnshaw, JB
Hosaka, S
Itow, Y
Kamiya, K
Kilmartin, PM
Kobara, S
Korpela, A
Lin, W
Ling, CH
Makita, S
Masuda, K
Matsubara, Y
Miyake, N
Muraki, Y
Nagaya, M
Nishimoto, K
Ohnishi, K
Okumura, T
Omori, K
Perrott, YC
Rattenbury, N
Saito, T
Skuljan, L
Sullivan, DJ
Suzuki, D
Sweatman, WL
Tristram, PJ
Wada, K
Yock, PCM
Szymanski, MK
Kubiak, M
Pietrzynski, G
Soszynski, I
Poleski, R
Ulaczyk, K
Wyrzykowski, L
Kozlowski, S
Pietrukowicz, P
Albrow, MD
Batista, V
Bramich, DM
Brillant, S
Caldwell, JAR
Calitz, JJ
Cassan, A
Cole, A
Cook, KH
Corrales, E
Coutures, C
Dieters, S
Prester, DD
Donatowicz, J
Fouque, P
Greenhill, J
Hoffman, M
Jorgensen, UG
Kane, SR
Kubas, D
Marquette, JB
Martin, R
Meintjes, P
Menzies, J
Pollard, KR
Sahu, KC
Wambsganss, J
Williams, A
Vinter, C
Zub, M
Allan, A
Browne, P
Horne, K
Snodgrass, C
Steele, I
Street, R
Tsapras, Y
Alsubai, KA
Bozza, V
Browne, P
Burgdorf, MJ
Novati, SC
Dodds, P
Dreizler, S
Finet, F
Gerner, T
Glitrup, M
Grundahl, F
Hardis, S
Harpsoe, K
Hessman, FV
Hinse, TC
Hundertmark, M
Kains, N
Kerins, E
Liebig, C
Maier, G
Mancini, L
Mathiasen, M
Penny, MT
Proft, S
Rahvar, S
Ricci, D
Scarpetta, G
Schafer, S
Schonebeck, F
Skottfelt, J
Surdej, J
Southworth, J
Zimmer, F
AF Shin, I. -G.
Choi, J. -Y.
Park, S. -Y.
Han, C.
Gould, A.
Sumi, T.
Udalski, A.
Beaulieu, J. -P.
Dominik, M.
Allen, W.
Bos, M.
Christie, G. W.
Depoy, D. L.
Dong, S.
Drummond, J.
Gal-Yam, A.
Gaudi, B. S.
Hung, L. -W.
Janczak, J.
Kaspi, S.
Lee, C. -U.
Mallia, F.
Maoz, D.
Maury, A.
McCormick, J.
Monard, L. A. G.
Moorhouse, D.
Munoz, J. A.
Natusch, T.
Nelson, C.
Park, B. -G.
Pogge, R. W.
Polishook, D.
Shvartzvald, Y.
Shporer, A.
Thornley, G.
Yee, J. C.
Abe, F.
Bennett, D. P.
Bond, I. A.
Botzler, C. S.
Fukui, A.
Furusawa, K.
Hayashi, F.
Hearnshaw, J. B.
Hosaka, S.
Itow, Y.
Kamiya, K.
Kilmartin, P. M.
Kobara, S.
Korpela, A.
Lin, W.
Ling, C. H.
Makita, S.
Masuda, K.
Matsubara, Y.
Miyake, N.
Muraki, Y.
Nagaya, M.
Nishimoto, K.
Ohnishi, K.
Okumura, T.
Omori, K.
Perrott, Y. C.
Rattenbury, N.
Saito, To.
Skuljan, L.
Sullivan, D. J.
Suzuki, D.
Sweatman, W. L.
Tristram, P. J.
Wada, K.
Yock, P. C. M.
Szymanski, M. K.
Kubiak, M.
Pietrzynski, G.
Soszynski, I.
Poleski, R.
Ulaczyk, K.
Wyrzykowski, L.
Kozlowski, S.
Pietrukowicz, P.
Albrow, M. D.
Batista, V.
Bramich, D. M.
Brillant, S.
Caldwell, J. A. R.
Calitz, J. J.
Cassan, A.
Cole, A.
Cook, K. H.
Corrales, E.
Coutures, Ch.
Dieters, S.
Prester, D. Dominis
Donatowicz, J.
Fouque, P.
Greenhill, J.
Hoffman, M.
Jorgensen, U. G.
Kane, S. R.
Kubas, D.
Marquette, J. -B.
Martin, R.
Meintjes, P.
Menzies, J.
Pollard, K. R.
Sahu, K. C.
Wambsganss, J.
Williams, A.
Vinter, C.
Zub, M.
Allan, A.
Browne, P.
Horne, K.
Snodgrass, C.
Steele, I.
Street, R.
Tsapras, Y.
Alsubai, K. A.
Bozza, V.
Browne, P.
Burgdorf, M. J.
Novati, S. Calchi
Dodds, P.
Dreizler, S.
Finet, F.
Gerner, T.
Glitrup, M.
Grundahl, F.
Hardis, S.
Harpsoe, K.
Hessman, F. V.
Hinse, T. C.
Hundertmark, M.
Kains, N.
Kerins, E.
Liebig, C.
Maier, G.
Mancini, L.
Mathiasen, M.
Penny, M. T.
Proft, S.
Rahvar, S.
Ricci, D.
Scarpetta, G.
Schaefer, S.
Schoenebeck, F.
Skottfelt, J.
Surdej, J.
Southworth, J.
Zimmer, F.
CA FUN Collaboration
MOA Collaboration
OGLE Collaboration
PLANET Collaboration
RoboNet Collaboration
MiNDSTEp Consortium
TI MICROLENSING BINARIES DISCOVERED THROUGH HIGH-MAGNIFICATION CHANNEL
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; gravitational lensing: micro
ID III EWS DATABASE; GRAVITATIONAL LENSING EXPERIMENT; GALACTIC BULGE;
EVENTS; PLANETARY; LENSES; MASS; ASTROPHYSICS
AB Microlensing can provide a useful tool to probe binary distributions down to low-mass limits of binary companions. In this paper, we analyze the light curves of eight binary-lensing events detected through the channel of high-magnification events during the seasons from 2007 to 2010. The perturbations, which are confined near the peak of the light curves, can be easily distinguished from the central perturbations caused by planets. However, the degeneracy between close and wide binary solutions cannot be resolved with a 3 sigma confidence level for three events, implying that the degeneracy would be an important obstacle in studying binary distributions. The dependence of the degeneracy on the lensing parameters is consistent with a theoretical prediction that the degeneracy becomes severe as the binary separation and the mass ratio deviate from the values of resonant caustics. The measured mass ratio of the event OGLE-2008-BLG-510/MOA-2008-BLG-369 is q similar to 0.1, making the companion of the lens a strong brown dwarf candidate.
C1 [Shin, I. -G.; Choi, J. -Y.; Park, S. -Y.; Han, C.] Chungbuk Natl Univ, Dept Phys, Inst Astrophys, Cheongju 371763, South Korea.
[Gould, A.; Gaudi, B. S.; Pogge, R. W.; Yee, J. C.; Batista, V.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Sumi, T.; Suzuki, D.; Wada, K.] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan.
[Udalski, A.; Szymanski, M. K.; Kubiak, M.; Pietrzynski, G.; Soszynski, I.; Poleski, R.; Ulaczyk, K.; Wyrzykowski, L.; Kozlowski, S.; Pietrukowicz, P.] Univ Warsaw Observ, PL-00478 Warsaw, Poland.
[Beaulieu, J. -P.; Cassan, A.; Corrales, E.; Coutures, Ch.; Dieters, S.; Kubas, D.; Marquette, J. -B.] Univ Paris 06, Inst Astrophys Paris, UMR7095, CNRS, F-75014 Paris, France.
[Dominik, M.; Browne, P.; Horne, K.; Browne, P.; Dodds, P.; Hundertmark, M.; Kains, N.; Liebig, C.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Allen, W.] Vintage Lane Observ, Blenheim, New Zealand.
[Bos, M.] Molehill Astron Observ, N Shore, New Zealand.
[Christie, G. W.; Natusch, T.] Auckland Observ, Auckland, New Zealand.
[Depoy, D. L.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA.
[Dong, S.] Inst Adv Study, Princeton, NJ 08540 USA.
[Drummond, J.] Possum Observ, Patutahi, New Zealand.
[Gal-Yam, A.] Weizmann Inst Sci, Benoziyo Ctr Astrophys, Weizmann, Israel.
[Hung, L. -W.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Janczak, J.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Kaspi, S.; Maoz, D.; Polishook, D.; Shvartzvald, Y.; Shporer, A.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Lee, C. -U.; Park, B. -G.; Hinse, T. C.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
[Mallia, F.; Maury, A.] Campo Catino Austral Observ, San Pedro De Atacama, Chile.
[McCormick, J.] Farm Cove Observ, Auckland, New Zealand.
[Monard, L. A. G.] Bronberg Observ, Pretoria, South Africa.
[Moorhouse, D.; Thornley, G.] Kumeu Observ, Kumeu, New Zealand.
[Munoz, J. A.] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain.
[Nelson, C.] Univ Arizona, Coll Opt Sci, Tucson, AZ 85721 USA.
[Abe, F.; Fukui, A.; Furusawa, K.; Hayashi, F.; Hosaka, S.; Itow, Y.; Kamiya, K.; Kobara, S.; Makita, S.; Masuda, K.; Matsubara, Y.; Miyake, N.; Nagaya, M.; Nishimoto, K.; Okumura, T.; Omori, K.] 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.; Lin, W.; Ling, C. H.; Skuljan, L.; Sweatman, W. L.] Massey Univ, Inst Informat & Math Sci, N Shore Mail Ctr, Auckland, New Zealand.
[Botzler, C. S.; Perrott, Y. C.; Rattenbury, N.; Yock, P. C. M.] Univ Auckland, Dept Phys, Auckland, New Zealand.
[Hearnshaw, J. B.; Albrow, M. D.; Pollard, K. R.] Univ Canterbury, Dept Phys & Astron, Christchurch 8020, New Zealand.
[Kilmartin, P. M.; Tristram, P. J.] Mt John Observ, Lake Tekapo 8770, New Zealand.
[Korpela, A.; Sullivan, D. J.] Victoria Univ, Sch Chem & Phys Sci, Wellington, New Zealand.
[Muraki, Y.] Konan Univ, Dept Phys, Kobe, Hyogo 6588501, Japan.
[Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan.
[Saito, To.] Tokyo Metropolitan Coll Ind Technol, Tokyo 1168523, Japan.
[Pietrzynski, G.] Univ Concepcion, Dept Fis, Concepcion, Chile.
[Wyrzykowski, L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Bramich, D. M.] European So Observ, D-85748 Garching, Germany.
[Brillant, S.; Kubas, D.; Snodgrass, C.] European So Observ, Santiago 19, Chile.
[Caldwell, J. A. R.] McDonald Observ, Ft Davis, TX 79734 USA.
[Calitz, J. J.; Hoffman, M.; 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.
[Cook, K. H.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys IGPP, Livermore, CA 94551 USA.
[Dieters, S.; Fouque, P.] Univ Toulouse, LATT, CNRS, F-31400 Toulouse, France.
[Prester, D. Dominis] Univ Rijeka, Dept Phys, Fac Arts & Sci, Rijeka 51000, Croatia.
[Donatowicz, J.] Vienna Univ Technol, Dept Comp, A-1060 Vienna, Austria.
[Jorgensen, U. G.; Vinter, C.; 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.
[Kane, S. R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Martin, R.; Williams, A.] Perth Observ, Perth, WA 6076, Australia.
[Menzies, J.] S African Astron Observ, ZA-7935 Observatory, South Africa.
[Sahu, K. C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Wambsganss, J.; Zub, M.] Heidelberg Univ, Astron Rechen Inst ARI, Zentrum Astron, D-69120 Heidelberg, Germany.
[Allan, A.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
[Snodgrass, C.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany.
[Steele, I.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England.
[Street, R.; Tsapras, Y.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA.
[Alsubai, K. A.] Qatar Fdn, Doha, Qatar.
[Bozza, V.; Novati, S. Calchi; Mancini, L.; Scarpetta, G.] Univ Salerno, Dipartimento Fis ER Caianiello, I-84081 Baronissi, SA, Italy.
[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] Ist Int Alti Studi Sci IIASS, Vietri Sul Mare, SA, Italy.
[Dreizler, S.; Hessman, F. V.; Hundertmark, M.; Schaefer, S.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
[Finet, F.; Ricci, D.; Surdej, J.] Inst Astrophys & Geophys, B-4000 Liege, Belgium.
[Gerner, T.; Liebig, C.; Maier, G.; Proft, S.; Schoenebeck, F.; Zimmer, F.] Heidelberg Univ, Astron Rechen Inst, Zentrum Astron, D-69120 Heidelberg, Germany.
[Glitrup, M.; Grundahl, F.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Hinse, T. C.] Armagh Observ, Armagh BT61 9DG, North Ireland.
[Kains, N.] ESO Headquarters, D-85748 Garching, Germany.
[Kerins, E.; Penny, M. T.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Mancini, L.] Max Planck Inst Astron, D-619117 Heidelberg, Germany.
[Rahvar, S.] Sharif Univ Technol, Dept Phys, Tehran, Iran.
[Scarpetta, G.] Ist Nazl Fis Nucl, Grp Collegato Salerno, Sez Napoli, Milan, Italy.
[Southworth, J.] Univ Keele, Astrophys Grp, Keele ST5 5BG, Staffs, England.
RP Shin, IG (reprint author), Chungbuk Natl Univ, Dept Phys, Inst Astrophys, Cheongju 371763, South Korea.
RI Gaudi, Bernard/I-7732-2012; Kozlowski, Szymon/G-4799-2013; Williams,
Andrew/K-2931-2013; Zimmer, Fabian/M-4765-2014; Hundertmark,
Markus/C-6190-2015; Rahvar, Sohrab/A-9350-2008; Dong, Subo/J-7319-2012;
Kane, Stephen/B-4798-2013; Greenhill, John/C-8367-2013
OI Ricci, Davide/0000-0002-9790-0552; Penny, Matthew/0000-0001-7506-5640;
Snodgrass, Colin/0000-0001-9328-2905; Kozlowski,
Szymon/0000-0003-4084-880X; Williams, Andrew/0000-0001-9080-0105;
Hundertmark, Markus/0000-0003-0961-5231; Rahvar,
Sohrab/0000-0002-7084-5725; Dominik, Martin/0000-0002-3202-0343; Cole,
Andrew/0000-0003-0303-3855;
FU Creative Research Initiative of National Research Foundation of Korea
[2009-0081561]; European Research Council under the European Community
[246678]; NSF [AST-1103471, 2009068160]; NASA [NNX08AF40G]; Qatar
National Research Fund; Deutsche Forschungsgemeinschaft; Communaute
francaise de Belgique-Actions de recherche concertees-Academie
universitaire Wallonie-Europe; [JSPS22403003]; [JSPS20340052];
[JSPS18253002]; [JSPS17340074]; [JSPS18749004]; [MEXT19015005];
[JSPS20740104]
FX Work by C. H. was supported by Creative Research Initiative Program
(2009-0081561) of National Research Foundation of Korea. 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. Work by B. S. G. and A. G. was supported in
part by NSF grant AST-1103471. Work by B. S. G., A. G., R. W. P., and
J.C.Y. was supported in part by NASA grant NNX08AF40G. Work by J.C.Y.
was supported by a National Science Foundation Graduate Research
Fellowship under grant No. 2009068160. Work by M. H. was supported by
Qatar National Research Fund and Deutsche Forschungsgemeinschaft. The
MOA experiment was supported by JSPS22403003, JSPS20340052,
JSPS18253002, and JSPS17340074. T. S. was supported by the grants
JSPS18749004, MEXT19015005, and JSPS20740104. F. F., D. R., and J.S.
were supported by the Communaute francaise de Belgique-Actions de
recherche concertees-Academie universitaire Wallonie-Europe.
NR 39
TC 12
Z9 12
U1 1
U2 11
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 FEB 20
PY 2012
VL 746
IS 2
AR 127
DI 10.1088/0004-637X/746/2/127
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 894DD
UT WOS:000300406300013
ER
PT J
AU Wright, M
Zhao, JH
Sandell, G
Corder, S
Goss, WM
Zhu, L
AF Wright, Melvyn
Zhao, Jun-Hui
Sandell, Goeran
Corder, Stuartt
Goss, W. M.
Zhu, Lei
TI OBSERVATIONS OF A HIGH-MASS PROTOSTAR IN NGC 7538 S
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; ISM: clouds; stars: formation; stars: pre-main
sequence; submillimeter: ISM
ID SUBMILLIMETER CONTINUUM OBSERVATIONS; STAR-FORMATION; CIRCUMSTELLAR
DISKS; NGC-7538 REGION; ACCRETION DISK; DUST EMISSION; ORION-KL; CORES;
OBJECTS; MASERS
AB We present high angular resolution continuum observations of the high-mass protostar NGC 7538 S with BIMA and CARMA at 3 and 1.4 mm, Very Large Array (VLA) observations at 1.3, 2, 3.5, and 6 cm, and archive Infrared Array Camera (IRAC) observations from the Spitzer Space Observatory, which detect the star at 4.5, 5.8, and 8 mu m. The star looks rather unremarkable in the mid-IR. The excellent positional agreement of the IRAC source with the VLA free-free emission, the OH, CH3OH, H2O masers, and the dust continuum confirms that this is the most luminous object in the NGC 7538 S core. The continuum emission at millimeter wavelengths is dominated by dust emission from the dense cold cloud core surrounding the protostar. Including all array configurations, the emission is dominated by an elliptical source with a size of similar to 8 '' x 3 ''. If we filter out the extended emission we find three compact millimeter sources inside the elliptical core. The strongest one, S-A, coincides with the VLA/IRAC source and resolves into a double source at 1.4 mm, where we have subarcsecond resolution. The measured spectral index, a, between 3 and 1.4 mm is similar to 2.3, and steeper at longer wavelengths, suggesting a low dust emissivity or that the dust is optically thick. We argue that the dust in these accretion disks is optically thick and estimate a mass of an accretion disk or infalling envelope surrounding S-A to be similar to 60 M-circle dot.
C1 [Wright, Melvyn] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA.
[Zhao, Jun-Hui] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Sandell, Goeran] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA.
[Corder, Stuartt] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Goss, W. M.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Zhu, Lei] Peking Univ, Dept Astron, Beijing 100871, Peoples R China.
RP Wright, M (reprint author), Univ Calif Berkeley, Radio Astron Lab, 601 Campbell Hall, Berkeley, CA 94720 USA.
FU National Science Foundation; state of California; state of Illinois;
state of Maryland; Gordon and Betty Moore Foundation; Kenneth T. and
Eileen L. Norris Foundation; California Institute of Technology; CARMA
partner universities
FX The BIMA array was operated by the Universities of California
(Berkeley), Illinois, and Maryland with support from the National
Science Foundation. Support for CARMA construction was derived from the
states of California, Illinois, and Maryland, the Gordon and Betty Moore
Foundation, the Kenneth T. and Eileen L. Norris Foundation, the
Associates of the California Institute of Technology, and the National
Science Foundation. Ongoing CARMA development and operations are
supported by the National Science Foundation under a cooperative
agreement, and by the CARMA partner universities.
NR 35
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 FEB 20
PY 2012
VL 746
IS 2
AR 187
DI 10.1088/0004-637X/746/2/187
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 894DD
UT WOS:000300406300073
ER
PT J
AU Kaur, R
Kaper, L
Ellerbroek, LE
Russell, DM
Altamirano, D
Wijnands, R
Yang, YJ
D'Avanzo, P
Postigo, AD
Flores, H
Fynbo, JPU
Goldoni, P
Thone, CC
van der Horst, A
van der Klis, M
Kouveliotou, C
Wiersema, K
Kuulkers, E
AF Kaur, Ramanpreet
Kaper, Lex
Ellerbroek, Lucas E.
Russell, David M.
Altamirano, Diego
Wijnands, Rudy
Yang, Yi-Jung
D'Avanzo, Paolo
Postigo, Antonio de Ugarte
Flores, Hector
Fynbo, Johan P. U.
Goldoni, Paolo
Thoene, Christina C.
van der Horst, Alexander
van der Klis, Michiel
Kouveliotou, Chryssa
Wiersema, Klaas
Kuulkers, Erik
TI VERY LARGE TELESCOPE/X-SHOOTER SPECTROSCOPY OF THE CANDIDATE BLACK HOLE
X-RAY BINARY MAXI J1659-152 IN OUTBURST
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; binaries: close; black hole physics; X-rays:
binaries
ID DIFFUSE INTERSTELLAR BANDS; LOW-HARD STATES; OPTICAL SPECTROSCOPY;
HIGH-SOFT; GX 339-4; ULTRAVIOLET; EMISSION; EXTINCTION; GX-339-4;
MISSION
AB We present the optical to near-infrared spectrum of MAXI J1659-152 during the onset of its 2010 X-ray outburst. The spectrum was obtained with X-shooter on the ESO Very Large Telescope early in the outburst simultaneous with high-quality observations at both shorter and longer wavelengths. At the time of the observations, the source was in the low-hard state. The X-shooter spectrum includes many broad (similar to 2000 km s(-1)), double-peaked emission profiles of H, He I, and He II, characteristic signatures of a low-mass X-ray binary during outburst. We detect no spectral signatures of the low-mass companion star. The strength of the diffuse interstellar bands results in a lower limit to the total interstellar extinction of A(V) similar or equal to 0.4 mag. Using the neutral hydrogen column density obtained from the X-ray spectrum we estimate A(V) similar or equal to 1 mag. The radial velocity structure of the interstellar Na I D and Ca II H&K lines results in a lower limit to the distance of similar to 4 +/- 1 kpc, consistent with previous estimates. With this distance and A(V), the dereddened spectral energy distribution represents a flat disk spectrum. The two 10 minute X-shooter spectra show significant variability in the red wing of the emission-line profiles, indicating a global change in the density structure of the disk, though on a timescale much shorter than the typical viscous timescale of the disk.
C1 [Kaur, Ramanpreet; Kaper, Lex; Ellerbroek, Lucas E.; Russell, David M.; Altamirano, Diego; Wijnands, Rudy; Yang, Yi-Jung; van der Horst, Alexander; van der Klis, Michiel] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Kaur, Ramanpreet] Univ Wisconsin, Dept Phys, Milwaukee, WI 53211 USA.
[D'Avanzo, Paolo] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy.
[Postigo, Antonio de Ugarte; Fynbo, Johan P. U.] Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Postigo, Antonio de Ugarte; Thoene, Christina C.] CSIC, IAA, E-18008 Granada, Spain.
[Flores, Hector] Univ Paris Diderot, GEPI, Observ Paris, CNRS, F-92195 Meudon, France.
[Goldoni, Paolo] Lab Astroparticule & Cosmol, F-75205 Paris 13, France.
[Goldoni, Paolo] CEA Saclay, Serv Astrophys, DSM, IRFU,SAp, F-91191 Gif Sur Yvette, France.
[Thoene, Christina C.] Niels Bohr Inst, Niels Bohr Int Acad, DK-2100 Copenhagen, Denmark.
[van der Horst, Alexander] NSSTC, USRA, Huntsville, AL 35806 USA.
[Kouveliotou, Chryssa] NASA, Space Sci Off, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Wiersema, Klaas] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Kuulkers, Erik] European Space Astron Ctr, European Space Agcy, Madrid 28691, Spain.
RP Kaur, R (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.
EM r.kaur@uva.nl
RI Fynbo, Johan/L-8496-2014;
OI Fynbo, Johan/0000-0002-8149-8298; Thone, Christina/0000-0002-7978-7648;
de Ugarte Postigo, Antonio/0000-0001-7717-5085
FU European Research Council
FX R.K., R.W., and J.P.U.F. acknowledge support from the European Research
Council starting grant.
NR 50
TC 10
Z9 10
U1 1
U2 4
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 FEB 20
PY 2012
VL 746
IS 2
AR L23
DI 10.1088/2041-8205/746/2/L23
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 896ZT
UT WOS:000300611100010
ER
PT J
AU King, AL
Miller, JM
Raymond, J
Fabian, AC
Reynolds, CS
Kallman, TR
Maitra, D
Cackett, EM
Rupen, MP
AF King, A. L.
Miller, J. M.
Raymond, J.
Fabian, A. C.
Reynolds, C. S.
Kallman, T. R.
Maitra, D.
Cackett, E. M.
Rupen, M. P.
TI AN EXTREME X-RAY DISK WIND IN THE BLACK HOLE CANDIDATE IGR J17091-3624
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; black hole physics; X-rays: binaries
ID GALAXY NGC 4051; ACCRETION DISKS; ABSORPTION-LINES; WARM ABSORBERS; GRO
J1655-40; OUTBURST; CHANDRA; RADIO; SPECTROSCOPY; OUTFLOWS
AB Chandra spectroscopy of transient stellar-mass black holes in outburst has clearly revealed accretion disk winds in soft, disk-dominated states, in apparent anti-correlation with relativistic jets in low/hard states. These disk winds are observed to be highly ionized, dense, and to have typical velocities of similar to 1000 km s(-1) or less projected along our line of sight. Here, we present an analysis of two Chandra High Energy Transmission Grating spectra of the Galactic black hole candidate IGR J17091-3624 and contemporaneous Expanded Very Large Array (EVLA) radio observations, obtained in 2011. The second Chandra observation reveals an absorption line at 6.91 +/- 0.01 keV; associating this line with He-like Fe XXV requires a blueshift of 9300(-400)(+500) km s(-1) (0.03c, or the escape velocity at 1000 R-Schw). This projected outflow velocity is an order of magnitude higher than has previously been observed in stellar-mass black holes, and is broadly consistent with some of the fastest winds detected in active galactic nuclei. A potential feature at 7.32 keV, if due to Fe XXVI, would imply a velocity of similar to 14,600 km s(-1) (0.05c), but this putative feature is marginal. Photoionization modeling suggests that the accretion disk wind in IGR J17091-3624 may originate within 43,300 Schwarzschild radii of the black hole and may be expelling more gas than it accretes. The contemporaneous EVLA observations strongly indicate that jet activity was indeed quenched at the time of our Chandra observations. We discuss the results in the context of disk winds, jets, and basic accretion disk physics in accreting black hole systems.
C1 [King, A. L.; Miller, J. M.; Maitra, D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Raymond, J.] Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fabian, A. C.; Cackett, E. M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Kallman, T. R.] NASA, High Energy Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cackett, E. M.] Wayne State Univ, Dept Phys & Astron, Detroit, MI 48201 USA.
[Rupen, M. P.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
RP King, AL (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA.
EM ashking@umich.edu
FU NASA; Chandra Guest Observer program
FX We thank the anonymous referee. We thank Michael Nowak for his
instrumental help as well. A.L.K. gratefully acknowledges support
through the NASA Earth and Space Sciences Fellowship. J.M.M. gratefully
acknowledges support through the Chandra Guest Observer program. The
National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc.
NR 38
TC 49
Z9 49
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 20
PY 2012
VL 746
IS 2
AR L20
DI 10.1088/2041-8205/746/2/L20
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 896ZT
UT WOS:000300611100007
ER
PT J
AU Liu, YD
Luhmann, JG
Mostl, C
Martinez-Oliveros, JC
Bale, SD
Lin, RP
Harrison, RA
Temmer, M
Webb, DF
Odstrcil, D
AF Liu, Ying D.
Luhmann, Janet G.
Moestl, Christian
Martinez-Oliveros, Juan C.
Bale, Stuart D.
Lin, Robert P.
Harrison, Richard A.
Temmer, Manuela
Webb, David F.
Odstrcil, Dusan
TI INTERACTIONS BETWEEN CORONAL MASS EJECTIONS VIEWED IN COORDINATED
IMAGING AND IN SITU OBSERVATIONS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE shock waves; solar-terrestrial relations; solar wind; Sun: coronal mass
ejections (CMEs)
ID COMPLEX EJECTA; STEREO MISSION; MAGNETIC CLOUD; EARTH; SIMULATION;
SHOCK; SUN; SIGNATURES
AB The successive coronal mass ejections (CMEs) from 2010 July 30 to August 1 present us the first opportunity to study CME-CME interactions with unprecedented heliospheric imaging and in situ observations from multiple vantage points. We describe two cases of CME interactions: merging of two CMEs launched close in time and overtaking of a preceding CME by a shock wave. The first two CMEs on August 1 interact close to the Sun and form a merged front, which then overtakes the July 30 CME near 1 AU, as revealed by wide-angle imaging observations. Connections between imaging observations and in situ signatures at 1 AU suggest that the merged front is a shock wave, followed by two ejecta observed at Wind which seem to have already merged. In situ measurements show that the CME from July 30 is being overtaken by the shock at 1 AU and is significantly compressed, accelerated, and heated. The interaction between the preceding ejecta and shock also results in variations in the shock strength and structure on a global scale, as shown by widely separated in situ measurements from Wind and STEREO B. These results indicate important implications of CME-CME interactions for shock propagation, particle acceleration, and space weather forecasting.
C1 [Liu, Ying D.; Luhmann, Janet G.; Moestl, Christian; Martinez-Oliveros, Juan C.; Bale, Stuart D.; Lin, Robert P.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Liu, Ying D.] Chinese Acad Sci, Natl Space Sci Ctr, State Key Lab Space Weather, Beijing, Peoples R China.
[Moestl, Christian; Temmer, Manuela] Graz Univ, Inst Phys, A-8010 Graz, Austria.
[Moestl, Christian] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria.
[Lin, Robert P.] Kyung Hee Univ, Sch Space Res, Yongin 446701, Gyeonggi, South Korea.
[Harrison, Richard A.] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England.
[Webb, David F.] Boston Coll, Inst Sci Res, Newton, MA 02459 USA.
[Odstrcil, Dusan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Liu, YD (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM liuxying@ssl.berkeley.edu
RI Bale, Stuart/E-7533-2011;
OI Bale, Stuart/0000-0002-1989-3596; Martinez Oliveros, Juan
Carlos/0000-0002-2587-1342; Liu, Ying/0000-0002-3483-5909; Moestl,
Christian/0000-0001-6868-4152; Temmer, Manuela/0000-0003-4867-7558
FU STEREO [NAS5-03131]; Marie Curie International Outgoing Fellowship;
Austrian Science Fund FWF [V195-N16]
FX The research was supported by the STEREO project under grant NAS5-03131.
C.M. is supported by a Marie Curie International Outgoing Fellowship.
M.T. acknowledges the Austrian Science Fund FWF V195-N16.
NR 28
TC 43
Z9 46
U1 1
U2 6
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 FEB 20
PY 2012
VL 746
IS 2
AR L15
DI 10.1088/2041-8205/746/2/L15
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 896ZT
UT WOS:000300611100002
ER
PT J
AU Mroczkowski, T
AF Mroczkowski, Tony
TI A NEW APPROACH TO OBTAINING CLUSTER MASS FROM SUNYAEV-ZEL'DOVICH EFFECT
OBSERVATIONS (vol 728, L35, 2011)
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Correction
ID ATACAMA COSMOLOGY TELESCOPE; RELAXED GALAXY CLUSTERS; SOUTH-POLE
TELESCOPE; REPRESENTATIVE SAMPLE; INTRACLUSTER MEDIUM; PRESSURE PROFILE;
POWER SPECTRUM; XMM-NEWTON; MATTER; SIMULATIONS
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mroczkowski, T (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 169-237, Pasadena, CA 91109 USA.
NR 36
TC 1
Z9 1
U1 0
U2 1
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 FEB 20
PY 2012
VL 746
IS 2
AR L29
DI 10.1088/2041-8205/746/2/L29
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 896ZT
UT WOS:000300611100016
ER
PT J
AU Patruno, A
Bult, P
Gopakumar, A
Hartman, JM
Wijnands, R
van der Klis, M
Chakrabarty, D
AF Patruno, Alessandro
Bult, Peter
Gopakumar, Achamveedu
Hartman, Jacob M.
Wijnands, Rudy
van der Klis, Michiel
Chakrabarty, Deepto
TI ACCELERATED ORBITAL EXPANSION AND SECULAR SPIN-DOWN OF THE ACCRETING
MILLISECOND PULSAR SAX J1808.4-3658
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE binaries: general; stars: individual (SAX J1808.4-3658); stars: neutron;
stars: rotation; X-rays: binaries; X-rays: stars
ID BINARY PSR B1957+20; X-RAY PULSAR; XMM-NEWTON; PERIOD CHANGES; 2002
OUTBURST; VARIABILITY; EVOLUTION; QUIESCENCE; J2051-0827; COMPANION
AB The accreting millisecond pulsar SAX J1808.4-3658 has shown a peculiar orbital evolution in the past with an orbital expansion much faster than expected from standard binary evolutionary scenarios. Previous limits on the pulsar spin frequency derivative during transient accretion outbursts were smaller than predicted by standard magnetic accretion torque theory, while the spin evolution between outbursts was consistent with magnetic dipole spin-down. In this Letter, we present the results of a coherent timing analysis of the 2011 outburst observed by the Rossi X-Ray Timing Explorer and extend our previous long-term measurements of the orbital and spin evolution over a baseline of 13 years. We find that the expansion of the 2 hr orbit is accelerating at a rate of (P) double over dot(b) similar or equal to 1.6 x 10(-20) s s(-2) and we interpret this as the effect of short-term angular momentum exchange between the mass donor and the orbit. The gravitational quadrupole coupling due to variations in the oblateness of the companion can be a viable mechanism for explaining the observations. No significant spin frequency derivatives are detected during the 2011 outburst (vertical bar(nu) over dot vertical bar less than or similar to 4 x 10(-13) Hz s(-1)) and the long-term spin-down remains stable over 13 years with (nu) over dot similar or equal to 10(-15) Hz s(-1).
C1 [Patruno, Alessandro; Bult, Peter; Wijnands, Rudy; van der Klis, Michiel] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Gopakumar, Achamveedu] Tata Inst Fundamental Res, Dept Astron & Astrophys, Bombay 400005, Maharashtra, India.
[Hartman, Jacob M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Chakrabarty, Deepto] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Chakrabarty, Deepto] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
RP Patruno, A (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands.
FU NWO-Veni; ERC
FX A.P. acknowledges support from an NWO-Veni fellowship. R.W. was partly
supported by an ERC starting grant.
NR 41
TC 27
Z9 27
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 20
PY 2012
VL 746
IS 2
AR L27
DI 10.1088/2041-8205/746/2/L27
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 896ZT
UT WOS:000300611100014
ER
PT J
AU Winebarger, AR
Warren, HP
Schmelz, JT
Cirtain, J
Mulu-Moore, F
Golub, L
Kobayashi, K
AF Winebarger, Amy R.
Warren, Harry P.
Schmelz, Joan T.
Cirtain, Jonathan
Mulu-Moore, Fana
Golub, Leon
Kobayashi, Ken
TI DEFINING THE "BLIND SPOT" OF HINODE EIS AND XRT TEMPERATURE MEASUREMENTS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: corona
ID X-RAY TELESCOPE; DIFFERENTIAL EMISSION MEASURE; ACTIVE-REGION; PLASMA;
LINES; DIAGNOSTICS; LOOPS; FLARE
AB Observing high-temperature, low emission measure plasma is key to unlocking the coronal heating problem. With current instrumentation, a combination of EUV spectral data from Hinode Extreme-ultraviolet Imaging Spectrometer (EIS; sensitive to temperatures up to 4 MK) and broadband filter data from Hinode X-ray Telescope (XRT; sensitive to higher temperatures) is typically used to diagnose the temperature structure of the observed plasma. In this Letter, we demonstrate that a "blind spot" exists in temperature-emission measure space for combined Hinode EIS and XRT observations. For a typical active region core with significant emission at 3-4 MK, Hinode EIS and XRT are insensitive to plasma with temperatures greater than similar to 6 MK and emission measures less than similar to 10(27) cm(-5). We then demonstrate that the temperature and emission measure limits of this blind spot depend upon the temperature distribution of the plasma along the line of sight by considering a hypothetical emission measure distribution sharply peaked at 1 MK. For this emission measure distribution, we find that EIS and XRT are insensitive to plasma with emission measures less than similar to 10(26) cm(-5). We suggest that a spatially and spectrally resolved 6-24 angstrom spectrum would improve the sensitivity to these high-temperature, low emission measure plasma.
C1 [Winebarger, Amy R.; Cirtain, Jonathan; Mulu-Moore, Fana] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Warren, Harry P.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA.
[Schmelz, Joan T.] Univ Memphis, Dept Phys, Memphis, TN 38152 USA.
[Golub, Leon] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kobayashi, Ken] Ctr Space Plasma & Aeron Res, Huntsville, AL 35805 USA.
RP Winebarger, AR (reprint author), NASA, George C Marshall Space Flight Ctr, VP 62, Huntsville, AL 35812 USA.
EM amy.r.winebarger@nasa.gov
OI Golub, Leon/0000-0001-9638-3082
NR 23
TC 22
Z9 22
U1 0
U2 2
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 FEB 20
PY 2012
VL 746
IS 2
AR L17
DI 10.1088/2041-8205/746/2/L17
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 896ZT
UT WOS:000300611100004
ER
PT J
AU Draper, CS
Reichle, RH
De Lannoy, GJM
Liu, Q
AF Draper, C. S.
Reichle, R. H.
De Lannoy, G. J. M.
Liu, Q.
TI Assimilation of passive and active microwave soil moisture retrievals
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID OPTICAL DEPTH RETRIEVAL; METHODOLOGY
AB Near-surface soil moisture observations from the active microwave ASCAT and the passive microwave AMSR-E satellite instruments are assimilated, both separately and together, into the NASA Catchment land surface model over 3.5 years using an ensemble Kalman filter. The impact of each assimilation is evaluated using in situ soil moisture observations from 85 sites in the US and Australia, in terms of the anomaly time series correlation-coefficient, R. The skill gained by assimilating either ASCAT or AMSR-E was very similar, even when separated by land cover type. Over all sites, the mean root-zone R was significantly increased from 0.45 for an open-loop, to 0.55, 0.54, and 0.56 by the assimilation of ASCAT, AMSR-E, and both, respectively. Each assimilation also had a positive impact over each land cover type sampled. For maximum accuracy and coverage it is recommended that active and passive microwave observations be assimilated together. Citation: Draper, C. S., R. H. Reichle, G. J. M. De Lannoy, and Q. Liu (2012), Assimilation of passive and active microwave soil moisture retrievals, Geophys. Res. Lett., 39, L04401, doi: 10.1029/2011GL050655.
C1 [Draper, C. S.; Reichle, R. H.; De Lannoy, G. J. M.; Liu, Q.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Draper, C. S.; De Lannoy, G. J. M.] Univ Space Res Assoc, GESTAR, Columbia, MD USA.
[De Lannoy, G. J. M.] Univ Ghent, Lab Hydrol & Water Management, B-9000 Ghent, Belgium.
[Liu, Q.] Sci Applicat Int Corp, Beltsville, MD USA.
RP Draper, CS (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Code 610-1, Greenbelt, MD 20771 USA.
EM clara.draper@nasa.gov
RI Reichle, Rolf/E-1419-2012; Draper, Clara/P-6097-2016
OI Draper, Clara/0000-0002-8299-4939
FU Research Foundation Flanders
FX We are grateful to all who contributed to the data sets used in this
study. In particular we acknowledge Richard de Jeu and colleagues (VUA),
Wolfgang Wagner and colleagues (TU-Wien), and staff at ESA, Monash
University, NASA, USDA, and the University of Melbourne. G. De Lannoy is
funded by the Research Foundation Flanders.
NR 15
TC 74
Z9 74
U1 5
U2 32
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 FEB 18
PY 2012
VL 39
AR L04401
DI 10.1029/2011GL050655
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 899MT
UT WOS:000300820700001
ER
PT J
AU Helmboldt, JF
Lazio, TJW
Intema, HT
Dymond, KF
AF Helmboldt, J. F.
Lazio, T. J. W.
Intema, H. T.
Dymond, K. F.
TI A new technique for spectral analysis of ionospheric TEC fluctuations
observed with the Very Large Array VHF system: From QP echoes to MSTIDs
SO RADIO SCIENCE
LA English
DT Article
ID NIGHTTIME MIDLATITUDE IONOSPHERE; SPORADIC-E EXPERIMENT; INSTABILITY
AB We have used a relatively long, contiguous VHF observation of a bright cosmic radio source (Cygnus A) with the Very Large Array (VLA) through the nighttime, midlatitude ionosphere to demonstrate the phenomena observable with this instrument. In a companion paper, we showed that the VLA can detect fluctuations in total electron content (TEC) with amplitudes of <= 10(-3) TECU and can measure TEC gradients with a precision of about 2 x 10(-4) TECU km(-1). We detail two complementary techniques for producing spectral analysis of these TEC gradient measurements. The first is able to track individual waves with wavelengths of about half the size of the array (similar to 20 km) or more. This technique was successful in detecting and characterizing many medium-scale traveling ionospheric disturbances (MSTIDs) seen intermittently throughout the night and has been partially validated using concurrent GPS measurements. Smaller waves are also seen with this technique at nearly all times, many of which move in similar directions as the detected MSTIDs. The second technique allows for the detection and statistical description of the properties of groups of waves moving in similar directions with wavelengths as small as 5 km. Combining the results of both spectral techniques, we found a class of intermediate and small scale waves which are likely the quasi-periodic (QP) echoes that have been observed to occur within sporadic-E (E-s) layers. We find two distinct populations of these waves. The members of one population are coincident in time with MSTIDs and are consistent with being generated within E-s layers by the E-F coupling instability. The other population seems more influenced by the neutral wind, similar to the predominant types of QP echoes found by the Sporadic-E Experiments over Kyushu (SEEK). We have also found that the spectra of background (i.e., isotropic) fluctuations can be interpreted as the sum of two turbulent components with maximum scales of about 300 km and 10 km.
C1 [Helmboldt, J. F.; Dymond, K. F.] USN, Res Lab, Washington, DC 20375 USA.
[Lazio, T. J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA.
[Intema, H. T.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
RP Helmboldt, JF (reprint author), USN, Res Lab, Code 7213,4555 Overlook Ave SW, Washington, DC 20375 USA.
EM joe.helmboldt@nrl.navy.mil; joseph.lazio@jpl.nasa.gov; hintema@nrao.edu;
kenneth.dymond@nrl.navy.mil
RI Helmboldt, Joseph/C-8105-2012; Intema, Huib/D-1438-2012;
OI Intema, Huib/0000-0002-5880-2730; Dymond, Kenneth/0000-0001-8060-9016
FU National Aeronautics and Space Administration
FX The authors would like to thank the referees for useful comments and
suggestions. Basic research in astronomy at the Naval Research
Laboratory is supported by 6.1 base funding. The VLA was operated by the
National Radio Astronomy Observatory which is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc. Part of this research was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
NR 26
TC 17
Z9 17
U1 1
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0048-6604
EI 1944-799X
J9 RADIO SCI
JI Radio Sci.
PD FEB 18
PY 2012
VL 47
AR RS0L02
DI 10.1029/2011RS004787
PG 21
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
GA 899PE
UT WOS:000300827500001
ER
PT J
AU Robertson, K
Furukawa, Y
Underwood, A
Black, L
Liu, JL
AF Robertson, Kelly
Furukawa, Yoko
Underwood, Alison
Black, Lindsay
Liu, Jinny L.
TI Deletion of the Hoc and Soc capsid proteins affects the surface and
cellular uptake properties of bacteriophage T4 derived nanoparticles
SO BIOCHEMICAL AND BIOPHYSICAL RESEARCH COMMUNICATIONS
LA English
DT Article
DE T4 NPs; Hoc; Soc; Zeta potentials; Cellular uptake
ID MOLECULAR ARCHITECTURE; HEAD; PARTICLES; PHAGE-T4; DELIVERY; DOMAINS
AB Recently the use of engineered viral scaffolds in biotechnology and medical applications has been increasing dramatically. T4 phage capsid derived nanoparticles (NPs) have potential advantages as sensors and in biotechnology. These applications require that the physical properties and cellular uptake of these NPs be understood. In this study we used a T4 deletion mutant to investigate the effects of removing both the Hoc and Soc proteins from the capsid surface on T4 tailless NPs. The surface charge, zeta potential, size, and cellular uptake efficiencies for both the T4 NP and T4 Delta Hoc Delta Soc NP mutant were measured and compared using dynamic light scattering and flow cytometry and significant differences were detected. Published by Elsevier Inc.
C1 [Robertson, Kelly; Liu, Jinny L.] USN, Res Lab, Ctr Bio Mol Sci & Engn, Washington, DC 20375 USA.
[Furukawa, Yoko] USN, Res Lab, Seafloor Sci Branch, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA.
[Black, Lindsay] Univ Maryland, Sch Med, Dept Biochem, Baltimore, MD 21230 USA.
RP Liu, JL (reprint author), USN, Res Lab, Ctr Bio Mol Sci & Engn, 4555 Overlook Ave SW, Washington, DC 20375 USA.
EM jinny.liu@nrl.navy.mil
RI Furukawa, Yoko/B-3099-2013
FU NRL
FX We thank Drs. Patricia Legler and Stella North for their comments on the
manuscript. This work is supported by NRL 6.2 base program. The opinions
expressed here are those of authors and do not represent those of the US
Navy, the US Department of Defense, or the US government.
NR 21
TC 4
Z9 4
U1 0
U2 4
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0006-291X
J9 BIOCHEM BIOPH RES CO
JI Biochem. Biophys. Res. Commun.
PD FEB 17
PY 2012
VL 418
IS 3
BP 537
EP 540
DI 10.1016/j.bbrc.2012.01.061
PG 4
WC Biochemistry & Molecular Biology; Biophysics
SC Biochemistry & Molecular Biology; Biophysics
GA 900XL
UT WOS:000300925300017
PM 22285187
ER
PT J
AU Jensen, AA
Thompson, AM
Schmidlin, FJ
AF Jensen, Anders A.
Thompson, Anne M.
Schmidlin, F. J.
TI Classification of Ascension Island and Natal ozonesondes using
self-organizing maps
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID TROPICAL SOUTH-ATLANTIC; TROPOSPHERIC OZONE MAXIMUM; MARINE
BOUNDARY-LAYER; DEEP CONVECTION; WAVE-ONE; TRANSPORT; AFRICA; OCEAN;
PACIFIC; TRACE
AB Ozone profiles from balloon-borne ozonesondes are used for development of satellite algorithms and in chemistry-climate model initialization, assimilation and evaluation. An important issue in the application of these profiles is how best to treat variations where varying photochemical and dynamical influences can cause the ozone mixing ratio in the tropospheric segments of the profile to change by of a factor of 2-3 within a day. Clustering techniques are an ideal way to approach the statistical classification of profile data and we apply self-organizing maps to tropical tropospheric SHADOZ data, hypothesizing that the data will sort according to various influences on ozone, namely anthropogenic sources like biomass burning, meteorological conditions, and stratospheric or extra-tropical intrusions. Self-organizing maps, that use a learning algorithm to reveal the most prominent features of a data set according to a specified number of clusters, have been determined for the 1998-2009 SHADOZ profiles over Ascension Island (512 profiles, 7.98 degrees S, 14.42 degrees W) and Natal, Brazil (425 profiles, 5.42 degrees S, 35.38 degrees W). The 2 x 2 self-organizing map, which creates 4 clusters, reveals that deviations from the average ozone in the free troposphere include both increased ozone resulting from seasonal biomass burning in Africa and locally reduced ozone brought about by convective lifting of unpolluted boundary-layer air. Expanding to a 4 x 4 self-organizing map shows how biomass burning influences the yearly cycle of tropospheric ozone at Ascension Island and captures the seasonality of ozone at both Ascension Island and Natal. Comparing Ascension Island and Natal using a 4 x 4 self-organizing map at each site reveals similarities in mid-tropospheric ozone, but shows differences in lower-tropospheric ozone due to Ascension Island being closer to African biomass burning and more affected by descent from the mean Walker circulation, with less convective activity, than Natal.
C1 [Jensen, Anders A.; Thompson, Anne M.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
[Schmidlin, F. J.] NASA, Wallops Flight Facil, Goddard Space Flight Ctr, Wallops Isl, VA 23337 USA.
RP Jensen, AA (reprint author), Penn State Univ, Dept Meteorol, 413 Walker Bldg, University Pk, PA 16802 USA.
EM amt16@psu.edu
RI Thompson, Anne /C-3649-2014
OI Thompson, Anne /0000-0002-7829-0920
FU Earth and Environmental Systems Institute (EESI) through Pennsylvania
State University; NASA SHADOZ [NNX09AJ23G]
FX This research was supported by the Earth and Environmental Systems
Institute (EESI) Environmental Scholar fund through Pennsylvania State
University and the NASA SHADOZ grant NNX09AJ23G for which M. J. Kurylo
and K. W. Jucks are thanked. We are grateful to the years of excellent
sounding data from Russell Yon (Ascension Island), Neusa M. Paes Leme
and Francisco DaSilva (INPE, Brazil). Conversations with Chris
Nowotarski were exceptionally helpful.
NR 56
TC 11
Z9 11
U1 0
U2 8
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 FEB 17
PY 2012
VL 117
AR D04302
DI 10.1029/2011JD016573
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 899NE
UT WOS:000300821900002
ER
PT J
AU Gomez, RM
Nedoluha, GE
Neal, HL
McDermid, IS
AF Gomez, R. Michael
Nedoluha, Gerald E.
Neal, Helen L.
McDermid, I. Stuart
TI The fourth-generation Water Vapor Millimeter-Wave Spectrometer
SO RADIO SCIENCE
LA English
DT Article
ID MIDDLE ATMOSPHERE; RADIOMETER
AB For 20 years the Naval Research Laboratory has been making continuous water vapor profile measurements at 22.235 GHz with the Water Vapor Millimeter-Wave Spectrometer (WVMS) instruments, with the program expanding from one to three instruments in the first 6 years. Since the initial deployments there have been gradual improvements in the instrument design which have improved data quality and reduced maintenance requirements. Recent technological developments have made it possible to entirely redesign the instrument and improve not only the quality of the measurements but also the capability of the instrument. We present the fourth-generation instrument now operating at Table Mountain, California, which incorporates the most recent advances in microwave radiometry. This instrument represents the most significant extension of our measurement capability to date, enabling us to measure middle atmospheric water vapor from similar to 26-80 km.
C1 [Gomez, R. Michael; Nedoluha, Gerald E.] USN, Remote Sensing Div, Res Lab, Washington, DC 20375 USA.
[Neal, Helen L.] Computat Phys Inc, Springfield, VA 22151 USA.
[McDermid, I. Stuart] Jet Prop Lab, Table Mt Facil, Wrightwood, CA 92397 USA.
RP Gomez, RM (reprint author), USN, Remote Sensing Div, Res Lab, Code 7227,4555 Overlook Ave SW, Washington, DC 20375 USA.
EM mike.gomez@nrl.navy.mil
FU Mauna Loa Observatory; NASA; Naval Research Laboratory; staff at the
Table Mountain Facility
FX We wish to thank the staff at the Table Mountain Facility and the Mauna
Loa Observatory for their assistance and support. This work is sponsored
by NASA under the Upper Atmosphere Research Program and the Naval
Research Laboratory.
NR 12
TC 3
Z9 3
U1 1
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0048-6604
J9 RADIO SCI
JI Radio Sci.
PD FEB 16
PY 2012
VL 47
AR RS1010
DI 10.1029/2011RS004778
PG 11
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
GA 899PC
UT WOS:000300827300001
ER
PT J
AU Helmboldt, JF
Lazio, TJW
Intema, HT
Dymond, KF
AF Helmboldt, J. F.
Lazio, T. J. W.
Intema, H. T.
Dymond, K. F.
TI High-precision measurements of ionospheric TEC gradients with the Very
Large Array VHF system
SO RADIO SCIENCE
LA English
DT Article
AB We have used a relatively long, contiguous VHF observation of a bright cosmic radio source (Cygnus A) with the Very Large Array (VLA) to demonstrate the capability of this instrument to study the ionosphere. This interferometer, and others like it, can observe ionospheric total electron content (TEC) fluctuations on a much wider range of scales than is possible with many other instruments. We have shown that with a bright source, the VLA can measure differential TEC values between pairs of antennas (delta TEC) with a precision of 3 x 10(-4) TECU. Here, we detail the data reduction and processing techniques used to achieve this level of precision. In addition, we demonstrate techniques for exploiting these high-precision delta TEC measurements to compute the TEC gradient observed by the array as well as small-scale fluctuations within the TEC gradient surface. A companion paper details specialized spectral analysis techniques used to characterize the properties of wave-like fluctuations within this data.
C1 [Helmboldt, J. F.; Dymond, K. F.] USN, Res Lab, Washington, DC 20375 USA.
[Lazio, T. J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA.
[Intema, H. T.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
RP Helmboldt, JF (reprint author), USN, Res Lab, Code 7213,4555 Overlook Ave SW, Washington, DC 20375 USA.
EM joe.helmboldt@nrl.navy.mil; joseph.lazio@jpl.nasa.gov; hintema@nrao.edu;
kenneth.dymond@nrl.navy.mil
RI Helmboldt, Joseph/C-8105-2012; Intema, Huib/D-1438-2012
OI Intema, Huib/0000-0002-5880-2730
FU 6.1 base funding; National Aeronautics and Space Administration
FX The authors would like to thank the referees for useful comments and
suggestions. Basic research in astronomy at the Naval Research
Laboratory is supported by 6.1 base funding. The VLA was operated by the
National Radio Astronomy Observatory which is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc. Part of this research was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
NR 16
TC 10
Z9 10
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0048-6604
J9 RADIO SCI
JI Radio Sci.
PD FEB 16
PY 2012
VL 47
AR RS0K02
DI 10.1029/2011RS004883
PG 13
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences; Remote Sensing; Telecommunications
GA 899PC
UT WOS:000300827300002
ER
PT J
AU Liu, DY
Jolliff, BL
Zeigler, RA
Korotev, RL
Wan, YS
Xie, HQ
Zhang, YH
Dong, CY
Wang, W
AF Liu, Dunyi
Jolliff, Bradley L.
Zeigler, Ryan A.
Korotev, Randy L.
Wan, Yushan
Xie, Hangqiang
Zhang, Yuhai
Dong, Chunyan
Wang, Wei
TI Comparative zircon U-Pb geochronology of impact melt breccias from
Apollo 12 and lunar meteorite SaU 169, and implications for the age of
the Imbrium impact
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE SHRIMP U-Pb analysis; impact-melt breccia; Apollo 12; SaU 169; Imbrium;
Moon
ID PROSPECTOR GAMMA-RAY; DECAY CONSTANTS; EVOLUTION; CATACLYSM; HISTORY;
ORIGIN; MOON; GEOCHEMISTRY; SPECTROMETER; STRATIGRAPHY
AB The ages of zircons from high-Th impact-melt breccias (IMBs) from meteorite Sayh al Uhaymir (SaU) 169 and from rock fragments in soil samples from Apollo 12 have been determined using the SHRIMP-II ion microprobe. The IMBs are very similar to each other in chemistry, mineralogy and texture, and the zircons from the KREEP-rich (high-Th) crystalline impact melt have similar U and Th contents and identical ages, within uncertainties, of 3920 +/- 13 (2 sigma) Ma (SaU 169) and 3914 +/- 7 (2 sigma) Ma (Apollo 12). The age results support the idea that the high-Th IMBs (Apollo 12 and SaU 169) formed in the same impact event. The similarity of composition and age suggest that SaU 169 and the high-Th IMB fragments of Apollo 12 originated from the same area of the Procellarum KREEP Terrane. We interpret the age of zircon grains in the Apollo 12 high-Th IMB as a precise and direct determination of the age of the Imbrium impact. This age is significantly older than the commonly cited age of 3.85 Ga but is similar to recent determinations from SIMS U-Pb dating of Apollo 14 apatite grains and with anticipated revision of ages by Ar-40-Ar-39 and Rb-87-Sr-86. The present zircon Pb-207-Pb-206 age is the first direct zircon age determination of the Imbrium impact event from an Apollo sample. Previous measurements of zircon ages of Apollo IMBs have recorded events pre-dating the Imbrium basin-forming event (C) 2011 Elsevier B.V. All rights reserved.
C1 [Jolliff, Bradley L.; Zeigler, Ryan A.; Korotev, Randy L.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA.
[Jolliff, Bradley L.; Zeigler, Ryan A.; Korotev, Randy L.] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA.
[Liu, Dunyi; Wan, Yushan; Xie, Hangqiang; Zhang, Yuhai; Dong, Chunyan; Wang, Wei] Chinese Acad Geol Sci, Inst Geol, Beijing SHRIMP Ctr, Beijing, Peoples R China.
[Zeigler, Ryan A.] NASA, ARES Acquisit & Curat, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Jolliff, BL (reprint author), Washington Univ, Dept Earth & Planetary Sci, 1 Brookings Dr, St Louis, MO 63130 USA.
EM blj@wustl.edu
FU NASA [NNG04GG10G]; Ministry of Science and Technology of China
[2009IM030800]; McDonnell Center for the Space Sciences
FX We thank NASA for support through grant NNG04GG10G (RLK). We also
acknowledge the Ministry of Science and Technology of China for support
through grant 2009IM030800. We are grateful for support from the
McDonnell Center for the Space Sciences, which enabled BLJ and RAZ to
visit the SHRIMP-II lab in Beijing and provided seed funds for this
collaboration. We thank Beda Hoffman and the Natural History Museum of
Bern for providing the SaU 169 samples for analysis. We thank R. T.
Pidgeon for assistance during preparation of the manuscript. The
manuscript was greatly improved by comments from reviews by Marc Norman
and an anonymous reviewer.
NR 46
TC 28
Z9 29
U1 3
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 FEB 15
PY 2012
VL 319
BP 277
EP 286
DI 10.1016/j.epsl.2011.12.014
PG 10
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 913WW
UT WOS:000301909100029
ER
PT J
AU Kokkila, SI
Bera, PP
Francisco, JS
Lee, TJ
AF Kokkila, Sara I.
Bera, Partha P.
Francisco, Joseph S.
Lee, Timothy J.
TI A group increment scheme for infrared absorption intensities of
greenhouse gases
SO JOURNAL OF MOLECULAR STRUCTURE
LA English
DT Article
DE IR intensities; ab initio calculations; Additivity models; Global
warming molecules; Hydrofluorocarbons; Hydrofluoroethers
ID GLOBAL WARMING POTENTIALS; GAUSSIAN BASIS FUNCTIONS; FIRST-ROW ATOMS;
HYDROFLUOROETHERS HFES; MOLECULAR CALCULATIONS; RADIATIVE EFFICIENCY;
HYDROFLUOROCARBONS; ALTERNATIVES
AB A molecule's absorption in the atmospheric infrared (IR) window (IRW) is an indicator of its efficiency as a greenhouse gas. A model for estimating the absorption of a fluorinated molecule within the IRW was developed to assess its radiative impact. This model will be useful in comparing different hydrofluorocarbons and hydrofluoroethers contribution to global warming. The absorption of radiation by greenhouse gases, in particular hydrofluoroethers and hydrofluorocarbons, was investigated using ab initio quantum mechanical methods. Least squares regression techniques were used to create a model based on this data. The placement and number of fluorines in the molecule were found to affect the absorption in the IR window and were incorporated into the model. Several group increment models are discussed. An additive model based on one-carbon groups is found to work satisfactorily in predicting the ab initio calculated vibrational intensities. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Bera, Partha P.; Lee, Timothy J.] NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
[Kokkila, Sara I.] Coll St Benedict, St Joseph, MN 56374 USA.
[Kokkila, Sara I.] St Johns Univ, St Joseph, MN 56374 USA.
[Francisco, Joseph S.] Purdue Univ, Dept Chem, W Lafayette, IN 47907 USA.
[Francisco, Joseph S.] Purdue Univ, Dept Earth & Atmospher Sci, W Lafayette, IN 47907 USA.
RP Lee, TJ (reprint author), NASA, Ames Res Ctr, Mountain View, CA 94035 USA.
EM Timothy.J.Lee@nasa.gov
RI Lee, Timothy/K-2838-2012; Bera, Partha /K-8677-2012;
OI Kokkila Schumacher, Sara/0000-0002-2338-4815
FU NASA Ames Research Center; NASA
FX This paper is dedicated to Professor Boris Galabov on the occasion of
his 70th birthday, who has made seminal contributions to the study of IR
intensities. SIK gratefully acknowledges an Undergraduate Student
Research Program (USRP) summer fellowship at the NASA Ames Research
Center. PPB gratefully acknowledges a NASA Postdoctoral Program
Fellowship award. Helpful conversations with Dr. Jeff Cuzzi are
gratefully acknowledged.
NR 32
TC 1
Z9 1
U1 3
U2 14
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-2860
J9 J MOL STRUCT
JI J. Mol. Struct.
PD FEB 15
PY 2012
VL 1009
SI SI
BP 89
EP 95
DI 10.1016/j.molstruc.2011.11.048
PG 7
WC Chemistry, Physical
SC Chemistry
GA 905ZY
UT WOS:000301315900013
ER
PT J
AU Lin, ZW
Adams, JH
Barghouty, AF
Randeniya, SD
Tripathi, RK
Watts, JW
Yepes, PP
AF Lin, Z. W.
Adams, J. H., Jr.
Barghouty, A. F.
Randeniya, S. D.
Tripathi, R. K.
Watts, J. W.
Yepes, P. P.
TI Comparisons of several transport models in their predictions in typical
space radiation environments
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Transport code; Space radiation; Radiation shielding; Solar particle
events; Galactic cosmic rays
ID ACCURATE UNIVERSAL PARAMETERIZATION; ABSORPTION CROSS-SECTIONS; CODE
AB We have used several transport codes to calculate dose and dose equivalent values as well as the particle spectra behind a slab or inside a spherical shell shielding in typical space radiation environments. Two deterministic codes, HZETRN and UPROP, and two Monte Carlo codes, FLUKA and Geant4, are included. A soft solar particle event, a hard solar particle event, and a solar minimum galactic cosmic rays environment are considered; and the shielding material is either aluminum or polyethylene. We find that the dose values and particle spectra from HZETRN are in general rather consistent with Geant4 except for neutrons. The dose equivalent values from HZETRN and Geant4 are not far from each other, but the HZETRN values behind shielding are often lower than the Geant4 values. Results from FLUKA and Geant4 are mostly consistent for considered cases. However, results from the legacy code UPROP are often quite different from the other transport codes, partly due to its non-consideration of neutrons. Comparisons for the spherical shell geometry exhibit the same qualitative features as for the slab geometry. In addition, results from both deterministic and Monte Carlo transport codes show that the dose equivalent inside the spherical shell decreases from the center to the inner surface and this decrease is large for solar particle events; consistent with an earlier study based on deterministic radiation transport results. This study demonstrates both the consistency and inconsistency among these transport models in their typical space radiation predictions; further studies will be required to pinpoint the exact physics modules in these models that cause the differences and thus may be improved. (C) 2011 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Lin, Z. W.] E Carolina Univ, Dept Phys, Greenville, NC 27858 USA.
[Adams, J. H., Jr.; Barghouty, A. F.; Watts, J. W.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
[Randeniya, S. D.] Univ Texas MD Anderson Canc Ctr, Houston, TX 77030 USA.
[Tripathi, R. K.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Watts, J. W.] Univ Alabama, CSPAR, Huntsville, AL 35805 USA.
[Yepes, P. P.] Rice Univ, Dept Phys, Houston, TX 77005 USA.
RP Lin, ZW (reprint author), E Carolina Univ, Dept Phys, C-209 Howell Sci Complex, Greenville, NC 27858 USA.
EM linz@ecu.edu; James.h.adams@nasa.gov; Abdulnasser.F.Barghouty@nasa.gov;
kdrandeniya@mdanderson.org; Ram.K.Tripathi@nasa.gov; yepes@rice.edu
FU NASA [NNM07AC99P]
FX Z.W.L. gratefully acknowledges support provided under NASA Contract No.
NNM07AC99P.
NR 25
TC 11
Z9 11
U1 0
U2 4
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
J9 ADV SPACE RES
JI Adv. Space Res.
PD FEB 15
PY 2012
VL 49
IS 4
BP 797
EP 806
DI 10.1016/j.asr.2011.11.025
PG 10
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 905YO
UT WOS:000301312300018
ER
PT J
AU Sayer, AM
Hsu, NC
Bettenhausen, C
Ahmad, Z
Holben, BN
Smirnov, A
Thomas, GE
Zhang, J
AF Sayer, A. M.
Hsu, N. C.
Bettenhausen, C.
Ahmad, Z.
Holben, B. N.
Smirnov, A.
Thomas, G. E.
Zhang, J.
TI SeaWiFS Ocean Aerosol Retrieval (SOAR): Algorithm, validation, and
comparison with other data sets
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID OPTICAL DEPTH; ATMOSPHERIC CORRECTION; DATA-ASSIMILATION; SPECTRAL
RADIANCES; MODIS; SATELLITE; AERONET; LAND; DUST; REFLECTANCE
AB The Sea-viewing Wide Field-of-view Sensor (SeaWiFS) provides a well-calibrated 13-year (1997-2010) record of top-of-atmosphere radiance, suitable for use in retrieval of atmospheric aerosol optical depth (AOD). This paper presents and validates a SeaWiFS Ocean Aerosol Retrieval (SOAR) algorithm, which retrieves the AOD at 550 nm and the partition of aerosol particle volume between fine and coarse modes. The algorithm has been applied over water to the whole SeaWiFS record. The data set includes quality flags to identify those retrievals suitable for quantitative use. SOAR has been validated against Aerosol Robotic Network (AERONET) and Maritime Aerosol Network (MAN) data and found to compare well (correlation 0.86 at 550 nm and 0.88 at 870 nm for AERONET, and 0.87 at 550 nm and 0.85 at 870 nm for MAN, using recommended quality control settings). These comparisons are used to identify the typical level of uncertainty on the AOD, estimated as 0.03 + 15% at 550 nm and 0.03 + 10% at 870 nm. The data set also includes the (A) over circle ngstrom exponent, although as expected this is noisy for low aerosol loadings (correlation 0.50; 0.78 for points where the AOD at 550 nm is 0.3 or more). Retrieved AOD is compared with colocated observations from other satellite sensors; regional and seasonal patterns are found to be common between all data sets, and differences generally linked to factors such as cloud screening and retrieval assumptions. Citation: Sayer, A. M., N. C. Hsu, C. Bettenhausen, Z. Ahmad, B. N. Holben, A. Smirnov, G. E. Thomas, and J. Zhang (2012), SeaWiFS Ocean Aerosol Retrieval (SOAR): Algorithm, validation, and comparison with other data sets, J. Geophys. Res., 117, D03206, doi:10.1029/2011JD016599.
C1 [Sayer, A. M.; Hsu, N. C.; Bettenhausen, C.; Ahmad, Z.; Holben, B. N.; Smirnov, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Thomas, G. E.] Univ Oxford, Oxford OX1 3PU, England.
[Zhang, J.] Univ N Dakota, Dept Atmospher Sci, Grand Forks, ND 58202 USA.
[Sayer, A. M.] Univ Space Res Assoc, Columbia, MD USA.
[Bettenhausen, C.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Ahmad, Z.] Sci & Data Syst Inc, Silver Spring, MD USA.
[Smirnov, A.] Sigma Space Corp, Lanham, MD USA.
RP Sayer, AM (reprint author), Univ Space Res Assoc, Columbia, MD USA.
EM andrew.sayer@nasa.gov
RI Smirnov, Alexander/C-2121-2009; Sayer, Andrew/H-2314-2012; Hsu, N.
Christina/H-3420-2013
OI Smirnov, Alexander/0000-0002-8208-1304; Sayer,
Andrew/0000-0001-9149-1789;
FU NASA
FX This work was supported by a grant from the NASA MEaSUREs program,
managed by Martha Maiden. SeaWiFS level 1a data, the SeaDAS software,
and NCEP meteorological fields were obtained from the SeaWiFS Ocean
Biology Processing Group data distribution service. GlobAerosol was an
ESA Data User Element project. The Naval Research Laboratory are thanked
for the DA-MODIS data. MODIS data were obtained from the NASA LAADS, and
MISR from the NASA Langley ASDC. The AERONET and MAN PIs are thanked for
the creation and maintenance of the Sun photometer data records. The
authors thank M. Chin, T. Diehl, R. A. Kahn, R. C. Levy, S. Mattoo, L.
A. Remer, and Q. Tan for helpful discussions and comments on the
manuscript. The authors acknowledge the detailed and constructive
comments of three anonymous reviewers, whose suggestions strengthened
the manuscript.
NR 71
TC 28
Z9 28
U1 0
U2 9
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 FEB 15
PY 2012
VL 117
AR D03206
DI 10.1029/2011JD016599
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 899MY
UT WOS:000300821200001
ER
PT J
AU Xiong, S
Briggs, MS
Connaughton, V
Fishman, GJ
Tierney, D
Fitzpatrick, G
Foley, S
Guiriec, S
Holzworth, RH
Hutchins, ML
AF Xiong, S.
Briggs, M. S.
Connaughton, V.
Fishman, G. J.
Tierney, D.
Fitzpatrick, G.
Foley, S.
Guiriec, S.
Holzworth, R. H.
Hutchins, M. L.
TI Location prediction of electron TGFs
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID GAMMA-RAY FLASHES; RUNAWAY BREAKDOWN; SPRITES; THUNDERSTORM; AIR
AB Terrestrial Gamma-ray Flashes (TGFs) are brief pulses of energetic radiation that correlate with thunderstorms and lightning. Most TGFs are observed as gamma-ray pulses; less frequently they can be observed as electrons and positrons that travel along the geomagnetic field line from the source to the detector. In this paper we predict where electron TGFs should be observed by tracing geomagnetic field lines from likely TGF sources and determining the intersections with satellite orbits. TGF source locations are based upon lightning maps by the Lightning Imaging Sensor (LIS) and the Optical Transient Detector (OTD). Predictions are made both for existing spacecraft with instruments observing TGFs and for other orbits. We compare the predictions to the locations of TGFs that have been observed as electron TGFs. 12 of the 13 known electron TGFs are within the predicted high-rate regions. Based on the predicted location maps of electron TGFs, we find that electron TGFs should sometimes be observed above areas with low lightning activity and that electron TGFs are best observed at low altitudes (below approximately 1000 km).
C1 [Fishman, G. J.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
[Tierney, D.; Fitzpatrick, G.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Foley, S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Holzworth, R. H.; Hutchins, M. L.] Univ Washington, Seattle, WA 98195 USA.
[Xiong, S.; Briggs, M. S.; Connaughton, V.; Guiriec, S.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
RP Xiong, S (reprint author), NSSTC, 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM shaolin.xiong@uah.edu
FU NASA in the United States; BMWi/DLR in Germany; Fermi Guest Investigator
Program
FX We thank the reviewers for their comments that improved this paper. The
Fermi GBM Collaboration acknowledges support for GBM development,
operations, and data analysis from NASA in the United States and from
BMWi/DLR in Germany. This work was supported in part by the Fermi Guest
Investigator Program. The v2.2 gridded satellite lightning data were
produced by the NASA LIS/OTD Science Team (Principal Investigator, Hugh
J. Christian, NASA / Marshall Space Flight Center) and are available
from the Global Hydrology Resource Center (http://ghrc.msfc.nasa.gov).
The authors wish to thank the World Wide Lightning Location Network
(http://wwlln.net), a collaboration among over 50 universities and
institutions, for providing the lightning location data used in this
paper. The authors appreciate David M. Smith for helpful comments. SF
acknowledges the support of the Irish Research Council for Science,
Engineering and Technology, cofunded by Marie Curie Actions under FP7.
NR 31
TC 3
Z9 3
U1 0
U2 7
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 FEB 15
PY 2012
VL 117
AR A02309
DI 10.1029/2011JA017085
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 899OH
UT WOS:000300825100001
ER
PT J
AU Mishchenko, MI
Dlugach, JM
AF Mishchenko, Michael I.
Dlugach, Janna M.
TI Adhesion of mineral and soot aerosols can strongly affect their
scattering and absorption properties
SO OPTICS LETTERS
LA English
DT Article
ID T-MATRIX; RADIATIVE PROPERTIES; PARTICLES; HYGROSCOPICITY; MORPHOLOGY
AB We use the numerically exact superposition T-matrix method to compute the optical cross sections and the Stokes scattering matrix for polydisperse mineral aerosols (modeled as homogeneous spheres) covered with a large number of much smaller soot particles. These results are compared with the Lorenz-Mie results for a uniform external mixture of mineral and soot aerosols. We show that the effect of soot particles adhering to large mineral particles can be to change the extinction and scattering cross sections and the asymmetry parameter quite substantially. The effect on the phase function and degree of linear polarization can be equally significant. (C) 2012 Optical Society of America
C1 [Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Dlugach, Janna M.] Natl Acad Sci Ukraine, Main Astron Observ, UA-03680 Kiev, Ukraine.
RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM michael.i.mishchenko@nasa.gov
RI Mishchenko, Michael/D-4426-2012
FU NASA; National Academy of Sciences of Ukraine
FX We thank Ping Yang and an anonymous referee for constructive reviews.
This research was partly funded by the NASA Radiation Sciences Program
managed by Hal Maring and by the NASA Remote Sensing Theory Program
managed by Lucia Tsaoussi. We also acknowledge support from the National
Academy of Sciences of Ukraine under the Main Astronomical Observatory
GRAPE/GPU/GRID Computing Cluster Project.
NR 19
TC 7
Z9 7
U1 1
U2 13
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 0146-9592
EI 1539-4794
J9 OPT LETT
JI Opt. Lett.
PD FEB 15
PY 2012
VL 37
IS 4
BP 704
EP 706
PG 3
WC Optics
SC Optics
GA 898AF
UT WOS:000300706500087
PM 22344154
ER
PT J
AU Weng, QH
Quattrochi, DA
Carlson, TN
AF Weng, Qihao
Quattrochi, Dale A.
Carlson, Toby N.
TI Remote sensing of urban environments: Special issue Preface
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Editorial Material
C1 [Weng, Qihao] Indiana State Univ, Ctr Urban & Environm Change, Terre Haute, IN 47809 USA.
[Quattrochi, Dale A.] NASA, George C Marshall Space Flight Ctr, Redstone Arsenal, AL USA.
[Carlson, Toby N.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
RP Weng, QH (reprint author), Indiana State Univ, Ctr Urban & Environm Change, Terre Haute, IN 47809 USA.
EM qweng@indstate.edu
OI Weng, Qihao/0000-0002-2498-0934
NR 12
TC 2
Z9 2
U1 1
U2 18
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 FEB 15
PY 2012
VL 117
BP 1
EP 2
DI 10.1016/j.rse.2011.08.005
PG 2
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 894WX
UT WOS:000300459300001
ER
PT J
AU Roberts, DA
Quattrochi, DA
Hulley, GC
Hook, SJ
Green, RO
AF Roberts, Dar A.
Quattrochi, Dale A.
Hulley, Glynn C.
Hook, Simon J.
Green, Robert O.
TI Synergies between VSWIR and TIR data for the urban environment: An
evaluation of the potential for the Hyperspectral Infrared Imager
(HyspIRI) Decadal Survey mission
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE HyspIRI; Urban remote sensing; Spectral Mixture Analysis; Land surface
temperature; Spectroscopy
ID SPECTRAL MIXTURE ANALYSIS; LAND-SURFACE TEMPERATURE; IMAGING
SPECTROMETER AVIRIS; SENSIBLE HEAT-FLUX; IMPERVIOUS SURFACE;
WATER-VAPOR; MULTISENSOR DATA; VEGETATION; EMISSIVITY; REFLECTANCE
AB This study provides an introduction to the HyspIRI mission a National Research Council "Decadal Survey" mission that combines a 213 channel visible, near-infrared and shortwave infrared (VSWIR) imaging spectrometer with an 8 channel multispectral thermal infrared (TIR) instrument and evaluates some of its potential in urban science. Potential synergies between VSWIR and TIR data are explored using analogous airborne data acquired over the Santa Barbara metropolitan region in June, 2008. These data were analyzed at both their native spatial resolutions (7.5 m VSWIR and 15 m TIR), and aggregated 60 m spatial resolution similar to HyspIRI. A spectral library of dominant urban materials (e.g., grass, trees, soil, roof types, roads) was developed from field and airborne-measured spectra using Multiple-Endmember Spectral Mixture Analysis (MESMA) and used to map fractions of impervious, soil, green vegetation (CV, e.g., trees, lawn) and non-photosynthetic vegetation (NPV). Land Surface Temperature (LST) and emissivity were also retrieved from the airborne data. Co-located pixels from the VSWIR and TIR airborne data were used to generate reflectance/emissivity spectra for a subset of urban materials. MESMA was used to map GV, NPV, soil and impervious fractions at the different spatial resolutions and compare the fractional estimates across spatial scales. Important surface energy parameters, including albedo, vegetation cover fraction, broadband emissivity and surface temperature were also determined for and evaluated for 14 urban and natural land-cover classes in the region. Fractions were validated using 1 m digital photography.
Fractions for GV and NPV were highly correlated with validation fractions at all spatial scales, producing a near 1:1 relationship but with a <10% overestimate of CV from MESMA. Similar, high correlations were observed for impervious surfaces, although impervious was significantly underestimated in most urban areas and soil overestimated. Comparison of fractions across scales showed high correlation between CV and NPV at 7.5 and 60 m resolution, suggesting that HyspIRI will provide accurate measures of these two measures in urban areas. An inverse relationship between vegetation cover and LST was observed. Albedo proved to be highly variable and poorly correlated with LST. Broadband emissivity was far less variable with high emissivity surfaces (similar to 0.95) including vegetation, water and asphalt, and low emissivity surfaces (<0.95) including selected roof types, beach sands and senesced grasslands. Residential and commercial areas showed a general pattern of increasing LST with increasing impervious fraction with the highest impervious fractions mapped in commercial areas, roads and roofs. Fine scale spatial structure in cover fractions and LST demonstrated important departures from a simple inverse relationship between CV and LST, even at 60 m. The results demonstrate the utility of HyspIRI data for urban studies and provide an insight of what will be possible on a global scale when HyspIRI data become available. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Roberts, Dar A.] Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA.
[Quattrochi, Dale A.] NASA, George C Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL 35812 USA.
[Hulley, Glynn C.; Hook, Simon J.; Green, Robert O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Roberts, DA (reprint author), Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA.
EM dar@geog.ucsb.edu
FU NASA [NNX07AC89G, NNX11AE44G]
FX We wish to thank Michael Toomey and Eliza Bradley for their assistance
in translating polygons from Google Earth to ENVI vector files. We wish
to thank the Jet Propulsion Laboratory for providing radiometrically
calibrated, orthorectified AVIRIS and MASTER data. AVIRIS/MASTER data
analyzed in this study were acquired as part of the NASA North American
Carbon Program (NACP) for research grant NNX07AC89G, Remote-Sensing
methane emissions: field-validation with Seepage from marine, urban, and
submerged-city sources. The analysis was partially supported by a NASA
HyspIRI Preparatory Grant, NNX11AE44G. A portion of this work was
carried out at the Jet Propulsion Laboratory/California Institute of
Technology, Pasadena, California, under contract with NASA We also wish
to thank the reviewers for constructive comments.
NR 65
TC 79
Z9 81
U1 9
U2 79
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 FEB 15
PY 2012
VL 117
BP 83
EP 101
DI 10.1016/j.rse.2011.07.021
PG 19
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 894WX
UT WOS:000300459300008
ER
PT J
AU Moore, TS
Dowell, MD
Franz, BA
AF Moore, Timothy S.
Dowell, Mark D.
Franz, Bryan A.
TI Detection of coccolithophore blooms in ocean color satellite imagery: A
generalized approach for use with multiple sensors
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Ocean color; Classification; Coccolithophores; Optical water types
ID PHYTOPLANKTON FUNCTIONAL-GROUPS; SEA-SURFACE DISTRIBUTION; LATE AUSTRAL
SUMMER; SOUTHERN-OCEAN; EMILIANIA-HUXLEYI; ATLANTIC-OCEAN; VARIABILITY;
DYNAMICS; ALGORITHM; SECTOR
AB A generalized coccolithophore bloom classifier has been developed for use with ocean color imagery. The bloom classifier was developed using extracted satellite reflectance data from SeaWiFS images screened by the default bloom detection mask. In the current application, we extend the optical water type (OWT) classification scheme by adding a new coccolithophore bloom class formed from these extracted reflectances. Based on an in situ coccolithophore data set from the North Atlantic, the detection levels with the new scheme were between 1,500 and 1,800 coccolithophore cells/mL and 43,000 and 78,000 liths/mL The detected bloom area using the OWT method was an average of 1.75 times greater than the default bloom detector based on a collection of SeaWiFS 1 km imagery. The versatility of the scheme is shown with SeaWiFS, MODIS Aqua, CZCS and MERIS imagery at the 1 km scale. The OWT scheme was applied to the daily global SeaWiFS imagery mission data set (years 1997-2010). Based on our results, average annual coccolithophore bloom area was more than two times greater in the southern hemisphere compared to the northern hemisphere with values of 2.00 x 10(6) km(2) and 0.75 x 10(6) km(2), respectively. The new algorithm detects larger bloom areas in the Southern Ocean compared to the default algorithm, and our revised global annual average of 2.75 x 10(6) km(2) is dominated by contributions from the Southern Ocean. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Moore, Timothy S.] Univ New Hampshire, Ocean Proc Anal Lab, Durham, NH 03824 USA.
[Dowell, Mark D.] European Commiss, JRC, Inst Environm & Sustainabil, I-21027 Ispra, VA, Italy.
[Franz, Bryan A.] NASA, Goddard Space Flight Ctr, Ocean Biol Proc Grp, Greenbelt, MD 20771 USA.
RP Moore, TS (reprint author), Univ New Hampshire, Ocean Proc Anal Lab, Morse Hall, Durham, NH 03824 USA.
EM timothy.moore@unh.edu; mark.dowell@jrc.ec.europa.eu;
bryan.a.franz@nasa.gov
RI Franz, Bryan/D-6284-2012
OI Franz, Bryan/0000-0003-0293-2082
FU NASA [NNX08AG80A]
FX This work was supported by NASA grant NNX08AG80A. Thanks to Tim Smyth
for providing the North Atlantic in situ data set that added
significantly to the work. The authors thank the anonymous reviewers for
their time in providing helpful comments and suggestions.
NR 45
TC 29
Z9 30
U1 5
U2 35
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 FEB 15
PY 2012
VL 117
BP 249
EP 263
DI 10.1016/j.rse.2011.10.001
PG 15
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 894WX
UT WOS:000300459300021
ER
PT J
AU Wang, ZS
Schaaf, CB
Chopping, MJ
Strahler, AH
Wang, JD
Roman, MO
Rocha, AV
Woodcock, CE
Shuai, YM
AF Wang, Zhuosen
Schaaf, Crystal B.
Chopping, Mark J.
Strahler, Alan H.
Wang, Jindi
Roman, Miguel O.
Rocha, Adrian V.
Woodcock, Curtis E.
Shuai, Yanmin
TI Evaluation of Moderate-resolution Imaging Spectroradiometer (MODIS) snow
albedo product (MCD43A) over tundra
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE MODIS standard and daily Albedo product; Snow; High latitude tundra;
Spatial representativeness
ID LAND-SURFACE ALBEDO; REFLECTANCE DISTRIBUTION FUNCTION; RADIATION
MEASUREMENT PROGRAM; IN-SITU MEASUREMENTS; BIDIRECTIONAL REFLECTANCE;
CLIMATE MODEL; NADIR REFLECTANCE; BOREAL FORESTS; NORTH-AMERICA; BRDF
MODELS
AB This study assesses the MODIS standard Bidirectional Reflectance Distribution Function (BRDF)/Albedo product, and the daily Direct Broadcast BRDF/Albedo algorithm at tundra locations under large solar zenith angles and high anisotropic diffuse illumination and multiple scattering conditions. These products generally agree with ground-based albedo measurements during the snow cover period when the Solar Zenith Angle (SZA) is less than 70 degrees. An integrated validation strategy, including analysis of the representativeness of the surface heterogeneity, is performed to decide whether direct comparisons between field measurements and 500-m satellite products were appropriate or if the scaling of finer spatial resolution airborne or spaceborne data was necessary. Results indicate that the Root Mean Square Errors (RMSEs) are less than 0.047 during the snow covered periods for all MCD43 albedo products at several Alaskan tundra areas. The MCD43 1-day daily albedo product is particularly well suited to capture the rapidly changing surface conditions during the spring snow melt. Results also show that a full expression of the blue sky albedo is necessary at these large SZA snow covered areas because of the effects of anisotropic diffuse illumination and multiple scattering. In tundra locations with dark residue as a result of fire, the MODIS albedo values are lower than those at the unburned site from the start of snowmelt. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Wang, Zhuosen; Schaaf, Crystal B.; Strahler, Alan H.; Woodcock, Curtis E.] Boston Univ, Ctr Remote Sensing, Dept Geog & Environm, Boston, MA 02215 USA.
[Wang, Zhuosen; Wang, Jindi] Beijing Normal Univ, State Key Lab Remote Sensing Sci, Ctr Remote Sensing, Beijing 100875, Peoples R China.
[Wang, Zhuosen; Wang, Jindi] Beijing Normal Univ, Beijing Key Lab Remote Sensing Environm & Digital, GIS Geog Coll, Beijing 100875, Peoples R China.
[Chopping, Mark J.] Montclair State Univ, Dept Earth & Environm Studies, Montclair, NJ USA.
[Roman, Miguel O.] NASA, Goddard Space Flight Ctr, Terr Informat Syst Lab Code 619, Greenbelt, MD 20771 USA.
[Rocha, Adrian V.] Marine Biol Lab, Ctr Ecosyst, Woods Hole, MA 02543 USA.
[Shuai, Yanmin] Earth Resources Technol Inc, Laurel, MD 20707 USA.
[Schaaf, Crystal B.] Univ Massachusetts, Boston, MA 02125 USA.
RP Wang, ZS (reprint author), Boston Univ, Ctr Remote Sensing, Dept Geog & Environm, Boston, MA 02215 USA.
EM wangzhs@bu.edu
RI Shuai, Yanmin/G-1329-2012; Rocha, Adrian/B-6504-2013; Roman,
Miguel/D-4764-2012
OI Roman, Miguel/0000-0003-3953-319X
FU NASA [NNX09AL03G, NNX08AE94A, NNX11AD58G]; NSF [OPP-0856853,
DEB-0423385]; National Natural Science Foundation of China [40871163]
FX This research was supported by NASA awards NNX09AL03G, NNX08AE94A, and
NNX11AD58G, NSF grants OPP-0856853 and DEB-0423385, National Natural
Science Foundation of China (40871163). The MODIS data were obtained
from the NASA Distributed Active Archive Centers (DAACs). The Landsat
data were obtained from the USGS Earth Resources Observation and Science
(EROS) Center. We also thank Dr. Ellsworth Dutton for providing the ARM
ground data.
NR 98
TC 44
Z9 51
U1 1
U2 22
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD FEB 15
PY 2012
VL 117
BP 264
EP 280
DI 10.1016/j.rse.2011.10.002
PG 17
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 894WX
UT WOS:000300459300022
ER
PT J
AU Goossens, S
Ishihara, Y
Matsumoto, K
Sasaki, S
AF Goossens, Sander
Ishihara, Yoshiaki
Matsumoto, Koji
Sasaki, Sho
TI Local lunar gravity field analysis over the South Pole-Aitken basin from
SELENE farside tracking data
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID MASS ANOMALIES; PROSPECTOR; MISSION; KAGUYA; LINE; MOON; CLEMENTINE;
RESOLUTION; GANYMEDE; SPHERE
AB We present a method with which we determined the local lunar gravity field model over the South Pole-Aitken (SPA) basin on the farside of the Moon by estimating adjustments to a global lunar gravity field model using SELENE tracking data. Our adjustments are expressed in localized functions concentrated over the SPA region in a spherical cap with a radius of 45 degrees centered at (191.1 degrees E, 53.2 degrees S), and the resolution is equivalent to a 150th degree and order spherical harmonics expansion. The new solution over SPA was used in several applications of geophysical analysis. It shows an increased correlation with high-resolution lunar topography in the frequency band l = 40-70, and admittance values are slightly different and more leveled when compared to other, global gravity field models using the same data. The adjustments expressed in free-air anomalies and differences in Bouguer anomalies between the local solution and the a priori global solution correlate with topographic surface features. The Moho structure beneath the SPA basin is slightly modified in our solution, most notably at the southern rim of the Apollo basin and around the Zeeman crater.
C1 [Goossens, Sander; Ishihara, Yoshiaki; Matsumoto, Koji; Sasaki, Sho] Natl Astron Observ Japan, RISE Project, Oshu, Iwate 0230861, Japan.
[Goossens, Sander] NASA, Goddard Space Flight Ctr, CRESST Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
[Goossens, Sander] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21228 USA.
RP Goossens, S (reprint author), Natl Astron Observ Japan, RISE Project, 2-12 Hoshigaoka, Oshu, Iwate 0230861, Japan.
EM sander.j.goossens@nasa.gov; ishihara@miz.nao.ac.jp;
matumoto@miz.nao.ac.jp; sho@miz.nao.ac.jp
RI Ishihara, Yoshiaki/A-8499-2011; Goossens, Sander/K-2526-2015;
OI Goossens, Sander/0000-0002-7707-1128; Ishihara,
Yoshiaki/0000-0002-0375-6300
FU Noriyuki Namiki (PERC, Chiba Institute of Technology, Japan); Takahiro
Iwata (ISAS/JAXA, Japan); Japan Society for the Promotion of Science
[20244073]
FX We thank the Planetary Geodynamics Laboratory of NASA/GSFC for providing
the GEODYN II/SOLVE software, and we are especially grateful to David
Rowlands and Frank Lemoine for discussions concerning the software. We
thank Mark Wieczorek for comments on the manuscript, particularly those
concerning the localization procedures. The localization transformations
applied in this work make extensive use of his SHTOOLS library, which is
freely available from "http://www.ipgp.fr/similar to
wieczor/SHTOOLS/SHTOOLS.html". We also acknowledge support from Noriyuki
Namiki (PERC, Chiba Institute of Technology, Japan) and Takahiro Iwata
(ISAS/JAXA, Japan). Two anonymous reviewers are thanked for their
comments which helped improve this manuscript. All figures were
generated with the free Generic Mapping Tools (GMT) software [Wessel and
Smith, 1991]. This work was supported by Grant-in-Aid for Scientific
Research (to S. S.) (grant 20244073) from the Japan Society for the
Promotion of Science.
NR 39
TC 2
Z9 2
U1 1
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD FEB 14
PY 2012
VL 117
AR E02005
DI 10.1029/2011JE003831
PG 16
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 899OR
UT WOS:000300826100001
ER
PT J
AU Schoepp-Cothenet, B
van Lis, R
Philippot, P
Magalon, A
Russell, MJ
Nitschke, W
AF Schoepp-Cothenet, Barbara
van Lis, Robert
Philippot, Pascal
Magalon, Axel
Russell, Michael J.
Nitschke, Wolfgang
TI The ineluctable requirement for the trans-iron elements molybdenum
and/or tungsten in the origin of life
SO SCIENTIFIC REPORTS
LA English
DT Article
ID MULTIPLE SEQUENCE ALIGNMENT; OXIDATION-STATE; EVOLUTION; PROTEIN;
ENVIRONMENT; ATMOSPHERE; TOOLS
AB An evolutionary tree of key enzymes from the Complex-Iron-Sulfur-Molybdoenzyme (CISM) superfamily distinguishes "ancient" members, i.e. enzymes present already in the last universal common ancestor (LUCA) of prokaryotes, from more recently evolved subfamilies. The majority of the presented subfamilies and, as a consequence, the Molybdo-enzyme superfamily as a whole, appear to have existed in LUCA. The results are discussed with respect to the nature of bioenergetic substrates available to early life and to problems arising from the low solubility of molybdenum under conditions of the primordial Earth.
C1 [Schoepp-Cothenet, Barbara; van Lis, Robert; Nitschke, Wolfgang] Univ Aix Marseille, CNRS, Lab Bioenerget & Ingn Prot BIP, Marseille, France.
[Magalon, Axel] Univ Aix Marseille, CNRS, LCB, Marseille, France.
[Philippot, Pascal] IPGP, Paris, France.
[Russell, Michael J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Nitschke, W (reprint author), Univ Aix Marseille, CNRS, Lab Bioenerget & Ingn Prot BIP, Marseille, France.
EM nitschke@imm.cnrs.fr
OI Nitschke, Wolfgang/0000-0003-2084-3032
FU National Aeronautics and Space Administration
FX MJR's contribution was carried out at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration.
NR 31
TC 29
Z9 29
U1 2
U2 32
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 FEB 13
PY 2012
VL 2
AR 263
DI 10.1038/srep00263
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 896PQ
UT WOS:000300582000002
PM 22355775
ER
PT J
AU Samanta, A
Knyazikhin, Y
Xu, L
Dickinson, RE
Fu, R
Costa, MH
Saatchi, SS
Nemani, RR
Myneni, RB
AF Samanta, Arindam
Knyazikhin, Yuri
Xu, Liang
Dickinson, Robert E.
Fu, Rong
Costa, Marcos H.
Saatchi, Sassan S.
Nemani, Ramakrishna R.
Myneni, Ranga B.
TI Seasonal changes in leaf area of Amazon forests from leaf flushing and
abscission
SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES
LA English
DT Article
ID SPECTRAL VEGETATION INDEXES; LAND-SURFACE; TROPICAL FOREST;
SOUTH-AMERICA; RAIN-FOREST; DRY SEASON; WET SEASON; MODIS; PHENOLOGY;
CLIMATE
AB A large increase in near-infrared (NIR) reflectance of Amazon forests during the light-rich dry season and a corresponding decrease during the light-poor wet season has been observed in satellite measurements. This increase has been variously interpreted as seasonal change in leaf area resulting from net leaf flushing in the dry season or net leaf abscission in the wet season, enhanced photosynthetic activity during the dry season from flushing new leaves and as change in leaf scattering and absorption properties between younger and older leaves covered with epiphylls. Reconciling these divergent views using theory and observations is the goal of this article. The observed changes in NIR reflectance of Amazon forests could be due to similar, but small, changes in NIR leaf albedo (reflectance plus transmittance) resulting from the exchange of older leaves for newer ones, but with the total leaf area unchanged. However, this argument ignores accumulating evidence from ground-based reports of higher leaf area in the dry season than the wet season, seasonal changes in litterfall and does not satisfactorily explain why NIR reflectance of these forests decreases in the wet season. More plausibly, the increase in NIR reflectance during the dry season and the decrease during the wet season would result from changes in both leaf area and leaf optical properties. Such change would be consistent with known phenological behavior of tropical forests, ground-based reports of seasonal changes in leaf area, litterfall, leaf optical properties and fluxes of evapotranspiration, and thus, would reconcile the various seemingly divergent views.
C1 [Samanta, Arindam] Atmospher & Environm Res Inc, Lexington, MA 02421 USA.
[Samanta, Arindam; Knyazikhin, Yuri; Xu, Liang; Myneni, Ranga B.] Boston Univ, Dept Geog & Environm, Boston, MA 02215 USA.
[Dickinson, Robert E.; Fu, Rong] Univ Texas Austin, Dept Geol Sci, Austin, TX 78712 USA.
[Costa, Marcos H.] Univ Fed Vicosa, BR-36570000 Vicosa, MG, Brazil.
[Saatchi, Sassan S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Nemani, Ramakrishna R.] NASA, Biospher Sci Branch, AMES Res Ctr, Moffett Field, CA 94035 USA.
RP Samanta, A (reprint author), Atmospher & Environm Res Inc, Lexington, MA 02421 USA.
EM arindam.sam@gmail.com
RI Xu, Liang/D-1247-2013; Myneni, Ranga/F-5129-2012
FU NASA Earth Science Enterprise
FX This work was supported by the NASA Earth Science Enterprise.
NR 57
TC 27
Z9 27
U1 0
U2 27
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-8953
EI 2169-8961
J9 J GEOPHYS RES-BIOGEO
JI J. Geophys. Res.-Biogeosci.
PD FEB 11
PY 2012
VL 117
AR G01015
DI 10.1029/2011JG001818
PG 13
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA 891UT
UT WOS:000300242800003
ER
PT J
AU Silver, BJ
Raymond, R
Sigman, DM
Prokopeko, M
Lollar, BS
Lacrampe-Couloume, G
Fogel, ML
Pratt, LM
Lefticariu, L
Onstott, TC
AF Silver, Bianca J.
Raymond, R.
Sigman, Daniel M.
Prokopeko, Masha
Lollar, Barbara Sherwood
Lacrampe-Couloume, Georges
Fogel, Marilyn L.
Pratt, Lisa M.
Lefticariu, Liliana
Onstott, T. C.
TI The origin of NO3- and N-2 in deep subsurface fracture water of South
Africa
SO CHEMICAL GEOLOGY
LA English
DT Article
DE N isotopes; Deep; Subsurface microbial ecosystems; Radiolysis; N cycle
ID WITWATERSRAND BASIN; ISOTOPIC COMPOSITION; AQUEOUS-SOLUTIONS;
STABLE-ISOTOPE; HIGH-PRESSURE; NOBLE-GASES; FRESH-WATER; NITROGEN;
NITRATE; GROUNDWATER
AB Deep (>0.8 km depth) fracture water with residence time estimates on the order of several Ma from the Witwatersrand Basin, South Africa contains up to 40 mu M of NO3-, up to 50 mM N-2 (90 times air saturation at surface) and 1 to -400 mu M NH3/NH4+ To determine whether the oxidized N species were introduced by mining activity, by recharge of paleometeoric water, or by subsurface geochemical processes, we undertook N and 0 isotopic analyses of N species from fracture water, mining water, pore water, fluid inclusion leachate and whole rock cores.
The NO2-, NO3- and NH3/NH4+ concentrations of the pore water and fluid inclusion leachate recovered from the low porosity quartzite, shale and metavolcanic units were similar to 10(4) times that of the fracture water. The delta N-15-NO3- and delta O-18-NO3- of the pore water and fluid inclusion leachate, however, overlapped that of the fracture water with the delta N-15-NO3- ranging from 2 to 7 parts per thousand and the delta N-18-NO3- ranging from 20 to 50 parts per thousand. The delta N-15-NO3- of the mining water ranged from 0 to 16 parts per thousand and its delta N-18-NO3- from 0 to 14 parts per thousand making the mining water NO3- isotopically distinct from that of the fracture, pore and fluid inclusion water. The delta N-15-N-2 of the fracture water and the delta N-15-N from the cores ranged from -5 to 10 parts per thousand and overlapped the delta N-15-NO3-. The delta N-15-NO4+ of the fracture water and pore water NH3/NH4+ ranged from -15 to 4 parts per thousand. Although the NO3- concentrations in the pore water and fluid inclusions were high, mass balance calculations indicate that NO3- accounts for <= 10% of the total rock N, whereas NH3/NH4+ trapped in fluid inclusions or NH4+ present in phyllosilicates account for >= 90% of the total N.
Based on these findings, the fluid inclusion NO3- appears to be the source of the pore water and fracture water NO3- rather than paleometeoric recharge or mining contamination. Irradiation experiments indicate that radiolytic oxidation of NH3 to NO3- can explain the fluid inclusion NO3- concentrations and, perhaps, its isotopic composition, but only if the NO3- did not attain isotopic equilibrium with the hydrothermal fluid 2 billion years ago. The delta N-15-N, delta N-15-N-2 and delta N-15-NO4+ suggest that the reduction of N-2 to NH4+ also must have occurred in the Witwatersrand Basin in order to explain the abundance of NH4+ throughout the strata. Although the depleted NH3- concentrations in the fracture water relative to the pore water are consistent with microbial NH3- reduction, further analyses will be required to determine the relative importance of biological processes in the subsurface N cycle and whether a complete subsurface N cycle exists. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Silver, Bianca J.; Raymond, R.; Sigman, Daniel M.; Onstott, T. C.] Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA.
[Silver, Bianca J.] ARCADISUS Inc, Cranbury, NJ 08512 USA.
[Prokopeko, Masha] Univ So Calif, Dept Earth Sci, Los Angeles, CA 90089 USA.
[Lollar, Barbara Sherwood; Lacrampe-Couloume, Georges] Univ Toronto, Dept Geol, Toronto, ON M5S 3B1, Canada.
[Fogel, Marilyn L.] Carnegie Inst Washington, Geophys Lab, Washington, DC 20005 USA.
[Lefticariu, Liliana] Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA.
[Lefticariu, Liliana] So Illinois Univ, Dept Geol, Carbondale, IL 62901 USA.
[Silver, Bianca J.; Raymond, R.; Lollar, Barbara Sherwood; Lacrampe-Couloume, Georges; Fogel, Marilyn L.; Pratt, Lisa M.; Lefticariu, Liliana; Onstott, T. C.] Indiana Univ, IPTAI, NASA Astrobiol Inst, Bloomington, IN USA.
RP Onstott, TC (reprint author), Princeton Univ, Dept Geosci, Guyot Hall, Princeton, NJ 08544 USA.
EM Bianca.silver@arcadis-us.com; prokopen@usc.edu;
bslollar@chem.utoronto.ca; m.fogel@gl.ciw.edu; prattl@indiana.edu;
tullis@princeton.edu
RI Sigman, Daniel/A-2649-2008; Fogel, Marilyn/M-2395-2015
OI Sigman, Daniel/0000-0002-7923-1973; Fogel, Marilyn/0000-0002-1176-3818
FU NASA Astrobiology Institute [NNA04CC03A]; National Science Foundation
[EAR-9978267]; NSERC; Canada Research Chair Funds
FX This work was supported by the NASA Astrobiology Institute through award
NNA04CC03A to the IPTAI Team co-directed by LMP and TCO, by National
Science Foundation LExEn Program grant EAR-9978267 to TCO and by the
NSERC Discovery and Accelerator Programs and Canada Research Chair Funds
to BSL. We are indebted to Colin Ralston and Walter Seymore of Evander
Au Mine (Harmony Gold Mining Co. Ltd.) and Arnand vanHeerden of Kloof Au
Mine (Gold Fields Ltd.) for logistical support in acquiring the cores
for this study. We also are grateful to the comments from two reviewers
which greatly improved the manuscript.
NR 77
TC 12
Z9 12
U1 1
U2 37
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0009-2541
J9 CHEM GEOL
JI Chem. Geol.
PD FEB 10
PY 2012
VL 294
BP 51
EP 62
DI 10.1016/j.chemgeo.2011.11.017
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 944ON
UT WOS:000304213800005
ER
PT J
AU Horesh, A
Kulkarni, SR
Fox, DB
Carpenter, J
Kasliwal, MM
Ofek, EO
Quimby, R
Gal-Yam, A
Cenko, B
de Bruyn, AG
Kamble, A
Wijers, RAMJ
van der Horst, AJ
Kouveliotou, C
Podsiadlowski, P
Sullivan, M
Maguire, K
Howell, DA
Nugent, PE
Gehrels, N
Law, NM
Poznanski, D
Shara, M
AF Horesh, Assaf
Kulkarni, S. R.
Fox, Derek B.
Carpenter, John
Kasliwal, Mansi M.
Ofek, Eran O.
Quimby, Robert
Gal-Yam, Avishay
Cenko, Bradley
de Bruyn, A. G.
Kamble, Atish
Wijers, Ralph A. M. J.
van der Horst, Alexander J.
Kouveliotou, Chryssa
Podsiadlowski, Philipp
Sullivan, Mark
Maguire, Kate
Howell, D. Andrew
Nugent, Peter E.
Gehrels, Neil
Law, Nicholas M.
Poznanski, Dovi
Shara, Michael
TI EARLY RADIO AND X-RAY OBSERVATIONS OF THE YOUNGEST NEARBY TYPE Ia
SUPERNOVA PTF 11kly (SN 2011fe)
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE radio continuum: general; supernovae: general; X-rays: general
ID SYMBIOTIC-STAR PROGENITOR; WHITE-DWARF MODELS; RS-OPHIUCHI; EMISSION;
NOVAE; EXPLOSION; EVOLUTION; BINARIES; CHANNEL; SWIFT
AB On 2011 August 24 (UT) the Palomar Transient Factory (PTF) discovered PTF11kly (SN 2011fe), the youngest and most nearby Type Ia supernova (SN Ia) in decades. We followed this event up in the radio (centimeter and millimeter bands) and X-ray bands, starting about a day after the estimated explosion time. We present our analysis of the radio and X-ray observations, yielding the tightest constraints yet placed on the pre-explosion mass-loss rate from the progenitor system of this supernova. We find a robust limit of (M)over dot less than or similar to 10(-8)(w/100 km s (1)) M-circle dot yr(-1) from sensitive X-ray non-detections, as well as a similar limit from radio data, which depends, however, on assumptions about microphysical parameters. We discuss our results in the context of single-degenerate models for SNe Ia and find that our observations modestly disfavor symbiotic progenitor models involving a red giant donor, but cannot constrain systems accreting from main-sequence or sub-giant stars, including the popular supersoft channel. In view of the proximity of PTF11kly and the sensitivity of our prompt observations, we would have to wait for a long time (a decade or longer) in order to more meaningfully probe the circumstellar matter of SNe Ia.
C1 [Horesh, Assaf; Kulkarni, S. R.; Carpenter, John; Kasliwal, Mansi M.; Ofek, Eran O.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Fox, Derek B.] Penn State Univ, Eberly Coll Sci, University Pk, PA 16802 USA.
[Kasliwal, Mansi M.] Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Ofek, Eran O.; Gal-Yam, Avishay] Weizmann Inst Sci, Fac Phys, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel.
[Quimby, Robert] Univ Tokyo, IPMU, Kashiwa, Chiba, Japan.
[Cenko, Bradley] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[de Bruyn, A. G.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands.
[de Bruyn, A. G.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AA Groningen, Netherlands.
[Kamble, Atish; Wijers, Ralph A. M. J.] Univ Wisconsin, Ctr Gravitat & Cosmol, Milwaukee, WI 53211 USA.
[van der Horst, Alexander J.] Univ Space Res Assoc, NSSTC, Huntsville, AL 35805 USA.
[Kouveliotou, Chryssa] NASA, Space Sci Off, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA.
[Podsiadlowski, Philipp; Sullivan, Mark; Maguire, Kate] Univ Oxford, Dept Phys Astrophys, Oxford OX1 3RH, England.
[Howell, D. Andrew] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA.
[Howell, D. Andrew] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Nugent, Peter E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA.
[Gehrels, Neil] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Law, Nicholas M.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Poznanski, Dovi] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Shara, Michael] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA.
RP Horesh, A (reprint author), CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
RI Horesh, Assaf/O-9873-2016;
OI Horesh, Assaf/0000-0002-5936-1156; Wijers, Ralph/0000-0002-3101-1808;
Sullivan, Mark/0000-0001-9053-4820
FU NSF [AST-0908886, AST-1008353]; NASA [NNH07ZDA001-GLAST]; Israeli
Science Foundation; BSF; Hubble Fellowship; Carnegie-Princeton
Fellowship; Netherlands Organization for Scientific Research (NWO); Gary
& Cynthia Bengier; Richard & Rhoda Goldman Fund; NASA/Swift [NNX10AI21G,
GO-7100028]; TABASGO Foundation
FX We thank the CARMA and EVLA staff for promptly scheduling this target of
opportunity. This work made use of data supplied by the UK Swift Science
Data Centre at the University of Leicester. We thank the ASTRON Radio
Observatory for the generous and swift allocation of observing time. PTF
is a fully automated, wide-field survey aimed at a systematic
exploration of explosions and variable phenomena in optical wavelengths.
The participating institutions are Caltech, Columbia University,
Weizmann Institute of Science, Lawrence Berkeley Laboratory, University
of Oxford, and University of California at Berkeley. The program is
centered on a 12K x 8K, 7.8 square degree CCD array (CFH12K)
re-engineered for the 1.2 m Oschin Telescope at the Palomar Observatory
by Caltech Optical Observatories. Photometric follow-up is undertaken by
the automated Palomar 1.5 m telescope. Research at Caltech is supported
by grants from NSF and NASA. The Weizmann PTF partnership is supported
in part by the Israeli Science Foundation via grants to A. G.
Weizmann-Caltech Collaboration is supported by a grant from the BSF to
A. G. and S. R. K. A. G. further acknowledges the Lord Sieff of Brimpton
Foundation. M. M. K. acknowledges support from a Hubble Fellowship and
Carnegie-Princeton Fellowship. We thank the ASTRON Radio Observatory for
the generous and swift allocation of observing time. The Westerbork
Synthesis Radio Telescope is operated by ASTRON (Netherlands Foundation
for Radio Astronomy) with support from the Netherlands Organization for
Scientific Research (NWO). A.J.v.d.H. was supported by NASA grant
NNH07ZDA001-GLAST. S. B. C. acknowledges generous financial assistance
from Gary & Cynthia Bengier, the Richard & Rhoda Goldman Fund,
NASA/Swift grants NNX10AI21G and GO-7100028, the TABASGO Foundation, and
NSF grant AST-0908886. A. K. is partially supported by NSF award
AST-1008353.
NR 54
TC 72
Z9 72
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 FEB 10
PY 2012
VL 746
IS 1
AR 21
DI 10.1088/0004-637X/746/1/21
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 926VZ
UT WOS:000302861300021
ER
PT J
AU Kumar, P
Cho, KS
Bong, SC
Park, SH
Kim, YH
AF Kumar, Pankaj
Cho, K. -S.
Bong, S. -C.
Park, Sung-Hong
Kim, Y. H.
TI INITIATION OF CORONAL MASS EJECTION AND ASSOCIATED FLARE CAUSED BY
HELICAL KINK INSTABILITY OBSERVED BY SDO/AIA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: atmosphere; Sun: coronal mass ejections (CMEs); Sun: filaments,
prominences; Sun: flares; Sun: magnetic topology; Sun: particle emission
ID UNSTABLE FLUX ROPES; MAGNETIC-FIELDS; BALLOONING INSTABILITY; NUMERICAL
SIMULATIONS; TORUS INSTABILITY; DRIVEN EVOLUTION; SOLAR CORONA; MODEL;
ERUPTION; LOOP
AB In this paper, we present multiwavelength observations of helical kink instability as a trigger of a coronal mass ejection (CME) which occurred in active region NOAA 11163 on 2011 February 24. The CME was associated with an M3.5 limb flare. High-resolution observations from the Solar Dynamics Observatory/Atmospheric Imaging Assembly suggest the development of helical kink instability in the erupting prominence, which implies a flux rope structure of the magnetic field. A brightening starts below the apex of the prominence with its slow rising motion (similar to 100 km s (1)) during the activation phase. A bright structure, indicative of a helix with similar to 3-4 turns, was transiently formed at this position. The corresponding twist of similar to 6 pi-8 pi is sufficient to generate the helical kink instability in a flux rope according to recently developed models. A slowly rising blob structure was subsequently formed at the apex of the prominence, and a flaring loop was observed near the footpoints. Within 2 minutes, a second blob was formed in the northern prominence leg. The second blob erupts (like a plasmoid ejection) with the detachment of the northern prominence leg, and flare intensity maximizes. The first blob at the prominence apex shows rotational motion in the counterclockwise direction in the plane of sky, interpreted as the unwinding motion of a helix, and it also erupts to give the CME. RHESSI hard X-ray (HXR) sources show the two footpoint sources and a loop-top source during the flare. We found RHESSI HXR flux, soft X-ray flux derivative, and CME acceleration in the low corona correlate well, which is in agreement with the standard flare model (CSHKP). We also discuss the possible role of ballooning as well as torus instabilities in driving the CME. We conclude that the CME and flare were triggered by the helical kink instability in a flux rope and accelerated mainly by the torus instability.
C1 [Kumar, Pankaj; Cho, K. -S.; Bong, S. -C.; Park, Sung-Hong; Kim, Y. H.] Korea Astron & Space Sci Inst KASI, Taejon 305348, South Korea.
[Cho, K. -S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cho, K. -S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Kumar, P (reprint author), Korea Astron & Space Sci Inst KASI, Taejon 305348, South Korea.
EM pankaj@kasi.re.kr
RI Park, Sung-Hong/K-1578-2014
OI Park, Sung-Hong/0000-0001-9149-6547
NR 68
TC 36
Z9 36
U1 2
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 FEB 10
PY 2012
VL 746
IS 1
AR 67
DI 10.1088/0004-637X/746/1/67
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 926VZ
UT WOS:000302861300067
ER
PT J
AU Metzger, BD
Berger, E
AF Metzger, B. D.
Berger, E.
TI WHAT IS THE MOST PROMISING ELECTROMAGNETIC COUNTERPART OF A NEUTRON STAR
BINARY MERGER?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: general; gravitational waves; stars: neutron; surveys
ID GAMMA-RAY BURSTS; COMPACT OBJECT MERGERS; GRAVITATIONAL-WAVE
OBSERVATIONS; EXTENDED EMISSION; HOST GALAXY; R-PROCESS; OPTICAL
AFTERGLOW; STANDARD SIRENS; LIGHT CURVES; SCIENCE RUN
AB The final inspiral of double neutron star and neutron-star-black-hole binaries are likely to be detected by advanced networks of ground-based gravitational wave (GW) interferometers. Maximizing the science returns from such a discovery will require the identification of an electromagnetic counterpart. Here we critically evaluate and compare several possible counterparts, including short-duration gamma-ray bursts (SGRBs), "orphan" optical and radio afterglows, and day-long optical transients powered by the radioactive decay of heavy nuclei synthesized in the merger ejecta ("kilonovae"). We assess the promise of each counterpart in terms of four "Cardinal Virtues": detectability, high fraction, identifiability, and positional accuracy. Taking into account the search strategy for typical error regions of tens of square degrees, we conclude that SGRBs are the most useful to confirm the cosmic origin of a few GW events, and to test the association with neutron star mergers. However, for the more ambitious goal of localizing and obtaining redshifts for a large sample of GW events, kilonovae are instead preferred. Off-axis optical afterglows are detectable for at most tens of percent of events, while radio afterglows are promising only for energetic relativistic ejecta in a high-density medium. Our main recommendations are: (1) an all-sky gamma-ray satellite is essential for temporal coincidence detections, and for GW searches of gamma-ray-triggered events; (2) the Large Synoptic Survey Telescope should adopt a one-day cadence follow-up strategy, ideally with 0.5 hr per pointing to cover GW error regions; and (3) radio searches should focus on the relativistic case, which requires observations for a few months.
C1 [Metzger, B. D.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Berger, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Metzger, BD (reprint author), NASA, Washington, DC 20546 USA.
FU NASA [PF9-00065, NAS8-03060]; Chandra Xray Center; National Science
Foundation [AST-1107973]
FX We thank Hendrik van Eerten and Andrew MacFadyen for producing and
maintaining their online library of afterglow light curves. We thank
Ehud Nakar for providing theoretical light curves of supernova shock
breakout. We thank S. Nissanke and R. O'Shaughnessy for helpful
discussions and information. B. D. M. is supported by NASA through
Einstein Postdoctoral Fellowship grant No. PF9-00065 awarded by the
Chandra Xray Center, which is operated by the Smithsonian Astrophysical
Observatory for NASA under contract NAS8-03060. E. B. acknowledges
support for this work from the National Science Foundation through grant
AST-1107973.
NR 118
TC 211
Z9 212
U1 2
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 FEB 10
PY 2012
VL 746
IS 1
DI 10.1088/0004-637X/746/1/48
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 926VZ
UT WOS:000302861300048
ER
PT J
AU Millea, M
Dore, O
Dudley, J
Holder, G
Knox, L
Shaw, L
Song, YS
Zahn, O
AF Millea, M.
Dore, O.
Dudley, J.
Holder, G.
Knox, L.
Shaw, L.
Song, Y-S.
Zahn, O.
TI MODELING EXTRAGALACTIC FOREGROUNDS AND SECONDARIES FOR UNBIASED
ESTIMATION OF COSMOLOGICAL PARAMETERS FROM PRIMARY COSMIC MICROWAVE
BACKGROUND ANISOTROPY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmological parameters; cosmology: observations; cosmology: theory;
distance scale; large-scale structure of universe
ID ZELDOVICH POWER SPECTRUM; SOUTH-POLE TELESCOPE; STAR-FORMING GALAXIES;
HIGH-FREQUENCY; PATCHY REIONIZATION; POLARIZATION; CMB; SIMULATIONS;
CLUSTERS; IMPACT
AB Using the latest physical modeling and constrained by the most recent data, we develop a phenomenological parameterized model of the contributions to intensity and polarization maps at millimeter wavelengths from external galaxies and Sunyaev-Zeldovich effects. We find such modeling to be necessary for estimation of cosmological parameters from Planck data. For example, ignoring the clustering of the infrared background would result in a bias in ns of 7s in the context of an eight-parameter cosmological model. We show that the simultaneous marginalization over a full foreground model can eliminate such biases, while increasing the statistical uncertainty in cosmological parameters by less than 20%. The small increases in uncertainty can be significantly reduced with the inclusion of higher-resolution ground-based data. The multi-frequency analysis we employ involves modeling 46 total power spectra and marginalization over 17 foreground parameters. We show that we can also reduce the data to a best estimate of the cosmic microwave background power spectra, with just two principal components (with constrained amplitudes) describing residual foreground contamination.
C1 [Millea, M.; Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Dore, O.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Dore, O.] CALTECH, Pasadena, CA 91125 USA.
[Dudley, J.; Holder, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Song, Y-S.] Korea Inst Adv Study, Seoul 130722, South Korea.
[Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Zahn, O.] Lawrence Berkeley Natl Labs, Berkeley, CA 94720 USA.
RP Millea, M (reprint author), Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
FU National Aeronautics and Space Administration; Yale University; NSF
[AST-1009811, 0709498]
FX We benefited from conversations with A. Challinor, J. Dunkley, G.
Efstathiout, F. Finelli, S. Gratton, W. Holzapfel, C. Reichardt, D.
Scott, G. Ziemann, and G. de Zotti. Part of the research described in
this paper was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration. L. S. acknowledges the support of Yale
University and NSF grant AST-1009811. L. K. and M. M. acknowledge
support from NSF grant 0709498.
NR 77
TC 16
Z9 16
U1 0
U2 4
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 FEB 10
PY 2012
VL 746
IS 1
AR 4
DI 10.1088/0004-637X/746/1/4
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 926VZ
UT WOS:000302861300004
ER
PT J
AU Suzuki, N
Rubin, D
Lidman, C
Aldering, G
Amanullah, R
Barbary, K
Barrientos, LF
Botyanszki, J
Brodwin, M
Connolly, N
Dawson, KS
Dey, A
Doi, M
Donahue, M
Deustua, S
Eisenhardt, P
Ellingson, E
Faccioli, L
Fadeyev, V
Fakhouri, HK
Fruchter, AS
Gilbank, DG
Gladders, MD
Goldhaber, G
Gonzalez, AH
Goobar, A
Gude, A
Hattori, T
Hoekstra, H
Hsiao, E
Huang, X
Ihara, Y
Jee, MJ
Johnston, D
Kashikawa, N
Koester, B
Konishi, K
Kowalski, M
Linder, EV
Lubin, L
Melbourne, J
Meyers, J
Morokuma, T
Munshi, F
Mullis, C
Oda, T
Panagia, N
Perlmutter, S
Postman, M
Pritchard, T
Rhodes, J
Ripoche, P
Rosati, P
Schlegel, DJ
Spadafora, A
Stanford, SA
Stanishev, V
Stern, D
Strovink, M
Takanashi, N
Tokita, K
Wagner, M
Wang, L
Yasuda, N
Yee, HKC
AF Suzuki, N.
Rubin, D.
Lidman, C.
Aldering, G.
Amanullah, R.
Barbary, K.
Barrientos, L. F.
Botyanszki, J.
Brodwin, M.
Connolly, N.
Dawson, K. S.
Dey, A.
Doi, M.
Donahue, M.
Deustua, S.
Eisenhardt, P.
Ellingson, E.
Faccioli, L.
Fadeyev, V.
Fakhouri, H. K.
Fruchter, A. S.
Gilbank, D. G.
Gladders, M. D.
Goldhaber, G.
Gonzalez, A. H.
Goobar, A.
Gude, A.
Hattori, T.
Hoekstra, H.
Hsiao, E.
Huang, X.
Ihara, Y.
Jee, M. J.
Johnston, D.
Kashikawa, N.
Koester, B.
Konishi, K.
Kowalski, M.
Linder, E. V.
Lubin, L.
Melbourne, J.
Meyers, J.
Morokuma, T.
Munshi, F.
Mullis, C.
Oda, T.
Panagia, N.
Perlmutter, S.
Postman, M.
Pritchard, T.
Rhodes, J.
Ripoche, P.
Rosati, P.
Schlegel, D. J.
Spadafora, A.
Stanford, S. A.
Stanishev, V.
Stern, D.
Strovink, M.
Takanashi, N.
Tokita, K.
Wagner, M.
Wang, L.
Yasuda, N.
Yee, H. K. C.
CA Supernova Cosmology Project
TI THE HUBBLE SPACE TELESCOPE CLUSTER SUPERNOVA SURVEY. V. IMPROVING THE
DARK- ENERGY CONSTRAINTS ABOVE z > 1 AND BUILDING AN EARLY-TYPE-HOSTED
SUPERNOVA SAMPLE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmological parameters; distance scale; supernovae: general
ID DIGITAL SKY SURVEY; COLOR-MAGNITUDE RELATION; HIGH-REDSHIFT SUPERNOVAE;
PROBE WMAP OBSERVATIONS; LASER ADAPTIVE OPTICS; IA LIGHT CURVES;
ADVANCED CAMERA; GALAXY CLUSTERS; LEGACY SURVEY; COSMOLOGICAL
CONSTRAINTS
AB We present Advanced Camera for Surveys, NICMOS, and Keck adaptive-optics-assisted photometry of 20 Type Ia supernovae (SNe Ia) from the Hubble Space Telescope (HST) Cluster Supernova Survey. The SNe Ia were discovered over the redshift interval 0.623 < z < 1.415. Of these SNe Ia, 14 pass our strict selection cuts and are used in combination with the world's sample of SNe Ia to derive the best current constraints on dark energy. Of our new SNe Ia, 10 are beyond redshift z = 1, thereby nearly doubling the statistical weight of HST-discovered SNe Ia beyond this redshift. Our detailed analysis corrects for the recently identified correlation between SN Ia luminosity and host galaxy mass and corrects the NICMOS zero point at the count rates appropriate for very distant SNe Ia. Adding these SNe improves the best combined constraint on dark-energy density,rho(DE)(z), at redshifts 1.0 < z < 1.6 by 18% (including systematic errors). For a flat. CDM universe, we find Omega(A) = 0.729 +/- 0.014 (68% confidence level (CL) including systematic errors). For a flat wCDM model, we measure a constant dark-energy equation-of-state parameter w = -1.013(-0.073)(+0.068) (68% CL). Curvature is constrained to similar to 0.7% in the owCDM model and to similar to 2% in a model in which dark energy is allowed to vary with parameters w(0) and w(a). Further tightening the constraints on the time evolution of dark energy will require several improvements, including high-quality multi-passband photometry of a sample of several dozenz > 1 SNe Ia. We describe how such a sample could be efficiently obtained by targeting cluster fields with WFC3 on board HST. The updated supernova Union2.1 compilation of 580 SNe is available at http://supernova.lbl.gov/Union.
C1 [Suzuki, N.; Rubin, D.; Aldering, G.; Barbary, K.; Faccioli, L.; Fakhouri, H. K.; Goldhaber, G.; Hsiao, E.; Huang, X.; Linder, E. V.; Meyers, J.; Perlmutter, S.; Ripoche, P.; Schlegel, D. J.; Spadafora, A.; Strovink, M.] EO Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Suzuki, N.; Rubin, D.; Amanullah, R.; Barbary, K.; Botyanszki, J.; Faccioli, L.; Fakhouri, H. K.; Goldhaber, G.; Gude, A.; Hsiao, E.; Huang, X.; Linder, E. V.; Meyers, J.; Munshi, F.; Perlmutter, S.; Pritchard, T.; Ripoche, P.; Strovink, M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Lidman, C.] Australian Astron Observ, Epping, NSW 1710, Australia.
[Amanullah, R.; Goobar, A.] AlbaNova, Oskar Klein Ctr Cosmo Particle Phys, SE-10691 Stockholm, Sweden.
[Barrientos, L. F.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago, Chile.
[Brodwin, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Connolly, N.] Hamilton Coll, Dept Phys, Clinton, NY 13323 USA.
[Dawson, K. S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Dey, A.] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Doi, M.; Ihara, Y.; Morokuma, T.; Tokita, K.] Univ Tokyo, Grad Sch Sci, Inst Astron, Mitaka, Tokyo 1810015, Japan.
[Donahue, M.; Johnston, D.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Deustua, S.; Fruchter, A. S.; Panagia, N.; Postman, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Eisenhardt, P.; Rhodes, J.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ellingson, E.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Fadeyev, V.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 94064 USA.
[Gilbank, D. G.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
[Gladders, M. D.; Koester, B.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Goobar, A.; Stanishev, V.] Stockholm Univ, Albanova Univ Ctr, Dept Phys, SE-10691 Stockholm, Sweden.
[Gude, A.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Hattori, T.] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Hoekstra, H.] Leiden Univ, Leiden Observ, Leiden, Netherlands.
[Jee, M. J.; Lubin, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Johnston, D.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA.
[Kashikawa, N.; Morokuma, T.; Takanashi, N.] Natl Astron Observ Japan, Tokyo 1818588, Japan.
[Koester, B.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Konishi, K.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan.
[Kowalski, M.] Univ Bonn, Inst Phys, Bonn, Germany.
[Melbourne, J.; Rhodes, J.] CALTECH, Div Phys Math & Astron, Caltech Opt Observ, Pasadena, CA 91125 USA.
[Munshi, F.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Mullis, C.] Wachovia Corp, Winston Salem, NC 27101 USA.
[Oda, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Pritchard, T.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Rosati, P.] ESO, D-85748 Garching, Germany.
[Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA.
[Stanishev, V.] Inst Super Tecn, CENTRA Ctr Multidisciplinar Astrofis, P-1049001 Lisbon, Portugal.
[Wagner, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Wang, L.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA.
[Yasuda, N.] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan.
[Yee, H. K. C.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
RP Suzuki, N (reprint author), EO Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
EM nsuzuki@lbl.gov; rubind@berkeley.edu; clidman@aao.gov.au
RI Kowalski, Marek/G-5546-2012; Yasuda, Naoki/A-4355-2011; Stanishev,
Vallery/M-8930-2013; Perlmutter, Saul/I-3505-2015;
OI Stanishev, Vallery/0000-0002-7626-1181; Perlmutter,
Saul/0000-0002-4436-4661; Strovink, Mark/0000-0001-7020-7769; Meyers,
Joshua/0000-0002-2308-4230; Hoekstra, Henk/0000-0002-0641-3231
FU NASA from the Space Telescope Science Institute [GO-10496]; AURA, Inc.,
under NASA [NAS 5-26555]; Director, Office of Science, Office of High
Energy and Nuclear Physics, of the U.S. Department of Energy
[AC02-05CH11231]; JSPS [20040003]; U.S. Department of Energy by Lawrence
Livermore National Laboratory [W-7405-Eng-48, DE-AC52-07NA27344]; Japan
Society for the Promotion of Science; Netherlands Organization for
Scientific Research (WO); Marie Curie International Reintegration Grant
FX Financial support for this work was provided by NASA through program
GO-10496 from the Space Telescope Science Institute, which is operated
by AURA, Inc., under NASA contract NAS 5-26555. This work was also
supported in part by the Director, Office of Science, Office of High
Energy and Nuclear Physics, of the U.S. Department of Energy under
contract No. AC02-05CH11231, as well as a JSPS core-to-core program
"International Research Network for Dark Energy" and by JSPS research
grant 20040003. Support for M.B. was provided by the W. M. Keck
Foundation. The work of S.A.S. was performed under the auspices of the
U.S. Department of Energy by Lawrence Livermore National Laboratory in
part under Contract W-7405-Eng-48 and in part under contract
DE-AC52-07NA27344. The work of P.E., J.R., and D.S. was carried out at
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with NASA. T.M. and Y.I. have been financially supported by
the Japan Society for the Promotion of Science through its Research
Fellowship. H.H. acknowledges support from a VIDI grant from the
Netherlands Organization for Scientific Research (WO) and a Marie Curie
International Reintegration Grant. N.S., C.L., and S.P. wish to thank
the support and hospitality of the Aspen Center for Physics, where much
of this paper was written. We thank Jay Anderson, L. E. Bergeron, Ralph
Bohlin, Roelof de Jong, Anton Koekemoer, Jennifer Mack, Bahram Mobasher,
Adam Riess, Kenneth Sembach, and ACS and NICMOS teams at the Space
Telescope Science Institute for their advice on the HST data
calibration. We also thank Alex Conley for calibration discussions.
Finally, we thank our referee, who carefully read our paper and gave
valuable feedback.
NR 117
TC 673
Z9 678
U1 1
U2 38
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 FEB 10
PY 2012
VL 746
IS 1
AR 85
DI 10.1088/0004-637X/746/1/85
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 926VZ
UT WOS:000302861300085
ER
PT J
AU Teodoro, M
Damineli, A
Arias, JI
de Araujo, FX
Barba, RH
Corcoran, MF
Fernandes, MB
Fernandez-Lajus, E
Fraga, L
Gamen, RC
Gonzalez, JF
Groh, JH
Marshall, JL
McGregor, PJ
Morrell, N
Nicholls, DC
Parkin, ER
Pereira, CB
Phillips, MM
Solivella, GR
Steiner, JE
Stritzinger, M
Thompson, I
Torres, CAO
Torres, MAP
Herencia, MIZ
AF Teodoro, M.
Damineli, A.
Arias, J. I.
de Araujo, F. X.
Barba, R. H.
Corcoran, M. F.
Borges Fernandes, M.
Fernandez-Lajus, E.
Fraga, L.
Gamen, R. C.
Gonzalez, J. F.
Groh, J. H.
Marshall, J. L.
McGregor, P. J.
Morrell, N.
Nicholls, D. C.
Parkin, E. R.
Pereira, C. B.
Phillips, M. M.
Solivella, G. R.
Steiner, J. E.
Stritzinger, M.
Thompson, I.
Torres, C. A. O.
Torres, M. A. P.
Zevallos Herencia, M. I.
TI He II lambda 4686 IN eta CARINAE: COLLAPSE OF THE WIND-WIND COLLISION
REGION DURING PERIASTRON PASSAGE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE line: profiles; stars: early-type; stars: individual (eta Carinae);
stars: massive
ID BINARY V444 CYGNI; X-RAY MINIMUM; COLLIDING-WINDS; SPECTROSCOPIC EVENT;
EMISSION-LINES; HD 5980; RADIO-EMISSION; THETA-CARINAE; LIGHT-CURVE;
SYSTEM
AB The periodic spectroscopic events in eta Carinae are now well established and occur near the periastron passage of two massive stars in a very eccentric orbit. Several mechanisms have been proposed to explain the variations of different spectral features, such as an eclipse by the wind-wind collision (WWC) boundary, a shell ejection from the primary star or accretion of its wind onto the secondary. All of them have problems explaining all the observed phenomena. To better understand the nature of the cyclic events, we performed a dense monitoring of eta Carinae with five Southern telescopes during the 2009 low-excitation event, resulting in a set of data of unprecedented quality and sampling. The intrinsic luminosity of the He II lambda 4686 emission line (L similar to 310 L-circle dot) just before periastron reveals the presence of a very luminous transient source of extreme UV radiation emitted in the WWC region. Clumps in the primary's wind probably explain the flare-like behavior of both the X-ray and He II lambda 4686 light curves. After a short-lived minimum, He II lambda 4686 emission rises again to a new maximum, when X-rays are still absent or very weak. We interpret this as a collapse of the WWC onto the "surface" of the secondary star, switching off the hard X-ray source and diminishing the WWC shock cone. The recovery from this state is controlled by the momentum balance between the secondary's wind and the clumps in the primary's wind.
C1 [Teodoro, M.; Damineli, A.; Steiner, J. E.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508900 Sao Paulo, Brazil.
[Arias, J. I.] Univ La Serena, Dept Fis, La Serena, Chile.
[de Araujo, F. X.; Borges Fernandes, M.; Pereira, C. B.; Zevallos Herencia, M. I.] Observ Nacl, BR-20921400 Rio De Janeiro, Brazil.
[Barba, R. H.; Gonzalez, J. F.] Consejo Nacl Invest Cient & Tecn, ICATE, San Juan, Argentina.
[Corcoran, M. F.] CRESST, Greenbelt, MD 20771 USA.
[Corcoran, M. F.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Fernandez-Lajus, E.; Gamen, R. C.; Solivella, G. R.] Univ Nacl La Plata, Fac Ciencias Astron & Geofis, La Plata, BA, Argentina.
[Fraga, L.] So Observ Astrophys Res, La Serena, Chile.
[Groh, J. H.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Marshall, J. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA.
[McGregor, P. J.; Nicholls, D. C.; Parkin, E. R.] RSAA, Mt Stromlo Observ, Weston, ACT 2611, Australia.
[Morrell, N.; Phillips, M. M.] Observ Carnegie Inst Washington, Las Campanas Observ, La Serena, Chile.
[Stritzinger, M.] Stockholm Univ, Dept Astron, Oskar Klein Ctr, S-10691 Stockholm, Sweden.
[Thompson, I.] Observ Carnegie Inst, Pasadena, CA 91101 USA.
[Torres, C. A. O.] Lab Nacl Astrofis, BR-37504364 Bairro Das Nacoes, Itajuba, Brazil.
[Torres, M. A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Teodoro, M (reprint author), Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Rua Matao 1226,Cidade Univ, BR-05508900 Sao Paulo, Brazil.
EM mairan@astro.iag.usp.br
RI Borges Fernandes, Marcelo/K-6210-2016; Pereira, Claudio/L-3199-2016;
Damineli, Augusto/D-8210-2012; 7, INCT/H-6207-2013; Teodoro,
Mairan/H-9123-2013; Astrofisica, Inct/H-9455-2013; Damineli,
Augusto/P-8829-2016; Barba, Rodolfo/P-4649-2014; Gamen,
Roberto/A-1728-2015
OI Damineli, Augusto/0000-0002-7978-2994; Damineli,
Augusto/0000-0002-7978-2994; Barba, Rodolfo/0000-0003-1086-1579;
FU FAPESP [05/00190-8, 09/08013-9]; CNPq; Conselho Nacional de
Desenvolvimento Cientifico e Tecnologico (CNPq-Brazil); NASA; Chandra
[G07-8022A, G08-9018A, G09-0016A, GO0-11039A]; RXTE Guest Observer
facility at NASA/GSFC
FX We thank the referee for questions and suggestions that led to a
clarification of the ideas discussed in this paper. M. T., A. D., and
J.E.S. are grateful to the Brazilian agencies FAPESP and CNPq for
continuous financial support. M. T. is supported through grants FAPESP
05/00190-8 and 09/08013-9. M. B. F. acknowledges Conselho Nacional de
Desenvolvimento Cientifico e Tecnologico (CNPq-Brazil) for the
post-doctoral grant. M. F. C. gratefully acknowledges support from NASA
and Chandra via grants G07-8022A, G08-9018A, G09-0016A, and GO0-11039A,
along with continued aid from the RXTE Guest Observer facility at
NASA/GSFC. Calculations were performed with version 07.02 of Cloudy,
last described by Ferland et al. (1998). This research has made use of
NASA's Astrophysics Data System. In addition, 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.
NR 86
TC 18
Z9 18
U1 1
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 FEB 10
PY 2012
VL 746
IS 1
AR 73
DI 10.1088/0004-637X/746/1/73
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 926VZ
UT WOS:000302861300073
ER
PT J
AU Tessenyi, M
Ollivier, M
Tinetti, G
Beaulieu, JP
du Foresto, VC
Encrenaz, T
Micela, G
Swinyard, B
Ribas, I
Aylward, A
Tennyson, J
Swain, MR
Sozzetti, A
Vasisht, G
Deroo, P
AF Tessenyi, M.
Ollivier, M.
Tinetti, G.
Beaulieu, J. P.
du Foresto, V. Coude
Encrenaz, T.
Micela, G.
Swinyard, B.
Ribas, I.
Aylward, A.
Tennyson, J.
Swain, M. R.
Sozzetti, A.
Vasisht, G.
Deroo, P.
TI CHARACTERIZING THE ATMOSPHERES OF TRANSITING PLANETS WITH A DEDICATED
SPACE TELESCOPE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: planetary systems; planets and satellites: atmospheres; stars:
late-type; stars: low-mass
ID EXOPLANET HD 209458B; UPSILON ANDROMEDAE B; HOT NEPTUNE GJ436B; LOW-MASS
STARS; EXTRASOLAR PLANET; TRANSMISSION SPECTRUM; MU-M; ECCENTRIC
EXOPLANETS; EMISSION-SPECTRUM; DAYSIDE SPECTRUM
AB Exoplanetary science is one of the fastest evolving fields of today's astronomical research, continuously yielding unexpected and surprising results. Ground-based planet-hunting surveys, together with dedicated space missions such as Kepler and CoRoT, are delivering an ever-increasing number of exoplanets, over 690, and ESA's Gaia mission will escalate the exoplanetary census into the several thousands. The next logical step is the characterization of these new worlds. What is their nature? Why are they as they are? Use of the Hubble Space Telescope and Spitzer Space Telescope to probe the atmospheres of transiting hot, gaseous exoplanets has opened perspectives unimaginable even just 10 years ago, demonstrating that it is indeed possible with current technology to address the ambitious goal of characterizing the atmospheres of these alien worlds. However, these successful measurements have also shown the difficulty of understanding the physics and chemistry of these exotic environments when having to rely on a limited number of observations performed on a handful of objects. To progress substantially in this field, a dedicated facility for exoplanet characterization, able to observe a statistically significant number of planets over time and a broad spectral range will be essential. Additionally, the instrument design ( e. g., detector performances, photometric stability) will be tailored to optimize the extraction of the astrophysical signal. In this paper, we analyze the performance and tradeoffs of a 1.2/1.4 m space telescope for exoplanet transit spectroscopy from the visible to the mid-IR. We present the signal-to-noise ratio as a function of integration time and stellar magnitude/spectral type for the acquisition of spectra of planetary atmospheres for a variety of scenarios: hot, warm, and temperate planets orbiting stars ranging in spectral type from hot F-to cooler M-dwarfs. Our results include key examples of known planets (e. g., HD 189733b, GJ 436b, GJ 1214b, and Cancri 55 e) and simulations of plausible terrestrial and gaseous planets, with a variety of thermodynamical conditions. We conclude that even most challenging targets, such as super-Earths in the habitable zone of late-type stars, are within reach of an M-class, space-based spectroscopy mission.
C1 [Tessenyi, M.; Tinetti, G.; Swinyard, B.; Aylward, A.; Tennyson, J.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Tessenyi, M.; Beaulieu, J. P.] Univ Paris 06, Inst Astrophys Spatiale, CNRS, UMR7095, Paris, France.
[Ollivier, M.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Ollivier, M.] CNRS, UMR 8617, IAS, UMR8617, F-91405 Orsay, France.
[du Foresto, V. Coude; Encrenaz, T.] LESIA, Observ Paris, Meudon, France.
[Micela, G.] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy.
[Swinyard, B.] STFC Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England.
[Ribas, I.] CSIC IEEC, Inst Ciencies Espai, Bellaterra 08193, Spain.
[Swain, M. R.; Vasisht, G.; Deroo, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Sozzetti, A.] INAF Osservatorio Astron Torino, I-10025 Pino Torinese, TO, Italy.
RP Tessenyi, M (reprint author), UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England.
RI Tennyson, Jonathan/I-2222-2012; Ribas, Ignasi/M-2134-2014;
OI Tennyson, Jonathan/0000-0002-4994-5238; Ribas,
Ignasi/0000-0002-6689-0312; Micela, Giuseppina/0000-0002-9900-4751;
Sozzetti, Alessandro/0000-0002-7504-365X; Tinetti,
Giovanna/0000-0001-6058-6654
NR 71
TC 24
Z9 24
U1 1
U2 19
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 FEB 10
PY 2012
VL 746
IS 1
AR 45
DI 10.1088/0004-637X/746/1/45
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 926VZ
UT WOS:000302861300045
ER
PT J
AU Todorov, KO
Deming, D
Knutson, HA
Burrows, A
Sada, PV
Cowan, NB
Agol, E
Desert, JM
Fortney, JJ
Charbonneau, D
Laughlin, G
Langton, J
Showman, AP
Lewis, NK
AF Todorov, Kamen O.
Deming, Drake
Knutson, Heather A.
Burrows, Adam
Sada, Pedro V.
Cowan, Nicolas B.
Agol, Eric
Desert, Jean-Michel
Fortney, Jonathan J.
Charbonneau, David
Laughlin, Gregory
Langton, Jonathan
Showman, Adam P.
Lewis, Nikole K.
TI WARM SPITZER OBSERVATIONS OF THREE HOT EXOPLANETS: XO-4b, HAT-P-6b, AND
HAT-P-8b
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE eclipses; planetary systems; techniques: photometric
ID INFRARED-EMISSION SPECTRUM; SECONDARY ECLIPSE PHOTOMETRY; EXTRASOLAR
PLANET; THERMAL EMISSION; TEMPERATURE INVERSION; HD 189733B; TRANSITING
PLANET; GIANT PLANETS; LIGHT CURVES; F-STAR
AB We analyze Warm Spitzer/Infrared Array Camera observations of the secondary eclipses of three planets, XO-4b, HAT-P-6b, and HAT-P-8b. We measure secondary eclipse amplitudes at 3.6 mu m and 4.5 mu m for each target. XO-4b exhibits a stronger eclipse depth at 4.5 mu m than at 3.6 mu m, which is consistent with the presence of a temperature inversion. HAT-P-8b shows a stronger eclipse amplitude at 3.6 mu m and is best described by models without a temperature inversion. The eclipse depths of HAT-P-6b can be fitted with models with a small or no temperature inversion. We consider our results in the context of a postulated relationship between stellar activity and temperature inversion and a relationship between irradiation level and planet dayside temperature, as discussed by Knutson et al. and Cowan & Agol, respectively. Our results are consistent with these hypotheses, but do not significantly strengthen them. To measure accurate secondary eclipse central phases, we require accurate ephemerides. We obtain primary transit observations and supplement them with publicly available observations to update the orbital ephemerides of the three planets. Based on the secondary eclipse timing, we set upper boundaries for e cos(omega) for HAT-P-6b, HAT-P-8b, and XO-4b and find that the values are consistent with circular orbits.
C1 [Todorov, Kamen O.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Deming, Drake] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA.
[Knutson, Heather A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Knutson, Heather A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Sada, Pedro V.] Univ Monterrey, Dept Math & Phys, Monterrey, Mexico.
[Cowan, Nicolas B.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA.
[Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Desert, Jean-Michel; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fortney, Jonathan J.; Laughlin, Gregory] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Langton, Jonathan] Principia Coll, Dept Phys, Elsah, IL 62028 USA.
[Showman, Adam P.; Lewis, Nikole K.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Todorov, Kamen O.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
RP Todorov, KO (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
RI Agol, Eric/B-8775-2013;
OI Agol, Eric/0000-0002-0802-9145; Fortney, Jonathan/0000-0002-9843-4354;
Todorov, Kamen/0000-0002-9276-8118; Charbonneau,
David/0000-0002-9003-484X
FU NASA through JPL/Caltech; NASA; Pennsylvania State University; Eberly
College of Science; Pennsylvania Space Grant Consortium
FX This work is based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology under a contract with NASA. Support
for this work was provided by NASA through an award issued by
JPL/Caltech. The Center for Exoplanets and Habitable Worlds is supported
by the Pennsylvania State University, the Eberly College of Science, and
the Pennsylvania Space Grant Consortium. We thank the anonymous referee
for a careful review of this paper.
NR 51
TC 29
Z9 30
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 FEB 10
PY 2012
VL 746
IS 1
AR 111
DI 10.1088/0004-637X/746/1/111
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 926VZ
UT WOS:000302861300111
ER
PT J
AU Su, Y
Dennis, BR
Holman, GD
Wang, TJ
Chamberlin, PC
Savage, S
Veronig, A
AF Su, Yang
Dennis, Brian R.
Holman, Gordon D.
Wang, Tongjiang
Chamberlin, Phillip C.
Savage, Sabrina
Veronig, Astrid
TI OBSERVATIONS OF A TWO-STAGE SOLAR ERUPTIVE EVENT (SEE): EVIDENCE FOR
SECONDARY HEATING
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: coronal mass ejections (CMEs); Sun: flares; Sun: UV radiation; Sun:
X-rays, gamma rays
ID FLARES; ARCADE
AB We present RHESSI, SDO/AIA, SOHO/LASCO, STEREO, and GOES observations of a partially occulted solar eruptive event that occurred at the southwest limb on 2011 March 8. The GOES X-ray light curve shows two peaks separated by almost 2 hr that we interpret as two stages of a single event associated with the delayed eruption of a coronal mass ejection (CME). A hot flux rope formed during the first stage and continued expanding and rising throughout the event. The speed of the flux rope decreased from similar to 120 to 14 km s(-1) during the decay phase of the first stage and increased again during the second stage to become the CME with a speed of similar to 516 km s(-1). RHESSI and GOES data analyses show that the plasma temperature reached over 20 MK in the first stage, then decreased to similar to 10 MK and increased to 15 MK in the second stage. This event provides clear evidence for a secondary heating phase. The enhanced EUV and X-ray emission came from the high corona (similar to 60 arcsec above the limb) in the second stage, similar to 40 arcsec higher than the site of the initial flare emission. STEREO-A on-disk observations indicate that the post-flare loops during this stage were of larger scale sizes and spatially distinct from those in the first stage.
C1 [Su, Yang; Dennis, Brian R.; Holman, Gordon D.; Wang, Tongjiang; Chamberlin, Phillip C.; Savage, Sabrina] NASA, Goddard Space Flight Ctr, Solar Phys Lab Code 671, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Su, Yang; Wang, Tongjiang] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Su, Yang; Veronig, Astrid] Graz Univ, Inst Phys, A-8010 Graz, Austria.
RP Su, Y (reprint author), NASA, Goddard Space Flight Ctr, Solar Phys Lab Code 671, Heliophys Sci Div, Greenbelt, MD 20771 USA.
EM yang.su@uni-graz.at
RI Dennis, Brian/C-9511-2012; Chamberlin, Phillip/C-9531-2012; Holman,
Gordon/C-9548-2012; Veronig, Astrid/B-8422-2009; Su, Yang/J-5381-2014
OI Chamberlin, Phillip/0000-0003-4372-7405;
FU NASA at The Catholic University of America [NNG06GB96A]; European
Community [263086]; NASA [NNX08AE44G, NNX10AN10G]
FX We thank the referee for providing valuable comments and help in
improving this paper. We acknowledge the critical support provided by
Kim Tolbert and Richard Schwartz and their help with the IDL RHESSI data
analysis software and the SSW procedures. We are grateful to Frederick
C. Bruhweiler for managing the NASA Grant NNG06GB96A at The Catholic
University of America, through which one of us (Y.S.) was funded. This
work is also supported in part by the European Community Framework
Programme 7, "High Energy Solar PhysicsData in Europe (HESPE)," grant
agreement No. 263086. The work of T.W. was supported by NASA grants
NNX08AE44G and NNX10AN10G.
NR 12
TC 13
Z9 13
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
EI 2041-8213
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD FEB 10
PY 2012
VL 746
IS 1
AR L5
DI 10.1088/2041-8205/746/1/L5
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 892ZD
UT WOS:000300323500005
ER
PT J
AU Wessels, V
Gangopadhyay, AK
Sahu, KK
Hyers, RW
Canepari, SM
Rogers, JR
Kramer, MJ
Goldman, AI
Robinson, D
Lee, JW
Morris, JR
Kelton, KF
AF Wessels, V.
Gangopadhyay, A. K.
Sahu, K. K.
Hyers, R. W.
Canepari, S. M.
Rogers, J. R.
Kramer, M. J.
Goldman, A. I.
Robinson, D.
Lee, J. W.
Morris, J. R.
Kelton, K. F.
TI Reply to "Comment on 'Rapid chemical and topological ordering in
supercooled liquid Cu46Zr54'"
SO PHYSICAL REVIEW B
LA English
DT Editorial Material
ID BULK METALLIC-GLASS; HEMISPHERICAL TOTAL EMISSIVITY; CU-ZR ALLOYS;
THERMOPHYSICAL PROPERTIES; UNDERCOOLED LIQUID; FORMING LIQUID;
NONCONTACT MEASUREMENTS; HIGH-TEMPERATURES; THERMODYNAMICS; KINETICS
AB The criticisms of Harvey and Gheribi (HG) are directed towards supporting evidence for ordering in supercooled Cu46Zr54 liquid from specific heat measurements and molecular dynamics simulations, not on the direct evidence that came from x-ray diffraction studies. In this reply, we demonstrate that the unique features observed in the specific heat [Cp(T)] are not artifacts of any specific assumptions, as suggested by HG. We have furnished additional details of the MD simulations and clarified related issues raised by HG. The basic conclusions, however, remain unchanged.
C1 [Wessels, V.; Gangopadhyay, A. K.; Sahu, K. K.; Kelton, K. F.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Hyers, R. W.; Canepari, S. M.] Univ Massachusetts, Dept Mech Engn, Amherst, MA 01003 USA.
[Rogers, J. R.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Kramer, M. J.; Goldman, A. I.; Robinson, D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Kramer, M. J.; Goldman, A. I.; Robinson, D.] US DOE, Ames Lab, Ames, IA 50011 USA.
[Robinson, D.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Sahu, K. K.] Swiss Fed Inst Technol, Dept Mat, CH-8046 Zurich, Switzerland.
[Lee, J. W.; Morris, J. R.] Oak Ridge Natl Lab, Oak Ridge, TN 37831 USA.
RP Wessels, V (reprint author), Washington Univ, Dept Phys, St Louis, MO 63130 USA.
RI Morris, J/I-4452-2012
OI Morris, J/0000-0002-8464-9047
NR 38
TC 2
Z9 2
U1 1
U2 14
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1098-0121
J9 PHYS REV B
JI Phys. Rev. B
PD FEB 10
PY 2012
VL 85
IS 6
AR 066102
DI 10.1103/PhysRevB.85.066102
PG 5
WC Physics, Condensed Matter
SC Physics
GA 889QB
UT WOS:000300087200005
ER
PT J
AU Oskin, ME
Arrowsmith, JR
Corona, AH
Elliott, AJ
Fletcher, JM
Fielding, EJ
Gold, PO
Garcia, JJG
Hudnut, KW
Liu-Zeng, J
Teran, OJ
AF Oskin, Michael E.
Arrowsmith, J. Ramon
Hinojosa Corona, Alejandro
Elliott, Austin J.
Fletcher, John M.
Fielding, Eric J.
Gold, Peter O.
Gonzalez Garcia, J. Javier
Hudnut, Ken W.
Liu-Zeng, Jing
Teran, Orlando J.
TI Near-Field Deformation from the El Mayor-Cucapah Earthquake Revealed by
Differential LIDAR
SO SCIENCE
LA English
DT Article
ID 1999 HECTOR MINE; SURFACE RUPTURE; SLIP DISTRIBUTION; BAJA-CALIFORNIA;
LAGUNA-SALADA; FAULT; MEXICO; IRAN; CHINA; ZONE
AB Large [moment magnitude (M-w) >= 7] continental earthquakes often generate complex, multifault ruptures linked by enigmatic zones of distributed deformation. Here, we report the collection and results of a high-resolution (>= nine returns per square meter) airborne light detection and ranging (LIDAR) topographic survey of the 2010 M-w 7.2 El Mayor-Cucapah earthquake that produced a 120-kilometer-long multifault rupture through northernmost Baja California, Mexico. This differential LIDAR survey completely captures an earthquake surface rupture in a sparsely vegetated region with pre-earthquake lower-resolution (5-meter-pixel) LIDAR data. The postevent survey reveals numerous surface ruptures, including previously undocumented blind faults within thick sediments of the Colorado River delta. Differential elevation changes show distributed, kilometer-scale bending strains as large as similar to 10(3) microstrains in response to slip along discontinuous faults cutting crystalline bedrock of the Sierra Cucapah.
C1 [Oskin, Michael E.; Elliott, Austin J.; Gold, Peter O.] Univ Calif Davis, Dept Geol, Davis, CA 95618 USA.
[Arrowsmith, J. Ramon] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Hinojosa Corona, Alejandro; Fletcher, John M.; Gonzalez Garcia, J. Javier; Teran, Orlando J.] Ctr Invest Cient & Educ Super Ensenada, Ensenada 22860, Baja California, Mexico.
[Fielding, Eric J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hudnut, Ken W.] US Geol Survey, Pasadena, CA 91106 USA.
[Liu-Zeng, Jing] China Earthquake Adm, Inst Geol, Natl Key Lab Earthquake Dy nam, Beijing 100029, Peoples R China.
RP Oskin, ME (reprint author), Univ Calif Davis, Dept Geol, 1 Shields Ave, Davis, CA 95618 USA.
EM meoskin@ucdavis.edu
RI Liu-Zeng, Jing/F-8582-2011; Hudnut, Kenneth/B-1945-2009;
Hinojosa-Corona, Alejandro/L-5422-2015; Fielding, Eric/A-1288-2007;
OI Hudnut, Kenneth/0000-0002-3168-4797; Hinojosa-Corona,
Alejandro/0000-0002-2282-337X; Fielding, Eric/0000-0002-6648-8067;
Elliott, Austin/0000-0001-5924-7268
FU NSF RAPID [EAR-1039168, 1039147]; NSF [EAR-0106924]; U.S. Geological
Survey [02HQAG0008]; Consejo Nacional de Ciencia y Tecnologia
[CB-2007-81463]; NASA's Earth Surface and Interior Focus Area
FX LIDAR data acquisition supported by an NSF RAPID grant (EAR-1039168 and
1039147), with additional support from the Southern California
Earthquake Center (supported by NSF-EAR-0106924 and U.S. Geological
Survey grant 02HQAG0008) and Consejo Nacional de Ciencia y Tecnologia
(grant CB-2007-81463). Part of this research was supported by NASA's
Earth Surface and Interior Focus Area and performed at the Jet
Propulsion Laboratory, California Institute of Technology. Y. Fialko, D.
Sandwell, J. Galetzka, and A. Gonzalez assisted with Global Positioning
System data acquisition and processing. C. Crosby, D. Haddad, O.
Kreylos, A. Morelan, and T. Sato provided editorial and computational
assistance. The National Center for Airborne Laser Mapping gathered and
processed the postevent LIDAR data, distributed at OpenTopography
(http://opentopography.org/id/OTLAS.122010.32611.1). We thank INEGI for
granting access to the pre-event LIDAR data used for this study.
Pre-event LIDAR digital elevation model and derived elevation difference
data for the Sierra Cucapah rupture zone are available in the supporting
online material.
NR 29
TC 77
Z9 83
U1 0
U2 44
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 FEB 10
PY 2012
VL 335
IS 6069
BP 702
EP 705
DI 10.1126/science.1213778
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 889AY
UT WOS:000300047100048
PM 22323817
ER
PT J
AU Abbasi, R
Abdou, Y
Abu-Zayyad, T
Ackermann, M
Adams, J
Aguilar, JA
Ahlers, M
Allen, MM
Altmann, D
Andeen, K
Auffenberg, J
Bai, X
Baker, M
Barwick, SW
Bay, R
Alba, JLB
Beattie, K
Beatty, JJ
Bechet, S
Becker, JK
Becker, KH
Benabderrahmane, ML
BenZvi, S
Berdermann, J
Berghaus, P
Berley, D
Bernardini, E
Bertrand, D
Besson, DZ
Bindig, D
Bissok, M
Blaufuss, E
Blumenthal, J
Boersma, DJ
Bohm, C
Bose, D
Boser, S
Botner, O
Brown, AM
Buitink, S
Caballero-Mora, KS
Carson, M
Chirkin, D
Christy, B
Clevermann, F
Cohen, S
Colnard, C
Cowen, DF
Silva, AHC
D'Agostino, MV
Danninger, M
Daughhetee, J
Davis, JC
De Clercq, C
Degner, T
Demirors, L
Descamps, F
Desiati, P
de Vries-Uiterweerd, G
DeYoung, T
Diaz-Velez, JC
Dierckxsens, M
Dreyer, J
Dumm, JP
Dunkman, M
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
Fox, BD
Franckowiak, A
Franke, R
Gaisser, TK
Gallagher, J
Gerhardt, L
Gladstone, L
Glusenkamp, T
Goldschmidt, A
Goodman, JA
Gora, D
Grant, D
Griesel, T
Gross, A
Grullon, S
Gurtner, M
Ha, C
Ismail, AH
Hallgren, A
Halzen, F
Han, K
Hanson, K
Heinen, D
Helbing, K
Hellauer, R
Hickford, S
Hill, GC
Hoffman, KD
Hoffmann, B
Homeier, A
Hoshina, K
Huelsnitz, W
Hulss, JP
Hulth, PO
Hultqvist, K
Hussain, S
Ishihara, A
Jacobi, E
Jacobsen, J
Japaridze, GS
Johansson, H
Kampert, KH
Kappes, A
Karg, T
Karle, A
Kenny, P
Kiryluk, J
Kislat, F
Klein, SR
Kohne, JH
Kohnen, G
Kolanoski, H
Kopke, L
Kopper, S
Koskinen, DJ
Kowalski, M
Kowarik, T
Krasberg, M
Kroll, G
Kurahashi, N
Kuwabara, T
Labare, M
Laihem, K
Landsman, H
Larson, MJ
Lauer, R
Lunemann, J
Madsen, J
Marotta, A
Maruyama, R
Mase, K
Matis, HS
Meagher, K
Merck, M
Meszaros, P
Meures, T
Miarecki, S
Middell, E
Milke, N
Miller, J
Montaruli, T
Morse, R
Movit, SM
Nahnhauer, R
Nam, JW
Naumann, U
Nygren, DR
Odrowski, S
Olivas, A
Olivo, M
O'Murchadha, A
Panknin, S
Paul, L
de los Heros, CP
Petrovic, J
Piegsa, A
Pieloth, D
Porrata, R
Posselt, J
Price, CC
Price, PB
Przybylski, GT
Rawlins, K
Redl, P
Resconi, E
Rhode, W
Ribordy, M
Richman, M
Rodrigues, JP
Rothmaier, F
Rott, C
Ruhe, T
Rutledge, D
Ruzybayev, B
Ryckbosch, D
Sander, HG
Santander, M
Sarkar, S
Schatto, K
Schmidt, T
Schonwald, A
Schukraft, A
Schultes, A
Schulz, O
Schunck, M
Seckel, D
Semburg, B
Seo, SH
Sestayo, Y
Seunarine, S
Silvestri, A
Spiczak, GM
Spiering, C
Stamatikos, M
Stanev, T
Stezelberger, T
Stokstad, RG
Stossl, A
Strahler, EA
Strom, R
Stuer, M
Sullivan, GW
Swillens, Q
Taavola, H
Taboada, I
Tamburro, A
Tepe, A
Ter-Antonyan, S
Tilav, S
Toale, PA
Toscano, S
Tosi, D
van Eijndhoven, N
Vandenbroucke, J
Van Overloop, A
van Santen, J
Vehring, M
Voge, M
Walck, C
Waldenmaier, T
Wallraff, M
Walter, M
Weaver, C
Wendt, C
Westerhoff, S
Whitehorn, N
Wiebe, K
Wiebusch, CH
Williams, DR
Wischnewski, R
Wissing, H
Wolf, M
Wood, TR
Woschnagg, K
Xu, C
Xu, DL
Xu, XW
Yanez, JP
Yodh, G
Yoshida, S
Zarzhitsky, P
Zoll, M
AF Abbasi, R.
Abdou, Y.
Abu-Zayyad, T.
Ackermann, M.
Adams, J.
Aguilar, J. A.
Ahlers, M.
Allen, M. M.
Altmann, D.
Andeen, K.
Auffenberg, J.
Bai, X.
Baker, M.
Barwick, S. W.
Bay, R.
Alba, J. L. Bazo
Beattie, K.
Beatty, J. J.
Bechet, S.
Becker, J. K.
Becker, K. -H.
Benabderrahmane, M. L.
BenZvi, S.
Berdermann, J.
Berghaus, P.
Berley, D.
Bernardini, E.
Bertrand, D.
Besson, D. Z.
Bindig, D.
Bissok, M.
Blaufuss, E.
Blumenthal, J.
Boersma, D. J.
Bohm, C.
Bose, D.
Boeser, S.
Botner, O.
Brown, A. M.
Buitink, S.
Caballero-Mora, K. S.
Carson, M.
Chirkin, D.
Christy, B.
Clevermann, F.
Cohen, S.
Colnard, C.
Cowen, D. F.
Silva, A. H. Cruz
D'Agostino, M. V.
Danninger, M.
Daughhetee, J.
Davis, J. C.
De Clercq, C.
Degner, T.
Demiroers, L.
Descamps, F.
Desiati, P.
de Vries-Uiterweerd, G.
DeYoung, T.
Diaz-Velez, J. C.
Dierckxsens, M.
Dreyer, J.
Dumm, J. P.
Dunkman, M.
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.
Fox, B. D.
Franckowiak, A.
Franke, R.
Gaisser, T. K.
Gallagher, J.
Gerhardt, L.
Gladstone, L.
Gluesenkamp, T.
Goldschmidt, A.
Goodman, J. A.
Gora, D.
Grant, D.
Griesel, T.
Gross, A.
Grullon, S.
Gurtner, M.
Ha, C.
Ismail, A. Haj
Hallgren, A.
Halzen, F.
Han, K.
Hanson, K.
Heinen, D.
Helbing, K.
Hellauer, R.
Hickford, S.
Hill, G. C.
Hoffman, K. D.
Hoffmann, B.
Homeier, A.
Hoshina, K.
Huelsnitz, W.
Huelss, J. -P.
Hulth, P. O.
Hultqvist, K.
Hussain, S.
Ishihara, A.
Jacobi, E.
Jacobsen, J.
Japaridze, G. S.
Johansson, H.
Kampert, K. -H.
Kappes, A.
Karg, T.
Karle, A.
Kenny, P.
Kiryluk, J.
Kislat, F.
Klein, S. R.
Koehne, J. -H.
Kohnen, G.
Kolanoski, H.
Koepke, L.
Kopper, S.
Koskinen, D. J.
Kowalski, M.
Kowarik, T.
Krasberg, M.
Kroll, G.
Kurahashi, N.
Kuwabara, T.
Labare, M.
Laihem, K.
Landsman, H.
Larson, M. J.
Lauer, R.
Luenemann, J.
Madsen, J.
Marotta, A.
Maruyama, R.
Mase, K.
Matis, H. S.
Meagher, K.
Merck, M.
Meszaros, P.
Meures, T.
Miarecki, S.
Middell, E.
Milke, N.
Miller, J.
Montaruli, T.
Morse, R.
Movit, S. M.
Nahnhauer, R.
Nam, J. W.
Naumann, U.
Nygren, D. R.
Odrowski, S.
Olivas, A.
Olivo, M.
O'Murchadha, A.
Panknin, S.
Paul, L.
de los Heros, C. Perez
Petrovic, J.
Piegsa, A.
Pieloth, D.
Porrata, R.
Posselt, J.
Price, C. C.
Price, P. B.
Przybylski, G. T.
Rawlins, K.
Redl, P.
Resconi, E.
Rhode, W.
Ribordy, M.
Richman, M.
Rodrigues, J. P.
Rothmaier, F.
Rott, C.
Ruhe, T.
Rutledge, D.
Ruzybayev, B.
Ryckbosch, D.
Sander, H. -G.
Santander, M.
Sarkar, S.
Schatto, K.
Schmidt, T.
Schoenwald, A.
Schukraft, A.
Schultes, A.
Schulz, O.
Schunck, M.
Seckel, D.
Semburg, B.
Seo, S. H.
Sestayo, Y.
Seunarine, S.
Silvestri, A.
Spiczak, G. M.
Spiering, C.
Stamatikos, M.
Stanev, T.
Stezelberger, T.
Stokstad, R. G.
Stoessl, A.
Strahler, E. A.
Strom, R.
Stueer, M.
Sullivan, G. W.
Swillens, Q.
Taavola, H.
Taboada, I.
Tamburro, A.
Tepe, A.
Ter-Antonyan, S.
Tilav, S.
Toale, P. A.
Toscano, S.
Tosi, D.
van Eijndhoven, N.
Vandenbroucke, J.
Van Overloop, A.
van Santen, J.
Vehring, M.
Voge, M.
Walck, C.
Waldenmaier, T.
Wallraff, M.
Walter, M.
Weaver, Ch.
Wendt, C.
Westerhoff, S.
Whitehorn, N.
Wiebe, K.
Wiebusch, C. H.
Williams, D. R.
Wischnewski, 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.
Zoll, M.
CA IceCube Collaboration
TI OBSERVATION OF ANISOTROPY IN THE GALACTIC COSMIC-RAY ARRIVAL DIRECTIONS
AT 400 TeV WITH ICECUBE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astroparticle physics; cosmic rays; neutrinos
ID MAGNETOHYDRODYNAMIC TURBULENCE; INTERSTELLAR-MEDIUM; MAGNETIC-FIELD;
MILAGRO; DIFFUSION; ORIGIN
AB In this paper we report the first observation in the Southern hemisphere of an energy dependence in the Galactic cosmic-ray anisotropy up to a few hundred TeV. This measurement was performed using cosmic-ray-induced muons recorded by the partially deployed IceCube observatory between 2009 May and 2010 May. The data include a total of 33 x 10(9) muon events with a median angular resolution of similar to 3 degrees. A sky map of the relative intensity in arrival direction over the Southern celestial sky is presented for cosmic-ray median energies of 20 and 400 TeV. The same large-scale anisotropy observed at median energies around 20 TeV is not present at 400 TeV. Instead, the high-energy sky map shows a different anisotropy structure including a deficit with a post-trial significance of -6.3 sigma. This anisotropy reveals a new feature of the Galactic cosmic-ray distribution, which must be incorporated into theories of the origin and propagation of cosmic rays.
C1 [Abbasi, R.; Aguilar, J. A.; Andeen, K.; Baker, M.; BenZvi, S.; Chirkin, D.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Eisch, J.; Fadiran, O.; Feintzeig, J.; Gladstone, L.; Grullon, S.; Halzen, F.; Hanson, K.; Hill, G. C.; Hoshina, K.; Jacobsen, J.; Karle, A.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; Merck, M.; Montaruli, T.; Morse, R.; O'Murchadha, A.; Price, C. C.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Ackermann, M.; Alba, J. L. Bazo; Benabderrahmane, M. L.; Berdermann, J.; Bernardini, E.; Silva, A. H. Cruz; Franke, R.; Gluesenkamp, T.; Gora, D.; Han, K.; Jacobi, E.; Kislat, F.; Lauer, R.; Middell, E.; Nahnhauer, R.; Schoenwald, A.; Spiering, C.; Stoessl, A.; Tosi, D.; Walter, M.; Wischnewski, R.; Yanez, J. P.] DESY, D-15735 Zeuthen, Germany.
[Adams, J.; Brown, A. M.; Gross, A.; Hickford, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
[Ahlers, M.; Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England.
[Allen, M. M.; Caballero-Mora, K. S.; Cowen, D. F.; DeYoung, T.; Dunkman, M.; Fox, B. D.; Ha, C.; Koskinen, D. J.; Larson, M. J.; Meszaros, P.; Rutledge, D.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Altmann, D.; Bissok, M.; Blumenthal, J.; Boersma, D. J.; Euler, S.; Heinen, D.; Hoffmann, B.; Huelss, J. -P.; Laihem, K.; Paul, L.; Schukraft, A.; Schunck, M.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany.
[Auffenberg, J.; Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Gurtner, M.; Helbing, K.; Kampert, K. -H.; Karg, T.; Kopper, S.; Naumann, U.; Posselt, J.; Schultes, A.; Semburg, B.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
[Bai, X.; Berghaus, P.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tilav, S.; Xu, C.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Bai, X.; Berghaus, P.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Tilav, S.; Xu, C.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Barwick, S. W.; Nam, J. W.; Silvestri, A.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Bay, R.; D'Agostino, M. V.; Filimonov, K.; Gerhardt, L.; Kiryluk, J.; Klein, S. R.; Miarecki, S.; Porrata, R.; Price, P. B.; Vandenbroucke, J.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Beattie, K.; Gerhardt, L.; Goldschmidt, A.; Kiryluk, J.; Klein, S. R.; Matis, H. S.; Miarecki, S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Beatty, J. J.; Davis, J. C.; Rott, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Beatty, J. J.; Davis, J. 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.
[Bechet, S.; Bertrand, D.; Dierckxsens, M.; Hanson, K.; Marotta, A.; Meures, T.; Petrovic, J.; Swillens, Q.] Univ Libre Brussels, Sci Fac CP230, B-1050 Brussels, Belgium.
[Becker, J. K.; Dreyer, J.; Fedynitch, A.; Olivo, M.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany.
[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.
[Besson, D. Z.; Kenny, P.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Zoll, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Bose, D.; Buitink, S.; De Clercq, C.; Labare, M.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
[Boeser, S.; Degner, T.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Panknin, S.; Stueer, M.; Voge, M.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany.
[Botner, O.; Engdegard, O.; Hallgren, A.; Miller, J.; de los Heros, C. Perez; Strom, R.; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
[Clevermann, F.; Koehne, J. -H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany.
[Cohen, S.; Demiroers, L.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland.
[Colnard, C.; Gross, A.; Odrowski, S.; Resconi, E.; Schulz, O.; Sestayo, Y.; Wolf, M.] Max Planck Inst Kernphys, D-69177 Heidelberg, Germany.
[Cowen, D. F.; Meszaros, P.; Movit, S. M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] So Univ, Dept Phys, Baton Rouge, LA 70813 USA.
[Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Grant, D.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada.
[Griesel, T.; Koepke, L.; Kowarik, T.; Kroll, G.; Luenemann, J.; Piegsa, A.; Rothmaier, F.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany.
[Huelsnitz, W.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Ishihara, A.; Mase, K.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan.
[Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA.
[Kappes, A.; Kolanoski, H.; Waldenmaier, T.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany.
[Kohnen, G.] Univ Mons, B-7000 Mons, Belgium.
[Rawlins, K.] Univ Alaska Anchorage, Dept Phys & Astron, Anchorage, AK 99508 USA.
[Seunarine, S.] Univ W Indies, Dept Phys, BB-11000 Bridgetown, Barbados.
[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Toale, P. A.; Williams, D. R.; Xu, D. L.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Montaruli, T.] Dipartimento Fis, Sez INFN, I-70126 Bari, Italy.
[Abdou, Y.; Carson, M.; Descamps, F.; de Vries-Uiterweerd, G.; Feusels, T.; Ismail, A. Haj; Ryckbosch, D.; Van Overloop, A.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium.
[Abu-Zayyad, T.; Madsen, J.; Spiczak, G. M.; Tamburro, A.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA.
RP Abbasi, R (reprint author), Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA.
RI Taavola, Henric/B-4497-2011; Tjus, Julia/G-8145-2012; Wiebusch,
Christopher/G-6490-2012; Tamburro, Alessio/A-5703-2013; Auffenberg,
Jan/D-3954-2014; Botner, Olga/A-9110-2013; Hallgren, Allan/A-8963-2013;
Koskinen, David/G-3236-2014; Kowalski, Marek/G-5546-2012; Aguilar
Sanchez, Juan Antonio/H-4467-2015; Maruyama, Reina/A-1064-2013; Sarkar,
Subir/G-5978-2011; Beatty, James/D-9310-2011
OI Perez de los Heros, Carlos/0000-0002-2084-5866; Taavola,
Henric/0000-0002-2604-2810; Buitink, Stijn/0000-0002-6177-497X;
Benabderrahmane, Mohamed Lotfi/0000-0003-4410-5886; Wiebusch,
Christopher/0000-0002-6418-3008; Carson, Michael/0000-0003-0400-7819;
Auffenberg, Jan/0000-0002-1185-9094; Koskinen,
David/0000-0002-0514-5917; 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
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); Research Department of Plasmas with
Complex Interactions (Bochum), Germany; Fund for Scientific Research
(FNRS-FWO); FWO Odysseus; Flanders Institute to encourage scientific and
technological research in industry (IWT), Belgian Federal Science Policy
Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New
Zealand; Japan Society for Promotion of Science (JSPS); Swiss National
Science Foundation (SNSF), Switzerland; EU; Capes Foundation, Ministry
of Education of Brazil
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), 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, United Kingdom;
Marsden Fund, New Zealand; Japan Society for Promotion of Science
(JSPS); and the Swiss National Science Foundation (SNSF), Switzerland.
A. Gross acknowledges support by the EU Marie Curie OIF Program; J. P.
Rodrigues acknowledges support by the Capes Foundation, Ministry of
Education of Brazil.
NR 36
TC 70
Z9 71
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 FEB 10
PY 2012
VL 746
IS 1
DI 10.1088/0004-637X/746/1/33
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 926VZ
UT WOS:000302861300033
ER
PT J
AU Camilo, F
Kerr, M
Ray, PS
Ransom, SM
Johnston, S
Romani, RW
Parent, D
DeCesar, ME
Harding, AK
Donato, D
Parkinson, PMS
Ferrara, EC
Freire, PCC
Guillemot, L
Keith, M
Kramer, M
Wood, KS
AF Camilo, F.
Kerr, M.
Ray, P. S.
Ransom, S. M.
Johnston, S.
Romani, R. W.
Parent, D.
DeCesar, M. E.
Harding, A. K.
Donato, D.
Parkinson, P. M. Saz
Ferrara, E. C.
Freire, P. C. C.
Guillemot, L.
Keith, M.
Kramer, M.
Wood, K. S.
TI PSR J2030+3641: RADIO DISCOVERY AND GAMMA-RAY STUDY OF A MIDDLE-AGED
PULSAR IN THE NOW IDENTIFIED FERMI-LAT SOURCE 1FGL J2030.0+3641
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma rays: stars; pulsars: individual (PSR J2030+3641)
ID LARGE-AREA TELESCOPE; BLIND FREQUENCY SEARCHES; MILLISECOND PULSARS;
MAGNETIC-FIELD; LIGHT CURVES; SLOT GAPS; EMISSION; POLARIZATION;
ACCELERATION; RADIATION
AB In a radio search with the Green Bank Telescope of three unidentified low Galactic latitude Fermi Large Area Telescope (LAT) sources, we have discovered the middle-aged pulsar J2030+3641 associated with 1FGL J2030.0+3641 (2FGL J2030.0+3640). Following the detection of gamma-ray pulsations using a radio ephemeris, we have obtained a phase-coherent timing solution based on gamma-ray and radio pulse arrival times which spans the entire Fermi mission. With a rotation period of 0.2 s, a spin-down luminosity of 3 x 10(34) erg s(-1), and a characteristic age of 0.5 Myr, PSR J2030+3641 is a middle-aged neutron star with spin parameters similar to those of the exceedingly gamma-ray-bright and radio-undetected Geminga. Its gamma-ray flux is 1% that of Geminga, primarily because of its much larger distance, as suggested by the large integrated column density of free electrons, DM = 246 pc cm(-3). We fit the gamma-ray light curve, along with limited radio polarimetric constraints, to four geometrical models of magnetospheric emission, and while none of the fits have high significance some are encouraging and suggest that further refinements of these models may be worthwhile. We argue that not many more non-millisecond radio pulsars may be detected along the Galactic plane that are responsible for LAT sources, but that modified methods to search for gamma-ray pulsations should be productive-PSR J2030+3641 would have been found blindly in gamma rays if only >= 0.8 GeV photons had been considered, owing to its relatively flat spectrum and location in a region of high soft background.
C1 [Camilo, F.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Kerr, M.; Romani, R. W.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Kerr, M.; Romani, R. W.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Ray, P. S.; Wood, K. S.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA.
[Ransom, S. M.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Johnston, S.; Keith, M.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Parent, D.] George Mason Univ, Ctr Earth Observing & Space Res, Coll Sci, Fairfax, VA 22030 USA.
[DeCesar, M. E.; Harding, A. K.; Donato, D.; Ferrara, E. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Donato, D.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Donato, D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Donato, D.] CRESST, Greenbelt, MD 20771 USA.
[Parkinson, P. M. Saz] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Freire, P. C. C.; Guillemot, L.; Kramer, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Kramer, M.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
RP Camilo, F (reprint author), Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA.
EM fernando@astro.columbia.edu; kerrm@stanford.edu; Paul.Ray@nrl.navy.mil
RI Saz Parkinson, Pablo Miguel/I-7980-2013;
OI Ray, Paul/0000-0002-5297-5278; Ransom, Scott/0000-0001-5799-9714
FU NASA [PF0-110073, NAS8-03060]
FX The GBT is operated by the National Radio Astronomy Observatory, a
facility of the National Science Foundation operated under cooperative
agreement by Associated Universities, Inc. The Fermi-LAT Collaboration
acknowledges generous ongoing support from a number of agencies and
institutes that have supported both the development and the operation of
the LAT as well as scientific data analysis. These include the National
Aeronautics and Space Administration (NASA) and the Department of Energy
in the United States, the Commissariat a l'Energie Atomique and the
Centre National de la Recherche Scientifique/Institut National de
Physique Nucleaire et de Physique des Particules in France, the Agenzia
Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in
Italy, the Ministry of Education, Culture, Sports, Science and
Technology (MEXT), High Energy Accelerator Research Organization (KEK)
and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A.
Wallenberg Foundation, the Swedish Research Council, and the Swedish
National Space Board in Sweden. Support for this work was provided by
NASA through Einstein Postdoctoral Fellowship Award Number PF0-110073
issued by the Chandra X-ray Observatory Center, which is operated by the
Smithsonian Astrophysical Observatory for and on behalf of NASA under
contract NAS8-03060.
NR 54
TC 11
Z9 12
U1 0
U2 1
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 FEB 10
PY 2012
VL 746
IS 1
DI 10.1088/0004-637X/746/1/39
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 926VZ
UT WOS:000302861300039
ER
PT J
AU Geissler, K
Metchev, SA
Pham, A
Larkin, JE
McElwain, M
Hillenbrand, LA
AF Geissler, Kerstin
Metchev, Stanimir A.
Pham, Alfonse
Larkin, James E.
McElwain, Michael
Hillenbrand, Lynne A.
TI A SUBSTELLAR COMMON PROPER-MOTION COMPANION TO THE PLEIAD HII 1348
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: visual; brown dwarfs; instrumentation: adaptive optics; stars:
individual (Cl Melotte 22 1348); stars: low-mass
ID LOW-MASS STARS; INTEGRAL FIELD SPECTROGRAPH; ADAPTIVE OPTICS SYSTEM;
BROWN DWARF BINARIES; OPEN CLUSTERS; EVOLUTIONARY MODELS; WIDE BINARIES;
GIANT PLANETS; LITHIUM TEST; T-DWARFS
AB We announce the identification of a proper-motion companion to the star Hii 1348, a K5V member of the Pleiades open cluster. The existence of a faint point source 1.'' 1 away from Hii 1348 was previously known from adaptive optics imaging by Bouvier et al. However, because of a high likelihood of background star contamination and in the absence of follow-up astrometry, Bouvier et al. tentatively concluded that the candidate companion was not physically associated with Hii 1348. We establish the proper-motion association of the pair from adaptive optics imaging with the Palomar 5 m telescope. Adaptive optics spectroscopy with the integral field spectrograph OSIRIS on the Keck 10 m telescope reveals that the companion has a spectral type of M8 +/- 1. According to substellar evolution models, the M8 spectral type resides within the substellar mass regime at the age of the Pleiades. The primary itself is a known double-lined spectroscopic binary, which makes the resolved companion, Hii 1348B, the least massive and widest component of this hierarchical triple system and the first substellar companion to a stellar primary in the Pleiades.
C1 [Geissler, Kerstin; Metchev, Stanimir A.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Pham, Alfonse] Indiana Univ, Ctr Explorat Energy & Matter, Bloomington, IN 47408 USA.
[Larkin, James E.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[McElwain, Michael] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, Lab Exoplanets & Stellar Astrophys, Greenbelt, MD 20771 USA.
[Hillenbrand, Lynne A.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
RP Geissler, K (reprint author), SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
EM geissler@mail.astro.sunysb.edu
FU Spitzer Fellowship Program [1273192]
FX Partial support for S. A. M. was provided through the Spitzer Fellowship
Program under award 1273192. The authors also wish to extend special
thanks to those of Hawaiian ancestry on whose sacred mountain of Mauna
Kea we are privileged to be guests.
NR 55
TC 11
Z9 11
U1 0
U2 1
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 FEB 10
PY 2012
VL 746
IS 1
DI 10.1088/0004-637X/746/1/44
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 926VZ
UT WOS:000302861300044
ER
PT J
AU Luna, M
Karpen, JT
DeVore, CR
AF Luna, M.
Karpen, J. T.
DeVore, C. R.
TI FORMATION AND EVOLUTION OF A MULTI-THREADED SOLAR PROMINENCE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: corona; Sun: filaments; prominences; Sun: magnetic topology
ID MAGNETIC-FIELD; CORONAL LOOPS; THERMAL NONEQUILIBRIUM; QUIESCENT
PROMINENCES; ALPHA FILTERGRAMS; ACTIVE-REGION; FILAMENT; DYNAMICS;
FLOWS; MODEL
AB We investigate the process of formation and subsequent evolution of prominence plasma in a filament channel and its overlying arcade. We construct a three-dimensional time-dependent model of an intermediate quiescent prominence suitable to be compared with observations. We combine the magnetic field structure of a three-dimensional sheared double arcade with one-dimensional independent simulations of many selected flux tubes, in which the thermal nonequilibrium process governs the plasma evolution. We have found that the condensations in the corona can be divided into two populations: threads and blobs. Threads are massive condensations that linger in the flux tube dips. Blobs are ubiquitous small condensations that are produced throughout the filament and overlying arcade magnetic structure, and rapidly fall to the chromosphere. The threads are the principal contributors to the total mass, whereas the blob contribution is small. The total prominence mass is in agreement with observations, assuming reasonable filling factors of order 0.001 and a fixed number of threads. The motion of the threads is basically horizontal, while blobs move in all directions along the field. We have generated synthetic images of the whole structure in an Ha proxy and in two EUV channels of the Atmospheric Imaging Assembly instrument on board Solar Dynamics Observatory, thus showing the plasma at cool, warm, and hot temperatures. The predicted differential emission measure of our system agrees very well with observations in the temperature range log T = 4.6-5.7. We conclude that the sheared-arcade magnetic structure and plasma behavior driven by thermal nonequilibrium fit the abundant observational evidence well for typical intermediate prominences.
C1 [Luna, M.] NASA, CRESST, GSFC, Greenbelt, MD 20771 USA.
[Luna, M.] NASA, Space Weather Lab, GSFC, Greenbelt, MD 20771 USA.
[DeVore, C. R.] USN, Res Lab, Washington, DC 20375 USA.
RP Luna, M (reprint author), NASA, CRESST, GSFC, Greenbelt, MD 20771 USA.
RI DeVore, C/A-6067-2015; Karpen, Judith/E-1484-2012
OI DeVore, C/0000-0002-4668-591X;
FU University of Maryland at College Park; people of CRESST; NASA through
NASA Center for Climate Simulation (NCCS) at Goddard Space Flight
Center; ISSI
FX This work has been supported by the NASA Heliophysics SR&T program. M.
L. also acknowledges support from the University of Maryland at College
Park and the people of CRESST. Resources supporting this work were
provided by the NASA High-End Computing (HEC) Program through the NASA
Center for Climate Simulation (NCCS) at Goddard Space Flight Center. All
of us are grateful to our colleagues on international teams on solar
prominences hosted by the International Space Science Institute (ISSI)
in Bern, Switzerland, especially team leader N. Labrosse, and
acknowledge the support of ISSI, where this work has been presented.
Finally, we thank J. A. Klimchuk, T. A. Kucera, S. R. Habbal, and K. K.
Reeves for helpful discussions.
NR 63
TC 39
Z9 39
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 10
PY 2012
VL 746
IS 1
DI 10.1088/0004-637X/746/1/30
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 926VZ
UT WOS:000302861300030
ER
PT J
AU Weisskopf, MC
Elsner, RF
Kolodziejczak, JJ
O'Dell, SL
Tennant, AF
AF Weisskopf, Martin C.
Elsner, Ronald F.
Kolodziejczak, Jeffery J.
O'Dell, Stephen L.
Tennant, Allyn F.
TI UNRAVELING THE GEOMETRY OF THE CRAB NEBULA's "INNER RING"
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: individual (Crab Nebula)
ID PULSAR WIND NEBULAE; ORIGIN; TORUS
AB Chandra images of the Crab Nebula resolve the detailed structure of its "inner ring," possibly a termination shock where pulsar-accelerated relativistic particles begin to emit X radiation. Analysis of these images finds that the center of the ellipse-presumably a circular ring in projection-lies about 0.'' 9 (10 light days at 2 kpc) from the pulsar's image, at a position angle of about 300 degrees (east of north). This analysis also measures properties of the ellipse: the position angle of the semi-major axis is about 210 degrees (east of north); the aspect ratio is 0.49. In a simple-albeit, not unique-de-projection of the observed geometry, a circular ring is centered on the axis of symmetry of the pulsar wind nebula. This ring is not equatorial but rather lies near + 4.degrees 5 latitude in pulsar-centered coordinates. Alternative geometries are briefly discussed.
C1 [Weisskopf, Martin C.; Elsner, Ronald F.; Kolodziejczak, Jeffery J.; O'Dell, Stephen L.; Tennant, Allyn F.] NASA, Space Sci Off, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Weisskopf, MC (reprint author), NASA, Space Sci Off, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
OI O'Dell, Stephen/0000-0002-1868-8056
NR 15
TC 9
Z9 9
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 FEB 10
PY 2012
VL 746
IS 1
DI 10.1088/0004-637X/746/1/41
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 926VZ
UT WOS:000302861300041
ER
PT J
AU Tokar, RL
Johnson, RE
Thomsen, MF
Sittler, EC
Coates, AJ
Wilson, RJ
Crary, FJ
Young, DT
Jones, GH
AF Tokar, R. L.
Johnson, R. E.
Thomsen, M. F.
Sittler, E. C.
Coates, A. J.
Wilson, R. J.
Crary, F. J.
Young, D. T.
Jones, G. H.
TI Detection of exospheric O-2(+) at Saturn's moon Dione
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID ION-CYCLOTRON WAVES; PLASMA; RHEA; MAGNETOSPHERE; SATELLITES; TETHYS
AB During a close pass of Cassini through the plasma wake of Saturn's moon Dione on April 7, 2010 the Cassini Plasma Spectrometer (CAPS) detected molecular oxygen ions (O-2(+)) on pick up ring velocity distributions, thus providing the first in situ detection of a neutral exosphere surrounding the icy moon. The density of O-2(+) determined from the CAPS data ranges from 0.01 to 0.09 /cm(3) and is used to estimate the exosphere O-2 radial column density, obtaining the range 0.9 to 7 x 10(11)/cm(2). CAPS was unable to directly detect pick up H2O+ from the exosphere but the observations can be used to set an upper limit to their density of similar to 10 times the O-2(+) density. Citation: Tokar, R. L., R. E. Johnson, M. F. Thomsen, E. C. Sittler, A. J. Coates, R. J. Wilson, F. J. Crary, D. T. Young, and G. H. Jones (2012), Detection of exospheric O-2(+) at Saturn's moon Dione, Geophys. Res. Lett., 39, L03105, doi:10.1029/2011GL050452.
C1 [Tokar, R. L.; Thomsen, M. F.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Johnson, R. E.] Univ Virginia, Charlottesville, VA 22904 USA.
[Sittler, E. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Coates, A. J.; Jones, G. H.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Wilson, R. J.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA.
[Crary, F. J.; Young, D. T.] SW Res Inst, San Antonio, TX 78229 USA.
[Jones, G. H.] UCL Birkbeck, Ctr Planetary Sci, London, England.
RP Tokar, RL (reprint author), Los Alamos Natl Lab, Mail Stop D466, Los Alamos, NM 87545 USA.
EM rlt@lanl.gov
RI Wilson, Rob/C-2689-2009; Jones, Geraint/C-1682-2008; Coates,
Andrew/C-2396-2008;
OI Wilson, Rob/0000-0001-9276-2368; Coates, Andrew/0000-0002-6185-3125;
Jones, Geraint/0000-0002-5859-1136
FU JPL [1243218]; Southwest Research Institute; UK Science and Technology
Facilities Council (STFC); ESA via UK Space Agency; CAPS-ELS science by
STFC; STFC
FX The authors wish to thank Krishan Khurana for helpful conversations
regarding the Cassini Dione observations. The work of U.S. co-authors
was supported by JPL contracts 1243218 with Southwest Research
Institute. We acknowledge support of the CAPS ELS operations and
software team by the UK Science and Technology Facilities Council (STFC,
to 2010) and by ESA via UK Space Agency (from 2011), and support of
CAPS-ELS science by STFC. GHJ is supported by an STFC Advanced
Fellowship. Cassini is managed by the Jet Propulsion Laboratory for
NASA.
NR 23
TC 20
Z9 20
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 FEB 9
PY 2012
VL 39
AR L03105
DI 10.1029/2011GL050452
PG 7
WC Geosciences, Multidisciplinary
SC Geology
GA 891UB
UT WOS:000300241000004
ER
PT J
AU He, H
Li, C
Loughner, CP
Li, ZQ
Krotkov, NA
Yang, K
Wang, L
Zheng, YF
Bao, XD
Zhao, GQ
Dickerson, RR
AF He, Hao
Li, Can
Loughner, Christopher P.
Li, Zhanqing
Krotkov, Nickolay A.
Yang, Kai
Wang, Lei
Zheng, Youfei
Bao, Xiangdong
Zhao, Guoqiang
Dickerson, Russell R.
TI SO2 over central China: Measurements, numerical simulations and the
tropospheric sulfur budget
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID LONG-RANGE TRANSPORT; POLLUTION CONTROL POLICIES; AIR-QUALITY BENEFITS;
PEARL RIVER-DELTA; DRY DEPOSITION; INTEX-B; EAST-ASIA; PART I;
HOMOGENEOUS OXIDATION; AIRCRAFT MEASUREMENTS
AB SO2 in central China was measured in situ from an aircraft and remotely using the Ozone Monitoring Instrument (OMI) from the Aura satellite; results were used to develop a numerical tool for evaluating the tropospheric sulfur budget - sources, sinks, transformation and transport. In April 2008, measured ambient SO2 concentrations decreased from similar to 7 ppbv near the surface to similar to 1 ppbv at 1800 m altitude (an effective scale height of similar to 800 m), but distinct SO2 plumes were observed between 1800 and 4500 m, the aircraft's ceiling. These free tropospheric plumes play a major role in the export of SO2 and in the accuracy of OMI retrievals. The mean SO2 column contents from aircraft measurements (0.73 DU, Dobson Units) and operational OMI SO2 products (0.63 +/- 0.26 DU) were close. The OMI retrievals were well correlated with in situ measurements (r = 0.84), but showed low bias (slope = 0.54). A new OMI retrieval algorithm was tested and showed improved agreement and bias (r = 0.87, slope = 0.86). The Community Multiscale Air Quality (CMAQ) model was used to simulate sulfur chemistry, exhibiting reasonable agreement (r = 0.62, slope = 1.33) with in situ SO2 columns. The mean CMAQ SO2 loading over central and eastern China was 54 kT, similar to 30% more than the estimate from OMI SO2 products, 42 kT. These numerical simulations, constrained by observations, indicate that similar to 50% (35 to 61%) of the anthropogenic sulfur emissions were transported downwind, and the overall lifetime of tropospheric SO2 was 38 +/- 7 h.
C1 [He, Hao; Li, Zhanqing; Yang, Kai; Dickerson, Russell R.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
[Bao, Xiangdong; Zhao, Guoqiang] Henan Meteorol Bur, Zhengzhou 450003, Peoples R China.
[Li, Can; Loughner, Christopher P.; Krotkov, Nickolay A.; Yang, Kai] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Li, Can; Loughner, Christopher P.; Li, Zhanqing; Dickerson, Russell R.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Wang, Lei; Zheng, Youfei] Nanjing Univ Informat Sci Technol, Nanjing 210044, Jiangsu, Peoples R China.
[Li, Zhanqing] Beijing Normal Univ, State Key Lab Earth Surface Proc & Resource, GCESS, Beijing 100875, Peoples R China.
[Dickerson, Russell R.] Univ Maryland, Dept Chem & Biochem, College Pk, MD 20742 USA.
RP He, H (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA.
EM russ@atmos.umd.edu
RI Dickerson, Russell/F-2857-2010; Li, Can/F-6867-2011; Krotkov,
Nickolay/E-1541-2012; He, Hao/E-4771-2015; Li, Zhanqing/F-4424-2010;
OI Dickerson, Russell/0000-0003-0206-3083; Krotkov,
Nickolay/0000-0001-6170-6750; Li, Zhanqing/0000-0001-6737-382X;
Loughner, Christopher/0000-0002-3833-2014
FU NASA [NNX08AH71G]; DOE [DESC0007171]; UMD
FX We thank Qiang Zhang at Tsinghua University for the discussion on the
application of INTEX-B emission inventory. We thank R. J. Salawitch for
helpful comments. This work was supported by NASA (NNX08AH71G), DOE
(DESC0007171) and UMD.
NR 80
TC 32
Z9 32
U1 3
U2 38
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 FEB 9
PY 2012
VL 117
AR D00K37
DI 10.1029/2011JD016473
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 891QJ
UT WOS:000300231400005
ER
PT J
AU Kwok, R
Cunningham, GF
Manizade, SS
Krabill, WB
AF Kwok, R.
Cunningham, G. F.
Manizade, S. S.
Krabill, W. B.
TI Arctic sea ice freeboard from IceBridge acquisitions in 2009: Estimates
and comparisons with ICESat
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID LASER ALTIMETER MEASUREMENTS; AIRBORNE LASER; SHEET; RADAR
AB During the spring of 2009, the Airborne Topographic Mapper (ATM) system on the IceBridge mission acquired cross-basin surveys of surface elevations of Arctic sea ice. In this paper, the total freeboard derived from four similar to 2000 km transects are examined and compared with those from the 2009 ICESat campaign. Total freeboard, the sum of the snow and ice freeboards, is the elevation of the air-snow interface above the local sea surface. Prior to freeboard retrieval, signal dependent range biases are corrected. With data from a near co-incident outbound and return track on 21 April, we show that our estimates of the freeboard are repeatable to within similar to 4 cm but dependent locally on the density and quality of sea surface references. Overall difference between the ATM and ICESat freeboards for the four transects is 0.7 (8.5) cm (quantity in bracket is standard deviation), with a correlation of 0.78 between the data sets of one hundred seventy-eight 50 km averages. This establishes a level of confidence in the use of ATM freeboards to provide regional samplings that are consistent with ICESat. In early April, mean freeboards are 41 cm and 55 cm over first year and multiyear sea ice (MYI), respectively. Regionally, the lowest mean ice freeboard (28 cm) is seen on 5 April where the flight track sampled the large expanse of seasonal ice in the western Arctic. The highest mean freeboard (71 cm) is seen in the multiyear ice just west of Ellesmere Island from 21 April. The relatively large unmodeled variability of the residual sea surface resolved by ATM elevations is discussed.
C1 [Kwok, R.; Cunningham, G. F.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Manizade, S. S.] NASA, Wallops Flight Facil, URS Corp, Wallops Isl, VA 23337 USA.
[Krabill, W. B.] NASA, Goddard Space Flight Ctr, Lab Hydrospher Proc, Wallops Isl, VA 23337 USA.
RP Kwok, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ron.kwok@jpl.nasa.gov
RI Kwok, Ron/A-9762-2008
OI Kwok, Ron/0000-0003-4051-5896
FU National Aeronautics and Space Administration
FX We thank Ron Lindsay and another reviewer for providing valuable
comments that have contributed to improvements of our manuscript. The
QuikSCAT data were provided by the Physical Oceanography DAAC at the Jet
Propulsion Laboratory, Pasadena, California. The IceBridge data were
provided by the National Snow and Ice Data Center. RK and GFC carried
out this work at the Jet Propulsion Laboratory, California Institute of
Technology, under contract with the National Aeronautics and Space
Administration.
NR 11
TC 14
Z9 14
U1 1
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD FEB 9
PY 2012
VL 117
AR C02018
DI 10.1029/2011JC007654
PN 2012
PG 14
WC Oceanography
SC Oceanography
GA 893AY
UT WOS:000300328800005
ER
PT J
AU Parks, GK
Lee, E
McCarthy, M
Goldstein, M
Fu, SY
Cao, JB
Canu, P
Lin, N
Wilber, M
Dandouras, I
Reme, H
Fazakerley, A
AF Parks, G. K.
Lee, E.
McCarthy, M.
Goldstein, M.
Fu, S. Y.
Cao, J. B.
Canu, P.
Lin, N.
Wilber, M.
Dandouras, I.
Reme, H.
Fazakerley, A.
TI Entropy Generation across Earth's Collisionless Bow Shock
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID GYRATING IONS; ELECTRON; DISTRIBUTIONS
AB Earth's bow shock is a collisionless shock wave but entropy has never been directly measured across it. The plasma experiments on Cluster and Double Star measure 3D plasma distributions upstream and downstream of the bow shock allowing calculation of Boltzmann's entropy function H and his famous H theorem, dH/dt <= 0. The collisionless Boltzmann (Vlasov) equation predicts that the total entropy does not change if the distribution function across the shock becomes nonthermal, but it allows changes in the entropy density. Here, we present the first direct measurements of entropy density changes across Earth's bow shock and show that the results generally support the model of the Vlasov analysis. These observations are a starting point for a more sophisticated analysis that includes 3D computer modeling of collisionless shocks with input from observed particles, waves, and turbulences.
C1 [Parks, G. K.; Lin, N.; Wilber, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Lee, E.] Kyung Hee Univ, Sch Space Res, Yongin, South Korea.
[McCarthy, M.] Univ Washington, Seattle, WA 98195 USA.
[Goldstein, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fu, S. Y.] Peking Univ, Inst Space Phys & Appl Technol, Beijing 100871, Peoples R China.
[Cao, J. B.] Beihang Univ, Space Sci Inst, Sch Aeronaut, Beijing, Peoples R China.
[Canu, P.] Ecole Polytech, Plasma Phys Lab, F-75230 Paris, France.
[Dandouras, I.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Reme, H.] IRAP, CNRS, Toulouse 4, France.
[Fazakerley, A.] UCL, MSSL, London, England.
RP Parks, GK (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM parks@ssl.berkeley.edu
RI Lee, Ensang/E-2356-2013; Fu, Suiyan/E-9178-2013;
OI Dandouras, Iannis/0000-0002-7121-1118
FU NASA [NNX07AP96G]; WCU through NRF; MEST of Korea [R31-10016]
FX The research at UC Berkeley is funded by NASA Grant No. NNX07AP96G and
at Kyung Hee University by the WCU program through NRF funded by MEST of
Korea (Grant No. R31-10016).
NR 15
TC 4
Z9 4
U1 0
U2 5
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 FEB 9
PY 2012
VL 108
IS 6
AR 061102
DI 10.1103/PhysRevLett.108.061102
PG 4
WC Physics, Multidisciplinary
SC Physics
GA 889VA
UT WOS:000300101500003
PM 22401049
ER
PT J
AU Fressin, F
Torres, G
Rowe, JF
Charbonneau, D
Rogers, LA
Ballard, S
Batalha, NM
Borucki, WJ
Bryson, ST
Buchhave, LA
Ciardi, DR
Desert, JM
Dressing, CD
Fabrycky, DC
Ford, EB
Gautier, TN
Henze, CE
Holman, MJ
Howard, A
Howell, SB
Jenkins, JM
Koch, DG
Latham, DW
Lissauer, JJ
Marcy, GW
Quinn, SN
Ragozzine, D
Sasselov, DD
Seager, S
Barclay, T
Mullally, F
Seader, SE
Still, M
Twicken, JD
Thompson, SE
Uddin, K
AF Fressin, Francois
Torres, Guillermo
Rowe, Jason F.
Charbonneau, David
Rogers, Leslie A.
Ballard, Sarah
Batalha, Natalie M.
Borucki, William J.
Bryson, Stephen T.
Buchhave, Lars A.
Ciardi, David R.
Desert, Jean-Michel
Dressing, Courtney D.
Fabrycky, Daniel C.
Ford, Eric B.
Gautier, Thomas N., III
Henze, Christopher E.
Holman, Matthew J.
Howard, Andrew
Howell, Steve B.
Jenkins, Jon M.
Koch, David G.
Latham, David W.
Lissauer, Jack J.
Marcy, Geoffrey W.
Quinn, Samuel N.
Ragozzine, Darin
Sasselov, Dimitar D.
Seager, Sara
Barclay, Thomas
Mullally, Fergal
Seader, Shawn E.
Still, Martin
Twicken, Joseph D.
Thompson, Susan E.
Uddin, Kamal
TI Two Earth-sized planets orbiting Kepler-20
SO NATURE
LA English
DT Article
ID TRANSITING PLANET; BLEND SCENARIOS; MULTIPLE SYSTEM; GIANT IMPACTS;
CANDIDATES; VALIDATION; EXOPLANETS; COMPANION
AB Since the discovery of the first extrasolar giant planets around Sun-like stars(1,2), evolving observational capabilities have brought us closer to the detection of true Earth analogues. The size of an exoplanet can be determined when it periodically passes in front of (transits) its parent star, causing a decrease in starlight proportional to its radius. The smallest exoplanet hitherto discovered(3) has a radius 1.42 times that of the Earth's radius (R-circle plus), and hence has 2.9 times its volume. Here we report the discovery of two planets, one Earth-sized (1.03 R-circle plus) and the other smaller than the Earth (0.87 R-circle plus), orbiting the star Kepler-20, which is already known to host three other, larger, transiting planets(4). The gravitational pull of the new planets on the parent star is too small to measure with current instrumentation. We apply a statistical method to show that the likelihood of the planetary interpretation of the transit signals is more than three orders of magnitude larger than that of the alternative hypothesis that the signals result from an eclipsing binary star. Theoretical considerations imply that these planets are rocky, with a composition of iron and silicate. The outer planet could have developed a thick water vapour atmosphere.
C1 [Fressin, Francois; Torres, Guillermo; Charbonneau, David; Ballard, Sarah; Desert, Jean-Michel; Dressing, Courtney D.; Holman, Matthew J.; Latham, David W.; Quinn, Samuel N.; Ragozzine, Darin; Sasselov, Dimitar D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Rowe, Jason F.; Borucki, William J.; Bryson, Stephen T.; Henze, Christopher E.; Howell, Steve B.; Koch, David G.; Lissauer, Jack J.; Barclay, Thomas; Still, Martin] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rogers, Leslie A.; Seager, Sara] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
[Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
[Ciardi, David R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Fabrycky, Daniel C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32111 USA.
[Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Howard, Andrew; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Jenkins, Jon M.; Mullally, Fergal; Seader, Shawn E.; Twicken, Joseph D.; Thompson, Susan E.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Uddin, Kamal] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
RP Fressin, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ffressin@cfa.harvard.edu
RI Ragozzine, Darin/C-4926-2013;
OI Buchhave, Lars A./0000-0003-1605-5666; Ciardi,
David/0000-0002-5741-3047; Charbonneau, David/0000-0002-9003-484X;
Barclay, Thomas/0000-0001-7139-2724; Fabrycky,
Daniel/0000-0003-3750-0183
FU NASA's Science Mission Directorate
FX Kepler was competitively selected as the tenth Discovery mission.
Funding for this mission is provided by NASA's Science Mission
Directorate.
NR 28
TC 93
Z9 93
U1 7
U2 53
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD FEB 9
PY 2012
VL 482
IS 7384
BP 195
EP 198
DI 10.1038/nature10780
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 888HI
UT WOS:000299994100033
PM 22186831
ER
PT J
AU Zwart, SR
Jessup, JM
Ji, JP
Smith, SM
AF Zwart, Sara R.
Jessup, J. Milburn
Ji, Jiuping
Smith, Scott M.
TI Saturation Diving Alters Folate Status and Biomarkers of DNA Damage and
Repair
SO PLOS ONE
LA English
DT Article
ID RED-CELL MASS; NUTRITIONAL-STATUS; BODY IRON; BED REST; CANCER; DIVE;
HUMANS; NEOCYTOLYSIS; GAMMA-H2AX; DISEASE
AB Exposure to oxygen-rich environments can lead to oxidative damage, increased body iron stores, and changes in status of some vitamins, including folate. Assessing the type of oxidative damage in these environments and determining its relationships with changes in folate status are important for defining nutrient requirements and designing countermeasures to mitigate these effects. Responses of humans to oxidative stressors were examined in participants undergoing a saturation dive in an environment with increased partial pressure of oxygen, a NASA Extreme Environment Mission Operations mission. Six participants completed a 13-d saturation dive in a habitat 19 m below the ocean surface near Key Largo, FL. Fasting blood samples were collected before, twice during, and twice after the dive and analyzed for biochemical markers of iron status, oxidative damage, and vitamin status. Body iron stores and ferritin increased during the dive (P < 0.001), with a concomitant decrease in RBC folate (P < 0.001) and superoxide dismutase activity (P < 0.001). Folate status was correlated with serum ferritin (Pearson r = -0.34, P < 0.05). Peripheral blood mononuclear cell poly(ADP-ribose) increased during the dive and the increase was significant by the end of the dive (P < 0.001); gamma-H2AX did not change during the mission. Together, the data provide evidence that when body iron stores were elevated in a hyperoxic environment, a DNA damage repair response occurred in peripheral blood mononuclear cells, but double-stranded DNA damage did not. In addition, folate status decreases quickly in this environment, and this study provides evidence that folate requirements may be greater when body iron stores and DNA damage repair responses are elevated.
C1 [Zwart, Sara R.] Univ Space Res Assoc, Houston, TX USA.
[Jessup, J. Milburn; Ji, Jiuping] Natl Canc Inst, Bethesda, MD USA.
[Smith, Scott M.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Zwart, SR (reprint author), Univ Space Res Assoc, Houston, TX USA.
EM sara.zwart-1@nasa.gov
FU NASA
FX This study was supported by the NASA Human Research Program Human Health
and Countermeasures Element. The funders had no role in study design,
data collection and analysis, decision to publish, or preparation of the
manuscript.
NR 31
TC 8
Z9 9
U1 0
U2 6
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 FEB 7
PY 2012
VL 7
IS 2
AR e31058
DI 10.1371/journal.pone.0031058
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 917MF
UT WOS:000302180600027
PM 22347427
ER
PT J
AU Gorham, PW
Allison, P
Baughman, BM
Beatty, JJ
Belov, K
Besson, DZ
Bevan, S
Binns, WR
Chen, C
Chen, P
Clem, JM
Connolly, A
Detrixhe, M
De Marco, D
Dowkontt, PF
DuVernois, M
Grashorn, EW
Hill, B
Hoover, S
Huang, M
Israel, MH
Javaid, A
Liewer, KM
Matsuno, S
Mercurio, BC
Miki, C
Mottram, M
Nam, J
Nichol, RJ
Palladino, K
Romero-Wolf, A
Ruckman, L
Saltzberg, D
Seckel, D
Shang, RY
Varner, GS
Vieregg, AG
Wang, Y
AF Gorham, P. W.
Allison, P.
Baughman, B. M.
Beatty, J. J.
Belov, K.
Besson, D. Z.
Bevan, S.
Binns, W. R.
Chen, C.
Chen, P.
Clem, J. M.
Connolly, A.
Detrixhe, M.
De Marco, D.
Dowkontt, P. F.
DuVernois, M.
Grashorn, E. W.
Hill, B.
Hoover, S.
Huang, M.
Israel, M. H.
Javaid, A.
Liewer, K. M.
Matsuno, S.
Mercurio, B. C.
Miki, C.
Mottram, M.
Nam, J.
Nichol, R. J.
Palladino, K.
Romero-Wolf, A.
Ruckman, L.
Saltzberg, D.
Seckel, D.
Shang, R. Y.
Varner, G. S.
Vieregg, A. G.
Wang, Y.
TI Observational constraints on the ultrahigh energy cosmic neutrino flux
from the second flight of the ANITA experiment (vol 82, 022004, 2010)
SO PHYSICAL REVIEW D
LA English
DT Correction
C1 [Gorham, P. W.; Allison, P.; DuVernois, M.; Hill, B.; Matsuno, S.; Miki, C.; Romero-Wolf, A.; Ruckman, L.; Varner, G. S.] Univ Hawaii Manoa, Dept Phys & Astron, Honolulu, HI 96822 USA.
[Baughman, B. M.; Beatty, J. J.; Grashorn, E. W.; Mercurio, B. C.; Palladino, K.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Belov, K.; Hoover, S.; Saltzberg, D.; Vieregg, A. G.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Besson, D. Z.; Detrixhe, M.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Bevan, S.; Connolly, A.; Mottram, M.; Nichol, R. J.] UCL, Dept Phys & Astron, London, England.
[Binns, W. R.; Dowkontt, P. F.; Israel, M. H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Chen, C.; Chen, P.; Huang, M.; Nam, J.; Shang, R. Y.; Wang, Y.] Natl Taiwan Univ, Dept Phys, Taipei 10617, Taiwan.
[Clem, J. M.; De Marco, D.; Javaid, A.; Seckel, D.] Univ Delaware, Dept Phys, Newark, DE 19716 USA.
[Liewer, K. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Gorham, PW (reprint author), Univ Hawaii Manoa, Dept Phys & Astron, Honolulu, HI 96822 USA.
RI Vieregg, Abigail/D-2287-2012; Belov, Konstantin/D-2520-2013; Beatty,
James/D-9310-2011
OI Beatty, James/0000-0003-0481-4952
NR 4
TC 32
Z9 32
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 FEB 6
PY 2012
VL 85
IS 4
AR 049901
DI 10.1103/PhysRevD.85.049901
PG 2
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 887QM
UT WOS:000299943600013
ER
PT J
AU Osterstrom, FF
Nielsen, OJ
Andersen, MPS
Wallington, TJ
AF Osterstrom, Freja From
Nielsen, Ole John
Andersen, Mads P. Sulbaek
Wallington, Timothy J.
TI Atmospheric chemistry of CF3CH2OCH3: Reaction with chlorine atoms and OH
radicals, kinetics, degradation mechanism and global warming potential
SO CHEMICAL PHYSICS LETTERS
LA English
DT Article
ID STRATOSPHERIC OZONE; HYDROFLUOROCARBONS; AIR; HYDROFLUOROETHERS;
ACETYLENE; SERIES; ETHERS; 295-K
AB FTIR smog chamber techniques were used to measure k(Cl + CF3CH2OCH3) = (2.28 +/- 0.44) x 10(-11) and k(OH + CF3CH2OCH3) = (4.9 +/- 1.3) x 10(-13) cm(3) molecule(-1) s(-1) in 700 Torr total pressure of air at 296 +/- 2 K. The atmospheric lifetime of CF3CH2OCH3 is estimated at 25 days. Reaction of Cl atoms with CF3CH2OCH3 proceeds 79 +/- 4% at the -CH3 group and 22 +/- 2% at the -CH2- group. Reaction with OH radicals proceeds 55 +/- 5% at the -CH3 group yielding CF3CH2OCHO and 45 +/- 5% at the -CH2- group yielding COF2 and CH3OCHO as primary oxidation products. The infrared spectrum of CF3CH(O)OCH3 was measured and a global warming potential GWP(100) = 8 was estimated. The atmospheric chemistry and environmental impact of CF3CH2OCH3 is discussed in context of the use of hydrofluoroethers as CFC substitutes. (C) 2011 Elsevier B. V. All rights reserved.
C1 [Osterstrom, Freja From; Nielsen, Ole John] Univ Copenhagen, Dept Chem, Copenhagen Ctr Atmospher Res, DK-2100 Copenhagen, Denmark.
[Andersen, Mads P. Sulbaek] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Wallington, Timothy J.] Ford Motor Co, Syst Analyt & Environm Sci Dept, Dearborn, MI 48121 USA.
RP Osterstrom, FF (reprint author), Univ Copenhagen, Dept Chem, Copenhagen Ctr Atmospher Res, Univ Pk 5, DK-2100 Copenhagen, Denmark.
EM frejafrom@adslhome.dk
RI Sulbaek Andersen, Mads/C-4708-2008; Nielsen, Ole/B-9988-2011;
Osterstrom, Freja From/E-8646-2015
OI Sulbaek Andersen, Mads/0000-0002-7976-5852; Nielsen,
Ole/0000-0002-0088-3937; Osterstrom, Freja From/0000-0003-4125-3365
FU Danish Natural Science Research Council; Villum Kann Rasmussen
Foundation; EUROCHAMP2; National Aeronautics and Space Administration
FX The authors thank the Danish Natural Science Research Council, the
Villum Kann Rasmussen Foundation and EUROCHAMP2, for financial support.
We thank S. P. Sander (JPL) for helpful discussions. This work was
performed partly at the Jet Propulsion Laboratory, California Institute
of Technology, under a contract with the National Aeronautics and Space
Administration. M. P. S. A. is supported by an appointment to the NASA
Postdoctoral Program, administered by Oak Ridge Associated Universities
through a contract with NASA.
NR 20
TC 7
Z9 7
U1 0
U2 32
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0009-2614
J9 CHEM PHYS LETT
JI Chem. Phys. Lett.
PD FEB 6
PY 2012
VL 524
BP 32
EP 37
DI 10.1016/j.cplett.2011.12.047
PG 6
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 879GL
UT WOS:000299317600006
ER
PT J
AU Doeringer, D
Eldering, A
Boone, CD
Abad, GG
Bernath, PF
AF Doeringer, D.
Eldering, A.
Boone, C. D.
Abad, G. Gonzalez
Bernath, P. F.
TI Observation of sulfate aerosols and SO2 from the Sarychev volcanic
eruption using data from the Atmospheric Chemistry Experiment (ACE)
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID INFRARED TRANSMISSION MEASUREMENTS; VERTICAL PROFILES; PINATUBO AEROSOL;
OPTICAL-CONSTANTS; EFFECTIVE RADIUS; SURFACE-AREA; EL-CHICHON; SAGE-II;
INSTRUMENT; VOLUME
AB Infrared spectra measured by the Atmospheric Chemistry Experiment Fourier Transform Spectrometer (ACE-FTS) on the SCISAT satellite were used to analyze the Sarychev volcanic aerosol after the eruption in June 2009. Evidence of the Sarychev eruptions was first detected in July 2009 from enhanced SO2 concentrations and atmospheric extinction. By February 2010, the atmosphere had returned to pre-Sarychev conditions. In July 2009, the volcanic plume was found between 8.5 km and 17.5 km in altitude at mid-and high latitudes (55 degrees N-70 degrees N). The first SO2 and sulfate aerosol retrievals carried out using the infrared solar occultation spectra recorded with the ACE-FTS are presented here. The size distribution parameters, the aerosol volume slant column and the composition of the sulfate aerosol were obtained by using a least squares algorithm. The maximum volume slant column of the aerosols was found to be 850 mu m(3) cm(-3) km, which results in an approximate aerosol loading of 3 mu m(3) cm(-3). One month after the eruption, the composition of the aerosols providing the best-fit is a 75% sulfuric acid-water solution with an effective radius (R-eff) of 0.1-0.3 mu m.
C1 [Doeringer, D.] Univ York, Dept Phys, York YO10 5DD, N Yorkshire, England.
[Boone, C. D.] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada.
[Eldering, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Abad, G. Gonzalez; Bernath, P. F.] Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England.
[Eldering, A.] Univ Calif Los Angeles, Dept Atmospher Sci, Los Angeles, CA 90024 USA.
RP Doeringer, D (reprint author), Univ York, Dept Phys, York YO10 5DD, N Yorkshire, England.
EM dd557@york.ac.uk
RI Bernath, Peter/B-6567-2012;
OI Bernath, Peter/0000-0002-1255-396X; Gonzalez Abad,
Gonzalo/0000-0002-8090-6480
FU Canadian Space Agency; UK Natural Environment Research Council (NERC)
through the National Centre for Earth Observation (NCEO); NASA
FX The ACE mission is funded primarily by the Canadian Space Agency. Some
funding was provided by the UK Natural Environment Research Council
(NERC) through the National Centre for Earth Observation (NCEO). Work at
the Jet Propulsion Laboratory, California Institute of Technology was
carried out under contract with NASA.
NR 36
TC 15
Z9 15
U1 0
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD FEB 4
PY 2012
VL 117
AR D03203
DI 10.1029/2011JD016556
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 887WB
UT WOS:000299961100001
ER
PT J
AU Hurley, DM
Gladstone, GR
Stern, SA
Retherford, KD
Feldman, PD
Pryor, W
Egan, AF
Greathouse, TK
Kaufmann, DE
Steffl, AJ
Parker, JW
Miles, PF
Horvath, D
Davis, MW
Versteeg, MH
Slater, DC
Hendrix, AR
Hibbitts, CA
Ernst, CM
Vervack, RJ
Grieves, GA
AF Hurley, Dana M.
Gladstone, G. Randall
Stern, S. Alan
Retherford, Kurt D.
Feldman, Paul D.
Pryor, Wayne
Egan, Anthony F.
Greathouse, Thomas K.
Kaufmann, David E.
Steffl, Andrew J.
Parker, Joel William
Miles, Paul F.
Horvath, David
Davis, Michael W.
Versteeg, Maarten H.
Slater, David C.
Hendrix, Amanda R.
Hibbitts, Charles A.
Ernst, Carolyn M.
Vervack, Ronald J., Jr.
Grieves, Gregory A.
TI Modeling of the vapor release from the LCROSS impact: 2. Observations
from LAMP
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID LUNAR RADIOMETER OBSERVATIONS; WATER; ICE; VOLATILES; DEPOSITS;
SURFACES; MISSION; MERCURY; PLUME; MOON
AB Using a Monte Carlo model, we analyze the evolution of the vapor plume emanating from the Lunar Crater Observation and Sensing Satellite (LCROSS) impact into Cabeus as seen by the Lyman Alpha Mapping Project (LAMP), a far-ultraviolet (FUV) imaging spectrograph onboard the Lunar Reconnaissance Orbiter. The best fit to the data utilizes a bulk velocity between 3.0 and 4.0 km/s. The fits to the light curve comprised of Hg, Ca, and Mg are not strongly dependent on the temperature. In contrast, the best fit to the light curve from H-2 and CO corresponds to a 500 K thermal velocity distribution. The LAMP field of view primarily encounters particles released at low angles to the horizontal and misses fast moving particles released at more vertical angles. The isotropic model suggests that 117 +/- 16 kg H-2, 41 +/- 3 kg CO, 16 +/- 1 kg Ca, 12.4 +/- 0.8 kg Hg, and 3.8 +/- 0.3 kg Mg are released by the LCROSS impact. Additional errors could arise from an anisotropic plume, which cannot be distinguished with LAMP data. Mg and Ca are likely incompletely volatilized owing to their high vapor temperatures. The highly volatile components (H-2 and CO) might derive from a greater mass of material. To agree with predicted abundances by weight of 0.047%, 0.023%, 11%, 0.28% and 3.4% for H-2, CO, Ca, Hg, and Mg, respectively, the species would be released from 250,000 kg, 180,000 kg, 140 kg, 4400 kg, and 110 kg of regolith, respectively. This is consistent with the relative volatility of these species.
C1 [Hurley, Dana M.; Hibbitts, Charles A.; Ernst, Carolyn M.; Vervack, Ronald J., Jr.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Laurel, MD 20723 USA.
[Gladstone, G. Randall; Retherford, Kurt D.; Greathouse, Thomas K.; Miles, Paul F.; Horvath, David; Davis, Michael W.; Versteeg, Maarten H.; Slater, David C.] SW Res Inst, Space Sci & Engn Div, San Antonio, TX 78238 USA.
[Stern, S. Alan; Egan, Anthony F.; Kaufmann, David E.; Steffl, Andrew J.; Parker, Joel William] SW Res Inst, Space Sci & Engn Div, Boulder, CO 80302 USA.
[Feldman, Paul D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Pryor, Wayne] Cent Arizona Coll, Dept Sci, Coolidge, AZ 85128 USA.
[Hendrix, Amanda R.] CALTECH, Jet Prop Lab, Planetary Sci Sect, Pasadena, CA 91109 USA.
[Grieves, Gregory A.] Georgia Inst Technol, Sch Chem, Atlanta, GA 30332 USA.
RP Hurley, DM (reprint author), Johns Hopkins Univ, Appl Phys Lab, Dept Space, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA.
EM dana.hurley@jhuapl.edu
RI Ernst, Carolyn/I-4902-2012; Hurley, Dana/F-4488-2015; Vervack,
Ronald/C-2702-2016; Hibbitts, Charles/B-7787-2016;
OI Hurley, Dana/0000-0003-1052-1494; Vervack, Ronald/0000-0002-8227-9564;
Hibbitts, Charles/0000-0001-9089-4391; Retherford,
Kurt/0000-0001-9470-150X; Greathouse, Thomas/0000-0001-6613-5731
FU NASA Lunar Reconnaissance Orbiter; NASA Lunar Science Institute
[NNA09DB31A]
FX This work was supported by NASA Lunar Reconnaissance Orbiter and by the
NASA Lunar Science Institute through grant NNA09DB31A. We thank the
referees and editors for helpful comments.
NR 36
TC 9
Z9 9
U1 1
U2 5
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 FEB 4
PY 2012
VL 117
AR E00H07
DI 10.1029/2011JE003841
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 887UQ
UT WOS:000299956700001
ER
PT J
AU Xia, YL
Mitchell, K
Ek, M
Sheffield, J
Cosgrove, B
Wood, E
Luo, LF
Alonge, C
Wei, HL
Meng, J
Livneh, B
Lettenmaier, D
Koren, V
Duan, QY
Mo, K
Fan, Y
Mocko, D
AF Xia, Youlong
Mitchell, Kenneth
Ek, Michael
Sheffield, Justin
Cosgrove, Brian
Wood, Eric
Luo, Lifeng
Alonge, Charles
Wei, Helin
Meng, Jesse
Livneh, Ben
Lettenmaier, Dennis
Koren, Victor
Duan, Qingyun
Mo, Kingtse
Fan, Yun
Mocko, David
TI Continental-scale water and energy flux analysis and validation for the
North American Land Data Assimilation System project phase 2 (NLDAS-2):
1. Intercomparison and application of model products
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SURFACE PARAMETERIZATION SCHEMES; LATITUDE HYDROLOGICAL PROCESSES;
CONTERMINOUS UNITED-STATES; SOUTHERN GREAT-PLAINS; MESOSCALE ETA-MODEL;
TORNE-KALIX BASIN; RIVER-BASIN; PILPS PHASE-2(E); PRECIPITATION;
SIMULATION
AB Results are presented from the second phase of the multiinstitution North American Land Data Assimilation System (NLDAS-2) research partnership. In NLDAS, the Noah, Variable Infiltration Capacity, Sacramento Soil Moisture Accounting, and Mosaic land surface models (LSMs) are executed over the conterminous U.S. (CONUS) in realtime and retrospective modes. These runs support the drought analysis, monitoring and forecasting activities of the National Integrated Drought Information System, as well as efforts to monitor large-scale floods. NLDAS-2 builds upon the framework of the first phase of NLDAS (NLDAS-1) by increasing the accuracy and consistency of the surface forcing data, upgrading the land surface model code and parameters, and extending the study from a 3-year (1997-1999) to a 30-year (1979-2008) time window. As the first of two parts, this paper details the configuration of NLDAS-2, describes the upgrades to the forcing, parameters, and code of the four LSMs, and explores overall model-to-model comparisons of land surface water and energy flux and state variables over the CONUS. Focusing on model output rather than on observations, this study seeks to highlight the similarities and differences between models, and to assess changes in output from that seen in NLDAS-1. The second part of the two-part article focuses on the validation of model-simulated streamflow and evaporation against observations. The results depict a higher level of agreement among the four models over much of the CONUS than was found in the first phase of NLDAS. This is due, in part, to recent improvements in the parameters, code, and forcing of the NLDAS-2 LSMs that were initiated following NLDAS-1. However, large inter-model differences still exist in the northeast, Lake Superior, and western mountainous regions of the CONUS, which are associated with cold season processes. In addition, variations in the representation of sub-surface hydrology in the four LSMs lead to large differences in modeled evaporation and subsurface runoff. These issues are important targets for future research by the land surface modeling community. Finally, improvement from NLDAS-1 to NLDAS-2 is summarized by comparing the streamflow measured from U. S. Geological Survey stream gauges with that simulated by four NLDAS models over 961 small basins.
C1 [Xia, Youlong; Mitchell, Kenneth; Ek, Michael; Wei, Helin; Meng, Jesse] NOAA, Environm Modeling Ctr, Natl Ctr Environm & Predict, Camp Springs, MD 20746 USA.
[Xia, Youlong; Wei, Helin; Meng, Jesse] NCEP EMC, IMSG, Camp Springs, MD USA.
[Sheffield, Justin; Wood, Eric] Princeton Univ, Dept Environm & Civil Engn, Princeton, NJ 08544 USA.
[Cosgrove, Brian; Koren, Victor] NOAA, Off Hydrol Dev, Natl Weather Serv, Silver Spring, MD 20910 USA.
[Luo, Lifeng] Michigan State Univ, Dept Geog, E Lansing, MI 48824 USA.
[Alonge, Charles] AWS Truewind LLC, Albany, NY 12205 USA.
[Livneh, Ben; Lettenmaier, Dennis] Univ Washington, Dept Environm & Civil Engn, Seattle, WA 98195 USA.
[Duan, Qingyun] Beijing Normal Univ, Coll Global Change & Earth Syst Sci, Beijing 100875, Peoples R China.
[Mo, Kingtse] NOAA, Climate Predict Ctr, Natl Ctr Environm & Predict, Camp Springs, MD 20746 USA.
[Fan, Yun] NOAA, Natl Weather Serv, Off Sci & Technol, Silver Spring, MD 20910 USA.
[Mocko, David] NASA, Goddard Space Flight Ctr, Hydrol Sci Lab, Greenbelt, MD 20715 USA.
[Mocko, David] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20715 USA.
RP Xia, YL (reprint author), NOAA, Environm Modeling Ctr, Natl Ctr Environm & Predict, 5200 Auth Rd, Camp Springs, MD 20746 USA.
EM Youlong.Xia@noaa.gov
RI lettenmaier, dennis/F-8780-2011; Duan, Qingyun/C-7652-2011; Livneh,
Ben/I-2939-2015
OI lettenmaier, dennis/0000-0003-3317-1327; Duan,
Qingyun/0000-0001-9955-1512;
FU NOAA/CPO/CPPA
FX This work was supported by the NOAA/CPO/CPPA core project.
NR 59
TC 196
Z9 197
U1 2
U2 52
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 FEB 3
PY 2012
VL 117
AR D03109
DI 10.1029/2011JD016048
PG 27
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 887VW
UT WOS:000299960500001
ER
PT J
AU Czaja, AD
Johnson, CM
Yamaguchi, KE
Beard, BL
AF Czaja, Andrew D.
Johnson, Clark M.
Yamaguchi, Kosei E.
Beard, Brian L.
TI Comment on "Abiotic Pyrite Formation Produces a Large Fe Isotope
Fractionation"
SO SCIENCE
LA English
DT Editorial Material
ID BLACK-SEA; IRON; SEDIMENTS; EARTH
C1 [Czaja, Andrew D.; Johnson, Clark M.; Beard, Brian L.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.
[Czaja, Andrew D.; Johnson, Clark M.; Yamaguchi, Kosei E.; Beard, Brian L.] NASA, Astrobiol Inst, Washington, DC USA.
[Yamaguchi, Kosei E.] Toho Univ, Dept Chem, Funabashi, Chiba 2748510, Japan.
RP Czaja, AD (reprint author), Univ Wisconsin, Dept Geosci, 1215 W Dayton St, Madison, WI 53706 USA.
EM aczaja@geology.wisc.edu
NR 15
TC 6
Z9 7
U1 1
U2 20
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 FEB 3
PY 2012
VL 335
IS 6068
DI 10.1126/science.1211804
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 885HI
UT WOS:000299769200024
PM 22301304
ER
PT J
AU Fassett, CI
Head, JW
Kadish, SJ
Mazarico, E
Neumann, GA
Smith, DE
Zuber, MT
AF Fassett, C. I.
Head, J. W.
Kadish, S. J.
Mazarico, E.
Neumann, G. A.
Smith, D. E.
Zuber, M. T.
TI Lunar impact basins: Stratigraphy, sequence and ages from superposed
impact crater populations measured from Lunar Orbiter Laser Altimeter
(LOLA) data
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID LATE HEAVY BOMBARDMENT; INNER SOLAR-SYSTEM; CATACLYSM IMPACTORS; ORIGIN;
CONSTRAINTS; MOON; SATURATION; CHRONOLOGY; MISSION; EARTH
AB Impact basin formation is a fundamental process in the evolution of the Moon and records the history of impactors in the early solar system. In order to assess the stratigraphy, sequence, and ages of impact basins and the impactor population as a function of time, we have used topography from the Lunar Orbiter Laser Altimeter (LOLA) on the Lunar Reconnaissance Orbiter (LRO) to measure the superposed impact crater size-frequency distributions for 30 lunar basins (D >= 300 km). These data generally support the widely used Wilhelms sequence of lunar basins, although we find significantly higher densities of superposed craters on many lunar basins than derived by Wilhelms (50% higher densities). Our data also provide new insight into the timing of the transition between distinct crater populations characteristic of ancient and young lunar terrains. The transition from a lunar impact flux dominated by Population 1 to Population 2 occurred before the mid-Nectarian. This is before the end of the period of rapid cratering, and potentially before the end of the hypothesized Late Heavy Bombardment. LOLA-derived crater densities also suggest that many Pre-Nectarian basins, such as South Pole-Aitken, have been cratered to saturation equilibrium. Finally, both crater counts and stratigraphic observations based on LOLA data are applicable to specific basin stratigraphic problems of interest; for example, using these data, we suggest that Serenitatis is older than Nectaris, and Humboldtianum is younger than Crisium. Sample return missions to specific basins can anchor these measurements to a Pre-Imbrian absolute chronology.
C1 [Fassett, C. I.; Head, J. W.; Kadish, S. J.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Mazarico, E.; Neumann, G. A.; Smith, D. E.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Smith, D. E.; Zuber, M. T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Fassett, C. I.] Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA.
RP Fassett, CI (reprint author), Mt Holyoke Coll, Dept Astron, S Hadley, MA 01075 USA.
EM cfassett@mtholyoke.edu
RI Neumann, Gregory/I-5591-2013; Mazarico, Erwan/N-6034-2014;
OI Neumann, Gregory/0000-0003-0644-9944; Mazarico,
Erwan/0000-0003-3456-427X; Fassett, Caleb/0000-0001-9155-3804
FU Lunar Reconnaissance Orbiter Project; Lunar Orbiter Laser Altimeter team
[NNX09AM54G]
FX We would like to thank Clark Chapman, Matija Cuk and Stephanie Werner
for detailed reviews that helped improve the manuscript. Thanks are
extended to the Lunar Reconnaissance Orbiter Project and the Lunar
Orbiter Laser Altimeter team for funding (NNX09AM54G) to JWH.
NR 60
TC 33
Z9 34
U1 0
U2 15
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 FEB 2
PY 2012
VL 117
AR E00H06
DI 10.1029/2011JE003951
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 887UM
UT WOS:000299956200001
ER
PT J
AU Johnson, LF
Trout, TJ
AF Johnson, Lee F.
Trout, Thomas J.
TI Satellite NDVI Assisted Monitoring of Vegetable Crop Evapotranspiration
in California's San Joaquin Valley
SO REMOTE SENSING
LA English
DT Article
DE crop coefficient; water use; NDVI; Landsat; fractional cover
ID WATER-USE; VEGETATION INDEX; SEMIARID REGION; SHADED AREA; COEFFICIENTS;
REFLECTANCE; CANOPY; WHEAT; CORN; ALGORITHM
AB Reflective bands of Landsat-5 Thematic Mapper satellite imagery were used to facilitate the estimation of basal crop evapotranspiration (ETcb), or potential crop water use, in San Joaquin Valley fields during 2008. A ground-based digital camera measured green fractional cover (Fc) of 49 commercial fields planted to 18 different crop types (row crops, grains, orchard, vineyard) of varying maturity over 11 Landsat overpass dates. Landsat L1T terrain-corrected images were transformed to surface reflectance and converted to normalized difference vegetation index (NDVI). A strong linear relationship between NDVI and Fc was observed (r(2) = 0.96, RMSE = 0.062). The resulting regression equation was used to estimate Fc for crop cycles of broccoli, bellpepper, head lettuce, and garlic on nominal 7-9 day intervals for several study fields. Prior relationships developed by weighing lysimeter were used to transform Fc to fraction of reference evapotranspiration, also known as basal crop coefficient (Kcb). Measurements of grass reference evapotranspiration from the California Irrigation Management Information System were then used to calculate ETcb for each overpass date. Temporal profiles of Fc, Kcb, and ETcb were thus developed for the study fields, along with estimates of seasonal water use. Daily ETcb retrieval uncertainty resulting from error in satellite-based Fc estimation was <0.5 mm/d, with seasonal uncertainty of 6-10%. Results were compared with FAO-56 irrigation guidelines and prior lysimeter observations for reference.
C1 [Johnson, Lee F.] Calif State Univ, Div Sci & Environm Policy, Seaside, CA 93955 USA.
[Johnson, Lee F.] NASA, Div Earth Sci, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Trout, Thomas J.] USDA ARS, Water Management Res Unit, Ft Collins, CO 80526 USA.
RP Johnson, LF (reprint author), Calif State Univ, Div Sci & Environm Policy, Seaside, CA 93955 USA.
EM Lee.F.Johnson@nasa.gov; Thomas.Trout@ars.usda.gov
OI Trout, Thomas/0000-0003-1896-9170
FU California Dept. Water Resources; NASA's Applied Sciences Program
FX Field support was provided by Jim Gartung (USDA-ARS). LEDAPS atmospheric
correction processing was facilitated by the NASA Ames Ecological
Forecasting Lab. We are grateful for cooperation of commercial growers
at Tanimura & Antle, Red Rock Ranch, Britz, Terranova, and Harris Farms.
The project was funded by the California Dept. Water Resources. LJ
received additional support through NASA's Applied Sciences Program.
NR 35
TC 30
Z9 30
U1 3
U2 26
PU MDPI AG
PI BASEL
PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND
SN 2072-4292
J9 REMOTE SENS-BASEL
JI Remote Sens.
PD FEB
PY 2012
VL 4
IS 2
BP 439
EP 455
DI 10.3390/rs4020439
PG 17
WC Remote Sensing
SC Remote Sensing
GA 978PL
UT WOS:000306756400006
ER
PT J
AU Coustenis, A
Atreya, S
Castillo, J
Coll, P
Mueller-Wodarg, I
Spilker, L
AF Coustenis, A.
Atreya, S.
Castillo, J.
Coll, P.
Mueller-Wodarg, I.
Spilker, L.
TI Surfaces, atmospheres and magnetospheres of the outer planets and their
satellites and ring systems: Part VII Preface
SO PLANETARY AND SPACE SCIENCE
LA English
DT Editorial Material
C1 [Coustenis, A.] LESIA, Paris Meudon Observ, F-92195 Meudon, France.
[Atreya, S.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Castillo, J.] CALTECH, JPL, Pasadena, CA 91125 USA.
[Coll, P.] Univ Paris 07, LISA, Univ Paris Est Creteil, Creteil, France.
[Mueller-Wodarg, I.] Univ London Imperial Coll Sci Technol & Med, London, England.
[Spilker, L.] Jet Prop Lab, Pasadena, CA USA.
[Coll, P.] Hop Henri Mondor, CNRS, F-94010 Creteil, France.
RP Coustenis, A (reprint author), LESIA, Paris Meudon Observ, F-92195 Meudon, France.
RI Mueller-Wodarg, Ingo/M-9945-2014
OI Mueller-Wodarg, Ingo/0000-0001-6308-7826
NR 0
TC 1
Z9 1
U1 0
U2 0
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 FEB
PY 2012
VL 61
IS 1
SI SI
BP 1
EP 2
DI 10.1016/j.pss.2011.12.014
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 971IY
UT WOS:000306198800001
ER
PT J
AU Lipatov, AS
Sittler, EC
Hartle, RE
Cooper, JF
Simpson, DG
AF Lipatov, A. S.
Sittler, E. C., Jr.
Hartle, R. E.
Cooper, J. F.
Simpson, D. G.
TI Saturn's magnetosphere interaction with Titan for T9 encounter: 3D
hybrid modeling and comparison with CAPS observations
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Ionospheres; Atmospheres; Induced magnetospheres; Magnetic barrier;
Alfven wing; Plasma modeling
ID PLASMA ENVIRONMENT; SOLAR-WIND; MHD MODEL; SIMULATION; IONS;
SPECTROMETER; IONOSPHERE; ATOMS; COMET; SHOCK
AB Global dynamics of ionized and neutral gases in the environment of Titan plays an important role in the interaction of Saturn's magnetosphere with Titan. Several hybrid simulations of this problem have already been done (Brecht et al., 2000; Kallio et al., 2004; Modolo et al., 2007a; Simon et al., 2007a, 2007b; Modolo and Chanteur, 2008). Observational data from CAPS for the 19 encounter (Sittler et al., 2009) indicates an absence of 0 heavy ions in the upstream that change the models of interaction which were discussed in current publications (Kallio et al., 2004; Modolo et al., 2007a; Simon et al., 2007a, 20076; Ma et al., 2007; Szego et al., 2007). Further analysis of the CAPS data shows very low density or even an absence of H+ ions in upstream. In this paper we discuss two models of the interaction of Saturn's magnetosphere with Titan: (A) high density of H ions in the upstream flow (0.1 cm(-3)), and (B) low density of H+ ions in the upstream flow (0.02 cm(-3)). The hybrid model employs a fluid description for electrons and neutrals, whereas a particle approach is used for ions. We also take into account charge-exchange and photoionization processes and solve self-consistently for electric and magnetic fields. The model atmosphere includes exospheric H+, H-2(+), N-2(+) and CH4+ pickup ion production as well as an immobile background ionosphere and a shell distribution for active ionospheric ions (M-i=28 amu). The hybrid model allows us to account for the realistic anisotropic ion velocity distribution that cannot be done in fluid simulations with isotropic temperatures. Our simulation shows an asymmetry of the ion density distribution and the magnetic field, including the formation of Alfven wing-like structures.
The results of the ion dynamics in Titan's environment are compared with Cassini T9 encounter data (CAPS). (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Lipatov, A. S.; Sittler, E. C., Jr.; Hartle, R. E.; Cooper, J. F.; Simpson, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lipatov, A. S.] Univ Maryland Baltimore Cty, Goddard Planetary & Heliophys Inst, Baltimore, MD 21228 USA.
[Lipatov, A. S.] Russian Acad Sci, AA Dorodnitsyn Comp Ctr, Moscow 119991, Russia.
[Lipatov, A. S.] Moscow Inst Phys & Technol, Fac Problems Phys & Power Engn, Moscow, Russia.
RP Lipatov, AS (reprint author), NASA, Goddard Space Flight Ctr, Code 673,Bldg 21,Room 247,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM Alexander.Lipatov-1@nasa.gov; Edward.C.Sittler@nasa.gov;
Richard.E.Hartle@nasa.gov; John.F.Cooper@nasa.gov;
David.G.Simpson@nasa.gov
RI Cooper, John/D-4709-2012
FU NASA [08-CDAP08-0043]; GPHI/(GEST Center) UMBC [900-37-172, 670-90-315];
NASA GSFC [900-37-172, 670-90-315]; NASA Ames Advanced Supercomputing
(NAS) Division [SMD-09-1124, SMD-10-1517]
FX A.S.L., E.C.S., R.E.H., J.F.C., and D.G.S. were supported by the Grant
Analysis of Titan's Interaction with Saturn's Magnetosphere using
Cassini Titan Flyby Data and Kinetic-Fluid Model from the NASA Cassini
Data Analysis Program (08-CDAP08-0043). A.S.L. was also supported in
part by the Grants/Tasks 900-37-172 and 670-90-315 between the
GPHI/(GEST Center) UMBC and NASA GSFC. Computational resources were
provided by the NASA Ames Advanced Supercomputing (NAS) Division
(Projects SMD-09-1124 and SMD-10-1517). The authors thank the referees
for fruitful comments.
NR 42
TC 5
Z9 5
U1 0
U2 6
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 FEB
PY 2012
VL 61
IS 1
SI SI
BP 66
EP 78
DI 10.1016/j.pss.2011.08.017
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 971IY
UT WOS:000306198800008
ER
PT J
AU Stephan, K
Jaumann, R
Wagner, R
Clark, RN
Cruikshank, DP
Giese, B
Hibbitts, CA
Roatsch, T
Matz, KD
Brown, RH
Filacchione, G
Cappacioni, F
Scholten, F
Buratti, BJ
Hansen, GB
Nicholson, PD
Baines, KH
Nelson, RM
Matson, DL
AF Stephan, Katrin
Jaumann, Ralf
Wagner, Roland
Clark, Roger N.
Cruikshank, Dale P.
Giese, Bernd
Hibbitts, Charles A.
Roatsch, Thomas
Matz, Klaus-Dieter
Brown, Robert H.
Filacchione, Gianrico
Cappacioni, Fabrizio
Scholten, F.
Buratti, Bonnie J.
Hansen, Gary B.
Nicholson, Phil D.
Baines, Kevin H.
Nelson, Robert M.
Matson, Dennis L.
TI The Saturnian satellite Rhea as seen by Cassini VIMS
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Rhea; Icy satellites; Spectroscopy; Surfaces; Cassini/VIMS
ID OUTER SOLAR-SYSTEM; E-RING; ENCELADUS SURFACE; IMAGING SCIENCE; ICY
SATELLITES; MAGNETOSPHERE; SPECTROMETER; IAPETUS; PARTICLES; DYNAMICS
AB Since the arrival of the Cassini spacecraft at Saturn in June 2004, the Visual and Infrared Mapping Spectrometer has obtained new spectral data of the icy satellites of Saturn in the spectral range from 0.35 to 5.2 mu m. Numerous flybys were performed at Saturn's second largest satellite Rhea, providing a nearly complete coverage with pixel-ground resolutions sufficient to analyze variations of spectral properties across Rhea's surface in detail. We present an overview of the VIMS observations obtained so far, as well as the analysis of the spectral properties identified in the VIMS spectra and their variations across its surface compared with spatially highly resolved Cassini ISS images and digital elevation models.
Spectral variations measured across Rhea's surface are similar to the variations observed in the VIMS observations of its neighbor Dione, implying similar processes causing or at least inducing their occurrence. Thus, magnetospheric particles and dust impacting onto the trailing hemisphere appear to be responsible for the concentration of dark rocky/organic material and minor amounts of CO2 in the cratered terrain on the trailing hemisphere. Despite the prominent spectral signatures of Rhea's fresh impact crater Inktomi, radiation effects were identified that also affect the H2O ice-rich cratered terrain of the leading hemisphere. The concentration of H2O ice in the vicinity of steep tectonic scarps near 270 degrees W and geologically fresh impact craters implies that Rhea exhibits an icy crust at least in the upper few kilometers. Despite the evidence for past tectonic events, no indications of recent endogenically powered processes could be identified in the Cassini data. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Stephan, Katrin; Jaumann, Ralf; Wagner, Roland; Giese, Bernd; Roatsch, Thomas; Matz, Klaus-Dieter; Scholten, F.] DLR, Inst Planetary Res, D-12489 Berlin, Germany.
[Jaumann, Ralf] Free Univ Berlin, FR Planetol & Fernerkundung, D-12249 Berlin, Germany.
[Clark, Roger N.] US Geol Survey, Denver Fed Ctr, Denver, CO 80225 USA.
[Cruikshank, Dale P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Hibbitts, Charles A.] JHU Appl Phys Lab, Laurel, MD USA.
[Brown, Robert H.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Filacchione, Gianrico; Cappacioni, Fabrizio] INAF IASF, Rome, Italy.
[Buratti, Bonnie J.; Nelson, Robert M.; Matson, Dennis L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hansen, Gary B.] Univ Washington, Seattle, WA 98195 USA.
[Nicholson, Phil D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Baines, Kevin H.] Univ Wisconsin, SSEC, Madison, WI 53706 USA.
RP Stephan, K (reprint author), DLR, Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany.
EM Katrin.Stephan@dlr.de
RI Hibbitts, Charles/B-7787-2016;
OI Hibbitts, Charles/0000-0001-9089-4391; Filacchione,
Gianrico/0000-0001-9567-0055
FU DLR; Helmholtz Alliance 'Planetary evolution and Life'
FX We gratefully acknowledge the many years of work of the entire Cassini
team that allowed these data to be obtained. We want to thank E.
Hoffmann for his support with the data processing. This work has been
partly supported by DLR and the Helmholtz Alliance 'Planetary evolution
and Life'.
NR 88
TC 17
Z9 17
U1 0
U2 5
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 FEB
PY 2012
VL 61
IS 1
SI SI
BP 142
EP 160
DI 10.1016/j.pss.2011.07.019
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 971IY
UT WOS:000306198800016
ER
PT J
AU Orton, GS
Fletcher, LN
Liu, JJ
Schneider, T
Yanamandra-Fisher, PA
de Pater, I
Edwards, M
Geballe, TR
Hammel, HB
Fujiyoshi, T
Encrenaz, T
Pantin, E
Mousis, O
Fuse, T
AF Orton, Glenn S.
Fletcher, Leigh N.
Liu, Junjun
Schneider, Tapio
Yanamandra-Fisher, Padma A.
de Pater, Imke
Edwards, Michelle
Geballe, Thomas R.
Hammel, Heidi B.
Fujiyoshi, Takuya
Encrenaz, Therese
Pantin, Eric
Mousis, Olivier
Fuse, Tetsuharu
TI Recovery and characterization of Neptune's near-polar stratospheric hot
spot
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Neptune; Stratosphere; Temperature; Dynamics; Radiative heating
ID MIDINFRARED IMAGER; JUPITER; TEMPERATURES; SPECTROMETER; ATMOSPHERE
AB Images of Neptune obtained in 2006 at ESO's Very Large Telescope (Orton et al., 2007, Astronomy & Astrophysics 473, L5) revealed a near-polar hot spot near 70 degrees S latitude that was detectable in filters sampling both stratospheric methane (7 mu m) and ethane (similar to 12 mu m) emission. Such a feature was not present in 2003 Keck and 2005 Gemini North observations, which showed only a general warming trend toward Neptune's pole that was longitudinally homogeneous. Because of the paucity of longitudinal sampling in the 2003,2005 and 2006 images, it was not clear whether the failure to see this phenomenon in 2003 and 2005 was simply the result of insufficient longitudinal sampling or whether the phenomenon was truly variable in time. To unravel these two possibilities, we made follow-up observations on large telescopes that were capable of resolving Neptune at thermal-infrared wavelengths: Gemini South in 2007 and 2010 using the T-ReCS instrument, Subaru in 2008 using the COMICS instrument and VLT in 2008 and 2009 using the VISIR instrument. Two serendipitous T-ReCS images of Neptune were also obtained in 2007 using a broad N-band (8-14 mu m) filter, whose radiance is dominated by stratospheric emission from both methane and ethane. The feature was recovered (i) in 2007 with T-ReCS in the broad N-band image and (ii) in 2008 with COMICS in a 12.5-mu m image. However, T-ReCS observations in 2010 that covered up to 250 degrees of longitude did not show evidence of an off-polar hot spot. Although we have not definitively ruled out the possibility that various observers have simply missed a semi-permanent feature, it seems statistically very unlikely to be the case. With only 3 sightings in 13 independent observing epochs, it is likely that the phenomenon is ephemeral in time. A possible origin for the phenomenon is a large planetary wave that is dynamically confined to the high-latitude regions characterized by prograde zonal winds. It may be episodically excited by dynamical activity deeper in the atmosphere. This must be coupled with mixing near the poles that destroys or at least substantially attenuates the hot spot over the south pole that leads to an appearance of the typical polar stratospheric hot spot being offset in latitude. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Orton, Glenn S.; Yanamandra-Fisher, Padma A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Fletcher, Leigh N.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England.
[Liu, Junjun; Schneider, Tapio] CALTECH, Pasadena, CA 91125 USA.
[de Pater, Imke] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Edwards, Michelle] Gemini Observ, La Serena, Chile.
[Geballe, Thomas R.] Gemini Observ, Hilo, HI 96720 USA.
[Hammel, Heidi B.] Space Sci Inst, Ridgefield, CT 06877 USA.
[Fujiyoshi, Takuya] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Encrenaz, Therese] Observ Paris, LESIA, F-92195 Meudon, France.
[Pantin, Eric] Ctr Etud Atom, F-91190 Gif Sur Yvette, France.
[Mousis, Olivier] Univ Franche Comte, CNRS UMR 6213, Inst UTINAM, Observ Sci Univers THETA, F-25010 Besancon, France.
[Fuse, Tetsuharu] Natl Inst Informat & Commun Technol, Kashima Space Res Ctr, Ibaraki 3148501, Japan.
RP Orton, GS (reprint author), CALTECH, Jet Prop Lab, MS 169-237,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Glenn.Orton@jpl.nasa.gov
RI Fletcher, Leigh/D-6093-2011; Schneider, Tapio /A-7038-2014
OI Fletcher, Leigh/0000-0001-5834-9588; Schneider, Tapio
/0000-0001-5687-2287
FU NSF [AST-0908575]; University of Oxford; David and Lucile Packard
Fellowship; NASA [NNX10AQ05G]; National Astronomical Observatory of
Japan; Gemini Observatory; National Science Foundation (United States);
Science and Technology Facilities Council (United Kingdom); National
Research Council (Canada); CONICYT (Chile); Australian Research Council
(Australia); Ministrio da Cinica e Tecnologia (Brazil); Ministerio de
Cienica, Tecnologia e Innovacin Productiva (Argentina); European
Southern Observatory telescopes [081C-0496, 083C-0163]; Subaru Telescope
[S08-032]; Gemini North Telescope [GN-2007B-A-105]; Gemini South
Telescope [GS-2007B-Q-47, GS-2010B-A-42]
FX We thank Erich Karkoschka for helpful comments. Orton and
Yanamandra-Fisher conducted a portion of this research at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with NASA. They thank Mark Hofstadter, the Principal
Investigator of the relevant program, for this support. De Pater was
supported by NSF Grant AST-0908575. Fletcher was supported by a
Glasstone Science Fellowship at the University of Oxford. Schneider and
Liu acknowledge support by a David and Lucile Packard Fellowship and by
the NASA Outer Planets Research Program (Grant NNX10AQ05G). Fujiyoshi
and Fuse were supported by the National Astronomical Observatory of
Japan. Edwards and Geballe were supported by the Gemini Observatory, on
behalf of the Gemini partnership: the National Science Foundation
(United States), the Science and Technology Facilities Council (United
Kingdom), the National Research Council (Canada), CONICYT (Chile), the
Australian Research Council (Australia), Ministrio da Cinica e
Tecnologia (Brazil) and Ministerio de Cienica, Tecnologia e Innovacin
Productiva (Argentina). The simulations on which Fig. 5 is based were
performed on Caltech's Division of Geological and Planetary Sciences
Dell cluster.; The new results presented in this paper were based, in
part, on observations made at the European Southern Observatory
telescopes, in programs 081C-0496(A) and 083C-0163(A) and (B), obtained
from the ESO/ST-ECF Science Archive Facility; on data collected at
Subaru Telescope in program ID S08-032, which is operated by the
National Astronomical Observatory of Japan: and on data obtained from
the Gemini North Telescope in program GN-2007B-A-105 and the Gemini
South Telescope in programs GS-2007B-Q-47, GS-2010B-A-42, which are
operated by the Association of Universities for Research in Astronomy.
(C) 2010. All rights reserved.
NR 25
TC 7
Z9 7
U1 0
U2 4
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 FEB
PY 2012
VL 61
IS 1
SI SI
BP 161
EP 167
DI 10.1016/j.pss.2011.06.013
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 971IY
UT WOS:000306198800017
ER
PT J
AU Hepp, AF
AF Hepp, Aloysius F.
TI Untitled
SO MATERIALS SCIENCE IN SEMICONDUCTOR PROCESSING
LA English
DT Editorial Material
C1 NASA Glenn Res Ctr, Cleveland, OH USA.
RP Hepp, AF (reprint author), NASA Glenn Res Ctr, Cleveland, OH USA.
EM matscisemiproc@gmail.com
NR 0
TC 0
Z9 0
U1 1
U2 2
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 1369-8001
J9 MAT SCI SEMICON PROC
JI Mater. Sci. Semicond. Process
PD FEB
PY 2012
VL 15
IS 1
BP 1
EP 1
DI 10.1016/j.mssp.2012.03.016
PG 1
WC Engineering, Electrical & Electronic; Materials Science,
Multidisciplinary; Physics, Applied; Physics, Condensed Matter
SC Engineering; Materials Science; Physics
GA 956TL
UT WOS:000305111900001
ER
PT J
AU Ramsey, BD
Gaskin, JA
Elsner, RF
Chen, W
Carini, GA
De Geronimo, G
Keister, J
Li, S
Li, Z
Siddons, DP
Smith, G
AF Ramsey, B. D.
Gaskin, J. A.
Elsner, R. F.
Chen, W.
Carini, G. A.
De Geronimo, G.
Keister, J.
Li, S.
Li, Z.
Siddons, D. P.
Smith, G.
TI A low-power, radiation-resistant, Silicon-Drift-Detector array for
extraterrestrial element mapping
SO JOURNAL OF INSTRUMENTATION
LA English
DT Article
DE Solid state detectors; X-ray detectors and telescopes
ID ICY GALILEAN SATELLITES; X-RAY SPECTROMETERS; CMOS TECHNOLOGIES; EUROPAS
OCEAN; SURFACE; ORIGIN; TORUS
AB We are developing a modular Silicon Drift Detector (SDD) X-Ray Spectrometer (XRS) for measuring the abundances of light surface elements (C to Fe) fluoresced by ambient radiation on remote airless bodies. The value of fluorescence spectrometry for surface element mapping is demonstrated by its inclusion on three recent lunar missions and by exciting new data that have recently been announced from the Messenger Mission to Mercury.
The SDD-XRS instrument that we have been developing offers excellent energy resolution and an order of magnitude lower power requirement than conventional CCDs, making much higher sensitivities possible with modest spacecraft resources. In addition, it is significantly more radiation resistant than x-ray CCDs and therefore will not be subject to the degradation that befell recent lunar instruments. In fact, the intrinsic radiation resistance of the SDD makes it applicable even to the harsh environment of the Jovian system where it can be used to map the light surface elements of Europa.
In this paper, we first discuss our element-mapping science-measurement goals. We then derive the necessary instrument requirements to meet these goals and discuss our current instrument development status with respect to these requirements.
C1 [Ramsey, B. D.; Gaskin, J. A.; Elsner, R. F.] NASA, MSFC, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA.
[Chen, W.; Carini, G. A.; De Geronimo, G.; Keister, J.; Li, S.; Li, Z.; Siddons, D. P.; Smith, G.] Brookhaven Natl Lab, Upton, NY 11973 USA.
RP Ramsey, BD (reprint author), NASA, MSFC, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA.
EM Brian.Ramsey@nasa.gov
NR 42
TC 3
Z9 3
U1 0
U2 11
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 1748-0221
J9 J INSTRUM
JI J. Instrum.
PD FEB
PY 2012
VL 7
AR C02013
DI 10.1088/1748-0221/7/02/C02013
PG 14
WC Instruments & Instrumentation
SC Instruments & Instrumentation
GA 941CQ
UT WOS:000303940900013
ER
PT J
AU Andrews, RJ
AF Andrews, Russell J.
TI Nanotechnology and Drug Delivery: Getting There is Only Half of the
Challenge! (Commentary)
SO CNS & NEUROLOGICAL DISORDERS-DRUG TARGETS
LA English
DT Editorial Material
ID CARBON; STIMULATION; ADENOSINE
C1 NASA, Ames Res Ctr, Ames Associate Smart Syst & Nanotechnol, Moffett Field, CA 94035 USA.
RP Andrews, RJ (reprint author), NASA, Ames Res Ctr, Ames Associate Smart Syst & Nanotechnol, Moffett Field, CA 94035 USA.
EM rja@russelljandrews.org
NR 10
TC 3
Z9 3
U1 0
U2 0
PU BENTHAM SCIENCE PUBL LTD
PI SHARJAH
PA EXECUTIVE STE Y26, PO BOX 7917, SAIF ZONE, 1200 BR SHARJAH, U ARAB
EMIRATES
SN 1871-5273
J9 CNS NEUROL DISORD-DR
JI CNS Neurol. Disord.-Drug Targets
PD FEB
PY 2012
VL 11
IS 1
BP 96
EP 97
PG 2
WC Neurosciences; Pharmacology & Pharmacy
SC Neurosciences & Neurology; Pharmacology & Pharmacy
GA 934MW
UT WOS:000303449400011
PM 22380465
ER
PT J
AU Breger, M
Hareter, M
Endl, M
Kuschnig, R
Weiss, WW
Matthews, JM
Guenther, DB
Moffat, AFJ
Rowe, JF
Rucinski, SM
Sasselov, D
AF Breger, M.
Hareter, M.
Endl, M.
Kuschnig, R.
Weiss, W. W.
Matthews, J. M.
Guenther, D. B.
Moffat, A. F. J.
Rowe, J. F.
Rucinski, S. M.
Sasselov, D.
TI Delta Scuti stars in the Praesepe cluster observed by the MOST satellite
SO ASTRONOMISCHE NACHRICHTEN
LA English
DT Article
DE delta Scuti stars; open clusters and associations: individual
(Praesepe); stars: individual (BS Cnc, BT Cnc, EP Cnc, HD 73872); stars:
oscillations; techniques: photometric
ID STACC 1998 CAMPAIGN; BT CANCRI; F-STARS; PHOTOMETRY; SPACE; VARIABILITY;
PULSATION
AB The Praesepe cluster contains a number of delta Sct and gamma Dor pulsators. Asteroseismology of cluster stars is simplified by the common distance, age and stellar abundances. Since asteroseismology requires a large number of known frequencies, the small pulsation amplitudes of these stars require space satellite campaigns. The present study utilizes photometric MOST satellite measurements in order to determine the pulsation frequencies of two evolved (EP Cnc, BT Cnc) and two main-sequence (BS Cnc, HD 73872) delta Sct stars in the Praesepe cluster. The frequency analysis of the 2008 and 2009 data detected up to 34 frequencies per star with most amplitudes in the submillimag range. In BS Cnc, two modes showed strong amplitude variability between 2008 and 2009. The frequencies ranged from 0.76 to 41.7 cd(-1). After considering the different evolutionary states and mean stellar densities of these four stars, the differences and large ranges in frequency remain. (C) 2012 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim
C1 [Breger, M.; Hareter, M.; Endl, M.; Kuschnig, R.; Weiss, W. W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Breger, M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Matthews, J. M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Guenther, D. B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, 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 Breger, M (reprint author), Univ Vienna, Inst Astron, Turkenschanzstr 17, A-1180 Vienna, Austria.
EM michel.breger@univie.ac.at
FU Austrian Fonds zur Forderung der wissenschaftlichen Forschung [P
21830-N16, P 22691-N16]
FX This investigation has been supported by the Austrian Fonds zur
Forderung der wissenschaftlichen Forschung through projects P 21830-N16
and P 22691-N16.
NR 31
TC 6
Z9 6
U1 0
U2 2
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY
SN 0004-6337
J9 ASTRON NACHR
JI Astro. Nachr.
PD FEB
PY 2012
VL 333
IS 2
BP 131
EP 137
DI 10.1002/asna.201111640
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 932TH
UT WOS:000303312900005
ER
PT J
AU Nessel, JA
Acosta, RJ
AF Nessel, James A.
Acosta, Roberto J.
TI Predicting Sparse Array Performance From Two-Element Interferometer Data
SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION
LA English
DT Article
DE Arrays; phase noise; propagation measurements; sparse array antennas
ID WATER-VAPOR; TURBULENCE; SPECTRUM
AB Widely distributed (sparse) ground-based antenna arrays are being considered for deep space communications applications with the development of the proposed Next Generation Deep Space Network. However, atmospheric-induced phase fluctuations can impose daunting restrictions on the performance of such an array, particularly during transmit and particularly at Ka-band frequencies, which have yet to be successfully resolved. In this paper, an analysis of the uncompensated performance of a sparse antenna array, in terms of its directivity and pattern degradation, is performed utilizing real data. The theoretical derivation for array directivity degradation is validated with interferometric measurements (for a 2-element array) recorded at Goldstone, CA, from May 2007-May 2008. With the validity of the model established, an arbitrary 27-element array geometry is defined at Goldstone, CA, to ascertain its theoretical performance in the presence of phase fluctuations based on the measured data. Therein, a procedure in which array directivity performance can be determined based on site-specific interferometric measurements is established. It is concluded that a combination of compact array geometry and atmospheric compensation is necessary to minimize array loss impact for deep space communications.
C1 [Nessel, James A.; Acosta, Roberto J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Nessel, JA (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM james.a.nessel@nasa.gov; roberto.j.acosta@nasa.gov
FU NASA's Space Communications and Navigation (SCaN) under the Space
Operations Mission Directorate (SOMD)
FX Manuscript received September 02, 2010; revised March 14, 2011; accepted
June 04, 2011. Date of publication October 21, 2011; date of current
version February 03, 2012. This work was supported in part by NASA's
Space Communications and Navigation (SCaN) Program under the Space
Operations Mission Directorate (SOMD).
NR 19
TC 1
Z9 1
U1 0
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-926X
J9 IEEE T ANTENN PROPAG
JI IEEE Trans. Antennas Propag.
PD FEB
PY 2012
VL 60
IS 2
BP 886
EP 894
DI 10.1109/TAP.2011.2173110
PN 2
PG 9
WC Engineering, Electrical & Electronic; Telecommunications
SC Engineering; Telecommunications
GA 924VV
UT WOS:000302720300019
ER
PT J
AU Ajello, M
Baldini, L
Barbiellini, G
Bastieri, D
Bechtol, K
Bellazzini, R
Berenji, B
Bloom, ED
Bonamente, E
Borgland, AW
Bregeon, J
Brigida, M
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caraveo, PA
Casandjian, JM
Cecchi, C
Charles, E
Chekhtman, A
Chiang, J
Ciprini, S
Claus, R
Cohen-Tanugi, J
Conrad, J
Cutini, S
de Angelis, A
de Palma, F
Dermer, CD
Silva, EDE
Drell, PS
Drlica-Wagner, A
Enoto, T
Favuzzi, C
Fegan, SJ
Ferrara, EC
Fukazawa, Y
Fusco, P
Gargano, F
Gasparrini, D
Germani, S
Giglietto, N
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Graham, P
Grenier, IA
Guiriec, S
Gustafsson, M
Hadasch, D
Hayashida, M
Hughes, RE
Johnson, AS
Kamae, T
Katagiri, H
Kataoka, J
Knodlseder, J
Kuss, M
Lande, J
Latronico, L
Lionetto, AM
Longo, F
Loparco, F
Lovellette, MN
Lubrano, P
Mazziotta, MN
Michelson, PF
Mitthumsiri, W
Mizuno, T
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Norris, JP
Nuss, E
Ohsugi, T
Okumura, A
Orlando, E
Ormes, JF
Ozaki, M
Paneque, D
Pesce-Rollins, M
Pierbattista, M
Piron, F
Pivato, G
Raino, S
Razzano, M
Ritz, S
Roth, M
Parkinson, PMS
Scargle, JD
Schalk, TL
Sgro, C
Siskind, EJ
Spandre, G
Spinelli, P
Suson, DJ
Tajima, H
Takahashi, H
Tanaka, T
Thayer, JG
Thayer, JB
Tibaldo, L
Tinivella, M
Torres, DF
Troja, E
Uchiyama, Y
Usher, TL
Vandenbroucke, J
Vasileiou, V
Vianello, G
Vitale, V
Waite, AP
Winer, BL
Wood, KS
Wood, M
Yang, Z
Zimmer, S
AF Ajello, M.
Baldini, L.
Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Berenji, B.
Bloom, E. D.
Bonamente, E.
Borgland, A. W.
Bregeon, J.
Brigida, M.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caraveo, P. A.
Casandjian, J. M.
Cecchi, C.
Charles, E.
Chekhtman, A.
Chiang, J.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Conrad, J.
Cutini, S.
de Angelis, A.
de Palma, F.
Dermer, C. D.
do Couto e Silva, E.
Drell, P. S.
Drlica-Wagner, A.
Enoto, T.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Fukazawa, Y.
Fusco, P.
Gargano, F.
Gasparrini, D.
Germani, S.
Giglietto, N.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Graham, P.
Grenier, I. A.
Guiriec, S.
Gustafsson, M.
Hadasch, D.
Hayashida, M.
Hughes, R. E.
Johnson, A. S.
Kamae, T.
Katagiri, H.
Kataoka, J.
Knoedlseder, J.
Kuss, M.
Lande, J.
Latronico, L.
Lionetto, A. M.
Longo, F.
Loparco, F.
Lovellette, M. N.
Lubrano, P.
Mazziotta, M. N.
Michelson, P. F.
Mitthumsiri, W.
Mizuno, T.
Monte, C.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Norris, J. P.
Nuss, E.
Ohsugi, T.
Okumura, A.
Orlando, E.
Ormes, J. F.
Ozaki, M.
Paneque, D.
Pesce-Rollins, M.
Pierbattista, M.
Piron, F.
Pivato, G.
Raino, S.
Razzano, M.
Ritz, S.
Roth, M.
Parkinson, P. M. Saz
Scargle, J. D.
Schalk, T. L.
Sgro, C.
Siskind, E. J.
Spandre, G.
Spinelli, P.
Suson, D. J.
Tajima, H.
Takahashi, H.
Tanaka, T.
Thayer, J. G.
Thayer, J. B.
Tibaldo, L.
Tinivella, M.
Torres, D. F.
Troja, E.
Uchiyama, Y.
Usher, T. L.
Vandenbroucke, J.
Vasileiou, V.
Vianello, G.
Vitale, V.
Waite, A. P.
Winer, B. L.
Wood, K. S.
Wood, M.
Yang, Z.
Zimmer, S.
TI Limits on large extra dimensions based on observations of neutron stars
with the Fermi-LAT
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE extra dimensions; gravity; neutron stars; core-collapse supernovas
ID LARGE-AREA TELESCOPE; EGRET; CATALOG
AB We present limits for the compactification scale in the theory of Large Extra Dimensions (LED) proposed by Arkani-Hamed, Dimopoulos, and Dvali. We use 11 months of data from the Fermi Large Area Telescope (Fermi-LAT) to set gamma ray flux limits for 6 gamma-ray faint neutron stars (NS). To set limits on LED we use the model of Hannestad and Raffelt (HR) that calculates the Kaluza-Klein (KK) graviton production in supernova cores and the large fraction subsequently gravitationally bound around the resulting NS. The predicted decay of the bound KK gravitons to gamma gamma should contribute to the flux from NSs. Considering 2 to 7 extra dimensions of the same size in the context of the HR model, we use Monte Carlo techniques to calculate the expected differential flux of gamma-rays arising from these KK gravitons, including the effects of the age of the NS, graviton orbit, and absorption of gamma-rays in the magnetosphere of the NS. We compare our Monte Carlo-based differential flux to the experimental differential flux using maximum likelihood techniques to obtain our limits on LED. Our limits are more restrictive than past EGRET-based optimistic limits that do not include these important corrections. Additionally, our limits are more stringent than LHC based limits for 3 or fewer LED, and comparable for 4 LED. We conclude that if the effective Planck scale is around a TeV, then for 2 or 3 LED the compactification topology must be more complicated than a torus.
C1 [Ajello, M.; Bechtol, K.; Berenji, B.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Enoto, T.; Glanzman, T.; Godfrey, G.; Graham, P.; Hayashida, M.; Hughes, R. E.; Kamae, T.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Orlando, E.; Paneque, D.; Tajima, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wood, M.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Ajello, M.; Bechtol, K.; Berenji, B.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Enoto, T.; Glanzman, T.; Godfrey, G.; Graham, P.; Hayashida, M.; Hughes, R. E.; Kamae, T.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Orlando, E.; Paneque, D.; Tajima, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] INFN Sez Pisa, I-56127 Pisa, Italy.
[Barbiellini, G.; Longo, F.] INFN Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Buson, S.; Gustafsson, M.; Tibaldo, L.] INFN Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Pivato, G.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.] INFN Sez Perugia, I-06123 Perugia, Italy.
[Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bruel, P.; Fegan, S. J.] Ecole Polytech, Lab Leprince Ringuet, CNRS IN2P3, Palaiseau, France.
[Caliandro, G. A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEE CSIC, Barcelona 08193, Spain.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Casandjian, J. M.; Grenier, I. A.; Pierbattista, M.] CEA IRFU CNRS Univ Paris Diderot, Lab AIM, Serv Astrophys, CEA Saclay, F-91191 Gif Sur Yvette, France.
[Chekhtman, A.] Artep Inc, Ellicott City, MD 21042 USA.
[Ciprini, S.] ASI Sci Data Ctr, I-00044 Rome, Italy.
[Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, Lab Univers & Particules Montpellier, CNRS IN2P3, F-34095 Montpellier 05, France.
[Conrad, J.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Conrad, J.; Yang, Z.; Zimmer, S.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Conrad, J.] Royal Swedish Acad Sci Res, Stockholm, Sweden.
[Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Rome, Italy.
[de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.] Grp Collegato Udine, INFN Sez Trieste, I-33100 Udine, Italy.
[Dermer, C. D.; Lovellette, M. N.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Ferrara, E. C.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fukazawa, Y.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Guiriec, S.] Univ Alabama, Ctr Space Plasma & Aeron Res CSPAR, Huntsville, AL 35899 USA.
[Hughes, R. E.] Kyoto Univ, Dept Astron, Grad Sch Sci, Sakyo Ku, Kyoto 6068502, Japan.
[Johnson, A. S.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Katagiri, H.] Ibaraki Univ, Coll Sci, Bunkyo Ku, Mito, Ibaraki 3108512, Japan.
[Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Knoedlseder, J.] IRAP, CNRS, F-31028 Toulouse 4, France.
[Knoedlseder, J.] Univ Toulouse, GAHEC, UPS OMP, IRAP, Toulouse, France.
[Latronico, L.] INFN Sezioine Torino, I-10125 Turin, Italy.
[Lionetto, A. M.; Morselli, A.; Vitale, V.] INFN Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Lionetto, A. M.; Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Norris, J. P.] Boise State Univ, Dept Phys, Boise, ID 83725 USA.
[Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Okumura, A.; Ozaki, M.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Razzano, M.; Ritz, S.; Parkinson, P. M. Saz; Schalk, T. L.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Razzano, M.; Ritz, S.; Parkinson, P. M. Saz; Schalk, T. L.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Siskind, E. J.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Tajima, H.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan.
[Troja, E.] NASA Postdoctoral Program, Oak Ridge, TN USA.
[Vianello, G.] Consorzio Interuniv Fis Spaziale CIFS, I-10133 Turin, Italy.
[Torres, D. F.] Inst Catalana Recerca & Estudis Avancats ICREA, Barcelona, Spain.
RP Ajello, M (reprint author), Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
EM bijanb@alumni.stanford.edu; bberenji@uci.edu;
johann.cohen-tanugi@lupm.in2p3.fr
RI Orlando, E/R-5594-2016; Do, Changwoo/A-9670-2011; Baldini,
Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Morselli,
Aldo/G-6769-2011; Kuss, Michael/H-8959-2012; giglietto,
nicola/I-8951-2012; Ozaki, Masanobu/K-1165-2013; Loparco,
Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; Moskalenko,
Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro,
Carmelo/K-3395-2016; Torres, Diego/O-9422-2016;
OI Do, Changwoo/0000-0001-8358-8417; lubrano, pasquale/0000-0003-0221-4806;
Morselli, Aldo/0000-0002-7704-9553; giglietto,
nicola/0000-0002-9021-2888; Loparco, Francesco/0000-0002-1173-5673;
Gargano, Fabio/0000-0002-5055-6395; Moskalenko,
Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Torres,
Diego/0000-0002-1522-9065; Gasparrini, Dario/0000-0002-5064-9495;
Baldini, Luca/0000-0002-9785-7726; Graham, Peter/0000-0002-1600-1601; De
Angelis, Alessandro/0000-0002-3288-2517; Caraveo,
Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214;
SPINELLI, Paolo/0000-0001-6688-8864; Bastieri,
Denis/0000-0002-6954-8862; Pesce-Rollins, Melissa/0000-0003-1790-8018;
Giroletti, Marcello/0000-0002-8657-8852; Cutini,
Sara/0000-0002-1271-2924; Berenji, Bijan/0000-0002-4551-772X
FU National Aeronautics and Space Administration; Department of Energy in
the United States; Commissariat a l'Energie Atomique; Centre National de
la Recherche Scientifique / Institut National de Physique Nucleaire et
de Physique des Particules in France; Agenzia Spaziale Italiana;
Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education,
Culture, Sports, Science and Technology (MEXT), High Energy Accelerator
Research Organization (KEK); Japan Aerospace Exploration Agency (JAXA)
in Japan; K. A. Wallenberg Foundation; Swedish Research Council; Swedish
National Space Board in Sweden; Istituto Nazionale di Astrofisica in
Italy; Centre National d'Etudes Spatiales in France
FX The Fermi-LAT Collaboration acknowledges generous ongoing support from a
number of agencies and institutes that have supported both the
development and the operation of the LAT as well as scientific data
analysis. These include the National Aeronautics and Space
Administration and the Department of Energy in the United States, the
Commissariat a l'Energie Atomique and the Centre National de la
Recherche Scientifique / Institut National de Physique Nucleaire et de
Physique des Particules in France, the Agenzia Spaziale Italiana and the
Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of
Education, Culture, Sports, Science and Technology (MEXT), High Energy
Accelerator Research Organization (KEK) and Japan Aerospace Exploration
Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish
Research Council and the Swedish National Space Board in Sweden.;
Additional support for science analysis during the operations phase is
gratefully acknowledged from the Istituto Nazionale di Astrofisica in
Italy and the Centre National d'Etudes Spatiales in France.
NR 28
TC 2
Z9 2
U1 0
U2 7
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 FEB
PY 2012
IS 2
AR 012
DI 10.1088/1475-7516/2012/02/012
PG 25
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 904EE
UT WOS:000301176000013
ER
PT J
AU Bae, SY
Korniski, R
Ream, A
Shahinian, H
Manohara, HM
AF Bae, Sam Y.
Korniski, Ron
Ream, Allen
Shahinian, Hrayr
Manohara, Harish M.
TI New technique of three-dimensional imaging through a 3-mm single lens
camera
SO OPTICAL ENGINEERING
LA English
DT Article
DE 3-D imaging; stereo endoscope; multispectral imaging; minimally invasive
neurosurgery; skull base surgery; spectral illumination band (SIB);
complementary multi-bandpass filters
AB We present a technique for imaging full-color 3-D images with a single camera in this paper. Unlike a typical 3-D-imaging system comprising two independent cameras each contributing one viewpoint, the technique presented here creates two viewpoints using a single-lens camera with a bipartite filter whose bandpass characteristics are complementary to each other. The bipartite filter divides the camera's limiting aperture into two spatially separated apertures or viewpoints that alternately image an object field using filter-passband matched, time-sequenced illumination. This technique was applied to construct a 3-D camera to image scenes at a working distance of 10 mm. We evaluated the effectiveness of the 3-D camera in generating stereo images using statistical comparison of the depth resolutions achieved by the 3-D camera and a similar 2D camera arrangement. The comparison showed that the complementary filters produce effective stereopsis at prescribed working distances. (C) 2012 Society of Photo-Optical Instrumentation Engineers (SPIE). [DOI: 10.1117/1.OE.51.2.021106]
C1 [Bae, Sam Y.; Korniski, Ron; Manohara, Harish M.] CALTECH, Jet Prop Lab, Pasadena, CA 90041 USA.
[Bae, Sam Y.] Univ Calif Los Angeles, Los Angeles, CA USA.
[Ream, Allen] Montana State Univ, Bozeman, MT 59717 USA.
[Shahinian, Hrayr] SUNY Stony Brook, Skull Base Inst, Los Angeles, CA USA.
RP Bae, SY (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 90041 USA.
EM ybae@jpl.nasa.gov
FU Skull Base Institute of Los Angeles, California; National Aeronautics
and Space Administration
FX This research was carried out under funding from the Skull Base
Institute of Los Angeles, California. We thank Mr. Victor White and Dr.
Kirill Scheglov who inspired us to conduct this research. We are
grateful to Dr. Pantazis Mouroulis at JPL whose constructive comments
helped shape this work. We also thank Mr. Robert Kowalczyk of JPL for
his assistance in the laboratory. Mr. Sam Bae gives special thanks to
Professor Harold Monbouquette of UCLA for his support and guidance of
the project for his PhD work at UCLA. This research was carried out at
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with the National Aeronautics and Space Administration.
Government sponsorship acknowledged.
NR 18
TC 5
Z9 5
U1 0
U2 7
PU SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA
SN 0091-3286
J9 OPT ENG
JI Opt. Eng.
PD FEB
PY 2012
VL 51
IS 2
AR 021106
DI 10.1117/1.OE.51.2.021106
PG 7
WC Optics
SC Optics
GA 925RS
UT WOS:000302779500008
ER
PT J
AU Dove, A
Heldmann, J
McKay, C
Toon, OB
AF Dove, Adrienne
Heldmann, Jennifer
McKay, Christopher
Toon, Owen B.
TI Physics of a Thick Seasonal Snowpack with Possible Implications for Snow
Algae
SO ARCTIC ANTARCTIC AND ALPINE RESEARCH
LA English
DT Article
ID SURFACE-ENERGY EXCHANGES; ALPINE SITE; TEMPERATURES; BALANCE; MODEL;
RADIATION; MOISTURE; CLIMATE; REGION; COVER
AB Instrumentation to study snowpack in situ was deployed in Lassen Volcanic National Park (LVNP), California, in an area of deep seasonal snow accumulation and known snow algal bloom recurrence. included in the instrumentation were 11 temperature sensors, evenly spaced up to 2 m above the ground, which provided (1) temperature data within the snowpack when buried, and (2) estimates of snowpack height during accumulation and ablation periods. Beginning in April, moisture sensors measured a strong increase of snowpack liquid water content to greater than 15% by volume; this high melt content is usually coincident with the start of runoff from the snowpack. Snow depth profiles showed a rapid ablation of the final 2 m of the snowpack over about 23 days beginning in late June. SNTHERM numerical modeling confirmed that solar radiation was the dominant energy term throughout the melt season. By modeling a variety of snowpack parameters, such as albedo and initial snow density, we determined that the date of snow loss is the most sensitive observable that can be used to constrain the modeled parameters. These data sets from LVNP can also be applied to knowledge of snow algae lifecycles in deep snow to help understand whether the availability of light, water, or both controls the onset of snow algae germination at the base of a thick snowpack. Data and modeling indicate that meltwater was present throughout the snowpack beginning in March and runoff is initiated in April, when the snowpack was still several meters deep. However, significant levels of light did not penetrate to the soil until June, when the snow was less than 2 m deep.
C1 [Dove, Adrienne; Toon, Owen B.] Atmospher & Space Phys Lab, Boulder, CO 80303 USA.
[Heldmann, Jennifer; McKay, Christopher] NASA, Ames Res Ctr, Div Space Sci & Astrobiol, Mountain View, CA 94035 USA.
RP Dove, A (reprint author), Atmospher & Space Phys Lab, 1234 Innovat Dr, Boulder, CO 80303 USA.
EM adrienne.dove@colorado.edu
FU NASA
FX This work was funded through the NASA Planetary Geology and Geophysics
Program and a NASA Graduate Student Research Program Fellowship. We
gratefully acknowledge the machine shop at NASA Ames Research Center for
building the equipment stands, Lassen Volcanic National Park for access
and permits for the site, Steve Zachary for invaluable help and guidance
at the park, and the many field hands who have assisted in data
collection over several field seasons. Additionally, we would like to
thank the anonymous reviewers for their detailed comments and
suggestions, which greatly improved the manuscript.
NR 42
TC 2
Z9 2
U1 1
U2 13
PU INST ARCTIC ALPINE RES
PI BOULDER
PA UNIV COLORADO, BOULDER, CO 80309 USA
SN 1523-0430
J9 ARCT ANTARCT ALP RES
JI Arct. Antarct. Alp. Res.
PD FEB
PY 2012
VL 44
IS 1
BP 36
EP 49
DI 10.1657/1938-4246-44.1.36
PG 14
WC Environmental Sciences; Geography, Physical
SC Environmental Sciences & Ecology; Physical Geography
GA 918SO
UT WOS:000302271600005
ER
PT J
AU Wohl, CJ
Atkins, BM
Belcher, MA
Connell, JW
AF Wohl, Christopher J.
Atkins, Brad M.
Belcher, Marcus A.
Connell, John W.
TI Synthesis, characterization, topographical modification, and surface
properties of copoly(imide siloxane)s
SO HIGH PERFORMANCE POLYMERS
LA English
DT Article
DE polyimide; siloxane; abhesion; lunar dust; superhydrophobicity
ID BLOCK-COPOLYMERS; PHASE-SEPARATION; LUNAR DUST; BLENDS
AB Novel copoly(imide siloxane)s were synthesized from commercially available aminopropyl terminated siloxane oligomers, aromatic dianhydrides, and diamines. This synthetic approach produced copolymers with well-defined siloxane blocks linked with imide units in a random fashion. The copoly(amide acid)s were characterized by solution viscosity and subsequently used to cast thin films followed by thermal imidization in an inert atmosphere. Thin films were characterized using contact angle goniometry, attenuated total reflection Fourier transform infrared spectroscopy, confocal and optical microscopy, and tensile testing. Adhesion of micron-sized particles was determined quantitatively using a sonication device. The polydimethylsiloxane moieties lowered the copolymer surface energy due to migration of siloxane moieties to the film's surface, resulting in a notable reduction in particle adhesion. A further reduction in particle adhesion was achieved by introducing topographical features on a scale of several to tens of microns by a laser ablation technique.
C1 [Wohl, Christopher J.; Atkins, Brad M.; Connell, John W.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Belcher, Marcus A.] Natl Inst Aerosp, Hampton, VA USA.
RP Wohl, CJ (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM christopher.j.wohl@nasa.gov
FU NASA Langley Research Center
FX The authors would like to thank Dr Jeffrey A. Hinkley, NASA Langley
Research Center, for scientific discussion. This work was funded through
the NASA Langley Research Center's Creative and Innovative Research
Fund.
NR 31
TC 10
Z9 12
U1 3
U2 17
PU SAGE PUBLICATIONS LTD
PI LONDON
PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND
SN 0954-0083
J9 HIGH PERFORM POLYM
JI High Perform. Polym.
PD FEB
PY 2012
VL 24
IS 1
SI SI
BP 40
EP 49
DI 10.1177/0954008311431113
PG 10
WC Polymer Science
SC Polymer Science
GA 918YR
UT WOS:000302288100006
ER
PT J
AU Gao, Y
Zhou, N
Yang, F
Cui, Y
Kovarik, L
Hatcher, N
Noebe, R
Mills, MJ
Wang, Y
AF Gao, Y.
Zhou, N.
Yang, F.
Cui, Y.
Kovarik, L.
Hatcher, N.
Noebe, R.
Mills, M. J.
Wang, Y.
TI P-phase precipitation and its effect on martensitic transformation in
(Ni,Pt)Ti shape memory alloys
SO ACTA MATERIALIA
LA English
DT Article
DE Coherent precipitate; Elastic interaction; Nucleation; Aging effect;
Phase field simulation
ID CRYSTAL NI-AL; TI-NI; MICROSTRUCTURAL DEVELOPMENT; ORDERED
INTERMETALLICS; COMPUTER-SIMULATION; START TEMPERATURES; FIELD
SIMULATION; GROWTH-KINETICS; STRESS LEVELS; EVOLUTION
AB A new precipitate phase named P-phase has recently been identified in (Ni,Pt)Ti high temperature shape memory alloys. In order to understand the roles played by the fine coherent P-phase precipitates in determining the martensitic transformation temperature (M-s), strength of the B2 matrix phase, dimensional stability and shape memory effect of the alloys, a phase field model of P-phase precipitation is developed. Model inputs, including lattice parameters, precipitate matrix orientation relationship, elastic constants and free energy data, are obtained from experimental characterization, ab initio calculations and thermodynamic databases. Through computer simulations, the shape and spatial distribution of the P-phase precipitates, as well as the compositional and stress fields around them, are quantitatively determined. On this basis, the elastic interaction energy between the P-phase precipitates and a martenstic nucleus is calculated. It is found that both the chemical non-uniformity and stress field associated with the P-phase precipitates are in favor of the martensitic transformation. Their relative contributions to the increase in M-s temperature are quantified as a function of aging time and the result seems to agree with the experimental measurements. The shape and spatial distribution of the P-phase precipitates predicted by the simulations also agree well with experimental observations. (C) 2011 Acta Materialia Inc. Published by Elsevier Ltd. All rights reserved.
C1 [Gao, Y.; Zhou, N.; Yang, F.; Cui, Y.; Kovarik, L.; Mills, M. J.; Wang, Y.] Ohio State Univ, Dept Mat Sci & Engn, Columbus, OH 43210 USA.
[Hatcher, N.] Ruhr Univ Bochum, Interdisciplinary Ctr Adv Mat Simulat, Bochum, Germany.
[Noebe, R.] NASA, Glen Res Ctr, Cleveland, OH 44135 USA.
RP Wang, Y (reprint author), Ohio State Univ, Dept Mat Sci & Engn, 2041 Coll Rd,477 Watts Hall, Columbus, OH 43210 USA.
EM wang.363@osu.edu
RI Zhou, Ning/B-2624-2010; Wang, Yunzhi/B-2557-2010; Hatcher,
Nicholas/H-6450-2013; Mills, Michael/I-6413-2013; Kovarik,
Libor/L-7139-2016
OI Hatcher, Nicholas/0000-0001-7130-1618;
FU NASA; Supersonics Project (Dale Hopkins, API); NSF [DMRI008349]; US
Department of Energy, Office of Basic Energy Sciences [DE-SC0001258]
FX This work was supported by the NASA Fundamental Aeronautics Program,
Supersonics Project (Dale Hopkins, API), NSF under grant DMRI008349 (YW)
and US Department of Energy, Office of Basic Energy Sciences under grant
DE-SC0001258 (YG, FY and MJM).
NR 55
TC 22
Z9 23
U1 4
U2 58
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1359-6454
EI 1873-2453
J9 ACTA MATER
JI Acta Mater.
PD FEB
PY 2012
VL 60
IS 4
BP 1514
EP 1527
DI 10.1016/j.actamat.2011.11.043
PG 14
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA 914YK
UT WOS:000301989500008
ER
PT J
AU Mao, Z
Booth-Morrison, C
Sudbrack, CK
Martin, G
Seidman, DN
AF Mao, Zugang
Booth-Morrison, Christopher
Sudbrack, Chantal K.
Martin, Georges
Seidman, David N.
TI Kinetic pathways for phase separation: An atomic-scale study in Ni-Al-Cr
alloys
SO ACTA MATERIALIA
LA English
DT Article
DE Nickel-based superalloys; Kinetic pathways; Atom probe tomography;
Lattice kinetic Monte Carlo; Nanostructures
ID INITIO MOLECULAR-DYNAMICS; TOTAL-ENERGY CALCULATIONS; MONTE-CARLO
SIMULATIONS; WAVE BASIS-SET; AB-INITIO; PROBE TOMOGRAPHY; MULTICOMPONENT
ALLOYS; TEMPORAL EVOLUTION; SOLID-SOLUTIONS; LIQUID-METALS
AB The kinetic pathways involved in the formation of gamma'(Ll(2) structure)-precipitates during aging of concentrated Ni-Al-Cr alloys at 873 K, for three distinct alloy compositions, are studied experimentally by atom probe tomography, and computationally with lattice kinetic Monte Carlo (LKMC) simulations using parameters deduced from first-principles calculations of cohesive energies, and from experimental diffusion data. It is found that the compositional evolution of the gamma'-precipitate phase does not follow the predictions of a classical mean-field model for coarsening of precipitates in ternary alloys. LKMC simulations reveal that long-range vacancy solute binding plays a key role during the early stages of gamma'-precipitation. With the aid of Monte Carlo techniques using the parameters employed in the LKMC simulations, we compute the diffusion matrix in the terminal solid-solutions and demonstrate that key features of the observed kinetic pathways are the result of kinetic couplings among the diffusional fluxes. The latter are controlled by the long-range vacancy-solute binding energies. It is concluded that, because it neglects flux couplings, the classical mean-field approach to phase separation for a ternary alloy, despite its many qualitatively correct predictions, fails to describe quantitatively the true kinetic pathways that lead to phase separation in concentrated metallic alloys. (C) 2011 Published by Elsevier Ltd. on behalf of Acta Materialia Inc.
C1 [Mao, Zugang; Booth-Morrison, Christopher; Sudbrack, Chantal K.; Martin, Georges; Seidman, David N.] Northwestern Univ, Dept Mat Sci & Engn, Evanston, IL 60208 USA.
[Sudbrack, Chantal K.] NASA, Struct & Mat Div, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Martin, Georges] Cabinet Haut Commissaire, Commissariat Energie Atom, F-91191 Gif Sur Yvette, France.
[Seidman, David N.] Northwestern Univ, Ctr Atom Probe Tomog NUCAPT, 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-0241928]; NSF-MRI [DMR 0420532];
ONR-DURIP [N00014-0400798, N00014-0610539]
FX This research was sponsored by the National Science Foundation (NSF)
under Grant DMR-0241928, Dr. A.J. Ardell, grant monitor. Alloys were
processed at NASA Glenn Research Center courtesy of Dr. Ronald Noebe.
APT measurements were performed at the Northwestern University Center
for Atom Probe Tomography (NUCAPT). The LEAP tomograph was purchased
with initial funding from the NSF-MRI (DMR 0420532, Dr. Charles Bouldin,
grant officer) and ONR-DURIP (N00014-0400798, Dr. Julie Christodoulou,
grant officer) programs. Additionally, the LEAP tomograph was enhanced
with picosecond laser pulsing with funding from the ONR-DURIP
(N00014-0610539, J. Christodoulou, grant officer). We wish to thank
Prof. Pascal Bellon for discussions, Prof. Dieter Isheim for managing
NUCAPT, Dr. Stephen M. Foiles for his grand canonical Monte Carlo code,
and Dr. Carelyn Campbell for diffusivity databases.
NR 58
TC 18
Z9 18
U1 5
U2 43
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1359-6454
J9 ACTA MATER
JI Acta Mater.
PD FEB
PY 2012
VL 60
IS 4
BP 1871
EP 1888
DI 10.1016/j.actamat.2011.10.046
PG 18
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering
SC Materials Science; Metallurgy & Metallurgical Engineering
GA 914YK
UT WOS:000301989500042
ER
PT J
AU Marko, P
Nance, H
Dawson-Guynn, K
AF Marko, Peter
Nance, Holly
Dawson-Guynn, Kimberly
TI Seafood mislabeling: a response to Mariani
SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT
LA English
DT Letter
ID FISH
C1 [Marko, Peter] Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA.
[Nance, Holly] Florida Atlantic Univ, Harbor Branch Oceanog Inst, Ft Pierce, FL USA.
[Dawson-Guynn, Kimberly] NOAA, Natl Seafood Inspect Lab, Natl Marine Fisheries Serv, Pascagoula, MS USA.
RP Marko, P (reprint author), Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA.
EM pmarko@clemson.edu
NR 6
TC 0
Z9 0
U1 0
U2 11
PU ECOLOGICAL SOC AMER
PI WASHINGTON
PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA
SN 1540-9295
J9 FRONT ECOL ENVIRON
JI Front. Ecol. Environ.
PD FEB
PY 2012
VL 10
IS 1
BP 10
EP 11
DI 10.1890/12.WB.002
PG 2
WC Ecology; Environmental Sciences
SC Environmental Sciences & Ecology
GA 913GG
UT WOS:000301864000013
ER
PT J
AU Knuth, MA
Johnson, JB
Hopkins, MA
Sullivan, RJ
Moore, JM
AF Knuth, M. A.
Johnson, J. B.
Hopkins, M. A.
Sullivan, R. J.
Moore, J. M.
TI Discrete element modeling of a Mars Exploration Rover wheel in granular
material
SO JOURNAL OF TERRAMECHANICS
LA English
DT Article
DE Mars Exploration Rover; Discrete element method; Triaxial test; Lunar
regolith simulant
AB Three-dimensional discrete element method (DEM) simulations were developed for the Mars Exploration Rover (MER) mission to investigate: (1) rover wheel interactions with martian regolith; and (2) regolith deformation in a geotechnical triaxial strength cell (GTSC). These DEM models were developed to improve interpretations of laboratory and in situ rover data, and can simulate complicated regolith conditions. A DEM simulation was created of a laboratory experiment that involved a MER wheel digging into lunar regolith simulant. Sinkage and torques measured in the experiment were compared with those predicted numerically using simulated particles of increasing shape complexity (spheres, ellipsoids, and poly-ellipsoids). GTSC simulations, using the same model regolith used in the MER simulations, indicate a peak friction angle of approximately 37-38 degrees compared to internal friction angles of 36.5-37.7 degrees determined from the wheel digging experiments. Density of the DEM regolith was 1820 kg/m(3) compared to 1660 kg/m(3) for the lunar simulant used in the wheel digging experiment indicating that the number of grain contacts and grain contact resistance determined bulk strength in the DEM simulations, not density. An improved correspondence of DEM and actual test regolith densities is needed to simulate the evolution of regolith properties as density changes. Published by Elsevier Ltd. on behalf of ISTVS.
C1 [Knuth, M. A.; Hopkins, M. A.] USA, Engineer Res & Dev Ctr, Cold Reg Res & Engn Lab, Hanover, NH 03755 USA.
[Johnson, J. B.] Univ Alaska Fairbanks, Inst No Engn, Fairbanks, AK 99775 USA.
[Sullivan, R. J.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
[Moore, J. M.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA.
RP Knuth, MA (reprint author), USA, Engineer Res & Dev Ctr, Cold Reg Res & Engn Lab, 72 Lyme Rd, Hanover, NH 03755 USA.
EM Margaret.A.Knuth@usace.army.mil; jbjohnson5@alaska.edu;
Mark.A.Hopkins@usace.army.mil; rjs33@cornell.edu; jeffmoore@nasa.gov
FU NASA Lunar Science Institute; NASA's Kennedy Space Center; NASA MERPS
[NNH05ZDA001N]
FX This work was supported by the NASA Lunar Science Institute supported
project "Scientific Exploration Potential of the Lunar Poles", NASA's
Kennedy Space Center Technology Development project "Lunar regolith
mechanical properties, the NASA's Mars Fundamental Research Program
project "The relationship between the physical and mechanical properties
of Mars soils and their simulation", and the NASA Mars Exploration Rover
Program-NNH05ZDA001N-MERPS project "Physical and geologic Investigations
of the surface materials along the MER traverses.
NR 23
TC 20
Z9 21
U1 1
U2 18
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4898
J9 J TERRAMECHANICS
JI J. Terramech.
PD FEB
PY 2012
VL 49
IS 1
BP 27
EP 36
DI 10.1016/j.terra.2011.09.003
PG 10
WC Engineering, Environmental
SC Engineering
GA 913TO
UT WOS:000301900500003
ER
PT J
AU Braverman, AJ
Fetzer, EJ
Kahn, BH
Manning, EM
Oliphant, RB
Teixeira, JP
AF Braverman, Amy J.
Fetzer, Eric J.
Kahn, Brian H.
Manning, Evan M.
Oliphant, Robert B.
Teixeira, Joao P.
TI Massive Dataset Analysis for NASA's Atmospheric Infrared Sounder
SO TECHNOMETRICS
LA English
DT Article
DE Climate change; Data compression; Data reduction; Remote sensing;
Quantization
ID CONSTRAINED VECTOR QUANTIZATION
AB The National Aeronautics and Space Administration's (NASA) Atmospheric Infrared Sounder (AIRS) has been collecting large quantities of remote sensing data about the vertical structure of temperature, water vapor, and clouds in the Earth's atmosphere since its launch aboard the Aqua spacecraft in mid2002. These data are both global and high resolution, so they are uniquely able to provide distributional information about second- and higher-order interactions that are at the heart of understanding climate processes. However, these data are so large and complex that the structures of interest are not directly accessible without some form of data reduction, and data reduction is particularly problematic because of the way the data are staged and stored. Thus, AIRS data pose a classic problem in the analysis of modern massive datasets: how to quantify and understand global distributional relationships in datasets that are impossible to work with except in small pieces? Our approach is to hierarchically reduce the data in a way that preserves distributional characteristics across subsets formed by stratifying on intuitively meaningful variables. By exploring how distributions change as functions of the stratification variables, we gain insight into processes generating the data. In this article, we describe our implementation of methodology first proposed in two earlier papers. Here, we have operationalized the algorithm and demonstrated that it is both practical within the NASA data processing pipeline, and leads to important scientific insights that are only possible when massive datasets are reduced in a way that respects the structure of multivariate distributions.
C1 [Braverman, Amy J.; Fetzer, Eric J.; Kahn, Brian H.; Manning, Evan M.; Oliphant, Robert B.; Teixeira, Joao P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Braverman, AJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Amy.Braverman@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX The research described in this article was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration. The
NCEP Reanalysis Pressure level data are provided by the NOAA/OAR/ESRL
PSD, Boulder, CO.
NR 15
TC 2
Z9 2
U1 0
U2 1
PU AMER STATISTICAL ASSOC
PI ALEXANDRIA
PA 732 N WASHINGTON ST, ALEXANDRIA, VA 22314-1943 USA
SN 0040-1706
J9 TECHNOMETRICS
JI Technometrics
PD FEB
PY 2012
VL 54
IS 1
BP 1
EP 15
DI 10.1080/00401706.2012.650504
PG 15
WC Statistics & Probability
SC Mathematics
GA 914QZ
UT WOS:000301967900001
ER
PT J
AU Wong, AR
Toftul, A
Polzin, KA
Pearson, JB
AF Wong, Andrea R.
Toftul, Alexandra
Polzin, Kurt A.
Pearson, J. Boise
TI Non-contact thrust stand calibration method for repetitively pulsed
electric thrusters
SO REVIEW OF SCIENTIFIC INSTRUMENTS
LA English
DT Article
ID PERFORMANCE
AB A thrust stand calibration technique for use in testing repetitively pulsed electric thrusters for in-space propulsion has been developed and tested using a modified hanging pendulum thrust stand. In the implementation of this technique, current pulses are applied to a solenoid to produce a pulsed magnetic field that acts against a permanent magnet mounted to the thrust stand pendulum arm. The force on the magnet is applied in this non-contact manner, with the entire pulsed force transferred to the pendulum arm through a piezoelectric force transducer to provide a time-accurate force measurement. Modeling of the pendulum arm dynamics reveals that after an initial transient in thrust stand motion the quasi-steady average deflection of the thrust stand arm away from the unforced or "zero" position can be related to the average applied force through a simple linear Hooke's law relationship. Modeling demonstrates that this technique is universally applicable except when the pulsing period is increased to the point where it approaches the period of natural thrust stand motion. Calibration data were obtained using a modified hanging pendulum thrust stand previously used for steady-state thrust measurements. Data were obtained for varying impulse bit at constant pulse frequency and for varying pulse frequency. The two data sets exhibit excellent quantitative agreement with each other. The overall error on the linear regression fit used to determine the calibration coefficient was roughly %. (C) 2012 American Institute of Physics. [doi:10.1063/1.3680557]
C1 [Wong, Andrea R.; Toftul, Alexandra; Polzin, Kurt A.; Pearson, J. Boise] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Wong, AR (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
EM kurt.a.polzin@nasa.gov
FU NASA
FX We appreciate the continued management support of Mr. Jim Martin and Ms.
Mary Beth Koelbl and the continued academic affairs support of Ms. Mona
Miller and Ms. Tina Haymaker. We gratefully acknowledge the
contributions and support during the course of this effort by Tommy
Reid, Doug Galloway, Ashley Hallock, Derek Mayer, Adam Kimberlin, and
Kevin Bonds. This program was supported under NASA's Advanced In-Space
Propulsion program managed by Dr. Michael LaPointe.
NR 8
TC 2
Z9 2
U1 0
U2 4
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 FEB
PY 2012
VL 83
IS 2
AR 025103
DI 10.1063/1.3680557
PN 1
PG 7
WC Instruments & Instrumentation; Physics, Applied
SC Instruments & Instrumentation; Physics
GA 909LS
UT WOS:000301566600053
PM 22380121
ER
PT J
AU Meador, MAB
Malow, EJ
Silva, R
Wright, S
Quade, D
Vivod, SL
Guo, HQ
Guo, J
Cakmak, M
AF Meador, Mary Ann B.
Malow, Ericka J.
Silva, Rebecca
Wright, Sarah
Quade, Derek
Vivod, Stephanie L.
Guo, Haiquan
Guo, Jiao
Cakmak, Miko
TI Mechanically Strong, Flexible Polyimide Aerogels Cross-Linked with
Aromatic Triamine
SO ACS APPLIED MATERIALS & INTERFACES
LA English
DT Article
DE aerogel; polyimide; cross-linking; nanoporous materials; high
temperature insulation
ID MODIFIED SILICA AEROGELS; TEMPERATURE POLYMERS; ELASTIC PROPERTIES;
LAYERS
AB Polyimide gels are produced by cross-linking anhydride capped polyamic acid oligomers with aromatic triamine in solution and chemically imidizing. The gels are then supercritically dried to form nanoporous polyimide aerogels with densities as low as 0.14 g/cm(3) and surface areas as high as 512 m(2)/g. To understand the effect of the polyimide backbone on properties, aerogels from several combinations of diamine and dianhydride, and formulated oligomer chain length are examined. Formulations made from 2,2'-dimethylbenzidine as the diamine shrink the least but have among the highest compressive modulus. Formulations made using 4,4'-oxydianiline or 2,2'dimethylbenzidine can be fabricated into continuous thin films using a roll to roll casting process. The films are flexible enough to be rolled or folded back on themselves and recover completely without cracking or flaking, and have tensile strengths of 4-9 MPa. Finally, the highest onset of decomposition (above 600 degrees C) of the polyimide aerogels was obtained using p-phenylene diamine as the backbone diamine with either dianhydride studied. All of the aerogels are suitable candidates for high-temperature insulation with glass transition temperatures ranging from 270-340 degrees C and onsets of decomposition from 460-610 degrees C.
C1 [Meador, Mary Ann B.; Malow, Ericka J.; Silva, Rebecca; Wright, Sarah; Vivod, Stephanie L.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Quade, Derek; Guo, Haiquan] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
[Guo, Jiao; Cakmak, Miko] Univ Akron, Akron, OH 44325 USA.
RP Meador, MAB (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
EM maryann.meador@nasa.gov
OI Meador, Mary Ann/0000-0003-2513-7372
FU NASA; Third Frontier Program of the State of Ohio
FX We thank the NASA Fundamental Aeronautics Program (Hypersonics) for
financial support of this research. In addition, we thank Dan Schieman
(ARSC) for helium pycnometry measurements and thermal analysis, Linda
McCorkle (Ohio Aerospace Institute) for SEM images, and Anna Palczer for
nitrogen sorption measurements. We also thank the Third Frontier Program
of the State of Ohio for funding the construction of the roll to roll
film manufacturing line.
NR 34
TC 75
Z9 81
U1 25
U2 156
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1944-8244
J9 ACS APPL MATER INTER
JI ACS Appl. Mater. Interfaces
PD FEB
PY 2012
VL 4
IS 2
BP 536
EP 544
DI 10.1021/am2014635
PG 9
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary
SC Science & Technology - Other Topics; Materials Science
GA 897IW
UT WOS:000300644500007
PM 22233638
ER
PT J
AU Lin, Y
Bunker, CE
Fernando, KAS
Connell, JW
AF Lin, Yi
Bunker, Christopher E.
Fernando, K. A. Shiral
Connell, John W.
TI Aqueously Dispersed Silver Nanoparticle-Decorated Boron Nitride
Nanosheets for Reusable, Thermal Oxidation-Resistant Surface Enhanced
Raman Spectroscopy (SERS) Devices
SO ACS APPLIED MATERIALS & INTERFACES
LA English
DT Article
DE boron nitride nanosheets; nanometal decoration; reusable; SERS; wet
transfer
ID CARBON NANOTUBES; GRAPHENE OXIDE; METAL NANOPARTICLES; PHOTOCATALYTIC
REDUCTION; ANCHORING SEMICONDUCTOR; SCATTERING; FILM; GOLD; LAYER;
NANORIBBONS
AB The impurity-free aqueous dispersions of boron nitride nanosheets (BNNS) allowed the facile preparation of silver (Ag) nanoparticle-decorated BNNS by chemical reduction of an Ag salt with hydrazine. in the presence of BNNS. The resultant Ag BNNS nanohybrids remained dispersed in water, allowing convenient subsequent solution processing. By using substrate transfer techniques, Ag BNNS nanohybrid thin film coatings on quartz substrates were prepared and evaluated as reusable surface enhanced Raman spectroscopy (SERS) sensors that were robust against repeated solvent washing. In addition, because ofthe unique thermal oxidation-resistant properties of the BNNS, the sensor devices may be readily recycled by short-duration high temperature air oxidation to remove residual analyte molecules in repeated runs. The limiting factor associated with the thermal oxidation recycling process was the Ostwald ripening effect of Ag nanostructures.
C1 [Lin, Yi] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Bunker, Christopher E.] USAF, Prop Directorate, Res Lab, Wright Patterson AFB, OH 45433 USA.
[Fernando, K. A. Shiral] Univ Dayton, Res Inst, Nanotechnol Grp, Dayton, OH 45433 USA.
[Connell, John W.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA.
RP Lin, Y (reprint author), Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA.
EM yi.lin-1@nasa.gov; christopher.bunker@wpafb.af.mil;
john.w.connell@nasa.gov
NR 64
TC 64
Z9 65
U1 7
U2 144
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1944-8244
J9 ACS APPL MATER INTER
JI ACS Appl. Mater. Interfaces
PD FEB
PY 2012
VL 4
IS 2
BP 1110
EP 1117
DI 10.1021/am201747d
PG 8
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary
SC Science & Technology - Other Topics; Materials Science
GA 897IW
UT WOS:000300644500088
PM 22280102
ER
PT J
AU Vadrevu, KP
Ellicott, E
Giglio, L
Badarinath, KVS
Vermote, E
Justice, C
Lau, WKM
AF Vadrevu, Krishna Prasad
Ellicott, Evan
Giglio, Louis
Badarinath, K. V. S.
Vermote, Eric
Justice, Chris
Lau, William K. M.
TI Vegetation fires in the himalayan region - Aerosol load, black carbon
emissions and smoke plume heights
SO ATMOSPHERIC ENVIRONMENT
LA English
DT Article
DE Vegetation fires; Biomass burnt; Emissions; India
ID SATELLITE-OBSERVATIONS; INJECTION HEIGHTS; OPTICAL DEPTH; MODIS;
ALGORITHM; CALIPSO; INDIA; LIDAR
AB In this study, we investigate the potential of multi-satellite datasets for quantifying the biomass burning emissions from the Himalayan region. A variety of satellite products were used for characterizing fire events including active fire counts, burnt areas, aerosol optical depth (AOD) variations, aerosol index and smoke plume heights. Results from the MODerate-resolution Imaging Spectroradiometer (MODIS) fire product suggest March June as the major fire season with the peak during the April. An average of 3908 fire counts per year were recorded with sixty four percent of the fires occurring in the low elevation areas in the Himalayan Region. We estimate average burnt areas of 1129 sq. km, with the black carbon emissions of 431 Mg, per year. The mean AOD (2005-2010) was 0.287 +/- 0.105 (one sigma) with peak values in May. Correlation analysis between the fire counts and AOD resulted in a Pearson correlation coefficient of 0.553; the correlation between the FRP and AOD is relatively weaker (r = 0.499). Planetary boundary layer height retrieved from the Modern Era Retrospective-Analysis For Research And Applications (MERRA) product suggests typical PBL height of 1000-1200 m during the April-May peak biomass burning season. Cloud-Aerosol Lidar Orthogonal Polarisation (CALIOP) retrievals show the extent of smoke plume heights beyond the planetary boundary layer during the peak biomass burning month of April. However, comparison of fires in the Himalayan region with other regions and comparisons to aerosol index data from the Ozone Monitoring Instrument (OM!) suggest smoke plumes reaching less than 3 km. Our results on fires and smoke plume height relationships provide valuable information for addressing aerosol transport in the region. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Vadrevu, Krishna Prasad; Ellicott, Evan; Giglio, Louis; Vermote, Eric; Justice, Chris] Univ Maryland, Dept Geog, College Pk, MD 20740 USA.
[Badarinath, K. V. S.] Natl Remote Sensing Ctr, Atmospher Sci Sect, Hyderabad 500625, Andhra Pradesh, India.
[Lau, William K. M.] NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA.
RP Vadrevu, KP (reprint author), Univ Maryland, Dept Geog, College Pk, MD 20740 USA.
EM krisvkp@yahoo.com
RI Vermote, Eric/K-3733-2012; Lau, William /E-1510-2012;
OI Lau, William /0000-0002-3587-3691; Vadrevu, Krishna/0000-0003-4407-5605
FU NASA [NNX10AU77G]
FX We thank product developers of MODIS active fires and burnt areas in
addition to ATSR, MERIS, MERRA, OMI and CALIPSO datasets. This research
was supported by NASA grant NNX10AU77G.
NR 47
TC 40
Z9 40
U1 4
U2 26
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1352-2310
J9 ATMOS ENVIRON
JI Atmos. Environ.
PD FEB
PY 2012
VL 47
BP 241
EP 251
DI 10.1016/j.atmosenv.2011.11.009
PG 11
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 903XY
UT WOS:000301157700027
ER
PT J
AU Stenger, MB
Evans, JM
Knapp, CF
Lee, SMC
Phillips, TR
Perez, SA
Moore, AD
Paloski, WH
Platts, SH
AF Stenger, Michael B.
Evans, Joyce M.
Knapp, Charles F.
Lee, Stuart M. C.
Phillips, Tiffany R.
Perez, Sondra A.
Moore, Alan D., Jr.
Paloski, William H.
Platts, Steven H.
TI Artificial gravity training reduces bed rest-induced cardiovascular
deconditioning
SO EUROPEAN JOURNAL OF APPLIED PHYSIOLOGY
LA English
DT Article
DE Cardiovascular regulation; Neuroendocrine; Spectral power; Hypergravity;
Peak oxygen consumption
ID POWER SPECTRAL-ANALYSIS; HEAD-DOWN TILT; ORTHOSTATIC INTOLERANCE;
SPACE-FLIGHT; EXERCISE PERFORMANCE; DURATION SPACEFLIGHT;
ARTERIAL-PRESSURE; MAXIMAL EXERCISE; UPRIGHT EXERCISE; AMBULATORY MEN
AB We studied 15 men (8 treatment, 7 control) before and after 21 days of 6 head-down tilt to determine whether daily, 1-h exposures to 1.0 G(z) (at the heart) artificial gravity (AG) would prevent bed rest-induced cardiovascular deconditioning. Testing included echocardiographic analysis of cardiac function, plasma volume (PV), aerobic power (VO(2)pk) and cardiovascular and neuroendocrine responses to 80 degrees head-up tilt (HUT). Data collected during HUT were ECG, stroke volume (SV), blood pressure (BP) and blood for catecholamines and vasoactive hormones. Heart rate (HR), cardiac output (CO), total peripheral resistance, and spectral power of BP and HR were calculated. Bed rest decreased PV, supine and HUT SV, and indices of cardiac function in both groups. Although PV was decreased in control and AG after bed rest, AG attenuated the decrease in orthostatic tolerance [pre- to post-bed rest change; control: -11.8 +/- 2.0, AG: -6.0 +/- 2.8 min (p = 0.012)] and VO(2)pk [pre- to post-bed rest change; control: -0.39 +/- 0.11, AG: -0.17 +/- 0.06 L/min (p = 0.041)]. AG prevented increases in pre-tilt levels of plasma renin activity [pre- to post-bed rest change; control: 1.53 +/- 0.23, AG: -0.07 +/- 0.34 ng/mL/h (p = 0.001)] and angiotensin II [pre- to post-bed rest change; control: 3.00 +/- 1.04, AG: -0.63 +/- 0.81 pg/mL (p = 0.009)] and increased HUT aldosterone [post-bed rest; control: 107 +/- 30 pg/mL, AG: 229 +/- 68 pg/mL (p = 0.045)] and norepinephrine [post-bed rest; control: 453 +/- 107, AG: 732 +/- 131 pg/mL (p = 0.003)]. We conclude that AG can mitigate some aspects of bed rest-induced cardiovascular deconditioning, including orthostatic intolerance and aerobic power. Mechanisms of improvement were not cardiac-mediated, but likely through improved sympathetic responsiveness to orthostatic stress.
C1 [Stenger, Michael B.; Lee, Stuart M. C.; Phillips, Tiffany R.; Perez, Sondra A.; Moore, Alan D., Jr.] NASA, Lyndon B Johnson Space Ctr, Cardiovasc Lab, Wyle Integrated Sci & Engn Grp, Houston, TX 77058 USA.
[Evans, Joyce M.; Knapp, Charles F.] Univ Kentucky, Ctr Biomed Engn, Lexington, KY 40506 USA.
[Paloski, William H.; Platts, Steven H.] NASA JSC, Human Adaptat & Countermeasures Div, Houston, TX 77058 USA.
[Paloski, William H.] Univ Houston, Dept Hlth & Human Performance, Houston, TX 77204 USA.
RP Stenger, MB (reprint author), NASA, Lyndon B Johnson Space Ctr, Cardiovasc Lab, Wyle Integrated Sci & Engn Grp, Houston, TX 77058 USA.
EM michael.b.stenger@nasa.gov
FU UTMB GCRC; NASA; NIH [M01 RR 0073]
FX The authors gratefully acknowledge the support of the UTMB GCRC nursing
staff, the Short Radius Centrifuge team, the subjects who participated
in the study and JSC Cardiovascular Laboratory team members that
participated in data collection and reduction, particularly Christine
Ribeiro, Shang-Jin Shi, Ph.D., Timothy Matz, David Martin, and Natalia
Arzeno-Gonzalez. We would also like to thank Alan Feiveson, Ph.D., for
statistical support. This study was supported by the NASA Human Research
Program, and conducted at the NIH-funded [M01 RR 0073] GCRC at UTMB,
Galveston, TX.
NR 63
TC 17
Z9 18
U1 0
U2 14
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 FEB
PY 2012
VL 112
IS 2
BP 605
EP 616
DI 10.1007/s00421-011-2005-1
PG 12
WC Physiology; Sport Sciences
SC Physiology; Sport Sciences
GA 909LZ
UT WOS:000301567300021
PM 21626041
ER
PT J
AU Pe'er, A
Zhang, BB
Ryde, F
McGlynn, S
Zhang, B
Preece, RD
Kouveliotou, C
AF Pe'er, Asaf
Zhang, Bin-Bin
Ryde, Felix
McGlynn, Sinead
Zhang, Bing
Preece, Robert D.
Kouveliotou, Chryssa
TI The connection between thermal and non-thermal emission in gamma-ray
bursts: general considerations and GRB090902B as a case study
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE plasmas; radiation mechanisms: thermal; radiative transfer; scattering;
gamma-ray burst: general
ID INTERNAL SHOCK MODEL; HIGH-ENERGY EMISSION; SELF-COMPTON EMISSION; SCALE
MAGNETIC-FIELDS; PROMPT EMISSION; X-RAY; SYNCHROTRON EMISSION;
PHOTOSPHERIC EMISSION; PHYSICAL PARAMETERS; SPECTRAL PROPERTIES
AB Photospheric (thermal) emission is inherent to the gamma-ray burst (GRB) 'fireball' model. We show here that inclusion of this component in the analysis of the GRB prompt emission phase naturally explains some of the prompt GRB spectra seen by the Fermi satellite over its entire energy band. The sub-MeV peak is explained as multicolour blackbody emission, and the high-energy tail, extending up to the GeV band, results from roughly similar contributions of synchrotron emission, synchrotron self-Compton and Comptonization of the thermal photons by energetic electrons originating after dissipation of the kinetic energy above the photosphere. We show how this analysis method results in a complete, self-consistent picture of the physical conditions at both emission sites of the thermal and non-thermal radiation. We study the connection between the thermal and non-thermal parts of the spectrum, and show how the values of the free model parameters are deduced from the data. We demonstrate our analysis method on GRB090902B: we deduce a Lorentz factor in the range 920 <= eta <= 1070, photospheric radius r(ph) similar or equal to 7.2-8.4 x 10(11) cm and dissipation radius r(gamma) >= 3.5-4.1 x 10(15) cm. By comparison to afterglow data, we deduce that a large fraction epsilon(d) approximate to 85-95 per cent of the kinetic energy is dissipated, and that a large fraction, similar to equipartition of this energy, is carried by the electrons and the magnetic field. This high value of epsilon(d) questions the 'internal shock' scenario as the main energy dissipation mechanism for this GRB.
C1 [Pe'er, Asaf] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Pe'er, Asaf] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Zhang, Bin-Bin; Zhang, Bing] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA.
[Ryde, Felix; McGlynn, Sinead] Royal Inst Technol, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden.
[Preece, Robert D.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Kouveliotou, Chryssa] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
RP Pe'er, A (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM apeer@cfa.harvard.edu
RI Zhang, Binbin/C-9035-2013;
OI Zhang, Binbin/0000-0003-2002-116X; Preece, Robert/0000-0003-1626-7335
FU Space Telescope Science Institute; Fermi grant [31014]; Swedish National
Space Board
FX This research was supported by the Riccardo Giacconi Fellowship award of
the Space Telescope Science Institute, and Fermi grant award #31014. FR
acknowledges financial support by the Swedish National Space Board. AP
wishes to thank Dale Frail, Jeremy Schnittman, Andy Fruchter, Kuntal
Misra, Zeljka Bosnjak, Mario Livio and Kailash Sahu for useful
discussions.
NR 98
TC 52
Z9 52
U1 0
U2 5
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD FEB
PY 2012
VL 420
IS 1
BP 468
EP 482
DI 10.1111/j.1365-2966.2011.20052.x
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 905PL
UT WOS:000301284600053
ER
PT J
AU Ackermann, M
Ajello, M
Allafort, A
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Belfiore, A
Bellazzini, R
Berenji, B
Blandford, RD
Bloom, ED
Bonamente, E
Borgland, AW
Bottacini, E
Bregeon, J
Brigida, M
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caraveo, PA
Casandjian, JM
Cecchi, C
Chekhtman, A
Ciprini, S
Claus, R
Cohen-Tanugi, J
de Angelis, A
de Palma, F
Dermer, CD
Silva, EDE
Drell, PS
Dumora, D
Favuzzi, C
Fegan, SJ
Focke, WB
Fortin, P
Fukazawa, Y
Fusco, P
Gargano, F
Germani, S
Giglietto, N
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Guillemot, L
Guiriec, S
Hadasch, D
Hanabata, Y
Harding, AK
Hayashida, M
Hayashi, K
Hays, E
Johannesson, G
Johnson, AS
Kamae, T
Katagiri, H
Kataoka, J
Kerr, M
Knodlseder, J
Kuss, M
Lande, J
Latronico, L
Lee, SH
Longo, F
Loparco, F
Lott, B
Lovellette, MN
Lubrano, P
Martin, P
Mazziotta, MN
McEnery, JE
Mehault, J
Michelson, PF
Mitthumsiri, W
Mizuno, T
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Naumann-Godo, M
Nolan, PL
Norris, JP
Nuss, E
Ohsugi, T
Okumura, A
Omodei, N
Orlando, E
Ormes, JF
Ozaki, M
Paneque, D
Parent, D
Pesce-Rollins, M
Pierbattista, M
Piron, F
Porter, TA
Raino, S
Rando, R
Razzano, M
Reimer, O
Reposeur, T
Ritz, S
Parkinson, PMS
Sgro, C
Siskind, EJ
Smith, PD
Spinelli, P
Strong, AW
Takahashi, H
Tanaka, T
Thayer, JG
Thayer, JB
Thompson, DJ
Tibaldo, L
Torres, DF
Tosti, G
Tramacere, A
Troja, E
Uchiyama, Y
Vandenbroucke, J
Vasileiou, V
Vianello, G
Vitale, V
Waite, AP
Wang, P
Winer, BL
Wood, KS
Yang, Z
Zimmer, S
Bontemps, S
AF Ackermann, M.
Ajello, M.
Allafort, A.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Belfiore, A.
Bellazzini, R.
Berenji, B.
Blandford, R. D.
Bloom, E. D.
Bonamente, E.
Borgland, A. W.
Bottacini, E.
Bregeon, J.
Brigida, M.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caraveo, P. A.
Casandjian, J. M.
Cecchi, C.
Chekhtman, A.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
de Angelis, A.
de Palma, F.
Dermer, C. D.
do Couto e Silva, E.
Drell, P. S.
Dumora, D.
Favuzzi, C.
Fegan, S. J.
Focke, W. B.
Fortin, P.
Fukazawa, Y.
Fusco, P.
Gargano, F.
Germani, S.
Giglietto, N.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Guillemot, L.
Guiriec, S.
Hadasch, D.
Hanabata, Y.
Harding, A. K.
Hayashida, M.
Hayashi, K.
Hays, E.
Johannesson, G.
Johnson, A. S.
Kamae, T.
Katagiri, H.
Kataoka, J.
Kerr, M.
Knoedlseder, J.
Kuss, M.
Lande, J.
Latronico, L.
Lee, S. -H.
Longo, F.
Loparco, F.
Lott, B.
Lovellette, M. N.
Lubrano, P.
Martin, P.
Mazziotta, M. N.
McEnery, J. E.
Mehault, J.
Michelson, P. F.
Mitthumsiri, W.
Mizuno, T.
Monte, C.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Naumann-Godo, M.
Nolan, P. L.
Norris, J. P.
Nuss, E.
Ohsugi, T.
Okumura, A.
Omodei, N.
Orlando, E.
Ormes, J. F.
Ozaki, M.
Paneque, D.
Parent, D.
Pesce-Rollins, M.
Pierbattista, M.
Piron, F.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Reimer, O.
Reposeur, T.
Ritz, S.
Parkinson, P. M. Saz
Sgro, C.
Siskind, E. J.
Smith, P. D.
Spinelli, P.
Strong, A. W.
Takahashi, H.
Tanaka, T.
Thayer, J. G.
Thayer, J. B.
Thompson, D. J.
Tibaldo, L.
Torres, D. F.
Tosti, G.
Tramacere, A.
Troja, E.
Uchiyama, Y.
Vandenbroucke, J.
Vasileiou, V.
Vianello, G.
Vitale, V.
Waite, A. P.
Wang, P.
Winer, B. L.
Wood, K. S.
Yang, Z.
Zimmer, S.
Bontemps, S.
TI The cosmic-ray and gas content of the Cygnus region as measured in
gamma-rays by the Fermi Large Area Telescope
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: abundances; ISM: clouds; cosmic rays; gamma rays: ISM
ID BLIND FREQUENCY SEARCHES; GALACTIC PLANE SURVEY; MILKY-WAY; SUPERNOVA
REMNANT; INFRARED-EMISSION; MOLECULAR CLOUDS; DARK GAS; OUTER GALAXY;
X-RAY; H-I
AB Context. The Cygnus region hosts a giant molecular-cloud complex that actively forms massive stars. Interactions of cosmic rays with interstellar gas and radiation fields make it shine at gamma-ray energies. Several gamma-ray pulsars and other energetic sources are seen in this direction.
Aims. In this paper we analyze the gamma-ray emission measured by the Fermi Large Area Telescope (LAT) in the energy range from 100 MeV to 100 GeV in order to probe the gas and cosmic-ray content on the scale of the whole Cygnus complex. The gamma-ray emission on the scale of the central massive stellar clusters and from individual sources is addressed elsewhere.
Methods. The signal from bright pulsars is greatly reduced by selecting photons in their off-pulse phase intervals. We compare the diffuse gamma-ray emission with interstellar gas maps derived from radio/mm-wave lines and visual extinction data. A general model of the region, including other pulsars and gamma-ray sources, is sought.
Results. The integral HI emissivity above 100 MeV averaged over the whole Cygnus complex amounts to [2.06 +/- 0.11 (stat.) (+0.15)(-0.84) (syst.)] x 10(-26) photons s(-1) sr(-1) H-atom(-1), where the systematic error is dominated by the uncertainty on the HI opacity to calculate its column densities. The integral emissivity and its spectral energy distribution are both consistent within the systematics with LAT measurements in the interstellar space near the solar system. The average X-CO = N(H-2)/W-CO ratio is found to be [1.68 +/- 0.05 (stat.) (+0.87)(-0.10) (H I opacity)] x 10(20) molecules cm(-2) (K km s(-1))(-1), consistent with other LAT measurements in the Local Arm. We detect significant gamma-ray emission from dark neutral gas for a mass corresponding to similar to 40% of what is traced by CO. The total interstellar mass in the Cygnus complex inferred from its gamma-ray emission amounts to 8 (+5)(-1) x 10(6) M-circle dot at a distance of 1.4 kpc.
Conclusions. Despite the conspicuous star formation activity and high masses of the interstellar clouds, the cosmic-ray population in the Cygnus complex averaged over a few hundred parsecs is similar to that of the local interstellar space.
C1 [Ackermann, M.; Ajello, M.; Allafort, A.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Focke, W. B.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Kerr, M.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, O.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Tramacere, A.; Uchiyama, Y.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Ackermann, M.; Ajello, M.; Allafort, A.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Focke, W. B.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Kerr, M.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, O.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Tramacere, A.; Uchiyama, Y.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Latronico, L.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Naumann-Godo, M.; Pierbattista, M.; Tibaldo, L.] Univ Paris Diderot, CEA Saclay, Serv Astrophys, Lab AIM,CEA,IRFU,CNRS, F-91191 Gif Sur Yvette, France.
[Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Belfiore, A.; Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bruel, P.; Fegan, S. J.; Fortin, P.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Caliandro, G. A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEE CSIC, Barcelona 08193, Spain.
[Chekhtman, A.] Artep Inc, Ellicott City, MD 21042 USA.
[Ciprini, S.] ASI Sci Data Ctr, I-00044 Rome, Italy.
[Cohen-Tanugi, J.; Mehault, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier, Montpellier, France.
[de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy.
[Dermer, C. D.; Lovellette, M. N.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Dumora, D.; Lott, B.; Reposeur, T.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
[Fukazawa, Y.; Hanabata, Y.; Hayashi, K.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Guiriec, S.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Harding, A. K.; Hays, E.; McEnery, J. E.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Katagiri, H.] Ibaraki Univ, Coll Sci, Bunkyo Ku, Mito, Ibaraki 3108512, Japan.
[Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Knoedlseder, J.] IRAP, CNRS, F-31028 Toulouse 4, France.
[Knoedlseder, J.] Univ Toulouse, UPS, OMP, IRAP, Toulouse, France.
[Lee, S. -H.] Kyoto Univ, Yukawa Inst Theoret Phys, Sakyo Ku, Kyoto 6068502, Japan.
[Martin, P.; Orlando, E.; Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Norris, J. P.] Boise State Univ, Dept Phys, Boise, ID 83725 USA.
[Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Okumura, A.; Ozaki, M.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Parent, D.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA.
[Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Ritz, S.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Ritz, S.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Smith, P. D.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Tramacere, A.; Vianello, G.] CIFS, I-10133 Turin, Italy.
[Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland.
[Troja, E.] NASA, Postdoctoral Program, Greenbelt, MD 20771 USA.
[Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Yang, Z.; Zimmer, S.] Stockholm Univ, Dept Phys, S-10691 Stockholm, Sweden.
[Yang, Z.; Zimmer, S.] Oskar Klein Ctr Cosmoparticle Phys, S-10691 Stockholm, Sweden.
[Bontemps, S.] Univ Bordeaux, CNRS, INSU, Lab Astrophys Bordeaux, Floirac, France.
RP Ackermann, M (reprint author), Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
EM isabelle.grenier@cea.fr; luigi.tibaldo@pd.infn.it
RI Thompson, David/D-2939-2012; Harding, Alice/D-3160-2012; Hays,
Elizabeth/D-3257-2012; McEnery, Julie/D-6612-2012; Baldini,
Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Tosti,
Gino/E-9976-2013; Saz Parkinson, Pablo Miguel/I-7980-2013; Ozaki,
Masanobu/K-1165-2013; Morselli, Aldo/G-6769-2011; Kuss,
Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Reimer,
Olaf/A-3117-2013; Rando, Riccardo/M-7179-2013; Loparco,
Francesco/O-8847-2015; Johannesson, Gudlaugur/O-8741-2015; Gargano,
Fabio/O-8934-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario
/O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016;
Orlando, E/R-5594-2016;
OI Thompson, David/0000-0001-5217-9135; lubrano,
pasquale/0000-0003-0221-4806; Morselli, Aldo/0000-0002-7704-9553;
giglietto, nicola/0000-0002-9021-2888; Reimer, Olaf/0000-0001-6953-1385;
Loparco, Francesco/0000-0002-1173-5673; Johannesson,
Gudlaugur/0000-0003-1458-7036; Gargano, Fabio/0000-0002-5055-6395;
Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario
/0000-0001-9325-4672; Torres, Diego/0000-0002-1522-9065; Giordano,
Francesco/0000-0002-8651-2394; De Angelis,
Alessandro/0000-0002-3288-2517; Caraveo, Patrizia/0000-0003-2478-8018;
Sgro', Carmelo/0000-0001-5676-6214; Rando, Riccardo/0000-0001-6992-818X
FU National Aeronautics and Space Administration; Department of Energy in
the US; Commissariat a l'Energie Atomique; Centre National de la
Recherche Scientifique/Institut National de Physique Nucleaire et de
Physique des Particules in France; Agenzia Spaziale Italiana; Istituto
Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture,
Sports, Science and Technology (MEXT); High Energy Accelerator Research
Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan;
K. A. Wallenberg Foundation; Swedish Research Council; Swedish National
Space Board in Sweden; Istituto Nazionale di Astrofisica in Italy;
Centre National d'Etudes Spatiales in France; Natural Sciences and
Engineering Research Council of Canada
FX The Fermi LAT Collaboration acknowledges generous ongoing support from a
number of agencies and institutes that have supported both the
development and the operation of the LAT, as well as scientific data
analysis. These include the National Aeronautics and Space
Administration and the Department of Energy in the US, the Commissariat
a l'Energie Atomique and the Centre National de la Recherche
Scientifique/Institut National de Physique Nucleaire et de Physique des
Particules in France, the Agenzia Spaziale Italiana and the Istituto
Nazionale di Fisica Nucleare in Italy, the Ministry of Education,
Culture, Sports, Science and Technology (MEXT), High Energy Accelerator
Research Organization (KEK) and Japan Aerospace Exploration Agency
(JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish
Research Council, and the Swedish National Space Board in Sweden.
Additional support for science analysis during the operations phase is
gratefully acknowledged from the Istituto Nazionale di Astrofisica in
Italy and the Centre National d'Etudes Spatiales in France. We made use
of data from the Canadian Galactic Plane Survey (CGPS). CGPS is a
Canadian project with international partners. The Dominion Radio
Astrophysical Observatory is operated as a national facility by the
National Research Council of Canada. The CGPS is supported by a grant
from the Natural Sciences and Engineering Research Council of Canada. We
thank T. M. Dame for providing the moment-masked CO data.
NR 72
TC 17
Z9 17
U1 0
U2 6
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 FEB
PY 2012
VL 538
AR A71
DI 10.1051/0004-6361/201117539
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 897AX
UT WOS:000300614100071
ER
PT J
AU Blanchard, JM
Lovell, JEJ
Ojha, R
Kadler, M
Dickey, JM
Edwards, PG
AF Blanchard, J. M.
Lovell, J. E. J.
Ojha, R.
Kadler, M.
Dickey, J. M.
Edwards, P. G.
TI High resolution rapid response observations of compact radio sources
with the Ceduna Hobart Interferometer (CHI)
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE instrumentation: interferometers; galaxies: jets; quasars: general;
galaxies: active; galaxies: nuclei; gamma rays: galaxies
ID ACTIVE GALACTIC NUCLEI; SCINTILLATION-INDUCED VARIABILITY; VLBI;
QUASARS; JETS; CAPABILITIES; TELESCOPE; BLAZARS; OBJECTS
AB Context. Frequent, simultaneous observations across the electromagnetic spectrum are essential to the study of a range of astrophysical phenomena including active galactic nuclei. A key tool of such studies is the ability to observe an object when it flares i.e. exhibits a rapid and significant increase in its flux density.
Aims. We describe the specific observational procedures and the calibration techniques that have been developed and tested to create a single baseline radio interferometer that can rapidly observe a flaring object. This is the only facility that is dedicated to rapid high resolution radio observations of an object south of -30 degrees declination. An immediate application is to provide rapid contemporaneous radio coverage of AGN flaring at gamma-ray frequencies detected by the Fermi Gamma-ray Space Telescope.
Methods. A single baseline interferometer, the Ceduna Hobart Interferometer (CHI), was formed with radio telescopes in Hobart, Tasmania and Ceduna, South Australia. A software correlator was set up at the University of Tasmania to correlate these data.
Results. Measurements of the flux densities of flaring objects can be made using our observing strategy within half an hour of a triggering event. These observations can be calibrated with amplitude errors better than 15%. Lower limits to the brightness temperatures of the sources can also be calculated using CHI.
C1 [Blanchard, J. M.; Lovell, J. E. J.; Dickey, J. M.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia.
[Blanchard, J. M.; Edwards, P. G.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
[Kadler, M.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Ojha, R.] Catholic Univ Amer, Dept Phys, IACS, Washington, DC 20064 USA.
[Kadler, M.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany.
[Kadler, M.] Univ Erlangen Nurnberg, Dr Remeis Sternwarte, D-96049 Bamberg, Germany.
[Kadler, M.] Univ Erlangen Nurnberg, ECAP, D-96049 Bamberg, Germany.
[Kadler, M.] Univ Space Res Assoc, Columbia, MD 21044 USA.
RP Blanchard, JM (reprint author), Univ Tasmania, Sch Math & Phys, Private Bag 37, Hobart, Tas 7001, Australia.
EM jayb@utas.edu.au
RI Dickey, John/C-6156-2013;
OI Dickey, John/0000-0002-6300-7459; Kadler, Matthias/0000-0001-5606-6154
FU NASA through Fermi Guest Investigator [NNH09ZDA001N, 31263]; NASA at the
Goddard Space Flight Center
FX We are extremely grateful to Simon Ellingsen of the University of
Tasmania for providing the V255 PKS B1934-638 data essential to the
proper calibration of CHI. This research was funded in part by NASA
through Fermi Guest Investigator grant NNH09ZDA001N (proposal number
31263). 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. This
research has made use of data from the NASA/IPAC Extragalactic Database
(NED, 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). This research has made use of NASA's Astrophysics Data System.
This research has made use of the United States Naval Observatory (USNO)
Radio Reference Frame Image Database (RRFID).
NR 30
TC 3
Z9 3
U1 0
U2 1
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 FEB
PY 2012
VL 538
AR A150
DI 10.1051/0004-6361/201117593
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 897AX
UT WOS:000300614100150
ER
PT J
AU Farinelli, R
Ceccobello, C
Romano, P
Titarchuk, L
AF Farinelli, R.
Ceccobello, C.
Romano, P.
Titarchuk, L.
TI Numerical solution of the radiative transfer equation: X-ray spectral
formation from cylindrical accretion onto a magnetized neutron star
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE methods: numerical; X-rays: binaries; radiative transfer; magnetic
fields
ID CONVERGING FLUID-FLOW; COMPTONIZATION MODEL; DOMINATED SHOCK;
BLACK-HOLES; POWER-LAW; SCATTERING; BINARIES; PULSARS; INDEX; BULK
AB Context. Predicting the emerging X-ray spectra in several astrophysical objects is of great importance, in particular when the observational data are compared with theoretical models. This requires developing numerical routines for the solution of the radiative equation according to the expected physical conditions of the systems under study.
Aims. We have developed an algorithm solving the radiative transfer equation in the Fokker-Planck approximation when both thermal and bulk Comptonization take place. The algorithm is essentially a relaxation method, where stable solutions are obtained when the system has reached its steady-state equilibrium.
Methods. We obtained the solution of the radiative transfer equation in the two-dimensional domain defined by the photon energy E and optical depth of the system tau using finite-differences for the partial derivatives, and imposing specific boundary conditions for the solutions. We treated the case of cylindrical accretion onto a magnetized neutron star.
Results. We considered a blackbody seed spectrum of photons with exponential distribution across the accretion column and for an accretion where the velocity reaches its maximum at the stellar surface and at the top of the accretion column, respectively. In both cases higher values of the electron temperature and of the optical depth tau produce flatter and harder spectra. Other parameters contributing to the spectral formation are the steepness of the vertical velocity profile, the albedo at the star surface, and the radius of the accretion column. The latter parameter modifies the emerging spectra in a specular way for the two assumed accretion profiles.
Conclusions. The algorithm has been implemented in the xspec package for X-ray spectral fitting and is specifically dedicated to the physical framework of accretion at the polar cap of a neutron star with a high magnetic field (greater than or similar to 10(12) G). This latter case is expected to be typical of accreting systems such as X-ray pulsars and supergiant fast X-ray transients.
C1 [Farinelli, R.; Romano, P.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-90146 Palermo, Italy.
[Farinelli, R.; Ceccobello, C.; Titarchuk, L.] Univ Ferrara, Dipartimento Fis, I-44100 Ferrara, Italy.
[Titarchuk, L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Farinelli, R (reprint author), Ist Astrofis Spaziale & Fis Cosm, INAF, Via U La Malfa 153, I-90146 Palermo, Italy.
EM farinelli@ifc.inaf.it
FU [ASI-INAF I/009/10/0]
FX We acknowledge financial contribution from the agreement ASI-INAF
I/009/10/0.
NR 14
TC 15
Z9 15
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2012
VL 538
AR A67
DI 10.1051/0004-6361/201118008
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 897AX
UT WOS:000300614100067
ER
PT J
AU Guelbenzu, AN
Klose, S
Kruhler, T
Greiner, J
Rossi, A
Kann, DA
Olivares, F
Rau, A
Afonso, PMJ
Elliott, J
Filgas, R
Yoldas, AK
McBreen, S
Nardini, M
Schady, P
Schmidl, S
Sudilovsky, V
Updike, AC
Yoldas, A
AF Guelbenzu, A. Nicuesa
Klose, S.
Kruehler, T.
Greiner, J.
Rossi, A.
Kann, D. A.
Olivares, F.
Rau, A.
Afonso, P. M. J.
Elliott, J.
Filgas, R.
Yoldas, A. Kuepcue
McBreen, S.
Nardini, M.
Schady, P.
Schmidl, S.
Sudilovsky, V.
Updike, A. C.
Yoldas, A.
TI The late-time afterglow of the extremely energetic short burst GRB
090510 revisited
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE gamma-ray burst: individual: GRB 090510
ID GAMMA-RAY BURSTS; OPTICAL AFTERGLOWS; HOST GALAXIES; EMISSION; SWIFT;
ORIGIN; GROND; FERMI
AB Context. The Swift discovery of the short burst GRB 090510 has raised considerable attention mainly because of two reasons: first, it had a bright optical afterglow, and second it is among the most energetic events detected so far within the entire GRB population (long plus short). The afterglow of GRB 090510 was observed with Swift/UVOT and Swift/XRT and evidence of a jet break around 1.5 ks after the burst has been reported in the literature, implying that after this break the optical and X-ray light curve should fade with the same decay slope.
Aims. As noted by several authors, the post-break decay slope seen in the UVOT data is much shallower than the steep decay in the X-ray band, pointing to a (theoretically hard to understand) excess of optical flux at late times. We assess here the validity of this peculiar behavior.
Methods. We reduced and analyzed new afterglow light-curve data obtained with the multichannel imager GROND. These additional g' r' i' z data were then combined with the UVOT and XRT data to study the behavior of the afterglow at late times more stringently.
Results. Based on the densely sampled data set obtained with GROND, we find that the optical afterglow of GRB 090510 did indeed enter a steep decay phase starting around 22 ks after the burst. During this time the GROND optical light curve is achromatic, and its slope is identical to the slope of the X-ray data. In combination with the UVOT data this implies that a second break must have occurred in the optical light curve around 22 ks post burst, which, however, has no obvious counterpart in the X-ray band, contradicting the interpretation that this could be another jet break.
Conclusions. The GROND data provide the missing piece of evidence that the optical afterglow of GRB 090510 did follow a post-jet break evolution at late times. The break seen in the optical light curve around 22 ks in combination with its missing counterpart in the X-ray band could be due to the passage of the injection frequency across the optical bands, as already theoretically proposed in the literature. This is possibly the first time that this passage has been clearly seen in an optical afterglow. In addition, our results imply that there is no more evidence for an excess of flux in the optical bands at late times.
C1 [Guelbenzu, A. Nicuesa; Klose, S.; Rossi, A.; Kann, D. A.; Schmidl, S.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany.
[Kruehler, T.; Greiner, J.; Olivares, F.; Rau, A.; Afonso, P. M. J.; Elliott, J.; Filgas, R.; Nardini, M.; Schady, P.; Sudilovsky, V.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Kruehler, T.] Tech Univ Munich, D-85748 Garching, Germany.
[Kruehler, T.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Afonso, P. M. J.] Amer River Coll, Dept Phys & Astron, Sacramento, CA 95841 USA.
[Yoldas, A. Kuepcue; Yoldas, A.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[McBreen, S.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Updike, A. C.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA.
[Updike, A. C.] NASA, CRESST, GSFC, Greenbelt, MD 20771 USA.
[Updike, A. C.] NASA, Observat Cosmol Lab, GSFC, Greenbelt, MD 20771 USA.
[Updike, A. C.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Guelbenzu, AN (reprint author), Thuringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, Germany.
EM ana@tls-tautenburg.de
RI Rossi, Andrea/N-4674-2015;
OI Rossi, Andrea/0000-0002-8860-6538; Kruehler, Thomas/0000-0002-8682-2384
FU MPE; DFG [SA 2001/2-1, SA 2001/1-1]; DAAD; Leibniz-Prize (DFG) [HA
1850/28-1]; [DFG K1 766/16-1]
FX A.N.G., D.A.K., and S.K. acknowledge support by grant DFG K1 766/16-1.
A.N.G., A.R., D.A.K., and A.U. are grateful for travel funding support
through the MPE. T.K. acknowledges funding by the DFG cluster of
excellence "Origin and Structure of the Universe", F.O.E. funding of his
Ph.D. through the DAAD, M.N. support by DFG grant SA 2001/2-1 and P.S.
by DFG grant SA 2001/1-1. Part of the funding for GROND (both hardware
and personnel) was generously granted by the Leibniz-Prize to G.
Hasinger (DFG grant HA 1850/28-1). This work made use of data supplied
by the UK Swift science data center at the University of Leicester. We
thank the referee for a rapid reply and a careful reading of the
manuscript.
NR 38
TC 12
Z9 12
U1 0
U2 4
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 FEB
PY 2012
VL 538
AR L7
DI 10.1051/0004-6361/201118416
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 897AX
UT WOS:000300614100160
ER
PT J
AU Kunneriath, D
Eckart, A
Vogel, SN
Teuben, P
Muzic, K
Schodel, R
Garcia-Marin, M
Moultaka, J
Staguhn, J
Straubmeier, C
Zensus, JA
Valencia, M
Karas, V
AF Kunneriath, D.
Eckart, A.
Vogel, S. N.
Teuben, P.
Muzic, K.
Schoedel, R.
Garcia-Marin, M.
Moultaka, J.
Staguhn, J.
Straubmeier, C.
Zensus, J. A.
Valencia-S, M.
Karas, V.
TI The Galactic centre mini-spiral in the mm-regime
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE accretion, accretion disks; black hole physics; Galaxy: nucleus; radio
continuum: general; Galaxy: center
ID SAGITTARIUS-A-ASTERISK; DUST-EMBEDDED SOURCES; NUCLEAR STAR CLUSTER;
MASSIVE BLACK-HOLE; CENTRAL PARSEC; SGR-A; IONIZED-GAS; INFRARED
OBSERVATIONS; CIRCUMNUCLEAR DISK; SPECTROSCOPY
AB Context. The mini-spiral is a feature of the interstellar medium in the central similar to 2 pc of the Galactic center. It is composed of several streamers of dust and ionised and atomic gas with temperatures between a few 100 K to 10(4) K. There is evidence that these streamers are related to the so-called circumnuclear disk of molecular gas and are ionized by photons from massive, hot stars in the central parsec.
Aims. We attempt to constrain the emission mechanisms and physical properties of the ionized gas and dust of the mini-spiral region with the help of our multiwavelength data sets.
Methods. Our observations were carried out at 1.3 mm and 3 mm with the mm interferometric array CARMA in California in March and April 2009, with the MIR instrument VISIR at ESO's VLT in June 2006, and the NIR Br gamma with VLT NACO in August 2009.
Results. We present high resolution maps of the mini-spiral, and obtain a spectral index of 0.5 +/- 0.25 for Sgr A*, indicating an inverted synchrotron spectrum. We find electron densities within the range 0.8-1.5 x 10(4) cm(-3) for the mini-spiral from the radio continuum maps, along with a dust mass contribution of similar to 0.25 M-circle dot from the MIR dust continuum, and extinctions ranging from 1.8-3 at 2.16 mu m in the Br gamma line.
Conclusions. We observe a mixture of negative and positive spectral indices in our 1.3 mm and 3 mm observations of the extended emission of the mini-spiral, which we interpret as evidence that there are a range of contributions to the thermal free-free emission by the ionized gas emission and by dust at 1.3 mm.
C1 [Kunneriath, D.; Eckart, A.; Garcia-Marin, M.; Straubmeier, C.; Zensus, J. A.; Valencia-S, M.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany.
[Kunneriath, D.; Eckart, A.; Zensus, J. A.; Valencia-S, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Kunneriath, D.; Karas, V.] Acad Sci Czech Republic, Inst Astron, Prague 14100, Czech Republic.
[Vogel, S. N.; Teuben, P.; Staguhn, J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Muzic, K.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Schoedel, R.] CSIC, Inst Astrofis Andalucia, Madrid 18008, Spain.
[Moultaka, J.] Univ Toulouse, LATT, CNRS, F-31400 Toulouse, France.
[Staguhn, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Staguhn, J.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
RP Kunneriath, D (reprint author), Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany.
EM devaky@astro.cas.cz
RI Schoedel, Rainer/D-4751-2014; Karas, Vladimir/C-1559-2013; Kunneriath,
Devaky/G-8513-2014
OI Schoedel, Rainer/0000-0001-5404-797X; Karas,
Vladimir/0000-0002-5760-0459;
FU Ministerio de Ciencia y Innovacion of the government of Spain; German
federal department for education and research ( BMBF) [50OS0502,
50OS0801]; COST Action [MP0905]; PECS [98040]
FX D. Kunneriath and M. Valencia-S. are members of the International Max
Planck Research School (IMPRS) for Astronomy and Astrophysics at the
MPIfR and the Universities of Bonn and Cologne. R.S. acknowledges
support by the Ramon y Cajal programme by the Ministerio de Ciencia y
Innovacion of the government of Spain. Macarena Garcia-Marin is
supported by the German federal department for education and research
(BMBF) under the project numbers: 50OS0502 and 50OS0801. Part of this
work was supported by the COST Action MP0905: Black Holes in a violent
Universe and PECS project No. 98040. This research has made use of
NASA's Astrophysics Data System.
NR 50
TC 10
Z9 10
U1 0
U2 3
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2012
VL 538
AR A127
DI 10.1051/0004-6361/201117676
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 897AX
UT WOS:000300614100127
ER
PT J
AU Kylafis, ND
Contopoulos, I
Kazanas, D
Christodoulou, DM
AF Kylafis, N. D.
Contopoulos, I.
Kazanas, D.
Christodoulou, D. M.
TI Formation and destruction of jets in X-ray binaries
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: neutron; accretion, accretion disks; black holes physics; X-rays:
binaries; magnetic fields
ID BLACK-HOLE BINARIES; ADVECTION-DOMINATED ACCRETION; NEUTRON-STAR; HARD
STATE; LOW/HARD STATE; COSMIC BATTERY; AQUILA X-1; MILLISECOND PULSAR;
MHD SIMULATIONS; RADIO-EMISSION
AB Context. Neutron-star and black-hole X-ray binaries (XRBs) exhibit radio jets, whose properties depend on the X-ray spectral state and history of the source. In particular, black-hole XRBs emit compact, steady radio jets when they are in the so-called hard state. These jets become eruptive as the sources move toward the soft state, disappear in the soft state, and then re-appear when the sources return to the hard state. The jets from neutron-star X-ray binaries are typically weaker radio emitters than the black-hole ones at the same X-ray luminosity and in some cases radio emission is detected in the soft state.
Aims. Significant phenomenology has been developed to describe the spectral states of neutron-star and black-hole XRBs, and there is general agreement about the type of the accretion disk around the compact object in the various spectral states. We investigate whether the phenomenology describing the X-ray emission on one hand and the jet appearance and disappearance on the other can be put together in a consistent physical picture.
Methods. We consider the so-called Poynting-Robertson cosmic battery (PRCB), which has been shown to explain in a natural way the formation of magnetic fields in the disks of AGNs and the ejection of jets. We investigate whether the PRCB can also explain the formation, destruction, and variability of jets in XRBs.
Results. We find excellent agreement between the conditions under which the PRCB is efficient (i.e., the type of the accretion disk) and the emission or destruction of the radio jet.
Conclusions. The disk-jet connection in XRBs can be explained in a natural way using the PRCB.
C1 [Kylafis, N. D.] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece.
[Kylafis, N. D.] Inst Theoret & Computat Phys, Iraklion 71003, Crete, Greece.
[Kylafis, N. D.] Fdn Res & Technol Hellas, Iraklion 71110, Crete, Greece.
[Contopoulos, I.] Acad Athens, Res Ctr Astron, Athens 11527, Greece.
[Kazanas, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Christodoulou, D. M.] Univ Massachusetts Lowell, Dept Math Sci, Lowell, MA 01854 USA.
RP Kylafis, ND (reprint author), Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece.
EM kylafis@physics.uoc.gr
RI Kylafis, Nikolaos/C-4555-2011
OI Kylafis, Nikolaos/0000-0003-0928-0996
FU EU [39965]; EU REGPOT [206469]
FX This research has been supported in part by EU Marie Curie project No.
39965, and EU REGPOT project number 206469. N.D.K. thanks Tomaso Belloni
for providing hardness-intensity data of GX 339-4 during various
outbursts and Michiel van der Klis and Dimitrios Psaltis for useful
discussions concerning millisecond pulsars. I.C. thanks Maxim Lyutikov,
Ramesh Narayan, Roman Shcherbakov, and Sasha Tchekhovskoy for
discussions concerning accretion disks and the PRCB.
NR 76
TC 11
Z9 11
U1 0
U2 3
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD FEB
PY 2012
VL 538
AR A5
DI 10.1051/0004-6361/201117052
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 897AX
UT WOS:000300614100005
ER
PT J
AU Martins, F
Escolano, C
Wade, GA
Donati, JF
Bouret, JC
AF Martins, F.
Escolano, C.
Wade, G. A.
Donati, J. F.
Bouret, J. C.
CA MiMeS Collaboration
TI Observational effects of magnetism in O stars: surface nitrogen
abundances
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: massive; stars: atmospheres; stars: fundamental parameters;
stars: abundances; stars: magnetic field
ID DRIVEN STELLAR WINDS; THETA(1) ORIONIS-C; VLT-FLAMES SURVEY; B-TYPE
STARS; MASSIVE STARS; DIFFERENTIAL ROTATION; DYNAMICAL SIMULATIONS; LINE
SPECTROSCOPY; MAGELLANIC-CLOUD; LUMINOUS STARS
AB Aims. We investigate the surface nitrogen content of the six magnetic O stars known to date as well as of the early B-type star tau Sco. We compare these abundances to predictions of evolutionary models to isolate the effects of magnetic field on the transport of elements in stellar interiors.
Methods. We conduct a quantitative spectroscopic analysis of the sample stars with state-of-the-art atmosphere models. We rely on high signal-to-noise ratio, high resolution optical spectra obtained with ESPADONS at CFHT and NARVAL at TBL. Atmosphere models and synthetic spectra are computed with the code CMFGEN. Values of N/H together with their uncertainties are determined and compared to predictions of evolutionary models.
Results. We find that the magnetic stars can be divided into two groups: one with stars displaying no N enrichment (one object); and one with stars most likely showing extra N enrichment (5 objects). For one star (Theta(1) Ori C) no robust conclusion can be drawn due to its young age. The star with no N enrichment is the one with the weakest magnetic field, possibly of dynamo origin. It might be a star having experienced strong magnetic braking under the condition of solid body rotation, but its rotational velocity is still relatively large. The five stars with high N content were probably slow rotators on the zero age main sequence, but they have surface N/H typical of normal O stars, indicating that the presence of a (probably fossil) magnetic field leads to extra enrichment. These stars may have a strong differential rotation inducing shear mixing. Our results should be viewed as a basis on which new theoretical simulations can rely to better understand the effect of magnetism on the evolution of massive stars.
C1 [Martins, F.; Escolano, C.] CNRS, LUPM UMR 5299, F-34095 Montpellier 05, France.
[Martins, F.; Escolano, C.] Univ Montpellier 2, F-34095 Montpellier 05, France.
[Wade, G. A.] Royal Mil Coll Canada, Dept Phys, Kingston, ON K7K 7B4, Canada.
[Donati, J. F.] CNRS, IRAP UMR 5277, F-31400 Toulouse, France.
[Donati, J. F.] Univ Toulouse 3, F-31400 Toulouse, France.
[Escolano, C.; Bouret, J. C.] CNRS, LAM UMR 6110, F-13388 Marseille 13, France.
[Escolano, C.; Bouret, J. C.] Univ Aix Marseille 1, F-13388 Marseille 13, France.
[Bouret, J. C.] NASA GSFC, Greenbelt, MD 20771 USA.
RP Martins, F (reprint author), CNRS, LUPM UMR 5299, Pl Eugene Bataillon, F-34095 Montpellier 05, France.
EM fabrice.martins@univ-montp2.fr
FU Natural Science and Engineering Research Council of Canada
FX We thank the referee, Jo Puls, for valuable comments and for suggesting
to add the star tau Sco to our sample. Many thanks to John Hillier for
making his code CMFGEN available and for constant help with it. G. A. W.
acknowledges Discovery Grant support from the Natural Science and
Engineering Research Council of Canada.
NR 67
TC 22
Z9 22
U1 1
U2 1
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 FEB
PY 2012
VL 538
AR A29
DI 10.1051/0004-6361/201118039
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 897AX
UT WOS:000300614100029
ER
PT J
AU Masson, S
Demoulin, P
Dasso, S
Klein, KL
AF Masson, S.
Demoulin, P.
Dasso, S.
Klein, K. -L.
TI The interplanetary magnetic structure that guides solar relativistic
particles
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE solar-terrestrial relations; Sun: heliosphere; methods: data analysis
ID CORONAL MASS EJECTIONS; ADVANCED COMPOSITION EXPLORER; COSMIC-RAY EVENT;
ENERGETIC PARTICLES; CURRENT SHEETS; RELEASE TIMES; KEV ELECTRONS; FLUX
ROPE; ACCELERATION; PROTONS
AB Context. Relating in-situ measurements of relativistic solar particles to their parent activity in the corona requires understanding the magnetic structures that guide them from their acceleration site to the Earth. Relativistic particle events are observed at times of high solar activity, when transient magnetic structures such as interplanetary coronal mass ejections (ICMEs) often shape the interplanetary magnetic field (IMF). They may introduce interplanetary paths that are longer than nominal, and magnetic connections rooted far from the nominal Parker spiral.
Aims. We present a detailed study of the IMF configurations during ten relativistic solar particle events of the 23rd activity cycle to elucidate the actual IMF configuration that guides the particles to the Earth, where they are measured by neutron monitors.
Methods. We used magnetic field (MAG) and plasma parameter measurements (SWEPAM) from the ACE spacecraft and determined the interplanetary path lengths of energetic particles through a modified version of the velocity dispersion analysis based on energetic particle measurements with SoHO/ERNE.
Results. We find that the majority (7/10) of the events is detected in the vicinity of an ICME. Their interplanetary path lengths are found to be longer (1.5-2.6 AU) than those of the two events propagating in the slow solar wind (1.3 AU). The longest apparent path length is found in an event within the fast solar wind, probably caused by enhanced pitch angle scattering. The derived path lengths imply that the first energetic and relativistic protons are released at the Sun at the same time as electron beam emitting type III radio bursts.
Conclusions. The timing of the first high-energy particle arrival on Earth is mainly determined by the type of IMF in which the particles propagate. Initial arrival times are as expected from Parker's model in the slow solar wind, and significantly longer in or near transient structures such as ICMEs.
C1 [Masson, S.; Demoulin, P.; Klein, K. -L.] Univ Paris Diderot, UPMC, CNRS, Observ Paris,LESIA, F-92190 Meudon, France.
[Dasso, S.] CONICET UBA, Inst Astron & Fis Espacio, Buenos Aires, DF, Argentina.
[Dasso, S.] UBA, Fac Ciencias Exactas & Nat, Dept Fis, Buenos Aires, DF, Argentina.
RP Masson, S (reprint author), NASA, Space Weather Lab, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM sophie.masson@nasa.gov
OI Demoulin, Pascal/0000-0001-8215-6532
FU ECOS-Sud [A08U01]; Abdus Salam International Centre for Theoretical
Physics (ICTP); Delegation Generale pour l'Armement (DGA); NASA;
European Commission through the FP6 SOLAIRE Network
[MTRN-CT-2006-035484]; [UBACyT 20020090100264]; [PIP
11220090100825/10]; [PICT-2007-00856]
FX The authors gratefully acknowledge R. Wimmer-Schweingruber and A. Balogh
for helpful discussions on the contents of this paper. This research has
made use of NASA's Space Physics Data Facility (SPDF). We thank the ACE
instrument teams and their respective principal investigators, namely N.
F. Ness (ACE/MAG) and D. J. McComas (ACE/SWEPAM). The authors
acknowledge financial support from ECOS-Sud through their cooperative
science program (No. A08U01). This work was partially supported by the
Argentinean grants: UBACyT 20020090100264 (UBA), PIP 11220090100825/10
(CONICET), and PICT-2007-00856 (ANPCyT). S. D. acknowledges support from
the Abdus Salam International Centre for Theoretical Physics (ICTP), as
provided in the frame of his regular associateship. S. D. is member of
the Carrera del Investigador Cientifico, CONICET. The work of S. M. is
funded by a fellowship of Delegation Generale pour l'Armement (DGA). S.
M. thank the NASA Postdoctoral Program at the Goddard Space Flight
Center, administered by Oak Ridge Associated Universities through a
contract with NASA for financial support. Financial support by the
European Commission through the FP6 SOLAIRE Network
(MTRN-CT-2006-035484) is gratefully acknowledged. We thank E. Valtonen
for his very helpful assistance with the ERNE data.
NR 58
TC 17
Z9 17
U1 0
U2 4
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 FEB
PY 2012
VL 538
AR A32
DI 10.1051/0004-6361/201118145
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 897AX
UT WOS:000300614100032
ER
PT J
AU Rau, A
Schady, P
Greiner, J
Salvato, M
Ajello, M
Bottacini, E
Gehrels, N
Afonso, PMJ
Elliott, J
Filgas, R
Kann, DA
Klose, S
Kruhler, T
Nardini, M
Guelbenzu, AN
Olivares, F
Rossi, A
Sudilovsky, V
Updike, AC
Hartmann, DH
AF Rau, A.
Schady, P.
Greiner, J.
Salvato, M.
Ajello, M.
Bottacini, E.
Gehrels, N.
Afonso, P. M. J.
Elliott, J.
Filgas, R.
Kann, D. A.
Klose, S.
Kruehler, T.
Nardini, M.
Guelbenzu, A. Nicuesa
Olivares E, F.
Rossi, A.
Sudilovsky, V.
Updike, A. C.
Hartmann, D. H.
TI BL Lacertae objects beyond redshift 1.3-UV-to-NIR photometry and
photometric redshift for Fermi/LAT blazars
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: distances and redshifts; techniques: photometric; BL Lacertae
objects: general
ID LARGE-AREA TELESCOPE; OPTICAL VARIABILITY; CAMPAIGN; CATALOG; MISSION;
STARS; GROND
AB Context. Observations of the.-ray sky with Fermi led to significant advances towards understanding blazars, the most extreme class of active galactic nuclei. A large fraction of the population detected by Fermi is formed by BL Lacertae (BL Lac) objects, whose sample has always suffered from a severe redshift incompleteness due to the quasi-featureless optical spectra.
Aims. Our goal is to provide a significant increase of the number of confirmed high-redshift BL Lac objects contained in the 2 LAC Fermi/LAT cataloge.
Methods. For 103 Fermi/LAT blazars, photometric redshifts using spectral energy distribution fitting have been obtained. The photometry includes 13 broad-band filters from the far ultraviolet to the near-IR observed with Swift/UVOT and the multi-channel imager GROND at the MPG/ESO 2.2 m telescope. Data have been taken quasi-simultaneously and the remaining source-intrinsic variability has been corrected for.
Results. We release the UV-to-near-IR 13-band photometry for all 103 sources and provide redshift constraints for 75 sources without previously known redshift. Out of those, eight have reliable photometric redshifts at z greater than or similar to 1.3, while for the other 67 sources we provide upper limits. Six of the former eight are BL Lac objects, which quadruples the sample of confirmed high-redshift BL Lac. This includes three sources with redshifts higher than the previous record for BL Lac, including CRATES J0402-2615, with the best-fit solution at z approximate to 1.9.
C1 [Rau, A.; Schady, P.; Greiner, J.; Afonso, P. M. J.; Elliott, J.; Filgas, R.; Kruehler, T.; Nardini, M.; Olivares E, F.; Sudilovsky, V.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Salvato, M.] Max Planck Inst Plasma Phys & Excellence Cluster, D-85748 Garching, Germany.
[Salvato, M.; Kruehler, T.] Tech Univ Munich, D-85748 Garching, Germany.
[Ajello, M.; Bottacini, E.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Ajello, M.; Bottacini, E.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Ajello, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Afonso, P. M. J.] Amer River Coll, Phys & Astron Dpt, Sacramento, CA 95841 USA.
[Kann, D. A.; Klose, S.; Guelbenzu, A. Nicuesa; Rossi, A.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany.
[Kruehler, T.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Nardini, M.] Univ Milano Bicocca, I-20126 Milan, Italy.
[Updike, A. C.] Dickinson Coll, Dept Phys & Astron, Carlisle, PA 17013 USA.
[Hartmann, D. H.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA.
RP Rau, A (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany.
EM arau@mpe.mpg.de
RI Gehrels, Neil/D-2971-2012;
OI Kruehler, Thomas/0000-0002-8682-2384
FU DFG [HA 1850/28-1, Kl 766/16-1, SA 2001/2-1, SA 2001/1-1]; German
Deutsche Forschungsgemeinschaft, DFG [FKZ HA 1850/28-1]; DFG cluster of
excellence Origin and Structure of the Universe; European Commission;
DARK: The Dark Cosmology Centre; Danish National Research Foundation;
Deutscher Akademischer Austausch-Dienst (DAAD); BLANCEFLOR
Boncompagni-Ludovisi, ne Bildt foundation; MPE
FX We thank the referee for the valuable comments. Part of the funding for
GROND (both hardware as well as personnel) was generously granted from
the Leibniz-Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1). M. S.
acknowledges support by the German Deutsche Forschungsgemeinschaft, DFG
Leibniz Prize (FKZ HA 1850/28-1). T. K. acknowledges support by the DFG
cluster of excellence Origin and Structure of the Universe, by the
European Commission under the Marie Curie Intra-European Fellowship
Programme), as well as the DARK: The Dark Cosmology Centre, funded by
the Danish National Research Foundation. F.O.E. acknowledges funding of
his Ph.D. through the Deutscher Akademischer Austausch-Dienst (DAAD). S.
K., D. A. K. and A.N.G acknowledge support by DFG grant Kl 766/16-1.
ARossi acknowledges support from the BLANCEFLOR Boncompagni-Ludovisi, ne
Bildt foundation. M.N. acknowledges support by DFG grant SA 2001/2-1. P.
S. acknowledges support by DFG grant SA 2001/1-1. A. C. U., A.N.G., D.
A. K. and ARossi are grateful for travel funding support through MPE. We
also acknowledge the use of the TOPCAT tool (Taylor 2005).
NR 41
TC 33
Z9 33
U1 1
U2 1
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 FEB
PY 2012
VL 538
AR A26
DI 10.1051/0004-6361/201118159
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 897AX
UT WOS:000300614100026
ER
PT J
AU Riviere-Marichalar, P
Menard, F
Thi, WF
Kamp, I
Montesinos, B
Meeus, G
Woitke, P
Howard, C
Sandell, G
Podio, L
Dent, WRF
Mendigutia, I
Pinte, C
White, GJ
Barrado, D
AF Riviere-Marichalar, P.
Menard, F.
Thi, W. F.
Kamp, I.
Montesinos, B.
Meeus, G.
Woitke, P.
Howard, C.
Sandell, G.
Podio, L.
Dent, W. R. F.
Mendigutia, I.
Pinte, C.
White, G. J.
Barrado, D.
TI Detection of warm water vapour in Taurus protoplanetary discs by
Herschel
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE astrochemistry; stars: formation; protoplanetary disks; astrobiology;
molecular data; line: identification
ID CIRCUMSTELLAR DISKS; STATISTICAL-METHODS; ORGANIC-MOLECULES;
ASTRONOMICAL DATA; FORMING REGION; SPITZER SURVEY; UPPER LIMITS; STARS;
H2O; EXCITATION
AB Line spectra of 68 Taurus T Tauri stars were obtained with the Herschel-PACS (Photodetector Array Camera and Spectrometer) instrument as part of the GASPS (GAS evolution in Protoplanetary Systems) survey of protoplanetary discs. A careful examination of the linescans centred on the [OI] 63.18 mu m fine-structure line unveiled a line at 63.32 mu m in some of these spectra. We identify this line with the 8(18) -> 7(07) transition of ortho-water. It is detected confidently (i.e., > 3 sigma) in eight sources, i.e., similar to 24% of the sub-sample with gas-rich discs. Several statistical tests were used to search for correlations with other disc and stellar parameters such as line fluxes of [OI] 6300 angstrom and 63.18 mu m; X-ray luminosity and continuum levels at 63 mu m and 850 mu m. Correlations are found between the water line fluxes and the [OI] 63.18 mu m line luminosity, the dust continuum, and possibly with the stellar X-ray luminosity. This is the first time that this line of warm water vapour has been detected in protoplanetary discs. We discuss its origins, in particular whether it comes from the inner disc and/or disc surface or from shocks in outflows and jets. Our analysis favours a disc origin, with the observed water vapour line produced within 2-3 AU from the central stars, where the gas temperature is of the order of 500-600 K.
C1 [Riviere-Marichalar, P.; Montesinos, B.; Mendigutia, I.; Barrado, D.] CSIC INTA, Dept Astrofis, Ctr Astrobiol, Villanueva De La Canada 28691, Spain.
[Menard, F.; Thi, W. F.; Pinte, C.] UJF Grenoble 1, CNRS INSU, Inst Planetol & Astrophys IPAG, UMR 5274, F-38041 Grenoble, France.
[Kamp, I.; Podio, L.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands.
[Meeus, G.] Univ Autonoma Madrid, Fac Ciencias, Dep Fis Teor, E-28049 Madrid, Spain.
[Woitke, P.] Univ Vienna, Dept Astron, A-1180 Vienna, Austria.
[Woitke, P.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Woitke, P.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Howard, C.; Sandell, G.] NASA, SOFIA USRA, Ames Res Ctr, Washington, DC USA.
[Dent, W. R. F.] ALMA, Santiago, Chile.
[White, G. J.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England.
[White, G. J.] Rutherford Appleton Lab, Didcot OX11 OQL, Oxon, England.
[Barrado, D.] Ctr Astron Hispano Aleman, Calar Alto Observ, Almeria 04004, Spain.
RP Riviere-Marichalar, P (reprint author), CSIC INTA, Dept Astrofis, Ctr Astrobiol, POB 78, Villanueva De La Canada 28691, Spain.
EM riviere@cab.inta-csic.es
RI Barrado Navascues, David/C-1439-2017; Montesinos, Benjamin/C-3493-2017;
OI Barrado Navascues, David/0000-0002-5971-9242; Montesinos,
Benjamin/0000-0002-7982-2095; Mendigutia, Ignacio/0000-0002-0233-5328
FU Spanish grants [AYA 2010-21161-C02-02, CDS2006-00070,
PRICIT-S2009/ESP-1496]; ANR [ANR-07-BLAN-0221, ANR-2010-JCJC-0504-01];
CNES; PNPS of CNRS/INSU; Millennium Science Initiative (ICM) of the
Chilean ministry of Economy [P10-022-F]; EC [PERG06-GA-2009-256513]
FX We thank the anonymous referee for a constructive report that helped to
improve the paper. This research has been funded by Spanish grants AYA
2010-21161-C02-02, CDS2006-00070 and PRICIT-S2009/ESP-1496. In France we
thank ANR (contracts ANR-07-BLAN-0221 and ANR-2010-JCJC-0504-01); CNES;
PNPS of CNRS/INSU. The Millennium Science Initiative (ICM) of the
Chilean ministry of Economy (Nucleus P10-022-F) and an EC-FP7 grant
(PERG06-GA-2009-256513) are also acknowledged.
NR 32
TC 33
Z9 33
U1 0
U2 1
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 FEB
PY 2012
VL 538
AR L3
DI 10.1051/0004-6361/201118448
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 897AX
UT WOS:000300614100156
ER
PT J
AU Tilling, I
Woitke, P
Meeus, G
Mora, A
Montesinos, B
Riviere-Marichalar, P
Eiroa, C
Thi, WF
Isella, A
Roberge, A
Martin-Zaidi, C
Kamp, I
Pinte, C
Sandell, G
Vacca, WD
Menard, F
Mendigutia, I
Duchene, G
Dent, WRF
Aresu, G
Meijerink, R
Spaans, M
AF Tilling, I.
Woitke, P.
Meeus, G.
Mora, A.
Montesinos, B.
Riviere-Marichalar, P.
Eiroa, C.
Thi, W. -F.
Isella, A.
Roberge, A.
Martin-Zaidi, C.
Kamp, I.
Pinte, C.
Sandell, G.
Vacca, W. D.
Menard, F.
Mendigutia, I.
Duchene, G.
Dent, W. R. F.
Aresu, G.
Meijerink, R.
Spaans, M.
TI Gas modelling in the disc of HD 163296
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE circumstellar matter; astrochemistry; stars: pre-main sequence;
protoplanetary disks; stars: fundamental parameters; line: formation
ID HERBIG-AE STARS; PRE-MAIN-SEQUENCE; FINE-STRUCTURE EXCITATION;
NEAR-INFRARED EMISSION; PROTOPLANETARY DISKS; CIRCUMSTELLAR DUST; YOUNG
STARS; ROTATIONAL-EXCITATION; BETA-PICTORIS; GROUND-STATE
AB We present detailed model fits to observations of the disc around the Herbig Ae star HD 163296. This well-studied object has an age of similar to 4Myr, with evidence of a circumstellar disc extending out to similar to 540AU. We use the radiation thermo-chemical disc code ProDiMo to model the gas and dust in the circumstellar disc of HD 163296, and attempt to determine the disc properties by fitting to observational line and continuum data. These include new Herschel/PACS observations obtained as part of the open-time key program GASPS (GAS in Protoplanetary Systems), consisting of a detection of the [Oi] 63 mu m line and upper limits for several other far infrared lines. We complement this with continuum data and ground-based observations of the (CO)-C-12 3-2, 2-1 and (CO)-C-13 J = 1-0 line transitions, as well as an upper limit for the H-2 0-0 S(1) transition. We explore the effects of stellar ultraviolet variability and dust settling on the line emission, and on the derived disc properties. Our fitting efforts lead to derived gas/dust ratios in the range 9-100, depending on the assumptions made. We note that the line fluxes are sensitive in general to the degree of dust settling in the disc, with an increase in line flux for settled models. This is most pronounced in lines which are formed in the warm gas in the inner disc, but the low excitation molecular lines are also affected. This has serious implications for attempts to derive the disc gas mass from line observations. We derive fractional PAH abundances between 0.007 and 0.04 relative to ISM levels. Using a stellar and UV excess input spectrum based on a detailed analysis of observations, we find that the all observations are consistent with the previously assumed disc geometry.
C1 [Tilling, I.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Woitke, P.] Univ Vienna, Dept Astron, A-1180 Vienna, Austria.
[Woitke, P.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Woitke, P.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland.
[Meeus, G.; Eiroa, C.] Univ Autonoma Madrid, Fac Ciencias, Dep Fisica Teor, E-28049 Madrid, Spain.
[Mora, A.] ESA ESAC Gaia SOC, Madrid 28691, Spain.
[Montesinos, B.; Riviere-Marichalar, P.; Mendigutia, I.] INTA CSIC, CAB, Ctr Astrobiol, Dept Astrofis, Madrid 28691, Spain.
[Thi, W. -F.; Martin-Zaidi, C.; Pinte, C.; Menard, F.; Duchene, G.] UJF Grenoble 1, CNRS INSU, Inst Planetol Astrophys IPAG, UMR 5274, F-38041 Grenoble, France.
[Isella, A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Roberge, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kamp, I.; Aresu, G.; Spaans, M.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands.
[Sandell, G.; Vacca, W. D.] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA.
[Duchene, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Dent, W. R. F.] ESO ALMA, Santiago, Chile.
[Meijerink, R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Tilling, I (reprint author), Univ Edinburgh, Royal Observ, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland.
EM it@roe.ac.uk
RI Roberge, Aki/D-2782-2012; Montesinos, Benjamin/C-3493-2017;
OI Roberge, Aki/0000-0002-2989-3725; Montesinos,
Benjamin/0000-0002-7982-2095; Mendigutia, Ignacio/0000-0002-0233-5328
NR 98
TC 35
Z9 35
U1 0
U2 1
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 FEB
PY 2012
VL 538
AR A20
DI 10.1051/0004-6361/201116919
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 897AX
UT WOS:000300614100020
ER
PT J
AU Verdini, A
Grappin, R
Velli, M
AF Verdini, A.
Grappin, R.
Velli, M.
TI Coronal heating in coupled photosphere-chromosphere-coronal systems:
turbulence and leakage
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE methods: numerical; Sun: corona; magnetohydrodynamics (MHD); turbulence;
Sun: transition region; waves
ID FLUCTUATING ENERGY-STORAGE; MHD TURBULENCE; SHELL MODELS; LOOPS;
MAGNETOHYDRODYNAMICS; DYNAMICS; CASCADE
AB Context. Coronal loops act as resonant cavities for low-frequency fluctuations that are transmitted from the deeper layers of the solar atmosphere. These fluctuations are amplified in the corona and lead to the development of turbulence that in turn is able to dissipate the accumulated energy, thus heating the corona. However, trapping is not perfect, because some energy leaks down to the chromosphere on a long timescale, limiting the turbulent heating.
Aims. We consider the combined effects of turbulence and energy leakage from the corona to the photosphere in determining the turbulent energy level and associated heating rate in models of coronal loops, which include the chromosphere and transition region.
Methods. We use a piece-wise constant model for the Alfven speed in loops and a reduced MHD-shell model to describe the interplay between turbulent dynamics in the direction perpendicular to the mean field and propagation along the field. Turbulence is sustained by incoming fluctuations that are equivalent, in the line-tied case, to forcing by the photospheric shear flows. While varying the turbulence strength, we systematically compare the average coronal energy level and dissipation in three models with increasing complexity: the classical closed model, the open corona, and the open corona including chromosphere (or three-layer model), with the last two models allowing energy leakage.
Results. We find that (i) leakage always plays a role. Even for strong turbulence, the dissipation time never becomes much lower than the leakage time, at least in the three-layer model; therefore, both the energy and the dissipation levels are systematically lower than in the line-tied model; (ii) in all models, the energy level is close to the resonant prediction, i. e., assuming an effective turbulent correlation time longer than the Alfven coronal crossing time; (iii) the heating rate is close to the value given by the ratio of photospheric energy divided by the Alfven crossing time; (iv) the coronal spectral range is divided in two: an inertial range with 5/3 spectral slope, and a large-scale peak where nonlinear couplings are inhibited by trapped resonant modes; (v) in the realistic three-layer model, the two-component spectrum leads to a global decrease in damping equal to Kolmogorov damping reduced by a factor u(rms)/V-a(c) where V-a(c) is the coronal Alfven speed.
C1 [Verdini, A.] Royal Observ Belgium, Solar Terr Ctr Excellence SIDC, Brussels, Belgium.
[Grappin, R.] Observ Paris, LUTH, Meudon, France.
[Grappin, R.] Ecole Polytech, LPP, Palaiseau, France.
[Velli, M.] CALTECH, JPL, Pasadena, CA 91125 USA.
RP Verdini, A (reprint author), Royal Observ Belgium, Solar Terr Ctr Excellence SIDC, Brussels, Belgium.
EM verdini@oma.be
FU Belgian Federal Science Policy Office through the ESA-PRODEX; National
Aeronautics and Space Administration
FX We benefited from useful discussions with G. Belmont. A. V. acknowledges
support from the Belgian Federal Science Policy Office through the
ESA-PRODEX program. The research described in this paper was carried out
in part at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with the National Aeronautics and Space
Administration.
NR 19
TC 15
Z9 15
U1 0
U2 4
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 FEB
PY 2012
VL 538
AR A70
DI 10.1051/0004-6361/201118046
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 897AX
UT WOS:000300614100070
ER
PT J
AU Yong, A
Hough, SE
Iwahashi, J
Braverman, A
AF Yong, Alan
Hough, Susan E.
Iwahashi, Junko
Braverman, Amy
TI A Terrain-Based Site-Conditions Map of California with Implications for
the Contiguous United States
SO BULLETIN OF THE SEISMOLOGICAL SOCIETY OF AMERICA
LA English
DT Article
ID SHEAR-WAVE VELOCITY; SEISMIC GROUND-MOTION; SAN-FRANCISCO-BAY; SATELLITE
DATA; LOCAL GEOLOGY; EARTHQUAKE; AMPLIFICATION; LANDFORM; TOPOGRAPHY;
REGION
AB We present an approach based on geomorphometry to predict material properties and characterize site conditions using the V-S30 parameter (time-averaged shear-wave velocity to a depth of 30 m). Our framework consists of an automated terrain classification scheme based on taxonomic criteria (slope gradient, local convexity, and surface texture) that systematically identifies 16 terrain types from 1-km spatial resolution (30 arcsec) Shuttle Radar Topography Mission digital elevation models (SRTM DEMs). Using 853 V-S30 values from California, we apply a simulation-based statistical method to determine the mean V-S30 for each terrain type in California. We then compare the V-S30 values with models based on individual proxies, such as mapped surface geology and topographic slope, and show that our systematic terrain-based approach consistently performs better than semiempirical estimates based on individual proxies. To further evaluate our model, we apply our California-based estimates to terrains of the contiguous United States. Comparisons of our estimates with 325 V-S30 measurements outside of California, as well as estimates based on the topographic slope model, indicate our method to be statistically robust and more accurate. Our approach thus provides an objective and robust method for extending estimates of V-S30 for regions where in situ measurements are sparse or not readily available.
C1 [Yong, Alan; Hough, Susan E.] US Geol Survey, Pasadena, CA 91106 USA.
[Iwahashi, Junko] Geospatial Informat Author Japan, Tsukuba, Ibaraki, Japan.
[Braverman, Amy] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Yong, A (reprint author), US Geol Survey, 525 S Wilson Ave, Pasadena, CA 91106 USA.
EM yong@usgs.gov
NR 84
TC 22
Z9 22
U1 0
U2 3
PU SEISMOLOGICAL SOC AMER
PI ALBANY
PA 400 EVELYN AVE, SUITE 201, ALBANY, CA 94706-1375 USA
SN 0037-1106
J9 B SEISMOL SOC AM
JI Bull. Seismol. Soc. Amer.
PD FEB
PY 2012
VL 102
IS 1
BP 114
EP 128
DI 10.1785/0120100262
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 897BC
UT WOS:000300614700010
ER
PT J
AU Zaitchik, BF
Simane, B
Habib, S
Anderson, MC
Ozdogan, M
Foltz, JD
AF Zaitchik, Benjamin F.
Simane, Belay
Habib, Shahid
Anderson, Martha C.
Ozdogan, Mutlu
Foltz, Jeremy D.
TI Building Climate Resilience in the Blue Nile/Abay Highlands: A Role for
Earth System Sciences
SO INTERNATIONAL JOURNAL OF ENVIRONMENTAL RESEARCH AND PUBLIC HEALTH
LA English
DT Review
DE climate change; adaptation; resilience; land degradation; erosion
ID ETHIOPIAN HIGHLANDS; MODEL ANALYSIS; VARIABILITY; PRECIPITATION;
EROSION; NILE; CONSERVATION; DEGRADATION; INFORMATION; PRODUCTS
AB The Blue Nile (Abay) Highlands of Ethiopia are characterized by significant interannual climate variability, complex topography and associated local climate contrasts, erosive rains and erodible soils, and intense land pressure due to an increasing population and an economy that is almost entirely dependent on smallholder, low-input agriculture. As a result, these highland zones are highly vulnerable to negative impacts of climate variability. As patterns of variability and precipitation intensity alter under anthropogenic climate change, there is concern that this vulnerability will increase, threatening economic development and food security in the region. In order to overcome these challenges and to enhance sustainable development in the context of climate change, it is necessary to establish climate resilient development strategies that are informed by best-available Earth System Science (ESS) information. This requirement is complicated by the fact that climate projections for the Abay Highlands contain significant and perhaps irreducible uncertainties. A critical challenge for ESS, then, is to generate and to communicate meaningful information for climate resilient development in the context of a highly uncertain climate forecast. Here we report on a framework for applying ESS to climate resilient development in the Abay Highlands, with a focus on the challenge of reducing land degradation.
C1 [Zaitchik, Benjamin F.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21210 USA.
[Simane, Belay] Univ Addis Ababa, Coll Dev Studies, Addis Ababa, Ethiopia.
[Habib, Shahid] NASA, Goddard Space Flight Ctr, Off Appl Sci, Greenbelt, MD 20770 USA.
[Anderson, Martha C.] ARS, Hydrol & Remote Sensing Lab, USDA, Beltsville, MD 20705 USA.
[Ozdogan, Mutlu; Foltz, Jeremy D.] Univ Wisconsin, Madison, WI 53706 USA.
RP Zaitchik, BF (reprint author), Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21210 USA.
EM zaitchik@jhu.edu; simaneb@yahoo.com; shahid.habib@nasa.gov;
martha.anderson@ars.usda.gov; ozdogon@wisc.edu; jdfoltz@wisc.edu
RI Zaitchik, Benjamin/B-9461-2013; Brooks, Katya/J-4975-2014; Anderson,
Martha/C-1720-2015;
OI Anderson, Martha/0000-0003-0748-5525; Ozdogan, Mutlu/0000-0002-1707-3375
FU Johns Hopkins University; Addis Ababa University; NASA [NNX09AT61G]
FX The authors thank the Johns Hopkins University Global Water Program and
Addis Ababa University for providing funds for the workshop in Bahir
Dar. All 70+ workshop participants are also acknowledged for their
contribution to the ideas presented in this paper. Nile LDAS Research
results presented here were supported by NASA Applied Sciences grant
NNX09AT61G.
NR 71
TC 11
Z9 11
U1 5
U2 42
PU MDPI AG
PI BASEL
PA POSTFACH, CH-4005 BASEL, SWITZERLAND
SN 1660-4601
J9 INT J ENV RES PUB HE
JI Int. J. Environ. Res. Public Health
PD FEB
PY 2012
VL 9
IS 2
BP 435
EP 461
DI 10.3390/ijerph9020435
PG 27
WC Environmental Sciences; Public, Environmental & Occupational Health
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health
GA 898DE
UT WOS:000300714800007
PM 22470302
ER
PT J
AU Gabb, T
AF Gabb, Tim
TI Advances in Superalloys
SO JOM
LA English
DT Editorial Material
C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Gabb, T (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM timothy.p.gabb@nasa.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1047-4838
J9 JOM-US
JI JOM
PD FEB
PY 2012
VL 64
IS 2
BP 239
EP 240
DI 10.1007/s11837-012-0240-5
PG 2
WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical
Engineering; Mineralogy; Mining & Mineral Processing
SC Materials Science; Metallurgy & Metallurgical Engineering; Mineralogy;
Mining & Mineral Processing
GA 902LQ
UT WOS:000301040000009
ER
PT J
AU Bunderson, LD
Van de Water, P
Luvall, J
Levetin, E
AF Bunderson, L. D.
Van de Water, P.
Luvall, J.
Levetin, E.
TI When Is It Safe To Go Outside? Nighttime Juniper Pollen Concentrations
In Texas, Oklahoma, And New Mexico
SO JOURNAL OF ALLERGY AND CLINICAL IMMUNOLOGY
LA English
DT Meeting Abstract
CT Annual Meeting of the American-Academy-of-Allergy-Asthma-and-Immunology
(AAAAI)
CY MAR 02-06, 2012
CL Orlando, FL
SP Amer Acad Allergy Asthma & Immunol (AAAAI)
C1 [Bunderson, L. D.; Levetin, E.] Univ Tulsa, Tulsa, OK 74104 USA.
[Van de Water, P.] Calif State Univ Fresno, Fresno, CA 93740 USA.
[Luvall, J.] NASA, Huntsville, AL USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU MOSBY-ELSEVIER
PI NEW YORK
PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0091-6749
J9 J ALLERGY CLIN IMMUN
JI J. Allergy Clin. Immunol.
PD FEB
PY 2012
VL 129
IS 2
SU S
BP AB92
EP AB92
PG 1
WC Allergy; Immunology
SC Allergy; Immunology
GA 903QL
UT WOS:000301133400349
ER
PT J
AU Levetin, E
Bunderson, L
Van de Water, P
Luvall, J
AF Levetin, E.
Bunderson, L.
Van de Water, P.
Luvall, J.
TI Is Red-Berry Juniper an Overlooked Fall Allergen in the Southwest?
SO JOURNAL OF ALLERGY AND CLINICAL IMMUNOLOGY
LA English
DT Meeting Abstract
CT Annual Meeting of the American-Academy-of-Allergy-Asthma-and-Immunology
(AAAAI)
CY MAR 02-06, 2012
CL Orlando, FL
SP Amer Acad Allergy Asthma & Immunol (AAAAI)
C1 [Levetin, E.; Bunderson, L.] Univ Tulsa, Tulsa, OK 74104 USA.
[Van de Water, P.] Calif State Univ Fresno, Fresno, CA 93740 USA.
[Luvall, J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
NR 0
TC 1
Z9 1
U1 0
U2 0
PU MOSBY-ELSEVIER
PI NEW YORK
PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0091-6749
J9 J ALLERGY CLIN IMMUN
JI J. Allergy Clin. Immunol.
PD FEB
PY 2012
VL 129
IS 2
SU S
BP AB91
EP AB91
PG 1
WC Allergy; Immunology
SC Allergy; Immunology
GA 903QL
UT WOS:000301133400345
ER
PT J
AU Van de Water, PK
Bunderson, L
Luvall, J
Levetin, E
AF Van de Water, P. K.
Bunderson, L.
Luvall, J.
Levetin, E.
TI Urban Heat And Humidity Islands And The Preferential Deposition Of
Airborne Pollen
SO JOURNAL OF ALLERGY AND CLINICAL IMMUNOLOGY
LA English
DT Meeting Abstract
CT Annual Meeting of the American-Academy-of-Allergy-Asthma-and-Immunology
(AAAAI)
CY MAR 02-06, 2012
CL Orlando, FL
SP Amer Acad Allergy Asthma & Immunol (AAAAI)
C1 [Van de Water, P. K.] Calif State Univ Fresno, Fresno, CA 93740 USA.
[Bunderson, L.; Levetin, E.] Univ Tulsa, Tulsa, OK 74104 USA.
[Luvall, J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
NR 0
TC 0
Z9 0
U1 0
U2 4
PU MOSBY-ELSEVIER
PI NEW YORK
PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0091-6749
J9 J ALLERGY CLIN IMMUN
JI J. Allergy Clin. Immunol.
PD FEB
PY 2012
VL 129
IS 2
SU S
BP AB19
EP AB19
PG 1
WC Allergy; Immunology
SC Allergy; Immunology
GA 903QL
UT WOS:000301133400075
ER
PT J
AU Tapiador, FJ
Turk, FJ
Petersen, W
Hou, AY
Garcia-Ortega, E
Machado, LAT
Angelis, CF
Salio, P
Kidd, C
Huffman, GJ
de Castro, M
AF Tapiador, Francisco J.
Turk, F. J.
Petersen, Walt
Hou, Arthur Y.
Garcia-Ortega, Eduardo
Machado, Luiz A. T.
Angelis, Carlos F.
Salio, Paola
Kidd, Chris
Huffman, George J.
de Castro, Manuel
TI Global precipitation measurement: Methods, datasets and applications
SO ATMOSPHERIC RESEARCH
LA English
DT Review
DE Precipitation Regional Climate Models (RCM); Global Climate Models
(GCM); Quantitative Precipitation Estimation (QPE); Global Precipitation
Measurement (GPM) mission
ID RAINDROP SIZE DISTRIBUTION; SATELLITE RAINFALL ESTIMATION; VARIATIONAL
DATA ASSIMILATION; ENSEMBLE KALMAN FILTER; PROBABILITY-DISTRIBUTION
FUNCTIONS; DIFFERENT CLIMATIC REGIMES; SMALL-SCALE VARIABILITY;
DUAL-POLARIZED RADAR; SPACE-TIME CLIMATE; PASSIVE MICROWAVE
AB This paper explores the many aspects of precipitation measurement that are relevant to providing an accurate global assessment of this important environmental parameter. Methods discussed include ground data, satellite estimates and numerical models. First, the methods for measuring, estimating, and modeling precipitation are discussed. Then, the most relevant datasets gathering precipitation information from those three sources are presented. The third part of the paper illustrates a number of the many applications of those measurements and databases, namely hydropower, data assimilation and validation of Regional Climate Models (RCM). The aim of the paper is to organize the many links and feedbacks between precipitation measurement, estimation and modeling, indicating the uncertainties and limitations of each technique in order to identify areas requiring further attention, and to show the limits within which datasets can be used. Special emphasis is put on the central role of the upcoming Global Precipitation Measurement (GPM) mission in precipitation science. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Tapiador, Francisco J.; de Castro, Manuel] UCLM, Dept Environm Sci, Toledo, Spain.
[Turk, F. J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Petersen, Walt] NASA, Goddard Space Flight Ctr, Wallops Flight Facil, Wallops Isl, VA 23337 USA.
[Hou, Arthur Y.; Kidd, Chris; Huffman, George J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Garcia-Ortega, Eduardo] Univ Leon, Dept Phys, E-24071 Leon, Spain.
[Salio, Paola] Univ Buenos Aires, FCEN, Dept Ciencias Atmosfera & Oceanos, Buenos Aires, DF, Argentina.
[Kidd, Chris] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Huffman, George J.] Sci Syst & Applicat Inc, Lanham, MD USA.
RP Tapiador, FJ (reprint author), UCLM, Dept Environm Sci, Toledo, Spain.
EM francisco.tapiador@uclm.es; joseph.turk@jpl.nasa.gov;
walt.petersen@nasa.gov; arthur.y.hou@nasa.gov;
eduardo.garcia@unileon.es; luiz.machado@cptec.inpe.br;
angelis@cptec.inpe.br; salio@cima.fcen.uba.ar; chris.kidd@nasa.gov;
george.j.huffman@nasa.gov; manuel.castro@uclm.es
RI Garcia-Ortega, Eduardo/A-7088-2012; Hou, Arthur/D-8578-2012; Huffman,
George/F-4494-2014; Kidd, Christopher/H-9910-2014; Measurement,
Global/C-4698-2015; Machado, Luiz/C-4314-2012
OI Garcia-Ortega, Eduardo/0000-0002-6414-3081; Huffman,
George/0000-0003-3858-8308; Machado, Luiz/0000-0002-8243-1706
FU CENIT PROMETEO (MICCIN); JCCM [PPII10-0162-554]; National Aeronautics
and Space Administration; JCyL [LE176A11-2]; EU [EVK2-CT-2001-00132,
505539]; DoE; EPA; NOAA; NSF; [CGL2010-20787-C02-01];
[CGL2010-20787-C02-02]
FX The work of FTJ (Tapiador) has been funded through projects
CGL2010-20787-C02-01, CGL2010-20787-C02-02, CENIT PROMETEO (MICCIN), and
PPII10-0162-554 (JCCM). The contributions from FJT (Turk) were performed
at the Jet Propulsion Laboratory, California Institute of Technology,
under contract with the National Aeronautics and Space Administration.
EGO acknowledges research project LE176A11-2 (JCyL). GJH and WP
acknowledge the NASA PMM (Dr. Ramesh Kakar) and GPM Programs for funding
support. FJT (Tapiador), FJT (Turk), WP, AYH, LATM, CFA, PS, and GJH are
current Principal Investigators in the Precipitation Measurement
Missions (PMM, GPM + TRMM) science team. PRUDENCE project was funded by
the EU FP5 (Contract no. EVK2-CT-2001-00132). The ENSEMBLES data used in
this work was funded by the EU FP6 (Contract no. 505539). NAR-CAPP is
funded by the DoE, EPA, NOAA and NSF. The CMAP, CPC, CRU, GPCC, GPCP and
TRMM data providers are also gratefully acknowledged.
NR 155
TC 91
Z9 94
U1 9
U2 80
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 FEB
PY 2012
VL 104
BP 70
EP 97
DI 10.1016/j.atmosres.2011.10.021
PG 28
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 898JS
UT WOS:000300739300003
ER
PT J
AU Palmsten, ML
Holman, RA
AF Palmsten, Margaret L.
Holman, Robert A.
TI Laboratory investigation of dune erosion using stereo video
SO COASTAL ENGINEERING
LA English
DT Article
DE Stereo imaging; Dune erosion; Wave runup; Remote sensing
ID SCALE; IMPACT; RUNUP; COAST
AB Simple parameterizations of dune erosion are necessary for forecasting erosion potential prior to an oncoming storm. Dune erosion may be parameterized in terms of the elevation of the total water level (composed of surge, tide, and wave runup) above the dune base and period of exposure of the dune to waves. In this work, we test several versions of this model using observations from a large wave tank experiment designed to model a storm hydrograph, and we develop a new method for acquiring the appropriate data with confidence intervals using stereo video techniques.
The stereo method results in observations of dune morphology at higher spatial and temporal resolutions than traditional survey methods allow. Resolution of the stereo technique was 0.1 m in the horizontal and 0.04 m in the vertical, and errors in stereo observations were on the order of 0.02 to 0.08 m (1 to 2 pixels) when compared with surveys. A new method was developed to estimate confidence intervals on stereo observations. When the unchanging dune top was repeatedly sampled, the new confidence intervals encompassed 2 standard deviations of scatter about the mean dune surface 98% of the time.
Observations from the stereo method were used to quantify wave runup and dune erosion. We tested a variety of runup statistics based on a Gaussian distribution of swash properties, and found that the most predictive statistic for dune erosion was the 16% exceedance elevation above the dune base, lower than the often used 2% exceedance value. We found that the parameterization of runup was sensitive to the definition of beach slope and that the most accurate beach slope for predicting runup was through the region of the beach profile defined by the mean water level plus one standard deviation of swash. The dune base retreated along a relatively constant trajectory that was a half of the initial beach slope. Finally, a simple model for dune erosion was tested and found to reproduce 64% of the observed variance in dune erosion rate given known forcing at the dune and 49% of the observed variance in dune erosion rate given parameterized forcing. Integrating the simple model over time, 93% of the observed dune retreat distance was reproduced given offshore forcing. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Palmsten, Margaret L.] USN, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA.
[Palmsten, Margaret L.; Holman, Robert A.] Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA.
RP Palmsten, ML (reprint author), USN, Res Lab, Stennis Space Ctr, Code 7430, Stennis Space Ctr, MS 39529 USA.
EM margaret.palmsten.ctr@nrlssc.navy.mil
FU Oregon Sea Grant; United States Geological Survey; Office of Naval
Research
FX The authors would like to thank Linden Clarke for early development of
the stereo code, John Stanley for his hard work on this and other Argus
projects, and Peter Ruggiero and Tim Maddux for data collection and
project development. This work was completed with funding from the
Oregon Sea Grant, the United States Geological Survey, and the Office of
Naval Research.
NR 28
TC 11
Z9 15
U1 1
U2 11
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0378-3839
J9 COAST ENG
JI Coast. Eng.
PD FEB
PY 2012
VL 60
BP 123
EP 135
DI 10.1016/j.coastaleng.2011.09.003
PG 13
WC Engineering, Civil; Engineering, Ocean
SC Engineering
GA 900WF
UT WOS:000300921700011
ER
PT J
AU Chopping, M
North, M
Chen, JQ
Schaaf, CB
Blair, JB
Martonchik, JV
Bull, MA
AF Chopping, Mark
North, Malcolm
Chen, Jiquan
Schaaf, Crystal B.
Blair, J. Bryan
Martonchik, John V.
Bull, Michael A.
TI Forest Canopy Cover and Height From MISR in Topographically Complex
Southwestern US Landscapes Assessed With High Quality Reference Data
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Biomass; canopy; forestry; lidar; modeling; multiangle; topography
ID REMOTE-SENSING DATA; ANGLE SPECTRAL DATA; BIDIRECTIONAL REFLECTANCE;
NORTH-AMERICA; UNITED-STATES; ABOVEGROUND BIOMASS; CONIFER FOREST; TREE
MORTALITY; MODEL; INVERSION
AB This study addresses the retrieval of spatially contiguous canopy cover and height estimates in southwestern US forests via inversion of a geometric-optical (GO) model against surface bidirectional reflectance factor (BRF) estimates from the Multi-angle Imaging SpectroRadiometer (MISR). Model inversion can provide such maps if good estimates of the background bidirectional reflectance distribution function (BRDF) are available. The study area is in the Sierra National Forest in the Sierra Nevada of California. Tree number density, mean crown radius, and fractional cover reference estimates were obtained via analysis of QuickBird 0.6 m spatial resolution panchromatic imagery using the CANopy Analysis with Panchromatic Imagery (CANAPI) algorithm, while RH50, RH75 and RH100 (50%, 75%, and 100% energy return) height data were obtained from the NASA Laser Vegetation Imaging Sensor (LVIS), a full waveform light detection and ranging (lidar) instrument. These canopy parameters were used to drive a modified version of the simple GO model (SGM), accurately reproducing patterns of MISR 672 nm band surface reflectance (mean RMSE = 0.011, mean R-2 = 0.82, N = 1048). Cover and height maps were obtained through model inversion against MISR 672 nm reflectance estimates on a 250 m grid. The free parameters were tree number density and mean crown radius. RMSE values with respect to reference data for the cover and height retrievals were 0.05 and 6.65 m, respectively, with R-2 of 0.54 and 0.49. MISR can thus provide maps of forest cover and height in areas of topographic variation although refinements are required to improve retrieval precision.
C1 [Chopping, Mark] Montclair State Univ, Dept Earth & Environm Studies, Montclair, NJ 07043 USA.
[North, Malcolm] US Forest Serv, USDA, Pacific SW Res Stn, Davis, CA 95618 USA.
[Chen, Jiquan] Univ Toledo, Dept Environm Sci, Toledo, OH 43560 USA.
[Schaaf, Crystal B.] Univ Massachusetts, Dept Environm Earth & Ocean Sci, Boston, MA 02125 USA.
[Blair, J. Bryan] NASA, Goddard Space Flight Ctr, Laser Remote Sensing Lab, Greenbelt, MD 20771 USA.
[Martonchik, John V.; Bull, Michael A.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Chopping, M (reprint author), Montclair State Univ, Dept Earth & Environm Studies, Montclair, NJ 07043 USA.
EM chopping@pegasus.montclair.edu; mnorth@ucdavis.edu;
jiquan.chen@utoledo.edu; crystal.schaaf@umb.edu; james.b.blair@nasa.gov;
john.v.martonchik@jpl.nasa.gov; michael.a.bull@jpl.nasa.gov
RI Chen, Jiquan/D-1955-2009; Khachadourian, Diana/C-8513-2012; Blair,
James/D-3881-2013; Beckley, Matthew/D-4547-2013
FU National Aeronautics and Space Administration [NNX08AE71G, NNX11AF90G];
University of Maryland, College Park
FX This work was supported by National Aeronautics and Space Administration
Grant NNX08AE71G and Grant NNX11AF90G.; The authors acknowledge the LVIS
team for use of the LVIS data. They thank Xiaohong Chopping for informed
comment; Sawahiko Shimada (Agricultural University of Tokyo) for
assistance with large-scale BRDF model inversions; and Joseph Youn and
Michael Stoppay (Computer Operations for Research and Education, College
of Science and Mathematics, Montclair State University) for computing
support. They also thank the two anonymous reviewers for their insights
on the original manuscript. The MISR data were obtained from the NASA
Langley Atmospheric Science Data Center. LVIS data sets were provided by
the Laser Vegetation Imaging Sensor (LVIS) team in the Laser Remote
Sensing Branch at NASA Goddard Space Flight Center, with support from
the University of Maryland, College Park.
NR 50
TC 15
Z9 15
U1 2
U2 29
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 FEB
PY 2012
VL 5
IS 1
SI SI
BP 44
EP 58
DI 10.1109/JSTARS.2012.2184270
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 899VK
UT WOS:000300844400005
ER
PT J
AU Rahul, PRC
Bhawar, RL
Salvekar, PS
Devara, PCS
Jiang, JH
AF Rahul, P. R. C.
Bhawar, Rohini L.
Salvekar, P. S.
Devara, P. C. S.
Jiang, Jonathan H.
TI Evidence of Atmospheric Brown Clouds Over India During the 2009 Drought
Year
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Aerosols; clouds; greenhouse gases; satellites
ID MONSOON; CLIMATE; VARIABILITY; ABSORPTION; POLLUTION; RAIN
AB Using Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO) satellite derived vertical profiles (Total Attenuated Backscatter at 532 nm, Depolarization Ratios at 532 nm, Vertical Feature Mask, monthly mean vertical aerosol and extinction variability), monthly precipitation anomalies from National Centers for Environmental Prediction-Climate Prediction Center (NCEP-CPC) and NCEP wind anomalies; we report the presence of Atmospheric Brown Clouds (ABCs) over India (65 degrees E-95 degrees E; 8 degrees N-35 degrees N) during the summer monsoon of 2009. CALIPSO data revealed the persistent presence of a massive aerosol plume till 4 Km above sea level; this plume persisted for over 7 months (March through September 2009) over India and was loaded with anthropogenic aerosols like sulphates, black carbon products from biomass burning and fossil fuel combustion. The CALIPSO vertical profiles, NCEP-CPC monthly precipitation anomalies and NCEP monthly wind anomalies corroborate the presence of aerosol plume.
C1 [Rahul, P. R. C.; Salvekar, P. S.; Devara, P. C. S.] Indian Inst Trop Meteorol, Pune 411008, Maharashtra, India.
[Bhawar, Rohini L.; Jiang, Jonathan H.] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91125 USA.
RP Rahul, PRC (reprint author), Indian Inst Trop Meteorol, Pune 411008, Maharashtra, India.
FU CALTECH Jet Propulsion Laboratory; NASA
FX This work was supported by the CALTECH Jet Propulsion Laboratory,
sponsored by NASA.
NR 21
TC 4
Z9 4
U1 0
U2 11
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 FEB
PY 2012
VL 5
IS 1
SI SI
BP 236
EP 241
DI 10.1109/JSTARS.2011.2170554
PG 6
WC Engineering, Electrical & Electronic; Geography, Physical; Remote
Sensing; Imaging Science & Photographic Technology
SC Engineering; Physical Geography; Remote Sensing; Imaging Science &
Photographic Technology
GA 899VK
UT WOS:000300844400022
ER
PT J
AU Tarabalka, Y
Tilton, JC
Benediktsson, JA
Chanussot, J
AF Tarabalka, Yuliya
Tilton, James C.
Benediktsson, Jon Atli
Chanussot, Jocelyn
TI A Marker-Based Approach for the Automated Selection of a Single
Segmentation From a Hierarchical Set of Image Segmentations
SO IEEE JOURNAL OF SELECTED TOPICS IN APPLIED EARTH OBSERVATIONS AND REMOTE
SENSING
LA English
DT Article
DE Classification; hierarchical segmentation; hyperspectral images; marker
selection
ID HYPERSPECTRAL DATA; SPATIAL CLASSIFICATION; EXTRACTION; NETWORKS
AB The Hierarchical SEGmentation (HSEG) algorithm, which combines region object finding with region object clustering, has given good performances for multi-and hyperspectral image analysis. This technique produces at its output a hierarchical set of image segmentations. The automated selection of a single segmentation level is often necessary. We propose and investigate the use of automatically selected markers for this purpose. In this paper, a novel Marker-based HSEG (M-HSEG) method for spectral-spatial classification of hyperspectral images is proposed. Two classification-based approaches for automatic marker selection are adapted and compared for this purpose. Then, a novel constrained marker-based HSEG algorithm is applied, resulting in a spectral-spatial classification map. Three different implementations of the M-HSEG method are proposed and their performances in terms of classification accuracies are compared. The experimental results, presented for three hyperspectral airborne images, demonstrate that the proposed approach yields accurate segmentation and classification maps, and thus is attractive for remote sensing image analysis.
C1 [Tarabalka, Yuliya; Tilton, James C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Benediktsson, Jon Atli] Univ Iceland, Fac Elect & Comp Engn, IS-107 Reykjavik, Iceland.
[Chanussot, Jocelyn] Grenoble Inst Technol INPG, Grenoble Images Speech Signals & Automat Lab GIPS, F-38402 St Martin Dheres, France.
RP Tarabalka, Y (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM yuliya.tarabalka@nasa.gov; james.c.tilton@nasa.gov; benedikt@hi.is;
jocelyn.chanussot@gipsa-lab.grenoble-inp.fr
RI Benediktsson, Jon/F-2861-2010
OI Benediktsson, Jon/0000-0003-0621-9647
FU NASA
FX 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 38
TC 41
Z9 42
U1 2
U2 18
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 FEB
PY 2012
VL 5
IS 1
SI SI
BP 262
EP 272
DI 10.1109/JSTARS.2011.2173466
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 899VK
UT WOS:000300844400025
ER
PT J
AU Hamilton, DR
Sargsyan, AE
Garcia, K
Ebert, DJ
Whitson, PA
Feiveson, AH
Alferova, IV
Dulchavsky, SA
Matveev, VP
Bogomolov, VV
Duncan, JM
AF Hamilton, Douglas R.
Sargsyan, Ashot E.
Garcia, Kathleen
Ebert, Douglas J.
Whitson, Peggy A.
Feiveson, Alan H.
Alferova, Irina V.
Dulchavsky, Scott A.
Matveev, Vladimir P.
Bogomolov, Valery V.
Duncan, J. Michael
TI Cardiac and vascular responses to thigh cuffs and respiratory maneuvers
on crewmembers of the International Space Station
SO JOURNAL OF APPLIED PHYSIOLOGY
LA English
DT Article
DE microgravity; echocardiography; astronaut; occlusion cuffs; cardiac
function
ID CENTRAL VENOUS-PRESSURE; HEAD-DOWN TILT; CLINICAL ULTRASOUND ABOARD;
CARDIOVASCULAR-SYSTEM; MICROGRAVITY; FLIGHT; WEIGHTLESSNESS; VOLUME;
ECHOCARDIOGRAPHY; COUNTERMEASURES
AB Hamilton DR, Sargsyan AE, Garcia K, Ebert DJ, Whitson PA, Feiveson AH, Alferova IV, Dulchavsky SA, Matveev VP, Bogomolov VV, Duncan JM. Cardiac and vascular responses to thigh cuffs and respiratory maneuvers on crewmembers of the International Space Station. J Appl Physiol 112: 454-462, 2012. First published September 8, 2011; doi: 10.1152/japplphysiol.00557.2011.-Background: the transition to microgravity eliminates the hydrostatic gradients in the vascular system. The resulting fluid redistribution commonly manifests as facial edema, engorgement of the external neck veins, nasal congestion, and headache. This experiment examined the responses to modified Valsalva and Mueller maneuvers measured by cardiac and vascular ultrasound (ECHO) in a baseline steady state and under the influence of thigh occlusion cuffs available as a countermeasure device (Braslet cuffs). Methods: nine International Space Station crewmember subjects (expeditions 16-20) were examined in 15 experiment sessions 101 +/- 46 days after launch (mean +/- SD; 33-185). Twenty-seven cardiac and vascular parameters were obtained with/without respiratory maneuvers before and after tightening of the Braslet cuffs (162 parameter states/session). Quality of cardiac and vascular ultrasound examinations was assured through remote monitoring and guidance by investigators from the NASA Telescience Center in Houston, TX, and the Mission Control Center in Korolyov, Moscow region, Russia. Results: 14 of 81 conditions (27 parameters measured at baseline, Valsalva, and Mueller maneuver) were significantly different when the Braslet was applied. Seven of 27 parameters were found to respond differently to respiratory maneuvers depending on the presence or absence of thigh compression. Conclusions: acute application of Braslet occlusion cuffs causes lower extremity fluid sequestration and exerts commensurate measurable effects on cardiac performance in microgravity. Ultrasound techniques to measure the hemodynamic effects of thigh cuffs in combination with respiratory maneuvers may serve as an effective tool in determining the volume status of a cardiac or hemodynamically compromised patient at the "microgravity bedside."
C1 [Hamilton, Douglas R.; Sargsyan, Ashot E.; Garcia, Kathleen; Ebert, Douglas J.] Wyle Integrated Sci & Engn, Houston, TX USA.
[Whitson, Peggy A.; Feiveson, Alan H.; Duncan, J. Michael] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Alferova, Irina V.] Russian Acad Sci, Inst Biomed Problems, Moscow, Russia.
[Dulchavsky, Scott A.] Henry Ford Hosp, Detroit, MI 48202 USA.
[Matveev, Vladimir P.; Bogomolov, Valery V.] Yuri A Gagarin Cosmonaut Training Ctr, Star City, Russia.
RP Hamilton, DR (reprint author), 1290 Hercules Dr, Houston, TX 77058 USA.
EM dhamilton@wylehou.com
FU NASA [NAS9-02078]
FX Primary funding for this project was provided by the Exploration Medical
Capability element of NASA's Human Research Program through the
Bioastronautics Contract to Wyle Integrated Science and Engineering
Group (NAS9-02078).
NR 52
TC 8
Z9 9
U1 0
U2 9
PU AMER PHYSIOLOGICAL SOC
PI BETHESDA
PA 9650 ROCKVILLE PIKE, BETHESDA, MD 20814 USA
SN 8750-7587
J9 J APPL PHYSIOL
JI J. Appl. Physiol.
PD FEB
PY 2012
VL 112
IS 3
BP 454
EP 462
DI 10.1152/japplphysiol.00557.2011
PG 9
WC Physiology; Sport Sciences
SC Physiology; Sport Sciences
GA 894DX
UT WOS:000300408300017
PM 21903875
ER
PT J
AU Burns, JO
Lazio, J
Bale, S
Bowman, J
Bradley, R
Carilli, C
Furlanetto, S
Harker, G
Loeb, A
Pritchard, J
AF Burns, Jack O.
Lazio, J.
Bale, S.
Bowman, J.
Bradley, R.
Carilli, C.
Furlanetto, S.
Harker, G.
Loeb, A.
Pritchard, J.
TI Probing the first stars and black holes in the early Universe with the
Dark Ages Radio Explorer (DARE)
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Cosmology: first stars; dark ages; reionization; Radio lines: general;
Instrumentation: detectors
ID REIONIZATION EPOCH; HIGH-REDSHIFT; ARRAY; CONSTRAINTS; GALAXIES;
PARTICLE; BURSTS; NOISE; MHZ
AB A concept for a new space-based cosmology mission called the Dark Ages Radio Explorer (DARE) is presented in this paper. DARE's science objectives include: (1) When did the first stars form? (2) When did the first accreting black holes form? (3) When did Reionization begin? (4) What surprises does the end of the Dark Ages hold (e.g., Dark Matter decay)? DARE will use the highly-redshifted hyperfine 21-cm transition from neutral hydrogen to track the formation of the first luminous objects by their impact on the intergalactic medium during the end of the Dark Ages and during Cosmic Dawn (redshifts z = 11-35). It will measure the sky-averaged spin temperature of neutral hydrogen at the unexplored epoch 80-420 million years after the Big Bang, providing the first evidence of the earliest stars and galaxies to illuminate the cosmos and testing our models of galaxy formation. DARE's approach is to measure the expected spectral features in the sky-averaged, redshifted 21-cm signal over a radio bandpass of 40-120 MHz. DARE orbits the Moon for a mission lifetime of 3 years and takes data above the lunar farside, the only location in the inner solar system proven to be free of human-generated radio frequency interference and any significant ionosphere. The science instrument is composed of a low frequency radiometer, including electrically-short, tapered, bi-conical dipole antennas, a receiver, and a digital spectrometer. The smooth frequency response of the antennas and the differential spectral calibration approach using a Markov Chain Monte Carlo technique will be applied to detect the weak cosmic 21-cm signal in the presence of the intense solar system and Galactic foreground emissions. (C) 2011 COSPA R. Published by Elsevier Ltd. All rights reserved.
C1 [Burns, Jack O.; Harker, G.] Univ Colorado, Ctr Astrophys & Space Astron, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Burns, Jack O.; Lazio, J.; Bale, S.; Bowman, J.; Bradley, R.; Carilli, C.; Furlanetto, S.; Harker, G.; Loeb, A.; Pritchard, J.] NASA, Ames Res Ctr, Lunar Sci Inst, Moffett Field, CA 94035 USA.
[Lazio, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bale, S.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Bowman, J.] Arizona State Univ, Dept Phys, Tempe, AZ 85287 USA.
[Bradley, R.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Carilli, C.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Furlanetto, S.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Loeb, A.; Pritchard, J.] Ctr Astrophys, Cambridge, MA 02138 USA.
RP Burns, JO (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, Dept Astrophys & Planetary Sci, 593 UCB, Boulder, CO 80309 USA.
EM jack.burns@colorado.edu
RI Bale, Stuart/E-7533-2011; Harker, Geraint/C-4885-2012;
OI Bale, Stuart/0000-0002-1989-3596; Harker, Geraint/0000-0002-7894-4082;
Pritchard, Jonathan/0000-0003-4127-5353
FU NASA Ames Research Center (ARC); Lunar University Network for
Astro-physics Research (LUNAR); NLSI [NNA09DB30A]
FX The authors would like to thank the management of the NASA Ames Research
Center (ARC) for their strong support and investment in the DARE
concept, especially ARC Director P. Worden along with P. Klupar, B.J.
Jaroux, as well as NASA Lunar Science Institute (NLSI) Director Y.
Pendleton and NLSI Deputy Director G. Schmidt. We are particularly
grateful to L. Webster, J. Bauman, H. Sanchez, D. Santiago, T. Soderman,
and J. Baer at ARC, as well as I. O'Dwyer, A. Tanner, and R. Jarnot at
JPL. We would like to acknowledge Ball Aerospace and, especially, L.
Hardaway for their investment of resources and effort on the DARE
concept. This concept was conceived and supported by the Lunar
University Network for Astro-physics Research (LUNAR)
(http://lunar.colorado.edu), headquartered at the University of Colorado
Boulder, funded by the NLSI via Cooperative Agreement NNA09DB30A. Part
of this research was conducted at that the Jet Propulsion Laboratory,
California Institute of Technology, under contract to the National
Aeronautics and Space Administration.
NR 48
TC 62
Z9 62
U1 1
U2 8
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 FEB 1
PY 2012
VL 49
IS 3
BP 433
EP 450
DI 10.1016/j.asr.2011.10.014
PG 18
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 892DA
UT WOS:000300265700001
ER
PT J
AU Ruzmaikin, A
Aumann, HH
AF Ruzmaikin, Alexander
Aumann, Hartmut H.
TI Decadal variability of tropical Pacific temperature in relation to solar
cycles
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Climate decadal variability; Solar cycles
ID SEA-SURFACE TEMPERATURE; AIR-TEMPERATURE; OUTPUT
AB We use the 8-year long satellite temperature data (2002-2010) from Atmospheric Infra Red Sounder (AIRS) and Atmospheric Microwave Sounding Unit (AMSU) on the Aqua satellite to identify temperature trends in the troposphere and low stratosphere over the Nino 3.4 region of the Tropical Pacific Ocean in the most recent 11-year solar cycle. Employing more extended sea surface temperature (SST) data for five solar cycles (1950-2009) in this region we show that the satellite trends reflect a typical decrease of the sea surface temperature (SST) in the Nino 3.4 region in the declining phase of the solar cycle. The magnitude of the SST decrease depends on the solar cycle and ranges between 0.07 K/yr and 0.27 K/yr for the last five solar cycles. Published by Elsevier Ltd. on behalf of COSPAR.
C1 [Ruzmaikin, Alexander; Aumann, Hartmut H.] Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ruzmaikin, A (reprint author), Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Alexander.Ruzmaikin@jpl.nasa.gov
FU Jet Propulsion Laboratory of the California Institute of Technology
under National Aeronautics and Space Administration
FX This work was supported in part by the Jet Propulsion Laboratory of the
California Institute of Technology, under a contract with the National
Aeronautics and Space Administration. We thank two reviewers for helpful
critical comments.
NR 23
TC 2
Z9 2
U1 0
U2 0
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 FEB 1
PY 2012
VL 49
IS 3
BP 572
EP 578
DI 10.1016/j.asr.2011.11.010
PG 7
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 892DA
UT WOS:000300265700017
ER
PT J
AU Schlappi, B
Altwegg, K
Riesen, T
Rubin, M
AF Schlaeppi, Bernhard
Altwegg, Kathrin
Riesen, Timm
Rubin, Martin
TI An underestimated onboard generated recoil force contributing to the
Pioneer anomaly
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Pioneer anomaly; Spacecraft outgassing; Spacecraft contamination
AB The Pioneer anomaly, an unexpected acceleration of the Pioneer 10 and 11 spacecraft of similar to 8.5 x 10(-10) ms(-2) directed towards the inner Solar System, has been of great interest for the physics community during the past decade: considered explanations range from new physical concepts to conventional mechanism. It is shown that non-isotropic outgassing of the complete spacecraft structure is comparable in magnitude and direction to the effect and should be considered as a significant contribution to the anomalous acceleration. Although gas leaks from e.g. the propulsion system and propulsive mass loss mechanism have been discarded as possible explanations for the anomaly, the arguments used against such mechanisms do not apply to global outgassing from the spacecraft. (C) 2011 COSPAR. Published by Elsevier Ltd. All rights reserved.
C1 [Schlaeppi, Bernhard; Altwegg, Kathrin] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland.
[Riesen, Timm] NASA Astrobiol Inst, Inst Astron, Honolulu, HI 96822 USA.
[Rubin, Martin] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
RP Schlappi, B (reprint author), Univ Bern, Inst Phys, Sidlerstr 5, CH-3012 Bern, Switzerland.
EM schlaeppi@space.unibe.ch
RI Rubin, Martin/I-7777-2013
OI Rubin, Martin/0000-0001-6549-3318
FU Swiss National Science Foundation; JPL under NASA [1266313, NMO710889];
National Aeronautics and Space Administration through the NASA
Astrobiology Institute through the Office of Space Science [NNA09-DA77A]
FX Work at the University of Bern was funded by the Swiss National Science
Foundation. The work at the University of Michigan was supported by JPL
subcontract 1266313 under NASA prime contract NMO710889. This material
is based upon work supported by the National Aeronautics and Space
Administration through the NASA Astrobiology Institute under Cooperative
Agreement No. NNA09-DA77A issued through the Office of Space Science.
NR 17
TC 4
Z9 4
U1 0
U2 3
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
J9 ADV SPACE RES
JI Adv. Space Res.
PD FEB 1
PY 2012
VL 49
IS 3
BP 579
EP 585
DI 10.1016/j.asr.2011.10.016
PG 7
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 892DA
UT WOS:000300265700018
ER
PT J
AU Martinez, O
Sankar, B
Haftka, R
Blosser, ML
AF Martinez, Oscar
Sankar, Bhavani
Haftka, Raphael
Blosser, Max L.
TI Two-Dimensional Orthotropic Plate Analysis for an Integral Thermal
Protection System
SO AIAA JOURNAL
LA English
DT Article
ID CORE SANDWICH PANELS
AB This paper is concerned with homogenization of a corrugated-core sandwich panel, which is a candidate structure for integrated thermal protection systems for space vehicles. The focus is on determining the local stresses in an integrated thermal protection system panel subjected to mechanical and thermal loads. A micromechanical method is developed to homogenize the sandwich panel as an equivalent orthotropic plate. Mechanical and thermal loads are applied to the equivalent thick plate, and the resulting plate deformations were obtained through a shear deformable plate theory. The two-dimensional plate deformations are used to obtain local integrated thermal protection system stresses through reverse homogenization. In addition, simple beam models are used to obtain local facesheet deformations and stress. The local stresses and deflections computed using the analytical method were compared with those from a detailed finite element analysis of the integrated thermal protection system. For the integrated thermal protection system examples considered in this paper, the maximum error in stresses and deflections is less than 5%. This was true for both mechanical and thermal loads acting on the integrated thermal protection system.
C1 [Blosser, Max L.] NASA, Langley Res Ctr, Met & Thermal Struct Branch, Struct Concepts & Mech Branch, Hampton, VA 23681 USA.
[Martinez, Oscar; Sankar, Bhavani; Haftka, Raphael] Univ Florida, Dept Mech & Aerosp Engn, Gainesville, FL 32611 USA.
RP Martinez, O (reprint author), Engn Sci Contract Grp, Houston, TX USA.
OI Sankar, Bhavani/0000-0002-4556-1982
FU NASA under the Constellation University
FX This research is sponsored by a NASA grant under the Constellation
University Institutes Project. The program manager is Claudia Mayer at
NASA John H. Glenn Research Center at Lewis Field.
NR 20
TC 13
Z9 17
U1 0
U2 9
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
J9 AIAA J
JI AIAA J.
PD FEB
PY 2012
VL 50
IS 2
BP 387
EP 398
DI 10.2514/1.J051172
PG 12
WC Engineering, Aerospace
SC Engineering
GA 882TO
UT WOS:000299587000012
ER
PT J
AU Kelley, CA
Poole, JA
Tazaz, AM
Chanton, JP
Bebout, BM
AF Kelley, Cheryl A.
Poole, Jennifer A.
Tazaz, Amanda M.
Chanton, Jeffrey P.
Bebout, Brad M.
TI Substrate Limitation for Methanogenesis in Hypersaline Environments
SO ASTROBIOLOGY
LA English
DT Article
DE Carbon isotopes; Methane; Evaporites; Guerrero Negro; Life in extreme
environments
ID CARBON-ISOTOPE FRACTIONATION; MICROBIAL MATS; METHANOSARCINA-BARKERI;
EVAPORATION PONDS; BAJA-CALIFORNIA; GUERRERO-NEGRO; DIVERSITY; METHANE;
SEDIMENTS; SULFATE
AB Motivated by the increasingly abundant evidence for hypersaline environments on Mars and reports of methane in its atmosphere, we examined methanogenesis in hypersaline ponds in Baja California Sur, Mexico, and in northern California, USA. Methane-rich bubbles trapped within or below gypsum/halite crusts have delta C-13 values near -40 parts per thousand. Methane with these relatively high isotopic values would typically be considered thermogenic; however, incubations of crust samples resulted in the biological production of methane with similar isotopic composition. A series of measurements aimed at understanding the isotopic composition of methane in hypersaline systems was therefore undertaken. Methane production rates, as well as the concentrations and isotopic composition of the particulate organic carbon (POC), were measured. Methane production was highest from microbial communities living within gypsum crusts, whereas POC content at gypsum/halite sites was low, generally less than 1% of the total mass. The isotopic composition of the POC ranged from -26 parts per thousand to -10 parts per thousand. To determine the substrates used by the methanogens, C-13-labeled methylamines, methanol, acetate, and bicarbonate were added to individual incubation vials, and the methane produced was monitored for C-13 content. The main substrates used by the methanogens were the noncompetitive substrates, the methylamines, and methanol. When unlabeled trimethylamine (TMA) was added to incubating gypsum/halite crusts in increasing concentrations, the isotopic composition of the methane produced became progressively lower; the lowest methane delta C-13 values occurred when the most TMA was added (1000 mu M final concentration). This decrease in the isotopic composition of the methane produced with increasing TMA concentrations, along with the high in situ methane delta C-13 values, suggests that the methanogens within the crusts are operating at low substrate concentrations. It appears that substrate limitation is decreasing isotopic fractionation during methanogenesis, which results in these abnormally high biogenic methane delta C-13 values.
C1 [Kelley, Cheryl A.; Poole, Jennifer A.] Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA.
[Tazaz, Amanda M.; Chanton, Jeffrey P.] Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA.
[Bebout, Brad M.] NASA Ames Res Ctr, Exobiol Branch, Moffett Field, CA USA.
RP Kelley, CA (reprint author), Univ Missouri, Dept Geol Sci, 101 Geol Sci Bldg, Columbia, MO 65211 USA.
EM kelleyc@missouri.edu
RI Kelley, Cheryl/K-9392-2015
FU NASA; University of Missouri's Research Board and Council
FX We would like to thank Adrienne Frisbee and Angela Detweiler for
assistance in the field and lab, and the Exportadora de Sal de C.V. and
the U.S. Fish and Wildlife Service for allowing continued access to the
study sites. Financial support from the NASA Exobiology program and the
University of Missouri's Research Board and Council is gratefully
acknowledged.
NR 43
TC 16
Z9 17
U1 1
U2 19
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 FEB
PY 2012
VL 12
IS 2
BP 89
EP 97
DI 10.1089/ast.2011.0703
PG 9
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 895UW
UT WOS:000300523100001
PM 22248383
ER
PT J
AU Crisler, JD
Newville, TM
Chen, F
Clark, BC
Schneegurt, MA
AF Crisler, J. D.
Newville, T. M.
Chen, F.
Clark, B. C.
Schneegurt, M. A.
TI Bacterial Growth at the High Concentrations of Magnesium Sulfate Found
in Martian Soils
SO ASTROBIOLOGY
LA English
DT Article
DE Analogue; Mars; Planetary protection; Salts; Life in extreme
environments
ID SPACECRAFT-ASSEMBLY FACILITY; RED HALOPHILIC BACTERIA; DEAD-SEA
HALOBACTERIUM; GREAT SALT PLAINS; DEINOCOCCUS-RADIODURANS; CLEAN ROOMS;
DESICCATION TOLERANCE; RADIATION-RESISTANT; IONIZING-RADIATION; VIKING
SPACECRAFT
AB The martian surface environment exhibits extremes of salinity, temperature, desiccation, and radiation that would make it difficult for terrestrial microbes to survive. Recent evidence suggests that martian soils contain high concentrations of MgSO4 minerals. Through warming of the soils, meltwater derived from subterranean ice-rich regolith may exist for an extended period of time and thus allow the propagation of terrestrial microbes and create significant bioburden at the near surface of Mars. The current report demonstrates that halotolerant bacteria from the Great Salt Plains (GSP) of Oklahoma are capable of growing at high concentrations of MgSO4 in the form of 2 M solutions of epsomite. The epsotolerance of isolates in the GSP bacterial collection was determined, with 35% growing at 2 M MgSO4. There was a complex physiological response to mixtures of MgSO4 and NaCl coupled with other environmental stressors. Growth also was measured at 1 M concentrations of other magnesium and sulfate salts. The complex responses may be partially explained by the pattern of chaotropicity observed for high-salt solutions as measured by agar gelation temperature. Select isolates could grow at the high salt concentrations and low temperatures found on Mars. Survival during repetitive freeze-thaw or drying-rewetting cycles was used as other measures of potential success on the martian surface. Our results indicate that terrestrial microbes might survive under the high-salt, low-temperature, anaerobic conditions on Mars and present significant potential for forward contamination. Stringent planetary protection requirements are needed for future life-detection missions to Mars.
C1 [Crisler, J. D.; Newville, T. M.; Schneegurt, M. A.] Wichita State Univ, Dept Biol Sci, Wichita, KS 67260 USA.
[Chen, F.] NASA, Planetary Protect Grp, Jet Prop Lab, Pasadena, CA USA.
[Clark, B. C.] Space Sci Inst, Boulder, CO USA.
RP Schneegurt, MA (reprint author), Wichita State Univ, Dept Biol Sci, 1845 Fairmount, Wichita, KS 67260 USA.
EM mark.schneegurt@wichita.edu
FU NASA EPSCoR (KNEP); NASA ROSES; NIH NCRR KINBRE
FX The authors appreciate the contributions of Leela Bhattarai, Todd Caton,
Amy Gray, Roger Kern, Evan Moody, Hieu Nguyen, Ashley Peppers, and Noah
Schneegurt. Awards from Kansas NASA EPSCoR (KNEP), NASA ROSES, and NIH
NCRR KINBRE supported this work.
NR 68
TC 13
Z9 13
U1 1
U2 33
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 FEB
PY 2012
VL 12
IS 2
BP 98
EP 106
DI 10.1089/ast.2011.0720
PG 9
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 895UW
UT WOS:000300523100002
PM 22248384
ER
PT J
AU Summers, DP
Basa, RCB
Khare, B
Rodoni, D
AF Summers, David P.
Basa, Ranor C. B.
Khare, Bishun
Rodoni, David
TI Abiotic Nitrogen Fixation on Terrestrial Planets: Reduction of NO to
Ammonia by FeS
SO ASTROBIOLOGY
LA English
DT Article
DE Nitrogen fixation; Mars; Earth; Terrestrial; Abiotic; Prebiotic;
Nitrogen; Planetary habitability; Biosignatures
ID MERIDIANI-PLANUM; EARLY EARTH; OPPORTUNITY ROVER; OXIDATION-STATE; EARLY
MARS; ATMOSPHERE; NITRITE; WATER; SPECTROSCOPY; ENVIRONMENT
AB Understanding the abiotic fixation of nitrogen and how such fixation can be a supply of prebiotic nitrogen is critical for understanding both the planetary evolution of, and the potential origin of life on, terrestrial planets. As nitrogen is a biochemically essential element, sources of biochemically accessible nitrogen, especially reduced nitrogen, are critical to prebiotic chemistry and the origin of life. Loss of atmospheric nitrogen can result in loss of the ability to sustain liquid water on a planetary surface, which would impact planetary habitability and hydrological processes that shape the surface. It is known that NO can be photochemically converted through a chain of reactions to form nitrate and nitrite, which can be subsequently reduced to ammonia. Here, we show that NO can also be directly reduced, by FeS, to ammonia. In addition to removing nitrogen from the atmosphere, this reaction is particularly important as a source of reduced nitrogen on an early terrestrial planet. By converting NO directly to ammonia in a single step, ammonia is formed with a higher product yield (similar to 50%) than would be possible through the formation of nitrate/nitrite and subsequent conversion to ammonia. In conjunction with the reduction of NO, there is also a catalytic disproportionation at the mineral surface that converts NO to NO2 and N2O. The NO2 is then converted to ammonia, while the N2O is released back in the gas phase, which provides an abiotic source of nitrous oxide.
C1 [Summers, David P.] NASA, Carl Sagan Ctr, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Basa, Ranor C. B.; Rodoni, David] Foothill Coll, Los Altos, CA USA.
RP Summers, DP (reprint author), NASA, Carl Sagan Ctr, SETI Inst, Ames Res Ctr, Mail Stop 239-4, Moffett Field, CA 94035 USA.
EM David.P.Summers@nasa.gov
FU NASA Astrobiology Institute [NNA04CC05A]; Exobiology Program
FX The authors would like to thank the NASA Astrobiology Institute
(NNA04CC05A) and Exobiology Program for support.
NR 42
TC 11
Z9 12
U1 3
U2 28
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 FEB
PY 2012
VL 12
IS 2
BP 107
EP 114
DI 10.1089/ast.2011.0646
PG 8
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 895UW
UT WOS:000300523100003
PM 22283408
ER
PT J
AU Gleeson, DF
Pappalardo, RT
Anderson, MS
Grasby, SE
Mielke, RE
Wright, KE
Templeton, AS
AF Gleeson, Damhnait F.
Pappalardo, R. T.
Anderson, M. S.
Grasby, S. E.
Mielke, R. E.
Wright, K. E.
Templeton, A. S.
TI Biosignature Detection at an Arctic Analog to Europa
SO ASTROBIOLOGY
LA English
DT Article
DE Europa; Biosignatures; Life detection; Analog; Biomineralization
ID INORGANIC SULFUR-COMPOUNDS; NEAR-EDGE SPECTROSCOPY; ELEMENTAL SULFUR;
MORPHOLOGICAL BIOSIGNATURES; FILAMENTOUS SULFUR; RAMAN-SPECTROSCOPY;
SUBSURFACE OCEAN; SURFACE MATERIAL; CRYSTAL-GROWTH; DEATH-VALLEY
AB The compelling evidence for an ocean beneath the ice shell of Europa makes it a high priority for astrobiological investigations. Future missions to the icy surface of this moon will query the plausibly sulfur-rich materials for potential indications of the presence of life carried to the surface by mobile ice or partial melt. However, the potential for generation and preservation of biosignatures under cold, sulfur-rich conditions has not previously been investigated, as there have not been suitable environments on Earth to study. Here, we describe the characterization of a range of biosignatures within potentially analogous sulfur deposits from the surface of an Arctic glacier at Borup Fiord Pass to evaluate whether evidence for microbial activities is produced and preserved within these deposits. Optical and electron microscopy revealed microorganisms and extracellular materials. Elemental sulfur (S-0), the dominant mineralogy within field samples, is present as rhombic and needle-shaped mineral grains and spherical mineral aggregates, commonly observed in association with extracellular polymeric substances. Orthorhombic alpha-sulfur represents the stable form of S-0, whereas the monoclinic (needle-shaped) gamma-sulfur form rosickyite is metastable and has previously been associated with sulfide-oxidizing microbial communities. Scanning transmission electron microscopy showed mineral deposition on cellular and extracellular materials in the form of submicron-sized, needle-shaped crystals. X-ray diffraction measurements supply supporting evidence for the presence of a minor component of rosickyite. Infrared spectroscopy revealed parts-per-million level organics in the Borup sulfur deposits and organic functional groups diagnostic of biomolecules such as proteins and fatty acids. Organic components are below the detection limit for Raman spectra, which were dominated by sulfur peaks. These combined investigations indicate that sulfur mineral deposits may contain identifiable biosignatures that can be stabilized and preserved under low-temperature conditions. Borup Fiord Pass represents a useful testing ground for instruments and techniques relevant to future astrobiological exploration at Europa.
C1 [Gleeson, Damhnait F.; Pappalardo, R. T.; Anderson, M. S.; Mielke, R. E.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Grasby, S. E.] Geol Survey Canada, Calgary, AB T2L 2A7, Canada.
[Wright, K. E.; Templeton, A. S.] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA.
RP Gleeson, DF (reprint author), Ctr Astrobiol CSIC INTA, Madrid 28850, Spain.
EM damhnait.gleeson@sciops.esa.int
OI Grasby, Stephen/0000-0002-3910-4443; TEMPLETON,
ALEXIS/0000-0002-9670-0647
FU NASA; NASA Astrobiology Institute; American Philosophical Society; David
and Lucile Packard Foundation; Caltech postdoctoral program; Jupiter
Europa Orbiter Project
FX We acknowledge the assistance of Benoit Beauchamp at the Arctic
Institute of North America, Calgary, Canada, and Kennda Lynch at the
Colorado School of Mines. Portions of this work were carried out at the
Jet Propulsion Laboratory, California Institute of Technology, under
contract to NASA, and were also funded in part by the NASA Astrobiology
Institute Director's Discretionary Fund. We also acknowledge financial
support from the Lewis and Clark Fund of the American Philosophical
Society, the David and Lucile Packard Foundation, the Caltech
postdoctoral program, and the Jupiter Europa Orbiter Project. We also
wish to thank our anonymous reviewers, with whose help this manuscript
has been considerably streamlined and improved overall.
NR 84
TC 7
Z9 8
U1 2
U2 50
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 FEB
PY 2012
VL 12
IS 2
BP 135
EP 150
DI 10.1089/ast.2010.0579
PG 16
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 895UW
UT WOS:000300523100006
PM 22283368
ER
PT J
AU Ackermann, M
Ajello, M
Allafort, A
Atwood, WB
Baldini, L
Barbiellini, G
Bastieri, D
Bechtol, K
Bellazzini, R
Bhat, PN
Blandford, RD
Bonamente, E
Borgland, AW
Bregeon, J
Briggs, MS
Brigida, M
Bruel, P
Buehler, R
Burgess, JM
Buson, S
Caliandro, GA
Cameron, RA
Casandjian, JM
Cecchi, C
Charles, E
Chekhtman, A
Chiang, J
Ciprini, S
Claus, R
Cohen-Tanugi, J
Connaughton, V
Conrad, J
Cutini, S
Dennis, BR
de Palma, F
Dermer, CD
Digel, SW
Silva, EDE
Drell, PS
Drlica-Wagner, A
Dubois, R
Favuzzi, C
Fegan, SJ
Ferrara, EC
Fortin, P
Fukazawa, Y
Fusco, P
Gargano, F
Germani, S
Giglietto, N
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grillo, L
Grove, JE
Gruber, D
Guiriec, S
Hadasch, D
Hayashida, M
Hays, E
Horan, D
Iafrate, G
Johannesson, G
Johnson, AS
Johnson, WN
Kamae, T
Kippen, RM
Knodlseder, J
Kuss, M
Lande, J
Latronico, L
Longo, F
Loparco, F
Lott, B
Lovellette, MN
Lubrano, P
Mazziotta, MN
McEnery, JE
Meegan, C
Mehault, J
Michelson, PF
Mitthumsiri, W
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Murphy, R
Naumann-Godo, M
Nuss, E
Nymark, T
Ohno, M
Ohsugi, T
Okumura, A
Omodei, N
Orlando, E
Paciesas, WS
Panetta, JH
Parent, D
Pesce-Rollins, M
Petrosian, V
Pierbattista, M
Piron, F
Pivato, G
Poon, H
Porter, TA
Preece, R
Raino, S
Rando, R
Razzano, M
Razzaque, S
Reimer, A
Reimer, O
Ritz, S
Sbarra, C
Schwartz, RA
Sgro, C
Share, GH
Siskind, EJ
Spinelli, P
Takahashi, H
Tanaka, T
Tanaka, Y
Thayer, JB
Tibaldo, L
Tinivella, M
Tolbert, AK
Tosti, G
Troja, E
Uchiyama, Y
Usher, TL
Vandenbroucke, J
Vasileiou, V
Vianello, G
Vitale, V
von Kienlin, A
Waite, AP
Wilson-Hodge, C
Wood, DL
Wood, KS
Yang, Z
AF Ackermann, M.
Ajello, M.
Allafort, A.
Atwood, W. B.
Baldini, L.
Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Bhat, P. N.
Blandford, R. D.
Bonamente, E.
Borgland, A. W.
Bregeon, J.
Briggs, M. S.
Brigida, M.
Bruel, P.
Buehler, R.
Burgess, J. M.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Casandjian, J. M.
Cecchi, C.
Charles, E.
Chekhtman, A.
Chiang, J.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Connaughton, V.
Conrad, J.
Cutini, S.
Dennis, B. R.
de Palma, F.
Dermer, C. D.
Digel, S. W.
do Couto e Silva, E.
Drell, P. S.
Drlica-Wagner, A.
Dubois, R.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Fortin, P.
Fukazawa, Y.
Fusco, P.
Gargano, F.
Germani, S.
Giglietto, N.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grillo, L.
Grove, J. E.
Gruber, D.
Guiriec, S.
Hadasch, D.
Hayashida, M.
Hays, E.
Horan, D.
Iafrate, G.
Johannesson, G.
Johnson, A. S.
Johnson, W. N.
Kamae, T.
Kippen, R. M.
Knoedlseder, J.
Kuss, M.
Lande, J.
Latronico, L.
Longo, F.
Loparco, F.
Lott, B.
Lovellette, M. N.
Lubrano, P.
Mazziotta, M. N.
McEnery, J. E.
Meegan, C.
Mehault, J.
Michelson, P. F.
Mitthumsiri, W.
Monte, C.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Murphy, R.
Naumann-Godo, M.
Nuss, E.
Nymark, T.
Ohno, M.
Ohsugi, T.
Okumura, A.
Omodei, N.
Orlando, E.
Paciesas, W. S.
Panetta, J. H.
Parent, D.
Pesce-Rollins, M.
Petrosian, V.
Pierbattista, M.
Piron, F.
Pivato, G.
Poon, H.
Porter, T. A.
Preece, R.
Raino, S.
Rando, R.
Razzano, M.
Razzaque, S.
Reimer, A.
Reimer, O.
Ritz, S.
Sbarra, C.
Schwartz, R. A.
Sgro, C.
Share, G. H.
Siskind, E. J.
Spinelli, P.
Takahashi, H.
Tanaka, T.
Tanaka, Y.
Thayer, J. B.
Tibaldo, L.
Tinivella, M.
Tolbert, A. K.
Tosti, G.
Troja, E.
Uchiyama, Y.
Usher, T. L.
Vandenbroucke, J.
Vasileiou, V.
Vianello, G.
Vitale, V.
von Kienlin, A.
Waite, A. P.
Wilson-Hodge, C.
Wood, D. L.
Wood, K. S.
Yang, Z.
TI FERMI DETECTION OF gamma-RAY EMISSION FROM THE M2 SOFT X-RAY FLARE ON
2010 JUNE 12f
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; Sun: flares; Sun: particle emission; Sun:
X-rays, gamma rays
ID ACCELERATED-PARTICLE INTERACTIONS; LARGE-AREA TELESCOPE;
HIGH-ENERGY-NEUTRON; SOLAR-FLARES; BURST MONITOR; ELECTRONS;
SPECTROSCOPY; CALIBRATION; ABUNDANCES; COMPTON
AB The Geostationary Operational Environmental Satellite (GOES) M2-class solar flare, SOL2010-06-12T00: 57, was modest in many respects yet exhibited remarkable acceleration of energetic particles. The flare produced an similar to 50 s impulsive burst of hard X-and gamma-ray emission up to at least 400 MeV observed by the Fermi Gamma-ray Burst Monitor and Large Area Telescope experiments. The remarkably similar hard X-ray and high-energy gamma-ray time profiles suggest that most of the particles were accelerated to energies greater than or similar to 300 MeV with a delay of similar to 10 s from mildly relativistic electrons, but some reached these energies in as little as similar to 3 s. The gamma-ray line fluence from this flare was about 10 times higher than that typically observed from this modest GOES class of X-ray flare. There is no evidence for time-extended >100 MeV emission as has been found for other flares with high-energy gamma-rays.
C1 [Ackermann, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Ajello, M.; Allafort, A.; Bechtol, K.; Blandford, R. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Glanzman, T.; Godfrey, G.; Grillo, L.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Panetta, J. H.; Petrosian, V.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. B.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.] Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Ajello, M.; Allafort, A.; Bechtol, K.; Blandford, R. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Glanzman, T.; Godfrey, G.; Grillo, L.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Panetta, J. H.; Petrosian, V.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. B.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Atwood, W. B.; Razzano, M.; Ritz, S.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Atwood, W. B.; Razzano, M.; Ritz, S.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Barbiellini, G.; Iafrate, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Buson, S.; Rando, R.; Sbarra, C.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Pivato, G.; Poon, H.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Bhat, P. N.; Briggs, M. S.; Burgess, J. M.; Connaughton, V.; Guiriec, S.; Paciesas, W. S.; Preece, R.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bruel, P.; Fegan, S. J.; Fortin, P.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Caliandro, G. A.; Hadasch, D.] Inst Ciencies Espai IEEE CSIC, Barcelona 08193, Spain.
[Casandjian, J. M.; Naumann-Godo, M.; Pierbattista, M.] Univ Paris Diderot, La AIM, CEA IRFU, CNRS,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France.
[Chekhtman, A.] Artep Inc, Ellicott City, MD 21042 USA.
[Cutini, S.] ASI, Sci Data Ctr, I-00044 Rome, Italy.
[Cohen-Tanugi, J.; Mehault, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, Lab Univers & Particules Montpellier, CNRS, IN2P3, Montpellier, France.
[Conrad, J.; Yang, Z.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Conrad, J.; Nymark, T.; Yang, Z.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Dennis, B. R.; Ferrara, E. C.; Hays, E.; McEnery, J. E.; Schwartz, R. A.; Tolbert, A. K.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Murphy, R.; Wood, K. S.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA.
[Fukazawa, Y.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Gruber, D.; Orlando, E.; von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Iafrate, G.] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34143 Trieste, Italy.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Kippen, R. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Knoedlseder, J.] IRAP, CNRS, F-31028 Toulouse 4, France.
[Knoedlseder, J.] Univ Toulouse, GAHEC, UPS OMP, IRAP, Toulouse, France.
[Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Lott, B.] Univ Bordeaux 1, CNRS, IN2P3, CEN Bordeaux Gradignan, F-33175 Gradignan, France.
[McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McEnery, J. E.; Share, G. H.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Meegan, C.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Nymark, T.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden.
[Ohno, M.; Okumura, A.; Tanaka, Y.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Parent, D.; Razzaque, S.] George Mason Univ, Ctr Earth Observing & Space Res, Coll Sci, Fairfax, VA 22030 USA.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Vianello, G.] CIFS, I-10133 Turin, Italy.
[Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Wilson-Hodge, C.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Wood, D. L.] Praxis Inc, Alexandria, VA 22303 USA.
RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
EM michael.briggs@nasa.gov; dgruber@mpe.mpg.de;
francesco.longo@trieste.infn.it; nicola.omodei@gmail.com;
gerald.share@nrl.navy.mil
RI Dennis, Brian/C-9511-2012; McEnery, Julie/D-6612-2012; Baldini,
Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Kuss,
Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Morselli,
Aldo/G-6769-2011; Gargano, Fabio/O-8934-2015; Reimer, Olaf/A-3117-2013;
Tosti, Gino/E-9976-2013; Rando, Riccardo/M-7179-2013; Johnson,
Neil/G-3309-2014; Johannesson, Gudlaugur/O-8741-2015; Loparco,
Francesco/O-8847-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario
/O-8867-2015; Sgro, Carmelo/K-3395-2016; Orlando, E/R-5594-2016
OI lubrano, pasquale/0000-0003-0221-4806; giglietto,
nicola/0000-0002-9021-2888; Morselli, Aldo/0000-0002-7704-9553; Gargano,
Fabio/0000-0002-5055-6395; Reimer, Olaf/0000-0001-6953-1385;
Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco,
Francesco/0000-0002-1173-5673; Moskalenko, Igor/0000-0001-6141-458X;
Mazziotta, Mario /0000-0001-9325-4672;
FU K. A. Wallenberg Foundation; Fermi GI program
FX Royal Swedish Academy of Sciences Research Fellow, funded by a grant
from the K. A. Wallenberg Foundation.; We thank the referee for
suggesting a more detailed examination of the delay between the hard
X-ray bremsstrahlung and >30 MeV emission observed by LAT. The Fermi LAT
Collaboration acknowledges generous ongoing support from a number of
agencies and institutes that have supported both the development and the
operation of the LAT as well as scientific data analysis. These include
the National Aeronautics and Space Administration and the Department of
Energy in the United States, the Commissariat a l'Energie Atomique and
the Centre National de la Recherche Scientifique/Institut National de
Physique Nucleaire et de Physique des Particules in France, the Agenzia
Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in
Italy, the Ministry of Education, Culture, Sports, Science and
Technology (MEXT), High Energy Accelerator Research Organization (KEK)
and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A.
Wallenberg Foundation, the Swedish Research Council and the Swedish
National Space Board in Sweden.; Co-authors Briggs, Murphy, Schwartz,
Share, and Tolbert were partially funded by the Fermi GI program to
conduct the joint spectroscopic studies presented in this paper.
NR 45
TC 27
Z9 27
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 FEB 1
PY 2012
VL 745
IS 2
AR 144
DI 10.1088/0004-637X/745/2/144
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 893AI
UT WOS:000300326800042
ER
PT J
AU Borucki, WJ
Koch, DG
Batalha, N
Bryson, ST
Rowe, J
Fressin, F
Torres, G
Caldwell, DA
Christensen-Dalsgaard, J
Cochran, WD
DeVore, E
Gautier, TN
Geary, JC
Gilliland, R
Gould, A
Howell, SB
Jenkins, JM
Latham, DW
Lissauer, JJ
Marcy, GW
Sasselov, D
Boss, A
Charbonneau, D
Ciardi, D
Kaltenegger, L
Doyle, L
Dupree, AK
Ford, EB
Fortney, J
Holman, MJ
Steffen, JH
Mullally, F
Still, M
Tarter, J
Ballard, S
Buchhave, LA
Carter, J
Christiansen, JL
Demory, BO
Desert, JM
Dressing, C
Endl, M
Fabrycky, D
Fischer, D
Haas, MR
Henze, C
Horch, E
Howard, AW
Isaacson, H
Kjeldsen, H
Johnson, JA
Klaus, T
Kolodziejczak, J
Barclay, T
Li, J
Meibom, S
Prsa, A
Quinn, SN
Quintana, EV
Robertson, P
Sherry, W
Shporer, A
Tenenbaum, P
Thompson, SE
Twicken, JD
Van Cleve, J
Welsh, WF
Basu, S
Chaplin, W
Miglio, A
Kawaler, SD
Arentoft, T
Stello, D
Metcalfe, TS
Verner, GA
Karoff, C
Lundkvist, M
Lund, MN
Handberg, R
Elsworth, Y
Hekker, S
Huber, D
Bedding, TR
Rapin, W
AF Borucki, William J.
Koch, David G.
Batalha, Natalie
Bryson, Stephen T.
Rowe, Jason
Fressin, Francois
Torres, Guillermo
Caldwell, Douglas A.
Christensen-Dalsgaard, Jorgen
Cochran, William D.
DeVore, Edna
Gautier, Thomas N., III
Geary, John C.
Gilliland, Ronald
Gould, Alan
Howell, Steve B.
Jenkins, Jon M.
Latham, David W.
Lissauer, Jack J.
Marcy, Geoffrey W.
Sasselov, Dimitar
Boss, Alan
Charbonneau, David
Ciardi, David
Kaltenegger, Lisa
Doyle, Laurance
Dupree, Andrea K.
Ford, Eric B.
Fortney, Jonathan
Holman, Matthew J.
Steffen, Jason H.
Mullally, Fergal
Still, Martin
Tarter, Jill
Ballard, Sarah
Buchhave, Lars A.
Carter, Josh
Christiansen, Jessie L.
Demory, Brice-Olivier
Desert, Jean-Michel
Dressing, Courtney
Endl, Michael
Fabrycky, Daniel
Fischer, Debra
Haas, Michael R.
Henze, Christopher
Horch, Elliott
Howard, Andrew W.
Isaacson, Howard
Kjeldsen, Hans
Johnson, John Asher
Klaus, Todd
Kolodziejczak, Jeffery
Barclay, Thomas
Li, Jie
Meibom, Soren
Prsa, Andrej
Quinn, Samuel N.
Quintana, Elisa V.
Robertson, Paul
Sherry, William
Shporer, Avi
Tenenbaum, Peter
Thompson, Susan E.
Twicken, Joseph D.
Van Cleve, Jeffrey
Welsh, William F.
Basu, Sarbani
Chaplin, William
Miglio, Andrea
Kawaler, Steven D.
Arentoft, Torben
Stello, Dennis
Metcalfe, Travis S.
Verner, Graham A.
Karoff, Christoffer
Lundkvist, Mia
Lund, Mikkel N.
Handberg, Rasmus
Elsworth, Yvonne
Hekker, Saskia
Huber, Daniel
Bedding, Timothy R.
Rapin, William
TI Kepler-22b: A 2.4 EARTH-RADIUS PLANET IN THE HABITABLE ZONE OF A
SUN-LIKE STAR
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: fundamental parameters; stars: individual
(Kepler-22, KIC 10593626)
ID MAIN-SEQUENCE STARS; TRANSIT TIMING VARIATIONS; INITIAL CHARACTERISTICS;
TERRESTRIAL PLANETS; ASTEROSEISMIC DATA; FALSE POSITIVES;
SPACE-TELESCOPE; BLEND SCENARIOS; MULTIPLE SYSTEM; CADENCE DATA
AB A search of the time-series photometry from NASA's Kepler spacecraft reveals a transiting planet candidate orbiting the 11th magnitude G5 dwarf KIC 10593626 with a period of 290 days. The characteristics of the host star are well constrained by high-resolution spectroscopy combined with an asteroseismic analysis of the Kepler photometry, leading to an estimated mass and radius of 0.970 +/- 0.060 M-circle dot and 0.979 +/- 0.020 R-circle dot. The depth of 492 +/- 10 ppm for the three observed transits yields a radius of 2.38 +/- 0.13 Re for the planet. The system passes a battery of tests for false positives, including reconnaissance spectroscopy, high-resolution imaging, and centroid motion. A full BLENDER analysis provides further validation of the planet interpretation by showing that contamination of the target by an eclipsing system would rarely mimic the observed shape of the transits. The final validation of the planet is provided by 16 radial velocities (RVs) obtained with the High Resolution Echelle Spectrometer on Keck I over a one-year span. Although the velocities do not lead to a reliable orbit and mass determination, they are able to constrain the mass to a 3 sigma upper limit of 124 M-circle plus, safely in the regime of planetary masses, thus earning the designation Kepler-22b. The radiative equilibrium temperature is 262 K for a planet in Kepler-22b's orbit. Although there is no evidence that Kepler-22b is a rocky planet, it is the first confirmed planet with a measured radius to orbit in the habitable zone of any star other than the Sun.
C1 [Borucki, William J.; Klaus, Todd] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
[Batalha, Natalie] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
[Rowe, Jason; Caldwell, Douglas A.; DeVore, Edna; Jenkins, Jon M.; Doyle, Laurance; Mullally, Fergal; Tarter, Jill; Christiansen, Jessie L.; Li, Jie; Quintana, Elisa V.; Tenenbaum, Peter; Thompson, Susan E.; Twicken, Joseph D.; Van Cleve, Jeffrey] SETI Inst, Mountain View, CA 94043 USA.
[Fressin, Francois; Torres, Guillermo; Geary, John C.; Latham, David W.; Sasselov, Dimitar; Charbonneau, David; Dupree, Andrea K.; Holman, Matthew J.; Ballard, Sarah; Desert, Jean-Michel; Dressing, Courtney; Meibom, Soren; Quinn, Samuel N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Christensen-Dalsgaard, Jorgen; Kjeldsen, Hans; Arentoft, Torben; Karoff, Christoffer; Lundkvist, Mia; Lund, Mikkel N.; Handberg, Rasmus] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Christensen-Dalsgaard, Jorgen] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA.
[Cochran, William D.; Endl, Michael; Robertson, Paul] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Gautier, Thomas N., III; Johnson, John Asher] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gilliland, Ronald] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Marcy, Geoffrey W.; Howard, Andrew W.; Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Boss, Alan] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Ciardi, David] CALTECH, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Kaltenegger, Lisa] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Fortney, Jonathan; Fabrycky, Daniel] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Steffen, Jason H.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA.
[Still, Martin; Barclay, Thomas] Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
[Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark.
[Carter, Josh; Demory, Brice-Olivier] MIT, Cambridge, MA 02139 USA.
[Fischer, Debra; Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Horch, Elliott] So Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA.
[Kolodziejczak, Jeffery] MSFC, Huntsville, AL 35805 USA.
[Prsa, Andrej] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA.
[Sherry, William] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Shporer, Avi] Las Cumbres Observ, Goleta, CA 93117 USA.
[Chaplin, William; Miglio, Andrea; Verner, Graham A.; Elsworth, Yvonne; Hekker, Saskia] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Kawaler, Steven D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50014 USA.
[Stello, Dennis; Huber, Daniel; Bedding, Timothy R.] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia.
[Metcalfe, Travis S.] White Dwarf Res Corp, Boulder, CO 80301 USA.
[Hekker, Saskia] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Rapin, William] Ctr Spatial Toulouse, Ctr Natl Etud Spatiales, F-31401 Toulouse, France.
RP Borucki, WJ (reprint author), NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
EM William.J.Borucki@nasa.gov
RI Caldwell, Douglas/L-7911-2014; Howard, Andrew/D-4148-2015;
OI Caldwell, Douglas/0000-0003-1963-9616; Howard,
Andrew/0000-0001-8638-0320; Fortney, Jonathan/0000-0002-9843-4354;
Buchhave, Lars A./0000-0003-1605-5666; Bedding,
Timothy/0000-0001-5943-1460; Metcalfe, Travis/0000-0003-4034-0416;
Ciardi, David/0000-0002-5741-3047; Karoff,
Christoffer/0000-0003-2009-7965; Demory,
Brice-Olivier/0000-0002-9355-5165; Basu, Sarbani/0000-0002-6163-3472;
/0000-0001-6545-639X; Lund, Mikkel Norup/0000-0001-9214-5642; Fischer,
Debra/0000-0003-2221-0861; Handberg, Rasmus/0000-0001-8725-4502;
Kawaler, Steven/0000-0002-6536-6367; Fabrycky,
Daniel/0000-0003-3750-0183; Lundkvist, Mia Sloth/0000-0002-8661-2571;
Bedding, Tim/0000-0001-5222-4661
FU NASA's Science Mission Directorate; W. M. Keck Foundation; NASA; NASA
through JPL/Caltech; National Center for Atmospheric Research; National
Science Foundation; Netherlands Organisation for Scientific Research
(NWO)
FX Kepler was competitively selected as the tenth Discovery mission.
Funding for this mission is provided by NASA's Science Mission
Directorate. Some of the data presented herein were obtained at the W.
M. Keck Observatory, which is operated as a scientific partnership among
the California Institute of Technology, the University of California,
and the National Aeronautics and Space Administration. The Keck
Observatory was made possible by the generous financial support of the
W. M. Keck Foundation. Some of the observations were made with the
Spitzer Space Telescope, which is operated by the Jet Propulsion
Laboratory, California Institute of Technology under a contract with
NASA. Support for this work was provided by NASA through an award issued
by JPL/Caltech. Additional support for this work was also received from
National Center for Atmospheric Research which is sponsored by the
National Science Foundation. The authors thank the many people who gave
so generously of their time to make this Mission a success. S. H.
acknowledges financial support from the Netherlands Organisation for
Scientific Research (NWO).
NR 83
TC 139
Z9 139
U1 13
U2 60
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 FEB 1
PY 2012
VL 745
IS 2
AR 120
DI 10.1088/0004-637X/745/2/120
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 893AI
UT WOS:000300326800018
ER
PT J
AU Hammer, DM
Hornschemeier, AE
Salim, S
Smith, R
Jenkins, L
Mobasher, B
Miller, N
Ferguson, H
AF Hammer, D. M.
Hornschemeier, A. E.
Salim, S.
Smith, R.
Jenkins, L.
Mobasher, B.
Miller, N.
Ferguson, H.
TI DEEP ULTRAVIOLET LUMINOSITY FUNCTIONS AT THE INFALL REGION OF THE COMA
CLUSTER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: individual (Coma); galaxies: dwarf; galaxies:
luminosity function, mass function; ultraviolet: galaxies
ID EARLY-TYPE GALAXIES; HUBBLE-SPACE-TELESCOPE; STAR-FORMATION RATES;
DIGITAL SKY SURVEY; DWARF ELLIPTIC GALAXIES; HICKSON COMPACT-GROUPS;
STELLAR POPULATIONS; NEARBY CLUSTERS; VIRGO CLUSTER; REDSHIFT SURVEY
AB We have used deep GALEX observations at the infall region of the Coma cluster to measure the faintest ultraviolet (UV) luminosity functions (LFs) presented for a rich galaxy cluster thus far. The Coma UV LFs are measured to M-UV = -10.5 in the GALEX FUV and NUV bands, or 3.5 mag fainter than previous studies, and reach the dwarf early-type galaxy population in Coma for the first time. The Schechter faint-end slopes (alpha approximate to -1.39 in both GALEX bands) are shallower than reported in previous Coma UV LF studies owing to a flatter LF at faint magnitudes. A Gaussian-plus-Schechter model provides a slightly better parameterization of the UV LFs resulting in a faint-end slope of alpha approximate to -1.15 in both GALEX bands. The two-component model gives faint-end slopes shallower than alpha = -1 (a turnover) for the LFs constructed separately for passive and star-forming galaxies. The UV LFs for star-forming galaxies show a turnover at M-UV approximate to -14 owing to a deficit of dwarf star-forming galaxies in Coma with stellar masses below M-* = 10(8) M-circle dot. A similar turnover is identified in recent UV LFs measured for the Virgo cluster suggesting this may be a common feature of local galaxy clusters, whereas the field UV LFs continue to rise at faint magnitudes. We did not identify an excess of passive galaxies as would be expected if the missing dwarf star-forming galaxies were quenched inside the cluster. In fact, the LFs for both dwarf passive and star-forming galaxies show the same turnover at faint magnitudes. We discuss the possible origin of the missing dwarf star-forming galaxies in Coma and their expected properties based on comparisons to local field galaxies.
C1 [Hammer, D. M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Hammer, D. M.; Hornschemeier, A. E.; Jenkins, L.] NASA GSFC, Lab Xray Astrophys, Greenbelt, MD 20771 USA.
[Salim, S.] Indiana Univ, Dept Astron, Bloomington, IN 47404 USA.
[Smith, R.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Mobasher, B.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[Miller, N.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Ferguson, H.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Hammer, DM (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.
OI Jenkins, Leigh/0000-0001-9464-0719; Salim, Samir/0000-0003-2342-7501
FU GALEX [05-GALEX05-0046]; Alfred P. Sloan Foundation; NASA; NSF; DoE;
Monbukagakusho; Max Planck Society; Higher Education Funding Council for
England
FX We thank the anonymous referee for their detailed comments and
suggestions that have improved this paper. We thank R. Marzke and
members of the Coma Hectospec team for their work on the redshift
catalog, and M. Colless for providing an updated version of the GMP
catalog redshifts. We are grateful for the LF data shared by A. Boselli,
M. Treyer, and M. Blanton, and assistance with the GALEV software by R.
Kotulla. We thank T. Heckman for commenting on an early draft and A.
Basu-Zych, P. Tzanavaris, and B. Lehmer for helpful science discussion.
This research was partially supported by the GALEX Cycle 2 grant
05-GALEX05-0046 (PI: A. E. Hornschemeier). GALEX is a NASA Small
Explorer, developed in cooperation with the Centre National d'Etudes
Spatiales of France and the Korean Ministry of Science and Technology.
Funding for the creation and distribution of the SDSS Archive has been
provided by the Alfred P. Sloan Foundation, the Participating
Institutions, NASA, the NSF, DoE, Monbukagakusho, Max Planck Society,
and the Higher Education Funding Council for England. The SDSS Web site
is http://www.sdss.org/. This study made use of the NASA Extragalactic
Database (NED) which is operated by the Jet Propulsion Laboratory
(Caltech), under contract with NASA.
NR 119
TC 4
Z9 4
U1 0
U2 1
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 FEB 1
PY 2012
VL 745
IS 2
AR 177
DI 10.1088/0004-637X/745/2/177
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 893AI
UT WOS:000300326800075
ER
PT J
AU Joyce, CJ
Smith, CW
Isenberg, PA
Gary, SP
Murphy, N
Gray, PC
Burlaga, LF
AF Joyce, Colin J.
Smith, Charles W.
Isenberg, Philip A.
Gary, S. Peter
Murphy, Neil
Gray, Perry C.
Burlaga, Leonard F.
TI OBSERVATION OF BERNSTEIN WAVES EXCITED BY NEWBORN INTERSTELLAR PICKUP
IONS IN THE SOLAR WIND
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic rays; magnetic fields; turbulence; waves
ID PROTON-BEAM GENERATION; MAGNETIC-FIELD; COMETARY ENVIRONMENT; OUTER
HELIOSHEATH; WHISTLER WAVES; ULF WAVES; INSTABILITIES; FLUCTUATIONS;
EXCITATION; TURBULENCE
AB A recent examination of 1.9 s magnetic field data recorded by the Voyager 2 spacecraft in transit to Jupiter revealed several instances of strongly aliased spectra suggestive of unresolved high-frequency magnetic fluctuations at 4.4 AU. A closer examination of these intervals using the highest resolution data available revealed one clear instance of wave activity at spacecraft frame frequencies from 0.2 to 1 Hz. Using various analysis techniques, we have characterized these fluctuations as Bernstein mode waves excited by newborn interstellar pickup ions. We can find no other interpretation or source consistent with the observations, but this interpretation is not without questions. In this paper, we report a detailed analysis of the waves, including their frequency and polarization, that supports our interpretation.
C1 [Joyce, Colin J.; Smith, Charles W.; Isenberg, Philip A.] Univ New Hampshire, Dept Phys, Ctr Space Sci, Durham, NH 03824 USA.
[Gary, S. Peter] Los Alamos Natl Lab, Los Alamos, NM USA.
[Murphy, Neil] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Burlaga, Leonard F.] NASA, Goddard Space Flight Ctr, Geospace Phys Lab, Greenbelt, MD 20771 USA.
RP Joyce, CJ (reprint author), Univ New Hampshire, Dept Phys, Ctr Space Sci, Durham, NH 03824 USA.
EM cjl46@unh.edu; Charles.Smith@unh.edu; Phil.Isenberg@unh.edu;
pgary@lanl.gov; Neil.Murphy@jpl.nasa.gov; Perry.Gray@dtra.mil;
lburlagahsp@verizon.net
FU NASA [NNX07AH75G]; NSF [ATM0635863]; Caltech [44A1085631]
FX This work was supported in part by NASA Guest Investigator grant
NNX07AH75G and NSF grant ATM0635863. C. W. S. is supported by Caltech
subcontract 44A1085631 to the University of New Hampshire in support of
the ACE/MAG instrument. Part of the ACE mandate is to better understand
the role of pickup ions in the heliosphere. Portions of this research
were carried out at the Jet Propulsion Laboratory, California Institute
of Technology, under a contract with the National Aeronautics and Space
Administration. C.J.J. was an undergraduate in the Physics program at
UNH at the time this work was performed and is now a graduate student
working within that same program. Perry Gray died unexpectedly just two
weeks after this paper was first submitted to the journal. He was a
bright and creative scientist who made lifelong friends everywhere he
went. He will be greatly missed by friends and colleagues alike.
NR 36
TC 10
Z9 10
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 FEB 1
PY 2012
VL 745
IS 2
AR 112
DI 10.1088/0004-637X/745/2/112
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 893AI
UT WOS:000300326800010
ER
PT J
AU Suchy, S
Furst, F
Pottschmidt, K
Caballero, I
Kreykenbohm, I
Wilms, J
Markowitz, A
Rothschild, RE
AF Suchy, Slawomir
Fuerst, Felix
Pottschmidt, Katja
Caballero, Isabel
Kreykenbohm, Ingo
Wilms, Joern
Markowitz, Alex
Rothschild, Richard E.
TI BROADBAND SPECTROSCOPY USING TWO SUZAKU OBSERVATIONS OF THE HMXB GX
301-2
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE pulsars: individual (GX 301-2); stars: magnetic field; X-rays: binaries;
X-rays: stars
ID PULSE PHASE SPECTROSCOPY; CYCLOTRON LINE ENERGY; X-RAY PULSARS; VELA
X-1; ORBITAL CYCLE; NEUTRON-STARS; LIGHT-CURVE; 1A 1118-61; GX-301-2;
HERCULES-X-1
AB We present the analysis of two Suzaku observations of GX 301-2 at two orbital phases after the periastron passage. Variations in the column density of the line-of-sight absorber are observed, consistent with accretion from a clumpy wind. In addition to a cyclotron resonance scattering feature (CRSF), multiple fluorescence emission lines were detected in both observations. The variations in the pulse profiles and the CRSF throughout the pulse phase have a signature of a magnetic dipole field. Using a simple dipole model we calculated the expected magnetic field values for different pulse phases and were able to extract a set of geometrical angles, loosely constraining the dipole geometry in the neutron star. From the variation of the CRSF width and energy, we found a geometrical solution for the dipole, making the inclination consistent with previously published values.
C1 [Suchy, Slawomir; Markowitz, Alex; Rothschild, Richard E.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Fuerst, Felix; Kreykenbohm, Ingo; Wilms, Joern] Dr Karl Remeis Sternwarte, D-96049 Bamberg, Germany.
[Fuerst, Felix; Kreykenbohm, Ingo; Wilms, Joern] Erlangen Ctr Astroparticle Phys, D-96049 Bamberg, Germany.
[Pottschmidt, Katja] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Pottschmidt, Katja] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Pottschmidt, Katja] CRESST, Greenbelt, MD 20771 USA.
[Caballero, Isabel] Univ Paris 07, CEA Saclay, DSM IRFU SAp UMR AIM 7158, CNRS CEA, Gif Sur Yvette, France.
RP Suchy, S (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr, La Jolla, CA 92093 USA.
EM ssuchy@ucsd.edu
RI Wilms, Joern/C-8116-2013; Kreykenbohm, Ingo/H-9659-2013; XRAY,
SUZAKU/A-1808-2009
OI Wilms, Joern/0000-0003-2065-5410; Kreykenbohm, Ingo/0000-0001-7335-1803;
FU NASA [NAS5-30720, NNX08AX83G]; DLR [50 OR 0808]; DAAD; French Space
Agency CNES through CNRS
FX S.S. acknowledges support by NASA contract NAS5-30720 and grant
NNX08AX83G. F. F. is supported by DLR grant 50 OR 0808 and via a DAAD
Fellowship. I. C. acknowledges financial support from the French Space
Agency CNES through CNRS. This research has made use of data obtained
from the Suzaku satellite, a collaborative mission between the space
agencies of Japan (JAXA) and the USA (NASA).
NR 52
TC 18
Z9 19
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2012
VL 745
IS 2
AR 124
DI 10.1088/0004-637X/745/2/124
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 893AI
UT WOS:000300326800022
ER
PT J
AU Thejappa, G
MacDowall, RJ
Bergamo, M
AF Thejappa, G.
MacDowall, R. J.
Bergamo, M.
TI EMISSION PATTERNS OF SOLAR TYPE III RADIO BURSTS: STEREOSCOPIC
OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: coronal mass ejections (CMEs); Sun: flares; Sun: radio radiation
ID CORONAL SCATTERING; PLASMA; DIRECTIVITY; RADIOBURSTS; SPACECRAFT;
REFRACTION; WAVES; WIND
AB Simultaneous observations of solar type III radio bursts obtained by the STEREO A, B, and WIND spacecraft at low frequencies from different vantage points in the ecliptic plane are used to determine their directivity. The heliolongitudes of the sources of these bursts, estimated at different frequencies by assuming that they are located on the Parker spiral magnetic field lines emerging from the associated active regions into the spherically symmetric solar atmosphere, and the heliolongitudes of the spacecraft are used to estimate the viewing angle, which is the angle between the direction of the magnetic field at the source and the line connecting the source to the spacecraft. The normalized peak intensities at each spacecraft R-j = I-j/Sigma I-j (the subscript j corresponds to the spacecraft STEREO A, B, and WIND), which are defined as the directivity factors are determined using the time profiles of the type III bursts. It is shown that the distribution of the viewing angles divides the type III bursts into: (1) bursts emitting into a very narrow cone centered around the tangent to the magnetic field with angular width of similar to 2 degrees and (2) bursts emitting into a wider cone with angular width spanning from similar to-100 degrees to similar to 100 degrees. The plots of the directivity factors versus the viewing angles of the sources from all three spacecraft indicate that the type III emissions are very intense along the tangent to the spiral magnetic field lines at the source, and steadily fall as the viewing angles increase to higher values. The comparison of these emission patterns with the computed distributions of the ray trajectories indicate that the intense bursts visible in a narrow range of angles around the magnetic field directions probably are emitted in the fundamental mode, whereas the relatively weaker bursts visible to a wide range of angles are probably emitted in the harmonic mode.
C1 [Thejappa, G.; Bergamo, M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[MacDowall, R. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Thejappa, G (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM thejappa.golla@nasa.gov; Robert.MacDowall@nasa.gov; mbergamo@umd.edu
RI MacDowall, Robert/D-2773-2012
FU NASA [NNX08AO02G, NNX09AB19G]
FX The research of T. G. is supported by the NASA Grants NNX08AO02G and
NNX09AB19G. The SWAVES instruments include contributions from the
Observatoire of Paris, University of Minnesota, University of
California, Berkeley, and NASA/GSFC.
NR 29
TC 9
Z9 9
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 FEB 1
PY 2012
VL 745
IS 2
AR 187
DI 10.1088/0004-637X/745/2/187
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 893AI
UT WOS:000300326800085
ER
PT J
AU Winter, LM
Veilleux, S
McKernan, B
Kallman, TR
AF Winter, Lisa M.
Veilleux, Sylvain
McKernan, Barry
Kallman, T. R.
TI THE SWIFT BURST ALERT TELESCOPE DETECTED SEYFERT 1 GALAXIES: X-RAY
BROADBAND PROPERTIES AND WARM ABSORBERS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: Seyfert; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; XMM-NEWTON OBSERVATIONS; LINE RADIO GALAXIES;
ULTRA-FAST OUTFLOWS; BLACK-HOLE MASS; INTRINSIC ABSORPTION; SPECTRAL
PROPERTIES; SUZAKU OBSERVATION; COMPTON REFLECTION; SOFT EXCESS
AB We present results from an analysis of the broadband, 0.3-195 keV, X-ray spectra of 48 Seyfert 1-1.5 sources detected in the very hard X-rays with the Swift Burst Alert Telescope (BAT). This sample is selected in an all-sky survey conducted in the 14-195 keV band. Therefore, our sources are largely unbiased toward both obscuration and host galaxy properties. Our detailed and uniform model fits to Suzaku/BAT and XMM-Newton/BAT spectra include the neutral absorption, direct power-law, reflected emission, soft excess, warm absorption, and narrow Fe I K alpha emission properties for the entire sample. We significantly detect O VII and O VIII edges in 52% of our sample. The strength of these detections is strongly correlated with the neutral column density measured in the spectrum. Among the strongest detections, X-ray grating and UV observations, where available, indicate outflowing material. The ionized column densities of sources with O VII and O VIII detections are clustered in a narrow range with N-warm similar to 10(21) cm(-2), while sources without strong detections have column densities of ionized gas an order of magnitude lower. Therefore, we note that sources without strong detections likely have warm ionized outflows present but at low column densities that are not easily probed with current X-ray observations. Sources with strong complex absorption have a strong soft excess, which may or may not be due to difficulties in modeling the complex spectra of these sources. Still, the detection of a flat Gamma similar to 1 and a strong soft excess may allow us to infer the presence of strong absorption in low signal-to-noise active galactic nucleus spectra. Additionally, we include a useful correction from the Swift BAT luminosity to bolometric luminosity, based on a comparison of our spectral fitting results with published spectral energy distribution fits from 33 of our sources.
C1 [Winter, Lisa M.] Univ Colorado, Ctr Astrophys & Space Astron, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Veilleux, Sylvain] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[McKernan, Barry] CUNY, Dept Sci, Borough Manhattan Community Coll, New York, NY 10007 USA.
[McKernan, Barry] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA.
[McKernan, Barry] CUNY, Grad Ctr, New York, NY 10016 USA.
[Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Winter, LM (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, Dept Astrophys & Planetary Sci, UCB 391, Boulder, CO 80309 USA.
RI XRAY, SUZAKU/A-1808-2009;
OI Winter, Lisa/0000-0002-3983-020X
FU NASA [NNX09AV60G]; NASA through Space Telescope Science Institute
[HST-HF-51263.01-A]; Association of Universities for Research in
Astronomy, Incorporated, under NASA [NAS5-26555]
FX L.M.W. acknowledges CU undergraduate student Tatiana Taylor for
assistance with the initial data reductions. Also, we gratefully
acknowledge support from NASA grant NNX09AV60G for Suzaku guest observer
observations and NASA grant HST-HF-51263.01-A, through a Hubble
Fellowship from the Space Telescope Science Institute, which is operated
by the Association of Universities for Research in Astronomy,
Incorporated, under NASA contract NAS5-26555. This work utilizes
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.
NR 100
TC 38
Z9 39
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD FEB 1
PY 2012
VL 745
IS 2
AR 107
DI 10.1088/0004-637X/745/2/107
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 893AI
UT WOS:000300326800005
ER
PT J
AU Polyakov, IV
Walsh, JE
Kwok, R
AF Polyakov, Igor V.
Walsh, John E.
Kwok, Ronald
TI Recent Changes of Arctic Multiyear Sea Ice Coverage and the Likely
Causes
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Editorial Material
ID OCEAN; AMPLIFICATION; THICKNESS
C1 [Polyakov, Igor V.; Walsh, John E.] Univ Alaska Fairbanks, Int Arctic Res Ctr, Fairbanks, AK 99775 USA.
[Kwok, Ronald] CALTECH, Jet Prop Lab, Pasadena, CA USA.
RP Polyakov, IV (reprint author), Univ Alaska Fairbanks, Int Arctic Res Ctr, POB 757335, Fairbanks, AK 99775 USA.
EM igor@iarc.uaf.edu
RI Kwok, Ron/A-9762-2008
OI Kwok, Ron/0000-0003-4051-5896
NR 32
TC 46
Z9 50
U1 2
U2 32
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD FEB
PY 2012
VL 93
IS 2
BP 145
EP 151
DI 10.1175/BAMS-D-11-00070.1
PG 7
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 897FP
UT WOS:000300632200004
ER
PT J
AU Evans, C
Archambault, HRM
Cordeira, JM
Fritz, C
Galarneau, TJ
Gjorgjievska, S
Griffin, KS
Johnson, A
Komaromi, WA
Monette, S
Muradyan, P
Murphy, B
Riemer, M
Sears, J
Stern, D
Tang, B
Thompson, S
AF Evans, Clark
Archambault, Heathe R. M.
Cordeira, Jason M.
Fritz, Cody
Galarneau, Thomas J., Jr.
Gjorgjievska, Saska
Griffin, Kyle S.
Johnson, Alexandria
Komaromi, William A.
Monette, Sarah
Muradyan, Paytsar
Murphy, Brian
Riemer, Michael
Sears, John
Stern, Daniel
Tang, Brian
Thompson, Segayle
TI THE PRE-DEPRESSION INVESTIGATION OF CLOUD-SYSTEMS IN THE TROPICS
(PREDICT) FIELD CAMPAIGN Perspectives of Early Career Scientists
SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY
LA English
DT Article
ID CYCLOGENESIS; OPPORTUNITIES; CYCLONES; WAVES
C1 [Evans, Clark; Tang, Brian] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Archambault, Heathe R. M.; Cordeira, Jason M.; Griffin, Kyle S.] SUNY Albany, Albany, NY 12222 USA.
[Fritz, Cody] Univ Illinois, Urbana, IL USA.
[Galarneau, Thomas J., Jr.] Univ Colorado, CIRES, Boulder, CO 80309 USA.
[Gjorgjievska, Saska] New Mexico Inst Min & Technol, Socorro, NM 87801 USA.
[Johnson, Alexandria; Muradyan, Paytsar; Murphy, Brian] Purdue Univ, W Lafayette, IN 47907 USA.
[Komaromi, William A.] Univ Miami, Coral Gables, FL 33124 USA.
[Monette, Sarah; Sears, John] Univ Wisconsin, Madison, WI USA.
[Riemer, Michael] Johannes Gutenberg Univ Mainz, Mainz, Germany.
[Stern, Daniel] Penn State Univ, State Coll, PA USA.
[Thompson, Segayle] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Evans, C (reprint author), Univ Wisconsin, Dept Math Sci, POB 413, Milwaukee, WI 53201 USA.
EM evans36@uwm.edu
RI Riemer, Michael/C-5491-2009
FU PREDICT; NCAR's Earth Observing Laboratory; NASA [NNG09HG031]; NSF
[ATM-1016095]; NOAA GOES-R [NA06NES4400002, 144PH46]
FX The ECSs involved in PREDICT are indebted to their respective advisors
and mentors for enabling their participation during the field campaign.
In addition, these experiences and this manuscript would not have been
possible were it not for the support of the PREDICT principal
investigators and the staff of NCAR's Earth Observing Laboratory.
Contributions from Kathleen Legg, Peggy Lemone, Steve Williams, and Ed
Zipser were instrumental in formulating the discussion of the roles ECSs
played during GATE. Development of the dividing streamline product was
supported in part by NASA through Grant NNG09HG031, and its
implementation was aided by discussions with and assistance from Kayo
Ide, Mike Montgomery, Scott Braun, Mark Boothe, and Saurabh Barve. The
participation of author Fritz was supported in part by NSF Grant
ATM-1016095. The participation of author Monette was supported in part
by NOAA GOES-R Proving Ground Program Contract No. NA06NES4400002, Fund
144PH46.
NR 17
TC 4
Z9 4
U1 0
U2 3
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0003-0007
J9 B AM METEOROL SOC
JI Bull. Amer. Meteorol. Soc.
PD FEB
PY 2012
VL 93
IS 2
BP 173
EP 187
DI 10.1175/BAMS-D-11-00024.1
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 897FP
UT WOS:000300632200006
ER
PT J
AU Holdeman, JD
Clisset, JR
Moder, JP
AF Holdeman, James D.
Clisset, James R.
Moder, Jeffrey P.
TI Spreadsheet calculations of jets in crossflow: opposed rows of inline
and staggered round holes
SO HEAT AND MASS TRANSFER
LA English
DT Article
ID MULTIPLE JETS; ORIFICES
AB The objective of this study was to demonstrate and analyze empirical model results for jet-in-crossflow configurations which are typical in gas turbine combustors. Calculations in this paper, for opposed rows of round holes in both inline and staggered arrangements, were made with an Excel(A (R)) spreadsheet implementation of a NASA-developed empirical model for the mean conserved scalar field. Results for cases of opposed rows of jets with the orifices on one side shifted by half the orifice spacing shows that staggering can improve the mixing, particularly for cases that would overpenetrate if the orifices were in an aligned configuration. For all cases investigated, the dimensionless variance of the mixture fraction decreased significantly with increasing downstream distance. The variation between cases at a given downstream location was smaller, but the "best" mixers for opposed rows of jets were found to be inline and staggered arrangements at an orifice spacing that is optimum for inline jets.
C1 [Holdeman, James D.; Moder, Jeffrey P.] NASA, Combust Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Clisset, James R.] Univ Florida, Gainesville, FL 32611 USA.
RP Holdeman, JD (reprint author), NASA, Combust Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM jjdholdeman@aol.com
NR 9
TC 3
Z9 3
U1 0
U2 5
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0947-7411
J9 HEAT MASS TRANSFER
JI Heat Mass Transf.
PD FEB
PY 2012
VL 48
IS 2
BP 413
EP 424
DI 10.1007/s00231-011-0913-6
PG 12
WC Thermodynamics; Mechanics
SC Thermodynamics; Mechanics
GA 889OO
UT WOS:000300083200019
ER
PT J
AU O'Brien, S
Kent, NJ
Lucitt, M
Ricco, AJ
McAtamney, C
Kenny, D
Meade, G
AF O'Brien, Sinead
Kent, Nigel J.
Lucitt, Margaret
Ricco, Antonio J.
McAtamney, Colm
Kenny, Dermot
Meade, Gerardene
TI Effective Hydrodynamic Shaping of Sample Streams in a Microfluidic
Parallel-Plate Flow-Assay Device: Matching Whole Blood Dynamic Viscosity
SO IEEE TRANSACTIONS ON BIOMEDICAL ENGINEERING
LA English
DT Article
DE Arterial shear rate; dynamic viscosity; hydrodynamic focusing;
parallel-plate flow chamber; platelets
ID VON-WILLEBRAND-FACTOR; THROMBUS FORMATION; GLOBAL ASSESSMENT; ADHESION;
ENDOTHELIUM; HEMOSTASIS; MECHANISMS; SELECTIN; CELLS; VWF
AB We report the development of an aqueous buffer system tailored to the fluidic and hemodynamic requirements of our recently reported microfluidic platelet dynamic assay device, which uses hydrodynamic focusing to "shape" a blood sample into a thin flowing layer adjacent to its protein-functionalized surface. By matching the dynamic viscosity of whole blood (3.13 +/- 0.08 mPa.s, from healthy donors), the selected buffer minimizes interfacial fluid mixing and better controls shear rate within the device, permitting platelet/protein-surface interaction assays with as little as 50 mu L of whole blood. Buffers containing the viscosity-enhancing components bovine serum albumin (BSA), gelofusine/glycine, or histopaque (Ficoll gradient solution) were found not to activate platelets when incubated with blood at concentrations up to 50%, as assessed by flow cytometry quantitation of P-selectin expression and alpha IIb beta(3) activation. In contrast, glycerol-based buffer activated platelets (two-fold increase in P-selectin levels) at concentrations as low as 10% by volume. BSA- and gelofusine/glycine-based buffers were problematic in preparation and use, and therefore, were not used beyond initial characterization. The histopaque solution selected as the best choice for flow studies stabilizes sample contact with the device's thrombogenic surface, does not activate platelets, and does not interfere with the action of agonists added to deliberately activate platelets.
C1 [O'Brien, Sinead; Lucitt, Margaret; Kenny, Dermot; Meade, Gerardene] Royal Coll Surgeons Ireland, Biomed Diagnost Inst, Dublin 2, Ireland.
[Kent, Nigel J.; Ricco, Antonio J.; McAtamney, Colm] Dublin City Univ, Biomed Diagnost Inst, Dublin 9, Ireland.
[Kent, Nigel J.] Dublin Inst Technol, Coll Engn & Built Environm, Biomed Devices & Assist Technol Res Grp, Dublin 1, Ireland.
[Ricco, Antonio J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Meade, G (reprint author), Royal Coll Surgeons Ireland, Biomed Diagnost Inst, Dublin 2, Ireland.
EM sineadobrien2@rcsi.ie; nigel.kent@dcu.ie; LUCITTM@tcd.ie;
ajricco@stanford.edu; colm.mcatamney@dcu.ie; dkenny@rcsi.ie;
gmeade@rcsi.ie
RI Kenny, Dermot/C-3898-2012; Ricco, Antonio/A-5273-2010;
OI Ricco, Antonio/0000-0002-2355-4984
FU Science Foundation Ireland [10/CE/B1821]
FX Manuscript received February 11, 2011; revised August 8, 2011; accepted
September 14, 2011. Date of publication October 19, 2011; date of
current version January 20, 2012. This work was supported by the Science
Foundation Ireland under Grant No. 10/CE/B1821.1 Asterisk
indicates corresponding author.
NR 35
TC 2
Z9 2
U1 1
U2 21
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9294
J9 IEEE T BIO-MED ENG
JI IEEE Trans. Biomed. Eng.
PD FEB
PY 2012
VL 59
IS 2
BP 374
EP 382
DI 10.1109/TBME.2011.2172607
PG 9
WC Engineering, Biomedical
SC Engineering
GA 895PF
UT WOS:000300507800010
PM 22020664
ER
PT J
AU Bradford, AL
Weller, DW
Punt, AE
Ivashchenko, YV
Burdin, AM
VanBlaricom, GR
Brownell, RL
AF Bradford, Amanda L.
Weller, David W.
Punt, Andre E.
Ivashchenko, Yulia V.
Burdin, Alexander M.
VanBlaricom, Glenn R.
Brownell, Robert L., Jr.
TI Leaner leviathans: body condition variation in a critically endangered
whale population
SO JOURNAL OF MAMMALOGY
LA English
DT Article
DE density-independence; energy reserves; environmental variability;
fitness; Okhotsk Sea; ordinal logistic regression; photo-identification;
western gray whales
ID ESCHRICHTIUS-ROBUSTUS; NUTRITIONAL CONDITION; GRAY WHALE; CONDITION
INDEXES; SAKHALIN ISLAND; HIGH AGREEMENT; FAT CONDITION; ATLANTIC FIN;
POLAR BEARS; LOW KAPPA
AB The role of environmental limitation and density-dependent regulation in shaping populations is debated in ecology. Populations at low densities may offer an unobstructed view of basic environmental and physiological interactions that impact individual fitness and thus population productivity. The energy reserves of an organism are reflected in its body condition, a measure linking individual fitness and the environment. From 1997 to 2007, we monitored the critically endangered western gray whale (Eschrichtius robustus) population on its primary summer feeding ground off the northeastern coast of Sakhalin Island, Russia. This effort resulted in a large data set of photo-identification images from 5,007 sightings of 168 individual whales that we used to visually assess western gray whale body condition. We quantified temporal variation in the resulting 1,539 monthly body condition determinations with respect to observations of reproductive status and sex. Western gray whale body condition varied annually, and we identified years of significantly better (2004) and worse ((999, 2006, and 2007) body condition. This study is the 1st to track the within-season body condition of individual whales. Body condition improved significantly as the summer progressed, although results suggest that not all whales replenish their energy stores by the end of the season. The body condition of lactating females was significantly worse than that of other whales at all times and was most often determined to be compromised. The body condition of their weaning calves exhibited no temporal variation and was consistently good. It is possible lactating females provide an energetic buffer to their offspring at the expense of their own body condition and future reproductive success. Findings from the analysis establish a foundation for quantifying links between western gray whale body condition, demographic parameters, and environmental conditions; and provide a baseline for monitoring individual and population condition of an ecosystem sentinel species in a changing environment. Overall, this study highlights the presence of density-independent environmental and physiological mechanisms that affect the abundance and growth of populations.
C1 [Weller, David W.] NOAA, Protected Resources Div, SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, La Jolla, CA 92037 USA.
[Ivashchenko, Yulia V.] Seastar Sci, Yaroslavl 150033, Russia.
[Bradford, Amanda L.] Russian Acad Sci, Far E Branch, Kamchatka Branch, Pacific Inst Geog, Petropavlovsk Kamchatski 683024, Russia.
[Brownell, Robert L., Jr.] NOAA, SW Fisheries Sci Ctr, Natl Marine Fisheries Serv, Pacific Grove, CA 93950 USA.
[Bradford, Amanda L.; Punt, Andre E.; VanBlaricom, Glenn R.] Univ Washington, Sch Aquat & Fishery Sci, Seattle, WA 98195 USA.
RP Bradford, AL (reprint author), NOAA, Protected Species Div, Pacific Isl Fisheries Sci Ctr, Natl Marine Fisheries Serv, 1601 Kapiolani Blvd,Suite 1000, Honolulu, HI 96814 USA.
EM alb992@u.washington.edu
OI Punt, Andre/0000-0001-8489-2488
FU University of Washington; Alaska Sea Life Center; Exxon Neftegas
Limited; International Fund for Animal Welfare; International Whaling
Commission; United States Marine Mammal Commission; Texas A&M University
at Galveston; National Fish and Wildlife Foundation; United States
National Marine Fisheries Service; Ocean Park Conservation Foundation;
Sakhalin Energy Investment Company; School of Aquatic and Fishery
Sciences at the University of Washington; United States Environmental
Protection Agency; Washington Cooperative Fish and Wildlife Research
Unit
FX We thank the many individuals who have provided field assistance over
the years, especially S. Blokhin, H. W. Kim, A. Lang, S. Rickards, and
G. Tsidulko. Participants in the 2006 NOAA Large Whale Health Assessment
Workshop contributed valuable feedback on the body condition assessment
protocol. N. Ellis, P. Heagerty, and R. Christensen offered useful
advice on the statistical analysis. The edits of W. Perrin and 2
anonymous reviewers improved the manuscript. Support for ALB was funded
in part by a grant from the Washington Sea Grant Program, University of
Washington, pursuant to National Oceanic and Atmospheric Administration
Graduate Fellowship Program in Population Dynamics and Marine Resource
Economics. The views expressed herein are those of the authors and do
not necessarily reflect the views of National Oceanic and Atmospheric
Administration or any of its subagencies. Support and funding for the
Russia United States western gray whale research project were provided
(in alphabetical order) by Alaska Sea Life Center, Exxon Neftegas
Limited, the International Fund for Animal Welfare, the International
Whaling Commission, the United States Marine Mammal Commission, the
Marine Mammal Research Program at Texas A&M University at Galveston, the
National Fish and Wildlife Foundation, the United States National Marine
Fisheries Service, Ocean Park Conservation Foundation, Sakhalin Energy
Investment Company, the School of Aquatic and Fishery Sciences at the
University of Washington, the United States Environmental Protection
Agency, and the Washington Cooperative Fish and Wildlife Research Unit.
The project was conducted as part of the Marine Mammal Project under
Area V: Protection of Nature and the Organization of Reserves within the
United States Russia Agreement on Cooperation in the Field of
Environmental Protection.
NR 83
TC 14
Z9 15
U1 2
U2 26
PU ALLIANCE COMMUNICATIONS GROUP DIVISION ALLEN PRESS
PI LAWRENCE
PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA
SN 0022-2372
J9 J MAMMAL
JI J. Mammal.
PD FEB
PY 2012
VL 93
IS 1
BP 251
EP 266
DI 10.1644/11-MAMM-A-091.1
PG 16
WC Zoology
SC Zoology
GA 896VE
UT WOS:000300598700023
ER
PT J
AU Villanueva, GL
Mumma, MJ
Bonev, BP
Novak, RE
Barber, RJ
DiSanti, MA
AF Villanueva, G. L.
Mumma, M. J.
Bonev, B. P.
Novak, R. E.
Barber, R. J.
DiSanti, M. A.
TI Water in planetary and cometary atmospheres: H2O/HDO transmittance and
fluorescence models
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Planetary atmospheres; Water; Comets; Mars; Fluorescence
ID MOLECULAR SPECTROSCOPIC DATABASE; THERMAL EMISSION SPECTROMETER;
INFRARED SOLAR SPECTRA; C/1996 B2 HYAKUTAKE; COMPUTED LINE LIST;
DEUTERATED WATER; ENERGY-LEVELS; ISOTOPIC CO2; ANNUAL CYCLE; HALF-WIDTHS
AB We developed a modern methodology to retrieve water (H2O) and deuterated water (HDO) in planetary and cometary atmospheres, and constructed an accurate spectral database that combines theoretical and empirical results. On the basis of a greatly expanded set of spectroscopic parameters, we built a full non-resonance cascade fluorescence model and computed fluorescence efficiencies for H2O (500 million lines) and HDO (700 million lines). The new line list was also integrated into an advanced terrestrial radiative transfer code (LBLRTM) and adapted to the CO2 rich atmosphere of Mars, for which we adopted the complex Robert-Bonamy formalism for line shapes. We retrieved water and D/H in the atmospheres of Mars, comet C/2007 W1 (Boattini), and Earth by applying the new formalism to spectra obtained with the high-resolution spectrograph NIRSPEC/Keck II atop Mauna Kea (Hawaii). The new model accurately describes the complex morphology of the water bands and greatly increases the accuracy of the retrieved abundances (and the D/H ratio in water) with respect to previously available models. The new model provides improved agreement of predicted and measured intensities for many H2O lines already identified in comets, and it identifies several unassigned cometary emission lines as new emission lines of H2O. The improved spectral accuracy permits retrieval of more accurate rotational temperatures and production rates for cometary water. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Villanueva, G. L.; Mumma, M. J.; Bonev, B. P.; DiSanti, M. A.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Villanueva, G. L.; Bonev, B. P.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Novak, R. E.] Iona Coll, Dept Phys, New Rochelle, NY 10801 USA.
[Barber, R. J.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
RP Villanueva, GL (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Mailstop 690-3, Greenbelt, MD 20771 USA.
EM Geronimo.Villanueva@nasa.gov
RI mumma, michael/I-2764-2013
FU NASA [08-PAST08-0034, 08-PATM08-0031, RTOP 344-32-07, RTOP 344-53-51];
NSF [AST-0807939]; NSF-RUI [AST-0805540]
FX GLV acknowledges support from NASA's Planetary Astronomy Program
(08-PAST08-0034) and NASA's Planetary Atmospheres Program
(08-PATM08-0031). NASA's Planetary Astronomy Program (RTOP 344-32-07)
and NASA's Astrobiology Program (RTOP 344-53-51) supported MJM. BPB
acknowledges support from the NSF Astronomy and Astrophysics Research
Grants Program (AST-0807939). NSF-RUI supported REN through Grant
(AST-0805540). We thank Dr. Alan Tokunaga and Alain Khayat for assisting
with the acquisition of Mars data in 2010, Dr. Robert Gamache for
assisting with the application of his Robert-Bonamy algorithm, and Dr.
Jonathan Tennyson and Dr. Iouli Gordon for providing critical assistance
in the interpretation of the HITEMP and SELP databases. We greatly
acknowledge the valuable insights of the reviewers that led us to an
improved manuscript. We thank the staff of the W.M. Keck Observatory
(operated as a scientific partnership among CalTech, UCLA, and NASA) for
their exceptional support throughout our long Mars and cometary
observing Programs. 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.
NR 88
TC 30
Z9 30
U1 0
U2 9
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0022-4073
EI 1879-1352
J9 J QUANT SPECTROSC RA
JI J. Quant. Spectrosc. Radiat. Transf.
PD FEB
PY 2012
VL 113
IS 3
BP 202
EP 220
DI 10.1016/j.jqsrt.2011.11.001
PG 19
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 896SK
UT WOS:000300591500001
ER
PT J
AU Roseboom, IG
Ivison, RJ
Greve, TR
Amblard, A
Arumugam, V
Auld, R
Aussel, H
Bethermin, M
Blain, A
Bock, J
Boselli, A
Brisbin, D
Buat, V
Burgarella, D
Castro-Rodriguez, N
Cava, A
Chanial, P
Chapin, E
Chapman, S
Clements, DL
Conley, A
Conversi, L
Cooray, A
Dowell, CD
Dunlop, JS
Dwek, E
Eales, S
Elbaz, D
Farrah, D
Franceschini, A
Glenn, J
Griffin, M
Halpern, M
Hatziminaoglou, E
Ibar, E
Isaak, K
Lagache, G
Levenson, L
Lu, N
Madden, S
Maffei, B
Mainetti, G
Marchetti, L
Marsden, G
Morrison, G
Mortier, AMJ
Nguyen, HT
O'Halloran, B
Oliver, SJ
Omont, A
Page, MJ
Panuzzo, P
Papageorgiou, A
Pearson, CP
Perez-Fournon, I
Pohlen, M
Rawlings, JI
Raymond, G
Rigopoulou, D
Rizzo, D
Rodighiero, G
Rowan-Robinson, M
Schulz, B
Scott, D
Seymour, N
Shupe, DL
Smith, AJ
Stevens, JA
Symeonidis, M
Trichas, M
Tugwell, KE
Vaccari, M
Valtchanov, I
Vieira, JD
Viero, MP
Vigroux, L
Wardlow, J
Wang, L
Wright, G
Xu, CK
Zemcov, M
AF Roseboom, I. G.
Ivison, R. J.
Greve, T. R.
Amblard, A.
Arumugam, V.
Auld, R.
Aussel, H.
Bethermin, M.
Blain, A.
Bock, J.
Boselli, A.
Brisbin, D.
Buat, V.
Burgarella, D.
Castro-Rodriguez, N.
Cava, A.
Chanial, P.
Chapin, E.
Chapman, S.
Clements, D. L.
Conley, A.
Conversi, L.
Cooray, A.
Dowell, C. D.
Dunlop, J. S.
Dwek, E.
Eales, S.
Elbaz, D.
Farrah, D.
Franceschini, A.
Glenn, J.
Griffin, M.
Halpern, M.
Hatziminaoglou, E.
Ibar, E.
Isaak, K.
Lagache, G.
Levenson, L.
Lu, N.
Madden, S.
Maffei, B.
Mainetti, G.
Marchetti, L.
Marsden, G.
Morrison, G.
Mortier, A. M. J.
Nguyen, H. T.
O'Halloran, B.
Oliver, S. J.
Omont, A.
Page, M. J.
Panuzzo, P.
Papageorgiou, A.
Pearson, C. P.
Perez-Fournon, I.
Pohlen, M.
Rawlings, J. I.
Raymond, G.
Rigopoulou, D.
Rizzo, D.
Rodighiero, G.
Rowan-Robinson, M.
Schulz, B.
Scott, Douglas
Seymour, N.
Shupe, D. L.
Smith, A. J.
Stevens, J. A.
Symeonidis, M.
Trichas, M.
Tugwell, K. E.
Vaccari, M.
Valtchanov, I.
Vieira, J. D.
Viero, M. P.
Vigroux, L.
Wardlow, J.
Wang, L.
Wright, G.
Xu, C. K.
Zemcov, M.
TI The Herschel Multi-tiered Extragalactic Survey: SPIRE-mm photometric
redshifts
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: high-redshift - galaxies: statistics - submillimetre: galaxies
ID DEEP-FIELD-SOUTH; GOODS-N FIELD; FAR-INFRARED PROPERTIES; BRIGHTEST
SUBMILLIMETER SOURCE; SPECTRAL ENERGY-DISTRIBUTIONS; STAR-FORMATION
HISTORY; FAINT RADIO GALAXIES; MU-M OBSERVATIONS; LABOCA SURVEY;
MIDINFRARED COUNTERPARTS
AB We investigate the potential of submmmm and submmmmradio photometric redshifts using a sample of mm-selected sources as seen at 250, 350 and 500 mu m by the SPIRE instrument on Herschel. From a sample of 63 previously identified mm sources with reliable radio identifications in the Great Observatories Origins Deep Survey North and Lockman Hole North fields, 46 (73 per cent) are found to have detections in at least one SPIRE band. We explore the observed submm/mm colour evolution with redshift, finding that the colours of mm sources are adequately described by a modified blackbody with constant optical depth tau=(/nu0)beta, where beta=+1.8 and nu 0=c/100 mu m. We find a tight correlation between dust temperature and IR luminosity. Using a single model of the dust temperature and IR luminosity relation, we derive photometric redshift estimates for the 46 SPIRE-detected mm sources. Testing against the 22 sources with known spectroscopic or good quality optical/near-IR photometric redshifts, we find submm/mm photometric redshifts offer a redshift accuracy of vertical bar Delta z vertical bar/(1+z)= 0.16 (=0.51). Including constraints from the radiofar-IR correlation, the accuracy is improved to vertical bar Delta z vertical bar/(1+z)=0.15 (=0.45). We estimate the redshift distribution of mm-selected sources finding a significant excess at z > 3 when compared to similar to 850 mu m selected samples.
C1 [Roseboom, I. G.; Farrah, D.; Oliver, S. J.; Smith, A. J.; Wang, L.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England.
[Roseboom, I. G.; Ivison, R. J.; Dunlop, J. S.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ivison, R. J.; Arumugam, V.; Ibar, E.; Wright, G.] UK Astron Technol Ctr, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Greve, T. R.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark.
[Amblard, A.; Cooray, A.; Wardlow, J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Auld, R.; Eales, S.; Griffin, M.; Isaak, K.; Papageorgiou, A.; Pohlen, M.; Raymond, G.] Cardiff Univ, Cardiff Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Aussel, H.; Bethermin, M.; Chanial, P.; Elbaz, D.; Madden, S.; Panuzzo, P.] Univ Paris Diderot, Lab AIM Paris Saclay, CE Saclay, CEA,DSM,Irfu,CNRS, F-91191 Gif Sur Yvette, France.
[Bock, J.; Dowell, C. D.; Levenson, L.; Nguyen, H. T.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Boselli, A.; Buat, V.; Burgarella, D.] Univ Aix Marseille, CNRS, Lab Astrophys Marseille, OAMP, F-13388 Marseille 13, France.
[Brisbin, D.] Cornell Univ, Ithaca, NY 14853 USA.
[Castro-Rodriguez, N.; Cava, A.; Perez-Fournon, I.] Inst Astrofis Canarias IAC, E-38200 Tenerife, Spain.
[Castro-Rodriguez, N.; Cava, A.; Perez-Fournon, I.] Univ La Laguna ULL, Dept Astrofis, E-38205 Tenerife, Spain.
[Chapin, E.; Halpern, M.; Marsden, G.; Scott, Douglas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Chapman, S.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Clements, D. L.; Mortier, A. M. J.; O'Halloran, B.; Rizzo, D.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England.
[Conley, A.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Conversi, L.; Valtchanov, I.] European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain.
[Dwek, E.] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Franceschini, A.; Mainetti, G.; Marchetti, L.; Rodighiero, G.; Vaccari, M.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy.
[Glenn, J.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Hatziminaoglou, E.] ESO, D-85748 Garching, Germany.
[Lagache, G.] Univ Paris 11, Inst Astrophys Spatiale IAS, F-91405 Orsay, France.
[Lu, N.; Schulz, B.; Shupe, D. L.; Xu, C. K.] CALTECH, Infrared Proc & Anal Ctr, JPL, Pasadena, CA 91125 USA.
[Maffei, B.] Univ Manchester, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Morrison, G.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[Morrison, G.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA.
[Omont, A.; Vigroux, L.] UPMC Univ Paris 06, Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France.
[Page, M. J.; Rawlings, J. I.; Seymour, N.; Symeonidis, M.; Tugwell, K. E.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Pearson, C. P.; Rigopoulou, D.] Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England.
[Pearson, C. P.] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada.
[Rigopoulou, D.] Univ Oxford, Oxford OX1 3RH, England.
[Stevens, J. A.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Trichas, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Roseboom, IG (reprint author), Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England.
EM igr@roe.ac.uk
RI Dwek, Eli/C-3995-2012; amblard, alexandre/L-7694-2014; Wardlow,
Julie/C-9903-2015; Ivison, R./G-4450-2011; Vaccari, Mattia/R-3431-2016;
Cava, Antonio/C-5274-2017;
OI amblard, alexandre/0000-0002-2212-5395; Wardlow,
Julie/0000-0003-2376-8971; Ivison, R./0000-0001-5118-1313; Vaccari,
Mattia/0000-0002-6748-0577; Cava, Antonio/0000-0002-4821-1275; Scott,
Douglas/0000-0002-6878-9840; Marchetti, Lucia/0000-0003-3948-7621;
Seymour, Nicholas/0000-0003-3506-5536; Bethermin,
Matthieu/0000-0002-3915-2015; Rodighiero, Giulia/0000-0002-9415-2296
FU Science and Technology Facilities Council [ST/F002858/1]; Royal Society;
European Research Council; Italian Space Agency (ASI) [I/005/07/0]; CSA
(Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI
(Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); NASA (USA)
FX LW and SJO were supported by the Science and Technology Facilities
Council (ST/F002858/1).; JSD acknowledges the support of the Royal
Society via a Wolfson Research Merit award, and the support of the
European Research Council via the award of an Advanced Grant.; AF, GM,
LM and MV were supported by the Italian Space Agency (ASI Herschel
Science Contract I/005/07/0).; SPIRE has been developed by a consortium
of institutes led by Cardiff University (UK) and including University of
Lethbridge (Canada), NAOC (China), CEA, LAM(France), IFSI, University of
Padua (Italy), IAC (Spain), Stockholm Observatory (Sweden), Imperial
College London, RAL, UCL-MSSL, UK ATC, University of Sussex (UK),
Caltech, JPL, NHSC, University of Colorado (USA). This development has
been supported by national funding agencies: CSA (Canada); NAOC (China);
CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden);
STFC (UK) and NASA (USA).
NR 89
TC 63
Z9 63
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD FEB
PY 2012
VL 419
IS 4
BP 2758
EP 2773
DI 10.1111/j.1365-2966.2011.19827.x
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 873XZ
UT WOS:000298920600002
ER
PT J
AU Fischer, DA
Schwamb, ME
Schawinski, K
Lintott, C
Brewer, J
Giguere, M
Lynn, S
Parrish, M
Sartori, T
Simpson, R
Smith, A
Spronck, J
Batalha, N
Rowe, J
Jenkins, J
Bryson, S
Prsa, A
Tenenbaum, P
Crepp, J
Morton, T
Howard, A
Beleu, M
Kaplan, Z
vanNispen, N
Sharzer, C
DeFouw, J
Hajduk, A
Neal, JP
Nemec, A
Schuepbach, N
Zimmermann, V
AF Fischer, Debra A.
Schwamb, Megan E.
Schawinski, Kevin
Lintott, Chris
Brewer, John
Giguere, Matt
Lynn, Stuart
Parrish, Michael
Sartori, Thibault
Simpson, Robert
Smith, Arfon
Spronck, Julien
Batalha, Natalie
Rowe, Jason
Jenkins, Jon
Bryson, Steve
Prsa, Andrej
Tenenbaum, Peter
Crepp, Justin
Morton, Tim
Howard, Andrew
Beleu, Michele
Kaplan, Zachary
vanNispen, Nick
Sharzer, Charlie
DeFouw, Justin
Hajduk, Agnieszka
Neal, Joe P.
Nemec, Adam
Schuepbach, Nadine
Zimmermann, Valerij
TI Planet Hunters: the first two planet candidates identified by the public
using the Kepler public archive data
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: individual: KIC 10905746; stars: individual: KIC 6185331;
planetary systems
ID CHROMOSPHERIC ACTIVITY; Y-2 ISOCHRONES; STARS; SEARCH; DWARF; KECK
AB Planet Hunters is a new citizen science project designed to engage the public in an exoplanet search using NASA Kepler public release data. In the first month after launch, users identified two new planet candidates which survived our checks for false positives. The follow-up effort included analysis of Keck HIRES spectra of the host stars, analysis of pixel centroid offsets in the Kepler data and adaptive optics imaging at Keck using NIRC2. Spectral synthesis modelling coupled with stellar evolutionary models yields a stellar density distribution, which is used to model the transit orbit. The orbital periods of the planet candidates are 9.8844 +/- 0.0087 d (KIC 10905746) and 49.7696 +/- 0.000 39 d (KIC 6185331), and the modelled planet radii are 2.65 and 8.05 R-circle plus. The involvement of citizen scientists as part of Planet Hunters is therefore shown to be a valuable and reliable tool in exoplanet detection.
C1 [Fischer, Debra A.; Brewer, John; Giguere, Matt; Sartori, Thibault; Spronck, Julien; Beleu, Michele; Kaplan, Zachary; vanNispen, Nick; Sharzer, Charlie] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Schwamb, Megan E.; Schawinski, Kevin] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Schwamb, Megan E.; Schawinski, Kevin] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA.
[Lintott, Chris; Lynn, Stuart; Simpson, Robert; Smith, Arfon] Oxford Astrophys, Oxford OX1 3RH, England.
[Lintott, Chris; Parrish, Michael; Smith, Arfon] Adler Planetarium, Chicago, IL 60605 USA.
[Sartori, Thibault] Ecole Normale Super, F-75230 Paris 05, France.
[Batalha, Natalie] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
[Jenkins, Jon; Tenenbaum, Peter] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
[Prsa, Andrej] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA.
[Crepp, Justin; Morton, Tim] CALTECH, Det Astrophys, Pasadena, CA 91125 USA.
[Howard, Andrew] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Fischer, DA (reprint author), Yale Univ, Dept Astron, New Haven, CT 06511 USA.
EM debra.fischer@yale.edu
RI Howard, Andrew/D-4148-2015;
OI Howard, Andrew/0000-0001-8638-0320; Smith, Arfon/0000-0002-3957-2474;
Brewer, John/0000-0002-9873-1471; Schawinski, Kevin/0000-0001-5464-0888;
Fischer, Debra/0000-0003-2221-0861
FU Yale University; NASA [10-OUTRCH.210-0001, PF9-00069, NAS8-03060,
NAS5-26555]; NSF [AST-100325]; Leverhulme Trust; National Aeronautics
and Space Administration; NASA Office of Space Science [NNX09AF08G]
FX DAF acknowledges funding support from Yale University and support from
the NASA Supplemental Outreach Award, 10-OUTRCH.210-0001. DAF thanks the
Yale Keck TAC for telescope time used to obtain data for this paper. MES
is supported by an NSF Astronomy and Astrophysics Postdoctoral
Fellowship under award AST-100325. Support for the work of KS was
provided by NASA through Einstein Postdoctoral Fellowship grant number
PF9-00069, issued by the Chandra X-ray Observatory Center, which is
operated by the Smithsonian Astrophysical Observatory for and on behalf
of NASA under contract NAS8-03060. The Zooniverse is supported by The
Leverhulme Trust. We gratefully acknowledge the dedication and
achievements of Kepler Science Team and all those who contributed to the
success of the mission. We acknowledge use of public release data served
by the NASA/IPAC/NExScI Star and Exoplanet Database, which is operated
by the Jet Propulsion Laboratory, California Institute of Technology,
under contract with the National Aeronautics and Space Administration.
We particularly thank the organizers (Charles Beichman, Dawn Gelino and
Carolyn Brinkman) and lecturers (David Ciardi, Stephen Kane and Kaspar
von Braun) at the 2010 July Sagan Summer Workshop for providing
information and guidance that led to the inspiration for the Planet
Hunters site. The Kepler public release data is primarily hosted by the
Multimission Archive (MAST) at the Space Telescope Science Institute
(STScI) 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. This research has made use of NASA's Astrophysics Data
System Bibliographic Services.
NR 27
TC 50
Z9 50
U1 1
U2 13
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD FEB
PY 2012
VL 419
IS 4
BP 2900
EP 2911
DI 10.1111/j.1365-2966.2011.19932.x
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 873XZ
UT WOS:000298920600013
ER
PT J
AU Balona, LA
Lenz, P
Antoci, V
Bernabei, S
Catanzaro, G
Daszynska-Daszkiewicz, J
Di Criscienzo, M
Grigahcene, A
Handler, G
Kurtz, DW
Marconi, M
Molenda-Zakowicz, J
Moya, A
Nemec, JM
Pigulski, A
Pricopi, D
Ripepi, V
Smalley, B
Suarez, JC
Suran, M
Hall, JR
Kinemuchi, K
Klaus, TC
AF Balona, L. A.
Lenz, P.
Antoci, V.
Bernabei, S.
Catanzaro, G.
Daszynska-Daszkiewicz, J.
Di Criscienzo, M.
Grigahcene, A.
Handler, G.
Kurtz, D. W.
Marconi, M.
Molenda-Zakowicz, J.
Moya, A.
Nemec, J. M.
Pigulski, A.
Pricopi, D.
Ripepi, V.
Smalley, B.
Suarez, J. C.
Suran, M.
Hall, J. R.
Kinemuchi, K.
Klaus, T. C.
TI Kepler observations of the high-amplitude d Scuti star V2367 Cyg
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: individual: V2367 Cyg; stars: oscillations; stars: variables:
delta Scuti
ID STELLAR EVOLUTION CALCULATIONS; DELTA-SCUTI; VARIABLE-STARS; INITIAL
CHARACTERISTICS; CLASSICAL CEPHEIDS; INSTABILITY STRIP; PETERSEN
DIAGRAMS; ROTATING STARS; PERIOD RATIOS; CADENCE DATA
AB We analyse Kepler observations of the high-amplitude d Scuti (HADS) star V2367 Cyg (KIC 9408694). The variations are dominated by a mode with frequency f1= 5.6611 d-1. Two other independent modes with f2= 7.1490 d-1 and f3= 7.7756 d-1 have amplitudes an order of magnitude smaller than f1. Nearly all the light variation is due to these three modes and their combination frequencies, but several hundred other frequencies of very low amplitude are also present. The amplitudes of the principal modes may vary slightly with time. The star has twice the projected rotational velocity of any other HADS star, which makes it unusual. We find a correlation between the phases of the combination frequencies and their pulsation frequencies, which is not understood. Since modes of highest amplitude in HADS stars are normally radial modes, we assumed that this would also be true in this star. However, attempts to model the observed frequencies as radial modes without mode interaction were not successful. For a star with such a relatively high rotational velocity, it is important to consider the effect of mode interaction. Indeed, when this was done, we were able to obtain a model in which a good match with f1 and f2 is obtained, with f1 being the fundamental radial mode.
C1 [Balona, L. A.] S African Astron Observ, ZA-7935 Cape Town, South Africa.
[Lenz, P.; Handler, G.] Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
[Antoci, V.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Bernabei, S.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
[Catanzaro, G.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy.
[Daszynska-Daszkiewicz, J.; Molenda-Zakowicz, J.; Pigulski, A.] Uniwersytet Wroclawski, Inst Astron, PL-51622 Wroclaw, Poland.
[Di Criscienzo, M.] INAF Osservatorio Astron Roma, I-00040 Rome, Italy.
[Grigahcene, A.] Univ Porto, Fac Ciencias, Ctr Astrofis, P-4150762 Oporto, Portugal.
[Kurtz, D. W.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England.
[Marconi, M.; Ripepi, V.] INAF Osservatorio Astron Capodimonte, I-80131 Naples, Italy.
[Moya, A.] Dept Astrofis, Madrid 28691, Spain.
[Nemec, J. M.] Camosun Coll, Dept Phys & Astron, Victoria, BC V8P 5J2, Canada.
[Pricopi, D.; Suran, M.] Acad Romana, Astron Inst, Bucharest, Romania.
[Smalley, B.] Univ Keele, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Suarez, J. C.] Inst Astrofis Andalucia CSIC, Granada, Spain.
[Hall, J. R.; Kinemuchi, K.; Klaus, T. C.] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
RP Balona, LA (reprint author), S African Astron Observ, POB 9, ZA-7935 Cape Town, South Africa.
EM lab@saao.ac.za
RI Suarez, Juan Carlos/C-1015-2009;
OI Suarez, Juan Carlos/0000-0003-3649-8384; Antoci,
Victoria/0000-0002-0865-3650; Marconi, Marcella/0000-0002-1330-2927
FU NASA's Science Mission Directorate; South African Astronomical
Observatory; Polish MNiSW [N N203 379 636, N N203 302635]; Polish grant
[N N203 405139]; Austrian Fonds zur Forderung der wissenschaftlichen
Forschung [P20526-N16]; Astro-Madrid [CAMS2009/ESP-1496]; Spanish grant
[ESP2007-65475-C02-02, AYA 2010-21161-C02-02, CSD2006-00070]
FX The authors wish to thank the Kepler team for their generosity in
allowing the data to be released to the Kepler Asteroseismic Science
Consortium ahead of public release and for their outstanding efforts
which have made these results possible. Funding for the Kepler mission
is provided by NASA's Science Mission Directorate.; LAB wishes to thank
the South African Astronomical Observatory for financial support. PL
acknowledges partial financial support from the Polish MNiSW grant N
N203 379 636; AP acknowledges the Polish MNiSzW grant N N203 302635 and
JM-Z acknowledges the Polish grant N N203 405139. VA and GH were
supported by the Austrian Fonds zur Forderung der wissenschaftlichen
Forschung under grant P20526-N16. AM acknowledges the funding of
Astro-Madrid (CAMS2009/ESP-1496) and the Spanish grants
ESP2007-65475-C02-02, AYA 2010-21161-C02-02 and CSD2006-00070.
NR 63
TC 12
Z9 12
U1 0
U2 8
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD FEB
PY 2012
VL 419
IS 4
BP 3028
EP 3038
DI 10.1111/j.1365-2966.2011.19939.x
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 873XZ
UT WOS:000298920600022
ER
PT J
AU Miller, NA
O'Steen, R
Yen, S
Kuntz, KD
Hammer, D
AF Miller, Neal A.
O'Steen, Richard
Yen, Steffi
Kuntz, K. D.
Hammer, Derek
TI Using the XMM-Newton Optical Monitor to Study Cluster Galaxy Evolution
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID DIGITAL-SKY-SURVEY; STAR-FORMATION RATES; COLOR-MAGNITUDE DIAGRAM; DATA
RELEASE; STELLAR POPULATIONS; DUST ATTENUATION; LOCAL UNIVERSE; RICH
CLUSTERS; SDSS FILTERS; MILKY-WAY
AB We explore the application of XMM-Newton Optical Monitor (XMM-OM) ultraviolet (UV) data to study galaxy evolution. Our sample is constructed as the intersection of all Abell clusters with z < 0.05 and having archival XMM-OM data in either the UVM2 or UVW1 filters, plus optical and UV photometry from the Sloan Digital Sky Survey and GALEX, respectively. The 11 resulting clusters include 726 galaxies with measured redshifts, 520 of which have redshifts placing them within their parent Abell clusters. We develop procedures for manipulating the XMM-OM images and measuring galaxy photometry from them, and we confirm our results via comparison with published catalogs. Color-magnitude diagrams (CMDs) constructed using the XMM-OM data along with SDSS optical data show promise for evolutionary studies, with good separation between red and blue sequences and real variation in the width of the red sequence that is likely indicative of differences in star formation history. This is particularly true for UVW1 data, as the relative abundance of data collected using this filter and its depth make it an attractive choice. Available tools that use stellar synthesis libraries to fit the UV and optical photometric data may also be used, thereby better describing star formation history within the past billion years and providing estimates of total stellar mass that include contributions from young stars. Finally, color-color diagrams that include XMM-OM UV data appear useful to the photometric identification of both extragalactic and stellar sources.
C1 [Miller, Neal A.; Yen, Steffi] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[O'Steen, Richard] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA.
[Kuntz, K. D.; Hammer, Derek] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Kuntz, K. D.; Hammer, Derek] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA.
RP Miller, NA (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
EM nmiller@astro.umd.edu
FU NASA [NNX09AC76G]; ESA member states; Alfred P. Sloan Foundation;
National Science Foundation; US Department of Energy; Japanese
Monbukagakusho; Max Planck Society
FX N.A.M. gratefully acknowledges the support for this work, which was
provided by NASA Astrophysics Data Analysis Program grant NNX09AC76G. We
thank Antonio Talavera for his excellent work with XMM-OM calibration
and the confirmation of an exposure time error for A2063, and we thank
the anonymous referee for insightful comments that have improved the
analysis and discussion. 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 and 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. The
analysis in this article was based on observations obtained with
XMM-Newton, an ESA science mission with instruments and contributions
directly funded by ESA member states and NASA. Funding for the Sloan
Digital Sky Survey (SDSS) has been provided by the Alfred P. Sloan
Foundation, the participating institutions, the National Aeronautics and
Space Administration, the National Science Foundation, the US Department
of Energy, the Japanese Monbukagakusho, and the Max Planck Society. The
SDSS is managed by the Astrophysical Research Consortium (ARC) for the
participating institutions. The participating institutions are The
University of Chicago, Fermilab, the Institute for Advanced Study, the
Japan Participation Group, The Johns Hopkins University, the Korean
Scientist Group, Los Alamos National Laboratory, the
Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for
Astrophysics (MPA), New Mexico State University, University of
Pittsburgh, University of Portsmouth, Princeton University, the United
States Naval Observatory, and the University of Washington.
NR 51
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
EI 1538-3873
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD FEB
PY 2012
VL 124
IS 912
BP 95
EP 113
DI 10.1086/664187
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 897IB
UT WOS:000300641300001
ER
PT J
AU Patel, ZS
Grugan, KD
Rustgi, AK
Cucinotta, FA
Huff, JL
AF Patel, Zarana S.
Grugan, Katharine D.
Rustgi, Anil K.
Cucinotta, Francis A.
Huff, Janice L.
TI Ionizing Radiation Enhances Esophageal Epithelial Cell Migration and
Invasion Through a Paracrine Mechanism Involving Stromal-Derived
Hepatocyte Growth Factor
SO RADIATION RESEARCH
LA English
DT Article
ID PANCREATIC-CANCER CELLS; TUMOR MICROENVIRONMENT; IN-VITRO;
BREAST-CANCER; MET; FIBROBLASTS; CARCINOMA; INTERLEUKIN-8; METASTASIS;
ACTIVATION
AB Esophageal cancer is the sixth leading cause of cancer death worldwide and the seventh leading cause of cancer death in the U.S. male population. Ionizing radiation exposure is a risk factor for development of esophageal squamous cell carcinoma, a histological subtype of esophageal cancer that is highly aggressive and is associated with poor patient prognosis. This study investigated the effects of ionizing radiation on the microenvironment and intercellular communication as it relates to esophageal carcinogenesis. We demonstrate that normal esophageal epithelial cells exhibited increased migration and invasion when cultured in the presence of irradiated stromal fibroblasts or with conditioned medium derived from irradiated stromal fibroblasts. Cytokine antibody arrays and ELISAs were used to identify hepatocyte growth factor (HGF) as an abundant protein that is secreted by esophageal fibroblasts at twofold increased levels in culture medium after gamma irradiation. Reverse transcription qPCR analysis confirmed an approximately 50% increase in mRNA levels for HGF at 1 h in irradiated fibroblasts compared to unirradiated controls. Recombinant HGF stimulated increased wound healing, migration and invasion of esophageal epithelial cells, while blocking antibodies against HGF significantly decreased migration and invasion of epithelial cells in coculture with irradiated fibroblasts. Since HGF is known to direct cell migration, invasion and metastasis in a variety of tissues, including the esophagus, its modulation by ionizing radiation may have important implications for nontargeted pathways that influence radiation carcinogenesis in the esophagus. (C) 2012 by Radiation Research Society
C1 [Cucinotta, Francis A.; Huff, Janice L.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
[Patel, Zarana S.; Huff, Janice L.] Univ Space Res Assoc, Div Space Life Sci, Houston, TX 77058 USA.
[Grugan, Katharine D.; Rustgi, Anil K.] Univ Penn, Div Gastroenterol, Dept Med, Abramson Canc Ctr, Philadelphia, PA 19104 USA.
[Grugan, Katharine D.; Rustgi, Anil K.] Univ Penn, Div Gastroenterol, Dept Genet, Abramson Canc Ctr, Philadelphia, PA 19104 USA.
[Grugan, Katharine D.] Centocor R&D, Radnor, PA 19087 USA.
RP Huff, JL (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy,Mail Code SK-SRPE-B37, Houston, TX 77058 USA.
EM janice.l.huff@nasa.gov
FU NASA [NNJ06HG25A]; American Cancer Society; NIH/NDDK [P30-DK050306];
NIH/NRSA [F32DK-082149-01]; NIH/NCI [P01-CA098101]
FX This work was supported by a grant from NASA NNJ06HG25A (JLH), NIH/NCI
P01-CA098101 (AKR), American Cancer Society Research Professorship
(AKR), NIH/NDDK P30-DK050306 (Cell Culture Core), and NIH/NRSA
F32DK-082149-01 (KDG).
NR 52
TC 6
Z9 6
U1 1
U2 9
PU RADIATION RESEARCH SOC
PI LAWRENCE
PA 810 E TENTH STREET, LAWRENCE, KS 66044 USA
SN 0033-7587
J9 RADIAT RES
JI Radiat. Res.
PD FEB
PY 2012
VL 177
IS 2
BP 200
EP 208
DI 10.1667/RR2790.1
PG 9
WC Biology; Biophysics; Radiology, Nuclear Medicine & Medical Imaging
SC Life Sciences & Biomedicine - Other Topics; Biophysics; Radiology,
Nuclear Medicine & Medical Imaging
GA 896AR
UT WOS:000300538300007
PM 22077339
ER
PT J
AU Pucci, S
Poletto, G
Sterling, AC
Romoli, M
AF Pucci, Stefano
Poletto, Giannina
Sterling, Alphonse C.
Romoli, Marco
TI SOLAR POLAR X-RAY JETS AND MULTIPLE BRIGHT POINTS: EVIDENCE FOR
SYMPATHETIC ACTIVITY
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: activity; Sun: corona
ID IMAGING SPECTROMETER; CORONAL HOLES; TELESCOPE; HINODE
AB We present an analysis of X-ray bright points (BPs) and X-ray jets observed by Hinode/X-Ray Telescope on 2007 November 2-4, within the solar northern polar coronal hole. After selecting small subregions that include several BPs, we followed their brightness evolution over a time interval of a few hours, when several jets were observed. We find that most of the jets occurred in close temporal association with brightness maxima in multiple BPs: more precisely, most jets are closely correlated with the brightening of at least two BPs. We suggest that the jets result from magnetic connectivity changes that also induce the BP variability. We surmise that the jets and implied magnetic connectivity we describe are small-scale versions of the active-region-scale phenomenon, whereby flares and eruptions are triggered by interacting bipoles.
C1 [Pucci, Stefano; Romoli, Marco] Univ Florence, Dept Phys & Astron, Florence, Italy.
[Poletto, Giannina] INAF Arcetri Astrophys Observ, Florence, Italy.
[Sterling, Alphonse C.] Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
RP Pucci, S (reprint author), Univ Florence, Dept Phys & Astron, Florence, Italy.
EM stpucci@arcetri.astro.it
RI Romoli, Marco/H-6859-2012
FU ASI [I/023/09/0]; NASA's Science Mission Directorate
FX We thank R. Moore for useful discussions and the anonymous referee for
his/her constructive comments to the Letter. S.P. and G.P. acknowledge
support from ASI I/023/09/0. A.C.S. was supported by funding from NASA's
Science Mission Directorate through the Solar Physics SR&T and the LWS
TR&T programs. Hinode is a Japanese mission developed and launched by
ISAS/JAXA, collaborating with NAOJ as a domestic partner, NASA and STFC
(UK) as international partners. It is operated by these agencies in
cooperation with ESA and NSC (Norway).
NR 18
TC 3
Z9 3
U1 0
U2 2
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 FEB 1
PY 2012
VL 745
IS 2
AR L31
DI 10.1088/2041-8205/745/2/L31
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 891PJ
UT WOS:000300228800016
ER
PT J
AU Rezgui, S
Wilcox, EP
Lee, P
Carts, MA
Label, K
Nguyen, V
Telecco, N
McCollum, J
AF Rezgui, Sana
Wilcox, Edward P.
Lee, Poongyeub
Carts, Martin A.
Label, Kenneth
Victor Nguyen
Telecco, Nicola
McCollum, John
TI Investigation of Low Dose Rate and Bias Conditions on the Total Dose
Tolerance of a CMOS Flash-Based FPGA
SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE
LA English
DT Article
DE Annealing; CMOS; floating gate devices; low-dose rate tests;
reprogrammable flash-based FPGAs; TID
ID GATE; MEMORIES
AB TID test results of CMOS Flash-based FPGAs in gamma-rays are presented. The use of realistic low dose-rates and oriented bias-conditions are shown to extend the FPGA TID tolerance. Implications to qualification methods and to most of the new CMOS technologies are noted.
C1 [Rezgui, Sana; Wilcox, Edward P.; Victor Nguyen; Telecco, Nicola; McCollum, John] Microsemi Corp, Mountain View, CA 94043 USA.
[Wilcox, Edward P.] MEI Technol NASA GSFC, Greenbelt, MD 20771 USA.
[Carts, Martin A.] Radiat Effects & Anal Grp, Greenbelt, MD 20771 USA.
[Label, Kenneth] NASA GSFC, Greenbelt, MD 20771 USA.
RP Rezgui, S (reprint author), Microsemi Corp, Mountain View, CA 94043 USA.
EM sana.rezgui@microsemi.com; ted.wilcox@nasa.gov;
poongyeub.lee@microsemi.com; martin.a.carts@nasa.gov;
ken.label@nasa.gov; victor.nguyen@microsemi.com;
nicola.telecco@microsemi.com; john.mc-collum@microsemi.com
FU NASA EEE Parts and Packaging (NEPP)
FX Manuscript received July 23, 2011; revised September 18, 2011, October
10, 2011, October 15, 2011, and November 25, 2011; accepted November 28,
2011. Date of publication January 31, 2012; date of current version
February 10, 2012. This work was supported by NASA EEE Parts and
Packaging (NEPP) Program.
NR 16
TC 3
Z9 4
U1 1
U2 7
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0018-9499
J9 IEEE T NUCL SCI
JI IEEE Trans. Nucl. Sci.
PD FEB
PY 2012
VL 59
IS 1
BP 134
EP 143
DI 10.1109/TNS.2011.2179316
PN 2
PG 10
WC Engineering, Electrical & Electronic; Nuclear Science & Technology
SC Engineering; Nuclear Science & Technology
GA 894JN
UT WOS:000300423100001
ER
PT J
AU Cho, MG
Cooke, D
Ferguson, D
Garrett, HB
Hilgers, A
Lai, ST
Roussel, JF
Wheelock, A
AF Cho, Mengu
Cooke, David
Ferguson, Dale
Garrett, Henry B.
Hilgers, Alain
Lai, Shu T.
Roussel, Jean-Francois
Wheelock, Adrian
TI Special Issue on Spacecraft Charging Technology 2012
SO IEEE TRANSACTIONS ON PLASMA SCIENCE
LA English
DT Editorial Material
C1 [Cho, Mengu] Kyushu Inst Technol, Kitakyushu, Fukuoka 8048550, Japan.
[Cooke, David; Ferguson, Dale; Wheelock, Adrian] USAF, Res Lab, Albuquerque, NM 87117 USA.
[Garrett, Henry B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hilgers, Alain] ESA, NL-2200 AG Noordwijk, Netherlands.
[Lai, Shu T.] MIT, Space Prop Lab, Cambridge, MA 02139 USA.
[Roussel, Jean-Francois] Off Natl Etud & Rech Aerosp, F-31055 Toulouse, France.
RP Cho, MG (reprint author), Kyushu Inst Technol, Kitakyushu, Fukuoka 8048550, Japan.
NR 0
TC 0
Z9 0
U1 1
U2 5
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0093-3813
J9 IEEE T PLASMA SCI
JI IEEE Trans. Plasma Sci.
PD FEB
PY 2012
VL 40
IS 2
SI SI
BP 138
EP 138
DI 10.1109/TPS.2011.2180452
PN 1
PG 1
WC Physics, Fluids & Plasmas
SC Physics
GA 894LS
UT WOS:000300428800001
ER
PT J
AU Garrett, HB
Katz, I
Jun, I
Kim, W
Whittlesey, AC
Evans, RW
AF Garrett, Henry. B.
Katz, Ira
Jun, Insoo
Kim, Wousik
Whittlesey, Albert C.
Evans, Robin W.
TI The Jovian Charging Environment and Its Effects-A Review
SO IEEE TRANSACTIONS ON PLASMA SCIENCE
LA English
DT Review
DE Aurora; internal electrostatic discharge (IESD); Jupiter; space plasma;
spacecraft charging; vxB
ID JUPITER
AB Several space missions are being considered for Jupiter. These range from the recently launched Juno mission to possible joint NASA and ESA missions to Europa and Ganymede. Although the direct effects of radiation dose are normally considered the most pressing design issue for these missions, spacecraft charging, through surface charging, vxB, and, more importantly, internal charging, is also a key design concern. This paper reviews the current state of understanding of the jovian charging environment including the background plasma, high-energy electrons, and magnetic field. In conjunction with these environments, we will also review the range of effects to be expected in response to these environments. These effects need to be carefully considered in parallel with radiation effects in the design of the planned missions if they are to survive in the extremely challenging jovian environment.
C1 [Garrett, Henry. B.; Katz, Ira; Jun, Insoo; Kim, Wousik; Whittlesey, Albert C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Evans, Robin W.] Mori Associates, Montrose, CA 91020 USA.
RP Garrett, HB (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM henry.b.garrett@jpl.nasa.gov; ira.katz@jpl.nasa.gov;
insoo.jun@jpl.nasa.gov; wousik.kim@jpl.nasa.gov;
albert.whittlesey@jpl.nasa.gov; robin.w.evans@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX Copyright 2011. All rights reserved. We would like to acknowledge our
many colleagues who have contributed to this effort. Of particular note
are our two colleagues Drs. Robb Frederickson and N. J. Stevens who made
fundamental contributions to our field. Their loss is greatly regretted.
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 20
TC 2
Z9 2
U1 0
U2 7
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0093-3813
EI 1939-9375
J9 IEEE T PLASMA SCI
JI IEEE Trans. Plasma Sci.
PD FEB
PY 2012
VL 40
IS 2
SI SI
BP 144
EP 154
DI 10.1109/TPS.2011.2171369
PN 1
PG 11
WC Physics, Fluids & Plasmas
SC Physics
GA 894LS
UT WOS:000300428800003
ER
PT J
AU Mandell, MJ
Davis, VA
Davis, GT
Maurer, RH
Herrmann, C
AF Mandell, Myron J.
Davis, V. A.
Davis, G. T.
Maurer, R. H.
Herrmann, C.
TI Photoemission Driven Charging in Tenuous Plasma
SO IEEE TRANSACTIONS ON PLASMA SCIENCE
LA English
DT Article
DE Photoemission; spacecraft charging
ID LONG-TERM; SPACECRAFT; SURFACE; PROBE; DENSITY; CLUSTER; PLATE
AB In the cold, tenuous plasma commonly encountered in magnetospheric and interplanetary orbits, and in the case of scientific satellites with nearly all surfaces effectively conducting, surface charging is driven by photoemission current. The differential potential of the few insulating surfaces, such as lenses or insulating grout between solar cells, can be positive or negative depending on the photoemissivity of the material. We analyze this effect for spacecraft like those of the Magnetospheric MultiScale and the Radiation Belt Storm Probes missions. This paper develops a simple theory for the potentials of sunlit insulators, focusing on insulators that make up a small part of a large conductive surface. The shape of the photoemission spectrum places an absolute limit of about 12 V of positive differential charging on sunlit insulators. For small insulating surfaces, the conventional assumption-that the photoelectronsthat cannot energetically escape return to their surface of origin-is not valid because the photoelectron trajectory path length is large compared with the surface dimension. We describe a theory that accounts for photoelectron transport between small insulators and the surrounding conductive area. These calculations are done both for the case that the insulator has photoemission similar to the conductive area and for the case that the photoemission is far less, as is the case for many insulators. If the insulator has photoemission current density similar to that of a conductor, we predict positive differential potentials of about 2 V at low chassis potential and negligible differential at high chassis potential. In the opposite case that the insulator photoemission is low, we predict no differential at low chassis potentials and negative differential potentials of up to several volts at high chassis potential.
C1 [Mandell, Myron J.; Davis, V. A.] Sci Applicat Int Corp, San Diego, CA 92121 USA.
[Davis, G. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Maurer, R. H.; Herrmann, C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Mandell, MJ (reprint author), Sci Applicat Int Corp, San Diego, CA 92121 USA.
EM Myron.j.mandell@saic.com; victoria.a.davis@saic.com;
victoria.a.davis@saic.com; Richard.Maurer@jhuapl.edu;
Carl.Herrman@jhuapl.edu
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
FU Johns Hopkins University Applied Physics Laboratory; ADNET Systems, Inc.
FX This research was carried out under contracts with the Johns Hopkins
University Applied Physics Laboratory and ADNET Systems, Inc.
NR 19
TC 2
Z9 2
U1 0
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0093-3813
J9 IEEE T PLASMA SCI
JI IEEE Trans. Plasma Sci.
PD FEB
PY 2012
VL 40
IS 2
SI SI
BP 209
EP 216
DI 10.1109/TPS.2011.2179675
PN 1
PG 8
WC Physics, Fluids & Plasmas
SC Physics
GA 894LS
UT WOS:000300428800010
ER
PT J
AU Davis, VA
Mandell, MJ
Baker, NR
Brown-Hayes, M
Davis, GT
Maurer, RH
Herrmann, C
AF Davis, V. A.
Mandell, M. J.
Baker, N. R.
Brown-Hayes, M.
Davis, G. T.
Maurer, R. H.
Herrmann, C.
TI Surface-Charging Analysis of the Radiation Belt Storm Probe and
Magnetospheric MultiScale Spacecraft
SO IEEE TRANSACTIONS ON PLASMA SCIENCE
LA English
DT Article
DE Aeorspace simulation; electric field measurements; plasma measurements;
spacecraft charging; space environment effects; space-plasma
environment; space plasma interactions
ID GEOSYNCHRONOUS ORBIT
AB The Radiation Belt Storm Probes (RBSPs) are a pair of satellites to be launched in 2012 into 500 x 30 600 km 10 degrees-inclination orbits. The Magnetospheric MultiScale (MMS) mission spacecraft are a set of four satellites to be launched in 2014 into 1300 x 70 000 km (1.2 x 12 Re) 28 degrees-inclination orbits. The apogee will be boosted to 150 000 km (25 Re) during the mission. The spacecraft of both missions will measure magnetic and electric fields and the charged-particle distribution. As measurements of low-energy plasma and of electric fields are sensitive to surface potentials, stringent requirements for electrostatic cleanliness are imposed on both spacecraft designs. We present a surface-charging analysis of the RBSP and MMS spacecraft designs. The resulting chassis and differential potentials are used to estimate spacecraft-generated effects on the measurements and the risk of arcing.
C1 [Davis, V. A.; Mandell, M. J.; Baker, N. R.; Brown-Hayes, M.] Sci Applicat Int Corp, San Diego, CA 92121 USA.
[Davis, G. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Maurer, R. H.; Herrmann, C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
RP Davis, VA (reprint author), Sci Applicat Int Corp, San Diego, CA 92121 USA.
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
FU Johns Hopkins University Applied Physics Laboratory; ADNET Systems, Inc.
FX This research was carried out under contracts with the Johns Hopkins
University Applied Physics Laboratory and ADNET Systems, Inc.
NR 17
TC 5
Z9 6
U1 0
U2 7
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0093-3813
J9 IEEE T PLASMA SCI
JI IEEE Trans. Plasma Sci.
PD FEB
PY 2012
VL 40
IS 2
SI SI
BP 262
EP 273
DI 10.1109/TPS.2011.2178615
PN 1
PG 12
WC Physics, Fluids & Plasmas
SC Physics
GA 894LS
UT WOS:000300428800016
ER
PT J
AU Charro, M
Sanmartin, JR
Bombardelli, C
Sanchez-Torres, A
Lorenzini, EC
Garrett, HB
Evans, RW
AF Charro, Mario
Sanmartin, Juan R.
Bombardelli, Claudio
Sanchez-Torres, Antonio
Lorenzini, Enrico C.
Garrett, Henry B.
Evans, Robin W.
TI A Proposed Two-Stage Two-Tether Scientific Mission at Jupiter
SO IEEE TRANSACTIONS ON PLASMA SCIENCE
LA English
DT Article
DE Bare tether; plasma applications; power generation
ID ELECTRODYNAMIC TETHER; ENVIRONMENT; CONSTRAINTS
AB A two-stage mission to place a spacecraft (SC) below the Jovian radiation belts, using a spinning bare tether with plasma contactors at both ends to provide propulsion and power, is proposed. Capture by Lorentz drag on the tether, at the periapsis of a barely hyperbolic equatorial orbit, is followed by a sequence of orbits at near-constant periapsis, drag finally bringing the SC down to a circular orbit below the halo ring. Although increasing both tether heating and bowing, retrograde motion can substantially reduce accumulated dose as compared with prograde motion, at equal tether-to-SC mass ratio. In the second stage, the tether is cut to a segment one order of magnitude smaller, with a single plasma contactor, making the SC to slowly spiral inward over several months while generating large onboard power, which would allow multiple scientific applications, including in situ study of Jovian grains, auroral sounding of upper atmosphere, and space-and time-resolved observations of surface and subsurface.
C1 [Charro, Mario; Sanmartin, Juan R.; Bombardelli, Claudio; Sanchez-Torres, Antonio] Univ Politecn Madrid, E-28040 Madrid, Spain.
[Lorenzini, Enrico C.] Univ Padua, I-35122 Padua, Italy.
[Garrett, Henry B.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Evans, Robin W.] Mori Associates, Rockville, MD 20852 USA.
RP Charro, M (reprint author), Univ Politecn Madrid, E-28040 Madrid, Spain.
EM mario.charro@upm.es; juanr.sanmartin@upm.es; claudio.bombardelli@upm.es;
antonio.sanchezt@upm.es; enrico.lorenzini@unipd.it;
henry.b.garrett@jpl.nasa.gov; robin.w.evans@jpl.nasa.gov
RI Sanchez-Torres, Antonio/P-6978-2015
OI Sanchez-Torres, Antonio/0000-0001-5110-5724
FU Spanish Ministerio de Ciencia y Tecnologia [AYA2008-04769]; National
Aeronautics and Space Administration
FX Manuscript received March 15, 2011; revised August 2, 2011; accepted
September 26, 2011. Date of publication November 9, 2011; date of
current version February 10, 2012. This work was supported by the
Spanish Ministerio de Ciencia y Tecnologia under Grant AYA2008-04769.;
The research described in this paper by H. B. Garrett was carried out at
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with the National Aeronautics and Space Administration.
NR 16
TC 6
Z9 6
U1 1
U2 10
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0093-3813
J9 IEEE T PLASMA SCI
JI IEEE Trans. Plasma Sci.
PD FEB
PY 2012
VL 40
IS 2
SI SI
BP 274
EP 281
DI 10.1109/TPS.2011.2172637
PN 1
PG 8
WC Physics, Fluids & Plasmas
SC Physics
GA 894LS
UT WOS:000300428800017
ER
PT J
AU Hoang, B
Wong, FK
Corey, RL
Gardiner, G
Funderburk, VV
Gahart, RL
Wright, KH
Schneider, TA
Vaughn, JA
AF Hoang, Bao
Wong, Frankie K.
Corey, Ronald L.
Gardiner, George
Funderburk, Victor V.
Gahart, Richard L.
Wright, Kenneth H., Jr.
Schneider, Todd A.
Vaughn, Jason A.
TI Combined Space Environmental Exposure Test of Multijunction GaAs/Ge
Solar Array Coupons
SO IEEE TRANSACTIONS ON PLASMA SCIENCE
LA English
DT Article
DE Combined environmental space exposure; electrostatic discharge (ESD);
multijunction GaAs/Ge solar array; spacecraft charging
AB The purpose of this test program is to understand the changes and degradation of the space solar array panel components, including its electrostatic discharge (ESD) mitigation design features in their integrated form, after multiple years (up to 15) of simulated Earth geosynchronous (GEO) space environment. A set of multijunction GaAs/Ge solar array test coupons was subjected to five-year increments of combined environmental exposure tests. These tests consisted of the following: simulated ultraviolet (UV) radiation, ESD, electron/proton particle radiation, thermal cycling, and simulated ion thruster exposures. The solar radiation simulation was produced using a mercury-xenon lamp with wavelengths in the UV spectrum ranging from 230 to 400 nm. The ESD test was performed in the inverted-gradient mode using a low-energy electron (3-6 keV) beam exposure. The ESD test also included a simulated panel coverglass flashover for the primary arc event. The electron/proton radiation exposure included 1.0-MeV electrons, 100-keV electrons, and 40-keV protons. Thermal cycling included simulated transient Earth eclipse for satellites in geosynchronous orbit. With the increasing use of ion thruster engines on many satellites, the combined environmental exposure test also included ion thruster exposure to determine the impact on solar array performance, as well as the ion thruster interaction to ESD events. Before and after each increment of combined environmental exposures, the coupons underwent visual inspection using high power magnification and electrical tests that included characterization by large-area pulse solar simulator, dark I-V, insulation resistance, and electroluminescence. This paper discusses the test objective, test methodologies, and preliminary results after five and ten years of simulated combined environmental exposure tests.
C1 [Hoang, Bao] Space Syst Loral, Solar Array Deployable Grp, Palo Alto, CA USA.
[Wright, Kenneth H., Jr.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA.
[Schneider, Todd A.; Vaughn, Jason A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Gardiner, George] Space Syst Loral, Radiat Effects & ESD Anal & Tests, Motorola GED, Palo Alto, CA USA.
[Gardiner, George] Space Syst Loral, Space Environm Dept, Palo Alto, CA USA.
RP Hoang, B (reprint author), Space Syst Loral, Solar Array Deployable Grp, Palo Alto, CA USA.
EM hoang.bao@ssd.loral.com; wong.frankie@ssd.loral.com;
corey.ron@ssd.loral.com; gardiner.george@ssd.loral.com;
funderburk.vic@ssd.loral.com; gahart.richard@ssd.loral.com;
ken.wright@uah.edu; todd.schneider@nasa.gov; jason.a.vaughn@nasa.gov
NR 8
TC 5
Z9 5
U1 0
U2 9
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0093-3813
J9 IEEE T PLASMA SCI
JI IEEE Trans. Plasma Sci.
PD FEB
PY 2012
VL 40
IS 2
SI SI
BP 324
EP 333
DI 10.1109/TPS.2011.2174161
PN 1
PG 10
WC Physics, Fluids & Plasmas
SC Physics
GA 894LS
UT WOS:000300428800024
ER
PT J
AU Wright, KH
Schneider, TA
Vaughn, JA
Hoang, B
Funderburk, VV
Wong, FK
Gardiner, G
AF Wright, Kenneth H., Jr.
Schneider, Todd A.
Vaughn, Jason A.
Hoang, Bao
Funderburk, Victor V.
Wong, Frankie K.
Gardiner, George
TI Electrostatic Discharge Testing of Multijunction Solar Array Coupons
After Combined Space Environmental Exposures
SO IEEE TRANSACTIONS ON PLASMA SCIENCE
LA English
DT Article
DE Electrostatic discharges (ESDs); environmental testing; photovoltaic
cell testing
AB A set of multijunction GaAs/Ge solar array test coupons provided by Space Systems/Loral was subjected to a sequence of five-year increments of combined space environmental exposure tests. The test coupons capture an integrated design intended for use in a geosynchronous (GEO) space environment. A key component of this test campaign is performing electrostatic discharge (ESD) tests in the inverted gradient mode. The protocol of the ESD tests is based on the ISO standard for ESD testing on solar array panels [ISO-11221]. The test schematic in the ISO reference has been modified with Space System/Loral designed circuitry to better simulate the on-orbit operational conditions of its solar array design. Part of the modified circuitry is to simulate a solar array panel coverglass flashover discharge. All solar array coupons used in the test campaign consist of four cells constructed to form two strings. The ESD tests are performed at the beginning-of-life (BOL) and at each five-year environmental exposure point. The space environmental exposure sequence consists of ultraviolet radiation, electron/proton particle radiation, thermal cycling, and xenon ion thruster plume erosion. This paper discusses the coverglass flashover simulation, the ESD test setup, and the importance of the electrical test design in simulating the on-orbit operational conditions. Results from fifth-year testing are compared to the baseline ESD characteristics determined at the BOL condition.
C1 [Wright, Kenneth H., Jr.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA.
[Schneider, Todd A.; Vaughn, Jason A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Hoang, Bao; Gardiner, George] Space Syst Loral, Solar Array Deployable Grp, Palo Alto, CA USA.
[Wong, Frankie K.; Gardiner, George] Space Syst Loral, Space Environm Dept, Palo Alto, CA USA.
[Gardiner, George] Space Syst Loral, Motorola GED, Radiat Effects & ESD Anal & Tests, Palo Alto, CA USA.
RP Wright, KH (reprint author), Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA.
EM Ken.Wright@uah.edu; todd.a.schneider@nasa.gov; jason.a.vaughn@nasa.gov;
Hoang.Bao@ssd.loral.com; funderbv@ssd.loral.com;
Wong.Frankie@ssd.loral.com; Gardiner.George@ssd.loral.com
FU NASA/Marshall Space Flight Center [SAA8-084200]; Space Systems/Loral;
NASA; University of Alabama-Huntsville [NNM11AA01A]
FX Manuscript received April 6, 2011; revised September 30, 2011; accepted
October 23, 2011. Date of publication December 13, 2011; date of current
version February 10, 2012. The work at the NASA/Marshall Space Flight
Center is performed under Space Act Agreement (SAA8-084200) with Space
Systems/Loral. The work of K. H. Wright was supported by NASA through a
Cooperative Agreement with the University of Alabama-Huntsville
(NNM11AA01A).
NR 17
TC 11
Z9 12
U1 1
U2 5
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0093-3813
EI 1939-9375
J9 IEEE T PLASMA SCI
JI IEEE Trans. Plasma Sci.
PD FEB
PY 2012
VL 40
IS 2
SI SI
BP 334
EP 344
DI 10.1109/TPS.2011.2174447
PN 1
PG 11
WC Physics, Fluids & Plasmas
SC Physics
GA 894LS
UT WOS:000300428800025
ER
PT J
AU Vayner, B
Galofaro, JT
AF Vayner, Boris
Galofaro, Joel T.
TI Inception and Prevention of Sustained Discharges on Solar Arrays
SO IEEE TRANSACTIONS ON PLASMA SCIENCE
LA English
DT Article
DE Arc discharges; photovoltaic space power systems; plasma properties;
solar power generation; vacuum arcs
ID PLASMA; ARCS; ENVIRONMENT; TESTS; ORBIT
AB Sustained arc between adjacent cells is certainly a catastrophic event that results in significant loss in the power delivered to spacecraft systems. In order to prevent this kind of discharges, the threshold magnitudes of voltage and current should be determined in ground tests and compared with respective operational parameters. It is necessary to demonstrate that the results of ground tests depend on solar array designs but do not depend on the simulated environment and the electrical circuitry arrangement. A thorough analysis of about 20 tests performed in different laboratories has been conducted in this work. Sustained arc current thresholds were established for a variety of solar array designs and confronted with well-known magnitudes for vacuum arcs. If both voltage and string current magnitudes exceed the threshold values, the gaps between adjacent strings can be filled in with insulating material (RTV). Comprehensive ground tests demonstrated a high efficiency of this method. However, the lifetime of modern spacecraft spans for 10-15 years, and aging of RTV due to space radiation and temperature variations may cause critical changes in insulator properties. Thus, it seems reasonable to prepare a sample with RTV-grouted gaps, to undergo it proton fluence and thermal cycling equivalent to a few years in the geosynchronous orbit, and to test the sample against sustained arc inception. This program was also realized in the test described in this paper.
C1 [Vayner, Boris] Ohio Aerosp Inst, Cleveland, OH 44142 USA.
[Galofaro, Joel T.] NASA, John H Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Vayner, B (reprint author), Ohio Aerosp Inst, Cleveland, OH 44142 USA.
EM Boris.V.Vayner@nasa.gov
FU New Energy Development Organization (Japan)
FX The authors would like to thank D. Scheiman for performing the
photovoltaic tests. The authors would also like to thank New Energy
Development Organization Grant (Japan) for providing the samples.
NR 31
TC 4
Z9 4
U1 0
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0093-3813
J9 IEEE T PLASMA SCI
JI IEEE Trans. Plasma Sci.
PD FEB
PY 2012
VL 40
IS 2
SI SI
BP 388
EP 393
DI 10.1109/TPS.2011.2177480
PN 1
PG 6
WC Physics, Fluids & Plasmas
SC Physics
GA 894LS
UT WOS:000300428800031
ER
PT J
AU Comiso, JC
AF Comiso, Josefino C.
TI Large Decadal Decline of the Arctic Multiyear Ice Cover
SO JOURNAL OF CLIMATE
LA English
DT Article
ID SEA-ICE; TEMPERATURE; OSCILLATION; OCEAN; AMPLIFICATION; VARIABILITY;
TRENDS; WIND
AB The perennial ice area was drastically reduced to 38% of its climatological average in 2007 but recovered slightly in 2008, 2009, and 2010 with the areas being 10%, 24%, and 11% higher than in 2007, respectively. However, trends in extent and area remained strongly negative at -12.2% and -13.5% decade(-1), respectively. The thick component of the perennial ice, called multiyear ice, as detected by satellite data during the winters of 1979-2011 was studied, and results reveal that the multiyear ice extent and area are declining at an even more rapid rate of -15.1% and -17.2% decade(-1), respectively, with a record low value in 2008 followed by higher values in 2009, 2010, and 2011. Such a high rate in the decline of the thick component of the Arctic ice cover means a reduction in the average ice thickness and an even more vulnerable perennial ice cover. The decline of the multiyear ice area from 2007 to 2008 was not as strong as that of the perennial ice area from 2006 to 2007, suggesting a strong role of second-year ice melt in the latter. The sea ice cover is shown to be strongly correlated with surface temperature, which is increasing at about 3 times the global average in the Arctic but appears weakly correlated with the Arctic Oscillation (AO), which controls the atmospheric circulation in the region. An 8-9-yr cycle is apparent in the multiyear ice record, which could explain, in part, the slight recovery in the last 3 yr.
C1 NASA, Cryospher Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Comiso, JC (reprint author), NASA, Cryospher Sci Branch, Goddard Space Flight Ctr, Code 614-1, Greenbelt, MD 20771 USA.
EM josefino.c.comiso@nasa.gov
FU NASA
FX The author is thankful to R. Gersten of RSI/SESDA-2 and L. Stock of SGT,
Inc. for excellent programming and analysis support. This paper also
benefitted substantially from the valuable comments and suggestions of
two anonymous reviewers. This work was funded by NASA's Cryospheric
Sciences Program.
NR 50
TC 199
Z9 208
U1 15
U2 111
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD FEB
PY 2012
VL 25
IS 4
BP 1176
EP 1193
DI 10.1175/JCLI-D-11-00113.1
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 894HU
UT WOS:000300418500007
ER
PT J
AU Dynys, FW
Berger, MH
Sehirlioglu, A
AF Dynys, Frederick W.
Berger, Marie-Helene
Sehirlioglu, Alp
TI Thermoelectric Properties of Undoped and Doped (Ti0.75Sn0.25)O-2
SO JOURNAL OF THE AMERICAN CERAMIC SOCIETY
LA English
DT Article
ID TIO2-SNO2 SYSTEM; SOLID-SOLUTIONS; ELECTRICAL-PROPERTIES; SEEBECK
COEFFICIENT; ALIOVALENT DOPANTS; DECOMPOSITION; TRANSPORT; POWER;
PRECIPITATION; CERAMICS
AB Thermoelectric properties of undoped and doped (Ti0.75Sn0.25)O-2 were investigated for high-temperature thermoelectric conversion application. Nano-composites were formed by annealing above 1000 degrees C. Outside the spinodal dome, ilmenite-type SnTiO3 precipitated from the rutile structure. Thermoelectric properties were measured in the temperature range from room temperature to 1000 degrees C. (Ti0.75Sn0.25)O-2 was doped with both acceptor and donor dopants. Both undoped and doped (Ti0.75Sn0.25)O-2 exhibit n-type electrical behavior independent of the type of the dopant. The electrical conductivity was enhanced three orders of magnitude by donor doping with Nb2O5 or Ta2O5; achieving a maximum of 546 S/m at 850 degrees C. The increase in electrical conductivity was accompanied by reduction of the absolute Seebeck coefficient. Seebeck coefficient reduction of -600 mu V/K was observed between undoped and 4% Ta2O5 doped samples. The solid solution and doping reduced the thermal conductivity to <4 W/mK, far below the parent materials TiO2 and SnO2. Lattice thermal conductivity decreased with increasing temperature, achieving 1.9 W/mK at 900 degrees C for 4% Ta2O5 doping. No further reduction in thermal conductivity was observed in annealed samples containing nano-sized SnTiO3 precipitates. Dimensionless figure of merit (ZT) attained was <0.1.
C1 [Dynys, Frederick W.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
[Berger, Marie-Helene] MINES ParisTech, Ctr Mat, CNRS, UMR 7633, F-91003 Evry, France.
[Sehirlioglu, Alp] Case Western Reserve Univ, Dept Mat Sci & Engn, Cleveland, OH 44106 USA.
RP Dynys, FW (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM frederick.w.dynys@nasa.gov
RI Berger, Marie-Helene/B-9785-2013
NR 26
TC 8
Z9 8
U1 2
U2 65
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0002-7820
J9 J AM CERAM SOC
JI J. Am. Ceram. Soc.
PD FEB
PY 2012
VL 95
IS 2
BP 619
EP 626
DI 10.1111/j.1551-2916.2011.04794.x
PG 8
WC Materials Science, Ceramics
SC Materials Science
GA 884UA
UT WOS:000299733100031
ER
PT J
AU Sato, Y
Suzuki, K
Iguchi, T
Choi, IJ
Kadowaki, H
Nakajima, T
AF Sato, Yousuke
Suzuki, Kentaroh
Iguchi, Takamichi
Choi, In-Jin
Kadowaki, Hiroyuki
Nakajima, Teruyuki
TI Characteristics of Correlation Statistics between Droplet Radius and
Optical Thickness of Warm Clouds Simulated by a Three-Dimensional
Regional-Scale Spectral Bin Microphysics Cloud Model
SO JOURNAL OF THE ATMOSPHERIC SCIENCES
LA English
DT Article
ID BOUNDARY-LAYER CLOUDS; MESOSCALE CELLULAR STRUCTURES; SOLAR-RADIATION
MEASUREMENTS; SHALLOW CUMULUS CONVECTION; GENERAL-CIRCULATION MODEL;
EFFECTIVE PARTICLE RADIUS; LARGE-EDDY SIMULATIONS; MARINE STRATOCUMULUS;
FRACTIONAL CLOUDINESS; CONDENSATION NUCLEI
AB Three-dimensional downscaling simulations using a spectral bin microphysics (SBM) model were conducted to investigate the effects of aerosol amount and dynamical stabilities of the atmosphere on the correlation statistics between cloud droplet effective radius (RE) and cloud optical thickness (COT) of warm clouds off the coast of California. The regeneration process of aerosols was implemented into the SBM and was found to be necessary for simulating the satellite-observed microphysical properties of warm clouds by the SBM model used in this study.
The results showed that the aerosol amount changed the correlation statistics in a way that changes the cloud particle number concentration, whereas the inversion height of the boundary layer, which is related to the atmospheric stability and the cloud-top height, changed the correlation statistics in a way that changes the liquid water path. These results showed that the dominant mechanisms that control the correlation statistics are similar to those suggested by previous modeling studies based on two-dimensional idealized simulations. On the other hand, the present three-dimensional modeling was also able to simulate some realistic patterns of the correlation statistics, namely, mixtures of characteristic patterns and the "high-heeled" pattern as observed by satellite remote sensing.
C1 [Sato, Yousuke; Nakajima, Teruyuki] Univ Tokyo, Atmosphere & Ocean Res Inst, Kashiwa, Chiba 2778568, Japan.
[Sato, Yousuke] Japan Soc Promot Sci, Chiyoda Ku, Tokyo, Japan.
[Suzuki, Kentaroh] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Iguchi, Takamichi] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Iguchi, Takamichi] NASA, Goddard Space Flight Ctr, Lab Atmosphere, Greenbelt, MD 20771 USA.
[Choi, In-Jin] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul, South Korea.
RP Sato, Y (reprint author), Univ Tokyo, Atmosphere & Ocean Res Inst, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778568, Japan.
EM satoy@aori.u-tokyo.ac.jp
RI Suzuki, Kentaroh/C-3624-2011; Nakajima, Teruyuki/H-2370-2013; Sato,
Yousuke/C-5416-2016
OI Nakajima, Teruyuki/0000-0002-9042-504X; Sato,
Yousuke/0000-0002-6857-3783
FU Initiative on Promotion of Supercomputing for Young Researchers,
Supercomputing Division, Information Technology Center, The University
of Tokyo; JAXA/GCOM-C; JAXA/EarthCARE; MEXT/VL for Climate System
Diagnostics; MOE [A-1101]; NIES/GOSAT; MEXT/RECCA/SALSA; Korea
Meteorological Administration [RACS 2010-1009]; [22-7893]
FX This study is supported by Initiative on Promotion of Supercomputing for
Young Researchers, Supercomputing Division, Information Technology
Center, The University of Tokyo. A part of authors are supported by
projects of JAXA/GCOM-C, JAXA/EarthCARE, MEXT/VL for Climate System
Diagnostics, MOE/Global Environment Research Fund A-1101, NIES/GOSAT,
and MEXT/RECCA/SALSA. Some authors are supported by Grant-in-Aid for
JSPS Fellows 22-7893. One of the authors is supported by the Korea
Meteorological Administration Research and Development Program under
Grant RACS 2010-1009. We are very grateful to Jorgen. B. Jensen of the
National Center for Atmospheric Research/Earth Observation Factory for
his valuable comment on an earlier version of this paper.
NR 63
TC 3
Z9 3
U1 1
U2 15
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0022-4928
J9 J ATMOS SCI
JI J. Atmos. Sci.
PD FEB
PY 2012
VL 69
IS 2
BP 484
EP 503
DI 10.1175/JAS-D-11-076.1
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 885SI
UT WOS:000299800700005
ER
PT J
AU Loeb, NG
Lyman, JM
Johnson, GC
Allan, RP
Doelling, DR
Wong, T
Soden, BJ
Stephens, GL
AF Loeb, Norman G.
Lyman, John M.
Johnson, Gregory C.
Allan, Richard P.
Doelling, David R.
Wong, Takmeng
Soden, Brian J.
Stephens, Graeme L.
TI Observed changes in top-of-the-atmosphere radiation and upper-ocean
heating consistent within uncertainty
SO NATURE GEOSCIENCE
LA English
DT Article
ID EARTHS ENERGY IMBALANCE; GLOBAL UPPER-OCEAN; SYSTEM; BUDGET; ERA
AB Global climate change results from a small yet persistent imbalance between the amount of sunlight absorbed by Earth and the thermal radiation emitted back to space(1). An apparent inconsistency has been diagnosed between interannual variations in the net radiation imbalance inferred from satellite measurements and upper-ocean heating rate from in situ measurements, and this inconsistency has been interpreted as 'missing energy' in the system(2). Here we present a revised analysis of net radiation at the top of the atmosphere from satellite data, and we estimate ocean heat content, based on three independent sources. We find that the difference between the heat balance at the top of the atmosphere and upper-ocean heat content change is not statistically significant when accounting for observational uncertainties in ocean measurements(3), given transitions in instrumentation and sampling. Furthermore, variability in Earth's energy imbalance relating to El Nino-Southern Oscillation is found to be consistent within observational uncertainties among the satellite measurements, a reanalysis model simulation and one of the ocean heat content records. We combine satellite data with ocean measurements to depths of 1,800 m, and show that between January 2001 and December 2010, Earth has been steadily accumulating energy at a rate of 0.50 +/- 0.43 Wm(-2) (uncertainties at the 90% confidence level). We conclude that energy storage is continuing to increase in the sub-surface ocean.
C1 [Loeb, Norman G.; Doelling, David R.; Wong, Takmeng] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Lyman, John M.] Univ Hawaii Manoa, Joint Inst Marine & Atmospher Res, Honolulu, HI 96822 USA.
[Lyman, John M.; Johnson, Gregory C.] NOAA, Pacific Marine Environm Lab, Seattle, WA 98115 USA.
[Allan, Richard P.] Univ Reading, Dept Meteorol, Reading RG6 6BB, Berks, England.
[Soden, Brian J.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Div Meteorol & Phys Oceanog, Miami, FL 33149 USA.
[Stephens, Graeme L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Loeb, NG (reprint author), NASA, Langley Res Ctr, 21 Langley Blvd, Hampton, VA 23681 USA.
EM norman.g.loeb@nasa.gov
RI Allan, Richard/B-5782-2008; Johnson, Gregory/I-6559-2012
OI Allan, Richard/0000-0003-0264-9447; Johnson, Gregory/0000-0002-8023-4020
FU NASA Science Mission Directorate; US National Oceanic and Atmospheric
Administration (NOAA) Climate Program Office; NOAA Research
FX We thank the CERES science, algorithm, and data management teams and the
NASA Science Mission Directorate for supporting this research. J.M.L.
and G.C.J. were funded by the US National Oceanic and Atmospheric
Administration (NOAA) Climate Program Office and NOAA Research. We thank
S. Good at the UK Met Office for providing OHCA data from the Hadley
Centre.
NR 30
TC 123
Z9 128
U1 5
U2 63
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 FEB
PY 2012
VL 5
IS 2
BP 110
EP 113
DI 10.1038/NGEO1375
PG 4
WC Geosciences, Multidisciplinary
SC Geology
GA 893ZU
UT WOS:000300397300013
ER
PT J
AU Koren, I
Altaratz, O
Remer, LA
Feingold, G
Martins, JV
Heiblum, RH
AF Koren, Ilan
Altaratz, Orit
Remer, Lorraine A.
Feingold, Graham
Martins, J. Vanderlei
Heiblum, Reuven H.
TI Aerosol-induced intensification of rain from the tropics to the
mid-latitudes
SO NATURE GEOSCIENCE
LA English
DT Article
ID PRECIPITATION; CLOUDS; INVIGORATION; POLLUTION; AMAZON; URBAN
AB Atmospheric aerosols affect cloud properties, and thereby the radiation balance of the planet and the water cycle. However, the influence of aerosols on clouds, and in particular on precipitation, is far from understood(1), and seems to depend on factors such as location, season(2) and the spatiotemporal scale of the analysis. Here, we examine the relationship between aerosol abundance and rain rate-a key factor in climate and hydrological processes-using rain data from a satellite-based instrument sensitive to stronger rain rates (Tropical Rainfall Measuring Mission(3), TRMM), aerosol and cloud property data from the Moderate Resolution Imaging Spectroradiometer onboard the Aqua satellite(4,5) and meteorological information from the Global Data Assimilation System(6). We show that for a range of conditions, increases in aerosol abundance are associated with the local intensification of rain rates detected by the TRMM. The relationship is apparent over both the ocean and land, and in the tropics, subtropics and mid-latitudes. Further work is needed to determine how aerosols influence weaker rain rates, not picked up in the analysis. We also find that increases in aerosol levels are associated with a rise in cloud-top height. We suggest that the invigoration of clouds and the intensification of rain rates is a preferred response to an increase in aerosol concentration.
C1 [Koren, Ilan; Altaratz, Orit; Heiblum, Reuven H.] Weizmann Inst Sci, Dept Environm Sci, IL-76100 Rehovot, Israel.
[Remer, Lorraine A.] NASA, Atmospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Feingold, Graham] NOAA, Earth Syst Res Lab, Div Chem Sci, Boulder, CO 80305 USA.
[Martins, J. Vanderlei] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Martins, J. Vanderlei] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, NASA, JCET,GSFC, Baltimore, MD 21250 USA.
RP Koren, I (reprint author), Weizmann Inst Sci, Dept Environm Sci, IL-76100 Rehovot, Israel.
EM ilan.koren@weizmann.ac.il
RI Feingold, Graham/B-6152-2009; Koren, Ilan/K-1417-2012; Manager, CSD
Publications/B-2789-2015
OI Koren, Ilan/0000-0001-6759-6265;
FU Israel Science Foundation [1172/10]; Minerva Foundation [780048]; NOAA
FX This work was supported in part by the Israel Science Foundation (grant
# 1172/10) and the Minerva Foundation (780048). G.F. acknowledges
support from NOAA's Climate Goal Program.
NR 30
TC 70
Z9 71
U1 3
U2 50
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 FEB
PY 2012
VL 5
IS 2
BP 118
EP 122
DI 10.1038/NGEO1364
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 893ZU
UT WOS:000300397300015
ER
PT J
AU Winter, JM
Eltahir, EAB
AF Winter, Jonathan M.
Eltahir, Elfatih A. B.
TI Modeling the hydroclimatology of the midwestern United States. Part 1:
current climate
SO CLIMATE DYNAMICS
LA English
DT Article
DE Hydrology; Regional climate modeling; Midwestern United States
ID CONVECTIVE PARAMETERIZATION; FUTURE CLIMATE; REGCM3; WATER;
PRECIPITATION; SENSITIVITY; SIMULATION; REPRESENTATION; VARIABILITY;
PREDICTION
AB An ensemble of six 22-year numerical experiments was conducted to evaluate the ability of Regional Climate Model version 3 (RegCM3) to simulate the energy and water budgets of the midwestern United States. RegCM3 was run using two surface physics schemes: Integrated Biosphere Simulator (IBIS) and Biosphere-Atmosphere Transfer Scheme 1e (BATS1e), and two convective closure assumptions: Fritsch & Chappell (FC80) and Arakawa & Schubert (AS74). Boundary conditions were provided by the National Centers for Environmental Prediction-Department of Energy Reanalysis 2 dataset and the ECHAM5 general circulation model. A companion paper examines the American Midwest under future climate scenarios. Overall, the model that reproduces the observed seasonal cycles of the midwestern United States climate system best is RegCM3 using IBIS and the AS74 convective closure assumption. IBIS simulates shortwave radiation more accurately, while BATS1e simulates longwave radiation more accurately. Summer two-meter air temperature is overestimated by the combination of IBIS and the FC80 convective closure assumption. All models contain a wet bias and overestimate evapotranspiration during the spring. Total runoff, surface runoff, groundwater runoff, and root zone soil moisture are best simulated by RegCM3 using IBIS and the AS74 convective closure assumption. While BATS1e does capture the seasonal cycle of total runoff, gross errors in the partitioning of total runoff between surface runoff and groundwater runoff exist. The seasonal cycle of root zone soil moisture simulated by RegCM3 using IBIS and the AS74 convective closure assumption is dry, but agrees with observations during the summer. The rest of the models underestimate root zone soil moisture.
C1 [Winter, Jonathan M.; Eltahir, Elfatih A. B.] MIT, Cambridge, MA 02139 USA.
RP Winter, JM (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
EM jwinter@mit.edu
FU National Science Foundation [EAR-04500341]; Martin Family Fellowship
FX We thank the International Centre for Theoretical Physics, the Eltahir
group, members of the Ralph M. Parsons Laboratory who aided in this
research, our reviewers, and our editor. Individuals who made
significant contributions to this work include Jeremy Pal and Marc
Marcella. This work was funded by the National Science Foundation (Award
EAR-04500341) and the Martin Family Fellowship.
NR 37
TC 6
Z9 6
U1 0
U2 9
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
EI 1432-0894
J9 CLIM DYNAM
JI Clim. Dyn.
PD FEB
PY 2012
VL 38
IS 3-4
BP 573
EP 593
DI 10.1007/s00382-011-1182-2
PG 21
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 887BE
UT WOS:000299899300009
ER
PT J
AU Winter, JM
Eltahir, EAB
AF Winter, Jonathan M.
Eltahir, Elfatih A. B.
TI Modeling the hydroclimatology of the midwestern United States. Part 2:
future climate
SO CLIMATE DYNAMICS
LA English
DT Article
DE Hydrology; Regional climate modeling; Climate change; Soil moisture;
Midwestern United States
ID SUMMER DRYNESS
AB An ensemble of six 22-year numerical experiments was conducted to quantify the response of soil moisture to multiple climate change scenarios over the American Midwest. Regional Climate Model version 3 (RegCM3) was run using two surface physics schemes: Integrated Biosphere Simulator (IBIS) and Biosphere-Atmosphere Transfer Scheme 1e (BATS1e); and two convective closure assumptions: Fritsch and Chappell and Arakawa and Schubert. Experiments were forced with a surrogate climate change scenario constructed using the National Centers for Environmental Prediction-Department of Energy Reanalysis 2 dataset and the ECHAM5 A1B climate change scenario. RegCM3-IBIS and RegCM3-BATS1e simulate increased two-meter air temperature and downward longwave radiation throughout the year under both climate change scenarios. While differences in shortwave radiation are relatively small; some model configurations and climate change scenarios produce additional precipitation, evapotranspiration, and total runoff during the spring and summer. Soil moisture is unchanged or increased throughout the growing season as enhanced rainfall offsets greater evaporative demand. Negligible drying in root zone soil moisture is found in all climate change experiments conducted, regardless of surface physics scheme, boundary conditions, or convective closure assumption.
C1 [Winter, Jonathan M.; Eltahir, Elfatih A. B.] MIT, Cambridge, MA 02139 USA.
RP Winter, JM (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
EM jwinter@mit.edu
FU National Science Foundation [EAR-04500341]; Martin Family Fellowship
FX We thank the International Centre for Theoretical Physics, the Eltahir
group, members of the Ralph M. Parsons Laboratory who aided in this
research, our reviewers, and our editor. Individuals who made
significant contributions to this work include Jeremy Pal and Marc
Marcella. This work was funded by the National Science Foundation (Award
EAR-04500341) and the Martin Family Fellowship.
NR 25
TC 4
Z9 4
U1 1
U2 10
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
EI 1432-0894
J9 CLIM DYNAM
JI Clim. Dyn.
PD FEB
PY 2012
VL 38
IS 3-4
BP 595
EP 611
DI 10.1007/s00382-011-1183-1
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 887BE
UT WOS:000299899300010
ER
PT J
AU Garcia, DB
Forman, R
Shindo, D
AF Garcia, D. B.
Forman, R.
Shindo, D.
TI Experimental evaluation of fatigue crack initiation from corroded
hemispherical notches in aerospace structural materials
SO FATIGUE & FRACTURE OF ENGINEERING MATERIALS & STRUCTURES
LA English
DT Article
DE aluminium 7075-T7351; D6AC steel; fatigue; corrosion pit; initiation;
residual stress
ID ALUMINUM-ALLOY; PITTING CORROSION; RESIDUAL-STRESS; LIFE; PROPAGATION;
GROWTH; STEEL; LIVES
AB A test program was developed and executed to evaluate the influence of corroded hemispherical notches on the fatigue crack initiation process in aluminium 7075-T7351, 4340 steel and D6AC steel. Surface enhancements such as shot peening and laser shock peening were also incorporated as part of the test effort with the intent of assessing any improvements in fatigue performance. The aluminium specimens exhibited a relative insensitivity to the surface enhancements for crack initiation in pits ranging from 0.3 to 2.0 mm, and localized yielding was only a factor for smaller pits operated at an elevated load ratio. Residual stresses created by the surface enhancements as well as localized yielding improved the crack initiation behavior from the base of the pits for both the 4340 and D6AC steel specimens. This behaviour was evident at high and low load ratios. In particular, laser shock peening induced residual stresses produced a significant increase in the crack initiation stress even when localized yielding was not a factor.
C1 [Garcia, D. B.] SAIC, Houston, TX 77058 USA.
[Forman, R.; Shindo, D.] NASA, JSC, Houston, TX 77058 USA.
RP Garcia, DB (reprint author), SAIC, 2450 NASA Pkwy, Houston, TX 77058 USA.
EM garciadb1004@hotmail.com
FU Department of Transportation/Federal Aviation Administration
[DTFACT-08-X-00004]; National Aeronautics and Space Administration
[DTFACT-08-X-00004]
FX The authors thank the support of Traci Stadtmueller, John Bakuckas,
Ph.D. and Cu Nguyen from the FAA William J. Hughes Technical Center.
This work was sponsored under the Interagency Agreement,
DTFACT-08-X-00004, between the Department of Transportation/Federal
Aviation Administration and the National Aeronautics and Space
Administration.
NR 27
TC 1
Z9 2
U1 1
U2 29
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 8756-758X
J9 FATIGUE FRACT ENG M
JI Fatigue Fract. Eng. Mater. Struct.
PD FEB
PY 2012
VL 35
IS 2
BP 122
EP 140
DI 10.1111/j.1460-2695.2011.01599.x
PG 19
WC Engineering, Mechanical; Materials Science, Multidisciplinary
SC Engineering; Materials Science
GA 889CH
UT WOS:000300050600004
ER
PT J
AU Pounder, NL
Hogan, RJ
Varnai, T
Battaglia, A
Cahalan, RF
AF Pounder, Nicola L.
Hogan, Robin J.
Varnai, Tamas
Battaglia, Alessandro
Cahalan, Robert F.
TI A Variational Method to Retrieve the Extinction Profile in Liquid Clouds
Using Multiple-Field-of-View Lidar
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID GREEN-FUNCTION; PART II; SCATTERING; RADAR; THICKNESS; RETURNS; STORAGE;
SCHEME; WATER
AB Liquid clouds play a profound role in the global radiation budget, but it is difficult to retrieve their vertical profile remotely. Ordinary narrow-field-of-view (FOV) lidars receive a strong return from such clouds, but the information is limited to the first few optical depths. Wide-angle multiple-FOV lidars can isolate radiation that is scattered multiple times before returning to the instrument, often penetrating much deeper into the cloud than does the single-scattered signal. These returns potentially contain information on the vertical profile of the extinction coefficient but are challenging to interpret because of the lack of a fast radiative transfer model for simulating them. This paper describes a variational algorithm that incorporates a fast forward model that is based on the time-dependent two-stream approximation, and its adjoint. Application of the algorithm to simulated data from a hypothetical airborne three-FOV lidar with a maximum footprint width of 600 m suggests that this approach should be able to retrieve the extinction structure down to an optical depth of around 6 and a total optical depth up to at least 35, depending on the maximum lidar FOV. The convergence behavior of Gauss-Newton and quasi-Newton optimization schemes are compared. Results are then presented from an application of the algorithm to observations of stratocumulus by the eight-FOV airborne Cloud Thickness from Off-Beam Lidar Returns (THOR) lidar. It is demonstrated how the averaging kernel can be used to diagnose the effective vertical resolution of the retrieved profile and, therefore, the depth to which information on the vertical structure can be recovered. This work enables more rigorous exploitation of returns from spaceborne lidar and radar that are subject to multiple scattering than was previously possible.
C1 [Pounder, Nicola L.; Hogan, Robin J.] Univ Reading, Dept Meteorol, Reading RG6 6BB, Berks, England.
[Varnai, Tamas] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Battaglia, Alessandro] Univ Leicester, Dept Phys & Astron, Earth Observat Sci, Leicester LE1 7RH, Leics, England.
[Cahalan, Robert F.] NASA, Goddard Space Flight Ctr, Climate & Radiat Lab, Greenbelt, MD 20771 USA.
RP Pounder, NL (reprint author), Univ Reading, Dept Meteorol, Earley Gate,POB 243, Reading RG6 6BB, Berks, England.
EM n.l.pounder@reading.ac.uk
RI Cahalan, Robert/E-3462-2012; Hogan, Robin/M-6549-2016;
OI Cahalan, Robert/0000-0001-9724-1270; Hogan, Robin/0000-0002-3180-5157;
Battaglia, Alessandro/0000-0001-9243-3484
FU NERC's National Centre for Atmospheric Science [NE/H003894/1]; European
Space Agency [22442/09/NL/CT]
FX This work benefited from the support of NERC's National Centre for
Atmospheric Science (Grant NE/H003894/1) and the European Space Agency
(Contract 22442/09/NL/CT). Marta Janiskova and Dong Huang are thanked
for useful discussions on adjoint coding and L-curve analysis,
respectively.
NR 35
TC 6
Z9 6
U1 0
U2 1
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 FEB
PY 2012
VL 51
IS 2
BP 350
EP 365
DI 10.1175/JAMC-D-10-05007.1
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 889JQ
UT WOS:000300070400011
ER
PT J
AU Leinonen, J
Moisseev, D
Leskinen, M
Petersen, WA
AF Leinonen, Jussi
Moisseev, Dmitri
Leskinen, Matti
Petersen, Walter A.
TI A Climatology of Disdrometer Measurements of Rainfall in Finland over
Five Years with Implications for Global Radar Observations
SO JOURNAL OF APPLIED METEOROLOGY AND CLIMATOLOGY
LA English
DT Article
ID RAINDROP SIZE DISTRIBUTION; POLARIMETRIC RADAR; DISTRIBUTION PARAMETERS;
DIFFERENTIAL REFLECTIVITY; POLARIZATION RADAR; DUAL-WAVELENGTH; DOPPLER
RADAR; PHASE-SHIFT; DISTRIBUTIONS; MODEL
AB To improve the understanding of high-latitude rain microphysics and its implications for the remote sensing of rainfall by ground-based and spaceborne radars, raindrop size measurements have been analyzed that were collected over five years with a Joss-Waldvogel disdrometer located in Jarvenpaa, Finland. The analysis shows that the regional climate is characterized by light rain and small drop size with narrow size distributions and that the mutual relations of drop size distribution parameters differ from those reported at lower latitudes. Radar parameters computed from the distributions demonstrate that the high latitudes are a challenging target for weather radar observations, particularly those employing polarimetric and dual-frequency techniques. Nevertheless, the findings imply that polarimetric ground radars can produce reliable "ground truth" estimates for space observations and identify dual-frequency radars utilizing a W-band channel as promising tools for observing rainfall in the high-latitude climate.
C1 [Leinonen, Jussi] Finnish Meteorol Inst, FIN-00101 Helsinki, Finland.
[Leinonen, Jussi] Aalto Univ, Dept Appl Phys, Espoo, Finland.
[Moisseev, Dmitri; Leskinen, Matti] Univ Helsinki, Dept Phys, Helsinki, Finland.
[Petersen, Walter A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Leinonen, J (reprint author), Finnish Meteorol Inst, POB 503, FIN-00101 Helsinki, Finland.
EM jussi.leinonen@fmi.fi
RI Moisseev, Dmitri/A-3288-2008; Measurement, Global/C-4698-2015;
OI Moisseev, Dmitri/0000-0002-4575-0409; Leinonen,
Jussi/0000-0002-6560-6316
FU Academy of Finland GPM [128255, 128328]; NASA
FX This work was supported by the Academy of Finland GPM Grants 128255 and
128328. Walter A. Petersen acknowledges funding from both the NASA PMM
Science Program (Dr. R. Kakar) and the NASA GPM Mission (Drs. A. Hou and
M. Schwaller). Jussi Leinonen thanks Dr. V. N. Bringi for valuable
discussions about the analysis.
NR 43
TC 15
Z9 15
U1 0
U2 9
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 FEB
PY 2012
VL 51
IS 2
BP 392
EP 404
DI 10.1175/JAMC-D-11-056.1
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 889JQ
UT WOS:000300070400014
ER
PT J
AU Lau, WKM
Zhou, YP
AF Lau, William K. M.
Zhou, Y. P.
TI Observed recent trends in tropical cyclone rainfall over the North
Atlantic and the North Pacific
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SEA-SURFACE TEMPERATURE; UNITED-STATES; CLIMATOLOGICAL RAINFALL; GLOBAL
PRECIPITATION; INTENSITY; CLIMATE; MODEL; SENSITIVITY; PERSPECTIVE;
REANALYSIS
AB In this study, we use Tropical Rainfall Measurement Mission and Global Precipitation Climatology Project rainfall data together with historical storm track records to examine the trend of tropical cyclone (TC) rainfall in the North Atlantic and the northeast and northwest Pacific during two recent decades (1988-1997 and 1998-2007). We find that there is an approximate linear relationship between TC rain (defined as accumulated total rainfall along storm tracks) and storm intensity as classified by the Saffir-Simpson scheme. During the data period, total TC rain has trended upward at a rate of 23.8% +/- 23.5% per decade over the North Atlantic but downward with a rate of 25.1% +/- 19.7% per decade over the northeast Pacific. Over the northwest Pacific, there is a reduction in TC rain of approximately 20.9% +/- 13.5% per decade, possibly associated with a strong interdecadal-scale oscillation. Storm characteristics such as duration and TC rain energy per storm (EPS) remain unchanged for the North Atlantic and the northeast Pacific. For the northwest Pacific, a 28% +/- 18% reduction in EPS from the first decade (1988-1997) to the second decade (1998-2007) is found with the track data from the Joint Typhoon Warning Center. Analyses of the probability distribution function of TC rain show that there is an overall increase in TC frequency across the entire TC rainfall spectrum over the North Atlantic but an overall decrease for the northeast Pacific. In the northwest Pacific, we find a redistribution in EPS with decreased frequency in heavy-rain storms and increased frequency in light-rain storms. Overall, trends in TC rain in the different ocean basins are consistent with long-term relative changes in the ambient large-scale sea surface temperature and vertical wind shear and, to a lesser extent, tropical cyclone Maximum Potential Intensity.
C1 [Lau, William K. M.] NASA, Atmospheres Lab, Div Earth Sci, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Zhou, Y. P.] Morgan State Univ, Greenbelt, MD USA.
RP Lau, WKM (reprint author), NASA, Atmospheres Lab, Div Earth Sci, Goddard Space Flight Ctr, Code 610, Greenbelt, MD 20771 USA.
EM william.k.lau@nasa.gov
RI Lau, William /E-1510-2012
OI Lau, William /0000-0002-3587-3691
FU Precipitation Measuring Mission, NASA Earth Science Division
FX This work is supported by the Precipitation Measuring Mission (R. Kakar,
Headquarters Manager), NASA Earth Science Division. The authors thank C.
Landsea, M. Shepherd, and another anonymous reviewer for their critical
comments on the earlier manuscript. NCEP Reanalysis data are obtained
from the NOAA/OAR/ESRL PSD, Boulder, Colorado, USA, from their Web site
at http://www.esrl.noaa.gov/psd/.
NR 51
TC 8
Z9 8
U1 2
U2 17
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 FEB 1
PY 2012
VL 117
AR D03104
DI 10.1029/2011JD016510
PG 13
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 887VQ
UT WOS:000299959900005
ER
PT J
AU Wells, KC
Martins, JV
Remer, LA
Kreidenweis, SM
Stephens, GL
AF Wells, Kelley C.
Martins, J. Vanderlei
Remer, Lorraine A.
Kreidenweis, Sonia M.
Stephens, Graeme L.
TI Critical reflectance derived from MODIS: Application for the retrieval
of aerosol absorption over desert regions
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID SKY RADIANCE MEASUREMENTS; RADIATIVE-TRANSFER; OPTICAL-PROPERTIES; DUST;
SCATTERING; SATELLITE; ALGORITHM; SENSITIVITY; ASSESSMENTS; NETWORK
AB The determination of aerosol direct radiative forcing over desert regions requires accurate information about the aerosol single-scattering albedo (SSA); however, the brightness of desert surfaces in the visible and near-IR range complicates the retrieval of aerosol optical properties using passive space-based measurements. Here we use the critical reflectance method to retrieve spectral aerosol absorption from space over North Africa, a desert region that is predominantly impacted by absorbing dust and biomass burning aerosol. We examine the sensitivity of the critical reflectance parameter to aerosol physical and optical properties that are representative of the region, and we find that the critical reflectance has low sensitivity to assumptions of aerosol size and refractive index for dust-like particles, except at scattering angles near 180 degrees, which should be avoided with this method. We use our findings to retrieve spectral SSA from critical reflectance derived from Moderate Resolution Imaging Spectroradiometer (MODIS) reflectances in the vicinity of two Aerosol Robotic Network (AERONET) stations: Tamanrasset, in the Algerian Sahara, and Banizoumbou, in the Sahel. We retrieve lower aerosol SSAs at Banizoumbou, which is often impacted by dust-smoke mixtures, and higher SSAs at Tamanrasset, where pure desert dust is the dominant aerosol. Our results generally fall within the AERONET uncertainty envelopes, although at Banizoumbou we retrieve a spectral dependence different from that of AERONET. On the basis of our analysis, we expect to be able to retrieve SSA from critical reflectance for pure dust with an uncertainty of 0.02 and to provide spatial and spectral SSA information that will help reduce current uncertainties in the aerosol radiative forcing over desert regions.
C1 [Wells, Kelley C.; Kreidenweis, Sonia M.; Stephens, Graeme L.] Colorado State Univ, Dept Atmospher Sci, Ft Collins, CO 80523 USA.
[Martins, J. Vanderlei] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Martins, J. Vanderlei] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA.
[Remer, Lorraine A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Wells, KC (reprint author), Univ Minnesota, Dept Soil Water & Climate, 439 Borlaug Hall,1991 Upper Buford Cir, St Paul, MN 55108 USA.
EM kcw@umn.edu; martins@umbc.edu; Lorraine.a.remer@nasa.gov;
sonia@atmos.colostate.edu; stephens@atmos.colostate.edu
RI Kreidenweis, Sonia/E-5993-2011
OI Kreidenweis, Sonia/0000-0002-2561-2914
FU Center for Earth-Atmosphere Studies through NASA [NNX08AT77G]; NOAA
[NA17RJ1228]
FX This work was supported by the Center for Earth-Atmosphere Studies
through NASA grant NNX08AT77G, with additional funding from NOAA grant
NA17RJ1228. We thank Didier Tanre, Emilio Cuevas-Agullo, and Mohamed
Mimouni for their efforts in establishing and maintaining the
Banizoumbou and Tamanrasset AERONET sites, and we thank the MODIS team
for their efforts in calibration and maintenance of the MODIS instrument
and data. We would also like to thank Li Zhu, Tom Eck, Rob Levy, Shana
Mattoo, and the anonymous reviewers for their helpful suggestions in
developing and revising this work.
NR 33
TC 3
Z9 3
U1 0
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 FEB 1
PY 2012
VL 117
AR D03202
DI 10.1029/2011JD016891
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 887VQ
UT WOS:000299959900009
ER
PT J
AU Burchill, JK
Clemmons, JH
Knudsen, DJ
Larsen, M
Nicolls, MJ
Pfaff, RF
Rowland, D
Sangalli, L
AF Burchill, J. K.
Clemmons, J. H.
Knudsen, D. J.
Larsen, M.
Nicolls, M. J.
Pfaff, R. F.
Rowland, D.
Sangalli, L.
TI High-latitude E region ionosphere-thermosphere coupling: A comparative
study using in situ and incoherent scatter radar observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID NEUTRAL COLLISION FREQUENCY; CHAMP OBSERVATIONS; WAVES; PLASMA; DRAG;
PARAMETERS; ATMOSPHERE; DENSITY; MODEL; WIND
AB We present in situ and ground-based measurements of the ratio kappa of ion cyclotron angular frequency to ion-neutral momentum transfer collision frequency to investigate ionosphere-thermosphere (IT) coupling in the auroral E region. In situ observations were obtained by NASA sounding rocket 36.234, which was launched into the nightside E region ionosphere at 1229 UT on 19 January 2007 from Poker Flat, AK. The payload carried instrumentation to determine ion drift angle and electric field vectors. Neutral winds were measured by triangulating a chemical tracer released from rocket 41.064 launched two minutes later. kappa is calculated from the rotation of the ion drift angle relative to the E-cross-B drift direction in a frame co-rotating with the payload. Between the altitudes of 118 km and 130 km kappa increases exponentially with a scale height of 9.3 +/- 0.7 km, deviating from an exponential above 130 km. kappa = 1 at an altitude z(0) of 119.9 +/- 0.5 km. The ratio was also estimated from Poker Flat Incoherent Scatter Radar (PFISR) measurements using the rotation of ion velocity with altitude. Exponential fits to the PFISR measurements made during the flight of 41.064 yield z(0) = 115.9 +/- 1.2 km and a scale height of 9.1 +/- 1.0 km. Differences between in situ and ground-based measurements show that the E region atmospheric densities were structured vertically and/or horizontally on scales of 1 km to 10 km. There were no signs of ionospheric structure in ion density or ion temperature below scales of 1 km. The observations demonstrate the accuracy with which the in situ and PFISR data may be used as probes of IT coupling.
C1 [Burchill, J. K.; Knudsen, D. J.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada.
[Clemmons, J. H.] Aerosp Corp, Space Sci Applicat Lab, El Segundo, CA 90245 USA.
[Larsen, M.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA.
[Nicolls, M. J.] SRI Int, Ctr Geospace Studies, Menlo Pk, CA 94025 USA.
[Pfaff, R. F.; Rowland, D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sangalli, L.] Royal Mil Coll Canada, Dept Phys, Kingston, ON K7K 7B4, Canada.
RP Burchill, JK (reprint author), Univ Calgary, Dept Phys & Astron, 2500 Univ Dr NW, Calgary, AB T2N 1N4, Canada.
EM burchill@phys.ucalgary.ca
RI Rowland, Douglas/F-5589-2012; Larsen, Miguel/A-1079-2013; Pfaff,
Robert/F-5703-2012; Nicolls, Michael/N-8680-2013;
OI Rowland, Douglas/0000-0003-0948-6257; Pfaff, Robert/0000-0002-4881-9715;
Nicolls, Michael/0000-0001-8267-6327; Clemmons,
James/0000-0002-5298-5222
FU Canadian Space Agency; Natural Sciences and Engineering Research Council
of Canada; NSF [ATM-0608577, ATM-0719808, AGS-1007539]; NASA
[NNX07AJ99G]
FX This research was supported by the Canadian Space Agency and the Natural
Sciences and Engineering Research Council of Canada. Joule II SII
development was supported by a contract from the Canadian Space Agency.
The authors acknowledge the contributions and expertise of the SII
development team, R. B. Hriskevich, J. T. Forshaw, R. M. Thomson, J. G.
Aase, and E. P. King, and of the Joule II payload team at the NASA
Wallops Flight Facility. PFISR data and collection and analysis was
supported by NSF cooperative agreement ATM-0608577, and work at SRI
International was supported by NSF grant ATM-0719808. MFL was partially
supported under NASA grant NNX07AJ99G and NSF grant AGS-1007539. JKB
appreciates valuable discussions with B. Jackel, R. Schunk and J.- P.
St.-Maurice.
NR 34
TC 5
Z9 6
U1 0
U2 9
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 FEB 1
PY 2012
VL 117
AR A02301
DI 10.1029/2011JA017175
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 888FR
UT WOS:000299989700002
ER
PT J
AU Vinukollu, RK
Sheffield, J
Wood, EF
Bosilovich, MG
Mocko, D
AF Vinukollu, Raghuveer K.
Sheffield, Justin
Wood, Eric F.
Bosilovich, Michael G.
Mocko, David
TI Multimodel Analysis of Energy and Water Fluxes: Intercomparisons between
Operational Analyses, a Land Surface Model, and Remote Sensing
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID GENERAL-CIRCULATION MODELS; ASSIMILATION SYSTEM NLDAS; RIVER-BASIN;
GLOBAL PRECIPITATION; ECMWF REANALYSIS; ETA-MODEL; RADIATION BUDGET;
PART I; BALANCE; CEOP
AB Using data from seven global model operational analyses (OA), one land surface model, and various remote sensing retrievals, the energy and water fluxes over global land areas are intercompared for 2003/04. Remote sensing estimates of evapotranspiration (ET) are obtained from three process-based models that use input forcings from multisensor satellites. An ensemble mean (linear average) of the seven operational (mean-OA) models is used primarily to intercompare the fluxes with comparisons performed at both global and basin scales. At the global scale, it is found that all components of the energy budget represented by the ensemble mean of the OA models have a significant bias. Net radiation estimates had a positive bias (global mean) of 234 MJ m(-2) yr(-1) (7.4 W m(-2)) as compared to the remote sensing estimates, with the latent and sensible heat fluxes biased by 470 MJ m(-2) yr(-1) (13.3 W m(-2)) and -367 MJ m(-2) yr(-1) (11.7 W m(-2)), respectively. The bias in the latent heat flux is affected by the bias in the net radiation, which is primarily due to the biases in the incoming shortwave and outgoing longwave radiation and to the nudging process of the operational models. The OA models also suffer from improper partitioning of the surface heat fluxes. Comparison of precipitation (P) analyses from the various OA models, gauge analysis, and remote sensing retrievals showed better agreement than the energy fluxes. Basin-scale comparisons were consistent with the global-scale results, with the results for the Amazon in particular showing disparities between OA and remote sensing estimates of energy fluxes. The biases in the fluxes are attributable to a combination of errors in the forcing from the OA atmospheric models and the flux calculation methods in their land surface schemes. The atmospheric forcing errors are mainly attributable to high shortwave radiation likely due to the underestimation of clouds, but also precipitation errors, especially in water-limited regions.
C1 [Vinukollu, Raghuveer K.; Sheffield, Justin; Wood, Eric F.] Princeton Univ, CEE Dept, Princeton, NJ 08544 USA.
[Vinukollu, Raghuveer K.] Swiss Re, Armonk, NY USA.
[Bosilovich, Michael G.; Mocko, David] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Mocko, David] Sci Applicat Int Corp, Mclean, VA 22102 USA.
RP Wood, EF (reprint author), Princeton Univ, CEE Dept, EQUAD Olden St, Princeton, NJ 08544 USA.
EM efwood@princeton.edu
RI Bosilovich, Michael/F-8175-2012; Houser, Paul/J-9515-2013
OI Houser, Paul/0000-0002-2991-0441
FU NASA [NNG04GQ32G, NNX08AN40A, NNX09AK35G]
FX This work was jointly supported by NASA Grants NNG04GQ32G "A Terrestrial
Evaporation Data Product Using MODIS Data," NNX08AN40A "Developing
Consistent Earth System Data Records for the Global Terrestrial Water
Cycle," and NNX09AK35G "Development and Diagnostic Analysis of a
Multidecadal Global Evaporation Product." The operational model data for
the current study were obtained from the authors of Bosilovich et al.
(2009), which is part of the Coordinated Energy and Water Observation
Project (CEOP, GEWEX), NASA Langley Research Center Atmospheric Science
Data Center, Global Precipitation Climatology Center (GPCC),
MEDIAS-France, and the Global River Discharge Center (GRDC).
NR 80
TC 11
Z9 11
U1 0
U2 24
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD FEB
PY 2012
VL 13
IS 1
BP 3
EP 26
DI 10.1175/2011JHM1372.1
PG 24
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 890IN
UT WOS:000300138400001
ER
PT J
AU Kidd, C
Bauer, P
Turk, J
Huffman, GJ
Joyce, R
Hsu, KL
Braithwaite, D
AF Kidd, C.
Bauer, P.
Turk, J.
Huffman, G. J.
Joyce, R.
Hsu, K. -L.
Braithwaite, D.
TI Intercomparison of High-Resolution Precipitation Products over Northwest
Europe
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID DIRECT 4D-VAR ASSIMILATION; MICROWAVE SOUNDING UNIT; GLOBAL
PRECIPITATION; RAINFALL ESTIMATION; PASSIVE MICROWAVE; TROPICAL
RAINFALL; PART I; SATELLITE; ALGORITHMS; RETRIEVAL
AB Satellite-derived high-resolution precipitation products (HRPP) have been developed to address the needs of the user community and are now available with 0.25 degrees X 0.25 degrees (or less) subdaily resolutions. This paper evaluates a number of commonly available satellite-derived HRPPs covering northwest Europe over a 6-yr period. Precipitation products include the Tropical Rainfall Measuring Mission (TRMM) Multisatellite Precipitation Analysis (TMPA), the Climate Prediction Center (CPC) morphing (CMORPH) technique, the CPC merged microwave technique, the Naval Research Laboratory (NRL) blended technique, and the Precipitation Estimation from Remotely Sensed Information using Artificial Neural Networks (PERSIANN) technique. In addition, the Geosynchronous Operational Environmental Satellite (GOES) precipitation index (GPI) and the European Centre for Medium-Range Weather Forecasting (ECMWF) operational forecast model products are included for comparison. Surface reference data from the European radar network is used as ground truth, supported by the Global Precipitation Climatology Centre (GPCC) precipitation gauge analysis and gauge data over the United Kingdom. Measures of correlation, bias ratio, probability of detection, and false alarm ratio are used to evaluate the products. Results show that satellite products generally exhibit a seasonal cycle in correlation, bias ratio, probability of detection, and false alarm ratio, with poorer statistics during the winter. The ECMWF model also shows a seasonal cycle in the correlation, although the results are poorer during the summer, while the bias ratio, probability of detection, and false alarm ratio are consistent through all seasons. Importantly, all the satellite HRPPs underestimate precipitation over northwest Europe in all seasons.
C1 [Kidd, C.; Huffman, G. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20706 USA.
[Kidd, C.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA.
[Bauer, P.] European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England.
[Turk, J.] NASA, Jet Prop Lab, Pasadena, CA USA.
[Huffman, G. J.] Sci Syst & Applicat Inc, Lanham, MD USA.
[Joyce, R.] NOAA, Natl Ctr Environm Predict, Climate Predict Ctr, Camp Springs, MD USA.
[Hsu, K. -L.; Braithwaite, D.] Univ Calif Irvine, Henry Samueli Sch Engn, Irvine, CA USA.
RP Kidd, C (reprint author), NASA, Goddard Space Flight Ctr, Code 612-0, Greenbelt, MD 20706 USA.
EM chris.kidd@nasa.gov
RI Huffman, George/F-4494-2014; Kidd, Christopher/H-9910-2014
OI Huffman, George/0000-0003-3858-8308;
NR 59
TC 56
Z9 57
U1 3
U2 42
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD FEB
PY 2012
VL 13
IS 1
BP 67
EP 83
DI 10.1175/JHM-D-11-042.1
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 890IN
UT WOS:000300138400004
ER
PT J
AU Mahanama, S
Livneh, B
Koster, R
Lettenmaier, D
Reichle, R
AF Mahanama, Sartih
Livneh, Ben
Koster, Randal
Lettenmaier, Dennis
Reichle, Rolf
TI Soil Moisture, Snow, and Seasonal Streamflow Forecasts in the United
States
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID LATITUDE HYDROLOGICAL PROCESSES; CATCHMENT-BASED APPROACH; LAND-SURFACE
PROCESSES; MESOSCALE ETA-MODEL; TORNE-KALIX BASIN; WESTERN US; PILPS
PHASE-2(E); RIVER-BASIN; PREDICTABILITY; SIMULATION
AB Land surface model experiments are used to quantify, for a number of U.S. river basins, the contributions (isolated and combined) of soil moisture and snowpack initialization to the skill of seasonal streamflow forecasts at multiple leads and for different start dates. Snow initialization has a major impact on skill during the spring melting season. Soil moisture initialization has a smaller but still statistically significant impact during this season, and in other seasons, its contribution to skill dominates. Realistic soil moisture initialization can contribute to skill at long leads (over 6 months) for certain basins and seasons. Skill levels in all seasons are found to be related to the ratio of initial total water storage (soil water plus snow) variance to the forecast period precipitation variance, allowing estimates of the potential for skill in areas outside the verification basins.
C1 [Mahanama, Sartih; Koster, Randal; Reichle, Rolf] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Mahanama, Sartih] Sci Applicat Int Corp, Beltsville, MD USA.
[Livneh, Ben; Lettenmaier, Dennis] Univ Washington, Dept Civil & Environm Engn, Seattle, WA 98195 USA.
RP Mahanama, S (reprint author), NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Mail Stop 610-1, Greenbelt, MD 20771 USA.
EM sarith.p.mahanama@nasa.gov
RI Reichle, Rolf/E-1419-2012; Koster, Randal/F-5881-2012; lettenmaier,
dennis/F-8780-2011; Livneh, Ben/I-2939-2015;
OI Koster, Randal/0000-0001-6418-6383; lettenmaier,
dennis/0000-0003-3317-1327; LIVNEH, BEN/0000-0001-5445-2473
FU NASA
FX We thank James Verdin for discussions at the onset of this study. We
also thank the providers of the naturalized western streamflow data:
U.S. Army Corps of Engineers, Omaha NB office, for the Missouri River
basin; U.S. Army Corps of Engineers, Tulsa OK office, for the Arkansas
Red River basin; Columbia River Basin Climate Change Scenarios Database
for the Columbia River basin; California Data Exchange Commission for
the California basins; and U.S. Bureau of Reclamation, Lower Colorado
Region, for the Colorado River basin. We further thank Professor Edwin
Maurer (Santa Clara University) for his assistance in obtaining
naturalized streamflow data for the eastern and central U.S. river
basins. Funding for much of this study was provided by NASA's
Terrestrial Hydrology Program.
NR 41
TC 47
Z9 47
U1 0
U2 23
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD FEB
PY 2012
VL 13
IS 1
BP 189
EP 203
DI 10.1175/JHM-D-11-046.1
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 890IN
UT WOS:000300138400011
ER
PT J
AU Tokay, A
Ozturk, K
AF Tokay, Ali
Ozturk, Kurtulus
TI An Experimental Study of the Small-Scale Variability of Rainfall
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID TRMM PRECIPITATION RADAR; MEASURING MISSION TRMM; GROUND-VALIDATION;
GAUGE MEASUREMENTS; STOCHASTIC-MODEL; FIELD CAMPAIGN; ERRORS; PRODUCTS
AB Small-scale variability of rainfall has been studied employing six dual rain gauge sites at Wallops Island, Virginia. The rain gauge sites were separated between 0.4 and 5 km, matching the beamwidth of Tropical Rainfall Measuring Mission (TRMM) and Global Precipitation Measurement (GPM) precipitation radars. During a 2-yr observational period, over 7100 rainy samples were received at 5-min integration. A single gauge did not report as high as 67% of the time when at least one of the other gauges had rainfall in one of the seasons. Since rainfall from one of the six rain gauges is sufficient for the rainy footprint from a satellite, this demonstrates the common occurrence of the partial beamfilling. For the periods where all gauges were reporting rainfall, a single gauge had at most 13% difference from the areal average rainfall in one of the seasons. This suggests that at the spatial scale of 5 km, the variability caused by the rain gradient is relatively less important than the variability arising from a partially tilled footprint. During the passage of frontal systems and tropical cyclones, the beam was filled by rain most of the time and this resulted in relatively higher correlation distances. The correlation distance had a sharp drop off from 45 km in moderately variable rainfall to 3 km in highly variable rainfall and ranged from 5 to 35 km between the different seasons. This demonstrates its highly variable nature. Considering temporal sampling, the monthly rainfall error was 35% and 73% for 3-hourly and twice-daily observations, respectively.
C1 [Tokay, Ali] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Tokay, Ali] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA.
[Ozturk, Kurtulus] Turkish State Meteorol Serv, Ankara, Turkey.
RP Tokay, A (reprint author), NASA, Goddard Space Flight Ctr, Code 613-1, Greenbelt, MD 20771 USA.
EM ali.tokay-1@nasa.gov
RI Measurement, Global/C-4698-2015
FU NASA [NNX07AF45G]
FX We thank our senior technician, Paul G. Bashor of Computer Science
Corporation, NASA Wallops Flight Facility for his dedicated work on
operating the gauge network and reviewing this manuscript. Discussions
with Prasun Kundu of the University of Maryland, Baltimore County; S.
Joseph Munchak of the University of Maryland, College Park; and Robert
Meneghini of NASA Goddard Space Flight Center were very helpful. Thanks
to David A. Marks of Science Systems Applications Inc., and Amy J.
Houghton of the University of Maryland, Baltimore County for the review.
Special thanks to Drs. Emad Habib of the University of Louisiana at
Lafayette, Gabriele Villarini of Princeton University, and an anonymous
reviewer for their constructive reviews. This work has been conducted
during the second author's visit to the NASA GSFC as a GEST fellow. This
work is funded through NASA under Grant NNX07AF45G.
NR 26
TC 11
Z9 11
U1 1
U2 10
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD FEB
PY 2012
VL 13
IS 1
BP 351
EP 365
DI 10.1175/JHM-D-11-014.1
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 890IN
UT WOS:000300138400022
ER
PT J
AU Lau, WKM
Kim, KM
AF Lau, William K. M.
Kim, Kyu-Myong
TI The 2010 Pakistan Flood and Russian Heat Wave: Teleconnection of
Hydrometeorological Extremes
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID MID-TROPOSPHERIC CYCLONES; PRECIPITATION; MONSOON; SUMMER
AB In this paper, preliminary results are presented showing that the two record-setting extreme events during 2010 summer (i.e., the Russian heat wave-wildfires and Pakistan flood) were physically connected. It is found that the Russian heat wave was associated with the development of an extraordinarily strong and prolonged extratropical atmospheric blocking event in association with the excitation of a large-scale atmospheric Rossby wave train spanning western Russia. Kazakhstan, and the northwestern China Tibetan Plateau region. The southward penetration of upper-level vorticity perturbations in the leading trough of the Rossby wave was instrumental in triggering anomalously heavy rain events over northern Pakistan and vicinity in mid- to late July. Also shown are evidences that the Russian heat wave was amplified by a positive feedback through changes in surface energy fluxes between the atmospheric blocking pattern and an underlying extensive land region with below-normal soil moisture. The Pakistan heavy rain events were amplified and sustained by strong anomalous southeasterly flow along the Himalayan foothills and abundant moisture transport from the Bay of Bengal in connection with the northward propagation of the monsoonal intraseasonal oscillation.
C1 [Lau, William K. M.] NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD 20771 USA.
[Kim, Kyu-Myong] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
RP Lau, WKM (reprint author), NASA, Goddard Space Flight Ctr, Div Earth Sci, Greenbelt, MD 20771 USA.
EM william.k.lau@nasa.gov
RI Kim, Kyu-Myong/G-5398-2014; Lau, William /E-1510-2012
OI Lau, William /0000-0002-3587-3691
FU NASA Interdisciplinary Investigation; Tropical Rainfall Measuring
Mission (TRMM); Korean Meteorological Administration [RACS_2010-2018]
FX This work was supported by the NASA Interdisciplinary Investigation and
the Tropical Rainfall Measuring Mission (TRMM). K.-M. Kim was supported
by the Korean Meteorological Administration Research and Development
Program under Grant RACS_2010-2018. We thank two anonymous reviewers for
their critical and detailed review of the paper.
NR 21
TC 66
Z9 69
U1 1
U2 24
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 FEB
PY 2012
VL 13
IS 1
BP 392
EP 403
DI 10.1175/JHM-D-11-016.1
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 890IN
UT WOS:000300138400025
ER
PT J
AU Seneviratne, SI
Koster, RD
AF Seneviratne, Sonia I.
Koster, Randal D.
TI A Revised Framework for Analyzing Soil Moisture Memory in Climate Data:
Derivation and Interpretation
SO JOURNAL OF HYDROMETEOROLOGY
LA English
DT Article
ID ATMOSPHERE COUPLING EXPERIMENT; MODELS; IMPACTS; EUROPE; SKILL; GLACE
AB A revised framework for the analysis of soil moisture memory characteristics of climate models and observational data is derived from the approach proposed by Koster and Suarez. The resulting equation allows the expression of the month-to-month soil moisture autocorrelation as a function of 1) the initial soil moisture variability, 2) the (atmospheric) forcing variability over the considered time period, 3) the correlation between initial soil moisture and subsequent forcing, 4) the sensitivity of evaporation to soil moisture, and 5) the sensitivity of runoff to soil moisture. A specific new feature is the disentangling of the roles of initial soil moisture variability and forcing variability, which were both (for the latter indirectly) contributing to the seasonality term of the original formulation. In addition, a version of the framework entirely based on explicit equations for the underlying relationships (i.e., independent of soil moisture statistics at the following time step) is proposed. The validity of the derived equation is exemplified with atmospheric general circulation model (AGCM) simulations from the Global Land Atmosphere Coupling Experiment (GLACE).
C1 [Seneviratne, Sonia I.] ETH, Inst Atmospher & Climate Sci, CH-8092 Zurich, Switzerland.
[Koster, Randal D.] NASA Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
RP Seneviratne, SI (reprint author), ETH, Inst Atmospher & Climate Sci, Univ Str 16, CH-8092 Zurich, Switzerland.
EM sonia.seneviratne@env.ethz.ch
RI Koster, Randal/F-5881-2012; Seneviratne, Sonia/G-8761-2011
OI Koster, Randal/0000-0001-6418-6383; Seneviratne,
Sonia/0000-0001-9528-2917
NR 19
TC 21
Z9 21
U1 1
U2 26
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 1525-755X
J9 J HYDROMETEOROL
JI J. Hydrometeorol.
PD FEB
PY 2012
VL 13
IS 1
BP 404
EP 412
DI 10.1175/JHM-D-11-044.1
PG 9
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 890IN
UT WOS:000300138400026
ER
PT J
AU Layton, BE
Lynch, B
Peter, T
Jamieson, B
AF Layton, Bradley E.
Lynch, Bernard
Peter, Thomas
Jamieson, Brian
TI Red blood cell sorting with a multi-bed microfabricated filter
SO JOURNAL OF MICROMECHANICS AND MICROENGINEERING
LA English
DT Article
ID ERYTHROCYTE AGGREGATION; HEART-FAILURE; SEPARATION; FLOW; MICROCHANNEL;
MICROSYSTEMS; FLUCTUATIONS; DYNAMICS; SURFACES; ANALYZER
AB A microfabricated fluidic chip for sorting red blood cells (RBCs) by size has been designed, fabricated and tested. The performance of the chip has been compared against a flow cytometer using samples from identical populations of cells, and statistically significant (p < 0.0005) differences in the measured cell size distributions were observed. The measurement paradigm reported here differs from previously demonstrated devices such as microfabricated Coulter counters or flow cytometers, in that the analysis is inherently parallel and is thus suitable for high throughput, point-of-care analysis. This study is empirical and semi-quantitative. However, important features of RBC trapping are characterized and indications for improved device design are described.
C1 [Layton, Bradley E.] Univ Montana, Dept Appl Comp & Elect, Missoula, MT 59802 USA.
[Lynch, Bernard; Jamieson, Brian] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Peter, Thomas] Univ Michigan, Dept Biomed Engn, Ann Arbor, MI 48109 USA.
[Jamieson, Brian] Sci & Biomed Microsyst, Columbia, MD 21046 USA.
RP Layton, BE (reprint author), Univ Montana, Dept Appl Comp & Elect, 909 S Ave W, Missoula, MT 59802 USA.
EM bradley.layton@umontana.edu
FU NASA [DDF-05-553]
FX This work was supported by NASA DDF-05-553. The authors would like to
acknowledge assistance from Ken Class of the University of Maryland for
consultation and use of equipment. We also thank Ms Stephanie Sullivan
for preliminary protocol development and Dr Kathleen Allen for
researching references. Any opinions, findings and conclusions or
recommendations expressed in this material are those of the authors and
do not necessarily reflect the views of the National Aeronautics and
Space Administration.
NR 51
TC 1
Z9 1
U1 0
U2 12
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0960-1317
J9 J MICROMECH MICROENG
JI J. Micromech. Microeng.
PD FEB
PY 2012
VL 22
IS 2
AR 025009
DI 10.1088/0960-1317/22/2/025009
PG 7
WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology;
Instruments & Instrumentation; Physics, Applied
SC Engineering; Science & Technology - Other Topics; Instruments &
Instrumentation; Physics
GA 887VI
UT WOS:000299959000009
ER
PT J
AU Chatterjee, A
Diordieva, I
Yumoto, K
Globus, RK
Bhattacharya, S
AF Chatterjee, Anuran
Diordieva, Inna
Yumoto, Kenji
Globus, Ruth K.
Bhattacharya, Sharmila
TI Protein array profiling of mouse serum, six months post whole body
radiation with Fe-56
SO JOURNAL OF TOXICOLOGICAL SCIENCES
LA English
DT Article
DE Proteomic; Microarray; Serum; Mice; Radiation
ID SPACE RADIATION; CELLS
AB To determine the chronic effects of heavy ion irradiation, an antibody based proteomic microarray technology was applied to monitor alterations in the serum proteome, six months after whole body irradiation of adult male C57B1/6 mice with 0.5 Gray of Fe-56. Out of 507 proteins, irradiation reduced expression of 25 proteins and enhanced expression of 12 proteins in serum (> 5% change relative to sham-irradiated controls). Of the 25 proteins found to be down-regulated, Poly ADP Ribose Polymerase (PARP) was 13% lower in the 0.5Gy mice and among the up-regulated proteins, beta-Tubulin was found to be 10% higher in the 0.5Gy group compared to the sham-irradiated 0Gy controls. Thus, irradiation with a relatively low dose of heavy ions caused persistent and selective changes in serum levels of proteins that are typically intracellular, suggesting chronic genotoxic damage.
C1 [Chatterjee, Anuran; Yumoto, Kenji; Globus, Ruth K.; Bhattacharya, Sharmila] NASA, Space Biosci Res Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Diordieva, Inna] Clontech Labs, Mountain View, CA 94035 USA.
RP Bhattacharya, S (reprint author), NASA, Space Biosci Res Branch, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM sharmila.bhattacharya@nasa.gov
FU NASA [NNH104Z-UU005N/RAD2004-0000-0110]; DOE-NASA [DE-SC0001507]; Office
of Science (BER), U.S. Department of Energy
FX Research was supported by a NASA grant
(NNH104Z-UU005N/RAD2004-0000-0110) and a DOE-NASA Interagency Award
#DE-SC0001507, supported by the Office of Science (BER), U.S. Department
of Energy to RKG.
NR 4
TC 1
Z9 1
U1 1
U2 3
PU JAPANESE SOC TOXICOLOGICAL SCIENCES
PI TOKYO
PA INTERNATIONAL MEDICAL INFORMATION CENTER, SHINANOMACHI RENGAKAN, 35
SHINANO-MACHI, SHINJUKU-KU, TOKYO, 160-0016, JAPAN
SN 0388-1350
EI 1880-3989
J9 J TOXICOL SCI
JI J. Toxicol. Sci.
PD FEB
PY 2012
VL 37
IS 1
BP 215
EP 217
PG 3
WC Toxicology
SC Toxicology
GA 890IX
UT WOS:000300139400020
PM 22293426
ER
PT J
AU Nakashima, D
Ushikubo, T
Zolensky, ME
Kita, NT
AF Nakashima, Daisuke
Ushikubo, Takayuki
Zolensky, Michael E.
Kita, Noriko T.
TI High precision oxygen three-isotope analyses of anhydrous chondritic
interplanetary dust particles
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID EARLY SOLAR NEBULA; CARBONACEOUS CHONDRITES; ISOTOPIC COMPOSITIONS;
COMET 81P/WILD-2; SILICATE GRAINS; ION MICROPROBE; CHONDRULES; SYSTEM;
ALLENDE; ORIGIN
AB Oxygen three-isotope ratios of three anhydrous chondritic interplanetary dust particles (IDPs) were analyzed using an ion microprobe with a 2 mu m small beam. The three anhydrous IDPs show Delta 17O values ranging from -5 parts per thousand to +1 parts per thousand, which overlap with those of ferromagnesian silicate particles from comet Wild 2 and anhydrous porous IDPs. For the first time, internal oxygen isotope heterogeneity was resolved in two IDPs at the level of a few per mil in Delta 17O values. Anhydrous IDPs are loose aggregates of fine-grained silicates (=3 mu m in this study), with only a few coarse-grained silicates (220 mu m in this study). On the other hand, Wild 2 particles analyzed so far show relatively coarse-grained (= few mu m) igneous textures. If anhydrous IDPs represent fine-grained particles from comets, the similar Delta 17O values between anhydrous IDPs and Wild 2 particles may imply that oxygen isotope ratios in cometary crystalline silicates are similar, independent of crystal sizes and their textures. The range of Delta 17O values of the three anhydrous IDPs overlaps also with that of chondrules in carbonaceous chondrites, suggesting a genetic link between cometary dust particles (Wild 2 particles and most anhydrous IDPs) and carbonaceous chondrite chondrules.
C1 [Nakashima, Daisuke; Ushikubo, Takayuki; Kita, Noriko T.] Univ Wisconsin, Dept Geosci, WiscSIMS, Madison, WI 53706 USA.
[Zolensky, Michael E.] NASA Johnson Space Ctr, Astromat Res & Explorat Sci, Houston, TX 77058 USA.
RP Nakashima, D (reprint author), Univ Wisconsin, Dept Geosci, WiscSIMS, Madison, WI 53706 USA.
EM naka@geology.wisc.edu
RI Kita, Noriko/H-8035-2016
OI Kita, Noriko/0000-0002-0204-0765
FU NASA LARS [NK, NNX09AC30G]; NSF-EAR [0319230, 0744079]; NASA
FX Thoughtful comments from T. Stephan, J. Aleon, S. Messenger, and C.
Floss improved the quality of this manuscript significantly. The authors
thank R. K. Noll for help with FE-SEM observation, P. E. Brown for
lending a high magnification objective lens for optical microscope, H.
Xu for allowing using a polarizing microscope, and J. Kern for SIMS
support. This work is supported by the NASA LARS program (NK,
NNX09AC30G). WiscSIMS is partly supported by NSF-EAR (0319230, 0744079).
M. Z. was supported by NASA's Cosmochemistry and Laboratory Analysis of
Returned Samples Programs.
NR 59
TC 9
Z9 9
U1 0
U2 10
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD FEB
PY 2012
VL 47
IS 2
BP 197
EP 208
DI 10.1111/j.1945-5100.2011.01319.x
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 887MI
UT WOS:000299931200003
ER
PT J
AU Angel, SM
Gomer, NR
Sharma, SK
Mckay, C
AF Angel, S. Michael
Gomer, Nathaniel R.
Sharma, Shiv K.
Mckay, Chris
TI Remote Raman Spectroscopy for Planetary Exploration: A Review
SO APPLIED SPECTROSCOPY
LA English
DT Review
DE Planetary Raman; Standoff Raman; Astrospectroscopy; Laser-induced
breakdown spectroscopy; LABS; Laser-induced fluorescence; LIE; Europa;
Enceladus; Astrobiology
ID NM LASER-PULSE; STANDOFF DETECTION; SUBSURFACE OCEAN; MINERAL
IDENTIFICATION; MARTIAN METEORITE; RADIAL DISTANCE; 100 METERS;
RIO-TINTO; SPECTRA; MARS
AB In this review, we discuss the current state of standoff Raman spectroscopy as it applies to remote planetary applications, including standoff instrumentation, the technique's ability to identify biologically and geologically important analytes, and the feasibility to make standoff Raman measurements under various planetary conditions. This is not intended to be an exhaustive review of standoff Raman and many excellent papers are not mentioned. Rather it is intended to give the reader a quick review of the types of standoff Raman systems that are being developed and that might be suitable for astrospectroscopy, a look at specific analytes that are of interest for planetary applications, planetary measurement opportunities and challenges that need to be solved, and a brief discussion of the feasibility of making surface and plume planetary Raman measurements from an orbiting spacecraft.
C1 [Angel, S. Michael; Gomer, Nathaniel R.] Univ S Carolina, Dept Chem & Biochem, Columbia, SC 29208 USA.
[Sharma, Shiv K.] Univ Hawaii, Hawaii Inst Geophys Planetol, Honolulu, HI 96822 USA.
[Mckay, Chris] NASA Ames, Moffett Field, CA 94035 USA.
RP Angel, SM (reprint author), Univ S Carolina, Dept Chem & Biochem, Columbia, SC 29208 USA.
EM angel@chem.sc.edu
OI Angel, Stanley/0000-0002-0328-0568
FU NSF [CHE 0526821]; NASA under a MIDDP [NNX08AR10G]
FX The authors at USC would like to thank NSF for funding for some of the
work presented under CHE 0526821, and additional thanks goes to
DOE/Lawrence Livermore National Laboratory for equipment and supplies.
The work at the University of Hawaii was supported in part by NASA under
a MIDDP grant NNX08AR10G.
NR 85
TC 29
Z9 29
U1 10
U2 56
PU SOC APPLIED SPECTROSCOPY
PI FREDERICK
PA 5320 SPECTRUM DRIVE SUITE C, FREDERICK, MD 21703 USA
SN 0003-7028
J9 APPL SPECTROSC
JI Appl. Spectrosc.
PD FEB
PY 2012
VL 66
IS 2
BP 137
EP 150
DI 10.1366/11-06535
PG 14
WC Instruments & Instrumentation; Spectroscopy
SC Instruments & Instrumentation; Spectroscopy
GA 886KZ
UT WOS:000299854600001
PM 22449277
ER
PT J
AU Oterkus, E
Madenci, E
Weckner, O
Silling, S
Bogert, P
Tessler, A
AF Oterkus, Erkan
Madenci, Erdogan
Weckner, Olaf
Silling, Stewart
Bogert, Philip
Tessler, Alexander
TI Combined finite element and peridynamic analyses for predicting failure
in a stiffened composite curved panel with a central slot
SO COMPOSITE STRUCTURES
LA English
DT Article
DE Progressive; Failure; Composites; Nonlocal; Peridynamic theory
AB This study presents an analysis approach based on a merger of the finite element method and the peridynamic theory. Its validity is established through qualitative and quantitative comparisons against the test results for a stiffened composite curved panel with a central slot under combined internal pressure and axial tension. The predicted initial and final failure loads, as well as the final failure modes, are in close agreement with the experimental observations. This approach demonstrates the capability of the PD approach to assess the durability of complex composite structures. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Oterkus, Erkan; Madenci, Erdogan] Univ Arizona, Dept Aerosp & Mech Engn, Tucson, AZ 85721 USA.
[Weckner, Olaf] Boeing Res & Technol, Seattle, WA 98124 USA.
[Silling, Stewart] Sandia Natl Labs, Multiscale Dynam Mat Modeling Dept, Albuquerque, NM 87185 USA.
[Bogert, Philip; Tessler, Alexander] NASA Langley Res Ctr, Struct Mech & Concepts Branch, Hampton, VA 23681 USA.
RP Madenci, E (reprint author), Univ Arizona, Dept Aerosp & Mech Engn, Tucson, AZ 85721 USA.
EM oterkus@email.arizona.edu; madenci@email.arizona.edu;
Olaf.Weckner@boeing.com; sasilli@sandia.gov; philip.b.bogert@nasa.gov;
alexander.tessler-1@nasa.gov
NR 10
TC 32
Z9 35
U1 3
U2 26
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0263-8223
J9 COMPOS STRUCT
JI Compos. Struct.
PD FEB
PY 2012
VL 94
IS 3
BP 839
EP 850
DI 10.1016/j.compstruct.2011.07.019
PG 12
WC Materials Science, Composites
SC Materials Science
GA 882WP
UT WOS:000299594900005
ER
PT J
AU Drossart, P
Limaye, SS
Smrekar, SA
AF Drossart, Pierre
Limaye, Sanjay S.
Smrekar, Suzanne A.
TI Introduction to advances in Venus science special issue
SO ICARUS
LA English
DT Editorial Material
C1 [Drossart, Pierre] Observ Paris, LESIA, F-92195 Meudon, France.
[Limaye, Sanjay S.] Univ Wisconsin, Ctr Space Sci & Engn, Madison, WI 53706 USA.
[Smrekar, Suzanne A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Drossart, P (reprint author), Observ Paris, LESIA, 5 Pl Jules Janssen, F-92195 Meudon, France.
OI Limaye, Sanjay/0000-0001-8659-2104
NR 0
TC 1
Z9 1
U1 0
U2 3
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 FEB
PY 2012
VL 217
IS 2
SI SI
BP 433
EP 433
DI 10.1016/j.icarus.2011.12.017
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 878FE
UT WOS:000299240100001
ER
PT J
AU Smrekar, SE
Sotin, C
AF Smrekar, Suzanne E.
Sotin, Christophe
TI Constraints on mantle plumes on Venus: Implications for volatile history
SO ICARUS
LA English
DT Article
DE Venus, Interior; Volcanism; Thermal histories; Planetary dynamics;
Geophysics
ID TEMPERATURE-DEPENDENT VISCOSITY; STAGNANT LID CONVECTION; PRANDTL NUMBER
FLUID; HIGH-RAYLEIGH-NUMBER; THERMAL-CONVECTION; TERRESTRIAL PLANETS;
WATER SOLUBILITY; TOPOGRAPHIC RISES; SPHERICAL-SHELL; EVOLUTION
AB The analysis of Venus' gravity field and topography suggests the presence of a small number of deep mantle plumes (similar to 9). This study predicts the number of plumes formed at the core-mantle boundary, their characteristics, and the production of partial melt from adiabatic decompression. Numerical simulations are performed using a 3D spherical code that includes large viscosity variations and internal heating. This study investigates the effect of several parameters including the core-mantle boundary temperature, the amount of internal heating, and the mantle viscosity. The smallest number of plumes is achieved when no internal heating is present. However, scaling Earth's radiogenic heating to Venus suggests a value of similar to 16 TW. Cases with internal heating produce more realistic lid thickness and partial melting, but produce either too many plumes or no plumes if a high mantle temperature precludes the formation of a hot thermal boundary layer. Mantle viscosity must be reduced to at least 10(20) Pa s in order to include significant internal heating and still produce hot plumes. In all cases that predict melting, melting occurs throughout the upper mantle. Only cases with high core temperature (>1700 K) produce dry melting. Over time the upper mantle may have lost significant volatiles. Depending on the water content of the lower mantle, deep plumes may contribute to present-day atmospheric water via volcanic outgassing. Assuming 50 ppm water in mantle, 10 plumes with a buoyancy flux of 500 kg/s continuously erupting for 4 myr will outgas an amount of water on the order of that in the lower atmosphere. A higher level of internal heating than achieved to date, as well as relatively low mantle viscosity, may be required to achieve simulations with similar to 10 plumes and a thinner lid. Alternatively, if the mantle is heating up due to the stagnant lid, the effect is equivalent to having lower rates of internal heating. A temperature increase of 110 K/byr is equivalent to -13 TW. This value along with the internal heating of 3 TW used in this study may represent the approximate heat budget of Venus' mantle. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Smrekar, Suzanne E.; Sotin, Christophe] CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA.
RP Smrekar, SE (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA.
EM ssmrekar@jpl.nasa.gov
FU JPL RTD; French space agency CNES; NASA
FX This work was performed at the Jet Propulsion Laboratory, California
Institute of Technology. CS acknowledges support by JPL R&TD and by the
French space agency CNES through support for his Interdisciplinary
Scientist role on Venus Express. S.S. acknowledges support from NASA's
Planetary Geology and Geophysics Program and NASA interdisciplinary
scientist funding for participation on Venus Express. This paper would
not have been possible without help from Gael Choblet with the OEDIPUS
code, and was significantly improved thanks to very constructive reviews
by Shijie Zhong and Anne Davaille. We thank Linda Elkins-Tanton for
discussions on melting and mantle water content. Computing was carried
out at both the NASA Ames and JPL supercomputer facilities. We thank the
undergraduate interns who have contributed to this work: Brian Anderson,
Ryen Lapham, Holly Taylor, Ian Bolliger, and Veronica Burnett. Special
thanks go to Timmary (Annie) Bonaccorso and Henry Tom, returning
students who persevered though numerous variations on plume counting
methods.
NR 70
TC 14
Z9 15
U1 1
U2 22
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 FEB
PY 2012
VL 217
IS 2
SI SI
BP 510
EP 523
DI 10.1016/j.icarus.2011.09.011
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 878FE
UT WOS:000299240100008
ER
PT J
AU Cottini, V
Ignatiev, NI
Piccioni, G
Drossart, P
Grassi, D
Markiewicz, WJ
AF Cottini, V.
Ignatiev, N. I.
Piccioni, G.
Drossart, P.
Grassi, D.
Markiewicz, W. J.
TI Water vapor near the cloud tops of Venus from Venus Express/VIRTIS
dayside data
SO ICARUS
LA English
DT Article
DE Venus; Atmosphere
ID MIDDLE ATMOSPHERE; SULFURIC-ACID; THERMODYNAMIC PROPERTIES;
MULTIPLE-SCATTERING; RADIATIVE-TRANSFER; MESOSPHERE; POLARIZATION;
VENERA-15; ABUNDANCE; SPECTRA
AB Observations of the dayside of Venus performed by the high spectral resolution channel (-H) of the Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) on board the ESA Venus Express mission have been used to measure the altitude of the cloud tops and the water vapor abundance around this level with a spatial resolution ranging from 100 to 10 km. CO2 and H2O bands between 2.48 and 2.60 mu m are analyzed to determine the cloud top altitude and water vapor abundance near this level. At low latitudes (+/- 40 degrees) mean water vapor abundance is equal to 3 +/- 1 ppm and the corresponding cloud top altitude at 2.5 mu m is equal to 69.5 +/- 2 km. Poleward from middle latitudes the cloud top altitude gradually decreases down to 64 km, while the average H2O abundance reaches its maximum of 5 PPm at 80 degrees of latitude with a large scatter from 1 to 15 ppm. The calculated mass percentage of the sulfuric acid solution in cloud droplets of mode 2 (similar to 1 mu m) particles is in the range 75-83%, being in even more narrow interval of 80-83% in low latitudes. No systematic correlation of the dark UV markings with the cloud top altitude or water vapor has been observed. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Cottini, V.] NASA GSFC, Greenbelt, MD 20771 USA.
[Cottini, V.; Ignatiev, N. I.; Piccioni, G.] Ist Astrofis Spaziale & Fis Cosm IASF INAF, Rome, Italy.
[Ignatiev, N. I.] Russian Acad Sci IKI RAN, Space Res Inst, Moscow, Russia.
[Ignatiev, N. I.; Markiewicz, W. J.] Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany.
[Drossart, P.] Observ Paris, LESIA, Meudon, France.
[Grassi, D.] Ist Fis Spazio Interplanetario IFSI INAF, Rome, Italy.
RP Cottini, V (reprint author), NASA GSFC, Code 693,Bldg 34,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM valeria.cottini@nasa.gov
OI Piccioni, Giuseppe/0000-0002-7893-6808; Grassi,
Davide/0000-0003-1653-3066
FU Agenzia Spaziale Italiana (ASI); Centre National d'Etudes Spatiales
(CNES); Russian Foundation of Basic Research [08-02-01383]
FX Venus Express is a mission of the European Space Agency. We thank the
Agenzia Spaziale Italiana (ASI) and the Centre National d'Etudes
Spatiales (CNES) for the support and funding of the VIRTIS experiment.
N.I. was supported by the Russian Foundation of Basic Research Grant
08-02-01383. We gratefully thank all members of the Venus Express
project and of the VIRTIS and VMC technical teams. We also thank D.V.
Titov, an anonymous referee, and C.A. Nixon for carefully reviewing this
manuscript and suggesting several improvements.
NR 53
TC 18
Z9 18
U1 0
U2 5
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 FEB
PY 2012
VL 217
IS 2
SI SI
BP 561
EP 569
DI 10.1016/j.icarus.2011.06.018
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 878FE
UT WOS:000299240100012
ER
PT J
AU Cotton, DV
Bailey, J
Crisp, D
Meadows, VS
AF Cotton, Daniel V.
Bailey, Jeremy
Crisp, D.
Meadows, V. S.
TI The distribution of carbon monoxide in the lower atmosphere of Venus
SO ICARUS
LA English
DT Article
DE Atmospheres, Chemistry; Atmospheres, Dynamics; Radiative transfer;
Spectroscopy; Venus, Atmosphere
ID DEEP ATMOSPHERE; NIGHTSIDE; CO; SPECTROSCOPY; TEMPERATURE; TROPOSPHERE;
MESOSPHERE; ABUNDANCE; SPECTRA; SURFACE
AB We have obtained spatially resolved near-infrared spectroscopy of the Venus nightside on 15 nights over three observing seasons. We use the depth of the CO absorption band at 2.3 mu m to map the two-dimensional distribution of CO across both hemispheres. Radiative transfer models are used to relate the measured CO band depth to the volume mixing ratio of CO. The results confirm previous investigations in showing a general trend of increased CO abundances at around 60 latitude north and south as compared with the equatorial regions. Observations taken over a few nights generally show very similar CO distributions, but significant changes are apparent over longer periods. In past studies it has been assumed that the CO latitudinal variation occurs near 35 km altitude, at which K-band sensitivity to CO is greatest. By modeling the detailed spectrum of the excess CO at high latitudes we show that it occurs at altitudes around 45 km, much higher than has previously been assumed, and that there cannot be significant contribution from levels of 36 km or lower. We suggest that this is most likely due to downwelling of CO-rich gas from the upper atmosphere at these latitudes, with the CO being removed by around 40 km through chemical processes such as the reaction with SO3. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Cotton, Daniel V.; Bailey, Jeremy] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
[Crisp, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Meadows, V. S.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Bailey, Jeremy; Crisp, D.; Meadows, V. S.] NASA Astrobiol Inst, Virtual Planetary Lab Lead Team, Washington, DC USA.
RP Bailey, J (reprint author), Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
EM j.bailey@unsw.edu.au
NR 44
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 FEB
PY 2012
VL 217
IS 2
SI SI
BP 570
EP 584
DI 10.1016/j.icarus.2011.05.020
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 878FE
UT WOS:000299240100013
ER
PT J
AU McGouldrick, K
Momary, TW
Baines, KH
Grinspoon, DH
AF McGouldrick, Kevin
Momary, Thomas W.
Baines, Kevin H.
Grinspoon, David H.
TI Quantification of middle and lower cloud variability and mesoscale
dynamics from Venus Express/VIRTIS observations at 1.74 mu m
SO ICARUS
LA English
DT Article
DE Venus, Atmosphere; Atmospheres, Dynamics; Atmospheres, Evolution;
Infrared observations; Meteorology
ID DARK SIDE; EVOLUTION; CLIMATE; VIRTIS; FEATURES; MISSION; MODEL; HOLES
AB We present an analysis of VIRTIS-M-IR observations of 1.74 mu m emission from the nightside of Venus. The 1.74 mu m window in the near infrared spectrum of Venus is an ideal proxy for investigating the evolution of middle and lower cloud deck opacity of Venus because it exhibits good signal to noise due to its brightness, good contrast between bright and dark regions, and few additional sources of extinction beside the clouds themselves. We have analyzed the data from the first 407 orbits (equivalent to 407 Earth days) of the Venus Express mission to determine the magnitude of variability in the 1.74 mu m radiance. We have also performed an analysis of the evolution of individual features over a span of roughly 5-6 h on two successive orbits of Venus Express. We find that the overall 1.74 mu m brightness of Venus has been increasing through the first 407 days of the mission, indicating a gradual diminishing of the cloud coverage and/or thickness, and that the lower latitudes exhibited more variability and more brightening than higher latitudes. We find that individual features evolve with a time scale of about 30 h, consistent with our previous analysis. Analysis of the evolution and motion of the clouds can be used to estimate the mesoscale dynamics within the clouds of Venus. We find that advection alone cannot explain the observed evolution of the features. The measured vorticity and divergence in the vicinity of the features are consistent with evolution under the influence of significant vertical motions likely driven by a radiative dynamical feedback. We measure a zonal wind speed of around 65 m/s, and a meridional wind speed around 2.5 m/s by tracking the motion of the central region of the features. But we also find that the measured wind speeds depend strongly on the points chosen for the wind speed analysis. (C) 2011 Elsevier Inc. All rights reserved.
C1 [McGouldrick, Kevin] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.
[Momary, Thomas W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Baines, Kevin H.] Univ Wisconsin, Dept Space Sci & Engn, Madison, WI 53706 USA.
[Grinspoon, David H.] Denver Museum Nat & Sci, Dept Space Sci, Denver, CO 80205 USA.
RP McGouldrick, K (reprint author), Univ Colorado, Lab Atmospher & Space Phys, 1234 Innovat Dr, Boulder, CO 80303 USA.
EM kevin.mcgouldrick@lasp.colorado.edu
FU National Aeronautics and Space Administration
FX We thank two anonymous reviewers for their helpful comments that have
led to the improvement of this paper, especially with regard to the
analysis of the mesoscale dynamics. We also thank Giuseppe Piccioni,
Pierre Drossart, and the VIRTIS team for their work in the preparation
of the data from the VIRTIS instrument. A portion of the work described
in this paper was carried out at the Jet Propulsion Laboratory,
Pasadena, CA, under contract with the National Aeronautics and Space
Administration. All authors were supported by NASA in support of ESA's
Venus Express mission.
NR 46
TC 4
Z9 4
U1 0
U2 1
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 FEB
PY 2012
VL 217
IS 2
SI SI
BP 615
EP 628
DI 10.1016/j.icarus.2011.07.009
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 878FE
UT WOS:000299240100017
ER
PT J
AU Titov, DV
Markiewicz, WJ
Ignatiev, NI
Song, L
Limaye, SS
Sanchez-Lavega, A
Hesemann, J
Almeida, M
Roatsch, T
Matz, KD
Scholten, F
Crisp, D
Esposito, LW
Hviid, SF
Jaumann, R
Keller, HU
Moissl, R
AF Titov, Dmitrij V.
Markiewicz, Wojciech J.
Ignatiev, Nikolay I.
Song, Li
Limaye, Sanjay S.
Sanchez-Lavega, Agustin
Hesemann, Jonas
Almeida, Miguel
Roatsch, Thomas
Matz, Klaus-Dieter
Scholten, Frank
Crisp, David
Esposito, Larry W.
Hviid, Stubbe F.
Jaumann, Ralf
Keller, Horst U.
Moissl, Richard
TI Morphology of the cloud tops as observed by the Venus Express Monitoring
Camera
SO ICARUS
LA English
DT Article
DE Venus; Cloud morphology; UV imaging; Venus Monitoring Camera
ID WINDS; ATMOSPHERE; MISSION; GALILEO; IMAGES; DYNAMICS; PATTERNS;
FEATURES; WAVES
AB Since the discovery of ultraviolet markings on Venus, their observations have been a powerful tool to study the morphology, motions and dynamical state at the cloud top level. Here we present the results of investigation of the cloud top morphology performed by the Venus Monitoring Camera (VMC) during more than 3 years of the Venus Express mission. The camera acquires images in four narrow-band filters centered at 365, 513, 965 and 1010 nm with spatial resolution from 50 km at apocentre to a few hundred of meters at pericentre. The VMC experiment provides a significant improvement in the Venus imaging as compared to the capabilities of the earlier missions. The camera discovered new cloud features like bright "lace clouds" and cloud columns at the low latitudes, dark polar oval and narrow circular and spiral "grooves" in the polar regions, different types of waves at the high latitudes. The VMC observations revealed detailed structure of the sub-solar region and the afternoon convective wake, the bow-shape features and convective cells, the mid-latitude transition region and the "polar cap". The polar orbit of the satellite enables for the first time nadir viewing of the Southern polar regions and an opportunity to zoom in on the planet. The experiment returned numerous images of the Venus limb and documented global and local brightening events. VMC provided almost continuous monitoring of the planet with high temporal resolution that allowed one to follow changes in the cloud morphology at various scales.
We present the in-flight performance of the instrument and focus in particular on the data from the ultraviolet channel, centered at the characteristic wavelength of the unknown UV absorber that yields the highest contrasts on the cloud top. Low latitudes are dominated by relatively dark clouds that have mottled and fragmented appearance clearly indicating convective activity in the sub-solar region. At similar to 50 degrees latitude this pattern gives way to streaky clouds suggesting that horizontal, almost laminar, flow prevails here. Poleward from about 60 degrees S the planet is covered by almost featureless bright polar hood sometimes crossed by dark narrow (similar to 300 km) spiral or circular structures. This global cloud pattern can change on time scales of a few days resulting in global and local "brightening events" when the bright haze can extend far into low latitudes and/or increase its brightness by 30%. Close-up snapshots reveal plenty of morphological details like convective cells, cloud streaks, cumulus-like columns, wave trains. Different kinds of small scale waves are frequently observed at the cloud top. The wave activity is mainly observed in the 65-80 degrees latitude band and is in particular concentrated in the region of Ishtar Terra that suggests their possible orographic origin. The VMC observations have important implications for the problems of the unknown UV absorber, microphysical processes, dynamics and radiative energy balance at the cloud tops. They are only briefly discussed in the paper, but each of them will be the subject of a dedicated study. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Titov, Dmitrij V.] ESA ESTEC, NL-2200 AG Noordwijk, Netherlands.
[Titov, Dmitrij V.; Markiewicz, Wojciech J.; Ignatiev, Nikolay I.; Song, Li; Hesemann, Jonas; Hviid, Stubbe F.; Keller, Horst U.; Moissl, Richard] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany.
[Ignatiev, Nikolay I.] Space Res Inst IKI, Moscow 117997, Russia.
[Limaye, Sanjay S.] Univ Wisconsin, Space Sci & Engn Ctr, Madison, WI 53706 USA.
[Sanchez-Lavega, Agustin] Univ Basque Country, ETSI, Bilbao 48013, Spain.
[Almeida, Miguel] SRE OS, ESA ESAC, Madrid 28691, Spain.
[Roatsch, Thomas; Matz, Klaus-Dieter; Scholten, Frank; Jaumann, Ralf] Inst Planetary Explorat DLR, D-12489 Berlin, Germany.
[Crisp, David] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Esposito, Larry W.] Univ Colorado, LASP, Boulder, CO 80309 USA.
RP Titov, DV (reprint author), ESA ESTEC, PB 299, NL-2200 AG Noordwijk, Netherlands.
EM Dmitri.Titov@esa.int
OI Limaye, Sanjay/0000-0001-8659-2104; Sanchez-Lavega,
Agustin/0000-0001-7355-1522
NR 49
TC 48
Z9 48
U1 0
U2 10
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD FEB
PY 2012
VL 217
IS 2
SI SI
BP 682
EP 701
DI 10.1016/j.icarus.2011.06.020
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 878FE
UT WOS:000299240100023
ER
PT J
AU Sonnabend, G
Krotz, P
Schmulling, F
Kostiuk, T
Goldstein, J
Sornig, M
Stupar, D
Livengood, T
Hewagama, T
Fast, K
Mahieux, A
AF Sonnabend, Guido
Kroetz, Peter
Schmuelling, Frank
Kostiuk, Theodor
Goldstein, Jeff
Sornig, Manuela
Stupar, Dusan
Livengood, Timothy
Hewagama, Tilak
Fast, Kelly
Mahieux, Arnaud
TI Thermospheric/mesospheric temperatures on Venus: Results from
ground-based high-resolution spectroscopy of CO2 in 1990/1991 and
comparison to results from 2009 and between other techniques
SO ICARUS
LA English
DT Article
DE Venus, Atmosphere; Infrared observations; Spectroscopy
ID MU-M WAVELENGTH; INFRARED HETERODYNE SPECTROSCOPY; NATURAL
LASER-EMISSION; UPPER-ATMOSPHERE; LINE OBSERVATIONS; THERMAL STRUCTURE;
WIND VELOCITIES; MARS; THERMOSPHERE; SPECTROMETER
AB We report temperatures in Venus' upper mesosphere/lower thermosphere, deduced from reanalyzing very high resolution infrared spectroscopy of CO2 emission lines acquired in 1990 and 1991. Kinetic temperatures at similar to 110 km altitude (0.15 Pa) are derived from the Doppler width of fully-resolved single line profiles measured near 10.4 mu m wavelength using the NASA GSFC Infrared Heterodyne Spectrometer (IRHS) at the NASA IRTF on Mauna Kea, HI, close to Venus inferior conjunction and two Venus solstices. Measured temperatures range from similar to 200 to 240 K with uncertainty typically less than 10 K. Temperatures retrieved from similar measurement in 2009 using the Cologne Tuneable Heterodyne Infrared Spectrometer (THIS) at the NOAO McMath Telescope at Kitt Peak, AZ are 10-20 K lower. Temperatures retrieved more recently from the SOIR instrument on Venus EXpress are consistent with these results when the geometry of observation is accounted for. It is difficult to compare ground-based sub-mm retrievals extrapolated to 110 km due to their much larger field of view, which includes the night side regions not accessible to infrared heterodyne observations. Temperature variability appears to be high on day-to-day as well as longer timescales. Observed short term and long term variability may be attributed to atmospheric dynamics, diurnal variability and changes over solar activity and seasons. The Venus International Reference Atmosphere (VIRA) model predicts cooler temperatures at the sampled altitudes in the lower thermosphere/upper mesosphere and is not consistent with these measurements. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Sonnabend, Guido; Kroetz, Peter; Stupar, Dusan] Univ Cologne, Inst Phys, D-50937 Cologne, Germany.
[Schmuelling, Frank; Kostiuk, Theodor; Fast, Kelly] NASA GSFC, Greenbelt, MD 20771 USA.
[Schmuelling, Frank] DLR, D-53227 Bonn, Germany.
[Goldstein, Jeff; Livengood, Timothy] NCESSE, Capital Hts, MD 20791 USA.
[Hewagama, Tilak] Univ Maryland, College Pk, MD 20742 USA.
[Sornig, Manuela] Rhein Inst Umweltforsch, D-50931 Cologne, Germany.
[Mahieux, Arnaud] Belgian Inst Space Aeron, B-1180 Brussels, Belgium.
RP Sonnabend, G (reprint author), Univ Cologne, Inst Phys, Zulpicher Str 77, D-50937 Cologne, Germany.
EM samstag@ph1.uni-koeln.de
RI Hewagama, T/C-8488-2012; Livengood, Timothy/C-8512-2012; Kostiuk,
Theodor/A-3077-2014
FU National Aeronautics and Space Administration; Deutsche
Forschungsgemeinschaft (DFG) [SO879/1-2]; Belgian Federal Science Policy
Office; European Space Agency (ESA, PRODEX) [C90268, 90113, 17645]
FX Research at the NASA Infrared Telescope Facility was supported by the
National Aeronautics and Space Administration Planetary Astronomy
Program. This work was supported by the Deutsche Forschungsgemeinschaft
(DFG) through Grant SO879/1-2. We would like to thank the SOIR team,
especially Jean-Loup Bertaux, PI of the instrument, and Ann Carine
Vandaele, group leader at the Belgian Institute for Space Aeronomy,
Brussels. The research program was supported by the Belgian Federal
Science Policy Office and the European Space Agency (ESA, PRODEX
program, contracts C90268, 90113, and 17645).
NR 35
TC 11
Z9 11
U1 2
U2 6
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 FEB
PY 2012
VL 217
IS 2
SI SI
BP 856
EP 862
DI 10.1016/j.icarus.2011.07.015
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 878FE
UT WOS:000299240100038
ER
PT J
AU Sornig, M
Livengood, TA
Sonnabend, G
Stupar, D
Kroetz, P
AF Sornig, M.
Livengood, T. A.
Sonnabend, G.
Stupar, D.
Kroetz, P.
TI Direct wind measurements from November 2007 in Venus' upper atmosphere
using ground-based heterodyne spectroscopy of CO2 at 10 mu m wavelength
SO ICARUS
LA English
DT Article
DE Venus; Atmospheres, Dynamics; Infrared observations
ID INFRARED OBSERVATIONS; GLOBAL CIRCULATION; MARTIAN ATMOSPHERE; THERMAL
STRUCTURE; LINE OBSERVATIONS; UPPER MESOSPHERE; EMISSION-LINES; NATURAL
LASER; EXPRESS; MARS
AB Between November 23 and 28, 2007, the Cologne Tuneable Heterodyne Infrared Spectrometer THIS was installed at the McMath-Pierce Solar Telescope (Kitt Peak, Arizona, USA) to determine zonal wind velocities and to estimate the subsolar-to-antisolar flow. We investigate dynamics in the upper atmosphere of Venus by measuring the Doppler shift of fully-resolved non-LTE CO2 emission lines at 959.3917 cm(-1) (10.423 mu m), which probe a narrow altitude region in Venus' atmosphere around 110 +/- 10 km (similar to 1 mu bar). The results show no significant zonal wind velocity at the equator. An increase with latitude up to 43 +/- 13 m/s at a latitude of 33 degrees N was observed. This confirms the deduction of a minor influence of Venus superrotation at an altitude of 110 km from previous measurements in May 2007 (Sornig et al., 2008). The specific observing geometry enables estimating the maximum cross terminator velocity of the subsolar-to-antisolar flow at 72 +/- 47 m/s. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Sornig, M.] Univ Cologne, Rhein Inst Umweltforsch, Abt Planetenforsch, D-50931 Cologne, Germany.
[Livengood, T. A.] NASA GSFC, Greenbelt, MD 20771 USA.
[Livengood, T. A.] NCESSE, Capital Hts, MD 20791 USA.
[Sonnabend, G.; Stupar, D.; Kroetz, P.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany.
RP Sornig, M (reprint author), Univ Cologne, Rhein Inst Umweltforsch, Abt Planetenforsch, Aachener Str 209, D-50931 Cologne, Germany.
EM sornig@ph1.uni-koeln.de; timothy.a.livengood@nasa.gov;
samstag@ph1.uni-koeln.de; stupar@ph1.uni-koeln.de;
kroetz@ph1.uni-koeln.de
RI Livengood, Timothy/C-8512-2012
FU Europlanet; Deutsche Forschungsgemeinschaft (DFG) [SO879/1-1]
FX This work was supported by Europlanet and the Deutsche
Forschungsgemeinschaft (DFG) special Grant SO879/1-1.
NR 49
TC 8
Z9 8
U1 2
U2 8
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD FEB
PY 2012
VL 217
IS 2
SI SI
BP 863
EP 874
DI 10.1016/j.icarus.2011.03.019
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 878FE
UT WOS:000299240100039
ER
PT J
AU Raney, RK
Freeman, A
Jordan, RL
AF Raney, Russell Keith
Freeman, Anthony
Jordan, Rolando L.
TI Improved Range Ambiguity Performance in Quad-Pol SAR
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Ambiguities; circular polarization; hybrid polarity; quadrature
polarimetric (quad-pol); synthetic aperture radar (SAR)
ID CALIBRATION; ANTENNA
AB Conventional quadrature-polarimetric (quad-pol) synthetic aperture radar (SAR) systems operating from space are severely constrained by their limited range of useful incident angles and their reduced swath widths particularly at larger incidence. These limitations are due primarily to relatively severe range ambiguities in the cross-polarized measurement channels. The conventional approach for quad-pol SAR systems uses linear polarizations on both transmit and receive. Range ambiguities can be markedly reduced by adopting hybrid-polarimetric architecture. In this approach, the radar transmits circularly polarized waves but receives on orthogonal linear polarizations. The sense of the circular polarization-left or right-is reversed on alternate transmissions. Hybrid-polarimetric quad-pol architecture leads to hardware that is more readily calibrated because neither receive channel is cross polarized with respect to the transmitted polarization; hence, their mean signal levels are the same. The data provided by a hybrid-polarimetric quad-pol SAR may be transformed into the conventional linearly polarized scattering matrix, thus preserving compatibility with the rich heritage of analysis tools developed for such radars.
C1 [Raney, Russell Keith] Johns Hopkins Univ, Appl Phys Lab, Baltimore, MD 20723 USA.
[Freeman, Anthony; Jordan, Rolando L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Raney, RK (reprint author), Johns Hopkins Univ, Appl Phys Lab, Baltimore, MD 20723 USA.
EM keith.raney@jhuapl.edu; Anthony.Freeman@jpl.nasa.gov;
Rolando.jordan@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX This work was supported in part by the National Aeronautics and Space
Administration.
NR 17
TC 10
Z9 13
U1 0
U2 5
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 FEB
PY 2012
VL 50
IS 2
BP 349
EP 356
DI 10.1109/TGRS.2011.2121075
PG 8
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 880UJ
UT WOS:000299432900003
ER
PT J
AU Kleidman, RG
Smirnov, A
Levy, RC
Mattoo, S
Tanre, D
AF Kleidman, Richard G.
Smirnov, Alexander
Levy, Robert C.
Mattoo, Shana
Tanre, Didier
TI Evaluation and Wind Speed Dependence of MODIS Aerosol Retrievals Over
Open Ocean
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Aerosols; remote sensing
ID OPTICAL-THICKNESS RETRIEVALS; TROPOSPHERIC AEROSOLS; SIZE DISTRIBUTION;
SUN PHOTOMETER; VALIDATION; SATELLITE; PRODUCT; DEPTH; ATLANTIC; SPACE
AB The Maritime Aerosol Network (MAN) data set provides high-quality ground truth to validate the Moderate Resolution Imaging Spectroradiometer (MODIS) aerosol product over open ocean. Prior validation of the ocean aerosol product has been limited to coastal and island sites. Comparing MODIS Collection 5 ocean aerosol retrieval products with collocated MAN measurements from ships shows that MODIS is meeting the prelaunch uncertainty estimates for aerosol optical depth (AOD) with 64% and 67% of retrievals at 550 nm and 74% and 78% of retrievals at 870 nm, falling within expected uncertainty for Terra and Aqua, respectively. Angstrom exponent comparisons show a high correlation between MODIS retrievals and shipboard measurements (R = 0.85 for Terra and 0.83 for Aqua), although the MODIS aerosol algorithm tends to underestimate particle size for large particles and overestimate size for small particles, as seen in earlier collections. Prior analysis noted an offset between Terra and Aqua ocean AODs, without concluding which sensor was more accurate. The simple linear regression reported here is consistent with other anecdotal evidence that Aqua agreement with the Aerosol Robotic Network is marginally better. However, we cannot claim based on the current study that the better Aqua comparison is statistically significant. A systematic increase of error as a function of wind speed is noted in both Terra and Aqua retrievals. This wind speed dependence enters the retrieval when winds deviate from the 6-m/s value assumed in the rough ocean surface and white cap parameterizations. Wind speed dependence in the results can be mitigated by using auxiliary National Centers for Environmental Prediction wind speed information in the retrieval process.
C1 [Kleidman, Richard G.; Levy, Robert C.; Mattoo, Shana] Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
[Kleidman, Richard G.; Levy, Robert C.; Mattoo, Shana] NASA, Atmospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Smirnov, Alexander] Sigma Space Corp, Lanham, MD 20706 USA.
[Smirnov, Alexander] NASA, Biospher Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Tanre, Didier] Univ Lille, Opt Atmospher Lab, F-59655 Villeneuve Dascq, France.
RP Kleidman, RG (reprint author), Sci Syst & Applicat Inc, Lanham, MD 20706 USA.
EM Richard.Kleidman@nasa.gov; Alexander.Smirnov-1@nasa.gov;
robert.c.levy@nasa.gov; Shana.Mattoo@nasa.gov;
didier.tanre@univ-lille1.fr
RI Smirnov, Alexander/C-2121-2009; Levy, Robert/M-7764-2013
OI Smirnov, Alexander/0000-0002-8208-1304; Levy, Robert/0000-0002-8933-5303
FU National Aeronautics and Space Administration [06-EOS/06-1037]
FX This work was supported by the National Aeronautics and Space
Administration Climate and Radiation Research and Analysis Program
managed by H. Maring under Grant 06-EOS/06-1037.
NR 47
TC 14
Z9 15
U1 0
U2 12
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 0196-2892
EI 1558-0644
J9 IEEE T GEOSCI REMOTE
JI IEEE Trans. Geosci. Remote Sensing
PD FEB
PY 2012
VL 50
IS 2
BP 429
EP 435
DI 10.1109/TGRS.2011.2162073
PG 7
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 880UJ
UT WOS:000299432900011
ER
PT J
AU Colliander, A
McDonald, K
Zimmermann, R
Schroeder, R
Kimball, JS
Njoku, EG
AF Colliander, Andreas
McDonald, Kyle
Zimmermann, Reiner
Schroeder, Ronny
Kimball, John S.
Njoku, Eni G.
TI Application of QuikSCAT Backscatter to SMAP Validation Planning:
Freeze/Thaw State Over ALECTRA Sites in Alaska From 2000 to 2007
SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING
LA English
DT Article
DE Alaska Ecological Transect (ALECTRA); freeze/thaw state; Quick
Scatterometer (QuikSCAT); Soil Moisture Active Passive (SMAP)
ID NASA SCATTEROMETER NSCAT; LANDSCAPE; SEASONS; BOREAL; CYCLES; FROZEN;
SOIL; SAR
AB The mapping of the predominant freeze/thaw state of the landscape is one of the main objectives of the National Aeronautics and Space Administration's proposed Soil Moisture Active Passive (SMAP) mission. This study applies Alaska Ecological Transect (ALECTRA) biophysical network temperature measurements and satellite radar scatterometer data from the Quick Scatterometer (QuikSCAT) to evaluate some of the validation issues regarding the planned SMAP freeze/thaw measurements. Although the QuikSCAT data are acquired at Ku-band frequency, rather than at the L-band frequency of the proposed SMAP instrument, QuikSCAT data do provide a high temporal fidelity over the ALECTRA sites, similar to SMAP. The results of this study show that multiple temperature measurements representative of individual landscape components (soil, snow cover, vegetation, and atmosphere) covering different types of terrain within the satellite field of view are important for understanding the freeze/thaw process and the aggregate radar backscatter response to that process. The backscatter temporal dynamics and relative contribution of the freeze/thaw state of these landscape elements to radar signal vary with land cover, seasonal weather, and climate conditions.
C1 [Colliander, Andreas; McDonald, Kyle; Schroeder, Ronny; Njoku, Eni G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[McDonald, Kyle] CUNY City Coll, Dept Earth & Atmospher Sci, New York, NY 10031 USA.
[Zimmermann, Reiner] Univ Hohenheim, Inst Bot & Bot Gardens, D-70593 Stuttgart, Germany.
[Schroeder, Ronny] CUNY City Coll, Cooperat Remote Sensing Sci & Technol Ctr CREST I, New York, NY 10031 USA.
[Kimball, John S.] Univ Montana, Coll Forestry & Conservat, Missoula, MT 59812 USA.
RP Colliander, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM andreas.colliander@jpl.nasa.gov; kmcdonald2@ccny.cuny.edu;
rzimmerm@uni-hohenheim.de; ronny.schroeder@jpl.nasa.gov;
johnk@ntsg.umt.edu; eni.g.njoku@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX The authors would like to thank T. Linke for his assistance in
processing the Alaska Ecological Transect data. The work described in
this paper was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, Pasadena, under a contract with the National
Aeronautics and Space Administration.
NR 17
TC 10
Z9 10
U1 0
U2 13
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 FEB
PY 2012
VL 50
IS 2
BP 461
EP 468
DI 10.1109/TGRS.2011.2174368
PG 8
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 880UJ
UT WOS:000299432900014
ER
PT J
AU Roberts, JB
Robertson, FR
Clayson, CA
Bosilovich, MG
AF Roberts, J. Brent
Robertson, Franklin R.
Clayson, Carol A.
Bosilovich, Michael G.
TI Characterization of Turbulent Latent and Sensible Heat Flux Exchange
between the Atmosphere and Ocean in MERRA
SO JOURNAL OF CLIMATE
LA English
DT Article
ID AIR-SEA FLUXES; BULK AERODYNAMIC ALGORITHMS; WIND STRESS; SURFACE
METEOROLOGY; RESPONSE EXPERIMENT; EQUATORIAL PACIFIC; REANALYSIS
PROJECT; GLOBAL ENERGY; NCEP-NCAR; ATLANTIC
AB Turbulent fluxes of heat and moisture across the atmosphere ocean interface are fundamental components of the earth's energy and water balance. Characterizing both the spatiotemporal variability and the fidelity of these exchanges of heat and moisture is critical to understanding the global water and energy cycle variations, quantifying atmosphere ocean feedbacks, and improving model predictability. This study examines the veracity of the recently completed NASA Modern-Era Retrospective Analysis for Research and Applications (MERRA) product in terms of its turbulent surface fluxes. This assessment employs a large dataset of directly measured turbulent fluxes as well as other turbulent surface flux datasets. The spatial and temporal variability of the surface fluxes are examined in terms of their annual-mean climatologies, their seasonal covariability of near-surface bulk parameters, and their representation of extremes. The impact of data assimilation on the near-surface parameters is assessed through evaluation of the incremental analysis update tendencies. It is found that MERRA turbulent surface fluxes are relatively accurate for typical conditions but have systematically weak vertical gradients in moisture and temperature and a weaker covariability between the near-surface gradients and wind speed than found in observations. This results in an underestimate of the surface latent and sensible heat fluxes over the western boundary current and storm-track regions. The assimilation of observations generally acts to bring MERRA closer to observational products by increasing moisture and temperature near the surface and decreasing the near-surface wind speeds.
C1 [Roberts, J. Brent; Robertson, Franklin R.] NASA, George C Marshall Space Flight Ctr, Earth Sci Off, Huntsville, AL 35805 USA.
[Clayson, Carol A.] Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA.
[Clayson, Carol A.] Florida State Univ, Inst Geophys Fluid Dynam, Tallahassee, FL 32306 USA.
[Bosilovich, Michael G.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
RP Roberts, JB (reprint author), NASA, George C Marshall Space Flight Ctr, Earth Sci Off, 320 Sparkman Dr, Huntsville, AL 35805 USA.
EM jason.b.roberts@nasa.gov
RI Bosilovich, Michael/F-8175-2012
NR 56
TC 9
Z9 10
U1 1
U2 11
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0894-8755
EI 1520-0442
J9 J CLIMATE
JI J. Clim.
PD FEB 1
PY 2012
VL 25
IS 3
BP 821
EP 838
DI 10.1175/JCLI-D-11-00029.1
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 885SG
UT WOS:000299800500001
ER
PT J
AU Wiese, DN
Nerem, RS
Lemoine, FG
AF Wiese, D. N.
Nerem, R. S.
Lemoine, F. G.
TI Design considerations for a dedicated gravity recovery satellite mission
consisting of two pairs of satellites
SO JOURNAL OF GEODESY
LA English
DT Article
DE Time variable gravity; GRACE; Temporal aliasing errors; Constellations;
Satellite geodesy
ID LOCALIZED SPECTRAL-ANALYSIS; GRACE MEASUREMENTS; CLIMATE EXPERIMENT;
FIELD MODELS; GLOBAL OCEAN; VARIABILITY; ASSIMILATION; SYSTEM; SPHERE;
TIDES
AB Future satellite missions dedicated to measuring time-variable gravity will need to address the concern of temporal aliasing errors; i.e., errors due to high-frequency mass variations. These errors have been shown to be a limiting error source for future missions with improved sensors. One method of reducing them is to fly multiple satellite pairs, thus increasing the sampling frequency of the mission. While one could imagine a system architecture consisting of dozens of satellite pairs, this paper explores the more economically feasible option of optimizing the orbits of two pairs of satellites. While the search space for this problem is infinite by nature, steps have been made to reduce it via proper assumptions regarding some parameters and a large number of numerical simulations exploring appropriate ranges for other parameters. A search space originally consisting of 15 variables is reduced to two variables with the utmost impact on mission performance: the repeat period of both pairs of satellites (shown to be near-optimal when they are equal to each other), as well as the inclination of one of the satellite pairs (the other pair is assumed to be in a polar orbit). To arrive at this conclusion, we assume circular orbits, repeat groundtracks for both pairs of satellites, a 100-km inter-satellite separation distance, and a minimum allowable operational satellite altitude of 290 km based on a projected 10-year mission lifetime. Given the scientific objectives of determining time-variable hydrology, ice mass variations, and ocean bottom pressure signals with higher spatial resolution, we find that an optimal architecture consists of a polar pair of satellites coupled with a pair inclined at 72A degrees, both in 13-day repeating orbits. This architecture provides a 67% reduction in error over one pair of satellites, in addition to reducing the longitudinal striping to such a level that minimal post-processing is required, permitting a substantial increase in the spatial resolution of the gravity field products. It should be emphasized that given different sets of scientific objectives for the mission, or a different minimum allowable satellite altitude, different architectures might be selected.
C1 [Wiese, D. N.; Nerem, R. S.] Univ Colorado, Colorado Ctr Astrodynam Res, Boulder, CO 80309 USA.
[Lemoine, F. G.] NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA.
RP Wiese, DN (reprint author), Univ Colorado, Colorado Ctr Astrodynam Res, 431 UCB, Boulder, CO 80309 USA.
EM wiese@colorado.edu; nerem@colorado.edu; frank.g.lemoine@nasa.gov
RI Lemoine, Frank/D-1215-2013
FU National Science Foundation; National Defense Science and Engineering
Graduate Fellowship Program; NASA GRACE Science Team investigation
[NNX08AH63G]
FX This research was funded by the National Science Foundation Graduate
Fellowship Program, the National Defense Science and Engineering
Graduate Fellowship Program, and the NASA GRACE Science Team
investigation (NNX08AH63G). The authors would like to thank NASA Goddard
Space Flight Center for providing GEODYN and SOLVEto perform the
numerical simulations, along with the NCEP model. We acknowledge
Jean-Paul Boy (EOST/University of Strasbourg, France) for providing the
ECMWF-derived and MOG-2D-derived datasets in this study to GSFC.
Additionally, we thank ESA and the Institute of Astronomical and
Physical Geodesy (IAPG) at the Technical University of Munich for
providing the ice model used in the simulations.
NR 44
TC 20
Z9 22
U1 1
U2 11
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0949-7714
EI 1432-1394
J9 J GEODESY
JI J. Geodesy
PD FEB
PY 2012
VL 86
IS 2
BP 81
EP 98
DI 10.1007/s00190-011-0493-8
PG 18
WC Geochemistry & Geophysics; Remote Sensing
SC Geochemistry & Geophysics; Remote Sensing
GA 881XH
UT WOS:000299524800001
ER
PT J
AU Davis, CJ
Davies, JA
St Cyr, OC
Campbell-Brown, M
Skelt, A
Kaiser, M
Meyer-Vernet, N
Crothers, S
Lintott, C
Smith, A
Bamford, S
Baeten, EML
AF Davis, C. J.
Davies, J. A.
St Cyr, O. C.
Campbell-Brown, M.
Skelt, A.
Kaiser, M.
Meyer-Vernet, Nicole
Crothers, S.
Lintott, C.
Smith, A.
Bamford, S.
Baeten, E. M. L.
TI The distribution of interplanetary dust between 0.96 and 1.04 au as
inferred from impacts on the STEREO spacecraft observed by the
heliospheric imagers
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE Sun: heliosphere; solar-terrestrial relations; meteorites, meteors,
meteoroids; zodiacal dust
ID METEOR ORBIT RADAR; RADIO; RADIANTS; S/WAVES; MISSION; SECCHI
AB The distribution of dust in the ecliptic plane between 0.96 and 1.04 au has been inferred from impacts on the two Solar Terrestrial Relations Observatory (STEREO) spacecraft through observation of secondary particle trails and unexpected off-points in the heliospheric imager (HI) cameras. This study made use of analysis carried out by members of a distributed web-based citizen science project Solar Stormwatch. A comparison between observations of the brightest particle trails and a survey of fainter trails shows consistent distributions. While there is no obvious correlation between this distribution and the occurrence of individual meteor streams at Earth, there are some broad longitudinal features in these distributions that are also observed in sources of the sporadic meteor population. The different position of the HI instrument on the two STEREO spacecraft leads to each sampling different populations of dust particles. The asymmetry in the number of trails seen by each spacecraft and the fact that there are many more unexpected off-points in the HI-B than in HI-A indicates that the majority of impacts are coming from the apex direction. For impacts causing off-points in the HI-B camera, these dust particles are estimated to have masses in excess of 10-17 kg with radii exceeding 0.1 mu m.
For off-points observed in the HI-A images, which can only have been caused by particles travelling from the anti-apex direction, the distribution is consistent with that of secondary 'storm' trails observed by HI-B, providing evidence that these trails also result from impacts with primary particles from an anti-apex source. Investigating the mass distribution for the off-points of both HI-A and HI-B, it is apparent that the differential mass index of particles from the apex direction (causing off-points in HI-B) is consistently above 2. This indicates that the majority of the mass is within the smaller particles of this population. In contrast, the differential mass index of particles from the anti-apex direction (causing off-points in HI-A) is consistently below 2, indicating that the majority of the mass is to be found in larger particles of this distribution.
C1 [Davis, C. J.; Davies, J. A.; Skelt, A.; Crothers, S.] Rutherford Appleton Lab, RAL Space, Chilton OX11 0DQ, Oxon, England.
[Davis, C. J.] Univ Reading, Dept Meteorol, Reading RG6 7BE, Berks, England.
[St Cyr, O. C.; Kaiser, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Campbell-Brown, M.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 5B8, Canada.
[Skelt, A.] Faringdon Community Coll, Farringdon SN7 7CB, Oxon, England.
[Meyer-Vernet, Nicole] Observ Paris, F-92195 Meudon, France.
[Lintott, C.; Smith, A.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
[Lintott, C.; Smith, A.] Adler Planetarium, Chicago, IL 60605 USA.
[Bamford, S.] Univ Nottingham, Ctr Astron & Particle Theory, Nottingham NG7 2RD, England.
[Baeten, E. M. L.] Zooniverse, Dept Astrophys, Oxford OX1 3RH, England.
RP Davis, CJ (reprint author), Rutherford Appleton Lab, RAL Space, Chilton OX11 0DQ, Oxon, England.
EM chris.davis@stfc.ac.uk
RI Scott, Christopher/H-8664-2012; Bamford, Steven/E-8702-2010;
OI Scott, Christopher/0000-0001-6411-5649; Bamford,
Steven/0000-0001-7821-7195; Smith, Arfon/0000-0002-3957-2474
FU UK Space Agency; Leverhulme Trust
FX The UK STEREO group is supported by funding from the UK Space Agency.
Solar Stormwatch is a collaborative project between the Zooniverse team,
the Royal Observatory Greenwich and the Science and Technology
Facilities Council. The Zooniverse is supported by the Leverhulme Trust.
The STEREO heliospheric imagers are supported by the UK Space Agency.
STEREO HI data are made available via the UK Solar System Data Centre
(www.ukssdc.ac.uk).
NR 23
TC 9
Z9 9
U1 0
U2 13
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD FEB
PY 2012
VL 420
IS 2
BP 1355
EP 1366
DI 10.1111/j.1365-2966.2011.20125.x
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 880OU
UT WOS:000299417600033
ER
PT J
AU Mandelbaum, R
Hirata, CM
Leauthaud, A
Massey, RJ
Rhodes, J
AF Mandelbaum, Rachel
Hirata, Christopher M.
Leauthaud, Alexie
Massey, Richard J.
Rhodes, Jason
TI Precision simulation of ground-based lensing data using observations
from space
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing: weak; methods: data analysis; techniques: image
processing; galaxies: structure
ID DIGITAL SKY SURVEY; SPECTROSCOPIC TARGET SELECTION; IMAGE-ANALYSIS
COMPETITION; TELESCOPE ADVANCED CAMERA; GALAXY CLUSTERS; DATA RELEASE;
GREAT08 CHALLENGE; ELLIPTIC GALAXIES; SHAPE MEASUREMENT; COSMIC SHEAR
AB Current and upcoming wide-field, ground-based, broad-band imaging surveys promise to address a wide range of outstanding problems in galaxy formation and cosmology. Several such uses of ground-based data, especially weak gravitational lensing, require highly precise measurements of galaxy image statistics with careful correction for the effects of the point spread function (PSF). In this paper, we introduce the shera (SHEar Reconvolution Analysis) software to simulate ground-based imaging data with realistic galaxy morphologies and observing conditions, starting from space-based data (from the Cosmological Evolution Survey, COSMOS) and accounting for the effects of the space-based PSF. This code simulates ground-based data, optionally with a weak lensing shear applied, in a model-independent way using a general Fourier space formalism. The utility of this pipeline is that it allows for a precise, realistic assessment of systematic errors due to the method of data processing, for example in extracting weak lensing galaxy shape measurements or galaxy radial profiles, given user-supplied observational conditions and real galaxy morphologies. Moreover, the simulations allow for the empirical test of error estimates and determination of parameter degeneracies, via generation of many noise maps. The public release of this software, along with a large sample of cleaned COSMOS galaxy images (corrected for charge transfer inefficiency), should enable upcoming ground-based imaging surveys to achieve their potential in the areas of precision weak lensing analysis, galaxy profile measurement and other applications involving detailed image analysis.
C1 [Mandelbaum, Rachel] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Hirata, Christopher M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Leauthaud, Alexie] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Massey, Richard J.] Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Rhodes, Jason] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mandelbaum, R (reprint author), Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA.
EM rmandelb@astro.princeton.edu
RI Mandelbaum, Rachel/N-8955-2014
OI Mandelbaum, Rachel/0000-0003-2271-1527
FU US National Science Foundation [AST-0807337]; US Department of Energy
[DE-FG03-02-ER40701]; Alfred P. Sloan Foundation; David and Lucile
Packard Foundation; LBNL; Berkeley Center for Cosmological Physics; STFC
[PP/E006450/1]; ERC [MIRG-CT-208994]; NASA
FX We thank the referee for many constructive comments about the
organization and content of this paper. The authors would also like to
thank Jim Gunn, Robert Lupton, Dustin Lang, David Hogg, Michael Blanton,
Barney Rowe, Peter Capak, Chiaki Hikage, Uros Seljak and Gary Bernstein
for useful conversations about this project, and Eric Huff both for
discussing it and giving the software a name. CMH is supported by the US
National Science Foundation (AST-0807337), the US Department of Energy
(DE-FG03-02-ER40701), the Alfred P. Sloan Foundation, and the David and
Lucile Packard Foundation. AL acknowledges support from the Chamberlain
Fellowship at LBNL and from the Berkeley Center for Cosmological
Physics. RJM is supported by STFC Advanced Fellowship #PP/E006450/1 and
ERC grant MIRG-CT-208994. This work was done in part at JPL, run under a
contract for NASA by Caltech.
NR 83
TC 38
Z9 38
U1 0
U2 1
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD FEB
PY 2012
VL 420
IS 2
BP 1518
EP 1540
DI 10.1111/j.1365-2966.2011.20138.x
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 880OU
UT WOS:000299417600046
ER
PT J
AU Sundqvist, JO
Owocki, SP
Cohen, DH
Leutenegger, MA
Townsend, RHD
AF Sundqvist, Jon O.
Owocki, Stanley P.
Cohen, David H.
Leutenegger, Maurice A.
Townsend, Richard H. D.
TI A generalized porosity formalism for isotropic and anisotropic effective
opacity and its effects on X-ray line attenuation in clumped O star
winds
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE line: profiles; radiative transfer; stars: early-type; stars: mass-loss;
stars: winds, outflows; X-rays: stars
ID DRIVEN STELLAR WINDS; MASS-LOSS RATE; ZETA-PUPPIS; EMISSION; PROFILES;
SPECTROSCOPY; INSTABILITY; SIMULATIONS; CONSTRAINTS; ABSORPTION
AB We present a generalized formalism for treating the porosity-associated reduction in continuum opacity that occurs when individual clumps in a stochastic medium become optically thick. As in previous work, we concentrate on developing bridging laws between the limits of optically thin and thick clumps. We consider geometries resulting in either isotropic or anisotropic effective opacity, and, in addition to an idealized model in which all clumps have the same local overdensity and scale, we also treat an ensemble of clumps with optical depths set by Markovian statistics. This formalism is then applied to the specific case of boundfree absorption of X-rays in hot star winds, a process not directly affected by clumping in the optically thin limit. We find that the Markov model gives surprisingly similar results to those found previously for the single-clump model, suggesting that porous opacity is not very sensitive to details of the assumed clump distribution function. Further, an anisotropic effective opacity favours escape of X-rays emitted in the tangential direction (the venetian blind effect), resulting in a bump of higher flux close to line centre as compared to profiles computed from isotropic porosity models. We demonstrate how this characteristic line shape may be used to diagnose the clump geometry, and we confirm previous results that for optically thick clumping to significantly influence X-ray line profiles, very large porosity lengths, defined as the mean free path between clumps, are required. Moreover, we present the first X-ray line profiles computed directly from line-driven instability simulations using a 3D patch method, and find that porosity effects from such models also are very small. This further supports the view that porosity has, at most, a marginal effect on X-ray line diagnostics in O stars, and therefore that these diagnostics do indeed provide a good clumping insensitive method for deriving O star mass-loss rates.
C1 [Sundqvist, Jon O.; Owocki, Stanley P.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Cohen, David H.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA.
[Leutenegger, Maurice A.] NASA, GSFC, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Leutenegger, Maurice A.] NASA, GSFC, CRESST, Greenbelt, MD 20771 USA.
[Leutenegger, Maurice A.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Townsend, Richard H. D.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
RP Sundqvist, JO (reprint author), Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
EM jon@bartol.udel.edu
FU NASA ATP [NNX11AC40G]; NASA ADAP [NNX11AD26G]
FX This work was supported in part by NASA ATP grant NNX11AC40G. DHC
acknowledges support from NASA ADAP grant NNX11AD26G to Swarthmore
College. We thank A. Feldmeier for providing the instability simulations
discussed in Section 5, and for suggesting the exploration of Markov
models discussed in Section 6.
NR 35
TC 17
Z9 17
U1 0
U2 4
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 FEB
PY 2012
VL 420
IS 2
BP 1553
EP 1561
DI 10.1111/j.1365-2966.2011.20141.x
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 880OU
UT WOS:000299417600048
ER
PT J
AU Guan, B
Waliser, DE
Molotch, NP
Fetzer, EJ
Neiman, PJ
AF Guan, Bin
Waliser, Duane E.
Molotch, Noah P.
Fetzer, Eric J.
Neiman, Paul J.
TI Does the Madden-Julian Oscillation Influence Wintertime Atmospheric
Rivers and Snowpack in the Sierra Nevada?
SO MONTHLY WEATHER REVIEW
LA English
DT Article
ID EXTREME PRECIPITATION; CALIFORNIA; SATELLITE; RETRIEVALS; WASHINGTON;
REANALYSIS; MOUNTAINS; FREQUENCY; CALJET; FLOODS
AB The relationships between the Madden-Julian oscillation (MJO), activities of atmospheric rivers (ARs), and the resulting snowpack accumulation in the California Sierra Nevada, are analyzed based on 13 yr of observations for water years 1998-2010 inclusive. The AR activity, as measured by the number of high-impact ARs, mean per event snow water equivalent (SWE) changes, and the cumulative SWE changes, is shown to be significantly augmented when MJO convection is active over the far western tropical Pacific (phase 6 on the Wheeler-Hendon diagram). The timing of high-impact ARs (early- versus late-winter occurrences) also appears to be regulated by the MJO.
Total snow accumulation in the Sierra Nevada (i.e., AR and non-AR accumulation combined) is most significantly increased when MJO convection is active over the eastern Indian Ocean (phase 3), and reduced when MJO convection is active over the Western Hemisphere (phase 8), with the magnitude of the daily anomaly being roughly half the cold-season mean daily snow accumulation over many snow sensor sites. The positive (negative) SWE anomaly is accompanied by a cold (warm) surface air temperature (SAT) anomaly and an onshore (offshore) water vapor flux anomaly. The contrasting SAT anomaly patterns associated with MJO phases 3 and 8, revealed by the in situ observations, are more realistically represented in the Atmospheric Infrared Sounder retrievals than in the European Centre for Medium-Range Weather Forecasts Interim reanalysis.
C1 [Guan, Bin; Waliser, Duane E.; Molotch, Noah P.; Fetzer, Eric J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Molotch, Noah P.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA.
[Molotch, Noah P.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA.
[Neiman, Paul J.] NOAA, Div Phys Sci, Earth Syst Res Lab, Boulder, CO USA.
RP Guan, B (reprint author), CALTECH, Jet Prop Lab, M-S 233-300,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM bin.guan@jpl.nasa.gov
RI Guan, Bin/F-6735-2010; Molotch, Noah/C-8576-2009
FU NASA [NNX08AH18G]; NSF [EAR 1032295]; ARRA; Water Resources Area of the
NASA
FX This research was supported by NASA Grant NNX08AH18G, NSF Grant EAR
1032295, and by ARRA funds. Additional support was provided by the Water
Resources Area of the NASA Applied Sciences Program. Thanks go to K.
Weickmann, R. Wood, P. Webster, I.-S. Kang, J. Wallace, and G. Kiladis
for helpful discussions and comments; and to F. Ralph for his
encouragement. DEW's, EJF's, and BG's contribution, and part of NPM's
contribution, to this study were carried out on behalf of the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
NR 38
TC 31
Z9 31
U1 1
U2 26
PU AMER METEOROLOGICAL SOC
PI BOSTON
PA 45 BEACON ST, BOSTON, MA 02108-3693 USA
SN 0027-0644
EI 1520-0493
J9 MON WEATHER REV
JI Mon. Weather Rev.
PD FEB
PY 2012
VL 140
IS 2
BP 325
EP 342
DI 10.1175/MWR-D-11-00087.1
PG 18
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 886JI
UT WOS:000299850300001
ER
PT J
AU Masson, S
Aulanier, G
Pariat, E
Klein, KL
AF Masson, S.
Aulanier, G.
Pariat, E.
Klein, K. -L.
TI Interchange Slip-Running Reconnection and Sweeping SEP Beams
SO SOLAR PHYSICS
LA English
DT Article
DE Flares: models; Flares: energetic particles; Magnetohydrodynamics
ID SOLAR-ENERGETIC PARTICLES; QUASI-SEPARATRIX LAYERS; CURRENT SHEET
FORMATION; SOFT-X-RAY; FLUX TUBES; MAGNETIC RECONNECTION; NULL-POINT;
INNER HELIOSPHERE; ALFVEN WAVES; FIELD LINES
AB We present a new model to explain how particles (solar energetic particles; SEPs), accelerated at a reconnection site that is not magnetically connected to the Earth, could eventually propagate along the well-connected open flux tube. Our model is based on the results of a low-beta resistive magnetohydrodynamics simulation of a three-dimensional line-tied and initially current-free bipole, which is embedded in a non-uniform open potential field. The topology of this configuration is that of an asymmetric coronal null point, with a closed fan surface and an open outer spine. When driven by slow photospheric shearing motions, field lines, initially fully anchored below the fan dome, reconnect at the null point, and jump to the open magnetic domain. This is the standard interchange mode as sketched and calculated in 2D. The key result in 3D is that reconnected open field lines located in the vicinity of the outer spine keep reconnecting continuously, across an open quasi-separatrix layer, as previously identified for non-open-null-point reconnection. The apparent slipping motion of these field lines leads to formation of an extended narrow magnetic flux tube at high altitude. Because of the slip-running reconnection, we conjecture that if energetic particles would be traveling through, or be accelerated inside, the diffusion region, they would be successively injected along continuously reconnecting field lines that are connected farther and farther from the spine. At the scale of the full Sun, owing to the super-radial expansion of field lines below 3 R (aS (TM)), such energetic particles could easily be injected in field lines slipping over significant distances, and could eventually reach the distant flux tube that is well-connected to the Earth.
C1 [Masson, S.] NASA, Space Weather Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Aulanier, G.; Pariat, E.; Klein, K. -L.] Univ Paris Diderot, Observ Paris, CNRS, LESIA,UPMC, F-92190 Meudon, France.
RP Masson, S (reprint author), NASA, Space Weather Lab, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM sophie.masson@nasa.gov
FU Direction Generale de l'Armement (DGA); NASA at Goddard Space Flight
Center; NASA; European Commission [MTRN-CT-2006-035484]
FX The authors thank the referee for helpful comments, which improved the
clarity of the paper. The MHD calculations were done on the quadri-core
bi-Xeon computers of the Cluster of the Division Informatique de
l'Observatoire de Paris (DIO). The work of S.M. is funded by a
fellowship of Direction Generale de l'Armement (DGA). S.M. thank the
NASA Postdoctoral Program at the Goddard Space Flight Center,
administrated by Oak Ridge Associated Universities through a contract
with NASA for financial support. Financial support by the European
Commission through the FP6 SOLAIRE Network (MTRN-CT-2006-035484) is
gratefully acknowledged.
NR 50
TC 34
Z9 34
U1 0
U2 1
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
J9 SOL PHYS
JI Sol. Phys.
PD FEB
PY 2012
VL 276
IS 1-2
BP 199
EP 217
DI 10.1007/s11207-011-9886-3
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 878YX
UT WOS:000299295100012
ER
PT J
AU Thompson, WT
Kliem, B
Torok, T
AF Thompson, W. T.
Kliem, B.
Toeroek, T.
TI 3D Reconstruction of a Rotating Erupting Prominence
SO SOLAR PHYSICS
LA English
DT Article
DE Corona, active; Prominences, active; Coronal mass ejections; Initiation
and propagation; Magnetic fields, corona
ID CORONAL MASS EJECTION; CURRENT SHEET; FILAMENTS; HINODE; SOHO;
TELESCOPE; HELICITY; MISSION; REGION; STEREO
AB A bright prominence associated with a coronal mass ejection (CME) was seen erupting from the Sun on 9 April 2008. This prominence was tracked by both the Solar Terrestrial Relations Observatory (STEREO) EUVI and COR1 telescopes, and was seen to rotate about the line of sight as it erupted; therefore, the event has been nicknamed the "Cartwheel CME." The threads of the prominence in the core of the CME quite clearly indicate the structure of a weakly to moderately twisted flux rope throughout the field of view, up to heliocentric heights of 4 solar radii. Although the STEREO separation was 48A degrees, it was possible to match some sharp features in the later part of the eruption as seen in the 304 line in EUVI and in the H alpha-sensitive bandpass of COR1 by both STEREO Ahead and Behind. These features could then be traced out in three-dimensional space, and reprojected into a view in which the eruption is directed toward the observer. The reconstructed view shows that the alignment of the prominence to the vertical axis rotates as it rises up to a leading-edge height of a parts per thousand aEuro parts per thousand 2.5 solar radii, and then remains approximately constant. The alignment at 2.5 solar radii differs by about 115A degrees from the original filament orientation inferred from H alpha and EUV data, and the height profile of the rotation, obtained here for the first time, shows that two thirds of the total rotation are reached within a parts per thousand aEuro parts per thousand 0.5 solar radii above the photosphere. These features are well reproduced by numerical simulations of an unstable moderately twisted flux rope embedded in external flux with a relatively strong shear field component.
C1 [Thompson, W. T.] NASA, Adnet Syst Inc, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kliem, B.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Kliem, B.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Toeroek, T.] Univ Paris Diderot, Observ Paris, CNRS, LESIA,UPMC, F-92190 Meudon, France.
RP Thompson, WT (reprint author), NASA, Adnet Syst Inc, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA.
EM William.T.Thompson@nasa.gov
RI Thompson, William/D-7376-2012
FU NASA [NNG06EB68C, NNX08AG44G]; DFG; STFC; European Commission through
SOTERIA Network [218816]; NASA HTP; LWS
FX We acknowledge the use of data provided by the Global High Resolution Ha
Network, and by the SECCHI instruments on the STEREO spacecraft.
Magnetic field extrapolations were supplied by the CCMC; special thanks
to Lutz Rastaetter and Peter MacNeice for help with the CCMC data. We
thank the anonymous referee for a constructive report which led to a
deeper consideration of PIL orientation vs. height, and S. Patsourakos
for information about his fitting of the CME orientation in the COR2
height range. WTT's work was supported by NASA Grant NNG06EB68C. BK's
work was supported by the DFG, the STFC, and by NASA through Grant
NNX08AG44G. TT's work was partially supported by the European Commission
through the SOTERIA Network (EU FP7 Space Science Project No. 218816)
and by the NASA HTP and LWS programs.
NR 30
TC 23
Z9 23
U1 0
U2 3
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
EI 1573-093X
J9 SOL PHYS
JI Sol. Phys.
PD FEB
PY 2012
VL 276
IS 1-2
BP 241
EP 259
DI 10.1007/s11207-011-9868-5
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 878YX
UT WOS:000299295100014
ER
PT J
AU Sheldon, JE
Griffith, PC
Peters, F
Sheldon, WM
Blanton, JO
Amft, J
Pomeroy, LR
AF Sheldon, Joan E.
Griffith, Peter C.
Peters, Francesc
Sheldon, Wade M., Jr.
Blanton, Jackson O.
Amft, Julie
Pomeroy, Lawrence R.
TI Southeastern USA continental shelf respiratory rates revisited
SO BIOGEOCHEMISTRY
LA English
DT Article
DE Microbial respiration; Southeastern U. S. continental shelf; Dissolved
oxygen; Bacteria
ID ATMOSPHERIC CO2; UNITED-STATES; WATERS; OCEAN; TRANSPORT; ESTUARINE;
MARGINS; GEORGIA; CARBON; OXYGEN
AB Respiratory rates on the U. S. southeastern continental shelf have been estimated several times by different investigators, most recently by Jiang et al. (Biogeochemistry 98:101-113, 2010) who report lower mean rates than were found in earlier work and attribute the differences to analytical error in all methods used in earlier studies. The differences are, instead, attributable to the differences in the geographical scope of the studies. The lower estimates of regional organic carbon flux of Jiang et al. (Biogeochemistry 98:101-113, 2010) are a consequence of their extrapolation of data from a small portion of the shelf to the entire South Atlantic Bight. This comment examines the methodologies used as well as the variability of respiratory rates in this region over space and time.
C1 [Sheldon, Joan E.; Sheldon, Wade M., Jr.] Univ Georgia, Dept Marine Sci, Athens, GA 30602 USA.
[Griffith, Peter C.] NASA Goddard Space Flight Ctr, Sigma Space Corp, Carbon Cycle & Ecosyst Off, Greenbelt, MD 20711 USA.
[Peters, Francesc] CSIC, Inst Ciencies Mar, E-08003 Barcelona, Spain.
[Blanton, Jackson O.; Amft, Julie] Skidaway Inst Oceanog, Savannah, GA 31411 USA.
[Pomeroy, Lawrence R.] Univ Georgia, Inst Ecol, Athens, GA 30602 USA.
RP Sheldon, JE (reprint author), Univ Georgia, Dept Marine Sci, Athens, GA 30602 USA.
EM jsheldon@uga.edu
RI Peters, Francesc/A-6364-2009; Griffith, Peter/I-1392-2016
OI Peters, Francesc/0000-0001-9405-4306; Griffith,
Peter/0000-0002-4267-7429
FU National Science Foundation [0620959]
FX J. E. Sheldon and W. M. Sheldon, Jr. were supported by the Georgia
Coastal Ecosystems Long-Term Ecological Research program (National
Science Foundation award number 0620959).
NR 29
TC 1
Z9 1
U1 0
U2 8
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0168-2563
J9 BIOGEOCHEMISTRY
JI Biogeochemistry
PD FEB
PY 2012
VL 107
IS 1-3
BP 501
EP 506
DI 10.1007/s10533-010-9552-0
PG 6
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA 864GV
UT WOS:000298226700031
ER
PT J
AU Yoo, SW
Chaudhuri, S
Sacksteder, KR
Zhang, P
Zhu, DL
Law, CK
AF Yoo, Sean W.
Chaudhuri, Swetaprovo
Sacksteder, Kurt R.
Zhang, Peng
Zhu, Delin
Law, Chung K.
TI Response of spherical diffusion flames subjected to rotation:
Microgravity experimentation and computational simulation
SO COMBUSTION AND FLAME
LA English
DT Article
DE Rotating spherical diffusion flame
ID COMBUSTION; DROPLET
AB Microgravity experiments were conducted in the 2.2-s drop tower and zero-gravity facility at NASA-GRC to gain fundamental understanding of the effects of spinning on an otherwise spherical diffusion flame. The flames were generated by injecting either a fuel or an oxidizer mixture from a porous burner to a controlled ambient of either an oxidizer or fuel mixture, respectively. Results show that the polar flame location scales with the angular velocity monotonically as omega(a), where a is greater and smaller than unity for small and large spinning velocities, respectively. On the contrary, the equatorial flame location responds nonmonotonically to increasing spinning velocity: first increasing and then decreasing. The experimental observations agree well with the computational simulation where the simulated results demonstrate that the nonmonotonic response of the equatorial flame location is caused by dilution of the reactant concentration in the outwardly-directed radial flow by the product and inert that are carried by the inwardly-directed polar flow upon traversing the flame segment in the polar region. (C) 2011 The Combustion Institute. Published by Elsevier Inc. All rights reserved.
C1 [Yoo, Sean W.; Chaudhuri, Swetaprovo; Zhang, Peng; Zhu, Delin; Law, Chung K.] Princeton Univ, Dept Mech & Aerosp Engn, Princeton, NJ 08544 USA.
[Sacksteder, Kurt R.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Chaudhuri, S (reprint author), Princeton Univ, Dept Mech & Aerosp Engn, Princeton, NJ 08544 USA.
EM sweto@princeton.edu
RI Chaudhuri, Swetaprovo/C-6542-2008; Law, Chung /E-1206-2013;
OI Chaudhuri, Swetaprovo/0000-0003-2294-5534; Zhang,
Peng/0000-0002-1806-4200; Chaudhuri, Swetaprovo/0000-0003-4109-8633
FU NASA; NASA GSRP
FX This work was supported by the NASA Microgravity Combustion Program and
a NASA GSRP fellowship program to S.W.Y. The authors would like to
acknowledge the assistance of Dr. P. Ferkul, as well as all personnel at
the 2.2-second drop tower and Zero-G facility at NASA Glenn Research
Center.
NR 13
TC 0
Z9 0
U1 0
U2 10
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0010-2180
J9 COMBUST FLAME
JI Combust. Flame
PD FEB
PY 2012
VL 159
IS 2
BP 665
EP 672
DI 10.1016/j.combustflame.2011.07.013
PG 8
WC Thermodynamics; Energy & Fuels; Engineering, Multidisciplinary;
Engineering, Chemical; Engineering, Mechanical
SC Thermodynamics; Energy & Fuels; Engineering
GA 875XJ
UT WOS:000299068200017
ER
PT J
AU Simon, TA
Ward, WA
Boss, AP
AF Simon, Tyler A.
Ward, William A., Jr.
Boss, Alan P.
TI Performance analysis of Intel multiprocessors using astrophysics
simulations
SO CONCURRENCY AND COMPUTATION-PRACTICE & EXPERIENCE
LA English
DT Article; Proceedings Paper
CT Conference on Frontiers of Multicore Computing
CY AUG, 2010
CL Univ Maryland, Baltimore County, Catonsville, MD
HO Univ Maryland, Baltimore County
DE FLASH; performance analysis; multicore
ID THERMONUCLEAR FLASHES; REFINEMENT; BENCHMARK; CODE
AB This paper provides a performance evaluation and investigation of the astrophysics code FLASH for a variety of Intel multiprocessors. This work was performed at the NASA Center for Computational Sciences (NCCS) on behalf of the Carnegie Institution of Washington (CIW) as a study preliminary to the acquisition of a high-performance computing (HPC) system at the CIW and for the NCCS itself to measure the relative performance of a recently acquired Intel Nehalem-based system against previously installed multicore HPC resources. A brief overview of computer performance evaluation is provided, followed by a description of the systems under test, a description of the FLASH test problem, and the test results. Additionally, the paper characterizes some of the effects of load imbalance imposed by adaptive mesh refinement. Copyright (C) 2012 John Wiley & Sons, Ltd.
C1 [Simon, Tyler A.] NASA, Ctr Climate Simulat, Goddard Space Flight Ctr, Greenbelt, MD 20706 USA.
[Ward, William A., Jr.] DoD High Performance Comp Modernizat Program, Lorton, VA USA.
[Boss, Alan P.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC USA.
RP Simon, TA (reprint author), NASA, Ctr Climate Simulat, Goddard Space Flight Ctr, Greenbelt, MD 20706 USA.
EM tyler.simon@nasa.gov
RI novacescu, florica/B-4503-2011
OI novacescu, florica/0000-0001-5561-4956
NR 28
TC 3
Z9 3
U1 0
U2 3
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1532-0626
J9 CONCURR COMP-PRACT E
JI Concurr. Comput.-Pract. Exp.
PD FEB
PY 2012
VL 24
IS 2
SI SI
BP 155
EP 166
DI 10.1002/cpe.1888
PG 12
WC Computer Science, Software Engineering; Computer Science, Theory &
Methods
SC Computer Science
GA 877RW
UT WOS:000299201000005
ER
PT J
AU Veraverbeke, S
Somers, B
Gitas, I
Katagis, T
Polychronaki, A
Goossens, R
AF Veraverbeke, S.
Somers, B.
Gitas, I.
Katagis, T.
Polychronaki, A.
Goossens, R.
TI Spectral mixture analysis to assess post-fire vegetation regeneration
using Landsat Thematic Mapper imagery: Accounting for soil brightness
variation
SO INTERNATIONAL JOURNAL OF APPLIED EARTH OBSERVATION AND GEOINFORMATION
LA English
DT Article
DE Fire; Vegetation recovery; Landsat Thematic Mapper; Spectral mixture
analysis; MESMA; Segmentation
ID 2007 PELOPONNESE WILDFIRES; SANTA-MONICA MOUNTAINS; LEAF-AREA INDEX;
BURN SEVERITY; SOUTHERN-CALIFORNIA; HYPERSPECTRAL DATA; ENDMEMBER
VARIABILITY; MEDITERRANEAN BASIN; TIME-SERIES; FIRE
AB Post-fire vegetation cover is a crucial parameter in rangeland management. This study aims to assess the post-fire vegetation recovery 3 years after the large 2007 Peloponnese (Greece) wildfires. Post-fire recovery landscapes typically are mixed vegetation-substrate environments which makes spectral mixture analysis (SMA) a very effective tool to derive fractional vegetation cover maps. Using a combination of field and simulation techniques this study aimed to account for the impact of background brightness variability on SMA model performance. The field data consisted out of a spectral library of in situ measured reflectance signals of vegetation and substrate and 78 line transect plots. In addition, a Landsat Thematic Mapper (TM) scene was employed in the study. A simple SMA, in which each constituting terrain feature is represented by its mean spectral signature, a multiple endmember SMA (MESMA) and a segmented SMA, which accounts for soil brightness variations by forcing the substrate endmember choice based on ancillary data (lithological map), were applied. In the study area two main spectrally different lithological units were present: relatively bright limestone and relatively dark flysch (sand-siltstone). Although the simple SMA model resulted in reasonable regression fits for the flysch and limestones subsets separately (coefficient of determination R-2 of respectively 0.67 and 0.72 between field and TM data), the performance of the regression model on the pooled dataset was considerably weaker (R-2=0.65). Moreover, the regression lines significantly diverged among the different subsets leading to systematic over-or underestimations of the vegetative fraction depending on the substrate type. MESMA did not solve the endmember variability issue. The MESMA model did not manage to select the proper substrate spectrum on a reliable basis due to the lack of shape differences between the flysch and limestone spectra,. The segmented SMA model which accounts for soil brightness variations minimized the variability problems. Compared to the simple SMA and MESMA models, the segmented SMA resulted in a higher overall correlation (R-2 = 0.70), its regression slope and intercept were more similar among the different substrate types and its resulting regression lines more closely resembled the expected one-one line. This paper demonstrates the improvement of a segmented approach in accounting for soil brightness variations in estimating vegetative cover using SMA. However, further research is required to evaluate the model's performance for other soil types, with other image data and at different post-fire timings. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Veraverbeke, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Veraverbeke, S.; Goossens, R.] Univ Ghent, Dept Geog, BE-9000 Ghent, Belgium.
[Somers, B.] Flemish Inst Technol Res VITO, Ctr Remote Sensing & Earth Observat Proc TAP, BE-2400 Mol, Belgium.
[Gitas, I.; Katagis, T.; Polychronaki, A.] Aristotle Univ Thessaloniki, Lab Forest Management & Remote Sensing, GR-54124 Thessaloniki, Greece.
RP Veraverbeke, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,US-91109, Pasadena, CA 91109 USA.
EM Sander.S.Veraverbeke@jpl.nasa.gov; ben.somers@vito.be;
igitas@for.auth.gr; thkatag@for.auth.gr; anpolych@for.auth.gr;
rudi.goossens@ugent.be
RI Veraverbeke, Sander/H-2301-2012; Gitas, Ioannis/C-3329-2008
OI Veraverbeke, Sander/0000-0003-1362-5125; Gitas,
Ioannis/0000-0003-0056-5629
FU Ghent University; National Aeronautics and Space Administration; Belgian
Science Policy Office [SR/67/146]
FX The study was financed by the Ghent University special research funds
(BOF: Bijzonder Onderzoeksfonds). Part of the work was carried out at
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with the National Aeronautics and Space Administration. The
contribution of Dr. Ben Somers is funded by the Belgian Science Policy
Office in the frame of the STEREO II programme - project VEGEMIX
(SR/67/146).
NR 78
TC 18
Z9 19
U1 3
U2 40
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0303-2434
J9 INT J APPL EARTH OBS
JI Int. J. Appl. Earth Obs. Geoinf.
PD FEB
PY 2012
VL 14
IS 1
BP 1
EP 11
DI 10.1016/j.jag.2011.08.004
PG 11
WC Remote Sensing
SC Remote Sensing
GA 871AB
UT WOS:000298708900001
ER
PT J
AU Martin, AM
Laporte, D
Koga, KT
Kawamoto, T
Hammouda, T
AF Martin, Audrey M.
Laporte, Didier
Koga, Kenneth T.
Kawamoto, Tatsuhiko
Hammouda, Tahar
TI Experimental Study of the Stability of a Dolomite plus Coesite
Assemblage in Contact With Peridotite: Implications for Sediment-Mantle
Interaction and Diamond Formation During Subduction
SO JOURNAL OF PETROLOGY
LA English
DT Article
DE decarbonation reaction; redox reaction; metastable graphite;
metasomatism; ultrahigh-pressure metamorphism
ID PRESSURE METAMORPHIC ROCKS; NORTHERN KAZAKSTAN; KOKCHETAV MASSIF; DABIE
MOUNTAINS; OCEAN CRUST; 2 CO2; 6 GPA; MAGNESITE; DECARBONATION; KINETICS
AB Carbonates carried by oceanic plates-in the form of sediment or alteration products of basalts-are introduced into the mantle by subduction. The high-pressure-high-temperature stability of carbonates in a closed system has been constrained by a number of studies, but the effects of the interactions between subducted carbonates and the surrounding mantle on carbonate stability are poorly known. These interactions may, however, influence the stability depth of the subducted material, the composition of the interaction zone, and the rate of carbon transfer from the slab to the mantle. To determine the exchange mechanisms at the interface between a subducted dolomite + coesite assemblage and the overlying mantle, we performed experiments at 6 GPa and 900 degrees C and 1100 degrees C in a multi-anvil apparatus. In a first series of experiments, we studied the reaction and migration processes operating along the interface between a cylinder of dolomite + coesite and a cylinder of garnet peridotite. In a second series of experiments, homogeneous mixtures of dolomite + coesite and garnet peridotite were equilibrated at high pressure and high temperature to characterize the phase relations as a function of the (dolomite + coesite)/peridotite ratio. We show that the destabilization temperature of a subducted dolomite + coesite assemblage is less than 900 degrees C at 6 GPa when in contact with a garnet lherzolite or a harzburgite. A reaction zone composed mainly of clinopyroxene + magnesite is produced at the interface between dolomite + coesite and peridotite. Carbon-in the form of a fluid or in a carbonatitic melt-also infiltrates the garnet peridotite to form magnesite and clinopyroxene. Moreover, graphite was observed in two experiments. We believe that it was produced by a redox reaction at the interface between dolomite + coesite and iron-bearing silicates in the peridotite. As our experimental conditions are in the stability field of diamond, this suggests a potential mechanism for diamond crystallization from subducted dolomite + coesite in contact with the mantle wedge.
C1 [Martin, Audrey M.] NASA, Lyndon B Johnson Space Ctr, Mailcode KT, Houston, TX 77058 USA.
[Kawamoto, Tatsuhiko] Kyoto Univ, Grad Sch Sci, Inst Geothermal Sci, Beppu, Oita 8740903, Japan.
[Martin, Audrey M.; Laporte, Didier; Koga, Kenneth T.; Hammouda, Tahar] IRD, LMV, R163, F-63038 Clermont Ferrand, France.
[Martin, Audrey M.; Laporte, Didier; Koga, Kenneth T.; Hammouda, Tahar] CNRS, LMV, UMR 6524, F-63038 Clermont Ferrand, France.
[Martin, Audrey M.; Laporte, Didier; Koga, Kenneth T.; Hammouda, Tahar] Univ Clermont Ferrand, Univ Clermont Ferrand 2, Lab Magmas & Volcans, F-63000 Clermont Ferrand, France.
RP Martin, AM (reprint author), NASA, Lyndon B Johnson Space Ctr, Mailcode KT, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM aud.martin23@gmail.com
RI Kawamoto, Tatsuhiko/H-6088-2011; Koga, Kenneth T./D-8170-2017;
OI Kawamoto, Tatsuhiko/0000-0002-6989-874X; Koga, Kenneth
T./0000-0002-0862-6804; Martin, Audrey/0000-0002-1165-8866
FU JSPS Japan-France; Institut National des Sciences de l'Univers
(INSU-CNRS); Centre National de la Recherche Scientifique (INSU National
Instrument)
FX The exchange visit to JASRI was supported by the JSPS Japan-France
integrated action program (SAKURA 2006-2007). This study was supported
by the DyETI program of the Institut National des Sciences de l'Univers
(INSU-CNRS), through grants to T. Hammouda. The multi-anvil apparatus of
Laboratoire Magmas et Volcans is financially supported by the Centre
National de la Recherche Scientifique (INSU National Instrument).
NR 54
TC 9
Z9 10
U1 0
U2 22
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0022-3530
J9 J PETROL
JI J. Petrol.
PD FEB
PY 2012
VL 53
IS 2
BP 391
EP 417
DI 10.1093/petrology/egr066
PG 27
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 879QW
UT WOS:000299348000006
ER
PT J
AU Jain, A
AF Jain, Abhinandan
TI Multibody graph transformations and analysis
SO NONLINEAR DYNAMICS
LA English
DT Article
DE Multibody dynamics; Simulation
ID SPATIAL OPERATOR ALGEBRA; SYSTEM DYNAMICS
AB This is the second part of a two-part paper that develops graph theoretic techniques for the topological transformation and analysis of multibody system dynamics. The first part focused on tree systems, and developed systematic and rigorous techniques for the partitioning, aggregation, and substructuring of multibody dynamics models. This second part, uses the aggregation techniques as the foundation to develop the constraint-embedding technique that enables the transformation of the nontree system graphs into tree graphs. This enables the application of a large family of analytical and computational techniques for trees to closed-chain systems. This is illustrated through an extension of the low-order articulated-body forward dynamics algorithm for tree systems to closed-chain systems.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Jain, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Abhi.Jain@jpl.nasa.gov
FU National Aeronautics and Space Administration; National Institute of
Health [RO1GM082896-01A2]
FX We would like to acknowledge the many detailed and insightful comments
by the anonymous reviewer that have helped us revise and improve this
paper. The research described in this paper was performed at the Jet
Propulsion Laboratory (JPL), California Institute of Technology, under
contract with the National Aeronautics and Space
Administration.3 This project was also supported in part by
Grant Number RO1GM082896-01A2 from the National Institute of Health.
NR 17
TC 1
Z9 1
U1 0
U2 1
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0924-090X
J9 NONLINEAR DYNAM
JI Nonlinear Dyn.
PD FEB
PY 2012
VL 67
IS 3
BP 2153
EP 2170
DI 10.1007/s11071-011-0136-x
PG 18
WC Engineering, Mechanical; Mechanics
SC Engineering; Mechanics
GA 876CW
UT WOS:000299085800037
PM 22267894
ER
PT J
AU Nitschke, W
Russell, MJ
AF Nitschke, Wolfgang
Russell, Michael J.
TI Redox bifurcations: Mechanisms and importance to life now, and at its
origin
SO BIOESSAYS
LA English
DT Article
ID METHANOGENIC ARCHAEA; CLOSTRIDIUM-KLUYVERI; ENERGY-CONSERVATION;
FERREDOXIN; REDUCTION; NADH; COMPLEX
C1 [Nitschke, Wolfgang] CNRS IFR88, Bioenerget & Ingn Prot UPR9036, Marseille, France.
[Russell, Michael J.] CALTECH, JPL, Pasadena, CA 91125 USA.
RP Nitschke, W (reprint author), CNRS IFR88, Bioenerget & Ingn Prot UPR9036, Marseille, France.
EM nitschke@ibsm.cnrs-mrs.fr
NR 12
TC 27
Z9 27
U1 4
U2 30
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0265-9247
J9 BIOESSAYS
JI Bioessays
PD FEB
PY 2012
VL 34
IS 2
BP 106
EP 109
DI 10.1002/bies.201100134
PG 4
WC Biochemistry & Molecular Biology; Biology
SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other
Topics
GA 874UL
UT WOS:000298983500023
PM 22045626
ER
PT J
AU Toth, G
van der Holst, B
Sokolov, IV
De Zeeuw, DL
Gombosi, TI
Fang, F
Manchester, WB
Meng, X
Najib, D
Powell, KG
Stout, QF
Glocer, A
Ma, YJ
Opher, M
AF Toth, Gabor
van der Holst, Bart
Sokolov, Igor V.
De Zeeuw, Darren L.
Gombosi, Tamas I.
Fang, Fang
Manchester, Ward B.
Meng, Xing
Najib, Dalal
Powell, Kenneth G.
Stout, Quentin F.
Glocer, Alex
Ma, Ying-Juan
Opher, Merav
TI Adaptive numerical algorithms in space weather modeling
SO JOURNAL OF COMPUTATIONAL PHYSICS
LA English
DT Article
DE 65D99 Numerical approximation; 77A05 Magnetohydrodynamics
ID CORONAL MASS EJECTIONS; HYPERBOLIC CONSERVATION-LAWS; 3-DIMENSIONAL MHD
SIMULATION; NONSYMMETRIC LINEAR-SYSTEMS; SOLAR-WIND; IDEAL
MAGNETOHYDRODYNAMICS; PARTICLE-ACCELERATION; ELECTRIC POTENTIALS;
MAGNETIC-FIELD; SCHEMES
AB Space weather describes the various processes in the Sun-Earth system that present danger to human health and technology. The goal of space weather forecasting is to provide an opportunity to mitigate these negative effects. Physics-based space weather modeling is characterized by disparate temporal and spatial scales as well as by different relevant physics in different domains. A multi-physics system can be modeled by a software framework comprising several components. Each component corresponds to a physics domain, and each component is represented by one or more numerical models. The publicly available Space Weather Modeling Framework (SWMF) can execute and couple together several components distributed over a parallel machine in a flexible and efficient manner. The framework also allows resolving disparate spatial and temporal scales with independent spatial and temporal discretizations in the various models.
Several of the computationally most expensive domains of the framework are modeled by the Block-Adaptive Tree Solarwind Roe-type Upwind Scheme (BATS-R-US) code that can solve various forms of the magnetohydrodynamic (MHD) equations, including Hall, semi-relativistic, multi-species and multi-fluid MHD, anisotropic pressure, radiative transport and heat conduction. Modeling disparate scales within BATS-R-US is achieved by a block-adaptive mesh both in Cartesian and generalized coordinates. Most recently we have created a new core for BATS-R-US: the Block-Adaptive Tree Library (BAIL) that provides a general toolkit for creating, load balancing and message passing in a 1,2 or 3 dimensional block-adaptive grid. We describe the algorithms of BATL and demonstrate its efficiency and scaling properties for various problems.
BATS-R-US uses several time-integration schemes to address multiple time-scales: explicit time stepping with fixed or local time steps, partially steady-state evolution, point-implicit, semi-implicit, explicit/implicit, and fully implicit numerical schemes. Depending on the application, we find that different time stepping methods are optimal. Several of the time integration schemes exploit the block-based granularity of the grid structure.
The framework and the adaptive algorithms enable physics-based space weather modeling and even short-term forecasting. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Toth, Gabor; van der Holst, Bart; Sokolov, Igor V.; De Zeeuw, Darren L.; Gombosi, Tamas I.; Fang, Fang; Manchester, Ward B.; Meng, Xing; Najib, Dalal; Powell, Kenneth G.; Stout, Quentin F.] Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA.
[Glocer, Alex] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
[Ma, Ying-Juan] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Opher, Merav] Boston Univ, Dept Astron, Boston, MA 02215 USA.
RP Toth, G (reprint author), Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA.
EM gtoth@umich.edu
RI Ma, Yingjuan/B-4895-2017; De Zeeuw, Darren/F-3667-2011; van der Holst,
Bart/A-3557-2013; Glocer, Alex/C-9512-2012; Manchester,
Ward/I-9422-2012; Gombosi, Tamas/G-4238-2011; Toth, Gabor/B-7977-2013;
Sokolov, Igor/H-9860-2013; feggans, john/F-5370-2012; Meng,
Xing/A-1929-2016
OI Ma, Yingjuan/0000-0003-2584-7091; Stout, Quentin/0000-0002-8047-7348;
van der Holst, Bart/0000-0001-5260-3944; Powell,
Kenneth/0000-0002-3708-8814; Glocer, Alex/0000-0001-9843-9094; Gombosi,
Tamas/0000-0001-9360-4951; Toth, Gabor/0000-0002-5654-9823; Sokolov,
Igor/0000-0002-6118-0469;
FU NSF [ATM 0642309, ATM-0639336, AGS-1027192, AGS 1023735]; NASA
[NNX07AC16G, NNX07AV80G]; AFOSR [FA9550-07-1-0434]; Department of Energy
NNSA [DEFC52-08NA28616]; Jet Propulsion Laboratory [DRDA-07-1583]; NASA
LWS [NNX09AJ78G]; NSF CAREER [ATM-0747654]
FX The heliospheric components of the SWMF are developed as part of the
Comprehensive Corona and Heliospheric Model supported by the NSF ATM
0642309 and NASA NNX07AC16G grants. The magnetospheric components are
developed as part of the Community-based Whole Magnetospheric Model
supported by NSF ATM-0639336 and AFOSR FA9550-07-1-0434 grants.
Extension of BATS-R-US to non-ideal MHD was supported by the NASA
Applied Information Systems Research Program grant NNX07AV80G. We also
acknowledge support from the NSF Cyber-Enabled Discovery and Innovation
grant AGS-1027192. The Block Adaptive Tree Library, the radiative
transfer and multi-material physics were developed by the Center for
Radiative Shock Hydrodynamics supported by the Department of Energy NNSA
under the Predictive Science Academic Alliance Program by grant
DEFC52-08NA28616. The General Input Parameter Handling Toolkit
development was supported by the DRDA-07-1583 grant from the Jet
Propulsion Laboratory. Ward Manchester and Fang Fang acknowledge support
by the NSF AGS 1023735 and NASA LWS NNX09AJ78G grants. Merav Opher
thanks the support of the NSF CAREER Grant ATM-0747654. We thank the
NASA Supercomputer Division at Ames and its helpful staff for making it
possible to perform many of the simulations presented in this paper.
NR 91
TC 168
Z9 170
U1 2
U2 26
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0021-9991
EI 1090-2716
J9 J COMPUT PHYS
JI J. Comput. Phys.
PD FEB 1
PY 2012
VL 231
IS 3
SI SI
BP 870
EP 903
DI 10.1016/j.jcp.2011.02.006
PG 34
WC Computer Science, Interdisciplinary Applications; Physics, Mathematical
SC Computer Science; Physics
GA 868LG
UT WOS:000298524200008
ER
PT J
AU Paranicas, C
Roussos, E
Krupp, N
Kollmann, P
Hendrix, AR
Cassidy, T
Johnson, RE
Schenk, P
Jones, G
Carbary, J
Mitchell, DG
Dialynas, K
AF Paranicas, C.
Roussos, E.
Krupp, N.
Kollmann, P.
Hendrix, A. R.
Cassidy, T.
Johnson, R. E.
Schenk, P.
Jones, G.
Carbary, J.
Mitchell, D. G.
Dialynas, K.
TI Energetic charged particle weathering of Saturn's inner satellites
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Planetary magnetospheres; Saturn; Planetary satellites
ID MAGNETOSPHERE; PROTONS; EUROPA; BOMBARDMENT; ALBEDO; RING
AB We characterize the relative importance of energetic electrons and protons to the weathering of five of the inner satellites of Saturn. To do this, we present data from the Magnetospheric Imaging Instrument on the Cassini spacecraft, some of which is averaged over the whole mission to date. We also compute averaged proton and electron energy spectra relevant to the distances of these inner satellites. Where data are available, we estimate the power per unit area into a satellite's surface. For electron energy deposition into satellite leading hemispheres, we find the power per unit area is greatest at Mimas and falls off with distance from Saturn. Using fluxes of 1-50 MeV protons detected within the sweeping corridors of Mimas and Enceladus, we find the corresponding deposition would be about 2 x 10(8) and 3.7 x 10(7) eV/cm(2) s. (C) 2011 Elsevier Ltd. All rights
C1 [Paranicas, C.; Carbary, J.; Mitchell, D. G.] APL, Laurel, MD 20723 USA.
[Roussos, E.; Krupp, N.; Kollmann, P.] MPS, D-37191 Katlenburg Lindau, Germany.
[Hendrix, A. R.; Cassidy, T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Johnson, R. E.] UVA, Charlottesville, VA 22904 USA.
[Schenk, P.] LPI, Houston, TX USA.
[Jones, G.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Dialynas, K.] Univ Athens, Athens, Greece.
RP Paranicas, C (reprint author), APL, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA.
EM chris.paranicas@jhuapl.edu
RI Jones, Geraint/C-1682-2008; Paranicas, Christopher/B-1470-2016; Carbary,
James/C-2086-2016; Kollmann, Peter/C-2583-2016;
OI Jones, Geraint/0000-0002-5859-1136; Paranicas,
Christopher/0000-0002-4391-8255; Carbary, James/0000-0003-1781-3078;
Kollmann, Peter/0000-0002-4274-9760; Roussos, Elias/0000-0002-5699-0678
NR 28
TC 12
Z9 12
U1 2
U2 6
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 FEB
PY 2012
VL 61
IS 1
SI SI
BP 60
EP 65
DI 10.1016/j.pss.2011.02.012
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 971IY
UT WOS:000306198800007
ER
PT J
AU Eckman, RS
Stackhouse, PW
AF Eckman, Richard S.
Stackhouse, Paul W., Jr.
TI CEOS contributions to informing energy management and policy decision
making using space-based Earth observations
SO APPLIED ENERGY
LA English
DT Article; Proceedings Paper
CT International Conference on Applied Energy (ICAE) on Energy Solutions
for a Sustainable World
CY APR 21-23, 2010
CL Singapore, SINGAPORE
DE Energy management; Renewable energy resource assessment; Committee on
Earth Observation Satellites; Group on Earth Observations; Energy
efficiency; Decision support
AB Earth observations are playing an increasingly significant role in informing decision making in the energy sector. In renewable energy applications, space-based observations now routinely augment sparse ground-based observations used as input for renewable energy resource assessment applications. As one of the nine Group on Earth Observations (GEO) societal benefit areas, the enhancement of management and policy decision making in the energy sector is receiving attention in activities conducted by the Committee on Earth Observation Satellites (CEOS). CEOS has become the "space arm" for the implementation of the Global Earth Observation System of Systems (GEOSS) vision. It is directly supporting the space-based, near-term tasks articulated in the GEO three-year work plan.
This paper describes a coordinated program of demonstration projects conducted by CEOS member agencies and partners to utilize Earth observations to enhance energy management end-user decision support systems. We discuss the importance of engagement with stakeholders and understanding their decision support needs in successfully increasing the uptake of Earth observation products for societal benefit. Several case studies are presented, demonstrating the importance of providing data sets in formats and units familiar and immediately usable by decision makers. These projects show the utility of Earth observations to enhance renewable energy resource assessment in the developing world, forecast space weather impacts on the power grid, and improve energy efficiency in the built environment. Published by Elsevier Ltd.
C1 [Eckman, Richard S.; Stackhouse, Paul W., Jr.] NASA, Sci Directorate, Langley Res Ctr, Hampton, VA 23681 USA.
[Eckman, Richard S.] NASA Headquarters, Div Earth Sci, Sci Miss Directorate, Washington, DC 20546 USA.
RP Eckman, RS (reprint author), NASA, Sci Directorate, Langley Res Ctr, Mail Stop 420, Hampton, VA 23681 USA.
EM Richard.S.Eckman@nasa.gov; Paul.W.Stackhouse@nasa.gov
NR 13
TC 8
Z9 8
U1 0
U2 5
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0306-2619
J9 APPL ENERG
JI Appl. Energy
PD FEB
PY 2012
VL 90
IS 1
SI SI
BP 206
EP 210
DI 10.1016/j.apenergy.2011.03.001
PG 5
WC Energy & Fuels; Engineering, Chemical
SC Energy & Fuels; Engineering
GA 853KV
UT WOS:000297426100032
ER
PT J
AU Leckey, CAC
Rogge, MD
Miller, CA
Hinders, MK
AF Leckey, Cara A. C.
Rogge, Matthew D.
Miller, Corey A.
Hinders, Mark K.
TI Multiple-mode Lamb wave scattering simulations using 3D elastodynamic
finite integration technique
SO ULTRASONICS
LA English
DT Article
DE Lamb waves; Nondestructive evaluation; Simulation
ID HELICAL ULTRASONIC TOMOGRAPHY; ALUMINUM-ALLOYS; PROPAGATION; TIME;
GEOMETRIES; DAMAGE
AB We have implemented three-dimensional (3D) elastodynamic finite integration technique (EFIT) simulations to model Lamb wave scattering for two flaw-types in an aircraft-grade aluminum plate, a rounded rectangle flat-bottom hole and a disbond of the same shape. The plate thickness and flaws explored in this work include frequency-thickness regions where several Lamb wave modes exist and sometimes overlap in phase and/or group velocity. For the case of the flat-bottom hole the depth was incrementally increased to explore progressive changes in multiple-mode Lamb wave scattering due to the damage. The flat-bottom hole simulation results have been compared to experimental data and are shown to provide key insight for this well-defined experimental case by explaining unexpected results in experimental waveforms. For the rounded rectangle disbond flaw, which would be difficult to implement experimentally, we found that Lamb wave behavior differed significantly from the flat-bottom hole flaw. Most of the literature in this field is restricted to low frequency-thickness regions due to difficulties in interpreting data when multiple modes exist. We found that benchmarked 3D EFIT simulations can yield an understanding of scattering behavior for these higher frequency-thickness regions and in cases that would be difficult to set up experimentally. Additionally, our results show that 2D simulations would not have been sufficient for modeling the complicated scattering that occurred. Published by Elsevier B.V.
C1 [Leckey, Cara A. C.; Rogge, Matthew D.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Miller, Corey A.; Hinders, Mark K.] Coll William & Mary, Dept Appl Sci, Williamsburg, VA USA.
RP Leckey, CAC (reprint author), NASA, Langley Res Ctr, MS 231, Hampton, VA 23681 USA.
EM cara.ac.leckey@nasa.gov
NR 43
TC 25
Z9 25
U1 0
U2 19
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0041-624X
J9 ULTRASONICS
JI Ultrasonics
PD FEB
PY 2012
VL 52
IS 2
BP 193
EP 207
DI 10.1016/j.ultras.2011.08.003
PG 15
WC Acoustics; Radiology, Nuclear Medicine & Medical Imaging
SC Acoustics; Radiology, Nuclear Medicine & Medical Imaging
GA 852EQ
UT WOS:000297335200001
PM 21908011
ER
PT J
AU Hillers, G
Graham, N
Campillo, M
Kedar, S
Landes, M
Shapiro, N
AF Hillers, G.
Graham, N.
Campillo, M.
Kedar, S.
Landes, M.
Shapiro, N.
TI Global oceanic microseism sources as seen by seismic arrays and
predicted by wave action models
SO GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS
LA English
DT Article
DE microseisms; noise seasonality; noise source; seismic noise; wave action
models
ID NOISE; TOMOGRAPHY; RADIATION; PACIFIC; COASTAL; PHASE; TIME; SEA; HUM
AB We analyze global microseism excitation patterns between July 2000 and June 2001. Seismological observations are compared with modeling results to isolate robust activity features of relevant source processes. First, we use observations of microseism source locations estimated by Landes et al. (2010) based on array processing of ambient noise correlations. Second, we construct synthetic activity patterns by coupling sea state estimates derived from wave action models to the excitation theory for microseisms. The overall spatiotemporal evolution of both estimates is characterized by a seasonal character that is associated with strong activity during winter months. The distribution of landmass causes seasonal changes on the Northern Hemisphere (NH) to exceed the variability on the Southern Hemisphere (SH). Our systematic comparison of the two estimates reveals significant microseism excitation along coastlines and in the open ocean. Since coastal reflections are not accounted for in the modeling approach, the consistent mismatch between near-coastal observations and predictions suggests that relevant microseism energy arriving at the networks is generated in these areas. Simultaneously, systematic coincidence away from coastlines verifies the open ocean generation hypothesis. These conclusions are universal and robust with respect to the seismic network locations on the NH. The spatially homogeneous resolution of our synthetics provides a valuable resource for the assessment of the global microseism weather. Similar to previously identified hot spot areas in the North Atlantic, the modeled distributions hypothesize regions of strong localized activity on the SH, which are only partially confirmed by the analyzed data sets.
C1 [Hillers, G.; Campillo, M.] Univ Grenoble 1, CNRS, Inst Sci Terre, F-38041 Grenoble 9, France.
[Graham, N.] Hydrol Res Ctr, San Diego, CA 92130 USA.
[Kedar, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Landes, M.] Commissariat Energie Atom & Energies Renouvelable, Direct Applicat Mil, Dept Ile de France, F-91297 Arpajon, France.
[Shapiro, N.] CNRS, UMR7154, Inst Phys Globe Paris, F-75238 Paris, France.
RP Hillers, G (reprint author), Univ Grenoble 1, CNRS, Inst Sci Terre, BP 53, F-38041 Grenoble 9, France.
EM hillersg@ujf-grenoble.fr
RI Shapiro, Nikolai/G-1049-2010; Campillo, Michel/K-6231-2012
OI Shapiro, Nikolai/0000-0002-0144-723X;
FU European Research Council [L27507]
FX We thank P. Roux for discussions on beamformer resolution. The
manuscript benefited from the comments of the Editor, Thorsten Becker,
and two anonymous reviewers. This work was supported by the European
Research Council (advanced grant Whisper L27507). Most figures were
constructed using Generic Mapping Tools (GMT) [Wessel and Smith, 1991].
NR 54
TC 37
Z9 38
U1 1
U2 20
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1525-2027
J9 GEOCHEM GEOPHY GEOSY
JI Geochem. Geophys. Geosyst.
PD JAN 31
PY 2012
VL 13
AR Q01021
DI 10.1029/2011GC003875
PG 19
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 888GA
UT WOS:000299990600001
ER
PT J
AU Hanna, KLD
Wyatt, MB
Thomas, IR
Bowles, NE
Greenhagen, BT
Maturilli, A
Helbert, J
Paige, DA
AF Hanna, Kerri L. Donaldson
Wyatt, Michael B.
Thomas, Ian R.
Bowles, Neil E.
Greenhagen, Benjamin T.
Maturilli, Alessandro
Helbert, Joern
Paige, David A.
TI Thermal infrared emissivity measurements under a simulated lunar
environment: Application to the Diviner Lunar Radiometer Experiment
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID REFLECTANCE SPECTRA; SURFACE FEATURES; MOON; SPECTROSCOPY; OLIVINE;
ROCK; PLAGIOCLASE; MINERALOGY; SILICATES; PYROXENES
AB We present new laboratory thermal infrared emissivity spectra of the major silicate minerals identified on the Moon measured under lunar environmental conditions and evaluate their application to lunar remote sensing data sets. Thermal infrared spectral changes between ambient and lunar environmental conditions are characterized for the first time over the 400 similar to 1700 cm(-1) (6-25 mu m) spectral range for a fine-particulate mineral suite including plagioclase (albite and anorthite), pyroxene (enstatite and augite), and olivine (forsterite). The lunar environment introduces observable effects in thermal infrared emissivity spectra of fine particulate minerals, which include: (1) a shift in the Christiansen feature (CF) position to higher wave numbers (shorter wavelengths), (2) an increase in the overall spectral contrast, and (3) decreases in the spectral contrast of the reststrahlen bands and transparency features. Our new measurements demonstrate the high sensitivity of thermal infrared emissivity spectra to environmental conditions under which they are measured and provide important constraints for interpreting new thermal infrared data sets of the Moon, including the Diviner Lunar Radiometer Experiment onboard NASA's Lunar Reconnaissance Orbiter. Full resolution laboratory mineral spectra convolved to Diviner's three spectral channels show that spectral shape, CF position and band ratios can be used to distinguish between individual mineral groups and lunar lithologies. The integration of the thermal infrared CF position with near infrared spectral parameters allows for robust mineralogical identifications and provides a framework for future integrations of data sets across two different wavelength regimes.
C1 [Hanna, Kerri L. Donaldson; Wyatt, Michael B.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA.
[Thomas, Ian R.; Bowles, Neil E.] Univ Oxford, Clarendon Lab, Oxford OX1 3PU, England.
[Greenhagen, Benjamin T.] Jet Prop Lab, Geophys & Planetary Geosci Grp, Pasadena, CA 91109 USA.
[Maturilli, Alessandro; Helbert, Joern] German Aerosp Ctr, Inst Planetary Res, D-12489 Berlin, Germany.
[Paige, David A.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
RP Hanna, KLD (reprint author), Brown Univ, Dept Geol Sci, Box 1846, Providence, RI 02912 USA.
EM kerri_donaldson_hanna@brown.edu
RI Greenhagen, Benjamin/C-3760-2016
OI Helbert, Jorn/0000-0001-5346-9505;
FU NASA [NNX08AM75G]
FX We would like to extend our appreciation to P. Christensen and Arizona
State University for donating the samples used in this study. The
authors would also like to thank S. Ruff and an anonymous reviewer for
comments and suggestions that have helped to improve the manuscript as
well as C. M. Pieters for comments and suggestions that greatly improved
the thermal- and near- infrared data integration portion of this
manuscript. K. L. Donaldson Hanna and M. B. Wyatt were supported by NASA
grant NNX08AM75G.
NR 68
TC 7
Z9 7
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-PLANET
JI J. Geophys. Res.-Planets
PD JAN 31
PY 2012
VL 117
AR E00H05
DI 10.1029/2011JE003862
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 887UL
UT WOS:000299956100001
ER
PT J
AU Abe, K
Fuke, H
Haino, S
Hams, T
Hasegawa, M
Horikoshi, A
Kim, KC
Kusumoto, A
Lee, MH
Makida, Y
Matsuda, S
Matsukawa, Y
Mitchell, JW
Nishimura, J
Nozaki, M
Orito, R
Ormes, JF
Sakai, K
Sasaki, M
Seo, ES
Shinoda, R
Streitmatter, RE
Suzuki, J
Tanaka, K
Thakur, N
Yamagami, T
Yamamoto, A
Yoshida, T
Yoshimura, K
AF Abe, K.
Fuke, H.
Haino, S.
Hams, T.
Hasegawa, M.
Horikoshi, A.
Kim, K. C.
Kusumoto, A.
Lee, M. H.
Makida, Y.
Matsuda, S.
Matsukawa, Y.
Mitchell, J. W.
Nishimura, J.
Nozaki, M.
Orito, R.
Ormes, J. F.
Sakai, K.
Sasaki, M.
Seo, E. S.
Shinoda, R.
Streitmatter, R. E.
Suzuki, J.
Tanaka, K.
Thakur, N.
Yamagami, T.
Yamamoto, A.
Yoshida, T.
Yoshimura, K.
TI Measurement of the Cosmic-Ray Antiproton Spectrum at Solar Minimum with
a Long-Duration Balloon Flight over Antarctica
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID BESS-POLAR EXPERIMENT; BLACK-HOLES; SPECTROMETER; PROGRESS; SEARCH;
MATTER; FLUX
AB The energy spectrum of cosmic-ray antiprotons ((p) over bar 's) from 0.17 to 3.5 GeV has been measured using 7886 (p) over bar 's detected by BESS-Polar II during a long-duration flight over Antarctica near solar minimum in December 2007 and January 2008. This shows good consistency with secondary (p) over bar calculations. Cosmologically primary (p) over bar 's have been investigated by comparing measured and calculated (p) over bar spectra. BESS-Polar II data show no evidence of primary (p) over bar 's from the evaporation of primordial black holes.
C1 [Hams, T.; Mitchell, J. W.; Sakai, K.; Sasaki, M.; Streitmatter, R. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Abe, K.; Kusumoto, A.; Matsukawa, Y.; Orito, R.] Kobe Univ, Kobe, Hyogo 6578501, Japan.
[Fuke, H.; Yamagami, T.; Yoshida, T.] Japan Aerosp Explorat Agcy ISAS JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Haino, S.; Hasegawa, M.; Horikoshi, A.; Makida, Y.; Matsuda, S.; Nozaki, M.; Suzuki, J.; Tanaka, K.; Yamamoto, A.; Yoshimura, K.] High Energy Accelerator Res Org KEK, Tsukuba, Ibaraki 3050801, Japan.
[Kim, K. C.; Lee, M. H.; Seo, E. S.] Univ Maryland, IPST, College Pk, MD 20742 USA.
[Nishimura, J.; Sakai, K.; Shinoda, R.; Yamamoto, A.] Univ Tokyo, Bunkyo Ku, Tokyo 1130033, Japan.
[Ormes, J. F.; Thakur, N.] Univ Denver, Denver, CO 80208 USA.
RP Sakai, K (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM Kenichi.Sakai@nasa.gov
OI Seo, Eun-Suk/0000-0001-8682-805X
FU KAKENHI; MEXT-JSPS; NASA
FX The BESS-Polar Collaboration is supported in Japan by the Grant-in-Aid
"KAKENHI" for specially promoted and basic researches, MEXT-JSPS, and in
the U.S. by NASA. Balloon flight operations were carried out by the NASA
Columbia Scientific Balloon Facility and the National Science Foundation
United States Antarctic Program. We would like to express our sincere
thanks for their continuous professional support.
NR 27
TC 43
Z9 43
U1 0
U2 3
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 JAN 31
PY 2012
VL 108
IS 5
AR 051102
DI 10.1103/PhysRevLett.108.051102
PG 5
WC Physics, Multidisciplinary
SC Physics
GA 886DU
UT WOS:000299832900002
PM 22400920
ER
PT J
AU Park, IH
Gangupomu, V
Wagner, J
Jain, A
Vaidehi, N
AF Park, In-Hee
Gangupomu, Vamshi
Wagner, Jeffrey
Jain, Abhinandan
Vaidehi, Nagarajan
TI Structure Refinement of Protein Low Resolution Models using GNEIMO
Constrained Dynamics Method
SO BIOPHYSICAL JOURNAL
LA English
DT Meeting Abstract
CT 56th Annual Meeting of the Biophysical-Society
CY FEB 25-29, 2012
CL San Diego, CA
SP Biophys Soc
C1 [Park, In-Hee; Gangupomu, Vamshi; Wagner, Jeffrey; Vaidehi, Nagarajan] City Hope Natl Med Ctr, Beckman Res Inst, Duarte, CA USA.
[Jain, Abhinandan] CALTECH, Jet Prop Lab, Pasadena, CA USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU CELL PRESS
PI CAMBRIDGE
PA 600 TECHNOLOGY SQUARE, 5TH FLOOR, CAMBRIDGE, MA 02139 USA
SN 0006-3495
J9 BIOPHYS J
JI Biophys. J.
PD JAN 31
PY 2012
VL 102
IS 3
SU 1
BP 25A
EP 25A
PG 1
WC Biophysics
SC Biophysics
GA 179ZF
UT WOS:000321561200124
ER
PT J
AU Moore, JP
Rogge, MD
AF Moore, Jason P.
Rogge, Matthew D.
TI Shape sensing using multi-core fiber optic cable and parametric curve
solutions
SO OPTICS EXPRESS
LA English
DT Article
ID BEND MEASUREMENT; BRAGG GRATINGS
AB The shape of a multi-core optical fiber is calculated by numerically solving a set of Frenet-Serret equations describing the path of the fiber in three dimensions. Included in the Frenet-Serret equations are curvature and bending direction functions derived from distributed fiber Bragg grating strain measurements in each core. The method offers advantages over prior art in that it determines complex three-dimensional fiber shape as a continuous parametric solution rather than an integrated series of discrete planar bends. Results and error analysis of the method using a tri-core optical fiber is presented. Maximum error expressed as a percentage of fiber length was found to be 7.2%. 2012 Optical Society of America
C1 [Moore, Jason P.; Rogge, Matthew D.] NASA Langley Res Ctr, Hampton, VA 23681 USA.
RP Moore, JP (reprint author), NASA Langley Res Ctr, Hampton, VA 23681 USA.
EM jason.p.moore@nasa.gov
NR 10
TC 44
Z9 44
U1 10
U2 31
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD JAN 30
PY 2012
VL 20
IS 3
BP 2967
EP 2973
DI 10.1364/OE.20.002967
PG 7
WC Optics
SC Optics
GA 895ME
UT WOS:000300499500103
PM 22330534
ER
PT J
AU Numata, K
Camp, J
AF Numata, Kenji
Camp, Jordan
TI Estimation of frequency noise in semiconductor lasers due to mechanical
thermal noise
SO PHYSICS LETTERS A
LA English
DT Article
DE Thermal noise; Semiconductor laser
ID 1/F NOISE; DEGRADATION; VCSELS
AB We evaluate mechanical thermal noise in semiconductor lasers, applying a methodology developed for fixed-spacer cavities for laser frequency stabilization. Our simple model determines an underlying fundamental limit for the frequency noise of free-running semiconductor laser, and provides a framework where the noise may be potentially reduced with improved design. (C) 2012 Elsevier B.V. All rights reserved.
C1 [Numata, Kenji; Camp, Jordan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Numata, Kenji] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Numata, K (reprint author), NASA, Goddard Space Flight Ctr, Code 663,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM kenji.numata@nasa.gov
NR 40
TC 0
Z9 1
U1 0
U2 5
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0375-9601
EI 1873-2429
J9 PHYS LETT A
JI Phys. Lett. A
PD JAN 30
PY 2012
VL 376
IS 6-7
BP 798
EP 802
DI 10.1016/j.physleta.2012.01.013
PG 5
WC Physics, Multidisciplinary
SC Physics
GA 904AZ
UT WOS:000301167300003
ER
PT J
AU Slavin, JA
Anderson, BJ
Baker, DN
Benna, M
Boardsen, SA
Gold, RE
Ho, GC
Imber, SM
Korth, H
Krimigis, SM
McNutt, RL
Raines, JM
Sarantos, M
Schriver, D
Solomon, SC
Travnicek, P
Zurbuchen, TH
AF Slavin, James A.
Anderson, Brian J.
Baker, Daniel N.
Benna, Mehdi
Boardsen, Scott A.
Gold, Robert E.
Ho, George C.
Imber, Suzanne M.
Korth, Haje
Krimigis, Stamatios M.
McNutt, Ralph L., Jr.
Raines, Jim M.
Sarantos, Menelaos
Schriver, David
Solomon, Sean C.
Travnicek, Pavel
Zurbuchen, Thomas H.
TI MESSENGER and Mariner 10 flyby observations of magnetotail structure and
dynamics at Mercury
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID STEADY MAGNETOSPHERIC CONVECTION; KELVIN-HELMHOLTZ INSTABILITY; LATITUDE
BOUNDARY-LAYER; SOLAR-WIND INTERACTION; MAGNETIC-FIELD; GEOMAGNETIC
TAIL; GEOTAIL OBSERVATIONS; EARTHS MAGNETOSPHERE; DISTANT MAGNETOTAIL;
NEAR-TAIL
AB The first (M1), second (M2), and third (M3) MESSENGER flybys of Mercury traversed the planet's magnetotail from 1.25 to 3.25 R-M downstream of the planet, where R-M is Mercury's radius (2440 km). The encounters took place under northward, southward, and variable-polarity interplanetary magnetic field (IMF), respectively. The magnetic field strength B in Mercury's magnetotail follows a power law decrease with increasing antisunward distance vertical bar X vertical bar, B similar to vertical bar X vertical bar(G), with G varying from -5.4 for northward to -1.6 for southward IMF. Low-latitude boundary layers (LLBLs) containing strong northward magnetic field were detected at the tail flanks during two of the flybys. The observed thickness of the LLBL was similar to 33% and 16% of the radius of the tail during M1 and M3, respectively, but the boundary layer was completely absent during M2. Clear signatures of tail reconnection are evident in the M2 and M3 magnetic field measurements. Plasmoids and traveling compression regions were observed during M2 and M3 with typical durations of similar to 1-3 s, suggesting diameters of similar to 500-1500 km. Overall, the response of Mercury's magnetotail to the steady southward IMF during M2 appeared very similar to steady magnetospheric convection events at Earth, which are believed to be driven by quasi-continuous reconnection. In contrast, the M3 measurements are dominated by tail loading and unloading events that resemble the large-scale magnetic field reconfigurations observed during magnetospheric substorms at Earth.
C1 [Slavin, James A.; Boardsen, Scott A.; Imber, Suzanne M.; Sarantos, Menelaos] NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD 20771 USA.
[Anderson, Brian J.; Gold, Robert E.; Ho, George C.; Korth, Haje; Krimigis, Stamatios M.; McNutt, Ralph L., Jr.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Baker, Daniel N.] Univ Colorado, Lab Solar & Atmospher Phys, Boulder, CO 80303 USA.
[Benna, Mehdi] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA.
[Boardsen, Scott A.; Imber, Suzanne M.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
[Krimigis, Stamatios M.; Sarantos, Menelaos] Acad Athens, Off Space Res & Technol, Athens, Greece.
[Raines, Jim M.; Zurbuchen, Thomas H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
[Schriver, David] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA.
[Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA.
[Travnicek, Pavel] Acad Sci Czech Republic, Astron Inst, Prague 14131, Czech Republic.
RP Slavin, JA (reprint author), NASA, Goddard Space Flight Ctr, Heliophys Sci Div, Code 670-0,Bldg 21,Greenbelt Rd, Greenbelt, MD 20771 USA.
RI Benna, Mehdi/F-3489-2012; Anderson, Brian/I-8615-2012; Slavin,
James/H-3170-2012; Sarantos, Menelaos/H-8136-2013; McNutt,
Ralph/E-8006-2010; Travnicek, Pavel/G-8608-2014; Ho, George/G-3650-2015
OI Slavin, James/0000-0002-9206-724X; McNutt, Ralph/0000-0002-4722-9166;
Ho, George/0000-0003-1093-2066
FU NASA [NASW-00002, NAS5-97271]
FX Computational assistance and data visualization support provided by J.
Feggans are gratefully acknowledged. We are also pleased to acknowledge
stimulating comments and discussions with V. Uritsky. The MESSENGER
project is supported by the NASA Discovery Program under contracts
NASW-00002 to the Carnegie Institution of Washington and NAS5-97271 to
the Johns Hopkins University Applied Physics Laboratory.
NR 97
TC 36
Z9 36
U1 1
U2 11
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 JAN 28
PY 2012
VL 117
AR A01215
DI 10.1029/2011JA016900
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 884JG
UT WOS:000299700300001
ER
PT J
AU Kim, JW
Nunez, JC
Siochi, EJ
Wise, KE
Lin, Y
Connell, JW
Smith, MW
AF Kim, Jae-Woo
Nunez, Jennifer Carpena
Siochi, Emilie J.
Wise, Kristopher E.
Lin, Yi
Connell, John W.
Smith, Michael W.
TI In situ mechanical property measurements of amorphous carbon-boron
nitride nanotube nanostructures
SO NANOTECHNOLOGY
LA English
DT Article
ID STRENGTH; ELECTRON; MODULUS; BUNDLES; FIBERS
AB To understand the mechanical properties of amorphous carbon (a-C)/boron nitride nanotube (BNNT) nanostructures, in situ mechanical tests are conducted inside a transmission electron microscope equipped with an integrated atomic force microscope system. The nanotube structure is modified with amorphous carbon deposited by controlled electron beam irradiation. We demonstrate multiple in situ tensile, compressive, and lap shear tests with a-C/BNNT hybrid nanostructures. The tensile strength of the a-C/BNNT hybrid nanostructure is 5.29 GPa with about 90 vol% of a-C. The tensile strength and strain of the end-to-end joint structure with a-C welding is 0.8 GPa and 5.2% whereas the lap shear strength of the side-by-side joint structure with a-C is 0.25 GPa.
C1 [Kim, Jae-Woo; Lin, Yi] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Nunez, Jennifer Carpena; Siochi, Emilie J.; Wise, Kristopher E.; Connell, John W.; Smith, Michael W.] NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA.
RP Kim, JW (reprint author), Natl Inst Aerosp, 100 Explorat Way, Hampton, VA 23666 USA.
EM jae-woo.kim-1@nasa.gov
RI Kim, Jae-Woo/A-8314-2008
NR 27
TC 4
Z9 4
U1 0
U2 21
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0957-4484
J9 NANOTECHNOLOGY
JI Nanotechnology
PD JAN 27
PY 2012
VL 23
IS 3
AR 035701
DI 10.1088/0957-4484/23/3/035701
PG 9
WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary;
Physics, Applied
SC Science & Technology - Other Topics; Materials Science; Physics
GA 877HQ
UT WOS:000299168800013
PM 22172920
ER
PT J
AU Welsh, WF
Orosz, JA
Carter, JA
Fabrycky, DC
Ford, EB
Lissauer, JJ
Prsa, A
Quinn, SN
Ragozzine, D
Short, DR
Torres, G
Winn, JN
Doyle, LR
Barclay, T
Batalha, N
Bloemen, S
Brugamyer, E
Buchhave, LA
Caldwell, C
Caldwell, DA
Christiansen, JL
Ciardi, DR
Cochran, WD
Endl, M
Fortney, JJ
Gautier, TN
Gilliland, RL
Haas, MR
Hall, JR
Holman, MJ
Howard, AW
Howell, SB
Isaacson, H
Jenkins, JM
Klaus, TC
Latham, DW
Li, J
Marcy, GW
Mazeh, T
Quintana, EV
Robertson, P
Shporer, A
Steffen, JH
Windmiller, G
Koch, DG
Borucki, WJ
AF Welsh, William F.
Orosz, Jerome A.
Carter, Joshua A.
Fabrycky, Daniel C.
Ford, Eric B.
Lissauer, Jack J.
Prsa, Andrej
Quinn, Samuel N.
Ragozzine, Darin
Short, Donald R.
Torres, Guillermo
Winn, Joshua N.
Doyle, Laurance R.
Barclay, Thomas
Batalha, Natalie
Bloemen, Steven
Brugamyer, Erik
Buchhave, Lars A.
Caldwell, Caroline
Caldwell, Douglas A.
Christiansen, Jessie L.
Ciardi, David R.
Cochran, William D.
Endl, Michael
Fortney, Jonathan J.
Gautier, Thomas N., III
Gilliland, Ronald L.
Haas, Michael R.
Hall, Jennifer R.
Holman, Matthew J.
Howard, Andrew W.
Howell, Steve B.
Isaacson, Howard
Jenkins, Jon M.
Klaus, Todd C.
Latham, David W.
Li, Jie
Marcy, Geoffrey W.
Mazeh, Tsevi
Quintana, Elisa V.
Robertson, Paul
Shporer, Avi
Steffen, Jason H.
Windmiller, Gur
Koch, David G.
Borucki, William J.
TI Transiting circumbinary planets Kepler-34 b and Kepler-35 b
SO NATURE
LA English
DT Article
ID HIERARCHICAL TRIPLE; ECLIPSING BINARIES; DATA RELEASE; STELLAR; STARS;
SYSTEMS; STABILITY; CATALOG
AB Most Sun-like stars in the Galaxy reside in gravitationally bound pairs of stars(1,2) (binaries). Although long anticipated(3-8), the existence of a 'circumbinary planet' orbiting such a pair of normal stars was not definitively established until the discovery(9) of the planet transiting (that is, passing in front of) Kepler-16. Questions remained, however, about the prevalence of circumbinary planets and their range of orbital and physical properties. Here we report two additional transiting circumbinary planets: Kepler-34 (AB)b and Kepler-35 (AB)b, referred to here as Kepler-34 b and Kepler-35 b, respectively. Each is a low-density gas-giant planet on an orbit closely aligned with that of its parent stars. Kepler-34 b orbits two Sun-like stars every 289 days, whereas Kepler-35 b orbits a pair of smaller stars (89% and 81% of the Sun's mass) every 131 days. The planets experience large multi-periodic variations in incident stellar radiation arising from the orbital motion of the stars. The observed rate of circumbinary planets in our sample implies that more than similar to 1% of close binary stars have giant planets in nearly coplanar orbits, yielding a Galactic population of at least several million.
C1 [Welsh, William F.; Orosz, Jerome A.; Short, Donald R.; Windmiller, Gur] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Fabrycky, Daniel C.] Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA.
[Ford, Eric B.] Univ Florida, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA.
[Lissauer, Jack J.; Barclay, Thomas; Batalha, Natalie; Christiansen, Jessie L.; Haas, Michael R.; Howell, Steve B.; Jenkins, Jon M.; Li, Jie; Quintana, Elisa V.; Koch, David G.; Borucki, William J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Carter, Joshua A.; Quinn, Samuel N.; Ragozzine, Darin; Torres, Guillermo; Holman, Matthew J.; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Prsa, Andrej] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA.
[Quinn, Samuel N.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA.
[Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Doyle, Laurance R.; Caldwell, Douglas A.; Christiansen, Jessie L.; Jenkins, Jon M.; Li, Jie; Quintana, Elisa V.] SETI Inst, Carl Sagan Ctr Study Life Universe, Mountain View, CA 94043 USA.
[Barclay, Thomas] Bay Area Environm Res Inst Inc, Sonoma, CA 95476 USA.
[Batalha, Natalie] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
[Bloemen, Steven] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark.
[Brugamyer, Erik; Cochran, William D.; Endl, Michael] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Ciardi, David R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Gautier, Thomas N., III] Jet Prop Lab, Pasadena, CA 91109 USA.
[Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Klaus, Todd C.] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Mazeh, Tsevi] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Shporer, Avi] Las Cumbres Observ, Global Telescope Network, Santa Barbara, CA 93117 USA.
[Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA.
RP Welsh, WF (reprint author), San Diego State Univ, Dept Astron, 5500 Campanile Dr, San Diego, CA 92182 USA.
EM wfw@sciences.sdsu.edu; jacarter@cfa.harvard.edu
RI Steffen, Jason/A-4320-2013; Carter, Joshua/A-8280-2013; Ragozzine,
Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014; Howard,
Andrew/D-4148-2015;
OI Caldwell, Douglas/0000-0003-1963-9616; Howard,
Andrew/0000-0001-8638-0320; Fortney, Jonathan/0000-0002-9843-4354;
Buchhave, Lars A./0000-0003-1605-5666; Ciardi,
David/0000-0002-5741-3047; Barclay, Thomas/0000-0001-7139-2724;
Fabrycky, Daniel/0000-0003-3750-0183
FU NASA's Science Mission Directorate; Kepler Participating Scientist
Program; NSF; NASA; STScI; European Research Council under the European
Community; Research Council of KU Leuven; FAS Science Division Research
Computing Group at Harvard University
FX Kepler was selected as the tenth NASA Discovery mission with funding
provided by NASA's Science Mission Directorate. We thank the many people
who made the Kepler mission a reality. W. F. W., J.A.O., E. B. F., A.
P., L. R. D., J.J.F., M.J.H., T. M. and J.H.S. were supported by the
Kepler Participating Scientist Program. W. F. W., J.A.O., D. R. S. and
G. W. were supported by the NSF. D. C. F. and J.A.C. acknowledge NASA
support through Hubble Fellowship grants, awarded by STScI, operated by
AURA. J.N.W. was supported by the NASA Origins programme. S. B.
acknowledges funding from the European Research Council under the
European Community's Seventh Framework Programme (PROSPERITY) and from
the Research Council of KU Leuven. Some of the reported computations
were run on the Odyssey cluster supported by the FAS Science Division
Research Computing Group at Harvard University. This Letter is based in
part on observations made with the Nordic Optical Telescope (operated on
the island of La Palma jointly by Denmark, Finland, Iceland, Norway and
Sweden, in the Spanish Observatorio del Roque de los Muchachos of the
Instituto de Astrofisica de Canarias), the W. M. Keck Observatory
(operated by the University of California and the California Institute
of Technology) and the Hobby-Eberly Telescope (HET; a joint project of
the University of Texas at Austin, the Pennsylvania State University,
Stanford University, Ludwig-Maximillians-Universitat Munchen, and
Georg-August-Universitat Goettingen).
NR 22
TC 200
Z9 201
U1 1
U2 17
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD JAN 26
PY 2012
VL 481
IS 7382
BP 475
EP U85
DI 10.1038/nature10768
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 881GY
UT WOS:000299471800033
PM 22237021
ER
PT J
AU Trattner, KJ
Petrinec, SM
Fuselier, SA
Omidi, N
Sibeck, DG
AF Trattner, K. J.
Petrinec, S. M.
Fuselier, S. A.
Omidi, N.
Sibeck, D. G.
TI Evidence of multiple reconnection lines at the magnetopause from cusp
observations
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID FLUX-TRANSFER EVENTS; LOW-ALTITUDE OBSERVATIONS; SHEET BOUNDARY-LAYER;
HIGH-LATITUDE; DAYSIDE RECONNECTION; MAGNETIC-FIELD; MAGNETOSPHERIC
CUSP; QUANTITATIVE MODEL; NORTHWARD IMF; ION OUTFLOW
AB Recent global hybrid simulations investigated the formation of flux transfer events (FTEs) and their convection and interaction with the cusp. Based on these simulations, we have analyzed several Polar cusp crossings in the Northern Hemisphere to search for the signature of such FTEs in the energy distribution of downward precipitating ions: precipitating ion beams at different energies parallel to the ambient magnetic field and overlapping in time. Overlapping ion distributions in the cusp are usually attributed to a combination of variable ion acceleration during the magnetopause crossing together with the time-of-flight effect from the entry point to the observing satellite. Most "step up" ion cusp structures (steps in the ion energy dispersions) only overlap for the populations with large pitch angles and not for the parallel streaming populations. Such cusp structures are the signatures predicted by the pulsed reconnection model, where the reconnection rate at the magnetopause decreased to zero, physically separating convecting flux tubes and their parallel streaming ions. However, several Polar cusp events discussed in this study also show an energy overlap for parallel-streaming precipitating ions. This condition might be caused by reopening an already reconnected field line, forming a magnetic island (flux rope) at the magnetopause similar to that reported in global MHD and Hybrid simulations.
C1 [Trattner, K. J.; Petrinec, S. M.; Fuselier, S. A.] Lockheed Martin Space Syst Co, Adv Technol Ctr, Palo Alto, CA 94304 USA.
[Omidi, N.] Solana Sci Inc, Solana Beach, CA 92075 USA.
[Sibeck, D. G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Trattner, KJ (reprint author), Lockheed Martin Space Syst Co, Adv Technol Ctr, 3251 Hanover St,Bldg B255,A022S, Palo Alto, CA 94304 USA.
EM karlheinz.j.trattner.dr@lmco.com
RI Sibeck, David/D-4424-2012
FU NASA [NNX08AF35G, NNX09AM72G, NNX11AJ09G, NNG05GE15G]; NSF [AGS-1007449]
FX We acknowledge the use of the ISTP KP database. Solar wind observations
were provided by the Wind Solar Wind Experiment (Wind/SWE) [Ogilvie et
al., 1995]. The IMF measurements were provided by the Wind Magnetic
Field Instrument (Wind/MFI) [Lepping et al., 1995]. The work at Lockheed
Martin was supported by NASA contracts NNX08AF35G, NNX09AM72G,
NNX11AJ09G, and NNG05GE15G. N. Omidi acknowledges support from NSF grant
AGS-1007449.
NR 61
TC 4
Z9 4
U1 0
U2 6
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 JAN 25
PY 2012
VL 117
AR A01213
DI 10.1029/2011JA017080
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 884IV
UT WOS:000299699000002
ER
PT J
AU Macedo, MN
DeFries, RS
Morton, DC
Stickler, CM
Galford, GL
Shimabukuro, YE
AF Macedo, Marcia N.
DeFries, Ruth S.
Morton, Douglas C.
Stickler, Claudia M.
Galford, Gillian L.
Shimabukuro, Yosio E.
TI Decoupling of deforestation and soy production in the southern Amazon
during the late 2000s
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE agriculture; land sparing; extensification; Brazilian Amazon
ID LAND-USE CHANGE; BRAZILIAN AMAZON; AGRICULTURAL INTENSIFICATION;
FORESTS; CONSEQUENCES; CONSERVATION; EXPANSION; REDD
AB From 2006 to 2010, deforestation in the Amazon frontier state of Mato Grosso decreased to 30% of its historical average (1996-2005) whereas agricultural production reached an all-time high. This study combines satellite data with government deforestation and production statistics to assess land-use transitions and potential market and policy drivers associated with these trends. In the forested region of the state, increased soy production from 2001 to 2005 was entirely due to cropland expansion into previously cleared pasture areas (74%) or forests (26%). From 2006 to 2010, 78% of production increases were due to expansion (22% to yield increases), with 91% on previously cleared land. Cropland expansion fell from 10 to 2% of deforestation between the two periods, with pasture expansion accounting for most remaining deforestation. Declining deforestation coincided with a collapse of commodity markets and implementation of policy measures to reduce deforestation. Soybean profitability has since increased to pre-2006 levels whereas deforestation continued to decline, suggesting that antideforestation measures may have influenced the agricultural sector. We found little evidence of direct leakage of soy expansion into cerrado in Mato Grosso during the late 2000s, although indirect land-use changes and leakage to more distant regions are possible. This study provides evidence that reduced deforestation and increased agricultural production can occur simultaneously in tropical forest frontiers, provided that land is available and policies promote the efficient use of already-cleared lands (intensification) while restricting deforestation. It remains uncertain whether government- and industry-led policies can contain deforestation if future market conditions favor another boom in agricultural expansion.
C1 [Macedo, Marcia N.; DeFries, Ruth S.] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA.
[Morton, Douglas C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Galford, Gillian L.] Woods Hole Res Ctr, Falmouth, MA 02540 USA.
[Stickler, Claudia M.] Inst Pesquisa Ambiental Amazonia, BR-71503505 Brasilia, DF, Brazil.
[Shimabukuro, Yosio E.] Inst Nacl Pesquisas Espaciais, Div Sensoriamento Remoto, BR-12227010 Sao Jose Dos Campos, SP, Brazil.
RP DeFries, RS (reprint author), Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA.
EM rd2402@columbia.edu
RI Morton, Douglas/D-5044-2012; Galford, Gillian/K-6240-2012
OI Galford, Gillian/0000-0003-2192-7385
FU National Aeronautics and Space Administration [NNX08AX08H]; Gordon and
Betty Moore Foundation; Packard Foundation; National Science Foundation
[DEB-0949996, DEB-0743703]
FX This manuscript was greatly improved by the constructive comments of
Arild Angelsen, Paulo Brando, Victor Gutierrez-Velez, Ramon Lopez, and
two anonymous reviewers. We thank Michael Coe, Christopher Neill, and
the Instituto de Pesquisa Ambiental da Amazonia for logistical support
in the field; and Rebecca de Sa and Darlisson Nunes da Costa for
assistance with data collection. This work was funded by National
Aeronautics and Space Administration Earth System Science Fellowship
NNX08AX08H, The Gordon and Betty Moore Foundation, the Packard
Foundation, and National Science Foundation Grants DEB-0949996 and
DEB-0743703.
NR 42
TC 159
Z9 163
U1 10
U2 122
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD JAN 24
PY 2012
VL 109
IS 4
BP 1341
EP 1346
DI 10.1073/pnas.1111374109
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 880NA
UT WOS:000299412600068
PM 22232692
ER
PT J
AU Fritts, DC
Janches, D
Iimura, H
Hocking, WK
Bageston, JV
Leme, NMP
AF Fritts, D. C.
Janches, D.
Iimura, H.
Hocking, W. K.
Bageston, J. V.
Leme, N. M. P.
TI Drake Antarctic Agile Meteor Radar first results: Configuration and
comparison of mean and tidal wind and gravity wave momentum flux
measurements with Southern Argentina Agile Meteor Radar
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID DIURNAL PROPAGATING TIDE; LATENT-HEAT RELEASE; AMSU-A RADIANCES;
JUNE-AUGUST 1999; LOWER THERMOSPHERE; PLANETARY-WAVES; MIDDLE
ATMOSPHERE; POKER FLAT; MU RADAR; INTERANNUAL VARIABILITY
AB A new generation meteor radar was installed at the Brazilian Antarctic Comandante Ferraz Base (62.1 degrees S) in March 2010. This paper describes the motivations for the radar location, its measurement capabilities, and comparisons of measured mean winds, tides, and gravity wave momentum fluxes from April to June of 2010 and 2011 with those by a similar radar on Tierra del Fuego (53.8 degrees S). Motivations for the radars include the "hotspot" of small-scale gravity wave activity extending from the troposphere into the mesosphere and lower thermosphere (MLT) centered over the Drake Passage, the maximum of the semidiurnal tide at these latitudes, and the lack of other MLT wind measurements in this latitude band. Mean winds are seen to be strongly modulated at planetary wave and longer periods and to exhibit strong coherence over the two radars at shorter time scales as well as systematic seasonal variations. The semidiurnal tide contributes most to the large-scale winds over both radars, with maximum tidal amplitudes during May and maxima at the highest altitudes varying from similar to 20 to >70 ms(-1). In contrast, the diurnal tide and various planetary waves achieve maximum winds of similar to 10 to 20 ms(-1). Monthly mean gravity wave momentum fluxes appear to reflect the occurrence of significant sources at lower altitudes, with relatively small zonal fluxes over both radars, but with significant, and opposite, meridional momentum fluxes below similar to 85 km. These suggest gravity waves propagating away from the Drake Passage at both sites, and may indicate an important source region accounting in part for this "hotspot."
C1 [Fritts, D. C.; Iimura, H.] NW Res Associates, Colorado Res Associates Div, Boulder, CO USA.
[Janches, D.] NASA, Goddard Space Flight Ctr, Space Weather Lab, Greenbelt, MD 20771 USA.
[Bageston, J. V.; Leme, N. M. P.] Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, SP, Brazil.
[Hocking, W. K.] Univ Western Ontario, Dept Phys, London, ON N6A 3K7, Canada.
RP Fritts, DC (reprint author), NW Res Associates, Colorado Res Associates Div, 3380 Mitchell Ln, Boulder, CO USA.
EM dave@cora.nwra.com
RI Janches, Diego/D-4674-2012
OI Janches, Diego/0000-0001-8615-5166
FU NSF [OPP-0839084, ATM-0634650]; Secretaria for the Interministerial
Commission of Sea Resources (SECIRM); Brazilian Antarctic Program
(PROANTAR); National Institute for Science and Technology; Antarctic
Environmental Research (INCT-APA); ATMANTAR/MCT/CNPq, FAPERJ; FAPESP
[2010/06608-2]
FX Research described in this paper was performed under NSF grants
OPP-0839084 and ATM-0634650. We are especially grateful to the
Secretaria for the Interministerial Commission of Sea Resources
(SECIRM), the Brazilian Antarctic Program (PROANTAR), the National
Institute for Science and Technology, Antarctic Environmental Research
(INCT-APA), and the ATMANTAR/MCT/CNPq project, FAPERJ, for their support
of this research and visits to Ferraz Station to install and service
DrAAMER. We are also very grateful for the valuable assistance of
personnel at Estacion Astronomica Rio Grande (EARG) with the operations
and maintenance of SAAMER. J. V. Bageston thanks FAPESP for his
postdoctorate fellowship under the process number 2010/06608-2. Finally,
we are indebted to MARDOC and Genesis Software for working with us to
devise a radar configuration that met our measurement objectives. We
also acknowledge use of the CEDAR database and the GSWM-09 website at
NCAR for GSWM-09 results employed for our comparisons.
NR 71
TC 13
Z9 13
U1 0
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 21
PY 2012
VL 117
AR D02105
DI 10.1029/2011JD016651
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 880FN
UT WOS:000299390400002
ER
PT J
AU Wood, EF
Roundy, JK
Troy, TJ
van Beek, R
Bierkens, M
Blyth, E
de Roo, A
Doll, P
Ek, M
Famiglietti, J
Gochis, D
van de Giesen, N
Houser, P
Jaffe, P
Kollet, S
Lehner, B
Lettenmaier, DP
Peters-Lidard, CD
Sivapalan, M
Sheffield, J
Wade, AJ
Whitehead, P
AF Wood, Eric F.
Roundy, Joshua K.
Troy, Tara J.
van Beek, Rens
Bierkens, Marc
Blyth, Eleanor
de Roo, Ad
Doell, Petra
Ek, Mike
Famiglietti, James
Gochis, David
van de Giesen, Nick
Houser, Paul
Jaffe, Peter
Kollet, Stefan
Lehner, Bernhard
Lettenmaier, Dennis P.
Peters-Lidard, Christa D.
Sivapalan, Murugesu
Sheffield, Justin
Wade, Andrew J.
Whitehead, Paul
TI Reply to comment by Keith J. Beven and Hannah L. Cloke on
"Hyperresolution global land surface modeling: Meeting a grand challenge
for monitoring Earth's terrestrial water''
SO WATER RESOURCES RESEARCH
LA English
DT Editorial Material
C1 [Wood, Eric F.; Roundy, Joshua K.; Troy, Tara J.; Jaffe, Peter; Sheffield, Justin] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA.
[van Beek, Rens; Bierkens, Marc] Univ Utrecht, Dept Phys Geog, NL-3508 TC Utrecht, Netherlands.
[Blyth, Eleanor] Ctr Ecol & Hydrol, Wallingford OX10 8BB, Oxon, England.
[de Roo, Ad] European Commiss Joint Res Ctr, Inst Environm & Sustainabil, I-21027 Ispra, Italy.
[Doell, Petra] Goethe Univ Frankfurt, Inst Phys Geog, D-60054 Frankfurt, Germany.
[Ek, Mike] Natl Ctr Environm Protect, Environm Modeling Ctr, Suitland, MD USA.
[Famiglietti, James] Univ Calif Irvine, UC Ctr Hydrol Modeling, Irvine, CA 92697 USA.
[Gochis, David] Natl Ctr Atmospher Res, Res Applicat Lab, Boulder, CO 80304 USA.
[van de Giesen, Nick] Delft Univ Technol, Dept Water Management, NL-2628 CN Delft, Netherlands.
[Houser, Paul] George Mason Univ, Dept Geog & GeoInformat Sci, Fairfax, VA 22030 USA.
[Kollet, Stefan] Univ Bonn, Inst Meteorol, D-53121 Bonn, Germany.
[Lehner, Bernhard] McGill Univ, Dept Geog, Montreal, PQ H3A 2K6, Canada.
[Lettenmaier, Dennis P.] Univ Washington, Dept Civil & Environm Engn, Seattle, WA 98195 USA.
[Peters-Lidard, Christa D.] NASA, Hydrol Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Sivapalan, Murugesu] Univ Illinois, Dept Civil & Environm Engn, Urbana, IL 61801 USA.
[Sivapalan, Murugesu] Univ Illinois, Dept Geog, Urbana, IL 61801 USA.
[Wade, Andrew J.] Univ Reading, Sch Human & Environm Sci, Reading RG6 6DW, Berks, England.
[Whitehead, Paul] Univ Oxford, Sch Geog & Environm, Oxford OX1 3QY, England.
RP Wood, EF (reprint author), Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA.
EM efwood@princeton.edu
RI Doll, Petra/A-3784-2009; Sivapalan, Murugesu/A-3538-2008; Blyth,
Eleanor/A-4010-2009; van de Giesen, Nick/B-5010-2008; Houser,
Paul/J-9515-2013; lettenmaier, dennis/F-8780-2011; Peters-Lidard,
Christa/E-1429-2012; Roundy, Joshua/H-9377-2016; van Beek,
Rens/B-4904-2014;
OI Doll, Petra/0000-0003-2238-4546; Sivapalan,
Murugesu/0000-0003-3004-3530; van de Giesen, Nick/0000-0002-7200-3353;
Houser, Paul/0000-0002-2991-0441; lettenmaier,
dennis/0000-0003-3317-1327; Peters-Lidard, Christa/0000-0003-1255-2876;
Roundy, Joshua/0000-0003-0328-3248; van Beek, Rens/0000-0002-4758-108X;
Troy, Tara/0000-0001-5366-0633; Wade, Andrew/0000-0002-5296-8350
NR 13
TC 9
Z9 9
U1 3
U2 42
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0043-1397
EI 1944-7973
J9 WATER RESOUR RES
JI Water Resour. Res.
PD JAN 21
PY 2012
VL 48
AR W01802
DI 10.1029/2011WR011202
PG 3
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA 880DV
UT WOS:000299385800004
ER
PT J
AU Abbasi, R
Abdou, Y
Abu-Zayyad, T
Adams, J
Aguilar, JA
Ahlers, M
Altmann, D
Andeen, K
Auffenberg, J
Bai, X
Baker, M
Barwick, SW
Bay, R
Alba, JLB
Beattie, K
Beatty, JJ
Bechet, S
Becker, JK
Becker, KH
Benabderrahmane, ML
BenZvi, S
Berdermann, J
Berghaus, P
Berley, D
Bernardini, E
Bertrand, D
Besson, DZ
Bindig, D
Bissok, M
Blaufuss, E
Blumenthal, J
Boersma, DJ
Bohm, C
Bose, D
Boser, S
Botner, O
Brown, AM
Buitink, S
Caballero-Mora, KS
Carson, M
Chirkin, D
Christy, B
Clem, J
Clevermann, F
Cohen, S
Colnard, C
Cowen, DF
D'Agostino, MV
Danninger, M
Daughhetee, J
Davis, JC
De Clercq, C
Demirors, L
Denger, T
Depaepe, O
Descamps, F
Desiati, P
de Vries-Uiterweerd, G
DeYoung, T
Diaz-Velez, JC
Dierckxsens, M
Dreyer, J
Dumm, JP
Ehrlich, R
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
Foerster, MM
Fox, BD
Franckowiak, A
Franke, R
Gaisser, TK
Gallagher, J
Gerhardt, L
Gladstone, L
Glusenkamp, T
Goldschmidt, A
Goodman, JA
Gora, D
Grant, D
Griesel, T
Gross, A
Grullon, S
Gurtner, M
Ha, C
Hajismail, A
Hallgren, A
Halzen, F
Han, K
Hanson, K
Heinen, D
Helbing, K
Herquet, P
Hickford, S
Hill, GC
Hoffman, KD
Homeier, A
Hoshina, K
Hubert, D
Huelsnitz, W
Hulss, JP
Hulth, PO
Hultqvist, K
Hussain, S
Ishihara, A
Jacobsen, J
Japaridze, GS
Johansson, H
Joseph, JM
Kampert, KH
Kappes, A
Karg, T
Karle, A
Kenny, P
Kiryluk, J
Kislat, F
Klein, SR
Kohne, JH
Kohnen, G
Kolanoski, H
Kopke, L
Kopper, S
Koskinen, DJ
Kowalski, M
Kowarik, T
Krasberg, M
Krings, T
Kroll, G
Kurahashi, N
Kuwabara, T
Labare, M
Lafebre, S
Laihem, K
Landsman, H
Larson, MJ
Lauer, R
Lunemann, J
Madsen, J
Majumdar, P
Marotta, A
Maruyama, R
Mase, K
Matis, HS
Meagher, K
Merck, M
Meszaros, P
Meures, T
Middell, E
Milke, N
Miller, J
Montaruli, T
Morse, R
Movit, SM
Nahnhauer, R
Nam, JW
Naumann, U
Niessen, P
Nygren, DR
Odrowski, S
Olivas, A
Olivo, M
O'Murchadha, A
Ono, M
Panknin, S
Paul, L
de los Heros, CP
Petrovic, J
Piegsa, A
Pieloth, D
Porrata, R
Posselt, J
Price, PB
Przybylski, GT
Rawlins, K
Redl, P
Resconi, E
Rhode, W
Ribordy, M
Rizzo, A
Rodrigues, JP
Roth, P
Rothmaier, F
Rott, C
Ruhe, T
Rutledge, D
Ruzybayev, B
Ryckbosch, D
Sander, HG
Santander, M
Sarkar, S
Schatto, K
Schmidt, T
Schonwald, A
Schukraft, A
Schultes, A
Schulz, O
Schunck, M
Seckel, D
Semburg, B
Seo, SH
Sestayo, Y
Seunarine, S
Silvestri, A
Slipak, A
Spiczak, GM
Spiering, C
Stamatikos, M
Stanev, T
Stephens, G
Stezelberger, T
Stokstad, RG
Stossl, A
Stoyanov, S
Strahler, EA
Straszheim, T
Stur, M
Sullivan, GW
Swillens, Q
Taavola, H
Taboada, I
Tamburro, A
Tepe, A
Ter-Antonyan, S
Tilav, S
Toale, PA
Toscano, S
Tosi, D
Turcan, D
van Eijndhoven, N
Vandenbroucke, J
Van Overloop, A
van Santen, J
Vehring, M
Voge, M
Walck, C
Waldenmaier, T
Wallraff, M
Walter, M
Weaver, C
Wendt, C
Westerhoff, S
Whitehorn, N
Wiebe, K
Wiebusch, CH
Williams, DR
Wischnewski, R
Wissing, H
Wolf, M
Wood, TR
Woschnagg, K
Xu, C
Xu, XW
Yodh, G
Yoshida, S
Zarzhitsky, P
Zoll, M
AF Abbasi, R.
Abdou, Y.
Abu-Zayyad, T.
Adams, J.
Aguilar, J. A.
Ahlers, M.
Altmann, D.
Andeen, K.
Auffenberg, J.
Bai, X.
Baker, M.
Barwick, S. W.
Bay, R.
Alba, J. L. Bazo
Beattie, K.
Beatty, J. J.
Bechet, S.
Becker, J. K.
Becker, K. -H.
Benabderrahmane, M. L.
BenZvi, S.
Berdermann, J.
Berghaus, P.
Berley, D.
Bernardini, E.
Bertrand, D.
Besson, D. Z.
Bindig, D.
Bissok, M.
Blaufuss, E.
Blumenthal, J.
Boersma, D. J.
Bohm, C.
Bose, D.
Boeser, S.
Botner, O.
Brown, A. M.
Buitink, S.
Caballero-Mora, K. S.
Carson, M.
Chirkin, D.
Christy, B.
Clem, J.
Clevermann, F.
Cohen, S.
Colnard, C.
Cowen, D. F.
D'Agostino, M. V.
Danninger, M.
Daughhetee, J.
Davis, J. C.
De Clercq, C.
Demiroers, L.
Denger, T.
Depaepe, O.
Descamps, F.
Desiati, P.
de Vries-Uiterweerd, G.
DeYoung, T.
Diaz-Velez, J. C.
Dierckxsens, M.
Dreyer, J.
Dumm, J. P.
Ehrlich, R.
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.
Foerster, M. M.
Fox, B. D.
Franckowiak, A.
Franke, R.
Gaisser, T. K.
Gallagher, J.
Gerhardt, L.
Gladstone, L.
Gluesenkamp, T.
Goldschmidt, A.
Goodman, J. A.
Gora, D.
Grant, D.
Griesel, T.
Gross, A.
Grullon, S.
Gurtner, M.
Ha, C.
Hajismail, A.
Hallgren, A.
Halzen, F.
Han, K.
Hanson, K.
Heinen, D.
Helbing, K.
Herquet, P.
Hickford, S.
Hill, G. C.
Hoffman, K. D.
Homeier, A.
Hoshina, K.
Hubert, D.
Huelsnitz, W.
Huelss, J. -P.
Hulth, P. O.
Hultqvist, K.
Hussain, S.
Ishihara, A.
Jacobsen, J.
Japaridze, G. S.
Johansson, H.
Joseph, J. M.
Kampert, K. -H.
Kappes, A.
Karg, T.
Karle, A.
Kenny, P.
Kiryluk, J.
Kislat, F.
Klein, S. R.
Koehne, J. -H.
Kohnen, G.
Kolanoski, H.
Koepke, L.
Kopper, S.
Koskinen, D. J.
Kowalski, M.
Kowarik, T.
Krasberg, M.
Krings, T.
Kroll, G.
Kurahashi, N.
Kuwabara, T.
Labare, M.
Lafebre, S.
Laihem, K.
Landsman, H.
Larson, M. J.
Lauer, R.
Luenemann, J.
Madsen, J.
Majumdar, P.
Marotta, A.
Maruyama, R.
Mase, K.
Matis, H. S.
Meagher, K.
Merck, M.
Meszaros, P.
Meures, T.
Middell, E.
Milke, N.
Miller, J.
Montaruli, T.
Morse, R.
Movit, S. M.
Nahnhauer, R.
Nam, J. W.
Naumann, U.
Niessen, P.
Nygren, D. R.
Odrowski, S.
Olivas, A.
Olivo, M.
O'Murchadha, A.
Ono, M.
Panknin, S.
Paul, L.
de los Heros, C. Perez
Petrovic, J.
Piegsa, A.
Pieloth, D.
Porrata, R.
Posselt, J.
Price, P. B.
Przybylski, G. T.
Rawlins, K.
Redl, P.
Resconi, E.
Rhode, W.
Ribordy, M.
Rizzo, A.
Rodrigues, J. P.
Roth, P.
Rothmaier, F.
Rott, C.
Ruhe, T.
Rutledge, D.
Ruzybayev, B.
Ryckbosch, D.
Sander, H. -G.
Santander, M.
Sarkar, S.
Schatto, K.
Schmidt, T.
Schoenwald, A.
Schukraft, A.
Schultes, A.
Schulz, O.
Schunck, M.
Seckel, D.
Semburg, B.
Seo, S. H.
Sestayo, Y.
Seunarine, S.
Silvestri, A.
Slipak, A.
Spiczak, G. M.
Spiering, C.
Stamatikos, M.
Stanev, T.
Stephens, G.
Stezelberger, T.
Stokstad, R. G.
Stoessl, A.
Stoyanov, S.
Strahler, E. A.
Straszheim, T.
Stuer, M.
Sullivan, G. W.
Swillens, Q.
Taavola, H.
Taboada, I.
Tamburro, A.
Tepe, A.
Ter-Antonyan, S.
Tilav, S.
Toale, P. A.
Toscano, S.
Tosi, D.
Turcan, D.
van Eijndhoven, N.
Vandenbroucke, J.
Van Overloop, A.
van Santen, J.
Vehring, M.
Voge, M.
Walck, C.
Waldenmaier, T.
Wallraff, M.
Walter, M.
Weaver, Ch.
Wendt, C.
Westerhoff, S.
Whitehorn, N.
Wiebe, K.
Wiebusch, C. H.
Williams, D. R.
Wischnewski, R.
Wissing, H.
Wolf, M.
Wood, T. R.
Woschnagg, K.
Xu, C.
Xu, X. W.
Yodh, G.
Yoshida, S.
Zarzhitsky, P.
Zoll, M.
TI NEUTRINO ANALYSIS OF THE 2010 SEPTEMBER CRAB NEBULA FLARE AND
TIME-INTEGRATED CONSTRAINTS ON NEUTRINO EMISSION FROM THE CRAB USING
ICECUBE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma rays: general; ISM: supernova remnants; neutrinos; pulsars:
individual (Crab Pulsar)
ID HIGH-ENERGY NEUTRINOS; GAMMA-RAY FLARES; PULSAR WINDS; TELESCOPES;
SIGNALS; SYSTEM
AB We present the results of a search for high-energy muon neutrinos with the IceCube detector in coincidence with the Crab Nebula flare reported on 2010 September by various experiments. Due to the unusual flaring state of the otherwise steady source we performed a prompt analysis of the 79-string configuration data to search for neutrinos that might be emitted along with the observed. gamma-rays. We performed two different and complementary data selections of neutrino events in the time window of 10 days around the flare. One event selection is optimized for discovery of E-upsilon(2). neutrino spectrum typical of first-order Fermi acceleration. A similar event selection has also been applied to the 40-string data to derive the time-integrated limits to the neutrino emission from the Crab. The other event selection was optimized for discovery of neutrino spectra with softer spectral index and TeV energy cutoffs as observed for various Galactic sources in. gamma-rays. The 90% confidence level (CL) best upper limits on the Crab flux during the 10 day flare are 4.73 x 10(-11) cm(-2) s(-1) TeV-1 for an E-upsilon(2). neutrino spectrum and 2.50 x 10(-10) cm(-2) s(-1) TeV-1 for a softer neutrino spectra of E-upsilon(-2.7), as indicated by Fermi measurements during the flare. In this paper, we also illustrate the impact of the time-integrated limit on the Crab neutrino steady emission. The limit obtained using 375.5 days of the 40-string configuration is compared to existing models of neutrino production from the Crab and its impact on astrophysical parameters is discussed. The most optimistic predictions of some models are already rejected by the IceCube neutrino telescope with more than 90% CL.
C1 [Abbasi, R.; Aguilar, J. A.; Andeen, K.; Baker, M.; BenZvi, S.; Chirkin, D.; Desiati, P.; Diaz-Velez, J. C.; Dumm, J. P.; Eisch, J.; Feintzeig, J.; Gladstone, L.; Grullon, S.; Halzen, F.; Hanson, K.; Hill, G. C.; Hoshina, K.; Jacobsen, J.; Karle, A.; Krasberg, M.; Kurahashi, N.; Landsman, H.; Maruyama, R.; Merck, M.; Montaruli, T.; Morse, R.; O'Murchadha, A.; Rodrigues, J. P.; Santander, M.; Toscano, S.; van Santen, J.; Weaver, Ch.; Wendt, C.; Westerhoff, S.; Whitehorn, N.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Abdou, Y.; Carson, M.; Descamps, F.; de Vries-Uiterweerd, G.; Feusels, T.; Hajismail, A.; Ryckbosch, D.; Van Overloop, A.] Univ Ghent, Dept Phys & Astron, B-9000 Ghent, Belgium.
[Abu-Zayyad, T.; Madsen, J.; Spiczak, G. M.; Tamburro, A.] Univ Wisconsin, Dept Phys, River Falls, WI 54022 USA.
[Adams, J.; Brown, A. M.; Gross, A.; Hickford, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand.
[Ahlers, M.; Sarkar, S.] Univ Oxford, Dept Phys, Oxford OX1 3NP, England.
[Altmann, D.; Bissok, M.; Blumenthal, J.; Boersma, D. J.; Euler, S.; Gluesenkamp, T.; Heinen, D.; Huelss, J. -P.; Krings, T.; Laihem, K.; Paul, L.; Schukraft, A.; Schunck, M.; Vehring, M.; Wallraff, M.; Wiebusch, C. H.] Rhein Westfal TH Aachen, Inst Phys 3, D-52056 Aachen, Germany.
[Auffenberg, J.; Becker, K. -H.; Bindig, D.; Fischer-Wasels, T.; Gurtner, M.; Helbing, K.; Kampert, K. -H.; Karg, T.; Kopper, S.; Naumann, U.; Posselt, J.; Schultes, A.; Semburg, B.] Univ Wuppertal, Dept Phys, D-42119 Wuppertal, Germany.
[Bai, X.; Berghaus, P.; Clem, J.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Niessen, P.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Stoyanov, S.; Tilav, S.; Xu, C.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Bai, X.; Berghaus, P.; Clem, J.; Evenson, P. A.; Gaisser, T. K.; Hussain, S.; Kuwabara, T.; Niessen, P.; Ruzybayev, B.; Seckel, D.; Stanev, T.; Stoyanov, S.; Tilav, S.; Xu, C.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Barwick, S. W.; Nam, J. W.; Silvestri, A.; Yodh, G.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Bay, R.; D'Agostino, M. V.; Filimonov, K.; Gerhardt, L.; Kiryluk, J.; Klein, S. R.; Porrata, R.; Price, P. B.; Vandenbroucke, J.; Woschnagg, K.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Alba, J. L. Bazo; Benabderrahmane, M. L.; Berdermann, J.; Bernardini, E.; Franke, R.; Gora, D.; Han, K.; Kislat, F.; Lauer, R.; Majumdar, P.; Middell, E.; Nahnhauer, R.; Schoenwald, A.; Spiering, C.; Stoessl, A.; Tosi, D.; Walter, M.; Wischnewski, R.] DESY, D-15735 Zeuthen, Germany.
[Beattie, K.; Gerhardt, L.; Goldschmidt, A.; Joseph, J. M.; Kiryluk, J.; Klein, S. R.; Matis, H. S.; Nygren, D. R.; Przybylski, G. T.; Stezelberger, T.; Stokstad, R. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Beatty, J. J.; Davis, J. C.; Rott, C.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Beatty, J. J.; Davis, J. 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.
[Bechet, S.; Bertrand, D.; Dierckxsens, M.; Hanson, K.; Marotta, A.; Meures, T.; Petrovic, J.; Swillens, Q.] Univ Libre Bruxelles, Sci Fac CP230, B-1050 Brussels, Belgium.
[Becker, J. K.; Dreyer, J.; Fedynitch, A.; Olivo, M.] Ruhr Univ Bochum, Fak Phys & Astron, D-44780 Bochum, Germany.
[Berley, D.; Blaufuss, E.; Christy, B.; Ehrlich, R.; Ellsworth, R. W.; Goodman, J. A.; Hoffman, K. D.; Huelsnitz, W.; Meagher, K.; Olivas, A.; Redl, P.; Roth, P.; Schmidt, T.; Straszheim, T.; Sullivan, G. W.; Turcan, D.; Wissing, H.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Besson, D. Z.; Kenny, P.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Zoll, M.] Stockholm Univ, Oskar Klein Ctr, SE-10691 Stockholm, Sweden.
[Bohm, C.; Danninger, M.; Finley, C.; Hulth, P. O.; Hultqvist, K.; Johansson, H.; Seo, S. H.; Walck, C.; Zoll, M.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Bose, D.; Buitink, S.; De Clercq, C.; Depaepe, O.; Hubert, D.; Labare, M.; Rizzo, A.; Strahler, E. A.; van Eijndhoven, N.] Vrije Univ Brussel, Dienst ELEM, B-1050 Brussels, Belgium.
[Boeser, S.; Denger, T.; Franckowiak, A.; Homeier, A.; Kowalski, M.; Panknin, S.; Stuer, M.; Voge, M.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany.
[Botner, O.; Engdegard, O.; Hallgren, A.; Miller, J.; de los Heros, C. Perez; Taavola, H.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden.
[Caballero-Mora, K. S.; Cowen, D. F.; DeYoung, T.; Foerster, M. M.; Fox, B. D.; Ha, C.; Koskinen, D. J.; Lafebre, S.; Larson, M. J.; Meszaros, P.; Rutledge, D.; Slipak, A.; Stephens, G.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA.
[Clevermann, F.; Koehne, J. -H.; Milke, N.; Pieloth, D.; Rhode, W.; Ruhe, T.] TU Dortmund Univ, Dept Phys, D-44221 Dortmund, Germany.
[Cohen, S.; Demiroers, L.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland.
[Colnard, C.; Gross, A.; Odrowski, S.; Resconi, E.; Schulz, O.; Sestayo, Y.; Wolf, M.] Max Planck Inst Kernphys, D-69177 Heidelberg, Germany.
[Cowen, D. F.; Meszaros, P.; Movit, S. M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA.
[Daughhetee, J.; Taboada, I.; Tepe, A.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA.
[Fadiran, O.; Japaridze, G. S.] Clark Atlanta Univ, CTSPS, Atlanta, GA 30314 USA.
[Fazely, A. R.; Ter-Antonyan, S.; Xu, X. W.] So Univ, Dept Phys, Baton Rouge, LA 70813 USA.
[Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Grant, D.; Wood, T. R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada.
[Griesel, T.; Koepke, L.; Kowarik, T.; Kroll, G.; Luenemann, J.; Piegsa, A.; Rothmaier, F.; Sander, H. -G.; Schatto, K.; Wiebe, K.] Johannes Gutenberg Univ Mainz, Inst Phys, D-55099 Mainz, Germany.
[Herquet, P.; Kohnen, G.] Univ Mons, B-7000 Mons, Belgium.
[Ishihara, A.; Mase, K.; Ono, M.; Yoshida, S.] Chiba Univ, Dept Phys, Chiba 2638522, Japan.
[Kappes, A.; Kolanoski, H.; Waldenmaier, T.] Univ Berlin, Inst Phys, D-12489 Berlin, Germany.
[Rawlins, K.] Univ Alaska, Dept Phys & Astron, Anchorage, AK 99508 USA.
[Seunarine, S.] Univ W Indies, Dept Phys, BB-11000 Bridgetown, Barbados.
[Toale, P. A.; Williams, D. R.; Zarzhitsky, P.] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA.
[Montaruli, T.] Univ Bari, Dipartmento Fis, I-70126 Bari, Italy.
[Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Abbasi, R (reprint author), Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA.
RI Taavola, Henric/B-4497-2011; Sarkar, Subir/G-5978-2011; Wiebusch,
Christopher/G-6490-2012; Beatty, James/D-9310-2011; Kowalski,
Marek/G-5546-2012; Tamburro, Alessio/A-5703-2013; Hallgren,
Allan/A-8963-2013; Botner, Olga/A-9110-2013; Tjus, Julia/G-8145-2012;
Auffenberg, Jan/D-3954-2014; Koskinen, David/G-3236-2014; Aguilar
Sanchez, Juan Antonio/H-4467-2015; Maruyama, Reina/A-1064-2013
OI Taavola, Henric/0000-0002-2604-2810; Buitink, Stijn/0000-0002-6177-497X;
Carson, Michael/0000-0003-0400-7819; Hubert, Daan/0000-0002-4365-865X;
Benabderrahmane, Mohamed Lotfi/0000-0003-4410-5886; Sarkar,
Subir/0000-0002-3542-858X; Wiebusch, Christopher/0000-0002-6418-3008;
Beatty, James/0000-0003-0481-4952; Perez de los Heros,
Carlos/0000-0002-2084-5866; Auffenberg, Jan/0000-0002-1185-9094;
Koskinen, David/0000-0002-0514-5917; Aguilar Sanchez, Juan
Antonio/0000-0003-2252-9514; Maruyama, Reina/0000-0003-2794-512X
FU U.S. National Science Foundation-Office; U.S. National Science
Foundation-Physics Division; University of Wisconsin Alumni Research
Foundation; Grid Laboratory of Wisconsin (GLOW); Open Science Grid (OSG)
grid infrastructure; U.S. Department of Energy; Louisiana Optical
Network Initiative (LONI); National Science and Engineering Research
Council of Canada; Swedish Research Council; Swedish Polar Research
Secretariat; Swedish National Infrastructure for Computing (SNIC);
Deutsche Forschungsgemeinschaft (DFG); Complex Interactions (Bochum),
Germany; Fund for Scientific Research (FNRS-FWO); FWO; Flanders
Institute to encourage scientific and technological research in industry
(IWT); Belgian Federal Science Policy Office (Belspo); University of
Oxford, United Kingdom; Marsden Fund, New Zealand; Japan Society for
Promotion of Science (JSPS); Swiss National Science Foundation (SNSF),
Switzerland; EU; Capes Foundation, Ministry of Education of Brazil;
National Energy Research Scientific Computing Center; Knut and Alice
Wallenberg Foundation, Sweden; German Ministry for Education and
Research (BMBF)
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), 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, United Kingdom;
Marsden Fund, New Zealand; Japan Society for Promotion of Science
(JSPS); the Swiss National Science Foundation (SNSF), Switzerland; A.
GroB acknowledges support by the EU Marie Curie OIF Program; J. P.
Rodrigues acknowledges support by the Capes Foundation, Ministry of
Education of Brazil.
NR 43
TC 7
Z9 7
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 JAN 20
PY 2012
VL 745
IS 1
AR 45
DI 10.1088/0004-637X/745/1/45
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 892WP
UT WOS:000300316600045
ER
PT J
AU Barbary, K
Aldering, G
Amanullah, R
Brodwin, M
Connolly, N
Dawson, KS
Doi, M
Eisenhardt, P
Faccioli, L
Fadeyev, V
Fakhouri, HK
Fruchter, AS
Gilbank, DG
Gladders, MD
Goldhaber, G
Goobar, A
Hattori, T
Hsiao, E
Huang, X
Ihara, Y
Kashikawa, N
Koester, B
Konishi, K
Kowalski, M
Lidman, C
Lubin, L
Meyers, J
Morokuma, T
Oda, T
Panagia, N
Perlmutter, S
Postman, M
Ripoche, P
Rosati, P
Rubin, D
Schlegel, DJ
Spadafora, AL
Stanford, SA
Strovink, M
Suzuki, N
Takanashi, N
Tokita, K
Yasuda, N
AF Barbary, K.
Aldering, G.
Amanullah, R.
Brodwin, M.
Connolly, N.
Dawson, K. S.
Doi, M.
Eisenhardt, P.
Faccioli, L.
Fadeyev, V.
Fakhouri, H. K.
Fruchter, A. S.
Gilbank, D. G.
Gladders, M. D.
Goldhaber, G.
Goobar, A.
Hattori, T.
Hsiao, E.
Huang, X.
Ihara, Y.
Kashikawa, N.
Koester, B.
Konishi, K.
Kowalski, M.
Lidman, C.
Lubin, L.
Meyers, J.
Morokuma, T.
Oda, T.
Panagia, N.
Perlmutter, S.
Postman, M.
Ripoche, P.
Rosati, P.
Rubin, D.
Schlegel, D. J.
Spadafora, A. L.
Stanford, S. A.
Strovink, M.
Suzuki, N.
Takanashi, N.
Tokita, K.
Yasuda, N.
CA Supernova Cosmology Project
TI THE HUBBLE SPACE TELESCOPE CLUSTER SUPERNOVA SURVEY. VI. THE VOLUMETRIC
TYPE Ia SUPERNOVA RATE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; supernovae: general; white dwarfs
ID DIGITAL SKY SURVEY; SUBARU DEEP FIELD; SIMILAR-TO 1; GALAXY CLUSTERS;
LEGACY SURVEY; STAR-FORMATION; COSMOLOGICAL CONSTRAINTS; XMMXCS
J2215.9-1738; II SUPERNOVAE; LIGHT CURVES
AB We present a measurement of the volumetric Type Ia supernova (SN Ia) rate out to z similar or equal to 1.6 from the Hubble Space Telescope Cluster Supernova Survey. In observations spanning 189 orbits with the Advanced Camera for Surveys we discovered 29 SNe, of which approximately 20 are SNe Ia. Twelve of these SNe Ia are located in the foregrounds and backgrounds of the clusters targeted in the survey. Using these new data, we derive the volumetric SN Ia rate in four broad redshift bins, finding results consistent with previous measurements at z greater than or similar to 1 and strengthening the case for an SN Ia rate that is greater than or similar to 0.6 x 10(-4) h(70)(3) yr(-1) Mpc(-3) at z similar to 1 and flattening out at higher redshift. We provide SN candidates and efficiency calculations in a form that makes it easy to rebin and combine these results with other measurements for increased statistics. Finally, we compare the assumptions about host-galaxy dust extinction used in different high-redshift rate measurements, finding that different assumptions may induce significant systematic differences between measurements.
C1 [Barbary, K.; Amanullah, R.; Fakhouri, H. K.; Goldhaber, G.; Huang, X.; Meyers, J.; Perlmutter, S.; Rubin, D.; Strovink, M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Barbary, K.; Aldering, G.; Dawson, K. S.; Fakhouri, H. K.; Goldhaber, G.; Hsiao, E.; Meyers, J.; Perlmutter, S.; Ripoche, P.; Rubin, D.; Schlegel, D. J.; Spadafora, A. L.; Strovink, M.; Suzuki, N.] EO Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Amanullah, R.; Faccioli, L.; Goobar, A.] Oskar Klein Ctr Cosmo Particle Phys, SE-10691 Stockholm, Sweden.
[Brodwin, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Connolly, N.] Dept Phys, Hamilton Coll, Clinton, NY 13323 USA.
[Dawson, K. S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Doi, M.; Ihara, Y.; Morokuma, T.; Tokita, K.] Univ Tokyo, Inst Astron, Grad Sch Sci, Mitaka, Tokyo 1810015, Japan.
[Eisenhardt, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Fadeyev, V.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 94064 USA.
[Fruchter, A. S.; Panagia, N.; Postman, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Gilbank, D. G.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
[Gladders, M. D.; Koester, B.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Goobar, A.] Stockholm Univ, Albanova Univ Ctr, Dept Phys, SE-10691 Stockholm, Sweden.
[Hattori, T.] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Kashikawa, N.; Morokuma, T.; Takanashi, N.] Univ Tokyo, Inst Ind Sci, Meguro Ku, Tokyo 1538505, Japan.
[Koester, B.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Konishi, K.; Yasuda, N.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan.
[Kowalski, M.] Univ Bonn, Inst Phys, Bonn, Germany.
[Lidman, C.] Australian Astron Observ, Epping, NSW 1710, Australia.
[Lubin, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95618 USA.
[Oda, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Rosati, P.] ESO, D-85748 Garching, Germany.
[Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA.
RP Barbary, K (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
EM kbarbary@lbl.gov
RI Kowalski, Marek/G-5546-2012; Perlmutter, Saul/I-3505-2015;
OI Perlmutter, Saul/0000-0002-4436-4661; Strovink,
Mark/0000-0001-7020-7769; Meyers, Joshua/0000-0002-2308-4230
FU NASA from Space Telescope Science Institute [GO-10496]; NASA [NAS
5-26555]; Office of Science, Office of High Energy and Nuclear Physics,
of the U.S. Department of Energy [AC02-05CH11231]; JSPS [20040003]
FX Financial support for this work was provided by NASA through program
GO-10496 from the Space Telescope Science Institute, which is operated
by AURA, Inc., under NASA contract NAS 5-26555. This work was also
supported in part by the Director, Office of Science, Office of High
Energy and Nuclear Physics, of the U.S. Department of Energy under
Contract No. AC02-05CH11231, as well as a JSPS core-to-core program
"International Research Network for Dark Energy" and by a JSPS research
grant (20040003). 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. Finally, this work would not have been possible without the
dedicated efforts of the daytime and nighttime support staff at the
Cerro Paranal Observatory.; STScI is operated by the association of
Universities for Research in Astronomy, Inc., under the NASA contract
NAS 5-26555. The observations are associated with program GO-10496.
NR 67
TC 15
Z9 15
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 JAN 20
PY 2012
VL 745
IS 1
AR 31
DI 10.1088/0004-637X/745/1/31
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 892WP
UT WOS:000300316600031
ER
PT J
AU Barbary, K
Aldering, G
Amanullah, R
Brodwin, M
Connolly, N
Dawson, KS
Doi, M
Eisenhardt, P
Faccioli, L
Fadeyev, V
Fakhouri, HK
Fruchter, AS
Gilbank, DG
Gladders, MD
Goldhaber, G
Goobar, A
Hattori, T
Hsiao, E
Huang, X
Ihara, Y
Kashikawa, N
Koester, B
Konishi, K
Kowalski, M
Lidman, C
Lubin, L
Meyers, J
Morokuma, T
Oda, T
Panagia, N
Perlmutter, S
Postman, M
Ripoche, P
Rosati, P
Rubin, D
Schlegel, DJ
Spadafora, AL
Stanford, SA
Strovink, M
Suzuki, N
Takanashi, N
Tokita, K
Yasuda, N
AF Barbary, K.
Aldering, G.
Amanullah, R.
Brodwin, M.
Connolly, N.
Dawson, K. S.
Doi, M.
Eisenhardt, P.
Faccioli, L.
Fadeyev, V.
Fakhouri, H. K.
Fruchter, A. S.
Gilbank, D. G.
Gladders, M. D.
Goldhaber, G.
Goobar, A.
Hattori, T.
Hsiao, E.
Huang, X.
Ihara, Y.
Kashikawa, N.
Koester, B.
Konishi, K.
Kowalski, M.
Lidman, C.
Lubin, L.
Meyers, J.
Morokuma, T.
Oda, T.
Panagia, N.
Perlmutter, S.
Postman, M.
Ripoche, P.
Rosati, P.
Rubin, D.
Schlegel, D. J.
Spadafora, A. L.
Stanford, S. A.
Strovink, M.
Suzuki, N.
Takanashi, N.
Tokita, K.
Yasuda, N.
CA Supernova Cosmology Project
TI THE HUBBLE SPACE TELESCOPE CLUSTER SUPERNOVA SURVEY. II. THE TYPE Ia
SUPERNOVA RATE IN HIGH-REDSHIFT GALAXY CLUSTERS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; supernovae: general; white dwarfs
ID DELAY-TIME DISTRIBUTION; DIGITAL SKY SURVEY; INTRACLUSTER
PLANETARY-NEBULAE; CORE-COLLAPSE SUPERNOVAE; DIFFUSE OPTICAL LIGHT; IRAC
SHALLOW SURVEY; SIMILAR-TO 1; X-RAY; LUMINOSITY FUNCTION; VIRGO-CLUSTER
AB We report a measurement of the Type Ia supernova (SN Ia) rate in galaxy clusters at 0.9 < z < 1.46 from the Hubble Space Telescope Cluster Supernova Survey. This is the first cluster SN Ia rate measurement with detected z > 0.9 SNe. Finding 8 +/- 1 cluster SNe Ia, we determine an SN Ia rate of 0.50(-0.19)(+0.23) (stat) (+0.10)(-0.09) (sys) h(70)(2) SNuB (SNuB equivalent to 10(-12) SNe (L-1)circle dot(,B) yr(-1)). In units of stellar mass, this translates to 0.36(-0.13)(+0.16) (stat) (+0.07)(-0.06) (sys) h(70)(2) SNuM (SNuM = 10(-12) SNe M-1 circle dot yr(-1)). This represents a factor of approximate to 5 +/- 2 increase over measurements of the cluster rate at z < 0.2. We parameterize the late-time SN Ia delay time distribution (DTD) with a power law: Psi(t) t(s). Under the approximation of a single-burst cluster formation redshift of z(f) = 3, our rate measurement in combination with lower-redshift cluster SN Ia rates constrains s = -1.41(-0.40)(+0.47), consistent with measurements of the DTD in the field. This measurement is generally consistent with expectations for the "double degenerate" scenario and inconsistent with some models for the "single degenerate" scenario predicting a steeper DTD at large delay times. We check for environmental dependence and the influence of younger stellar populations by calculating the rate specifically in cluster red-sequence galaxies and in morphologically early-type galaxies, finding results similar to the full cluster rate. Finally, the upper limit of one hostless cluster SN Ia detected in the survey implies that the fraction of stars in the intra-cluster medium is less than 0.47 (95% confidence), consistent with measurements at lower redshifts.
C1 [Barbary, K.; Amanullah, R.; Fakhouri, H. K.; Goldhaber, G.; Huang, X.; Meyers, J.; Perlmutter, S.; Rubin, D.; Strovink, M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Barbary, K.; Aldering, G.; Dawson, K. S.; Faccioli, L.; Fakhouri, H. K.; Goldhaber, G.; Hsiao, E.; Meyers, J.; Perlmutter, S.; Ripoche, P.; Rubin, D.; Schlegel, D. J.; Spadafora, A. L.; Strovink, M.; Suzuki, N.] EO Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Amanullah, R.; Goobar, A.] Oskar Klein Ctr Cosmo Particle Phys, SE-10691 Stockholm, Sweden.
[Brodwin, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Connolly, N.] Hamilton Coll, Dept Phys, Clinton, NY 13323 USA.
[Dawson, K. S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Doi, M.; Ihara, Y.; Morokuma, T.; Tokita, K.] Univ Tokyo, Grad Sch Sci, Inst Astron, Mitaka, Tokyo 1810015, Japan.
[Eisenhardt, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Fadeyev, V.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 94064 USA.
[Fruchter, A. S.; Panagia, N.; Postman, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Gilbank, D. G.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
[Gladders, M. D.; Koester, B.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Goobar, A.] Stockholm Univ, Albanova Univ Ctr, Dept Phys, SE-10691 Stockholm, Sweden.
[Hattori, T.] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
[Kashikawa, N.; Morokuma, T.; Takanashi, N.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Koester, B.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Konishi, K.; Yasuda, N.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan.
[Kowalski, M.] Univ Bonn, Inst Phys, Bonn, Germany.
[Lidman, C.] Australian Astron Observ, Epping, NSW 1710, Australia.
[Lubin, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95618 USA.
[Oda, T.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Rosati, P.] ESO, D-85748 Garching, Germany.
[Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA.
RP Barbary, K (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
EM kbarbary@lbl.gov
RI Kowalski, Marek/G-5546-2012; Perlmutter, Saul/I-3505-2015;
OI Perlmutter, Saul/0000-0002-4436-4661; Strovink,
Mark/0000-0001-7020-7769; Meyers, Joshua/0000-0002-2308-4230
FU Japan Society for the Promotion of Science (JSPS) [20040003]; Australian
Research Council (ARC); NASA from Space Telescope Science Institute
[GO-10496]; Office of Science, Office of High Energy and Nuclear Physics
U.S. Department of Energy [AC02-05CH11231]; NASA [NAS 5-26555]
FX We thank Eric Bell and DanMaoz for helpful discussion. T. M. is
financially supported by the Japan Society for the Promotion of Science
(JSPS) through the JSPS Research Fellowship. C. L. is financially
supported by the Australian Research Council (ARC) through the ARC
Future Fellowship program. Financial support for this work was provided
by NASA through program GO-10496 from the Space Telescope Science
Institute, which is operated by AURA, Inc., under NASA contract NAS
5-26555. This work was also supported in part by the Director, Office of
Science, Office of High Energy and Nuclear Physics, of the U.S.
Department of Energy under Contract No. AC02-05CH11231, as well as a
JSPS core-to-core program "International Research Network for Dark
Energy" and by a JSPS research grant (20040003). 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. Finally, this
work would not have been possible without the dedicated efforts of the
daytime and nighttime support staff at the Cerro Paranal Observatory.
NR 147
TC 25
Z9 27
U1 0
U2 1
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 JAN 20
PY 2012
VL 745
IS 1
AR 32
DI 10.1088/0004-637X/745/1/32
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 892WP
UT WOS:000300316600032
ER
PT J
AU Folatelli, G
Phillips, MM
Morrell, N
Tanaka, M
Maeda, K
Nomoto, K
Stritzinger, M
Burns, CR
Hamuy, M
Mazzali, P
Boldt, L
Campillay, A
Contreras, C
Gonzalez, S
Roth, M
Salgado, F
Freedman, WL
Madore, BF
Persson, SE
Suntzeff, NB
AF Folatelli, Gaston
Phillips, M. M.
Morrell, Nidia
Tanaka, Masaomi
Maeda, Keiichi
Nomoto, Ken'ichi
Stritzinger, Maximilian
Burns, Christopher R.
Hamuy, Mario
Mazzali, Paolo
Boldt, Luis
Campillay, Abdo
Contreras, Carlos
Gonzalez, Sergio
Roth, Miguel
Salgado, Francisco
Freedman, W. L.
Madore, Barry F.
Persson, S. E.
Suntzeff, Nicholas B.
TI UNBURNED MATERIAL IN THE EJECTA OF TYPE Ia SUPERNOVAE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE supernovae: general; techniques: spectroscopic
ID DELAYED DETONATION MODELS; EARLY SPECTRAL EVOLUTION; PHOTOMETRY DATA
RELEASE; WHITE-DWARF MODELS; LIGHT CURVES; EXPLOSION MODELS; ABUNDANCE
STRATIFICATION; SN 2004EO; CARBON; PROJECT
AB The presence of unburned material in the ejecta of normal Type Ia supernovae (SNe Ia) is investigated using early-time spectroscopy obtained by the Carnegie Supernova Project. The tell-tale signature of pristine material from a C+O white dwarf progenitor star is the presence of carbon, as oxygen is also a product of carbon burning. The most prominent carbon lines in optical spectra of SNe Ia are expected to arise from C II. We find that at least 30% of the objects in the sample show an absorption at approximate to 6300 angstrom which is attributed to C II lambda 6580. An alternative identification of this absorption as Ha is considered to be unlikely. These findings imply a larger incidence of carbon in SNe Ia ejecta than previously noted. We show how observational biases and physical conditions may hide the presence of weak C II lines, and account for the scarcity of previous carbon detections in the literature. This relatively large frequency of carbon detections has crucial implications on our understanding of the explosive process. Furthermore, the identification of the 6300 angstrom absorptions as carbon would imply that unburned material is present at very low expansion velocities, merely approximate to 1000 km s(-1) above the bulk of Si II. Based on spectral modeling, it is found that the detections are consistent with a mass of carbon of 10(-3) to 10(-2) M-circle dot. The presence of this material so deep in the ejecta would imply substantial mixing, which may be related to asymmetries of the flame propagation. Another possible explanation for the carbon absorptions may be the existence of clumps of unburned material along the line of sight. However, the uniformity of the relation between C II and Si II velocities is not consistent with such small-scale asymmetries. The spectroscopic and photometric properties of SNe Ia with and without carbon signatures are compared. A trend toward bluer color and lower luminosity at maximum light is found for objects which show carbon.
C1 [Folatelli, Gaston; Tanaka, Masaomi; Maeda, Keiichi; Nomoto, Ken'ichi] Univ Tokyo, IPMU, Kashiwa, Chiba 2778583, Japan.
[Folatelli, Gaston; Hamuy, Mario] Univ Chile, Dept Astron, Santiago, Chile.
[Phillips, M. M.; Morrell, Nidia; Campillay, Abdo; Gonzalez, Sergio; Roth, Miguel] Carnegie Observ, Las Campanas Observ, La Serena, Chile.
[Stritzinger, Maximilian] Stockholm Univ, Dept Astron, Oskar Klein Ctr, S-10691 Stockholm, Sweden.
[Stritzinger, Maximilian] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark.
[Burns, Christopher R.; Freedman, W. L.; Madore, Barry F.; Persson, S. E.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Mazzali, Paolo] Max Planck Inst Astrophys, D-85748 Garching, Germany.
[Mazzali, Paolo] Ist Naz Astrofis Oss Astron, I-35122 Padua, Italy.
[Boldt, Luis] Univ Bonn, Argelander Inst Astron, D-53111 Bonn, Germany.
[Contreras, Carlos] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Salgado, Francisco] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Madore, Barry F.] CALTECH, Jet Prop Lab, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA.
[Suntzeff, Nicholas B.] Texas A&M Univ, Dept Phys & Astron, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
RP Folatelli, G (reprint author), Univ Tokyo, IPMU, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778583, Japan.
EM gaston.folatelli@ipmu.jp
RI Nomoto, Ken'ichi/A-4393-2011; Hamuy, Mario/G-7541-2016;
OI stritzinger, maximilian/0000-0002-5571-1833
FU NSF [AST-0306969, AST-0908886, AST-0607438, AST-1008343]; Danish NSF;
World Premier International Research Center Initiative (WPI Initiative),
MEXT, Japan; CONICYT [1060808]; Centro de Astrofisica FONDAP [15010003];
Centro BASAL CATA [PFB-06]; Millennium Center for Supernova Science
[P06-045-F]; [23740175]
FX We are grateful to Wojtek Krzeminski for his dedicated efforts during
the CSP campaigns. We also thank Luc Dessart for his useful suggestions,
and Joseph Anderson, Francisco Forster, Giuliano Pignata, and the rest
of the MCSS team for interesting discussions on the topic of this paper.
This material is based upon work supported by NSF under grants
AST-0306969, AST-0908886, AST-0607438, and AST-1008343. The Dark
Cosmology Centre is funded by the Danish NSF. This research is supported
by the World Premier International Research Center Initiative (WPI
Initiative), MEXT, Japan. G. F. acknowledges financial support by
Grant-in-Aid for Scientific Research for Young Scientists (23740175). M.
H. acknowledges support by CONICYT through grants FONDECYT Regular
1060808, Centro de Astrofisica FONDAP 15010003, Centro BASAL CATA
(PFB-06), and by the Millennium Center for Supernova Science
(P06-045-F).
NR 76
TC 38
Z9 38
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 JAN 20
PY 2012
VL 745
IS 1
AR 74
DI 10.1088/0004-637X/745/1/74
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 892WP
UT WOS:000300316600074
ER
PT J
AU Fressin, F
Torres, G
Pont, F
Knutson, HA
Charbonneau, D
Mazeh, T
Aigrain, S
Fridlund, M
Henze, CE
Guillot, T
Rauer, H
AF Fressin, Francois
Torres, Guillermo
Pont, Frederic
Knutson, Heather A.
Charbonneau, David
Mazeh, Tsevi
Aigrain, Suzanne
Fridlund, Malcolm
Henze, Christopher E.
Guillot, Tristan
Rauer, Heike
TI SPITZER INFRARED OBSERVATIONS AND INDEPENDENT VALIDATION OF THE
TRANSITING SUPER- EARTH CoRoT-7 b
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; planetary systems; stars: individual: CoRoT-7;
stars: statistics; techniques: photometric
ID SPACE-TELESCOPE; EMISSION-SPECTRUM; PLANET CANDIDATES; BLEND SCENARIOS;
MULTIPLE SYSTEM; LIGHT CURVES; ARRAY CAMERA; HD 189733B; LOW-MASS;
VARIABILITY
AB The detection and characterization of the first transiting super-Earth, CoRoT-7 b, has required an unprecedented effort in terms of telescope time and analysis. Although the star does display a radial-velocity signal at the period of the planet, this has been difficult to disentangle from the intrinsic stellar variability and pinning down the velocity amplitude has been very challenging. As a result, the precise value of the mass of the planet-and even the extent to which it can be considered to be confirmed-has been debated in the recent literature, with six mass measurements published so far based on the same spectroscopic observations, ranging from about 2 to 8 Earth masses. Here we report on an independent validation of the planet discovery using one of the fundamental properties of a transit signal: its achromaticity. We observed four transits of CoRoT-7 b at 4.5 mu m and 8.0 mu m with the Infrared Array Camera (IRAC) on board the Spitzer Space Telescope in order to determine whether the depth of the transit signal in the near-infrared is consistent with that observed in the CoRoT bandpass, as expected for a planet. We detected the transit and found an average depth of 0.426 +/- 0.115 mmag at 4.5 mu m, which is in good agreement with the depth of 0.350 +/- 0.011 mmag (ignoring limb darkening) found by CoRoT. The observations at 8.0 mu m did not yield a significant detection. The 4.5 mu m observations place important constraints on the kinds of astrophysical false positives that could mimic the signal. Combining this with additional constraints reported earlier, we performed an exhaustive exploration of possible blend scenarios for CoRoT-7 b using the BLENDER technique. We are able to rule out the vast majority of false positives, and the remaining ones are found to be much less likely than a true transiting planet. We thus validate CoRoT-7 b as a bona fide planet with a very high degree of confidence, independently of any radial-velocity information. Our Spitzer observations have additionally allowed us to significantly improve the ephemeris of the planet, so that future transits should be recoverable well into the next decade. In its warm phase Spitzer is expected to be an essential tool for the validation, along the lines of the present analysis, of transiting planet candidates with shallow signals from CoRoT as well as from the Kepler mission, including potentially rocky planets in the habitable zones of their parent stars.
C1 [Fressin, Francois; Torres, Guillermo; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Pont, Frederic] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
[Knutson, Heather A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Mazeh, Tsevi] Tel Aviv Univ, Dept Astron & Astrophys, IL-69978 Tel Aviv, Israel.
[Aigrain, Suzanne] Univ Oxford, Oxford OX1 3RH, England.
[Fridlund, Malcolm] ESTEC ESA, NL-2200 AG Noordwijk, Netherlands.
[Henze, Christopher E.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Guillot, Tristan] Observ Cote Azur, F-06304 Nice, France.
[Rauer, Heike] Deutsch Zentrum Luft & Raumfahrt DLR, D-12489 Berlin, Germany.
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
FX We are grateful to the anonymous referee for many very helpful comments
and suggestions. This work is based on observations made with the
Spitzer Space Telescope, which is operated by the Jet Propulsion
Laboratory, California Institute of Technology, under contract to NASA.
Support for this work was provided by NASA through an award issued by
JPL/Caltech. This research has made use of the facilities at the NASA
Advanced Supercomputing Division (NASA Ames Research Center).
NR 42
TC 9
Z9 9
U1 1
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 JAN 20
PY 2012
VL 745
IS 1
AR 81
DI 10.1088/0004-637X/745/1/81
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 892WP
UT WOS:000300316600081
ER
PT J
AU Gong, Y
Cooray, A
Silva, M
Santos, MG
Bock, J
Bradford, CM
Zemcov, M
AF Gong, Yan
Cooray, Asantha
Silva, Marta
Santos, Mario G.
Bock, James
Bradford, C. Matt
Zemcov, Michael
TI INTENSITY MAPPING OF THE [C II] FINE STRUCTURE LINE DURING THE EPOCH OF
REIONIZATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: theory; diffuse radiation; intergalactic medium; large-scale
structure of universe
ID 158 MU-M; FAR-INFRARED SPECTROSCOPY; STAR-FORMATION RATE;
INTERSTELLAR-MEDIUM; CHEMICAL EVOLUTION; MOLECULAR GAS; GALAXIES;
EMISSION; CII; SIMULATIONS
AB The atomic C II fine-structure line is one of the brightest lines in a typical star-forming galaxy spectrum with a luminosity similar to 0.1%-1% of the bolometric luminosity. It is potentially a reliable tracer of the dense gas distribution at high redshifts and could provide an additional probe to the era of reionization. By taking into account the spontaneous, stimulated, and collisional emission of the C II line, we calculate the spin temperature and the mean intensity as a function of the redshift. When averaged over a cosmologically large volume, we find that the C II emission from ionized carbon in individual galaxies is larger than the signal generated by carbon in the intergalactic medium. Assuming that the C II luminosity is proportional to the carbon mass in dark matter halos, we also compute the power spectrum of the C II line intensity at various redshifts. In order to avoid the contamination from CO rotational lines at low redshift when targeting a C II survey at high redshifts, we propose the cross-correlation of C II and 21 cm line emission from high redshifts. To explore the detectability of the C II signal from reionization, we also evaluate the expected errors on the C II power spectrum and C II-21 cm cross power spectrum based on the design of the future millimeter surveys. We note that the C II-21 cm cross power spectrum contains interesting features that capture physics during reionization, including the ionized bubble sizes and the mean ionization fraction, which are challenging to measure from 21 cm data alone. We propose an instrumental concept for the reionization C II experiment targeting the frequency range of similar to 200-300 GHz with 1, 3, and 10 m apertures and a bolometric spectrometer array with 64 independent spectral pixels with about 20,000 bolometers.
C1 [Gong, Yan; Cooray, Asantha] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[Silva, Marta; Santos, Mario G.] Univ Tecn Lisboa, CENTRA, Inst Super Tecn, P-1049001 Lisbon, Portugal.
[Bock, James; Bradford, C. Matt; Zemcov, Michael] CALTECH, Pasadena, CA 91125 USA.
[Bock, James; Bradford, C. Matt; Zemcov, Michael] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Gong, Y (reprint author), Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
RI Santos, Mario/F-2484-2011;
OI Santos, Mario/0000-0003-3892-3073; Silva, Marta/0000-0003-0209-4816
FU NSF CAREER [AST-0645427]; NASA [NNX10AD42G]; FCT-Portugal
[PTDC/FIS/100170/2008]
FX We thank participants of the Keck Institute for Space Studies' (KISS)
Billion Years workshop for helpful discussions. This work was supported
by NSF CAREER AST-0645427 and NASA NNX10AD42G at UCI. M. G. S. and M. B.
S. acknowledge support from FCT-Portugal under grant
PTDC/FIS/100170/2008.
NR 55
TC 46
Z9 46
U1 0
U2 10
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2012
VL 745
IS 1
AR 49
DI 10.1088/0004-637X/745/1/49
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 892WP
UT WOS:000300316600049
ER
PT J
AU Holland, ST
De Pasquale, M
Mao, JR
Sakamoto, T
Schady, P
Covino, S
Fan, YZ
Jin, ZP
D'Avanzo, P
Antonelli, A
D'Elia, V
Chincarini, G
Fiore, F
Pandey, SB
Cobb, BE
AF Holland, Stephen T.
De Pasquale, Massimiliano
Mao, Jirong
Sakamoto, Takanori
Schady, Patricia
Covino, Stefano
Fan, Yi-Zhong
Jin, Zhi-Ping
D'Avanzo, Paolo
Antonelli, Angelo
D'Elia, Valerio
Chincarini, Guido
Fiore, Fabrizio
Pandey, Shashi Bhushan
Cobb, Bethany E.
TI GRB 081029: A GAMMA-RAY BURST WITH A MULTI-COMPONENT AFTERGLOW
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: general; gamma-ray burst: individual: GRB 081029
ID SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; SPECTRAL IRRADIANCE CALIBRATION;
LIGHT CURVES; COMMON ORIGIN; DUST; REDSHIFT; JET; PROMPT; BAT;
ENVIRONMENT
AB We present an analysis of the unusual optical light curve of the gamma-ray burst GRB 081029, a long-soft burst with a redshift of z = 3.8479. We combine X-ray and optical observations from the Swift X-Ray Telescope and the Swift UltraViolet/Optical Telescope with ground-based optical and infrared data obtained using the REM, ROTSE, and CTIO 1.3 m telescopes to construct a detailed data set extending from 86 s to similar to 100000 s after the BAT trigger. Our data cover a wide energy range from 10 keV to 0.77 eV (1.24 angstrom-16000 angstrom). The X-ray afterglow shows a shallow initial decay followed by a rapid decay starting at about 18000 s. The optical and infrared afterglow, however, shows an uncharacteristic rise at about 3000 s that does not correspond to any feature in the X-ray light curve. Our data are not consistent with synchrotron radiation from a jet interacting with an external medium, a two-component jet, or continuous energy injection from the central engine. We find that the optical light curves can be broadly explained by a collision between two ejecta shells within a two-component jet. A growing number of gamma-ray-burst afterglows are consistent with complex jets, which suggests that some (or all) gamma-ray-burst jets are complex and will require detailed modeling to fully understand them.
C1 [Holland, Stephen T.; Sakamoto, Takanori] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA.
[Holland, Stephen T.] Univ Space Res Assoc, Columbia, MD 21044 USA.
[Holland, Stephen T.; Sakamoto, Takanori] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA.
[De Pasquale, Massimiliano; Schady, Patricia] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Mao, Jirong; Covino, Stefano; Jin, Zhi-Ping; D'Avanzo, Paolo; Chincarini, Guido] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy.
[Mao, Jirong] Chinese Acad Sci, Yunnan Observ, Kunming 650011, Yunan Province, Peoples R China.
[Mao, Jirong] Korea Astron & Space Sci Inst, Int Ctr Astrophys, Taejon 305348, South Korea.
[Mao, Jirong] Chinese Acad Sci, Key Lab Struct & Evolut Celestial Objects, Kunming 650011, Yunnan Province, Peoples R China.
[Sakamoto, Takanori] Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Baltimore, MD 21250 USA.
[Schady, Patricia] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Fan, Yi-Zhong; Jin, Zhi-Ping] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China.
[Antonelli, Angelo; D'Elia, Valerio; Fiore, Fabrizio] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Roma, Italy.
[Pandey, Shashi Bhushan] Univ Michigan, Randall Lab Phys, Ann Arbor, MI 48109 USA.
[Pandey, Shashi Bhushan] Aryabhatta Res Inst Observat Sci, Manora Peak 263129, Nainital, India.
[Cobb, Bethany E.] George Washington Univ, Dept Phys, Washington, DC 20052 USA.
RP Holland, ST (reprint author), NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Code 660-1,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM Stephen.T.Holland@nasa.gov
OI D'Elia, Valerio/0000-0002-7320-5862; Covino,
Stefano/0000-0001-9078-5507; Fiore, Fabrizio/0000-0002-4031-4157
FU NASA [NNX08AV63G]; NSF [PHY-0801007]
FX We acknowledge the use of public data from HEASARC's Swift Data Archive.
The ROTSE project is supported by the NASA grant NNX08AV63G and the NSF
grant PHY-0801007. The authors thank Scott Barthelmy and the GRB
Coordinates Network for rapidly providing precise GRB positions to the
astronomical community. This research has made use of the NASA/IPAC
Extragalactic Database, which is operated by the Jet Propulsion
Laboratory, California Institute of Technology, under contract with
NASA. The authors thank the anonymous referee for a thorough review of
this paper.
NR 78
TC 10
Z9 10
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 JAN 20
PY 2012
VL 745
IS 1
AR 41
DI 10.1088/0004-637X/745/1/41
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 892WP
UT WOS:000300316600041
ER
PT J
AU Holman, GD
AF Holman, Gordon D.
TI UNDERSTANDING THE IMPACT OF RETURN-CURRENT LOSSES ON THE X-RAY EMISSION
FROM SOLAR FLARES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; plasmas; Sun: flares; Sun: X-rays, gamma rays
ID CONVERGING MAGNETIC-FIELD; NONTHERMAL ELECTRON-BEAMS; ENERGETIC
ELECTRONS; REVERSE-CURRENT; ANISOTROPIC DISTRIBUTIONS; THERMAL
ELECTRONS; BREMSSTRAHLUNG; ACCELERATION; SPECTRA; POWER
AB I obtain and examine the implications of one-dimensional analytic solutions for return-current losses on an initially power-law distribution of energetic electrons with a sharp low-energy cutoff in flare plasma with classical (collisional) resistivity. These solutions show, for example, that return-current losses are not sensitive to plasma density, but are sensitive to plasma temperature and the low-energy cutoff of the injected nonthermal electron distribution. A characteristic distance from the electron injection site, x(rc), is derived. At distances less than xrc the electron flux density is not reduced by return-current losses, but plasma heating can be substantial in this region, in the upper, coronal part of the flare loop. Before the electrons reach the collisional thick-target region of the flare loop, an injected power-law electron distribution with a low-energy cutoff maintains that structure, but with a flat energy distribution below the cutoff energy, which is now determined by the total potential drop experienced by the electrons. Modifications due to the presence of collisional losses are discussed. I compare these results with earlier analytical results and with more recent numerical simulations. Emslie's conjecture that there is a maximum integrated X-ray source brightness on the order of 10(-15) photons cm(-2) s(-1) cm(-2) is examined. I find that this is not actually the maximum brightness and its value is parameter dependent, but it is nevertheless a valuable benchmark for identifying return-current losses in hard X-ray spectra. I discuss an observational approach to identifying return-current losses in flare data, including identification of a return-current "bump" in X-ray light curves at low photon energies.
C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Holman, GD (reprint author), NASA, Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA.
EM Gordon.D.Holman@nasa.gov
RI Holman, Gordon/C-9548-2012
FU NASA [09-HGI09-0064]; RHESSI
FX This work was supported by NASA Heliophysics Guest Investigator Grant
09-HGI09-0064 and by the RHESSI Program. I thank the referee and Miriem
Alaoui Abdallaoui for valuable comments and questions that led to
improvements in the text.
NR 46
TC 14
Z9 14
U1 0
U2 1
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 JAN 20
PY 2012
VL 745
IS 1
AR 52
DI 10.1088/0004-637X/745/1/52
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 892WP
UT WOS:000300316600052
ER
PT J
AU Kempton, EMR
Zahnle, K
Fortney, JJ
AF Kempton, Eliza Miller-Ricci
Zahnle, Kevin
Fortney, Jonathan J.
TI THE ATMOSPHERIC CHEMISTRY OF GJ 1214b: PHOTOCHEMISTRY AND CLOUDS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems
ID TRANSITING PLANET ATMOSPHERES; EXTRASOLAR GIANT PLANETS;
HUBBLE-SPACE-TELESCOPE; EARTH-LIKE PLANETS; HD 189733B; TRANSMISSION
SPECTROSCOPY; HOT JUPITERS; LOW-MASS; DISEQUILIBRIUM CARBON; MODEL
ATMOSPHERES
AB Recent observations of the transiting super-Earth GJ 1214b reveal that its atmosphere may be hydrogen-rich or water-rich in nature, with clouds or hazes potentially affecting its transmission spectrum in the optical and very-near-IR. Here, we further examine the possibility that GJ 1214b does indeed possess a hydrogen-dominated atmosphere, which is the hypothesis that is favored by models of the bulk composition of the planet. We study the effects of non-equilibrium chemistry (photochemistry, thermal chemistry, and mixing) on the planet's transmission spectrum. We furthermore examine the possibility that clouds could play a significant role in attenuating GJ 1214b's transmission spectrum at short wavelengths. We find that non-equilibrium chemistry can have a large effect on the overall chemical composition of GJ 1214b's atmosphere, however these changes mostly take place above the height in the atmosphere that is probed by transmission spectroscopy. The effects of non-equilibrium chemistry on GJ 1214b's transmission spectrum are therefore minimal, with the largest effects taking place if the planet's atmosphere has super-solar metallicity and a low rate of vertical mixing. Interestingly, we find that the best fit to the observations of GJ 1214b's atmosphere in transmission occurs if the planet's atmosphere is deficient in CH4, and possesses a cloud layer at a pressure of similar to 200 mbar. This is consistent with a picture of efficient methane photolysis, accompanied by formation of organic haze that obscures the lower atmosphere of GJ 1214b at optical wavelengths. However, for methane to be absent from GJ 1214b's transmission spectrum, UV photolysis of this molecule must be efficient at pressures of greater than similar to 1 mbar, whereas we find that methane only photolyzes to pressures less than 0.1 mbar, even under the most optimistic assumptions. An alternative explanation of the observations of GJ 1214b is that the atmosphere is water-rich, although this interpretation conflicts with the findings of Croll et al., who measure a low mean molecular weight for the planet's atmosphere. Additional observations at wavelengths corresponding to mid-IR water and methane features in GJ 1214b's transmission spectrum should break the degeneracy between the two possible cases.
C1 [Kempton, Eliza Miller-Ricci; Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Zahnle, Kevin] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Kempton, EMR (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
EM ekempton@ucolick.org
OI Fortney, Jonathan/0000-0002-9843-4354
FU California Institute of Technology; NASA
FX E.M.-R.K was supported by a contract with the California Institute of
Technology funded by NASA through the Sagan Fellowship Program.
NR 56
TC 46
Z9 46
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 JAN 20
PY 2012
VL 745
IS 1
AR 3
DI 10.1088/0004-637X/745/1/3
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 892WP
UT WOS:000300316600003
ER
PT J
AU Konstantopoulos, IS
Gallagher, SC
Fedotov, K
Durrell, PR
Tzanavaris, P
Hill, AR
Zabludoff, AI
Maier, ML
Elmegreen, DM
Charlton, JC
Johnson, KE
Brandt, WN
Walker, LM
Eracleous, M
Maybhate, A
Gronwall, C
English, J
Hornschemeier, AE
Mulchaey, JS
AF Konstantopoulos, I. S.
Gallagher, S. C.
Fedotov, K.
Durrell, P. R.
Tzanavaris, P.
Hill, A. R.
Zabludoff, A. I.
Maier, M. L.
Elmegreen, D. M.
Charlton, J. C.
Johnson, K. E.
Brandt, W. N.
Walker, L. M.
Eracleous, M.
Maybhate, A.
Gronwall, C.
English, J.
Hornschemeier, A. E.
Mulchaey, J. S.
TI THE MERGER HISTORY, ACTIVE GALACTIC NUCLEUS, AND DWARF GALAXIES OF
HICKSON COMPACT GROUP 59
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: clusters: individual (HCG 59); galaxies:
dwarf; galaxies: evolution; galaxies: fundamental parameters; galaxies:
interactions; galaxies: star clusters: general
ID GLOBULAR-CLUSTER SYSTEMS; GEMINI SPECTROSCOPIC SURVEY; INTRAGROUP
DIFFUSE LIGHT; YOUNG STAR-CLUSTERS; X-RAY; SKY SURVEY; METALLICITY
DISTRIBUTION; ENERGY-DISTRIBUTIONS; FORMATION MECHANISM; SAGITTARIUS
STREAM
AB Compact group galaxies often appear unaffected by their unusually dense environment. Closer examination can, however, reveal the subtle, cumulative effects of multiple galaxy interactions. Hickson Compact Group (HCG) 59 is an excellent example of this situation. We present a photometric study of this group in the optical (Hubble Space Telescope), infrared (Spitzer), and X-ray (Chandra) regimes aimed at characterizing the star formation and nuclear activity in its constituent galaxies and intra-group medium. We associate five dwarf galaxies with the group and update the velocity dispersion, leading to an increase in the dynamical mass of the group of up to a factor of 10 (to 2.8 x 10(13) M circle dot), and a subsequent revision of its evolutionary stage. Star formation is proceeding at a level consistent with the morphological types of the four main galaxies, of which two are star-forming and the other are two quiescent. Unlike in some other compact groups, star-forming complexes across HCG 59 closely follow mass-radius scaling relations typical of nearby galaxies. In contrast, the ancient globular cluster populations in galaxies HCG 59A and B show intriguing irregularities, and two extragalactic H II regions are found just west of B. We age-date a faint stellar stream in the intra-group medium at similar to 1 Gyr to examine recent interactions. We detect a likely low-luminosity active galactic nucleus in HCG 59A by its similar to 10(40) erg s(-1) X-ray emission; the active nucleus rather than star formation can account for the UV+IR spectral energy distribution. We discuss the implications of our findings in the context of galaxy evolution in dense environments.
C1 [Konstantopoulos, I. S.; Charlton, J. C.; Brandt, W. N.; Eracleous, M.; Gronwall, C.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Gallagher, S. C.; Fedotov, K.; Hill, A. R.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Fedotov, K.] Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada.
[Durrell, P. R.] Youngstown State Univ, Dept Phys & Astron, Youngstown, OH 44555 USA.
[Tzanavaris, P.; Hornschemeier, A. E.] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA.
[Tzanavaris, P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Zabludoff, A. I.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Maier, M. L.] Gemini Observ, La Serena, Chile.
[Elmegreen, D. M.] Vassar Coll, Dept Phys & Astron, Poughkeepsie, NY 12604 USA.
[Johnson, K. E.; Walker, L. M.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Johnson, K. E.] Natl Radio Astron Observ, Charlottesville, VA USA.
[Maybhate, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[English, J.] Univ Manitoba, Winnipeg, MB, Canada.
[Mulchaey, J. S.] Carnegie Observ, Pasadena, CA 91101 USA.
RP Konstantopoulos, IS (reprint author), Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
EM iraklis@astro.psu.edu
RI Brandt, William/N-2844-2015;
OI Brandt, William/0000-0002-0167-2453; Konstantopoulos,
Iraklis/0000-0003-2177-0146
FU NASA from the Space Telescope Science Institute [HST-GO-10787.15-A];
NASA [NAS 5-26555, NAS8-03060, NNX10AE88G]; National Science
Foundation(NSF) [0908984, 0548103]; HST [HST-GO-10787.07-A]; David and
Lucile Packard Foundation; NASA at Goddard Space Flight Center; Space
Telescope Science Institute; Chandra X-ray Observatory Center,
[GO8-91248]
FX We thank the referee, Cristiano Da Rocha, for his constructive criticism
of the manuscript and suggested additions that elevated the work. I. S.
K. thanks Ranjan Vasudevan and Matt Povich for educational discussions
on the X-ray properties of AGNs and star-forming regions. We thank
Gordon Garmire for his contribution in obtaining the X-ray data set.
Support for this work was provided by NASA through grant number
HST-GO-10787.15-A from the Space Telescope Science Institute which is
operated by AURA, Inc., under NASA contract NAS 5-26555 and through
Chandra Award No. GO8-91248 issued by the Chandra X-ray Observatory
Center, which is operated by the Smithsonian Astrophysical Observatory
under NASA contract NAS8-03060. S.C.G., K. F., and A. R. H. thank the
National Science and Engineering Council of Canada and the Ontario Early
Researcher program. Funding was provided by the National Science
Foundation under award 0908984. P. R. D. acknowledges support from HST
grant HST-GO-10787.07-A. A.I.Z. acknowledges support from the NASA
Astrophysics Data Analysis Program through grant NNX10AE88G. K.E.J.
gratefully acknowledges support for this work provided by NSF through
CAREER award 0548103 and the David and Lucile Packard Foundation through
a Packard Fellowship. P. T. acknowledges support through a NASA
Postdoctoral Program Fellowship at Goddard Space Flight Center,
administered by Oak Ridge Associated Universities through a contract
with NASA. 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.
NR 96
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 JAN 20
PY 2012
VL 745
IS 1
AR 30
DI 10.1088/0004-637X/745/1/30
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 892WP
UT WOS:000300316600030
ER
PT J
AU Kopparapu, RK
Kasting, JF
Zahnle, KJ
AF Kopparapu, Ravi Kumar
Kasting, James F.
Zahnle, Kevin J.
TI A PHOTOCHEMICAL MODEL FOR THE CARBON-RICH PLANET WASP-12b
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems
ID EARTHS EARLY ATMOSPHERE; TRANSITING EXTRASOLAR PLANET; HOT JUPITER
ATMOSPHERES; EXOPLANET HD 209458B; GIANT PLANETS; THERMAL EMISSION;
DISEQUILIBRIUM CARBON; COMBUSTION CHEMISTRY; TERRESTRIAL PLANETS;
DAYSIDE SPECTRUM
AB The hot-Jupiter WASP-12b is a heavily irradiated exoplanet in a short-period orbit around a G0-star with twice the metallicity of the Sun. A recent thermochemical equilibrium analysis based on Spitzer and ground-based infrared observations suggests that the presence of CH4 in its atmosphere and the lack of H2O features can only be explained if the carbon-to-oxygen ratio in the planet's atmosphere is much greater than the solar ratio ([C]/[O] = 0.54). Here, we use a one-dimensional photochemical model to study the effect of disequilibrium chemistry on the observed abundances of H2O, CO, CO2, and CH4 in the WASP-12b atmosphere. We consider two cases: one with solar [C]/[O] and another with [C]/[O] = 1.08. The solar case predicts that H2O and CO are more abundant than CO2 and CH4, as expected, whereas the high [C]/[O] model shows that CO, C2H2, and HCN are more abundant. This indicates that the extra carbon from the high [C]/[O] model is in hydrocarbon species. H2O photolysis is the dominant disequilibrium mechanism that alters the chemistry at higher altitudes in the solar [C]/[O] case, whereas photodissociation of C2H2 and HCN is significant in the super-solar case. Furthermore, our analysis indicates that C2H2 is the major absorber in the atmosphere ofWASP-12b and the absorption features detected near 1.6 and 8 mu m may be arising from C2H2 rather than CH4. The Hubble Space Telescope's WFC3 can resolve this discrepancy, as C2H2 has absorption between 1.51 and 1.54 mu m, while CH4 does not.
C1 [Zahnle, Kevin J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Kopparapu, Ravi Kumar; Kasting, James F.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
FU NASA Astrobiology Institute's Virtual Planetary Laboratory lead team;
NASA [NNH05ZDA001C]; Penn State Astrobiology Research Center
FX The authors thank the referee, Julianne Moses, for pointing out to us
the importance of C2H2 and HCN chemistry and for
in-depth analysis of our work which helped in improved photochemical
models and our current manuscript. R. K. and J.F.K gratefully
acknowledge 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 72
TC 41
Z9 42
U1 0
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 JAN 20
PY 2012
VL 745
IS 1
AR 77
DI 10.1088/0004-637X/745/1/77
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 892WP
UT WOS:000300316600077
ER
PT J
AU Mainzer, A
Masiero, J
Grav, T
Bauer, J
Tholen, DJ
McMillan, RS
Wright, E
Spahr, T
Cutri, RM
Walker, R
Mo, W
Watkins, J
Hand, E
Maleszewski, C
AF Mainzer, A.
Masiero, J.
Grav, T.
Bauer, J.
Tholen, D. J.
McMillan, R. S.
Wright, E.
Spahr, T.
Cutri, R. M.
Walker, R.
Mo, W.
Watkins, J.
Hand, E.
Maleszewski, C.
TI NEOWISE STUDIES OF ASTEROIDS WITH SLOAN PHOTOMETRY: PRELIMINARY RESULTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE atlases; catalogs; infrared: general; minor planets, asteroids: general;
surveys
ID DIGITAL SKY SURVEY; NEAR-EARTH ASTEROIDS; THERMAL-MODEL CALIBRATION;
INFRARED-SURVEY-EXPLORER; MAIN BELT ASTEROIDS; SPECTROSCOPIC SURVEY;
MINOR PLANETS; DATA RELEASE; PHASE-II; TAXONOMY
AB We have combined the NEOWISE and Sloan Digital Sky Survey data to study the albedos of 24,353 asteroids with candidate taxonomic classifications derived using Sloan photometry. We find a wide range of moderate to high albedos for candidate S-type asteroids that are analogous to the S complex defined by previous spectrophotometrically based taxonomic systems. The candidate C-type asteroids, while generally very dark, have a tail of higher albedos that overlaps the S types. The albedo distribution for asteroids with a photometrically derived Q classification is extremely similar to those of the S types. Asteroids with similar colors to (4) Vesta have higher albedos than the S types, and most have orbital elements similar to known Vesta family members. Finally, we show that the relative reflectance at 3.4 and 4.6 mu m is higher for D-type asteroids and suggest that their red visible and near-infrared spectral slope extends out to these wavelengths. Understanding the relationship between size, albedo, and taxonomic classification is complicated by the fact that the objects with classifications were selected from the visible/near-infrared Sloan Moving Object Catalog, which is biased against fainter asteroids, including those with lower albedos.
C1 [Mainzer, A.; Masiero, J.; Bauer, J.; Hand, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Grav, T.; Mo, W.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Bauer, J.; Cutri, R. M.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Tholen, D. J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
[McMillan, R. S.; Maleszewski, C.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Wright, E.; Watkins, J.] UCLA Div Astron & Astrophys, Los Angeles, CA 90095 USA.
[Spahr, T.] Harvard Smithsonian Ctr Astrophys, Minor Planet Ctr, Cambridge, MA 02138 USA.
[Walker, R.] Monterey Inst Res Astron, Monterey, CA USA.
RP Mainzer, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
OI Masiero, Joseph/0000-0003-2638-720X
FU National Aeronautics and Space Administration; Planetary Science
Division of the National Aeronautics and Space Administration
FX This publication makes use of data products from the Widefield Infrared
Survey Explorer, which is a joint project of the University of
California, Los Angeles, and the Jet Propulsion Laboratory/California
Institute of Technology, funded by the National Aeronautics and Space
Administration. This publication also makes use of data products from
NEOWISE, which is a project of the Jet Propulsion Laboratory/California
Institute of Technology, funded by the Planetary Science Division of the
National Aeronautics and Space Administration. We thank our referee, Dr.
Schelte J. Bus, for his comments, which have greatly improved this
paper. We gratefully acknowledge the extraordinary services specific to
NEOWISE contributed by the International Astronomical Union's Minor
Planet Center, operated by the Harvard-Smithsonian Center for
Astrophysics, and the Central Bureau for Astronomical Telegrams,
operated by Harvard University. This research has made use of the
NASA/IPAC Infrared Science Archive, which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with the National Aeronautics and Space Administration.
NR 46
TC 13
Z9 13
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 JAN 20
PY 2012
VL 745
IS 1
AR 7
DI 10.1088/0004-637X/745/1/7
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 892WP
UT WOS:000300316600007
ER
PT J
AU Matt, SP
Pinzon, G
Greene, TP
Pudritz, RE
AF Matt, Sean P.
Pinzon, Giovanni
Greene, Thomas P.
Pudritz, Ralph E.
TI SPIN EVOLUTION OF ACCRETING YOUNG STARS. II. EFFECT OF ACCRETION-POWERED
STELLAR WINDS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; stars: evolution; stars: magnetic field;
stars: pre-main sequence; stars: rotation; stars: winds, outflows
ID T-TAURI STARS; MAGNETOCENTRIFUGALLY DRIVEN FLOWS; ORION NEBULA CLUSTER;
NONPOLYTROPIC ASTROPHYSICAL OUTFLOWS; 2-COMPONENT JET SIMULATIONS;
ANGULAR-MOMENTUM LOSS; LONG-TERM EVOLUTION; MAGNETOSPHERIC ACCRETION;
MAGNETIC-FIELDS; MAIN-SEQUENCE
AB We present amodel for the rotational evolution of a young, solar-mass star interactingmagnetically with an accretion disk. As in a previous paper (Paper I), the model includes changes in the star's mass and radius as it descends the Hayashi track, a decreasing accretion rate, and a prescription for the angular momentum transfer between the star and disk. Paper I concluded that, for the relatively strong magnetic coupling expected in real systems, additional processes are necessary to explain the existence of slowly rotating pre-main-sequence stars. In the present paper, we extend the stellar spin model to include the effect of a spin-down torque that arises from an accretion-powered stellar wind (APSW). For a range of magnetic field strengths, accretion rates, initial spin rates, and mass outflow rates, the modeled stars exhibit rotation periods within the range of 1-10 days in the age range of 1-3 Myr. This range coincides with the bulk of the observed rotation periods, with the slow rotators corresponding to stars with the lowest accretion rates, strongest magnetic fields, and/or highest stellar wind mass outflow rates. We also make a direct, quantitative comparison between the APSW scenario and the two types of disk-locking models (namely, the X-wind and Ghosh & Lamb type models) and identify some remaining theoretical issues for understanding young star spins.
C1 [Matt, Sean P.] Univ Paris Diderot, Lab AIM Paris Saclay, CEA Irfu, CNRS INSU, F-91191 Gif Sur Yvette, France.
[Matt, Sean P.; Greene, Thomas P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Pinzon, Giovanni] Univ Nacl Colombia, Observ Astron Nacl, Fac Ciencias, Bogota, Colombia.
[Pudritz, Ralph E.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada.
RP Matt, SP (reprint author), Univ Paris Diderot, Lab AIM Paris Saclay, CEA Irfu, CNRS INSU, F-91191 Gif Sur Yvette, France.
EM sean.matt@cea.fr; gapinzone@unal.edu.co; thomas.p.greene@nasa.gov;
pudritz@physics.mcmaster.ca
OI Matt, Sean/0000-0001-9590-2274
FU NASA; ERC [207430 STARS2]; NASA via WBS [811073.02.07.01.89]
FX We thank the anonymous referee for useful remarks on the manuscript.
S.P.M. was supported by an appointment to the NASA Postdoctoral Program
at Ames Research Center, administered by Oak Ridge Associated
Universities through a contract with NASA, and by the ERC through grant
207430 STARS2 (http://www.stars2.eu). T.P.G. acknowledges support from
NASA's Origins of Solar Systems program via WBS 811073.02.07.01.89.
NR 117
TC 33
Z9 33
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 JAN 20
PY 2012
VL 745
IS 1
AR 101
DI 10.1088/0004-637X/745/1/101
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 892WP
UT WOS:000300316600101
ER
PT J
AU Sitko, ML
Day, AN
Kimes, RL
Beerman, LC
Martus, C
Lynch, DK
Russell, RW
Grady, CA
Schneider, G
Lisse, CM
Nuth, JA
Cure, M
Henden, AA
Kraus, S
Motta, V
Tamura, M
Hornbeck, J
Williger, GM
Fugazza, D
AF Sitko, Michael L.
Day, Amanda N.
Kimes, Robin L.
Beerman, Lori C.
Martus, Cameron
Lynch, David K.
Russell, Ray W.
Grady, Carol A.
Schneider, Glenn
Lisse, Carey M.
Nuth, Joseph A.
Cure, Michel
Henden, Arne A.
Kraus, Stefan
Motta, Veronica
Tamura, Motohide
Hornbeck, Jeremy
Williger, Gerard M.
Fugazza, Dino
TI VARIABILITY OF DISK EMISSION IN PRE-MAIN SEQUENCE AND RELATED STARS. II.
VARIABILITY IN THE GAS AND DUST EMISSION OF THE HERBIG Fe STAR SAO
206462
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planet-disk interactions; protoplanetary disks; stars: individual (SAO
206462); stars: pre-main sequence; techniques: spectroscopic
ID T-TAURI STARS; INFRARED FILTER SET; YOUNG STELLAR OBJECTS;
PROTOPLANETARY DISK; MAGNETOSPHERIC ACCRETION; TRANSITIONAL DISKS;
TELESCOPE FACILITY; LINE DIAGNOSTICS; OPEN CLUSTERS; DEBRIS DISKS
AB We present 13 epochs of near-infrared (0.8-5 mu m) spectroscopic observations of the pre-transitional, "gapped" disk system in SAO 206462 (=HD 135344B). In all, six gas emission lines (Br alpha, Br gamma, Pa beta, Pa gamma, Pa delta, Pa epsilon, and the 0.8446 mu m line of O I) along with continuum measurements made near the standard J, H, K, and L photometric bands were measured. A mass accretion rate of approximately 2 x 10(-8) M circle dot yr(-1) was derived from the Br gamma and Pa beta lines. However, the fluxes of these lines varied by a factor of over two during the course of a few months. The continuum also varied, but by only similar to 30%, and even decreased at a time when the gas emission was increasing. The H I line at 1.083 mu m was also found to vary in a manner inconsistent with that of either the hydrogen lines or the dust. Both the gas and dust variabilities indicate significant changes in the region of the inner gas and the inner dust belt that may be common to many young disk systems. If planets are responsible for defining the inner edge of the gap, they could interact with the material on timescales commensurate with what is observed for the variations in the dust, while other disk instabilities (thermal, magnetorotational) would operate there on longer timescales than we observe for the inner dust belt. For SAO 206462, the orbital period would likely be 1-3 years. If the changes are being induced in the disk material closer to the star than the gap, a variety of mechanisms (disk instabilities, interactions via planets) might be responsible for the changes seen. The He I feature is most likely due to a wind whose orientation changes with respect to the observer on timescales of a day or less. To further constrain the origin of the gas and dust emission will require multiple spectroscopic and interferometric observations on both shorter and longer timescales that have been sampled so far.
C1 [Sitko, Michael L.; Day, Amanda N.; Kimes, Robin L.; Beerman, Lori C.; Martus, Cameron] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA.
[Sitko, Michael L.] Space Sci Inst, Boulder, CO USA.
[Lynch, David K.; Russell, Ray W.] Aerosp Corp, Los Angeles, CA 90009 USA.
[Grady, Carol A.] Eureka Sci Inc, Oakland, CA 94602 USA.
[Grady, Carol A.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA.
[Schneider, Glenn] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Lisse, Carey M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Cure, Michel; Motta, Veronica] Univ Valparaiso, Dept Fis & Astron, Valparaiso, Chile.
[Henden, Arne A.] Amer Assoc Variable Star Observers, Cambridge, MA 02138 USA.
[Kraus, Stefan] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Tamura, Motohide] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan.
[Hornbeck, Jeremy; Williger, Gerard M.] Univ Louisville, Dept Phys & Astron, Louisville, KY 40292 USA.
[Fugazza, Dino] Osserv Astron Brera, INAF, I-23807 Merate, Italy.
EM sitkoml@ucmail.uc.edu; David.K.Lynch@aero.org; Ray.W.Russell@aero.org;
Carol.A.Grady@nasa.gov; gschneid@email.arizons.edu;
carey.lisse@jhuapl.edu; joseph.a.nuth@nasa.gov; michel.cure@uv.cl;
arne@aavso.org; stefankr@umich.edu; vmotta@dfa.uv.cl;
motohide.tamura@nao.ac.jp; jbhorn02@louisville.edu;
williger@pha.jhu.edu; dino.fugazza@brera.inaf.it
RI Nuth, Joseph/E-7085-2012; Lisse, Carey/B-7772-2016
OI Lisse, Carey/0000-0002-9548-1526
FU NASA ADP [NNH06CC28C, NNX09AC73G]; Hubble Space Telescope grants
[HST-GO-10764, HST-GO-10864]; Chilean National TAC [CNTAC-010A-064,
CNTAC-011A-050]; Aerospace Corporation
FX The authors thank Bill Vacca, Mike Cushing, and John Rayner for many
useful discussions on the use of the SpeX instrument and the Spextool
processing package. We also thank the entire REM team for their
assistance with the scheduling and execution of those observations.
Thanks also to Alex Brown for the use of the unpublished X-ray
luminosity information. More thanks to Nuria Calvet, David Wilner, and
John Monnier for many useful discussions about this star and related
objects. This work was supported by NASA ADP grants NNH06CC28C and
NNX09AC73G, Hubble Space Telescope grants HST-GO-10764 and HST-GO-10864,
Chilean National TAC grants CNTAC-010A-064 and CNTAC-011A-050, and the
IR&D program at The Aerospace Corporation.
NR 67
TC 13
Z9 13
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 JAN 20
PY 2012
VL 745
IS 1
AR 29
DI 10.1088/0004-637X/745/1/29
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 892WP
UT WOS:000300316600029
ER
PT J
AU Summerlin, EJ
Baring, MG
AF Summerlin, Errol J.
Baring, Matthew G.
TI DIFFUSIVE ACCELERATION OF PARTICLES AT OBLIQUE, RELATIVISTIC,
MAGNETOHYDRODYNAMIC SHOCKS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; cosmic rays; gamma-ray burst: general;
magnetohydrodynamics (MHD); shock waves
ID EARTHS BOW SHOCK; ENERGETIC CHARGED-PARTICLES; MAGNETIC-FIELD
GENERATION; MONTE-CARLO SIMULATIONS; COSMIC-RAY ACCELERATION; ACTIVE
GALACTIC NUCLEI; INTERPLANETARY SHOCK; ION-ACCELERATION; COLLISIONLESS
SHOCKS; FERMI ACCELERATION
AB Diffusive shock acceleration (DSA) at relativistic shocks is expected to be an important acceleration mechanism in a variety of astrophysical objects including extragalactic jets in active galactic nuclei and gamma-ray bursts. These sources remain good candidate sites for the generation of ultrahigh energy cosmic rays. In this paper, key predictions of DSA at relativistic shocks that are germane to the production of relativistic electrons and ions are outlined. The technique employed to identify these characteristics is a Monte Carlo simulation of such diffusive acceleration in test-particle, relativistic, oblique, magnetohydrodynamic (MHD) shocks. Using a compact prescription for diffusion of charges in MHD turbulence, this approach generates particle angular and momentum distributions at any position upstream or downstream of the shock. Simulation output is presented for both small angle and large angle scattering scenarios, and a variety of shock obliquities including superluminal regimes when the de Hoffmann-Teller frame does not exist. The distribution function power-law indices compare favorably with results from other techniques. They are found to depend sensitively on the mean magnetic field orientation in the shock, and the nature of MHD turbulence that propagates along fields in shock environs. An interesting regime of flat-spectrum generation is addressed; we provide evidence for it being due to shock drift acceleration, a phenomenon well known in heliospheric shock studies. The impact of these theoretical results on blazar science is outlined. Specifically, Fermi Large Area Telescope gamma-ray observations of these relativistic jet sources are providing significant constraints on important environmental quantities for relativistic shocks, namely, the field obliquity, the frequency of scattering, and the level of field turbulence.
C1 [Summerlin, Errol J.] NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Greenbelt, MD 20770 USA.
[Baring, Matthew G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA.
RP Summerlin, EJ (reprint author), NASA, Goddard Space Flight Ctr, Heliospher Phys Lab, Code 672, Greenbelt, MD 20770 USA.
EM errol.summerlin@nasa.gov; baring@rice.edu
FU NASA [NNX10AC79G, NNG05GD42G]; National Science Foundation [PHY-0758158,
PHY05-51164]
FX We thank the anonymous referee, and Don Ellison and John Kirk for some
comments helpful to the polishing of the manuscript. M. G. B. is
grateful for the generous support of the NASA Astrophysics Theory and
Heliospheric Physics Programs through grants NNX10AC79G and NNG05GD42G,
and the National Science Foundation through grant PHY-0758158. M. G. B.
is also grateful to the Kavli Institute for Theoretical Physics,
University of California, Santa Barbara for hospitality during part of
the period when this research was performed, a visit that was supported
in part by the National Science Foundation under grant No. PHY05-51164.
NR 88
TC 41
Z9 41
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 JAN 20
PY 2012
VL 745
IS 1
AR 63
DI 10.1088/0004-637X/745/1/63
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 892WP
UT WOS:000300316600063
ER
PT J
AU Tassis, K
Gnedin, NY
Kravtsov, AV
AF Tassis, Konstantinos
Gnedin, Nickolay Y.
Kravtsov, Andrey V.
TI ULTRA-FAINT DWARF GALAXIES AS A TEST OF EARLY ENRICHMENT AND
METALLICITY-DEPENDENT STAR FORMATION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: theory; galaxies: evolution; galaxies: formation; methods:
numerical; stars: formation
ID METAL-POOR STARS; KENNICUTT-SCHMIDT RELATION; LY-ALPHA SYSTEMS; CA II
TRIPLET; HIGH-REDSHIFT; INTERSTELLAR-MEDIUM; CHEMICAL EVOLUTION;
FUNDAMENTAL LINE; COLUMN DENSITIES; MAGELLANIC-CLOUD
AB The close relation of star formation with molecular gas indicated by observations and assumed in recent models implies that the efficiency with which galaxies convert their gas into stars depends on gas metallicity. This is because abundance of molecular hydrogen is sensitive to abundance of dust, which catalyzes formation of H-2 and helps to shield it from dissociating radiation. In this study, we point out that in the absence of significant pre-enrichment by Population III stars forming out of zero metallicity gas, such H-2-based star formation is expected to leave an imprint in the form of bi-modality in the metallicity distribution among dwarf galaxies and in the metallicity distribution of stars within individual galaxies. The bi-modality arises because when gas metallicity (and dust abundance) is low, formation of molecular gas is inefficient, the gas consumption timescale is long, and star formation and metal enrichment proceed slowly. When metallicity reaches a critical threshold value star formation and enrichment accelerate, which leads to rapid increase in both stellar mass and metallicity of galaxies. We demonstrate this process both using a simple analytical model and full cosmological simulations. In contrast, the observed metallicity distributions of dwarf galaxies or stars within them are not bi-modal. We argue that this discrepancy points to substantial early stochastic pre-enrichment by Population III stars to levels Z similar to 10(-2) Z(circle dot) in dense, star-forming regions of early galaxies.
C1 [Tassis, Konstantinos] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gnedin, Nickolay Y.] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Gnedin, Nickolay Y.; Kravtsov, Andrey V.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Gnedin, Nickolay Y.; Kravtsov, Andrey V.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Gnedin, Nickolay Y.; Kravtsov, Andrey V.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Kravtsov, Andrey V.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
RP Tassis, K (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
RI Tassis, Konstantinos/C-3155-2011;
OI Tassis, Konstantinos/0000-0002-8831-2038
FU DOE at Fermilab; NSF [AST-0507596, AST-0708154]; NASA [NNX-09AJ54G];
Kavli Institute for Cosmological Physics at the University of Chicago
through the NSF [PHY-0551142]; Fermilab; Kavli Institute for
Cosmological Physics; University of Chicago
FX This work was supported in part by the DOE at Fermilab, by the NSF
grants AST-0507596 and AST-0708154, by the NASA grant NNX-09AJ54G, and
by the Kavli Institute for Cosmological Physics at the University of
Chicago through the NSF grant PHY-0551142 and an endowment from the
Kavli Foundation. The simulations used in this work have been performed
on the Joint Fermilab-KICP Supercomputing Cluster, supported by grants
from Fermilab, Kavli Institute for Cosmological Physics, and the
University of Chicago. Part of this work was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. This
work made extensive use of the NASA Astrophysics Data System and
arXiv.org preprint server.
NR 56
TC 9
Z9 9
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 JAN 20
PY 2012
VL 745
IS 1
AR 68
DI 10.1088/0004-637X/745/1/68
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 892WP
UT WOS:000300316600068
ER
PT J
AU Temim, T
Slane, P
Arendt, RG
Dwek, E
AF Temim, Tea
Slane, Patrick
Arendt, Richard G.
Dwek, Eli
TI INFRARED AND X-RAY SPECTROSCOPY OF THE Kes 75 SUPERNOVA REMNANT SHELL:
CHARACTERIZING THE DUST AND GAS PROPERTIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; infrared: ISM; ISM: individual objects (SNR
G29.7-0.3); ISM: supernova remnants; pulsars: individual (PSR
J1846-0258); X-rays: ISM
ID SPITZER-SPACE-TELESCOPE; LARGE-MAGELLANIC-CLOUD; INTERSTELLAR-MEDIUM;
EARLY UNIVERSE; RADIO OBSERVATIONS; GALACTIC PLANE; PSR J1846-0258;
DESTRUCTION; CASSIOPEIA; PULSAR
AB We present deep Chandra observations and Spitzer Space Telescope infrared (IR) spectroscopy of the shell in the composite supernova remnant (SNR) Kes 75 (G29.7-0.3). The remnant is composed of a central pulsar wind nebula and a bright partial shell in the south that is visible at radio, IR, and X-ray wavelengths. The X-ray emission can be modeled by either a single thermal component with a temperature of similar to 1.5 keV, or with two thermal components with temperatures of 1.5 and 0.2 keV. Previous studies suggest that the hot component may originate from reverse-shocked supernova (SN) ejecta. However, our new analysis shows no definitive evidence for enhanced abundances of Si, S, Ar, Mg, and Fe, as expected from SN ejecta, or for the IR spectral signatures characteristic of confirmed SN condensed dust, thus favoring a circumstellar or interstellar origin for the X-ray and IR emission. The X-ray and IR emission in the shell are spatially correlated, suggesting that the dust particles are collisionally heated by the X-ray emitting gas. The IR spectrum of the shell is dominated by continuum emission from dust with little, or no line emission. Modeling the IR spectrum shows that the dust is heated to a temperature of similar to 140 K by a relatively dense, hot plasma that also gives rise to the hot X-ray emission component. The density inferred from the IR emission is significantly higher than the density inferred from the X-ray models, suggesting a low filling factor for this X-ray emitting gas. The total mass of the warm dust component is at least 1.3 x 10(-2) M-circle dot, assuming no significant dust destruction has occurred in the shell. The IR data also reveal the presence of an additional plasma component with a cooler temperature, consistent with the 0.2 keV gas component. Our IR analysis therefore provides an independent verification of the cooler component of the X-ray emission. The complementary analyses of the X-ray and IR emission provide quantitative estimates of density and filling factors of the clumpy medium swept up by the SNR.
C1 [Temim, Tea; Arendt, Richard G.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Temim, Tea; Dwek, Eli] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA.
[Slane, Patrick] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Arendt, Richard G.] Univ Maryland Baltimore Cty, CRESST, Baltimore, MD 21250 USA.
RP Temim, T (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA.
EM tea.temim@nasa.gov
RI Dwek, Eli/C-3995-2012;
OI Arendt, Richard/0000-0001-8403-8548; Temim, Tea/0000-0001-7380-3144
FU NASA [RSA1343487, NAS8-03060]
FX This work is partly based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology under a contract with NASA. Support
for this work was provided by NASA through an award issued by
JPL/Caltech (RSA1343487). The research has made use of software provided
by the CXC in the application packages CIAO, ChIPS, and Sherpa. P.O.S.
acknowledges partial support from NASA Contract NAS8-03060. We
acknowledge Stephen Reynolds and Kazik Borkwoski at North Carolina State
University for the useful discussion and suggestions, and George
Sonneborn at NASA GSFC for helpful comments.
NR 44
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 JAN 20
PY 2012
VL 745
IS 1
AR 46
DI 10.1088/0004-637X/745/1/46
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 892WP
UT WOS:000300316600046
ER
PT J
AU Traub, WA
AF Traub, Wesley A.
TI TERRESTRIAL, HABITABLE-ZONE EXOPLANET FREQUENCY FROM KEPLER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astronomical databases: miscellaneous; planets and satellites:
detection; stars: statistics
AB Data from Kepler's first 136 days of operation are analyzed to determine the distribution of exoplanets with respect to radius, period, and host-star spectral type. The analysis is extrapolated to estimate the percentage of terrestrial, habitable-zone (HZ) exoplanets. The Kepler census is assumed to be complete for bright stars ( magnitude < 14.0) having transiting planets >0.5 Earth radius and periods <42 days. It is also assumed that the size distribution of planets is independent of orbital period and that there are no hidden biases in the data. Six significant statistical results are found: there is a paucity of small planet detections around faint target stars, probably an instrumental effect; the frequency of mid-size planet detections is independent of whether the host star is bright or faint; there are significantly fewer planets detected with periods <3 days, compared to longer periods, almost certainly an astrophysical effect; the frequency of all planets in the population with periods <42 days is 29%, broken down as terrestrials 9%, ice giants 18%, and gas giants 3%; the population has a planet frequency with respect to period which follows a power-law relation dN/dP similar to P beta-1, with beta similar or equal to 0.71 +/- 0.08; and an extrapolation to longer periods gives the frequency of terrestrial planets in the HZs of FGK stars as eta(circle plus) (34 +/- 14)%. Thus about one-third of FGK stars are predicted to have at least one terrestrial, HZ planet.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Traub, WA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM wtraub@jpl.nasa.gov
FU National Aeronautics and Space Administration
FX I thank the Kepler team for providing such abundant and precise data and
for helpful comments on this paper. I thank the staff at the Computation
Facility of the Harvard-Smithsonian Center for Astrophysics. Finally, I
thank the referees, Jim Kasting and anonymous, who made especially
useful comments, and who therefore had a key influence on the final
version of this paper. Part of this research was carried out at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration.
NR 7
TC 39
Z9 39
U1 0
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 JAN 20
PY 2012
VL 745
IS 1
AR 20
DI 10.1088/0004-637X/745/1/20
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 892WP
UT WOS:000300316600020
ER
PT J
AU Wilkes, BJ
Lal, DV
Worrall, DM
Birkinshaw, M
Haas, M
Willner, SP
Antonucci, R
Ashby, MLN
Avara, M
Barthel, P
Chini, R
Fazio, GG
Hardcastle, M
Lawrence, C
Leipski, C
Ogle, P
Schulz, B
AF Wilkes, Belinda J.
Lal, Dharam V.
Worrall, D. M.
Birkinshaw, Mark
Haas, Martin
Willner, S. P.
Antonucci, Robert
Ashby, M. L. N.
Avara, Mark
Barthel, Peter
Chini, Rolf
Fazio, G. G.
Hardcastle, Martin
Lawrence, Charles
Leipski, Christian
Ogle, Patrick
Schulz, Bernhard
TI CHANDRA X-RAY OBSERVATIONS OF THE REDSHIFT 1.53 RADIO-LOUD QUASAR 3C
270.1
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE quasars: individual: 3C 270.1; X-rays: galaxies: clusters
ID ACTIVE GALACTIC NUCLEI; DUAL-FREQUENCY OBSERVATIONS; MAGNETIC-FIELD
STRENGTHS; ASYMMETRIC DEPOLARIZATION; GALAXIES; JETS; LUMINOSITY;
EMISSION; SPECTRA; VIEW
AB Chandra X-ray observations of the high redshift (z = 1.532) radio-loud quasar 3C 270.1 in 2008 February show the nucleus to have a power-law spectrum, Gamma = 1.66 +/- 0.08, typical of a radio-loud quasar, and a marginally detected Fe K alpha emission line. The data also reveal extended X-ray emission, about half of which is associated with the radio emission from this source. The southern emission is co-spatial with the radio lobe and peaks at the position of the double radio hot spot. Modeling this hot spot, including Spitzer upper limits, rules out synchrotron emission from a single power-law population of electrons, favoring inverse Compton emission with a field of similar to 11 nT, roughly a third of the equipartition value. The northern emission is concentrated close to the location of a 40 degrees bend where the radio jet is presumed to encounter an external medium. It can be explained by inverse Compton emission involving cosmic microwave background photons with a field of similar to 3 nT, a factor of 7-10 below the equipartition value. The remaining, more diffuse X-ray emission is harder (HR = -0.09 +/- 0.22). With only 22.8 +/- 5.6 counts, the spectral form cannot be constrained. Assuming thermal emission with a temperature of 4 keV yields an estimate for the luminosity of 1.8 x 10(44) erg s(-1), consistent with the luminosity-temperature relation of lower-redshift clusters. However, deeper Chandra X-ray observations are required to delineate the spatial distribution and better constrain the spectrum of the diffuse emission to verify that we have detected X-ray emission from a high-redshift cluster.
C1 [Wilkes, Belinda J.; Lal, Dharam V.; Willner, S. P.; Ashby, M. L. N.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Worrall, D. M.; Birkinshaw, Mark] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England.
[Haas, Martin; Chini, Rolf] Ruhr Univ Bochum, Inst Astron, Bochum, Germany.
[Antonucci, Robert] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Avara, Mark] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Barthel, Peter] Univ Groningen, Kapteyn Astron Inst, Groningen, Netherlands.
[Chini, Rolf] Univ Catolica Norte, Inst Astron, Antofagasta, Chile.
[Hardcastle, Martin] Univ Hertfordshire, Sch Phys & Astron, Hatfield AL10 9AB, Herts, England.
[Lawrence, Charles] JPL, Pasadena, CA 91109 USA.
[Leipski, Christian] MPIA, Heidelberg, Germany.
[Ogle, Patrick] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Schulz, Bernhard] CALTECH, IPAC, Pasadena, CA 91125 USA.
RP Wilkes, BJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Hardcastle, Martin/E-2264-2012;
OI Hardcastle, Martin/0000-0003-4223-1117; Wilkes,
Belinda/0000-0003-1809-2364
FU National Aeronautics and Space Administration [G08-9106X]; Chandra X-ray
Center [NAS8-03060]
FX Support for this work was provided by the National Aeronautics and Space
Administration through Chandra Award Number G08-9106X issued by the
Chandra X-ray Center, which is operated by the Smithsonian Astrophysical
Observatory for and on behalf of the National Aeronautics Space
Administration under contract NAS8-03060 (Chandra X-ray Center). The
National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc. Observations reported here were obtained at the MMT
Observatory, a joint facility of the Smithsonian Institution and the
University of Arizona. This work is based in part on observations made
with the Spitzer Space Telescope, which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with NASA.
NR 32
TC 5
Z9 5
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 JAN 20
PY 2012
VL 745
IS 1
AR 84
DI 10.1088/0004-637X/745/1/84
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 892WP
UT WOS:000300316600084
ER
PT J
AU Wuyts, E
Rigby, JR
Gladders, MD
Gilbank, DG
Sharon, K
Gralla, MB
Bayliss, MB
AF Wuyts, Eva
Rigby, Jane R.
Gladders, Michael D.
Gilbank, David G.
Sharon, Keren
Gralla, Megan B.
Bayliss, Matthew B.
TI STELLAR POPULATIONS OF HIGHLY MAGNIFIED LENSED GALAXIES: YOUNG
STARBURSTS AT z similar to 2
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: high-redshift; gravitational lensing: strong; infrared:
galaxies
ID STAR-FORMING GALAXIES; LYMAN BREAK GALAXY; FORMATION RATES;
HIGH-REDSHIFT; MS 1512-CB58; HII-REGIONS; H-ALPHA; LUMINOSITY FUNCTION;
INFRARED GALAXIES; MASSIVE GALAXIES
AB We present a comprehensive analysis of the rest-frame UV to near-IR spectral energy distributions (SEDs) and restframe optical spectra of four of the brightest gravitationally lensed galaxies in the literature: RCSGA032727-132609 at z = 1.70, MS1512-cB58 at z = 2.73, SGAS J152745.1+065219 at z = 2.76, and SGAS J122651.3+ 215220 at z = 2.92. This includes new Spitzer imaging for RCSGA0327 as well as new spectra, near-IR imaging and Spitzer imaging for SGAS1527 and SGAS1226. Lensing magnifications of 3-4 mag allow a detailed study of the stellar populations and physical conditions. We compare star formation rates (SFRs) as measured from the SED fit, the Ha and [O II] lambda 3727 emission lines, and the UV+IR bolometric luminosity where 24 mu m photometry is available. The SFR estimate from the SED fit is consistently higher than the other indicators, which suggests that the Calzetti dust extinction law used in the SED fitting is too flat for young star-forming galaxies at z similar to 2. Our analysis finds similar stellar population parameters for all four lensed galaxies: stellar masses (3-7) x 10(9) M-circle dot, young ages similar to 100 Myr, little dust content E(B - V) = 0.10-0.25, and SFRs around 20-100 M-circle dot yr(-1). Compared to typical values for the galaxy population at z similar to 2, this suggests we are looking at newly formed, starbursting systems that have only recently started the buildup of stellar mass. These results constitute the first detailed, uniform analysis of a sample of the growing number of strongly lensed galaxies known at z similar to 2.
C1 [Wuyts, Eva; Gladders, Michael D.; Gralla, Megan B.; Bayliss, Matthew B.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Wuyts, Eva; Gladders, Michael D.; Sharon, Keren; Gralla, Megan B.; Bayliss, Matthew B.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Rigby, Jane R.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA.
[Gilbank, David G.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
RP Wuyts, E (reprint author), Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
RI Rigby, Jane/D-4588-2012
OI Rigby, Jane/0000-0002-7627-6551
FU Carnegie-Brinson Predoctoral Fellowship
FX We thank the referee for useful comments and suggestions that helped
improve the quality and presentation of the paper. We are grateful to
Vithal Tilvi and James Rhoads for additional observations of SGAS1527
with NIRSPEC. We thank Wiphu Rujopakarn and George Rieke for sharing
their new conversions between 24 mu m emission and IR luminosity for
high-redshift galaxies in advance of publication. We thank Brian Siana
for helpful discussions. E. W. acknowledges support from the
Carnegie-Brinson Predoctoral Fellowship. Data presented in this paper
were partly obtained at the W. M. Keck Observatory from telescope time
allocated to the National Aeronautics and Space Administration through
the scientific partnership with the California Institute of Technology
and the University of California. The Observatory was made possible by
the generous financial support of the W. M. Keck Foundation. We
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.
NR 73
TC 26
Z9 26
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 JAN 20
PY 2012
VL 745
IS 1
AR 86
DI 10.1088/0004-637X/745/1/86
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 892WP
UT WOS:000300316600086
ER
PT J
AU Zank, GP
Dosch, A
Hunana, P
Florinski, V
Matthaeus, WH
Webb, GM
AF Zank, G. P.
Dosch, A.
Hunana, P.
Florinski, V.
Matthaeus, W. H.
Webb, G. M.
TI THE TRANSPORT OF LOW-FREQUENCY TURBULENCE IN ASTROPHYSICAL FLOWS. I.
GOVERNING EQUATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetohydrodynamics (MHD); Sun: heliosphere; turbulence
ID LATITUDE SOLAR-WIND; MAGNETO-HYDRODYNAMIC TURBULENCE; INTERSTELLAR
PICKUP PROTONS; EJECTION-DRIVEN SHOCKS; MAGNETOHYDRODYNAMIC TURBULENCE;
ALFVEN WAVES; RADIAL EVOLUTION; MHD TURBULENCE; INERTIAL-RANGE;
HYDROMAGNETIC TURBULENCE
AB Numerous problems in space physics and astrophysics require a detailed understanding of the transport and dissipation of low-frequency turbulence in an expanding magnetized flow. We employ a scale-separated decomposition of the incompressible MHD equations (based on an Elssasser description) and develop a moment hierarchy to describe the transport of the total energy density in fluctuations, the cross-helicity, the energy difference, and correlation lengths corresponding to forward-and backward-propagating modes and to the energy difference. The dissipation terms for the various transport equations are derived. One-point closure schemes are utilized. The technical elements of this work that distinguish it from previous studies are (1) the inclusion of the large-scale background inhomogeneous Alfvenic velocity V-A at a level of detail greater than before, (2) the introduction of a tractable slow timescale closure to eliminate high-frequency interference terms that is likely to prove a useful approximation for practical problems related to the transport of turbulence in an inhomogeneous flow such as the solar wind or solar corona, and finally, (3) we develop a simplified phenomenology for the energy difference or equivalently residual energy that may be useful for practical applications. This yields a coupled system of six equations that describes the transport of turbulence in inhomogeneous sub-Alfvenic and super-Alfvenic flows. The turbulence transport equations are quasi-linear in their spatial evolution operators and nonlinear in the dissipation terms, making the model equations relatively tractable to analysis.
C1 [Zank, G. P.; Dosch, A.; Florinski, V.; Webb, G. M.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35805 USA.
[Zank, G. P.; Florinski, V.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
[Hunana, P.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-06304 Nice 4, France.
[Hunana, P.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Matthaeus, W. H.] Univ Delaware, Bartol Res Inst, Newark, DE 19711 USA.
RP Zank, GP (reprint author), Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35805 USA.
RI Hunana, Peter/H-6239-2012
FU NASA [NNX08AJ33G, 37102-2, NNX09AG70G, NNX09AG63G, NNX09AJ79G,
NNG05EC85C, A991132BT, NNX09AP74A, NNX10AE46G, NNX09AW45G]; NSF
[ATM-0904007]
FX 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. P.H. was supported by the NASA Postdoctoral Program which
is administered by ORAU.
NR 94
TC 31
Z9 31
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 20
PY 2012
VL 745
IS 1
AR 35
DI 10.1088/0004-637X/745/1/35
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 892WP
UT WOS:000300316600035
ER
PT J
AU Nikzad, S
Hoenk, ME
Greer, F
Jacquot, B
Monacos, S
Jones, TJ
Blacksberg, J
Hamden, E
Schiminovich, D
Martin, C
Morrissey, P
AF Nikzad, Shouleh
Hoenk, Michael E.
Greer, Frank
Jacquot, Blake
Monacos, Steve
Jones, Todd J.
Blacksberg, Jordana
Hamden, Erika
Schiminovich, David
Martin, Chris
Morrissey, Patrick
TI Delta-doped electron-multiplied CCD with absolute quantum efficiency
over 50% in the near to far ultraviolet range for single photon counting
applications
SO APPLIED OPTICS
LA English
DT Article
ID CHARGE-COUPLED-DEVICE; SILICON; PHOTODIODES; INTENSIFIER; DETECTOR;
DESIGN
AB We have used molecular beam epitaxy (MBE) based delta-doping technology to demonstrate nearly 100% internal quantum efficiency (QE) on silicon electron-multiplied charge-coupled devices (EMCCDs) for single photon counting detection applications. We used atomic layer deposition (ALD) for antireflection (AR) coatings and achieved atomic-scale control over the interfaces and thin film materials parameters. By combining the precision control of MBE and ALD, we have demonstrated more than 50% external QE in the far and near ultraviolet in megapixel arrays. We have demonstrated that other important device performance parameters such as dark current are unchanged after these processes. In this paper, we briefly review ultraviolet detection, report on these results, and briefly discuss the techniques and processes employed. (C) 2012 Optical Society of America
C1 [Nikzad, Shouleh; Hoenk, Michael E.; Greer, Frank; Jacquot, Blake; Monacos, Steve; Jones, Todd J.; Blacksberg, Jordana] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Hamden, Erika; Schiminovich, David] Columbia Univ, New York, NY 10025 USA.
[Martin, Chris; Morrissey, Patrick] CALTECH, Pasadena, CA 91125 USA.
RP Nikzad, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Shouleh.Nikzad@jpl.nasa.gov
FU NASA
FX The work presented in this paper was performed by the Jet Propulsion
Laboratory (JPL), California Institute of Technology, under a contract
with NASA. We gratefully acknowledge the generous collaborative effort
by e2v Inc. and helpful discussions with Peter Pool, Paul Jorden, and
Paul Jerram of e2v.
NR 25
TC 17
Z9 17
U1 0
U2 4
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD JAN 20
PY 2012
VL 51
IS 3
BP 365
EP 369
DI 10.1364/AO.51.000365
PG 5
WC Optics
SC Optics
GA 891YE
UT WOS:000300252100011
PM 22270664
ER
PT J
AU Bloemhof, EE
An, X
Kuan, G
Moore, D
O'Shay, B
Page, N
Tang, H
AF Bloemhof, E. E.
An, X.
Kuan, G.
Moore, D.
O'Shay, B.
Page, N.
Tang, H.
TI Telescope alignment from sparsely sampled wavefront measurements over
pupil subapertures
SO APPLIED OPTICS
LA English
DT Article
ID OPTICAL-SYSTEMS; COLLIMATION
AB We present a simple formalism that has proven useful in on-axis alignment of two-element telescopes when wavefront information is available from only a limited region (here two noncontiguous subapertures) of the pupil. Misalignments cause predictable full-aperture aberrations, which in turn cause predictable tip/tilt modes in the subapertures. For the most useful case in which secondary mirror tilts are independently constrained by optical monitoring, the four subaperture tip/tilt modes provide enough information to solve for the state of misalignment uniquely. A practically important and intuitively appealing simplification of this inversion occurs if the tip/tilts of the two subapertures are first transformed into a new basis consisting of differential and common-mode tilts in each of the x and y directions. Then the matrices interpreting subaperture modes as full-aperture aberrations and those in turn as mechanical misalignments become diagonal, so the mechanical adjustment required to align each degree of freedom is just a constant sensitivity multiplying one of the measured differential or common-mode tilt basis modes. Knowing that this simplification occurs allows rapid empirical calibration of sensitivities in the lab and then deterministic alignment, simply and transparently, with no need for ray tracing to model the optical effects of the adjustments at each step of the alignment.
C1 [Bloemhof, E. E.] Natl Sci Fdn, Arlington, VA 22230 USA.
[An, X.; Kuan, G.; Moore, D.; O'Shay, B.; Page, N.; Tang, H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Bloemhof, EE (reprint author), Natl Sci Fdn, 4201 Wilson Blvd, Arlington, VA 22230 USA.
EM ebloemho@nsf.gov
FU SIM; Exoplanet Exploration Program office; National Aeronautics and
Space Administration
FX We thank Jim Marr of the SIM project and Mike Devirian of the Exoplanet
Exploration Program office for supporting this work and its publication.
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. Any
opinion, finding, and conclusions or recommendations expressed in this
material are those of the authors and do not necessarily reflect the
views of the National Science Foundation (NSF).
NR 12
TC 0
Z9 1
U1 4
U2 4
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD JAN 20
PY 2012
VL 51
IS 3
BP 394
EP 400
DI 10.1364/AO.51.000394
PG 7
WC Optics
SC Optics
GA 891YE
UT WOS:000300252100016
PM 22270669
ER
PT J
AU Lin, YT
Stanford, SA
Eisenhardt, PRM
Vikhlinin, A
Maughan, BJ
Kravtsov, A
AF Lin, Yen-Ting
Stanford, S. Adam
Eisenhardt, Peter R. M.
Vikhlinin, Alexey
Maughan, Ben J.
Kravtsov, Andrey
TI BARYON CONTENT OF MASSIVE GALAXY CLUSTERS AT z=0-0.6
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: clusters: general; galaxies: clusters: intracluster medium;
galaxies: elliptical and lenticular, cD; galaxies: luminosity function,
mass function
ID LUMINOSITY FUNCTION; STELLAR; GAS; PROJECT; LIGHT
AB We study the relationship between two major baryonic components in galaxy clusters, namely the stars in galaxies and the ionized gas in the intracluster medium (ICM), using 94 clusters that span the redshift range 0-0.6. Accurately measured total and ICM masses from Chandra observations and stellar masses derived from the Wide-field Infrared Survey Explorer and the Two Micron All Sky Survey allow us to trace the evolution of cluster baryon content in a self-consistent fashion. We find that, within r(500), the evolution of the ICM-mass-total-mass relation is consistent with the expectation of the self-similar model, while there is no evidence for redshift evolution in the stellar-mass-total-mass relation. This suggests that the stellar mass and ICM mass in the inner parts of clusters evolve differently.
C1 [Lin, Yen-Ting] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan.
[Lin, Yen-Ting] Univ Tokyo, Todai Inst Adv Study, Inst Phys & Math Universe, Kashiwa, Chiba, Japan.
[Stanford, S. Adam] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Stanford, S. Adam] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA.
[Eisenhardt, Peter R. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Vikhlinin, Alexey] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Maughan, Ben J.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England.
[Kravtsov, Andrey] Univ Chicago, Kavli Inst Cosmol Phys, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Kravtsov, Andrey] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
RP Lin, YT (reprint author), Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan.
EM ytl@asiaa.sinica.edu.tw
FU World Premier International Research Center Initiative, MEXT, Japan; NSF
[NSF PHY05-51164]; NASA; 2MASS; UMass; IPAC/Caltech; Sloan Foundation
FX We are very grateful to G. Bruzual and S. Charlot for providing an
updated version of their model, to M. Tanaka and C. Mancone for help
with the BC model predictions, and to an anonymous referee for very
helpful comments. Y.T.L. thanks E. Komatsu, J. Gunn, C. Conroy, M.
Fukugita, M. Takada, and D. Spergel for helpful discussions, and I. H.
for constant encouragement. Y.T.L. acknowledges supports from the World
Premier International Research Center Initiative, MEXT, Japan. This
research was supported in part by the NSF under grant no. NSF
PHY05-51164. This publication makes use of data products from WISE, a
joint project of UCLA and JPL/Caltech, funded by NASA, and 2MASS, a
joint project of UMass and IPAC/Caltech, funded by NASA and NSF. Funding
for SDSS-III has been provided by the Sloan Foundation, the
Participating Institutions, NSF, and DOE. This work makes use of data
from CFHTLS and UKIDSS.
NR 30
TC 39
Z9 39
U1 0
U2 1
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 JAN 20
PY 2012
VL 745
IS 1
AR L3
DI 10.1088/2041-8205/745/1/L3
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 891PC
UT WOS:000300228100003
ER
PT J
AU Hu, CM
Lee, Z
Franz, B
AF Hu, Chuanmin
Lee, Zhongping
Franz, Bryan
TI Chlorophyll a algorithms for oligotrophic oceans: A novel approach based
on three-band reflectance difference
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID SPECTRAL-CURVATURE ALGORITHMS; AEROSOL OPTICAL-THICKNESS; WATER-LEAVING
RADIANCES; ATMOSPHERIC CORRECTION; IMAGING SPECTROMETER; GLOBAL OCEAN;
COLOR OBSERVATIONS; COASTAL WATERS; SEAWIFS OCEAN; BAND-RATIO
AB A new empirical algorithm is proposed to estimate surface chlorophyll a (Chl) concentrations in the global ocean for Chl <= 0.25 mg m(-3) (similar to 78% of the global ocean area). The algorithm is based on a color index (CI), defined as the difference between remote-sensing reflectance (R-rs, sr(-1)) in the green and a reference formed linearly between R-rs in the blue and red. For low-Chl waters, in situ data showed a tighter (and therefore better) relationship between CI and Chl than between traditional band ratios and Chl, which was further validated using global data collected concurrently by ship-borne and Sea-viewing Wide Field-of-view Sensor (SeaWiFS) and Moderate Resolution Imaging Spectroradiometer (MODIS)/Aqua instruments. Model simulations showed that for low-Chl waters, compared with the band-ratio algorithm, the CI-based algorithm (CIA) was more tolerant to changes in chlorophyll-specific backscattering coefficient and performed similarly for different relative contributions of nonphytoplankton absorption. Simulations using existing atmospheric correction approaches further demonstrated that the CIA was much less sensitive than band-ratio algorithms to various errors induced by instrument noise and imperfect atmospheric correction (including sun glint and whitecap corrections). Image and time series analyses of SeaWiFS and MODIS/Aqua data also showed improved performance in terms of reduced image noise, more coherent spatial and temporal patterns, and better consistency between the two sensors. The reduction in noise and other errors is particularly useful to improve the detection of various ocean features such as eddies. Preliminary tests over Medium-Resolution Imaging Spectrometer and Coastal Zone Color Scanner data indicate that the new approach should be generally applicable to all past, current, and future ocean color instruments.
C1 [Hu, Chuanmin] Univ S Florida, Coll Marine Sci, St Petersburg, FL 33701 USA.
[Franz, Bryan] NASA GSFC, Greenbelt, MD 20771 USA.
[Lee, Zhongping] Univ Massachusetts, Dept Environm Earth & Ocean Sci, Boston, MA 02125 USA.
RP Hu, CM (reprint author), Univ S Florida, Coll Marine Sci, St Petersburg, FL 33701 USA.
EM hu@marine.usf.edu
RI Franz, Bryan/D-6284-2012; hu, chuanmin/J-5021-2012
OI Franz, Bryan/0000-0003-0293-2082;
FU NASA; Gulf of Mexico program; Energy and Water Cycle program; Naval
Research Lab
FX This work is impossible without the collective effort from the entire
ocean color community, from sensor calibration, field campaign,
algorithm development, product validation, to data sharing. We are
particularly thankful to the researchers who collected and contributed
in situ bio-optical data to the SeaBASS archive, as well as to the
NASA/GSFC OBPG team (Sean Bailey and Jeremy Werdell) who quality
controlled, maintained, and distributed the data set for community use.
We thank Howard Gordon (University of Miami) for the useful discussions
on atmospheric correction uncertainties. We also thank the NASA/GSFC for
sharing the global ocean color data at all data levels. Financial
support has been provided by the NASA Ocean Biology and Biogeochemistry
(OBB) program (Hu, Lee, Franz), Gulf of Mexico program (Hu, Lee), the
Energy and Water Cycle program (Lee, Hu), and the Naval Research Lab
(Lee). We are indebted to two anonymous reviewers who provided numerous
suggestions to improve the quality of this work.
NR 80
TC 72
Z9 74
U1 3
U2 25
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 JAN 20
PY 2012
VL 117
AR C01011
DI 10.1029/2011JC007395
PG 25
WC Oceanography
SC Oceanography
GA 880FP
UT WOS:000299390600002
ER
PT J
AU Schrijver, CJ
Brown, JC
Battams, K
Saint-Hilaire, P
Liu, W
Hudson, H
Pesnell, WD
AF Schrijver, C. J.
Brown, J. C.
Battams, K.
Saint-Hilaire, P.
Liu, W.
Hudson, H.
Pesnell, W. D.
TI Destruction of Sun-Grazing Comet C/2011 N3 (SOHO) Within the Low Solar
Corona
SO SCIENCE
LA English
DT Article
AB Observations of comets in Sun-grazing orbits that survive solar insolation long enough to penetrate into the Sun's inner corona provide information on the solar atmosphere and magnetic field as well as on the makeup of the comet. On 6 July 2011, the Solar Dynamics Observatory (SDO) observed the demise of comet C/2011 N3 (SOHO) within the low solar corona in five wavelength bands in the extreme ultraviolet (EUV). The comet penetrated to within 0.146 solar radius (similar to 100,000 kilometers) of the solar surface before its EUV signal disappeared. Before that, material released into the coma-at first seen in absorption-formed a variable EUV-bright tail. During the final 10 minutes of observation by SDO's Atmospheric Imaging Assembly, similar to 6 x 10(8) to 6 x 10(10) grams of total mass was lost (corresponding to an effective nucleus diameter of similar to 10 to 50 meters), as estimated from the tail's deceleration due to interaction with the surrounding coronal material; the EUV absorption by the comet and the brightness of the tail suggest that the mass was at the high end of this range. These observations provide evidence that the nucleus had broken up into a family of fragments, resulting in accelerated sublimation in the Sun's intense radiation field.
C1 [Schrijver, C. J.; Liu, W.] Lockheed Martin Adv Technol Ctr, Palo Alto, CA 94304 USA.
[Brown, J. C.; Hudson, H.] Univ Glasgow, Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland.
[Battams, K.] USN, Res Lab, Washington, DC 20375 USA.
[Saint-Hilaire, P.; Hudson, H.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Liu, W.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Pesnell, W. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Schrijver, CJ (reprint author), Lockheed Martin Adv Technol Ctr, 3251 Hanover St, Palo Alto, CA 94304 USA.
EM schrijver@lmsal.com
RI Pesnell, William/D-1062-2012
OI Pesnell, William/0000-0002-8306-2500
FU NASA SDO/AIA [NNG04EA00C]
FX Supported by NASA SDO/AIA contract NNG04EA00C to Lockheed Martin's Solar
and Astrophysics Laboratory. The SDO/AIA data can be accessed at
http://aia.lmsal.com; the STEREO/SECCHI data can be accessed at
http://stereo-ssc.nascom.nasa.gov/data/ins_data/secchi. We thank the
four reviewers and the editor for their help in improving the
manuscript.
NR 10
TC 15
Z9 15
U1 0
U2 3
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 JAN 20
PY 2012
VL 335
IS 6066
BP 324
EP 328
DI 10.1126/science.1211688
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 878RE
UT WOS:000299273400044
PM 22267810
ER
PT J
AU De Lannoy, GJM
Reichle, RH
Arsenault, KR
Houser, PR
Kumar, S
Verhoest, NEC
Pauwels, VRN
AF De Lannoy, Gabrielle J. M.
Reichle, Rolf H.
Arsenault, Kristi R.
Houser, Paul R.
Kumar, Sujay
Verhoest, Niko E. C.
Pauwels, Valentijn R. N.
TI Multiscale assimilation of Advanced Microwave Scanning Radiometer-EOS
snow water equivalent and Moderate Resolution Imaging Spectroradiometer
snow cover fraction observations in northern Colorado
SO WATER RESOURCES RESEARCH
LA English
DT Article
ID LAND-SURFACE MODEL; ENSEMBLE KALMAN FILTER; PASSIVE MICROWAVE;
INFORMATION-SYSTEM; DEPLETION CURVES; MODIS; VARIABILITY; CLIMATE;
DEPTH; UNCERTAINTY
AB Eight years (2002-2010) of Advanced Microwave Scanning Radiometer-EOS (AMSR-E) snow water equivalent (SWE) retrievals and Moderate Resolution Imaging Spectroradiometer (MODIS) snow cover fraction (SCF) observations are assimilated separately or jointly into the Noah land surface model over a domain in Northern Colorado. A multiscale ensemble Kalman filter (EnKF) is used, supplemented with a rule-based update. The satellite data are either left unscaled or are scaled for anomaly assimilation. The results are validated against in situ observations at 14 high-elevation Snowpack Telemetry (SNOTEL) sites with typically deep snow and at 4 lower-elevation Cooperative Observer Program (COOP) sites. Assimilation of coarse-scale AMSR-E SWE and fine-scale MODIS SCF observations both result in realistic spatial SWE patterns. At COOP sites with shallow snowpacks, AMSR-E SWE and MODIS SCF data assimilation are beneficial separately, and joint SWE and SCF assimilation yields significantly improved root-mean-square error and correlation values for scaled and unscaled data assimilation. In areas of deep snow where the SNOTEL sites are located, however, AMSR-E retrievals are typically biased low and assimilation without prior scaling leads to degraded SWE estimates. Anomaly SWE assimilation could not improve the interannual SWE variations in the assimilation results because the AMSR-E retrievals lack realistic interannual variability in deep snowpacks. SCF assimilation has only a marginal impact at the SNOTEL locations because these sites experience extended periods of near-complete snow cover. Across all sites, SCF assimilation improves the timing of the onset of the snow season but without a net improvement of SWE amounts.
C1 [De Lannoy, Gabrielle J. M.; Verhoest, Niko E. C.; Pauwels, Valentijn R. N.] Univ Ghent, Lab Hydrol & Water Management, B-9000 Ghent, Belgium.
[Arsenault, Kristi R.; Houser, Paul R.] George Mason Univ, Dept Atmospher Ocean & Earth Sci, Calverton, MD 20705 USA.
[De Lannoy, Gabrielle J. M.; Reichle, Rolf H.; Kumar, Sujay] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP De Lannoy, GJM (reprint author), Univ Ghent, Lab Hydrol & Water Management, Coupure Links 653, B-9000 Ghent, Belgium.
EM gabrielle.delannoy@ugent.be
RI Reichle, Rolf/E-1419-2012; Verhoest, Niko/C-9726-2010; Houser,
Paul/J-9515-2013; Kumar, Sujay/B-8142-2015;
OI Verhoest, Niko/0000-0003-4116-8881; Houser, Paul/0000-0002-2991-0441;
Pauwels, Valentijn/0000-0002-1290-9313
FU NASA
FX Gabrielle De Lannoy is a postdoctoral research fellow of the Research
Foundation Flanders (FWO). Rolf Reichle was supported by the NASA
program on Earth System Science Research using Data and Products from
the Terra, Aqua, and ACRIMSAT Satellites. We acknowledge IGES/CREW for
the use of computer facilities during the first author's research visit
(NA07OAR4310221). Thanks go also to James Foster and Richard Kelly for
their shared insight in the AMSR-E SWE data, to the reviewers for their
constructive comments, and to Bart Forman and Ally Toure for helpful
discussions.
NR 86
TC 55
Z9 55
U1 5
U2 27
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0043-1397
EI 1944-7973
J9 WATER RESOUR RES
JI Water Resour. Res.
PD JAN 19
PY 2012
VL 48
AR W01522
DI 10.1029/2011WR010588
PG 17
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA 880DS
UT WOS:000299385500004
ER
PT J
AU Williams, CA
Collatz, GJ
Masek, J
Goward, SN
AF Williams, Christopher A.
Collatz, G. James
Masek, Jeffrey
Goward, Samuel N.
TI Carbon consequences of forest disturbance and recovery across the
conterminous United States
SO GLOBAL BIOGEOCHEMICAL CYCLES
LA English
DT Article
ID NET PRIMARY PRODUCTIVITY; LAND-USE CHANGE; ATMOSPHERIC CO2; BOREAL
FOREST; ECOSYSTEM PRODUCTION; CONIFER FOREST; US FORESTS; LONG-TERM;
FLUXES; GROWTH
AB Forests of North America are thought to constitute a significant long-term sink for atmospheric carbon. The United States Forest Service Forest Inventory and Analysis (FIA) program has developed a large database of stock changes derived from consecutive estimates of growing stock volume in the U.S. These data reveal a large and relatively stable increase in forest carbon stocks over the last two decades or more. The mechanisms underlying this national increase in forest stocks may include recovery of forests from past disturbances, net increases in forest area, and growth enhancement driven by climate or fertilization by CO2 and Nitrogen. Here we estimate the forest recovery component of the observed stock changes using FIA data on the age structure of U.S. forests and carbon stocks as a function of age. The latter are used to parameterize forest disturbance and recovery processes in a carbon cycle model. We then apply resulting disturbance/recovery dynamics to landscapes and regions based on the forest age distributions. The analysis centers on 28 representative climate settings spread about forested regions of the conterminous U.S. We estimate carbon fluxes for each region and propagate uncertainties in calibration data through to the predicted fluxes. The largest recovery-driven carbon sinks are found in the South Central, Pacific Northwest, and Pacific Southwest regions, with spatially averaged net ecosystem productivity (NEP) of about 100 g C m(-2) a(-1) driven by forest age structure. Carbon sinks from recovery in the Northeast and Northern Lakes States remain moderate to large owing to the legacy of historical clearing and relatively low modern disturbance rates from harvest and fire. At the continental scale, we find a conterminous U.S. forest NEP of only 0.16 Pg C a(-1) from age structure in 2005, or only 0.047 Pg C a(-1) of forest stock change after accounting for fire emissions and harvest transfers. Recent estimates of NEP derived from inventory stock change, harvest, and fire data show twice the NEP sink we derive from forest age distributions. We discuss possible reasons for the discrepancies including modeling errors and the possibility of climate and/or fertilization (CO2 or N) growth enhancements.
C1 [Williams, Christopher A.] Clark Univ, Grad Sch Geog, Worcester, MA 01610 USA.
[Collatz, G. James; Masek, Jeffrey] NASA, Biospher Sci Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Goward, Samuel N.] Univ Maryland, Dept Geog, College Pk, MD 20782 USA.
RP Williams, CA (reprint author), Clark Univ, Grad Sch Geog, 950 Main St, Worcester, MA 01610 USA.
EM cwilliams@clarku.edu
RI collatz, george/D-5381-2012; Masek, Jeffrey/D-7673-2012
FU NASA [NNH05ZDA001N]; North American Carbon Program; U.S. National
Science Foundation [ATM-0910766]
FX We thank Charles (Chip) Scott and his team at the USFS National
Inventory and Monitoring Applications Center for providing us with FIA
data. We acknowledge helpful discussions and/or comments from Skee
Houghton, Jim Randerson, Warren Cohen, Linda Heath, and an anonymous
reviewer. This work was funded by NASA NNH05ZDA001N, North American
Carbon Program. In addition, CAW was supported by the U.S. National
Science Foundation under grant ATM-0910766.
NR 79
TC 50
Z9 51
U1 1
U2 55
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0886-6236
EI 1944-9224
J9 GLOBAL BIOGEOCHEM CY
JI Glob. Biogeochem. Cycle
PD JAN 18
PY 2012
VL 26
AR GB1005
DI 10.1029/2010GB003947
PG 13
WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric
Sciences
GA 880FF
UT WOS:000299389500001
ER
PT J
AU Heays, AN
Lewis, BR
Gibson, ST
Malone, CP
Johnson, PV
Kanik, I
Khakoo, MA
AF Heays, A. N.
Lewis, B. R.
Gibson, S. T.
Malone, C. P.
Johnson, P. V.
Kanik, I.
Khakoo, M. A.
TI Tuning out vibrational levels in molecular electron energy-loss spectra
SO PHYSICAL REVIEW A
LA English
DT Article
ID SCATTERING CROSS-SECTIONS; OSCILLATOR-STRENGTHS; DIATOMIC-MOLECULES;
IMPACT EXCITATION; N-2; STATES; O-2; PREDISSOCIATION; PERTURBATIONS;
ABSORPTION
AB The phenomenon whereby features associated with certain vibrational levels in molecular states of mixed electronic character disappear under specific scattering conditions in electron energy-loss spectra is investigated. In particular, using a combination of experimental measurements and coupled-channel calculations, anomalous vibrational intensities in the mixed valence-Rydberg (1)Pi(u) <- X (1)Sigma(+)(g) transition of N(2) are explained. A single parameter, i. e., the ratio of the generalized electronic transition moments to the diabatic valence and Rydberg components of the mixed states, dependent on the experimental scattering conditions, is found to be essentially capable of describing all observed relative vibrational intensities, including the near disappearance of the b (1)Pi(u) (v = 5) feature for momentum-transfer-squared values K(2) approximate to 0.3 a. u. This result highlights the interesting possibility of experimental control of molecular quantum-interference effects in electron energy-loss spectra, something that is not possible in optical spectra.
C1 [Heays, A. N.; Lewis, B. R.; Gibson, S. T.] Australian Natl Univ, Res Sch Phys & Engn, Canberra, ACT 0200, Australia.
[Malone, C. P.; Johnson, P. V.; Kanik, I.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Khakoo, M. A.] Calif State Univ Fullerton, Dept Phys, Fullerton, CA 92834 USA.
RP Heays, AN (reprint author), Australian Natl Univ, Res Sch Phys & Engn, GPO Box 4, Canberra, ACT 0200, Australia.
RI Malone, Charles/A-6294-2010; Johnson, Paul/D-4001-2009;
OI Malone, Charles/0000-0001-8418-1539; Johnson, Paul/0000-0002-0186-8456;
Gibson, Stephen/0000-0002-3767-6114; Heays, Alan/0000-0002-7716-9192
FU Australian Research Council [DP0558962, DP0773050]; National Aeronautics
and Space Administration (NASA); National Science Foundation
[NSF-PHY-RUI-0653452, NSF-AGS-0938223]
FX The theoretical component of this work was supported by the Australian
Research Council Discovery Program, through Grants No. DP0558962 and No.
DP0773050. Experimental aspects of this work were performed at the Jet
Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration (NASA),
and at the California State University, Fullerton. Financial support
through NASA's Planetary Atmospheres and Outer Planets research
programs, and the National Science Foundation (Grants No.
NSF-PHY-RUI-0653452 and No. NSF-AGS-0938223) is gratefully acknowledged.
NR 49
TC 3
Z9 3
U1 2
U2 14
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 JAN 18
PY 2012
VL 85
IS 1
AR 012705
DI 10.1103/PhysRevA.85.012705
PG 8
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 878NY
UT WOS:000299265000004
ER
PT J
AU Liu, D
Hostetler, C
Miller, I
Cook, A
Hair, J
AF Liu, Dong
Hostetler, Chris
Miller, Ian
Cook, Anthony
Hair, Johnathan
TI System analysis of a tilted field-widened Michelson interferometer for
high spectral resolution lidar
SO OPTICS EXPRESS
LA English
DT Article
ID AEROSOL EXTINCTION; COEFFICIENTS; PROFILES
AB High spectral resolution lidars (HSRLs) have shown great value in aircraft aerosol remote sensing application and are planned for future satellite missions. A compact, robust, quasi-monolithic tilted field-widened Michelson interferometer is being developed as the spectral discrimination filter for an second-generation HSRL(HSRL-2) at NASA Langley Research Center. The Michelson interferometer consists of a cubic beam splitter, a solid arm and an air arm. Piezo stacks connect the air arm mirror to the body of the interferometer and can tune the interferometer within a small range. The whole interferometer is tilted so that the standard Michelson output and the reflected complementary output can both be obtained. In this paper, the transmission ratio is proposed to evaluate the performance of the spectral filter for HSRL. The transmission ratios over different types of system imperfections, such as cumulative wavefront error, locking error, reflectance of the beam splitter and anti-reflection coatings, system tilt, and depolarization angle are analyzed. The requirements of each imperfection for good interferometer performance are obtained. (C)2012 Optical Society of America
C1 [Liu, Dong; Hostetler, Chris; Cook, Anthony; Hair, Johnathan] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
[Miller, Ian] LightMachinery Inc, Nepean, ON K2E 7L2, Canada.
RP Liu, D (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM dong.liu@nasa.gov
RI Liu, Dong/F-9016-2012
FU NASA at NASA Langley Research Center
FX This research was supported by NASA Postdoctoral Program at NASA Langley
Research Center, administered by Oak Ridge Associated Universities
through a contract with NASA.
NR 18
TC 19
Z9 23
U1 3
U2 19
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD JAN 16
PY 2012
VL 20
IS 2
BP 1406
EP 1420
DI 10.1364/OE.20.001406
PG 15
WC Optics
SC Optics
GA 889EZ
UT WOS:000300057700070
PM 22274485
ER
PT J
AU Mazin, BA
Bumble, B
Meeker, SR
O'Brien, K
McHugh, S
Langman, E
AF Mazin, Benjamin A.
Bumble, Bruce
Meeker, Seth R.
O'Brien, Kieran
McHugh, Sean
Langman, Eric
TI A superconducting focal plane array for ultraviolet, optical, and
near-infrared astrophysics
SO OPTICS EXPRESS
LA English
DT Article
ID SPECTROPHOTOMETER
AB Microwave Kinetic Inductance Detectors, or MKIDs, have proven to be a powerful cryogenic detector technology due to their sensitivity and the ease with which they can be multiplexed into large arrays. A MKID is an energy sensor based on a photon-variable superconducting inductance in a lithographed microresonator, and is capable of functioning as a photon detector across the electromagnetic spectrum as well as a particle detector. Here we describe the first successful effort to create a photon-counting, energy-resolving ultraviolet, optical, and near infrared MKID focal plane array. These new Optical Lumped Element (OLE) MKID arrays have significant advantages over semiconductor detectors like charge coupled devices (CCDs). They can count individual photons with essentially no false counts and determine the energy and arrival time of every photon with good quantum efficiency. Their physical pixel size and maximum count rate is well matched with large telescopes. These capabilities enable powerful new astrophysical instruments usable from the ground and space. MKIDs could eventually supplant semiconductor detectors for most astronomical instrumentation, and will be useful for other disciplines such as quantum optics and biological imaging. (C) 2012 Optical Society of America
C1 [Mazin, Benjamin A.; Meeker, Seth R.; O'Brien, Kieran; McHugh, Sean; Langman, Eric] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Bumble, Bruce] NASA, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mazin, BA (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
EM bmazin@physics.ucsb.edu
RI Mazin, Ben/B-8704-2011
OI Mazin, Ben/0000-0003-0526-1114
FU National Aeronautics and Space Administration through Science Mission
Directorate [NNX09AD54G]; Jet Propulsion Laboratory, California
Institute of Technology, under the National Aeronautics and Space
Administration; Jet Propulsion Lab; W.M. Keck Institute for Space
Studies; National Aeronautics and Space Administration
FX This material is based upon work supported by the National Aeronautics
and Space Administration under Grant NNX09AD54G, issued through the
Science Mission Directorate, Jet Propulsion Lab's Research & Technology
Development Program, and a grant from the W.M. Keck Institute for Space
Studies. Part of the research was carried out at the Jet Propulsion
Laboratory, California Institute of Technology, under a contract with
the National Aeronautics and Space Administration. The authors would
like to thank Rick LeDuc, Jonas Zmuidzinas, Sunil Golwala, David Moore,
Peter Day, and Omid Noroozian for useful insights.
NR 29
TC 38
Z9 38
U1 2
U2 11
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD JAN 16
PY 2012
VL 20
IS 2
BP 1503
EP 1511
DI 10.1364/OE.20.001503
PG 9
WC Optics
SC Optics
GA 889EZ
UT WOS:000300057700079
PM 22274494
ER
PT J
AU Koskulics, J
Englehardt, S
Long, S
Hu, YX
Stamnes, K
AF Koskulics, Jeffrey
Englehardt, Steven
Long, Steven
Hu, Yongxiang
Stamnes, Knut
TI Method of surface topography retrieval by direct solution of sparse
weighted seminormal equations
SO OPTICS EXPRESS
LA English
DT Article
ID WATER-SURFACE; CURVATURE MEASUREMENTS; WIND-WAVES; RECONSTRUCTION; SLOPE
AB A new method is presented to estimate the topography of a rough surface. A formulation is provided in which immediate measurements and a priori observations of surface elevation, slope and curvature, are considered simultaneously as a linear algebraic system of finite difference equations. Least squares solutions are computed directly by sparse orthogonal-triangular (QR) factorization of the weighted seminormal equations, an approach made practical for large systems with powerful computational hardware and algorithms that have become available recently. Retrievals are demonstrated from synthetic slope data and from measurements of slope on a rough water surface. The method provides a general approach to retrieving topography from measurements of elevation, slope and curvature. (C) 2012 Optical Society of America
C1 [Koskulics, Jeffrey; Englehardt, Steven; Stamnes, Knut] Stevens Inst Technol, Hoboken, NJ 07030 USA.
[Long, Steven] NASA, GSFC WFF Air Sea Interact Res Facil, Wallops Isl, VA 23337 USA.
[Hu, Yongxiang] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Koskulics, J (reprint author), Stevens Inst Technol, Hoboken, NJ 07030 USA.
EM jkoskuli@stevens.edu
RI Hu, Yongxiang/K-4426-2012
FU NASA; NASA HQ
FX The authors acknowledge support from the NASA Calipso Project and
Radiation Science Program. The authors would also like to thank the
anonymous reviewers for their detailed comments and suggestions. S. Long
wishes to thank NASA HQ for their support over the past 36 years, right
up to this final work that marks the facility's end of operations.
NR 32
TC 4
Z9 4
U1 0
U2 1
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1094-4087
J9 OPT EXPRESS
JI Opt. Express
PD JAN 16
PY 2012
VL 20
IS 2
BP 1714
EP 1726
DI 10.1364/OE.20.001714
PG 13
WC Optics
SC Optics
GA 889EZ
UT WOS:000300057700099
PM 22274514
ER
PT J
AU Davami, K
Ghassemi, HM
Yassar, RS
Lee, JS
Meyyappan, M
AF Davami, Keivan
Ghassemi, Hessam M.
Yassar, Reza S.
Lee, Jeong-Soo
Meyyappan, M.
TI Thermal Breakdown of ZnTe Nanowires
SO CHEMPHYSCHEM
LA English
DT Article
DE nanowires; surface analysis; thermal breakdown; thermal stress;
thermoelectrics
ID OPTICAL-PROPERTIES; ZNO NANOWIRES; TEMPERATURE; GROWTH; NANOSTRUCTURES;
ARRAYS
AB As the applications for inorganic nanowires continuously grow, studies on the stability of these structures under high electrical/thermal stress conditions are needed. ZnTe nanowires are grown by the vapor-liquid-solid technique and their breakdown under Joule heating is studied through in situ monitoring in a transmission electron microscope (TEM). The experimental setup, consisting of a scanning tunneling microscope (STM) and a movable piezotube inside the TEM, allows the manipulation of a single nanowire. A voltage applied to the STM tip in contact with a ZnTe nanowire leads to the breakdown of the nanowire into Zn and Te particles or balls which is observed in real time. These balls grow by Ostwald ripening, rendering the surface morphology of the ZnTe nanowire progressively rough. Diffraction patterns along the stem of the wire after the partial breakdown showed substantially smaller lattice spacing compared to 0.35 nm for pristine ZnTe nanowires.
C1 [Davami, Keivan; Lee, Jeong-Soo; Meyyappan, M.] Pohang Univ Sci & Technol, Div IT Convergence Engn, Pohang, South Korea.
[Ghassemi, Hessam M.; Yassar, Reza S.] Michigan Technol Univ, Dept Mech Engn, Houghton, MI 49931 USA.
[Meyyappan, M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Lee, JS (reprint author), Pohang Univ Sci & Technol, Div IT Convergence Engn, Pohang, South Korea.
EM ljs6951@postech.ac.kr; m.meyyappan@nasa.gov
RI Davami, Keivan/Q-5283-2016
FU National Research Foundation of Korea; Ministry of Education, Science
and Technology [R31-10100]; NSF-DMR [0820884]; NSF-CMMI [0926819]
FX This work 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. Part of this
work was done at MTU during KD's visit and Professor Yassar's group is
acknowledged for hosting the visit. RSY would like to acknowledge the
funding support through the NSF-DMR Grant 0820884 and NSF-CMMI Grant
0926819. Dr. Bin Chen is acknowledged for her insightful comments on the
Raman analysis.
NR 23
TC 7
Z9 7
U1 1
U2 23
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA POSTFACH 101161, 69451 WEINHEIM, GERMANY
SN 1439-4235
EI 1439-7641
J9 CHEMPHYSCHEM
JI ChemPhysChem
PD JAN 16
PY 2012
VL 13
IS 1
BP 347
EP 352
DI 10.1002/cphc.201100486
PG 6
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 873WG
UT WOS:000298913500046
PM 22131283
ER
PT J
AU Forouhar, S
Briggs, RM
Frez, C
Franz, KJ
Ksendzov, A
AF Forouhar, Siamak
Briggs, Ryan M.
Frez, Clifford
Franz, Kale J.
Ksendzov, Alexander
TI High-power laterally coupled distributed-feedback GaSb-based diode
lasers at 2 mu m wavelength
SO APPLIED PHYSICS LETTERS
LA English
DT Article
ID ROOM-TEMPERATURE
AB We report on GaSb-based laterally coupled distributed-feedback (DFB) diode lasers designed to operate at wavelengths near 2.05 mu m. Second-order Bragg gratings were etched alongside narrow ridge waveguides to enable single-mode DFB operation in 2-mm-long laser diodes. At a heat-sink temperature of 10 degrees C, the lasers emit more than 40mW continuous-wave in a single longitudinal mode, while increasing the current beyond 300 mA results in multimode operation due to spectral shifting of the laser gain with respect to the peak grating reflectivity. At 10 degrees C, we observe DFB operation at higher current, with single-facet emission exceeding 80 mW. (C) 2012 American Institute of Physics. [doi:10.1063/1.3678187]
C1 [Forouhar, Siamak; Briggs, Ryan M.; Frez, Clifford; Franz, Kale J.; Ksendzov, Alexander] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Forouhar, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM siamak.forouhar@jpl.nasa.gov
FU Jet Propulsion Laboratory, California Institute of Technology; National
Aeronautics and Space Administration
FX The epitaxial laser wafers used in this work were designed and grown by
Leon Shterengas and Gregory Belenky and purchased through Power
Photonic, Inc. The authors acknowledge Robert Menzies and Gary Spiers
for their technical advice and Jason Hyon and Gary Lau for their
support. This work was sponsored by the Research and Technology
Development Program through the Jet Propulsion Laboratory, California
Institute of Technology, under contract with the National Aeronautics
and Space Administration.
NR 15
TC 33
Z9 33
U1 3
U2 23
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 JAN 16
PY 2012
VL 100
IS 3
AR 031107
DI 10.1063/1.3678187
PG 4
WC Physics, Applied
SC Physics
GA 880EE
UT WOS:000299386800007
ER
PT J
AU Fletcher, LE
Valdivia-Silva, JE
Perez-Montano, S
Condori-Apaza, RM
Conley, CA
McKay, CP
AF Fletcher, Lauren E.
Valdivia-Silva, Julio E.
Perez-Montano, Saul
Condori-Apaza, Renee M.
Conley, Catharine A.
McKay, Christopher P.
TI Variability of organic material in surface horizons of the hyper-arid
Mars-like soils of the Atacama Desert
SO ADVANCES IN SPACE RESEARCH
LA English
DT Article
DE Soil organic carbon; Organic-variability; Atacama Desert; Extreme
environments; Hyper-arid; Mars analog
ID SHORTGRASS STEPPE; MICROBIAL LIFE; TAYLOR VALLEY; CHILE; MATTER; CARBON;
ANTARCTICA; RANGELAND; PATTERNS; ORIGIN
AB The objective of this work was to investigate the variability of surface organic carbon within the hyper-arid Yungay region of the Atacama Desert. The fraction of Labile Organic Carbon (LOC) in these samples varied from 2 to 73 mu g per gram of soil with a bi-modal distribution with average content of 17 +/- 9 mu g LOC and 69 +/- 3 mu g LOC for "low" and "high" samples, respectively. Interestingly, there was no relation between organic levels and geomorphologic shapes. While organics are deposited and distributed in these soils via colic processes, it is suggested that fog is the dynamic mechanism that is responsible for the variability and peaks in organic carbon throughout the area, where a "high" LOC content sample could be indicative of a biological process. It was determined that there was no significant difference between topological feature or geographical position within the hyper-arid samples and LOC. This very curious result has implications for the investigation of run-off gullies on the planet Mars as our work suggests a need for careful consideration of the expectation of increases in concentrations of organic materials associated with following aqueous altered topology. (C) 2011 Published by Elsevier Ltd. on behalf of COSPAR.
C1 [Fletcher, Lauren E.] Univ Oxford, Clarendon Lab, AOPP, Oxford OX1 3PU, England.
[Fletcher, Lauren E.; Valdivia-Silva, Julio E.; Perez-Montano, Saul; McKay, Christopher P.] NASA, Div Space Sci, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Valdivia-Silva, Julio E.] Univ Nacl Autonoma Mexico, Lab Quim Plasmas & Estudios Planetarios, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico.
[Perez-Montano, Saul] San Jose State Univ, Dept Chem, San Jose, CA 95192 USA.
[Condori-Apaza, Renee M.] Univ Nacl San Agustin, Arequipa, Peru.
[Conley, Catharine A.] NASA Headquarters, Planetary Sci Div, Sci Mission Directorate, Washington, DC USA.
RP Fletcher, LE (reprint author), Univ Oxford, Clarendon Lab, AOPP, Parks Rd, Oxford OX1 3PU, England.
EM Lauren@atm.ox.ac.uk
OI CONDORI APAZA, RENEE/0000-0002-1097-5026
FU ASTEP
FX We would like to thank Dr. Benito Gomez for many years of support and
access to the Yungay Desert Research Station, Chile; Dr. Benjamin Paz
and Dr. Eleana Vargas de Nieto for providing laboratory research space
and support at the Universidad Nacional de San Agustin (Arequipa, Peru);
and to Antonio Ball On and Nicanor their help in the collection of
samples. Acknowledgement is given to the ASTEP grant for providing
partial funds in support of this research work.
NR 46
TC 6
Z9 6
U1 2
U2 17
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0273-1177
J9 ADV SPACE RES
JI Adv. Space Res.
PD JAN 15
PY 2012
VL 49
IS 2
BP 271
EP 279
DI 10.1016/j.asr.2011.10.001
PG 9
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences
GA 890GB
UT WOS:000300132000007
ER
PT J
AU Tyra, MA
Farquhar, J
Guan, Y
Leshin, LA
AF Tyra, M. A.
Farquhar, J.
Guan, Y.
Leshin, L. A.
TI An oxygen isotope dichotomy in CM2 chondritic carbonates-A SIMS approach
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID METEORITE PARENT BODIES; CARBONACEOUS CHONDRITES; AQUEOUS ALTERATION;
WEATHERING PRODUCTS; HYDROUS ASTEROIDS; ELEPHANT MORAINE; CI CHONDRITES;
CONSTRAINTS; EVOLUTION; RECORD
AB We present petrologic and Secondary Ion Mass Spectrometry (SIMS) oxygen isotope analyses of Ca-carbonate within a group of paired Antarctic CM2 chondrites. The carbonates can be grouped into two isotopically and morphologically distinct populations. Type 1 grains (small matrix grains) possess average delta O-18 of 33.7 perpendicular to 2.3 parts per thousand (1 sigma) and average Delta O-17 of -0.81 parts per thousand +/- 0.90 parts per thousand (1 sigma). Type 2 grains (calcite aggregates) possess distinct oxygen isotopic compositions, average delta O-18 of 19.4 parts per thousand +/- 1.5 parts per thousand (1 sigma) and average Delta O-17 of -1.98 +/- 0.9 parts per thousand (1 sigma). These differences are interpreted to indicate that the two populations of calcite formed under different conditions at different times. The carbonates have textural features that suggest an extraterrestrial origin. The data presented here fall within error of a previously measured array for carbonates from CM falls (Benedix et al., 2003). The presence of two generations of carbonate suggests carbonate formation in two discrete events on the parent body of these meteorites. The oxygen isotopic data presented here deviate from prior bulk carbonate measurements undertaken for these meteorites. Most likely, this deviation is because bulk carbonate analyses included vein carbonate which formed during terrestrial weathering. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Tyra, M. A.] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA.
[Tyra, M. A.; Farquhar, J.] Univ Maryland, Dept Geol, College Pk, MD 21742 USA.
[Tyra, M. A.; Farquhar, J.] Univ Maryland, ESSIC, College Pk, MD 21742 USA.
[Guan, Y.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
[Leshin, L. A.] NASA Headquarters, Explorat Syst Mission Directorate, Washington, DC 20024 USA.
RP Tyra, MA (reprint author), Univ New Mexico, Dept Earth & Planetary Sci, Northrop Hall,Room 141,MSC 03 2040,1 Univ New Mex, Albuquerque, NM 87131 USA.
EM matyra@unm.edu
FU NASA [NAG5-11979, NNX09AF72G]; NSF [EAR01-15488]; University of
Maryland; New Mexico Space Grant
FX We thank A.N. Krot (AE), L. Bonal, and one anonymous reviewer for their
careful edits. Phillip M. Piccoli, Richard J. Walker, Penny King, Paul
Niles, Adrian Brearley, and Alan J. Kaufman all contributed ideas,
expertise, and/or their red pen to this work. This work was supported by
NASA Cosmochemistry Grants NAG5-11979 and NNX09AF72G, NSF Grant
EAR01-15488, a University of Maryland GRB award, and the New Mexico
Space Grant.
NR 63
TC 16
Z9 16
U1 2
U2 23
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
EI 1872-9533
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD JAN 15
PY 2012
VL 77
BP 383
EP 395
DI 10.1016/j.gca.2011.10.003
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 875DK
UT WOS:000299010400026
ER
PT J
AU Cecil, DJ
Blankenship, CB
AF Cecil, Daniel J.
Blankenship, Clay B.
TI Toward a Global Climatology of Severe Hailstorms as Estimated by
Satellite Passive Microwave Imagers
SO JOURNAL OF CLIMATE
LA English
DT Article
ID HAIL SUPPRESSION EXPERIMENT; SEVERE THUNDERSTORM; NORTHEAST COLORADO;
ICE-SCATTERING; CONVECTION; RADAR; SIZE; REGION; CHINA; TRMM
AB An 8-yr climatology of storms producing large hail is estimated from satellite measurements using Advanced Microwave Scanning Radiometer for Earth Observing System (AMSR-E). This allows a unique, consistent comparison between regions that cannot be consistently compared using ground-based records because of varying data collection standards. Severe hailstorms are indicated most often in a broad region of northern Argentina and southern Paraguay and a smaller region in Bangladesh and eastern India. Numerous hailstorms are also estimated in the central and southeastern United States, northern Pakistan and northwestern India, central and western Africa, and southeastern Africa (and adjacent waters). Fewer hailstorms are estimated for other regions over land and scattered across subtropical oceans. Very few are estimated in the deep tropics other than in Africa. Most continental regions show seasonality with hailstorms peaking in late spring or summer. The South Asian monsoon alters the hailstorm climatology around the Indian subcontinent. About 75% of the hailstorms on the eastern side (around Bangladesh) occur from April through June, generally before monsoon onset. Activity shifts northwest to northern India in late June and July. An arc along the foothills in northern Pakistan becomes particularly active from mid-June through mid-August. The AMSR-E measurements are limited to early afternoon and late night. Tropical Rainfall Measuring Mission (TRMM) measurements are used to investigate diurnal variability in the tropics and subtropics. All of the prominent regions have hailstorm peaks in late afternoon and early evening. The United States and central Africa have the fewest overnight and early morning storms, while subtropical South America and Bangladesh have the most.
C1 [Cecil, Daniel J.] Univ Alabama, Ctr Earth Syst Sci, Huntsville, AL 35805 USA.
[Blankenship, Clay B.] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA.
RP Cecil, DJ (reprint author), Univ Alabama, Ctr Earth Syst Sci, 320 Sparkman Dr NW, Huntsville, AL 35805 USA.
EM cecild@uah.edu
RI Nesbitt, Stephen/I-3965-2013
OI Nesbitt, Stephen/0000-0003-0348-0452
FU NASA [NNX07AD73G, NNX10AG78G]
FX This work was supported by NASA precipitation science program Grants
NNX07AD73G and NNX10AG78G. AMSR-E data were downloaded from the National
Snow and Ice Data Center. Hail reports were downloaded from the Storm
Prediction Center. TRMM data in precipitation feature format were
downloaded from the TRMM Science Data and Information System and from
the University of Utah. We appreciate the comments of the four anonymous
reviewers, whose suggestions improved the original manuscript.
NR 32
TC 35
Z9 36
U1 1
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 JAN 15
PY 2012
VL 25
IS 2
BP 687
EP 703
DI 10.1175/JCLI-D-11-00130.1
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 883QU
UT WOS:000299649600017
ER
PT J
AU Hall, DK
Foster, JL
DiGirolamo, NE
Riggs, GA
AF Hall, Dorothy K.
Foster, James L.
DiGirolamo, Nicolo E.
Riggs, George A.
TI Snow cover, snowmelt timing and stream power in the Wind River Range,
Wyoming
SO GEOMORPHOLOGY
LA English
DT Article
DE Wind River Range; MODIS; Seasonal snow cover; Streamflow runoff
ID WESTERN NORTH-AMERICA; RUNOFF MODEL; MODIS; PRODUCTS; TEMPERATURE;
HEMISPHERE; TRANSPORT; TRENDS
AB Earlier onset of springtime weather, including earlier snowmelt, has been documented in the western United States over at least the last 50 years. Because the majority (>70%) of the water supply in the western U.S. comes from snowmelt, analysis of the declining spring snowpack (and shrinking glaciers) has important implications for the management of streamflow. The amount of water in a snowpack influences stream discharge which can also influence erosion and sediment transport by changing stream power, or the rate at which a stream can do work, such as move sediment and erode the stream bed. The focus of this work is the Wind River Range (WRR) in west-central Wyoming. Ten years of Moderate-Resolution Imaging Spectro-radiometer (MODIS) snow-cover, cloud-gap-filled (CGF) map products and 30 years of discharge and meteorological station data are studied. Streamflow data from streams in WRR drainage basins show lower annual discharge and earlier snowmelt in the decade of the 2000s than in the previous three decades, though no trend of either lower streamflow or earlier snowmelt was observed within the decade of the 2000s. Results show a statistically-significant trend at the 95% confidence level (or higher) of increasing weekly maximum air temperature (for three out of the five meteorological stations studied) in the decade of the 1970s, and also for the 40-year study period as a whole. The extent of snow-cover (percent of basin covered) derived from the lowest elevation zone (2500-3000 m) of the WRR, using MODIS CGF snow-cover maps, is strongly correlated with maximum monthly discharge on 30 April, where Spearman's Rank correlation, r(s), = 0.89 for the decade of the 2000s. We also investigated stream power for Bull Lake Creek above Bull Lake; and found a trend (significant at the 90% confidence level) toward reduced stream power from 1970 to 2009. Observed changes in streamflow and stream power may be related to increasing weekly maximum air temperature measured during the 40-year study period, possibly contributing to a reduction in snow cover. In addition, the strong relationship between percent of basin that was snow covered, and maximum monthly streamflow indicates that MODIS snow-cover maps are useful for predicting streamflow, and can be used to improve management of water resources in the drought-prone western United States. Published by Elsevier B.V.
C1 [Hall, Dorothy K.; Foster, James L.] NASA, Lab Hydrospher & Biospher Proc, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[DiGirolamo, Nicolo E.; Riggs, George A.] SSAI, Lanham, MD 20706 USA.
RP Hall, DK (reprint author), NASA, Lab Hydrospher & Biospher Proc, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM dorothy.k.hall@nasa.gov
RI Hall, Dorothy/D-5562-2012
FU NASA
FX The authors thank Dr. Dan Cayan/University of California San Diego and
USGS and Dr. Kelly Redmond/Desert Research Institute for discussions
about snow extent and snowmelt-timing trends in the western United
States. We also thank Dr. Jonathan Barton, NASA/GSFC and Oak Ridge
Associated Universities, for providing insightful ideas and information
on stream power, and for his review of the paper. Dr. Allan James, the
Guest Editor, provided additional valuable suggestions. Finally we thank
the two anonymous reviewers for their constructive comments. This work
is supported by NASA's Earth Observing System Program.
NR 36
TC 24
Z9 26
U1 1
U2 23
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0169-555X
J9 GEOMORPHOLOGY
JI Geomorphology
PD JAN 15
PY 2012
VL 137
IS 1
SI SI
BP 87
EP 93
DI 10.1016/j.geomorph.2010.11.011
PG 7
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA 868GN
UT WOS:000298511800007
ER
PT J
AU Sayer, AM
Thomas, GE
Grainger, RG
Carboni, E
Poulsen, C
Siddans, R
AF Sayer, Andrew M.
Thomas, Gareth E.
Grainger, Roy G.
Carboni, Elisa
Poulsen, Caroline
Siddans, Richard
TI Use of MODIS-derived surface reflectance data in the ORAC-AATSR aerosol
retrieval algorithm: Impact of differences between sensor spectral
response functions
SO REMOTE SENSING OF ENVIRONMENT
LA English
DT Article
DE Aerosol; AATSR; BRDF; MODIS; Optimal estimation; ORAC; Retrieval;
Surface albedo
ID BIDIRECTIONAL REFLECTANCE; OPTICAL-PROPERTIES; LAND; ALBEDO;
CAPABILITIES; DERIVATION; INTENSITY; MODELS; CLOUDS; BRDF
AB The aerosol component of the Oxford-Rutherford Appleton Laboratory (RAL) Aerosol and Clouds (ORAC) retrieval scheme for the Advanced Along-Track Scanning Radiometer (AATSR) uses data derived from the Moderate Resolution Imaging Spectroradiometer (MOD'S) to constrain the brightness of the surface. However, the spectral response functions of the channels used (centred near 550 nm, 660 nm, 870 nm, and 1.6 mu m) do not exactly match between the two sensors. It is shown that failure to account for differences between the instruments' spectral response functions leads to errors of typically 0.001-0.01 in spectral surface albedo, and distinct biases, dependent on wavelength and surface type. A technique based on singular value decomposition (SVD) is used to reduce these random errors by an average of 35% at 670 nm and over 60% at the other wavelengths used. The technique reduces the biases so that they are negligible. In principle, the method can be extended to any combination of sensors. The SVD-based scheme is applied to AATSR data from the month of July 2008 and found to increase the number of successful aerosol retrievals, the speed of retrieval convergence, and improve the level of consistency between the measurements and the retrieved state. Additionally, retrieved aerosol optical depth at 550 nm shows an improvement in correspondence when compared to Aerosol Robotic Network (AERONET) data. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Sayer, Andrew M.; Thomas, Gareth E.; Grainger, Roy G.; Carboni, Elisa] Univ Oxford, Dept Phys, Oxford OX1 3PU, England.
[Sayer, Andrew M.; Poulsen, Caroline; Siddans, Richard] Sci & Technol Facil Council Rutherford Appleton L, Didcot OX11 0QX, Oxon, England.
RP Sayer, AM (reprint author), NASA, Goddard Space Flight Ctr, Goddard Earth Sci Technol & Res GESTAR, Code 661, Greenbelt, MD 20771 USA.
EM andrew.sayer@nasa.gov
RI Sayer, Andrew/H-2314-2012; Carboni, Elisa/K-9404-2013; Grainger,
Roy/E-8823-2011
OI Sayer, Andrew/0000-0001-9149-1789; Carboni, Elisa/0000-0002-0236-7856;
Grainger, Roy/0000-0003-0709-1315
FU Natural Environment Research Council [NE/F001452/1]
FX This work was supported by the Natural Environment Research Council
(grant number NE/F001452/1). The authors would also like to thank JPL
and USGS for the spectral databases used in SVD calculation, ESA and the
NEODC for the AATSR Level 1b data, and Crystal Schaaf and the MODIS BRDF
team at BU for the MODIS BRDF product (and many helpful discussions
about it). More generally, NASA are thanked for the MODIS sensors and
the NASA LAADS for making the data available for download. NASA and the
AERONET PIs are thanked for the creation and maintenance of the AERONET
record. Environment Canada and the Universite de Sherbrooke are thanked
for running AEROCAN, the Canadian subnetwork of AERONET
(http://www.aerocanonline.com/templates/nature/index.html). Finally, the
authors would like to thank the anonymous reviewers for their comments
on the manuscript.
NR 38
TC 13
Z9 13
U1 1
U2 16
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0034-4257
EI 1879-0704
J9 REMOTE SENS ENVIRON
JI Remote Sens. Environ.
PD JAN 15
PY 2012
VL 116
SI SI
BP 177
EP 188
DI 10.1016/j.rse.2011.02.029
PG 12
WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic
Technology
SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science &
Photographic Technology
GA 867LA
UT WOS:000298454700014
ER
PT J
AU Kharangate, CR
Mudawar, I
Hasan, MM
AF Kharangate, Chirag R.
Mudawar, Issam
Hasan, Mohammad M.
TI Experimental and theoretical study of critical heat flux in vertical
upflow with inlet vapor void
SO INTERNATIONAL JOURNAL OF HEAT AND MASS TRANSFER
LA English
DT Article
DE Flow boiling; Separated flow; Critical heat flux (CHF)
ID FLOW BOILING CHF; RECTANGULAR CHANNEL; WATER-FLOW; TRIGGER MECHANISM;
EARTH GRAVITY; MODEL; MICROGRAVITY; ORIENTATION; TUBES; WALL
AB This study explores the mechanism of flow boiling critical heat flux (CHF) for FC-72 in a 2.5 mm x 5 mm vertical upflow channel that is heated along its 2.5 mm sidewall downstream of an adiabatic development section. Unlike most prior CHF studies, where the working fluid enters the channel in liquid state, the present study concerns saturated inlet conditions with finite vapor void. Temperature measurements and high-speed video imaging techniques are used to investigate the influence of the inlet vapor void on interfacial behavior at heat fluxes up to CHF as well during the CHF transient. The flow entering the heated portion of the channel consists of a thin liquid layer covering the entire perimeter surrounding a large central vapor core. Just prior to CHF, a fairly continuous wavy vapor layer begins to develop between the liquid layer covering the heated wall and the heated wall itself, resulting in a complex four-layer flow consisting of the liquid layer covering the insulated walls, the central vapor core, the now separated liquid layer adjacent to the heated wall, and the newly formed wavy vapor layer along the heated wall. This behavior in captured in a new separated control-volume-based model that facilities the determination of axial variations of thicknesses and mean velocities of the four layers. Incorporating the results of this model in a modified form of the Interfacial Lift-off CHF Model is shown to provide fairly good predictions of CHF data for mass velocities between 185 and 1600 kg/m(2) s, evidenced by a mean absolute error of 24.52%. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Kharangate, Chirag R.; Mudawar, Issam] Purdue Univ, Sch Mech Engn, Boiling & Twophase Flow Lab, W Lafayette, IN 47907 USA.
[Hasan, Mohammad M.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Mudawar, I (reprint author), Purdue Univ, Sch Mech Engn, Boiling & Twophase Flow Lab, 585 Purdue Mall, W Lafayette, IN 47907 USA.
EM mudawar@ecn.purdue.edu
FU National Aeronautics and Space Administration (NASA) [NNX09AJ51A]
FX The authors are grateful for the support of the National Aeronautics and
Space Administration (NASA) under Grant No. NNX09AJ51A.
NR 35
TC 15
Z9 15
U1 1
U2 4
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0017-9310
J9 INT J HEAT MASS TRAN
JI Int. J. Heat Mass Transf.
PD JAN 15
PY 2012
VL 55
IS 1-3
BP 360
EP 374
DI 10.1016/j.ijheatmasstransfer.2011.09.028
PG 15
WC Thermodynamics; Engineering, Mechanical; Mechanics
SC Thermodynamics; Engineering; Mechanics
GA 853ME
UT WOS:000297429600035
ER
PT J
AU Bauer, SE
Menon, S
AF Bauer, Susanne E.
Menon, Surabi
TI Aerosol direct, indirect, semidirect, and surface albedo effects from
sector contributions based on the IPCC AR5 emissions for preindustrial
and present-day conditions
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID GISS MODELE; CLIMATE; SOOT; PARAMETERIZATION; MICROPHYSICS; SIMULATIONS;
SENSITIVITY; CONVECTION; IMPACTS; CLOUDS
AB The anthropogenic increase in aerosol concentrations since preindustrial times and its net cooling effect on the atmosphere is thought to mask some of the greenhouse gas-induced warming. Although the overall effect of aerosols on solar radiation and clouds is most certainly negative, some individual forcing agents and feedbacks have positive forcing effects. Recent studies have tried to identify some of those positive forcing agents and their individual emission sectors, with the hope that mitigation policies could be developed to target those emitters. Understanding the net effect of multisource emitting sectors and the involved cloud feedbacks is very challenging, and this paper will clarify forcing and feedback effects by separating direct, indirect, semidirect and surface albedo effects due to aerosols. To this end, we apply the Goddard Institute for Space Studies climate model including detailed aerosol microphysics to examine aerosol impacts on climate by isolating single emission sector contributions as given by the Coupled Model Intercomparison Project Phase 5 (CMIP5) emission data sets developed for Intergovernmental Panel on Climate Change (IPCC) AR5. For the modeled past 150 years, using the climate model and emissions from preindustrial times to present-day, the total global annual mean aerosol radiative forcing is -0.6 W/m(2), with the largest contribution from the direct effect (-0.5 W/m(2)). Aerosol-induced changes on cloud cover often depends on cloud type and geographical region. The indirect (includes only the cloud albedo effect with -0.17 W/m(2)) and semidirect effects (-0.10 W/m(2)) can be isolated on a regional scale, and they often have opposing forcing effects, leading to overall small forcing effects on a global scale. Although the surface albedo effects from aerosols are small (0.016 W/m(2)), triggered feedbacks on top of the atmosphere (TOA) radiative forcing can be 10 times larger. Our results point out that each emission sector has varying impacts by geographical region. For example, the single sector most responsible for a net positive radiative forcing is the transportation sector in the United States, agricultural burning and transportation in Europe, and the domestic emission sector in Asia. These sectors are attractive mitigation targets.
C1 [Bauer, Susanne E.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Bauer, Susanne E.] Columbia Univ, Earth Inst, New York, NY USA.
[Menon, Surabi] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
RP Bauer, SE (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA.
EM sb2273@columbia.edu
RI Bauer, Susanne/P-3082-2014
FU NASA [NN-H-04-Z-YS-008-N, NN-H-08-Z-DA-001-N]; U.S. Department of Energy
[DE-AC02-05CH11231]
FX This work has been supported by the NASA MAP program Modeling, Analysis
and Prediction Climate Variability and Change (NN-H-04-Z-YS-008-N) and
(NN-H-08-Z-DA-001-N). S.M. was also supported by the U.S. Department of
Energy under contract DE-AC02-05CH11231 at LBNL and the DOE Earth System
Modeling Program. We thank Greg Faluvegi for processing the emission
data sets for the GISS model.
NR 39
TC 39
Z9 40
U1 2
U2 49
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 14
PY 2012
VL 117
AR D01206
DI 10.1029/2011JD016816
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 877LJ
UT WOS:000299182300002
ER
PT J
AU Liu, XM
Shemansky, DE
Johnson, PV
Malone, CP
Khakoo, MA
Kanik, I
AF Liu, Xianming
Shemansky, Donald E.
Johnson, Paul V.
Malone, Charles P.
Khakoo, Murtadha A.
Kanik, Isik
TI Electron and photon dissociation cross sections of the H-2 singlet
ungerade continua
SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS
LA English
DT Article
ID QUANTUM-DEFECT THEORY; SPONTANEOUS RADIATIVE DISSOCIATION; RESOLUTION
LASER SPECTROSCOPY; DIFFUSE INTERSTELLAR BANDS; VACUUM-ULTRAVIOLET
REGION; MINIMUM 1-SIGMA-G+ STATES; ION-PAIR FORMATION;
MOLECULAR-HYDROGEN; IMPACT EXCITATION; TRANSITION MOMENTS
AB Photodissociation cross sections and oscillator strengths for H-2 from the X-1 Sigma(+)(g) (v(i), J(i)) levels to the continuum levels of the B-1 Sigma(+)(u), C-1 Pi(u), B ''(B) over bar (1)Sigma(+)(u), D' (1) Pi(u) and 5p sigma (1) Sigma(+)(u) states have been calculated. The (v(i), J(i)) state-specific electron impact dissociation cross sections to the continuum levels of these states have been obtained for the first time over a wide energy range using calculated continuum oscillator strengths along with previously published excitation functions of the Lyman and Werner bands. Estimated cross sections to the higher (n >= 5) np sigma (1) Sigma(+)(u) and np pi (1) Pi(u) continua are also provided. Both photon and electron impact excitation cross sections show strong dependences on the initial (v(i), J(i)) quantum numbers. Thermally averaged electron impact cross sections of all singlet ungerade states increase monotonically with temperature. While excitation to the B' (1) Sigma(+)(u) continuum is the dominant dissociation channel at room temperature, the C-1 Pi(u) and B (1) Sigma(+)(u) continua become more important at high temperature (>5000 K). This work, along with the previous calculation of the B' (1)Sigma(+)(u) and D-1 Pi(u) states by Liu et al (2009a J. Phys. B: At. Mol. Opt. Phys. 42 185203), provides the complete electron impact dissociation cross section of H-2 through the singlet ungerade continua. Electron dissociation cross sections of the singlet ungerade continua are provided for the purpose of modelling atmospheric heating, analysis of occultation measurements and the hot atomic hydrogen plume observed at Saturn.
C1 [Liu, Xianming; Shemansky, Donald E.] Space Environm Technol, Planetary & Space Sci Div, Pacific Palisades, CA 90272 USA.
[Johnson, Paul V.; Malone, Charles P.; Kanik, Isik] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Malone, Charles P.; Khakoo, Murtadha A.] Calif State Univ Fullerton, Dept Phys, Fullerton, CA 92834 USA.
RP Liu, XM (reprint author), Space Environm Technol, Planetary & Space Sci Div, 1676 Palisades Dr, Pacific Palisades, CA 90272 USA.
EM xliu@spacenvironment.net
RI Malone, Charles/A-6294-2010; Johnson, Paul/D-4001-2009
OI Malone, Charles/0000-0001-8418-1539; Johnson, Paul/0000-0002-0186-8456
FU Cassini UVIS; University of Colorado; NSF [AGS-0938223]; NASA
FX The authors wish to thank Professor Lutoslaw Wolniewicz for making
results of his ab initio calculations accessible. The analysis described
in this paper was carried out at Space Environment Technologies (SET)
and Jet Propulsion Laboratory (JPL), California Institute of Technology.
Work performed at SET is supported by the Cassini UVIS contract with the
University of Colorado, by NSF AGS-0938223, and NASA Cassini Data
Analysis program. XL, PVJ and CPM acknowledge financial support through
NASA's Planetary Atmospheres Research programs.
NR 121
TC 4
Z9 4
U1 0
U2 10
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0953-4075
EI 1361-6455
J9 J PHYS B-AT MOL OPT
JI J. Phys. B-At. Mol. Opt. Phys.
PD JAN 14
PY 2012
VL 45
IS 1
AR 015201
DI 10.1088/0953-4075/45/1/015201
PG 15
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 869QV
UT WOS:000298613800005
ER
PT J
AU Shindell, D
Kuylenstierna, JCI
Vignati, E
van Dingenen, R
Amann, M
Klimont, Z
Anenberg, SC
Muller, N
Janssens-Maenhout, G
Raes, F
Schwartz, J
Faluvegi, G
Pozzoli, L
Kupiainen, K
Hoglund-Isaksson, L
Emberson, L
Streets, D
Ramanathan, V
Hicks, K
Oanh, NTK
Milly, G
Williams, M
Demkine, V
Fowler, D
AF Shindell, Drew
Kuylenstierna, Johan C. I.
Vignati, Elisabetta
van Dingenen, Rita
Amann, Markus
Klimont, Zbigniew
Anenberg, Susan C.
Muller, Nicholas
Janssens-Maenhout, Greet
Raes, Frank
Schwartz, Joel
Faluvegi, Greg
Pozzoli, Luca
Kupiainen, Kaarle
Hoeglund-Isaksson, Lena
Emberson, Lisa
Streets, David
Ramanathan, V.
Hicks, Kevin
Oanh, N. T. Kim
Milly, George
Williams, Martin
Demkine, Volodymyr
Fowler, David
TI Simultaneously Mitigating Near-Term Climate Change and Improving Human
Health and Food Security
SO SCIENCE
LA English
DT Article
ID BLACK CARBON; HYDROLOGICAL CYCLE; TIBETAN PLATEAU; AIR-QUALITY;
EMISSIONS; OZONE; IMPACTS; PROJECTIONS; MORTALITY; AEROSOLS
AB Tropospheric ozone and black carbon (BC) contribute to both degraded air quality and global warming. We considered similar to 400 emission control measures to reduce these pollutants by using current technology and experience. We identified 14 measures targeting methane and BC emissions that reduce projected global mean warming similar to 0.5 degrees C by 2050. This strategy avoids 0.7 to 4.7 million annual premature deaths from outdoor air pollution and increases annual crop yields by 30 to 135 million metric tons due to ozone reductions in 2030 and beyond. Benefits of methane emissions reductions are valued at $700 to $5000 per metric ton, which is well above typical marginal abatement costs ( less than $250). The selected controls target different sources and influence climate on shorter time scales than those of carbon dioxide-reduction measures. Implementing both substantially reduces the risks of crossing the 2 degrees C threshold.
C1 [Shindell, Drew; Faluvegi, Greg; Milly, George] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Shindell, Drew; Faluvegi, Greg; Milly, George] Columbia Univ, Columbia Earth Inst, New York, NY 10025 USA.
[Kuylenstierna, Johan C. I.; Emberson, Lisa; Hicks, Kevin] Univ York, Dept Environm, Stockholm Environm Inst, York YO10 5DD, N Yorkshire, England.
[Vignati, Elisabetta; van Dingenen, Rita; Janssens-Maenhout, Greet; Raes, Frank; Pozzoli, Luca] European Commiss, Joint Res Ctr, I-21027 Ispra, Italy.
[Amann, Markus; Klimont, Zbigniew; Kupiainen, Kaarle; Hoeglund-Isaksson, Lena] Int Inst Appl Syst Anal, A-2361 Laxenburg, Austria.
[Anenberg, Susan C.] US EPA, Washington, DC 20460 USA.
[Muller, Nicholas] Middlebury Coll, Dept Econ, Middlebury, VT 05753 USA.
[Schwartz, Joel] Harvard Univ, Sch Publ Hlth, Dept Environm Hlth, Boston, MA 02215 USA.
[Streets, David] Argonne Natl Lab, Argonne, IL 60439 USA.
[Ramanathan, V.] Univ Calif San Diego, Scripps Inst Oceanog, San Diego, CA 92093 USA.
[Oanh, N. T. Kim] Asian Inst Technol, Bangkok 10400, Thailand.
[Williams, Martin] Kings Coll London, Environm Res Grp, London SE1 9NH, England.
[Demkine, Volodymyr] UNEP, Nairobi 00100, Kenya.
[Fowler, David] Ctr Ecol & Hydrol, Penicuik EH26 0QB, Midlothian, Scotland.
RP Shindell, D (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
EM drew.t.shindell@nasa.gov
RI Shindell, Drew/D-4636-2012; fowler, david/B-5446-2010; Klimont,
Zbigniew/P-7641-2015;
OI fowler, david/0000-0002-2999-2627; Klimont,
Zbigniew/0000-0003-2630-198X; Streets, David/0000-0002-0223-1350;
Pozzoli, Luca/0000-0003-0485-9624
FU UNEP; World Meteorlogical Organization (WMO), NASA; Clean Air Task Force
FX Funding was provided by UNEP and the World Meteorlogical Organization
(WMO), NASA's Applied Sciences and Atmospheric Chemistry Modeling and
Analysis Programs, and the Clean Air Task Force to IIASA. We thank all
the authors and reviewers who contributed to the UNEP/WMO Integrated
Assessment of Black Carbon and Tropospheric Ozone.
NR 40
TC 368
Z9 378
U1 57
U2 337
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 JAN 13
PY 2012
VL 335
IS 6065
BP 183
EP 189
DI 10.1126/science.1210026
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 875LZ
UT WOS:000299033100044
PM 22246768
ER
PT J
AU Ackermann, M
Ajello, M
Ballet, J
Barbiellini, G
Bastieri, D
Belfiore, A
Bellazzini, R
Berenji, B
Blandford, RD
Bloom, ED
Bonamente, E
Borgland, AW
Bregeon, J
Brigida, M
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caraveo, PA
Cavazzuti, E
Cecchi, C
Celik, O
Charles, E
Chaty, S
Chekhtman, A
Cheung, CC
Chiang, J
Ciprini, S
Claus, R
Cohen-Tanugi, J
Corbel, S
Corbet, RHD
Cutini, S
de Luca, A
den Hartog, PR
de Palma, F
Dermer, CD
Digel, SW
Silva, EDE
Donato, D
Drell, PS
Drlica-Wagner, A
Dubois, R
Dubus, G
Favuzzi, C
Fegan, SJ
Ferrara, EC
Focke, WB
Fortin, P
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Gehrels, N
Germani, S
Giglietto, N
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Grove, JE
Guiriec, S
Hadasch, D
Hanabata, Y
Harding, AK
Hayashida, M
Hays, E
Hill, AB
Hughes, RE
Johannesson, G
Johnson, AS
Johnson, TJ
Kamae, T
Katagiri, H
Kataoka, J
Kerr, M
Knodlseder, J
Kuss, M
Lande, J
Longo, F
Loparco, F
Lovellette, MN
Lubrano, P
Mazziotta, MN
McEnery, JE
Michelson, PF
Mitthumsiri, W
Mizuno, T
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Nakamori, T
Naumann-Godo, M
Norris, JP
Nuss, E
Ohno, M
Ohsugi, T
Okumura, A
Omodei, N
Orlando, E
Ozaki, M
Paneque, D
Parent, D
Pesce-Rollins, M
Pierbattista, M
Piron, F
Pivato, G
Porter, TA
Raino, S
Rando, R
Razzano, M
Reimer, A
Reimer, O
Ritz, S
Romani, RW
Roth, M
Parkinson, PMS
Sgro, C
Siskind, EJ
Spandre, G
Spinelli, P
Suson, DJ
Takahashi, H
Tanaka, T
Thayer, JG
Thayer, JB
Thompson, DJ
Tibaldo, L
Tinivella, M
Torres, DF
Tosti, G
Troja, E
Uchiyama, Y
Usher, TL
Vandenbroucke, J
Vianello, G
Vitale, V
Waite, AP
Winer, BL
Wood, KS
Wood, M
Yang, Z
Zimmer, S
Coe, MJ
Di Mille, F
Edwards, PG
Filipovic, MD
Payne, JL
Stevens, J
Torres, MAP
AF Ackermann, M.
Ajello, M.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Belfiore, A.
Bellazzini, R.
Berenji, B.
Blandford, R. D.
Bloom, E. D.
Bonamente, E.
Borgland, A. W.
Bregeon, J.
Brigida, M.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caraveo, P. A.
Cavazzuti, E.
Cecchi, C.
Celik, Oe.
Charles, E.
Chaty, S.
Chekhtman, A.
Cheung, C. C.
Chiang, J.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Corbel, S.
Corbet, R. H. D.
Cutini, S.
de Luca, A.
den Hartog, P. R.
de Palma, F.
Dermer, C. D.
Digel, S. W.
do Couto e Silva, E.
Donato, D.
Drell, P. S.
Drlica-Wagner, A.
Dubois, R.
Dubus, G.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Focke, W. B.
Fortin, P.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Gehrels, N.
Germani, S.
Giglietto, N.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Grove, J. E.
Guiriec, S.
Hadasch, D.
Hanabata, Y.
Harding, A. K.
Hayashida, M.
Hays, E.
Hill, A. B.
Hughes, R. E.
Johannesson, G.
Johnson, A. S.
Johnson, T. J.
Kamae, T.
Katagiri, H.
Kataoka, J.
Kerr, M.
Knoedlseder, J.
Kuss, M.
Lande, J.
Longo, F.
Loparco, F.
Lovellette, M. N.
Lubrano, P.
Mazziotta, M. N.
McEnery, J. E.
Michelson, P. F.
Mitthumsiri, W.
Mizuno, T.
Monte, C.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Nakamori, T.
Naumann-Godo, M.
Norris, J. P.
Nuss, E.
Ohno, M.
Ohsugi, T.
Okumura, A.
Omodei, N.
Orlando, E.
Ozaki, M.
Paneque, D.
Parent, D.
Pesce-Rollins, M.
Pierbattista, M.
Piron, F.
Pivato, G.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Reimer, A.
Reimer, O.
Ritz, S.
Romani, R. W.
Roth, M.
Parkinson, P. M. Saz
Sgro, C.
Siskind, E. J.
Spandre, G.
Spinelli, P.
Suson, D. J.
Takahashi, H.
Tanaka, T.
Thayer, J. G.
Thayer, J. B.
Thompson, D. J.
Tibaldo, L.
Tinivella, M.
Torres, D. F.
Tosti, G.
Troja, E.
Uchiyama, Y.
Usher, T. L.
Vandenbroucke, J.
Vianello, G.
Vitale, V.
Waite, A. P.
Winer, B. L.
Wood, K. S.
Wood, M.
Yang, Z.
Zimmer, S.
Coe, M. J.
Di Mille, F.
Edwards, P. G.
Filipovic, M. D.
Payne, J. L.
Stevens, J.
Torres, M. A. P.
CA Fermi LAT Collaboration
TI Periodic Emission from the Gamma-Ray Binary 1FGL J1018.6-5856
SO SCIENCE
LA English
DT Article
ID LARGE-AREA TELESCOPE; LS 5039; MICROQUASAR LS-5039; FERMI; MODULATION;
DISCOVERY; PULSARS; CATALOG; STARS; MASS
AB Gamma-ray binaries are stellar systems containing a neutron star or black hole, with gamma-ray emission produced by an interaction between the components. These systems are rare, even though binary evolution models predict dozens in our Galaxy. A search for gamma-ray binaries with the Fermi Large Area Telescope (LAT) shows that 1FGL J1018.6-5856 exhibits intensity and spectral modulation with a 16.6-day period. We identified a variable x-ray counterpart, which shows a sharp maximum coinciding with maximum gamma-ray emission, as well as an O6V((f)) star optical counterpart and a radio counterpart that is also apparently modulated on the orbital period. 1FGL J1018.6-5856 is thus a gamma-ray binary, and its detection suggests the presence of other fainter binaries in the Galaxy.
C1 [Ackermann, M.; Ajello, M.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; den Hartog, P. R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Kerr, M.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wood, M.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Ackermann, M.; Ajello, M.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; den Hartog, P. R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Kerr, M.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Ballet, J.; Chaty, S.; Corbel, S.; Grenier, I. A.; Naumann-Godo, M.; Pierbattista, M.] Univ Paris Diderot, CNRS, CEA IRFU, Lab AIM,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France.
[Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Pivato, G.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Belfiore, A.; Razzano, M.; Ritz, S.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Belfiore, A.; Razzano, M.; Ritz, S.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Belfiore, A.] Univ Pavia, I-27100 Pavia, Italy.
[Belfiore, A.; Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bruel, P.; Fegan, S. J.; Fortin, P.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Caliandro, G. A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEE CSIC, Barcelona 08193, Spain.
[Cavazzuti, E.; Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Rome, Italy.
[Celik, Oe.; Corbet, R. H. D.; Ferrara, E. C.; Gehrels, N.; Harding, A. K.; Hays, E.; McEnery, J. E.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Celik, Oe.; Donato, D.] Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA.
[Celik, Oe.; Corbet, R. H. D.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Chekhtman, A.] Artep Inc, Ellicott City, MD 21042 USA.
[Cheung, C. C.; Johnson, T. J.] Natl Acad Sci, Natl Res Council, Washington, DC 20001 USA.
[Ciprini, S.] ASI Sci Data Ctr, I-00044 Rome, Italy.
[Cohen-Tanugi, J.; Nuss, E.; Piron, F.] Univ Montpellier 2, CNRS, IN2P3, Lab Universe & Particules Montpellier, Montpellier, France.
[Corbel, S.] Inst Univ France, F-75005 Paris, France.
[de Luca, A.] Ist Univ Super, I-27100 Pavia, Italy.
[Dermer, C. D.; Grove, J. E.; Lovellette, M. N.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Donato, D.; McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[Donato, D.; McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Dubus, G.] Univ Grenoble 1, CNRS, UMR 5274, Inst Planetol & Astrophys Grenoble,INSU, F-38041 Grenoble, France.
[Fukazawa, Y.; Hanabata, Y.; Kataoka, J.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan.
[Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Guiriec, S.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA.
[Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Hill, A. B.; Coe, M. J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Hughes, R. E.; Winer, B. L.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Dept Phys, Columbus, OH 43210 USA.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Katagiri, H.] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan.
[Nakamori, T.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Knoedlseder, J.] IRAP, CNRS, F-31028 Toulouse 4, France.
[Knoedlseder, J.] Univ Toulouse, UPS OMP, IRAP, GAHEC, Toulouse, France.
[Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Norris, J. P.; Vitale, V.] Boise State Univ, Dept Phys, Boise, ID 83725 USA.
[Ohno, M.; Okumura, A.; Ozaki, M.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan.
[Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Parent, D.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Vianello, G.] CIFS, I-10133 Turin, Italy.
[Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Yang, Z.; Zimmer, S.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Yang, Z.; Zimmer, S.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Di Mille, F.] Las Campanas Observ, Australian Astron Observ, La Serena, Chile.
[Edwards, P. G.] CSIRO Astron & Space Sci, Australia Telescope Natl Facil, Narrabri, NSW 2390, Australia.
[Filipovic, M. D.; Payne, J. L.] Univ Western Sydney, Penrith, NSW 2751, Australia.
[Stevens, J.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Torres, M. A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Cheung, CC (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
EM teddy.cheung.ctr@nrl.navy.mil; robin.corbet@nasa.gov; kerrm@stanford.edu
RI Funk, Stefan/B-7629-2015; Johannesson, Gudlaugur/O-8741-2015; Loparco,
Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; Moskalenko,
Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro,
Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016;
Thompson, David/D-2939-2012; Gehrels, Neil/D-2971-2012; Harding,
Alice/D-3160-2012; Hays, Elizabeth/D-3257-2012; McEnery,
Julie/D-6612-2012; lubrano, pasquale/F-7269-2012; Morselli,
Aldo/G-6769-2011; Kuss, Michael/H-8959-2012; giglietto,
nicola/I-8951-2012; Reimer, Olaf/A-3117-2013; Tosti, Gino/E-9976-2013;
Saz Parkinson, Pablo Miguel/I-7980-2013; Ozaki, Masanobu/K-1165-2013;
Rando, Riccardo/M-7179-2013
OI Chaty, Sylvain/0000-0002-5769-8601; Pesce-Rollins,
Melissa/0000-0003-1790-8018; De Luca, Andrea/0000-0001-6739-687X;
Giroletti, Marcello/0000-0002-8657-8852; Cutini,
Sara/0000-0002-1271-2924; Gasparrini, Dario/0000-0002-5064-9495; Funk,
Stefan/0000-0002-2012-0080; Johannesson, Gudlaugur/0000-0003-1458-7036;
Loparco, Francesco/0000-0002-1173-5673; Gargano,
Fabio/0000-0002-5055-6395; Moskalenko, Igor/0000-0001-6141-458X;
Mazziotta, Mario /0000-0001-9325-4672; Torres,
Diego/0000-0002-1522-9065; Caraveo, Patrizia/0000-0003-2478-8018; Sgro',
Carmelo/0000-0001-5676-6214; Hill, Adam/0000-0003-3470-4834; Bastieri,
Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Thompson,
David/0000-0001-5217-9135; lubrano, pasquale/0000-0003-0221-4806;
Morselli, Aldo/0000-0002-7704-9553; giglietto,
nicola/0000-0002-9021-2888; Reimer, Olaf/0000-0001-6953-1385;
FU NASA (United States); U.S. Department of Energy (United States);
CEA/Irfu (France); IN2P3/CNRS (France); ASI (Italy); INFN (Italy); MEXT
(Japan); KEK (Japan); JAXA (Japan); K. A. Wallenberg Foundation; Swedish
Research Council; National Space Board (Sweden); CNES in France;
European Community [ERC-StG-200911]
FX The Fermi LAT Collaboration acknowledges support from a number of
agencies and institutes for both development and the operation of the
LAT as well as scientific data analysis. These include NASA and the U.S.
Department of Energy (United States); CEA/Irfu and IN2P3/CNRS (France);
ASI and INFN (Italy); MEXT, KEK, and JAXA (Japan); and the K. A.
Wallenberg Foundation, the Swedish Research Council, and the National
Space Board (Sweden). Additional support from INAF in Italy and CNES in
France for science analysis during the operations phase is also
gratefully acknowledged. Fermi LAT data are available from the Fermi
Science Support Center (http://fermi.gsfc.nasa.gov/ssc). This work made
use of data supplied by the UK Swift Science Data Centre at the
University of Leicester. G. D. was supported by European Community
contract ERC-StG-200911.
NR 26
TC 37
Z9 37
U1 1
U2 17
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
EI 1095-9203
J9 SCIENCE
JI Science
PD JAN 13
PY 2012
VL 335
IS 6065
BP 189
EP 193
DI 10.1126/science.1213974
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 875LZ
UT WOS:000299033100045
ER
PT J
AU Walker, TW
Jones, DBA
Parrington, M
Henze, DK
Murray, LT
Bottenheim, JW
Anlauf, K
Worden, JR
Bowman, KW
Shim, C
Singh, K
Kopacz, M
Tarasick, DW
Davies, J
von der Gathen, P
Thompson, AM
Carouge, CC
AF Walker, T. W.
Jones, D. B. A.
Parrington, M.
Henze, D. K.
Murray, L. T.
Bottenheim, J. W.
Anlauf, K.
Worden, J. R.
Bowman, K. W.
Shim, C.
Singh, K.
Kopacz, M.
Tarasick, D. W.
Davies, J.
von der Gathen, P.
Thompson, A. M.
Carouge, C. C.
TI Impacts of midlatitude precursor emissions and local photochemistry on
ozone abundances in the Arctic
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID ADJOINT SENSITIVITY-ANALYSIS; CHEMICAL-DATA ASSIMILATION;
NITROGEN-OXIDES; TROPOSPHERIC OZONE; AIR-POLLUTION; GEOS-CHEM;
SATELLITE-OBSERVATIONS; PEROXYACETYL NITRATE; INTEGRATED ANALYSIS;
REACTIVE NITROGEN
AB We assess the impact of transport of pollution from midlatitudes on the abundance of ozone in the Arctic in summer 2006 using the GEOS-Chem global chemical transport model and its adjoint. We find that although the impact of midlatitude emissions on ozone abundances in the Arctic is at a maximum in fall and winter, in July transport from North America, Asia, and Europe together contributed about 25% of surface ozone abundances in the Arctic. Throughout the summer, the dominant source of ozone in the Arctic troposphere was photochemical production within the Arctic, which accounted for more than 50% of the ozone in the Arctic boundary layer and as much as 30%-40% of the ozone in the middle troposphere. An adjoint sensitivity analysis of the impact of NOx emissions on ozone at Alert shows that on synoptic time scales in both the lower and middle troposphere, ozone abundances are more sensitive to emissions between 50 degrees N and 70 degrees N, with important influences from anthropogenic, biomass burning, soil, and lightning sources. Although local surface NOx emissions contribute to ozone formation, transport of NOx in the form of peroxyacetyl nitrate ( PAN) from outside the Arctic and from the upper troposphere also contributed to ozone production in the lower troposphere. We find that in late May and June the release of NOx from PAN decomposition accounted for 93% and 55% of ozone production at the Arctic surface, respectively.
C1 [Walker, T. W.; Jones, D. B. A.; Parrington, M.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Bottenheim, J. W.; Anlauf, K.; Tarasick, D. W.; Davies, J.] Environm Canada, Downsview, ON, Canada.
[Worden, J. R.; Bowman, K. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Murray, L. T.; Carouge, C. C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Henze, D. K.] Univ Colorado, Dept Mech Engn, Boulder, CO 80309 USA.
[Kopacz, M.] Princeton Univ, Woodrow Wilson Sch Publ & Int Affairs, Princeton, NJ 08544 USA.
[Shim, C.] Korea Environm Inst, Seoul 122706, South Korea.
[Singh, K.] Virginia Polytech Inst & State Univ, Dept Comp Sci, Blacksburg, VA 24061 USA.
[Thompson, A. M.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
[von der Gathen, P.] Alfred Wegener Inst Polar & Marine Res, Res Unit Potsdam, D-14473 Potsdam, Germany.
[Parrington, M.] Univ Edinburgh, Sch Geosci, Edinburgh, Midlothian, Scotland.
RP Walker, TW (reprint author), Univ Toronto, Dept Phys, 60 St George St, Toronto, ON M5S 1A7, Canada.
EM twalker@atmosp.physics.utoronto.ca
RI von der Gathen, Peter/B-8515-2009; Parrington, Mark/E-7148-2013; Chem,
GEOS/C-5595-2014; Murray, Lee/F-2296-2014; Jones, Dylan/O-2475-2014;
Singh, Kumaresh/P-4857-2016; Thompson, Anne /C-3649-2014
OI von der Gathen, Peter/0000-0001-7409-1556; Parrington,
Mark/0000-0003-4313-6218; Murray, Lee/0000-0002-3447-3952; Jones,
Dylan/0000-0002-1935-3725; Carouge, Claire/0000-0002-0313-8385;
Tarasick, David/0000-0001-9869-0692; Thompson, Anne /0000-0002-7829-0920
FU Natural Sciences and Engineering Research Council of Canada; Canadian
Foundation for Climate and Atmospheric Sciences
FX This work was supported by funding from the Natural Sciences and
Engineering Research Council of Canada and the Canadian Foundation for
Climate and Atmospheric Sciences. Ozonesonde data were retrieved from
the World Ozone and Ultraviolet Radiation Data Centre (WOUDC) at
http://www.woudc.org/.
NR 86
TC 23
Z9 23
U1 1
U2 21
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JAN 11
PY 2012
VL 117
AR D01305
DI 10.1029/2011JD016370
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 877LA
UT WOS:000299181000001
ER
PT J
AU Hobbs, WR
Willis, JK
AF Hobbs, Will R.
Willis, Joshua K.
TI Midlatitude North Atlantic heat transport: A time series based on
satellite and drifter data
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID MERIDIONAL OVERTURNING CIRCULATION; OCEAN HEAT; THERMOHALINE
CIRCULATION; DECADAL CHANGES; VARIABILITY; CLIMATE; RAINFALL; FLUX;
36-DEGREES-N; MODEL
AB Using temperature, salinity, and displacement data from Argo floats combined with satellite sea surface height, a time series of the Atlantic meridional heat transport from January 2002 to August 2010 has been estimated for 41 degrees N. The calculation method is validated against hydrographic climatologies and output from the ECCO2 ocean data assimilation model, and the assumptions are shown to be reasonable; the greatest source of error is from the sparse distribution of Argo floats. The mean heat transport is 0.50 +/- 0.1 PW, which is consistent with previous estimates made using surface flux data but is low compared estimates from hydrographic cruise data. Consistent with results from the RAPID array, the heat transport has a significant annual cycle and high degree of subannual variability, indicating that statistical uncertainty in previous calculations may have been underestimated. There is little evidence of a trend over the short period of available data. Correlations with sea surface temperature suggest clear physical relationships between heat transport and SST, even on the short time scales of available data.
C1 [Hobbs, Will R.; Willis, Joshua K.] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA.
RP Hobbs, WR (reprint author), CALTECH, NASA Jet Prop Lab, 4800 Oak Grove Dr,M-S 300-323, Pasadena, CA 91109 USA.
EM william.r.hobbs@jpl.nasa.gov
RI Hobbs, Will/G-5116-2014
OI Hobbs, Will/0000-0002-2061-0899
FU NASA
FX The authors wish to thank W. Johns for helpful discussions over the
course of this work, and for supplying MHT data from the RAPID array. We
also thank three anonymous reviewers. Altimeter products were produced
by Ssalto/Duacs and distributed by Aviso with support from CNES. Argo
data were collected and made freely available by the International Argo
Project (http://www.argo.ucsd.edu). Scatterometer products were produced
and distributed by IFREMER. Data analysis was performed using the NCAR
Command Language (http://www.ncl.ucar.edu). This work was carried out at
the Jet Propulsion Laboratory, California Institute of Technology, under
a contract with NASA.
NR 48
TC 23
Z9 24
U1 0
U2 7
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 JAN 11
PY 2012
VL 117
AR C01008
DI 10.1029/2011JC007039
PG 14
WC Oceanography
SC Oceanography
GA 877LE
UT WOS:000299181600001
ER
PT J
AU Mohamed, AA
Gopalswamy, N
Yashiro, S
Akiyama, S
Makela, P
Xie, H
Jung, H
AF Mohamed, A. A.
Gopalswamy, N.
Yashiro, S.
Akiyama, S.
Maekelae, P.
Xie, H.
Jung, H.
TI The relation between coronal holes and coronal mass ejections during the
rise, maximum, and declining phases of Solar Cycle 23
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID ENERGETIC PARTICLE EVENTS; ART. NO. A12105; INTERPLANETARY SHOCKS;
MAGNETIC CLOUDS; WIND; EVOLUTION; LASCO
AB We study the interaction between coronal holes (CHs) and coronal mass ejections (CMEs) using a resultant force exerted by all the coronal holes present on the disk and is defined as the coronal hole influence parameter (CHIP). The CHIP magnitude for each CH depends on the CH area, the distance between the CH centroid and the eruption region, and the average magnetic field within the CH at the photospheric level. The CHIP direction for each CH points from the CH centroid to the eruption region. We focus on Solar Cycle 23 CMEs originating from the disk center of the Sun (central meridian distance <= 15 degrees) and resulting in magnetic clouds (MCs) and non-MCs in the solar wind. The CHIP is found to be the smallest during the rise phase for MCs and non-MCs. The maximum phase has the largest CHIP value (2.9 G) for non-MCs. The CHIP is the largest (5.8 G) for driverless (DL) shocks, which are shocks at 1 AU with no discernible MC or non-MC. These results suggest that the behavior of non-MCs is similar to that of the DL shocks and different from that of MCs. In other words, the CHs may deflect the CMEs away from the Sun-Earth line and force them to behave like limb CMEs with DL shocks. This finding supports the idea that all CMEs may be flux ropes if viewed from an appropriate vantage point.
C1 [Mohamed, A. A.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia.
[Mohamed, A. A.; Gopalswamy, N.; Yashiro, S.; Akiyama, S.; Maekelae, P.; Xie, H.; Jung, H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mohamed, A. A.; Yashiro, S.; Akiyama, S.; Maekelae, P.; Xie, H.; Jung, H.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
[Mohamed, A. A.] Natl Res Inst Astron & Geophys, Cairo, Egypt.
RP Mohamed, AA (reprint author), Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia.
EM amaal.shahin@nasa.gov
RI Gopalswamy, Nat/D-3659-2012
FU Ministry of Higher Education in Egypt; NASA [NNXO9AT38A]
FX We thank the SOHO, Wind and ACE science teams for making the shock data
available online. A.A.M. acknowledges the scholarship from the Ministry
of Higher Education in Egypt and NASA grant NNXO9AT38A.
NR 37
TC 11
Z9 11
U1 0
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9380
EI 2169-9402
J9 J GEOPHYS RES-SPACE
JI J. Geophys. Res-Space Phys.
PD JAN 11
PY 2012
VL 117
AR A01103
DI 10.1029/2011JA016589
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 877KE
UT WOS:000299177900001
ER
PT J
AU Forman, BA
Reichle, RH
Rodell, M
AF Forman, B. A.
Reichle, R. H.
Rodell, M.
TI Assimilation of terrestrial water storage from GRACE in a snow-dominated
basin
SO WATER RESOURCES RESEARCH
LA English
DT Article
ID ENSEMBLE KALMAN SMOOTHER; SOIL-MOISTURE ESTIMATION; EQUIVALENT; DEPTH;
MODEL; GRAVITY; CLIMATE; IMPACT; FLUX
AB Terrestrial water storage (TWS) information derived from gravity recovery and climate experiment (GRACE) measurements is assimilated into a land surface model over the Mackenzie River basin located in northwest Canada. Assimilation is conducted using an ensemble Kalman smoother (EnKS). Model estimates with and without assimilation are compared against independent observational data sets of snow water equivalent (SWE) and runoff. For SWE, modest improvements in mean difference (MD) and root-mean-square difference (RMSD) are achieved as a result of the assimilation. No significant differences in temporal correlations of SWE resulted. Runoff statistics of MD remain relatively unchanged while RMSD statistics, in general, are improved in most of the sub-basins. Temporal correlations are degraded within the most upstream sub-basin, but are, in general, improved at the downstream locations, which are more representative of an integrated basin response. GRACE assimilation using an EnKS offers improvements in hydrologic state/flux estimation, though comparisons with observed runoff would be enhanced by the use of river routing and lake storage routines within the prognostic land surface model. Further, GRACE hydrology products would benefit from the inclusion of better constrained models of postglacial rebound, which significantly affects GRACE estimates of interannual hydrologic variability in the Mackenzie River basin.
C1 [Forman, B. A.; Reichle, R. H.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Rodell, M.] NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA.
[Forman, B. A.] Oak Ridge Associated Univ, Oak Ridge, TN USA.
RP Forman, BA (reprint author), Univ Maryland, Dept Civil & Environm Engn, 1159 Glenn Martin Hall, College Pk, MD 20742 USA.
EM barton.a.forman@nasa.gov
RI Reichle, Rolf/E-1419-2012; Rodell, Matthew/E-4946-2012; Forman,
Barton/I-2227-2012
OI Rodell, Matthew/0000-0003-0106-7437;
FU NASA [NNH06CC03B]
FX Funding for this work was provided by the NASA Postdoctoral Program
Fellowship (contract NNH06CC03B). Additional thanks go to Ross Brown for
answers to our questions regarding the CMC snow analysis product, Derek
Faria for access to the INAC snow surveys, Ulrich Looser for access to
the GRDC database, John Wahr, Sean Swenson, and Felix Landerer for
discussions on PGR, and Bailing Li and Gabrielle De Lannoy for many
constructive conversations. Helpful comments by three anonymous
reviewers are also gratefully acknowledged.
NR 39
TC 26
Z9 27
U1 1
U2 35
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0043-1397
EI 1944-7973
J9 WATER RESOUR RES
JI Water Resour. Res.
PD JAN 11
PY 2012
VL 48
AR W01507
DI 10.1029/2011WR011239
PG 14
WC Environmental Sciences; Limnology; Water Resources
SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water
Resources
GA 877LP
UT WOS:000299183000002
ER
PT J
AU Schmidt, F
Leauthaud, A
Massey, R
Rhodes, J
George, MR
Koekemoer, AM
Finoguenov, A
Tanaka, M
AF Schmidt, Fabian
Leauthaud, Alexie
Massey, Richard
Rhodes, Jason
George, Matthew R.
Koekemoer, Anton M.
Finoguenov, Alexis
Tanaka, Masayuki
TI A DETECTION OF WEAK-LENSING MAGNIFICATION USING GALAXY SIZES AND
MAGNITUDES
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE dark matter; gravitational lensing: weak; large-scale structure of
universe
ID WIDE-FIELD SURVEY; LARGE-SCALE STRUCTURE; COSMOS FIELD; ENVIRONMENTAL
DEPENDENCE; IMAGE SIMULATION; SOURCE CATALOG; SHAPELETS; TELESCOPE;
MASS; REDSHIFTS
AB Weak lensing is commonly measured using shear through galaxy ellipticities or using the effect of magnification bias on galaxy number densities. Here, we report on the first detection of weak-lensing magnification with a new, independent technique using the distribution of galaxy sizes and magnitudes. These data come for free in galaxy surveys designed for measuring shear. We present the magnification estimator and apply it to an X-ray-selected sample of galaxy groups in the COSMOS Hubble Space Telescope survey. The measurement of the projected surface density Sigma(r) is consistent with the shear measurements within the uncertainties and has roughly 40% of the signal to noise of the latter. We discuss systematic issues and challenges to realizing the potential of this new probe of weak lensing.
C1 [Schmidt, Fabian; Rhodes, Jason] CALTECH, Pasadena, CA 91125 USA.
[Leauthaud, Alexie; Tanaka, Masayuki] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2778582, Japan.
[Massey, Richard] Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Rhodes, Jason] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[George, Matthew R.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Finoguenov, Alexis] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Finoguenov, Alexis] Univ Maryland Baltimore Cty, Ctr Space Sci Technol, Baltimore, MD 21250 USA.
RP Schmidt, F (reprint author), CALTECH, MC 350-17,1200 E Calif Blvd, Pasadena, CA 91125 USA.
OI Schmidt, Fabian/0000-0002-6807-7464; Koekemoer,
Anton/0000-0002-6610-2048
FU Gordon and Betty Moore Foundation; STFC; JPL; World Premier
International Research Center Initiative (WPI Initiative), MEXT, Japan
FX We thank Jessica Ford, Hendrik Hildebrandt, Bhuvnesh Jain, Donghui
Jeong, Eric Jullo, James Taylor, and Ludovic van Waerbeke for helpful
discussions. F. S. is supported by the Gordon and Betty Moore
Foundation. R. M. is supported by an STFC Advanced Fellowship. J.R. was
supported by JPL, run by Caltech for NASA. This work was supported by
World Premier International Research Center Initiative (WPI Initiative),
MEXT, Japan.
NR 38
TC 35
Z9 35
U1 1
U2 2
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 JAN 10
PY 2012
VL 744
IS 2
AR L22
DI 10.1088/2041-8205/744/2/L22
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 891OR
UT WOS:000300227000006
ER
PT J
AU Chuss, DT
Wollack, EJ
Henry, R
Hui, H
Juarez, AJ
Krejny, M
Moseley, SH
Novak, G
AF Chuss, David T.
Wollack, Edward J.
Henry, Ross
Hui, Howard
Juarez, Aaron J.
Krejny, Megan
Moseley, S. Harvey
Novak, Giles
TI Properties of a variable-delay polarization modulator
SO APPLIED OPTICS
LA English
DT Article
ID SUBMILLIMETER WAVELENGTHS; WIRE GRIDS; POLARIMETER; MILLIMETER;
INTERFEROMETER; PERFORMANCE; HERTZ
AB We investigate the polarization modulation properties of a variable-delay polarization modulator (VPM). The VPM modulates polarization via a variable separation between a polarizing grid and a parallel mirror. We find that in the limit where the wavelength is much larger than the diameter of the metal wires that comprise the grid, the phase delay derived from the geometric separation between the mirror and the grid is sufficient to characterize the device. However, outside of this range, additional parameters describing the polarizing grid geometry must be included to fully characterize the modulator response. In this paper, we report test results of a VPM at wavelengths of 350 mu m and 3 mm. Electromagnetic simulations of wire grid polarizers were performed and are summarized using a simple circuit model that incorporates the loss and polarization properties of the device.
C1 [Chuss, David T.; Wollack, Edward J.; Henry, Ross; Moseley, S. Harvey] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Novak, Giles] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA.
[Krejny, Megan] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA.
[Juarez, Aaron J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Hui, Howard] CALTECH, Pasadena, CA 91125 USA.
RP Chuss, DT (reprint author), NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA.
EM David.T.Chuss@nasa.gov
RI Chuss, David/D-8281-2012; Wollack, Edward/D-4467-2012
OI Wollack, Edward/0000-0002-7567-4451
FU NASA ROSES/APRA; Graduate Student Researchers Program [NNG05-GL31H];
Goddard Space Flight Center
FX This work was funded by a NASA ROSES/APRA award. M. Krejny was supported
by Graduate Student Researchers Program grant NNG05-GL31H. H. Hui was
supported by an Undergraduate Student Research Program grant at Goddard
Space Flight Center. We would like to thank G. Voellmer for his work on
design and construction of the VPMs. We would also like to thank R. F.
Loewenstein, C. Walker, C. Kulesa, C. Y. Drouet d'Aubigny, and D. Golish
for their work on Hertz-VPM. We thank Roger Hildebrand for the use of
the Hertz cryostat and Bob Pernic for critical cryostat repairs during
the laboratory testing. We also thank the anonymous reviewers whose
comments have helped to improve the paper.
NR 44
TC 22
Z9 22
U1 0
U2 3
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD JAN 10
PY 2012
VL 51
IS 2
BP 197
EP 208
PG 12
WC Optics
SC Optics
GA 879EY
UT WOS:000299313700008
PM 22270517
ER
PT J
AU Wan, P
Liu, J
Yang, LM
Amzajerdian, F
AF Wan, Peng
Liu, Jian
Yang, Lih-Mei
Amzajerdian, Farzin
TI Pulse shaping fiber laser at 1.5 mu m
SO APPLIED OPTICS
LA English
DT Article
ID COMMUNICATION; TRANSMITTERS; THRESHOLD; NM
AB In this paper we present, for the first time to our knowledge, a new pulse shaping technology (modulation schemes for seed laser) used to mitigate pulse narrowing effect and SBS effect in a high energy Er:Yb codoped fiber master oscillator power amplifier system at 1.5 mu m to obtain longer pulse duration and higher energy. An average power of over 1.3 W and a pulse energy of over 0.13 mJ were obtained at 10 kHz repetition rate with a pulse duration of 200 ns and near-diffraction-limited beam quality (M-2 < 1.2). (C) 2012 Optical Society of America
C1 [Wan, Peng; Liu, Jian; Yang, Lih-Mei] PolarOnyx Inc, San Jose, CA 95131 USA.
[Amzajerdian, Farzin] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Wan, P (reprint author), PolarOnyx Inc, 2526 Qume Dr,Suites 17 & 18, San Jose, CA 95131 USA.
EM pwan@polaronyx.com
FU NASA
FX This paper is supported in part by NASA Small Business Innovation
Research contracts.
NR 13
TC 2
Z9 2
U1 2
U2 3
PU OPTICAL SOC AMER
PI WASHINGTON
PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA
SN 1559-128X
EI 2155-3165
J9 APPL OPTICS
JI Appl. Optics
PD JAN 10
PY 2012
VL 51
IS 2
BP 214
EP 219
PG 6
WC Optics
SC Optics
GA 879EY
UT WOS:000299313700010
PM 22270519
ER
PT J
AU Abdo, AA
Wood, KS
DeCesar, ME
Gargano, F
Giordano, F
Ray, PS
Parent, D
Harding, AK
Miller, MC
Wood, DL
Wolff, MT
AF Abdo, A. A.
Wood, K. S.
DeCesar, M. E.
Gargano, F.
Giordano, F.
Ray, P. S.
Parent, D.
Harding, A. K.
Miller, M. Coleman
Wood, D. L.
Wolff, M. T.
TI PSR J0007+7303 IN THE CTA1 SUPERNOVA REMNANT: NEW GAMMA-RAY RESULTS FROM
TWO YEARS OF FERMI LARGE AREA TELESCOPE OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma rays: stars; pulsars: individual: PSR J0007+7303; supernovae:
individual (G119.5+10.2)
ID X-RAY; EGRET DATA; PARAMETER-ESTIMATION; NEUTRINO EMISSION; LIGHT
CURVES; PULSAR; RADIO; SEARCH; CATALOG; NEBULA
AB One of the main results of the Fermi Gamma-Ray Space Telescope is the discovery of gamma-ray selected pulsars. The high magnetic field pulsar, PSR J0007+7303 in CTA1, was the first ever to be discovered through its gamma-ray pulsations. Based on analysis of two years of Large Area Telescope (LAT) survey data, we report on the discovery of gamma-ray emission in the off-pulse phase interval at the similar to 6 sigma level. The emission appears to be extended at the similar to 2 sigma level with a disk of extension similar to 0.degrees 6. level. The flux from this emission in the energy range E >= 100 MeV is F-100 = (1.73 +/- 0.40(stat) +/- 0.18(sys)) x 10(-8) photons cm(-2) s(-1) and is best fitted by a power law with a photon index of Gamma = 2.54 +/- 0.14(stat) +/- 0.05(sys). The pulsed gamma-ray flux in the same energy range is F-100 = (3.95 +/- 0.07(stat) +/- 0.30(sys)) x 10 (7) photons cm (2) s (1) and is best fitted by an exponentially cutoff power-law spectrum with a photon index of Gamma = 1.41 +/- 0.23(stat) +/- 0.03(sys) and a cutoff energy E-c = 4.04 +/- 0.20(stat) +/- 0.67(sys) GeV. We find no flux variability either at the 2009 May glitch or in the long-term behavior. We model the gamma-ray light curve with two high-altitude emission models, the outer gap and slot gap, and find that the preferred model depends strongly on the assumed origin of the off-pulse emission. Both models favor a large angle between the magnetic axis and observer line of sight, consistent with the nondetection of radio emission being a geometrical effect. Finally, we discuss how the LAT results bear on the understanding of the cooling of this neutron star.
C1 [Abdo, A. A.; Parent, D.] George Mason Univ, Ctr Earth Observing & Space Res, Coll Sci, Fairfax, VA 22030 USA.
[Wood, K. S.; Ray, P. S.; Wolff, M. T.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA.
[DeCesar, M. E.; Harding, A. K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[DeCesar, M. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[DeCesar, M. E.; Miller, M. Coleman] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Gargano, F.; Giordano, F.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Giordano, F.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Giordano, F.] Politecn Bari, I-70126 Bari, Italy.
[Wood, D. L.] Praxis Inc, Alexandria, VA 22303 USA.
RP Abdo, AA (reprint author), George Mason Univ, Ctr Earth Observing & Space Res, Coll Sci, Fairfax, VA 22030 USA.
RI Harding, Alice/D-3160-2012; Gargano, Fabio/O-8934-2015
OI Giordano, Francesco/0000-0002-8651-2394; Ray, Paul/0000-0002-5297-5278;
Gargano, Fabio/0000-0002-5055-6395
FU National Aeronautics and Space Administration; Department of Energy in
the United States; Commissariat a l'Energie Atomique; Centre National de
la Recherche Scientifique/Institut National de Physique Nucleaire et de
Physique des Particules in France; Agenzia Spaziale Italiana and the
Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education,
Culture, Sports, Science and Technology (MEXT); High Energy Accelerator
Research Organization (KEK); Japan Aerospace Exploration Agency (JAXA)
in Japan; K. A. Wallenberg Foundation; Swedish Research Council; Swedish
National Space Board in Sweden; Naval Research Laboratory
[N000173-08-2-C004]
FX The Fermi-LAT Collaboration acknowledges generous ongoing support from a
number of agencies and institutes that have supported both the
development and the operation of the LAT as well as scientific data
analysis. These include the National Aeronautics and Space
Administration and the Department of Energy in the United States, the
Commissariat a l'Energie Atomique and the Centre National de la
Recherche Scientifique/Institut National de Physique Nucleaire et de
Physique des Particules in France, the Agenzia Spaziale Italiana and the
Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of
Education, Culture, Sports, Science and Technology (MEXT), High Energy
Accelerator Research Organization (KEK), and Japan Aerospace Exploration
Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish
Research Council, and the Swedish National Space Board in Sweden.; This
work was performed under contract with the Naval Research Laboratory,
contract N000173-08-2-C004 and was sponsored under a grant by NASA.
NR 35
TC 16
Z9 16
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2012
VL 744
IS 2
AR 146
DI 10.1088/0004-637X/744/2/146
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 870JW
UT WOS:000298666400066
ER
PT J
AU Bhat, PN
Briggs, MS
Connaughton, V
Kouveliotou, C
van der Horst, AJ
Paciesas, W
Meegan, CA
Bissaldi, E
Burgess, M
Chaplin, V
Diehl, R
Fishman, G
Fitzpatrick, G
Foley, S
Gibby, M
Giles, MM
Goldstein, A
Greiner, J
Gruber, D
Guiriec, S
von Kienlin, A
Kippen, M
McBreen, S
Preece, R
Rau, A
Tierney, D
Wilson-Hodge, C
AF Bhat, P. N.
Briggs, Michael S.
Connaughton, Valerie
Kouveliotou, Chryssa
van der Horst, Alexander J.
Paciesas, William
Meegan, Charles A.
Bissaldi, Elisabetta
Burgess, Michael
Chaplin, Vandiver
Diehl, Roland
Fishman, Gerald
Fitzpatrick, Gerard
Foley, Suzanne
Gibby, Melissa
Giles, Misty M.
Goldstein, Adam
Greiner, Jochen
Gruber, David
Guiriec, Sylvain
von Kienlin, Andreas
Kippen, Marc
McBreen, Sheila
Preece, Robert
Rau, Arne
Tierney, Dave
Wilson-Hodge, Colleen
TI TEMPORAL DECONVOLUTION STUDY OF LONG AND SHORT GAMMA-RAY BURST LIGHT
CURVES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: general; methods: data analysis; relativistic processes
ID LOGNORMAL DISTRIBUTIONS; TIME; SPECTROSCOPY; VARIABILITY; PULSES; STARS;
BRIGHTEST; PROFILES; MONITOR; ENGINE
AB The light curves of gamma-ray bursts (GRBs) are believed to result from internal shocks reflecting the activity of the GRB central engine. Their temporal deconvolution can reveal potential differences in the properties of the central engines in the two populations of GRBs which are believed to originate from the deaths of massive stars (long) and from mergers of compact objects (short). We present here the results of the temporal analysis of 42 GRBs detected with the Gamma-ray Burst Monitor onboard the Fermi Gamma-ray Space Telescope. We deconvolved the profiles into pulses, which we fit with lognormal functions. The distributions of the pulse shape parameters and intervals between neighboring pulses are distinct for both burst types and also fit with lognormal functions. We have studied the evolution of these parameters in different energy bands and found that they differ between long and short bursts. We discuss the implications of the differences in the temporal properties of long and short bursts within the framework of the internal shock model for GRB prompt emission.
C1 [Bhat, P. N.; Briggs, Michael S.; Connaughton, Valerie; Paciesas, William; Burgess, Michael; Chaplin, Vandiver; Goldstein, Adam; Guiriec, Sylvain; Preece, Robert] Univ Alabama, NSSTC, CSPAR, Huntsville, AL 35805 USA.
[Kouveliotou, Chryssa; Fishman, Gerald; Wilson-Hodge, Colleen] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA.
[van der Horst, Alexander J.; Meegan, Charles A.] NSSTC, Univ Space Res Assoc, CSPAR, Huntsville, AL 35805 USA.
[Bissaldi, Elisabetta] Univ Innsbruck, Inst Astro & Particle Phys, A-6020 Innsbruck, Austria.
[Diehl, Roland; Foley, Suzanne; Greiner, Jochen; Gruber, David; von Kienlin, Andreas; Rau, Arne] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Fitzpatrick, Gerard; McBreen, Sheila; Tierney, Dave] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Gibby, Melissa; Giles, Misty M.] Jacobs Technol Inc, Huntsville, AL 35806 USA.
[Kippen, Marc] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
RP Bhat, PN (reprint author), Univ Alabama, NSSTC, CSPAR, 320 Sparkman Dr, Huntsville, AL 35805 USA.
RI Bissaldi, Elisabetta/K-7911-2016;
OI Bissaldi, Elisabetta/0000-0001-9935-8106; Preece,
Robert/0000-0003-1626-7335
FU German Bundesministerium fur Wirtschaft und Technologie (BMWi) via the
Deutsches Zentrum fur Luft-und Raumfahrt (DLR) [50 QV 0301, 50 OG 0502];
NASA [NNH07ZDA001-GLAST]; Union Marie Curie European Reintegration Grant
within the 7th Program [PERG04-GA-2008-239176]; Irish Research Council
for Science, Engineering and Technology; Marie Curie Actions under FP7
FX The GBM project is supported by the German Bundesministerium fur
Wirtschaft und Technologie (BMWi) via the Deutsches Zentrum fur Luft-und
Raumfahrt (DLR) under the contract nos. 50 QV 0301 and 50 OG 0502.
A.J.v.d.H. was supported by NASA Grant NNH07ZDA001-GLAST. S. M. B.
acknowledges support of the Union Marie Curie European Reintegration
Grant within the 7th Program under contract no. PERG04-GA-2008-239176.
S. F. acknowledges the support of the Irish Research Council for
Science, Engineering and Technology, cofunded by Marie Curie Actions
under FP7. We also acknowledge the constructive comments and suggestions
from the anonymous referee which improved the quality of presentation.
NR 44
TC 16
Z9 16
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2012
VL 744
IS 2
AR 141
DI 10.1088/0004-637X/744/2/141
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 870JW
UT WOS:000298666400061
ER
PT J
AU Cordiner, MA
Charnley, SB
Wirstrom, ES
Smith, RG
AF Cordiner, Martin A.
Charnley, Steven B.
Wirstroem, Eva S.
Smith, Robert G.
TI ORGANIC CHEMISTRY OF LOW-MASS STAR-FORMING CORES. I. 7 mm SPECTROSCOPY
OF CHAMAELEON MMS1
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; ISM: abundances; radio lines: ISM; radio lines: stars;
stars: formation
ID DENSE INTERSTELLAR CLOUDS; 1ST HYDROSTATIC CORE; CARBON-CHAIN-CHEMISTRY;
DARK CLOUDS; PROTOSTELLAR ENVELOPES; MOLECULAR CLOUDS; DEUTERATED
MOLECULES; CHEMICAL EVOLUTION; DEUTERIUM FRACTIONATION; LINE
OBSERVATIONS
AB Observations are presented of emission lines from organic molecules at frequencies 32-50 GHz in the vicinity of Chamaeleon MMS1. This chemically rich dense cloud core harbors an extremely young, very low luminosity protostellar object and is a candidate first hydrostatic core. Column densities are derived and emission maps are presented for species including polyynes, cyanopolyynes, sulphuretted carbon chains, and methanol. The polyyne emission peak lies about 5000 AU from the protostar, whereas methanol peaks about 15,000 AU away. Averaged over the telescope beam, the molecular hydrogen number density is calculated to be 10(6) cm(-3) and the gas kinetic temperature is in the range 5-7 K. The abundances of long carbon chains are very large and are indicative of a non-equilibrium carbon chemistry; C6H and HC7N column densities are 5.9(-1.3)(+2.9) x 10(11) cm(-2) and 3.3(-1.5)(+8.0) x 10(12) cm(-2), respectively, which are similar to the values found in the most carbon-chain-rich protostars and prestellar cores known, and are unusually large for star-forming gas. Column density upper limits were obtained for the carbon-chain anions C4H- and C6H-, with anion-to-neutral ratios [C4H-]/[C4H] < 0.02% and [C6H-]/[C6H] < 10%, consistent with previous observations in interstellar clouds and low-mass protostars. Deuterated HC3N and c-C3H2 were detected. The [DC3N]/[HC3N] ratio of approximately 4% is consistent with the value typically found in cold interstellar gas.
C1 [Cordiner, Martin A.; Charnley, Steven B.; Wirstroem, Eva S.] Astrochem Lab, Greenbelt, MD 20770 USA.
[Cordiner, Martin A.; Charnley, Steven B.; Wirstroem, Eva S.] NASA, Goddard Ctr Astrobiol, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA.
[Smith, Robert G.] Univ New S Wales, Australian Def Force Acad, Sch Phys Environm & Math Sci, Canberra, ACT 2600, Australia.
[Cordiner, Martin A.; Wirstroem, Eva S.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Cordiner, MA (reprint author), Astrochem Lab, Greenbelt, MD 20770 USA.
EM martin.cordiner@nasa.gov
RI Charnley, Steven/C-9538-2012;
OI Wirstrom, Eva/0000-0002-0656-876X
FU Goddard Center for Astrobiology; NASA
FX We gratefully acknowledge the assistance of Balt Indermuehle at Mopra
for providing support during on-site and remote observations. Thanks to
Arnaud Belloche for comments on the manuscript. This work was supported
by the Goddard Center for Astrobiology and NASA's Origins of Solar
Systems and Exobiology programs.
NR 86
TC 12
Z9 12
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 JAN 10
PY 2012
VL 744
IS 2
AR 131
DI 10.1088/0004-637X/744/2/131
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 870JW
UT WOS:000298666400051
ER
PT J
AU Flock, M
Dzyurkevich, N
Klahr, H
Turner, N
Henning, T
AF Flock, M.
Dzyurkevich, N.
Klahr, H.
Turner, N.
Henning, Th
TI LARGE-SCALE AZIMUTHAL STRUCTURES OF TURBULENCE IN ACCRETION DISKS:
DYNAMO TRIGGERED VARIABILITY OF ACCRETION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; dynamo; magnetic fields;
magnetohydrodynamics (MHD); protoplanetary disks
ID 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS; WEAKLY MAGNETIZED DISKS;
LOCAL SHEAR INSTABILITY; GLOBAL MHD SIMULATIONS; ANGULAR-MOMENTUM
TRANSPORT; PROTOPLANETARY DISKS; MAGNETOROTATIONAL INSTABILITY;
ROTATIONAL INSTABILITY; STRATIFIED DISKS; ISOTHERMAL DISKS
AB We investigate the significance of large-scale azimuthal, magnetic, and velocity modes for the magnetorotational instability (MRI) turbulence in accretion disks. We perform three-dimensional global ideal MHD simulations of global stratified protoplanetary disk models. Our domains span azimuthal angles of pi/4, pi/2, pi, and pi p. We observe up to 100% stronger magnetic fields and stronger turbulence for the restricted azimuthal domain models pi/2 and pi/4 compared to the full 2 pi model. We show that for those models the Maxwell stress is larger due to strong axisymmetric magnetic fields generated by the alpha Omega dynamo. Large radial extended axisymmetric toroidal fields trigger temporal magnification of accretion stress. All models display a positive dynamo-alpha in the northern hemisphere (upper disk). The parity is distinct in each model and changes on timescales of 40 local orbits. In model 2 pi, the toroidal field is mostly antisymmetric with respect to the midplane. The eddies of the MRI turbulence are highly anisotropic. The major wavelengths of the turbulent velocity and magnetic fields are between one and two disk scale heights. At the midplane, we find magnetic tilt angles around 8 degrees-9 degrees increasing up to 12 degrees-13 degrees in the corona. We conclude that an azimuthal extent of pi is sufficient to reproduce most turbulent properties in three-dimensional global stratified simulations of magnetized accretion disks.
C1 [Flock, M.; Dzyurkevich, N.; Klahr, H.; Turner, N.; Henning, Th] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Turner, N.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Flock, M (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
FU Deutsche Forschungsgemeinschaft DFG through DFG Forschergruppe [759];
NASA through the Jet Propulsion Laboratory, California Institute of
Technology; Alexander von Humboldt Foundation
FX We thank Andrea Mignone for providing us with the newest code version
and the discussion on the numerical configuration, Sebastien Fromang for
the helpful comments on the global models, Gunther Rudiger and Rainer
Arlt for their comments on the manuscript, and Geoffroy Lesur for the
discussion about the dynamo effect. H. K., N.D., and M. F. have been
supported in part by the Deutsche Forschungsgemeinschaft DFG through
grant DFG Forschergruppe 759 "The Formation of Planets. The Critical
FirstGrowth Phase." N.T. was supported by a NASA Solar Systems Origins
grant through the Jet Propulsion Laboratory, California Institute of
Technology, and by an Alexander von Humboldt Foundation Fellowship for
Experienced Researchers. Parallel computations have been performed on
the Theo cluster of the Max Planck Institute for Astronomy, Heidelberg,
as well as the GENIUS Blue Gene/P cluster, both located at the computing
center of the Max Planck Society in Garching.
NR 59
TC 25
Z9 25
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2012
VL 744
IS 2
AR 144
DI 10.1088/0004-637X/744/2/144
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 870JW
UT WOS:000298666400064
ER
PT J
AU Grav, T
Mainzer, AK
Bauer, J
Masiero, J
Spahr, T
McMillan, RS
Walker, R
Cutri, R
Wright, E
Eisenhardt, PR
Blauvelt, E
DeBaun, E
Elsbury, D
Gautier, T
Gomillion, S
Hand, E
Wilkins, A
AF Grav, T.
Mainzer, A. K.
Bauer, J.
Masiero, J.
Spahr, T.
McMillan, R. S.
Walker, R.
Cutri, R.
Wright, E.
Eisenhardt, P. R.
Blauvelt, E.
DeBaun, E.
Elsbury, D.
Gautier, T.
Gomillion, S.
Hand, E.
Wilkins, A.
TI WISE/NEOWISE OBSERVATIONS OF THE HILDA POPULATION: PRELIMINARY RESULTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: planetary systems; minor planets, asteroids: general; surveys
ID ASTEROID SPECTROSCOPIC SURVEY; THERMAL-MODEL CALIBRATION;
INFRARED-SURVEY-EXPLORER; LATE HEAVY BOMBARDMENT; NEAR-EARTH ASTEROIDS;
SOLAR-SYSTEM; ORBITAL ARCHITECTURE; SURFACE-COMPOSITION; TROJAN
ASTEROIDS; GIANT PLANETS
AB We present the preliminary analysis of 1023 known asteroids in the Hilda region of the solar system observed by the NEOWISE component of the Wide-field Infrared Survey Explorer (WISE). The sizes of the Hildas observed range from similar to 3 to 200 km. We find no size-albedo dependency as reported by other projects. The albedos of our sample are low, with a weighted mean value of p(V) = 0.055 +/- 0.018, for all sizes sampled by the NEOWISE survey. We observed a significant fraction of the objects in the two known collisional families in the Hilda population. It is found that the Hilda collisional family is brighter, with a weighted mean albedo of p(V) = 0.061 +/- 0.011, than the general population and dominated by D-type asteroids, while the Schubart collisional family is darker, with a weighted mean albedo of p(V) = 0.039 +/- 0.013. Using the reflected sunlight in the two shortest WISE bandpasses, we are able to derive a method for taxonomic classification of similar to 10% of the Hildas detected in the NEOWISE survey. For the Hildas with diameter larger than 30 km, there are 67(-15)(+7) % D-type asteroids and 26(-5)(+17) % C-/P-type asteroids (with the majority of these being P-types).
C1 [Grav, T.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Mainzer, A. K.; Bauer, J.; Masiero, J.; Eisenhardt, P. R.; Blauvelt, E.; DeBaun, E.; Elsbury, D.; Gautier, T.; Gomillion, S.; Hand, E.; Wilkins, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bauer, J.; Cutri, R.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
[Spahr, T.] Harvard Smithsonian Ctr Astrophys, Minor Planet Ctr, Cambridge, MA 02138 USA.
[McMillan, R. S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA.
[Walker, R.] Monterey Inst Res Astron, Marina, CA 93933 USA.
[Wright, E.] UCLA Astron, Los Angeles, CA 90095 USA.
[Wilkins, A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Grav, T (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
EM tgrav@pha.jhu.edu
OI Blauvelt, Erin/0000-0002-2944-5818; Masiero, Joseph/0000-0003-2638-720X
FU National Aeronautics and Space Administration; Planetary Science
Division of the National Aeronautics and Space Administration
FX This publication makes use of data products from the Wide-field Infrared
Survey Explorer, which is a joint project of the University of
California, Los Angeles, and the Jet Propulsion Laboratory/California
Institute of Technology, funded by the National Aeronautics and Space
Administration. This publication also makes use of data products from
NEOWISE, which is a project of the Jet Propulsion Laboratory/California
Institute of Technology, funded by the Planetary Science Division of the
National Aeronautics and Space Administration. We gratefully acknowledge
the extraordinary services specific to NEOWISE contributed by the
International Astronomical Union's Minor Planet Center, operated by the
Harvard-Smithsonian Center for Astrophysics, and the Central Bureau for
Astronomical Telegrams, operated by Harvard University. We also thank
the worldwide community of dedicated amateur and professional
astronomers devoted to minor planet follow-up observations. This
research has made use the NASA/IPAC Infrared Science Archive, which is
operated by the Jet Propulsion Laboratory/California Institute of
Technology, under contract with the National Aeronautics and Space
Administration.
NR 52
TC 24
Z9 24
U1 0
U2 1
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 JAN 10
PY 2012
VL 744
IS 2
AR 197
DI 10.1088/0004-637X/744/2/197
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 870JW
UT WOS:000298666400116
ER
PT J
AU Kocevski, DD
Faber, SM
Mozena, M
Koekemoer, AM
Nandra, K
Rangel, C
Laird, ES
Brusa, M
Wuyts, S
Trump, JR
Koo, DC
Somerville, RS
Bell, EF
Lotz, JM
Alexander, DM
Bournaud, F
Conselice, CJ
Dahlen, T
Dekel, A
Donley, JL
Dunlop, JS
Finoguenov, A
Georgakakis, A
Giavalisco, M
Guo, YC
Grogin, NA
Hathi, NP
Juneau, S
Kartaltepe, JS
Lucas, RA
McGrath, EJ
McIntosh, DH
Mobasher, B
Robaina, AR
Rosario, D
Straughn, AN
van der Wel, A
Villforth, C
AF Kocevski, Dale D.
Faber, S. M.
Mozena, Mark
Koekemoer, Anton M.
Nandra, Kirpal
Rangel, Cyprian
Laird, Elise S.
Brusa, Marcella
Wuyts, Stijn
Trump, Jonathan R.
Koo, David C.
Somerville, Rachel S.
Bell, Eric F.
Lotz, Jennifer M.
Alexander, David M.
Bournaud, Frederic
Conselice, Christopher J.
Dahlen, Tomas
Dekel, Avishai
Donley, Jennifer L.
Dunlop, James S.
Finoguenov, Alexis
Georgakakis, Antonis
Giavalisco, Mauro
Guo, Yicheng
Grogin, Norman A.
Hathi, Nimish P.
Juneau, Stephanie
Kartaltepe, Jeyhan S.
Lucas, Ray A.
McGrath, Elizabeth J.
McIntosh, Daniel H.
Mobasher, Bahram
Robaina, Aday R.
Rosario, David
Straughn, Amber N.
van der Wel, Arjen
Villforth, Carolin
TI CANDELS: CONSTRAINING THE AGN-MERGER CONNECTION WITH HOST MORPHOLOGIES
AT z similar to 2
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: evolution; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; DEEP FIELD-SOUTH; QUASAR LUMINOSITY FUNCTION;
SUPERMASSIVE BLACK-HOLES; EXTENDED GROTH STRIP; MS SOURCE CATALOGS;
FAINT X-RAY; GALAXY MERGERS; STAR-FORMATION; HIGH-REDSHIFT
AB Using Hubble Space Telescope/WFC3 imaging taken as part of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey, we examine the role that major galaxy mergers play in triggering active galactic nucleus (AGN) activity at z similar to 2. Our sample consists of 72 moderate-luminosity (L-X similar to 10(42-44) erg s(-1)) AGNs at 1.5 < z < 2.5 that are selected using the 4 Ms Chandra observations in the Chandra Deep Field South, the deepest X-ray observations to date. Employing visual classifications, we have analyzed the rest-frame optical morphologies of the AGN host galaxies and compared them to a mass-matched control sample of 216 non-active galaxies at the same redshift. We find that most of the AGNs reside in disk galaxies (51.4(-5.9)(+5.8)%), while a smaller percentage are found in spheroids (27.8(-4.6)(+5.8)%). Roughly 16.7(-3.5)(+5.3)% of the AGN hosts have highly disturbed morphologies and appear to be involved in a major merger or interaction, while most of the hosts (55.6(-5.9)(+5.6)%) appear relatively relaxed and undisturbed. These fractions are statistically consistent with the fraction of control galaxies that show similar morphological disturbances. These results suggest that the hosts of moderate-luminosity AGNs are no more likely to be involved in an ongoing merger or interaction relative to non-active galaxies of similar mass at z similar to 2. The high disk fraction observed among the AGN hosts also appears to be at odds with predictions that merger-driven accretion should be the dominant AGN fueling mode at z similar to 2, even at moderate X-ray luminosities. Although we cannot rule out that minor mergers are responsible for triggering these systems, the presence of a large population of relatively undisturbed disk-like hosts suggests that the stochastic accretion of gas plays a greater role in fueling AGN activity at z similar to 2 than previously thought.
C1 [Kocevski, Dale D.; Faber, S. M.; Mozena, Mark; Trump, Jonathan R.; Koo, David C.; McGrath, Elizabeth J.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA.
[Koekemoer, Anton M.; Lotz, Jennifer M.; Dahlen, Tomas; Donley, Jennifer L.; Grogin, Norman A.; Lucas, Ray A.; Villforth, Carolin] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Nandra, Kirpal; Brusa, Marcella; Wuyts, Stijn; Finoguenov, Alexis; Rosario, David] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Rangel, Cyprian; Laird, Elise S.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, London SW7 2AZ, England.
[Somerville, Rachel S.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Bell, Eric F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Alexander, David M.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Bournaud, Frederic] CEA, IRFU, SAp, F-91191 Gif Sur Yvette, France.
[Bournaud, Frederic] Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France.
[Conselice, Christopher J.] Univ Nottingham, Ctr Astron & Particle Theory, Nottingham NG7 2RD, England.
[Dekel, Avishai] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel.
[Dunlop, James S.] Univ Maryland Baltimore Cty, Ctr Space Sci Technol, Baltimore, MD 21228 USA.
[Finoguenov, Alexis] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Georgakakis, Antonis] Natl Observ Athens, V Paulou 11532, Greece.
[Georgakakis, Antonis] Natl Observ Athens, I Metaxa 11532, Greece.
[Giavalisco, Mauro; Guo, Yicheng] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Hathi, Nimish P.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Juneau, Stephanie] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Kartaltepe, Jeyhan S.] NOAO Tucson, Tucson, AZ 85719 USA.
[McIntosh, Daniel H.] Univ Missouri, Dept Phys, Kansas City, MO 64110 USA.
[Mobasher, Bahram] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[Robaina, Aday R.] IEEC, ICC UB, Inst Ciencies Cosmos, E-08028 Barcelona, Spain.
[Straughn, Amber N.] NASA, Goddard Space Flight Ctr, Lab Observat Cosmol, Greenbelt, MD 20771 USA.
[van der Wel, Arjen] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
RP Kocevski, DD (reprint author), Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA.
EM kocevski@ucolick.org
RI Conselice, Christopher/B-4348-2013; Bournaud, Frederic/K-1263-2013;
Georgakakis, Antonis/K-4457-2013; Hathi, Nimish/J-7092-2014;
OI Hathi, Nimish/0000-0001-6145-5090; Alexander, David/0000-0002-5896-6313;
Koekemoer, Anton/0000-0002-6610-2048; Bell, Eric/0000-0002-5564-9873
FU NASA through the Space Telescope Science Institute [HST-GO-12060]; NASA
[NAS5-26555]; NSF [AST-0808133]
FX Support for Program number HST-GO-12060 was provided by NASA through a
grant from the Space Telescope Science Institute, which is operated by
the Association of Universities for Research in Astronomy, Incorporated,
under NASA contract NAS5-26555. Furthermore, D. K. is funded in part by
the NSF under grant No. AST-0808133.
NR 72
TC 168
Z9 168
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 JAN 10
PY 2012
VL 744
IS 2
AR 148
DI 10.1088/0004-637X/744/2/148
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 870JW
UT WOS:000298666400068
ER
PT J
AU Koenig, XP
Leisawitz, DT
Benford, DJ
Rebull, LM
Padgett, DL
Assef, RJ
AF Koenig, X. P.
Leisawitz, D. T.
Benford, D. J.
Rebull, L. M.
Padgett, D. L.
Assef, R. J.
TI WIDE-FIELD INFRARED SURVEY EXPLORER OBSERVATIONS OF THE EVOLUTION OF
MASSIVE STAR-FORMING REGIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; H II regions; infrared: stars; stars: formation;
stars: pre-main sequence
ID SPITZER-SPACE-TELESCOPE; YOUNG STELLAR OBJECTS; MAIN-SEQUENCE STARS;
RADIATION-DRIVEN IMPLOSION; MOLECULAR CLOUD COMPLEX; H-II REGIONS; DISK
EVOLUTION; OPEN CLUSTER; MILKY-WAY; INTERSTELLAR CLOUDS
AB We present the results of a mid-infrared survey of 11 outer Galaxy massive star-forming regions and 3 open clusters with data from the Wide-field Infrared Survey Explorer (WISE). Using a newly developed photometric scheme to identify young stellar objects and exclude extragalactic contamination, we have studied the distribution of young stars within each region. These data tend to support the hypothesis that latter generations may be triggered by the interaction of winds and radiation from the first burst of massive star formation with the molecular cloud material leftover from that earlier generation of stars. We dub this process the "fireworks hypothesis" since star formation by this mechanism would proceed rapidly and resemble a burst of fireworks. We have also analyzed small cutout WISE images of the structures around the edges of these massive star-forming regions. We observe large (1-3 pc size) pillar and trunk-like structures of diffuse emission nebulosity tracing excited polycyclic aromatic hydrocarbon molecules and small dust grains at the perimeter of the massive star-forming regions. These structures contain small clusters of emerging Class I and Class II sources, but some are forming only a single to a few new stars.
C1 [Koenig, X. P.; Leisawitz, D. T.; Benford, D. J.; Padgett, D. L.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Rebull, L. M.] CALTECH, Spitzer Sci Ctr SSC, Pasadena, CA 91125 USA.
[Assef, R. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Koenig, XP (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RI Benford, Dominic/D-4760-2012;
OI Benford, Dominic/0000-0002-9884-4206; Koenig,
Xavier/0000-0002-9478-4170; Rebull, Luisa/0000-0001-6381-515X
FU National Aeronautics and Space Administration (NASA); National Science
Foundation
FX The authors thank Britt Griswold and Dan Stern for vital contributions
to this paper. We thank the referee for a helpful report that improved
the paper and its conclusions. 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. This work is based on data obtained from (1) the
Wide-Field Infrared Survey Explorer, which is a joint project of the
University of California, Los Angeles, and the Jet Propulsion Laboratory
(JPL), California Institute of Technology (Caltech), funded by the
National Aeronautics and Space Administration (NASA); (2) the Two Micron
All Sky Survey, a joint project of the University of Massachusetts and
the Infrared Processing and Analysis Center (IPAC)/Caltech, funded by
NASA and the National Science Foundation; (3) the SIMBAD database,
operated at CDS, Strasbourg, France; and (4) the NASA/IPAC Infrared
Science Archive, which is operated by JPL, Caltech, under a contract
with NASA.
NR 108
TC 83
Z9 83
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 JAN 10
PY 2012
VL 744
IS 2
AR 130
DI 10.1088/0004-637X/744/2/130
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 870JW
UT WOS:000298666400050
ER
PT J
AU Leauthaud, A
Tinker, J
Bundy, K
Behroozi, PS
Massey, R
Rhodes, J
George, MR
Kneib, JP
Benson, A
Wechsler, RH
Busha, MT
Capak, P
Cortes, M
Ilbert, O
Koekemoer, AM
Le Fevre, O
Lilly, S
McCracken, HJ
Salvato, M
Schrabback, T
Scoville, N
Smith, T
Taylor, JE
AF Leauthaud, Alexie
Tinker, Jeremy
Bundy, Kevin
Behroozi, Peter S.
Massey, Richard
Rhodes, Jason
George, Matthew R.
Kneib, Jean-Paul
Benson, Andrew
Wechsler, Risa H.
Busha, Michael T.
Capak, Peter
Cortes, Marina
Ilbert, Olivier
Koekemoer, Anton M.
Le Fevre, Oliver
Lilly, Simon
McCracken, Henry J.
Salvato, Mara
Schrabback, Tim
Scoville, Nick
Smith, Tristan
Taylor, James E.
TI NEW CONSTRAINTS ON THE EVOLUTION OF THE STELLAR-TO-DARK MATTER
CONNECTION: A COMBINED ANALYSIS OF GALAXY-GALAXY LENSING, CLUSTERING,
AND STELLAR MASS FUNCTIONS FROM z=0.2 to z=1
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dark matter; galaxies: evolution; galaxies: formation; galaxies:
luminosity function, mass function; galaxies: stellar content;
gravitational lensing: weak
ID DIGITAL SKY SURVEY; HALO OCCUPATION DISTRIBUTION;
HUBBLE-SPACE-TELESCOPE; TULLY-FISHER RELATION; ACTIVE GALACTIC NUCLEI;
LAMBDA-CDM UNIVERSE; STAR-FORMATION; FIELD GALAXIES; DISK GALAXIES;
X-RAY
AB Using data from the COSMOS survey, we perform the first joint analysis of galaxy-galaxy weak lensing, galaxy spatial clustering, and galaxy number densities. Carefully accounting for sample variance and for scatter between stellar and halo mass, we model all three observables simultaneously using a novel and self-consistent theoretical framework. Our results provide strong constraints on the shape and redshift evolution of the stellar-to-halo mass relation (SHMR) from z = 0.2 to z = 1. At low stellar mass, we find that halo mass scales as M-h proportional to M-*(0.46) and that this scaling does not evolve significantly with redshift from z = 0.2 to z = 1. The slope of the SHMR rises sharply at M-* > 5 x 10(10)M(circle dot) and as a consequence, the stellar mass of a central galaxy becomes a poor tracer of its parent halo mass. We show that the dark-to-stellar ratio, Mh/M*, varies from low to high masses, reaching a minimum of Mh/M-* similar to 27 at M-* = 4.5 x 10(10) M-circle dot and M-h = 1.2 x 10(12) M-circle dot. This minimum is important for models of galaxy formation because it marks the mass at which the accumulated stellar growth of the central galaxy has been themost efficient. We describe the SHMR at this minimum in terms of the " pivot stellarmass," M-*(piv) the "pivot halo mass," M-h(piv), and the "pivot ratio," (M-h/M-*)(piv). Thanks to a homogeneous analysis of a single data set spanning a large redshift range, we report the first detection of mass downsizing trends for both M-h(piv) and M-*(piv) The pivot stellar mass decreases from M-*(piv) = 5.75 +/- 0.13x10(10) M-circle dot at z = 0.88 to M-*(piv) = 3.55 +/- 0.17x10(10) M-circle dot at z = 0.37. Intriguingly, however, the corresponding evolution of M-h(piv) leaves the pivot ratio constant with redshift at (M-h/M-*)(piv) similar to 27. We use simple arguments to show how this result raises the possibility that star formation quenching may ultimately depend on M-h/M-* and not simply onMh, as is commonly assumed. We show that simple models with such a dependence naturally lead to downsizing in the sites of star formation. Finally, we discuss the implications of our results in the context of popular quenching models, including disk instabilities and active galactic nucleus feedback.
C1 [Leauthaud, Alexie] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778582, Japan.
[Leauthaud, Alexie; Cortes, Marina] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Leauthaud, Alexie; Smith, Tristan] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Tinker, Jeremy] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA.
[Bundy, Kevin; George, Matthew R.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Behroozi, Peter S.; Wechsler, Risa H.; Busha, Michael T.; Schrabback, Tim] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Behroozi, Peter S.; Wechsler, Risa H.; Busha, Michael T.; Schrabback, Tim] SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Salvato, Mara] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Rhodes, Jason; Benson, Andrew; Scoville, Nick] CALTECH, Pasadena, CA 91125 USA.
[Rhodes, Jason] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kneib, Jean-Paul; Ilbert, Olivier; Le Fevre, Oliver] UNiv Aix Marseille, CNRS, LAM, F-13013 Marseille, France.
[Busha, Michael T.] Univ Zurich, Dept Phys, Inst Theoret Phys, CH-8057 Zurich, Switzerland.
[Capak, Peter] Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Lilly, Simon] ETH, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland.
[McCracken, Henry J.] Inst Astrophys Paris, UMR 7095, F-75014 Paris, France.
[Schrabback, Tim] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands.
[Taylor, James E.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
RP Leauthaud, A (reprint author), Univ Tokyo, Inst Phys & Math Universe, Chiba 2778582, Japan.
EM asleauthaud@lbl.gov
RI Kneib, Jean-Paul/A-7919-2015;
OI Kneib, Jean-Paul/0000-0002-4616-4989; Cortes,
Marina/0000-0003-0485-3767; Koekemoer, Anton/0000-0002-6610-2048
FU LBNL; Berkeley Center for Cosmological Physics; CNRS; CNES; NASA
[HST-AR-12159, NAS5-26555, HST-GO-09822]; U.S. Department of Energy
[DE-AC02-76SF00515]; Space Telescope Science Institute; Netherlands
Organization for Scientific Research (NWO), NSF [AST-0444059-001];
Smithsonian Astrophysics Observatory [GO0-11147A]; World Premier
International Research Center Initiative (WPI Initiative), MEXT, Japan
FX We thank Uros Seljak, Beth Reid, Martin White, Surhud More, Rachel
Mandelbaum, Marcello Cacciato, Phil Hopkins, Charlie Conroy, Ian
McCarthy, and Frank van den Bosch for insightful discussions. We thank
the anonymous referee for a careful reading of the manuscript and for
providing very useful comments. We are grateful to Rachel Mandelbaum,
Benjamin Moster, Michael Blanton, Surhud More, Henk Hoekstra, and Chris
Bildfell for providing data in electronic format. We thank Ian Harnett
for inspiration, for a careful reading of the manuscript, and for
introducing us to "the dynamics of dust."A. L. acknowledges support from
the Chamberlain Fellowship at LBNL and from the Berkeley Center for
Cosmological Physics. J.P.K. acknowledges CNRS and CNES for support.
J.D.R. was supported by JPL, operated under a contract by Caltech for
NASA. This research received partial support from the U.S. Department of
Energy under contract number DE-AC02-76SF00515. R. H. W. and P. S. B.
received additional support from NASA Program HST-AR-12159. A, provided
through a grant from the Space Telescope Science Institute, which is
operated by the Association of Universities for Research in Astronomy,
Incorporated, under NASA contract NAS5-26555. M. T. B. and R. H. W. also
thank their collaborators on the LasDamas project for critical input on
the Consuelo simulation, which was performed on the Orange cluster at
SLAC. T. S. acknowledges support from the Netherlands Organization for
Scientific Research (NWO), NSF through grant AST-0444059-001, and the
Smithsonian Astrophysics Observatory through grant GO0-11147A. The HST
COSMOS Treasury program was supported through NASA grant HST-GO-09822.
We thank Tony Roman, Denise Taylor, and David Soderblom for their
assistance in planning and scheduling of the extensive COSMOS
observations. We gratefully acknowledge the contributions of the entire
COSMOS collaboration consisting of more than 70 scientists. More
information on the COSMOS survey is available at
http://cosmos.astro.caltech.edu/. It is a pleasure to acknowledge the
excellent services provided by the NASA IPAC/IRSA staff (Anastasia
Laity, Anastasia Alexov, Bruce Berriman and John Good) in providing
online archive and server capabilities for the COSMOS data sets.; This
work was supported by World Premier International Research Center
Initiative (WPI Initiative), MEXT, Japan.
NR 155
TC 208
Z9 208
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 JAN 10
PY 2012
VL 744
IS 2
AR 159
DI 10.1088/0004-637X/744/2/159
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 870JW
UT WOS:000298666400079
ER
PT J
AU Loeffler, MJ
Baragiola, RA
AF Loeffler, M. J.
Baragiola, R. A.
TI BLISTERING AND EXPLOSIVE DESORPTION OF IRRADIATED AMMONIA-WATER MIXTURES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; comets: general; ISM: general; methods: laboratory;
planets and satellites: surfaces; radiation mechanisms: general;
techniques: spectroscopic
ID ICY SATELLITES; TRAILING HEMISPHERES; INFRARED-SPECTRUM; CRYSTALLINE
WATER; THERMAL EVOLUTION; ION IRRADIATION; ENCELADUS; SPECTROSCOPY;
ICES; VOLCANISM
AB We present laboratory studies on the thermal evolution of a solid ammonia-water mixture after it has been irradiated at 20, 70, and 120 K. In samples irradiated at <= 70 K, we observed fast outbursts that appear to indicate grain ejection and correlate well with the formation of micron-sized scattering centers. The occurrence of this phenomenon at the lower irradiation temperatures indicates that our results may be most relevant for understanding the release of gas and grains by comets and the surfaces of some of the colder icy satellites. We observe outgassing at temperatures below those where ice sublimates, which suggests that comets containing radiolyzed material may have outbursts farther from the Sun that those that are passive. In addition, the estimated size of the grains ejected from our sample is on the order of the size of E-ring particles, suggesting that our results give a plausible mechanism for how micron-sized grains could be formed from an icy surface. Finally, we propose that the presence of the similar to 4.5 mu m N2O absorption band on an icy surface in outer space will serve to provide indirect evidence for radiation-processed ices that originally contained ammonia or nitrogen, which could be particularly useful since nitrogen is such a weak absorber in the infrared and ammonia is rapidly decomposed by radiolysis.
C1 [Loeffler, M. J.; Baragiola, R. A.] Univ Virginia, Lab Atom & Surface Phys, Charlottesville, VA 22904 USA.
[Loeffler, M. J.] NASA, Goddard Space Flight Ctr, Astrochem Lab, Greenbelt, MD 20771 USA.
RP Loeffler, MJ (reprint author), Univ Virginia, Lab Atom & Surface Phys, Charlottesville, VA 22904 USA.
EM mark.loeffler@nasa.gov; raul@virginia.edu
RI Loeffler, Mark/C-9477-2012
FU NASA
FX This research was supported by the NASA Planetary Geology and Geophysics
and Planetary Atmospheres programs.
NR 39
TC 5
Z9 5
U1 2
U2 12
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2012
VL 744
IS 2
AR 102
DI 10.1088/0004-637X/744/2/102
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 870JW
UT WOS:000298666400022
ER
PT J
AU Luhman, KL
Burgasser, AJ
Labbe, I
Saumon, D
Marley, MS
Bochanski, JJ
Monson, AJ
Persson, SE
AF Luhman, K. L.
Burgasser, A. J.
Labbe, I.
Saumon, D.
Marley, M. S.
Bochanski, J. J.
Monson, A. J.
Persson, S. E.
TI CONFIRMATION OF ONE OF THE COLDEST KNOWN BROWN DWARFS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: visual; brown dwarfs; infrared: planetary systems; planetary
systems; planets and satellites: atmospheres
ID INFRARED SURVEY EXPLORER; SPITZER-SPACE-TELESCOPE; T-DWARFS;
BINARY-SYSTEM; DISCOVERY; WISE; PHOTOMETRY; CFBDSIR; MISSION; 2MASS
AB Using two epochs of 4.5 mu m images from the Infrared Array Camera (IRAC) on board the Spitzer Space Telescope, we recently identified a common proper motion companion to the white dwarf WD 0806-661 that is a candidate for the coldest known brown dwarf. To verify its cool nature, we have obtained images of this object at 3.6 mu m with IRAC, at J with the High Acuity Wide-field K-band Imager (HAWK-I) on the Very Large Telescope, and in a filter covering the red half of J with FourStar on Magellan. WD 0806-661 B is detected by IRAC but not HAWK-I or FourStar. From these data we measure colors of [3.6] - [4.5] = 2.77 +/- 0.16 and J - [4.5] > 7.0 (S/N < 3). Based on these colors and its absolute magnitudes, WD 0806-661 B is the coldest companion directly imaged outside of the solar system and is a contender for the coldest known brown dwarf with the Y dwarf WISEP J1828+2650. It is unclear which of these two objects is colder given the available data. A comparison of its absolute magnitude at 4.5 mu m to the predictions of theoretical spectra and evolutionary models suggests that WD 0806-661 B has T-eff = 300-345 K.
C1 [Luhman, K. L.; Bochanski, J. J.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Luhman, K. L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Burgasser, A. J.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
[Labbe, I.; Monson, A. J.; Persson, S. E.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA.
[Saumon, D.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
[Marley, M. S.] NASA, Space Sci & Astrobiol Div, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Luhman, KL (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
EM kluhman@astro.psu.edu
RI Marley, Mark/I-4704-2013;
OI Marley, Mark/0000-0002-5251-2943
FU National Science Foundation [AST-0544588]; NASA; NASA/IPAC Infrared
Science Archive; Pennsylvania State University; Eberly College of
Science; Pennsylvania Space Grant Consortium; ESO Telescopes at Paranal
Observatory [ID 286.C-5042]
FX We acknowledge support from grant AST-0544588 from the National Science
Foundation (K. L., J.B.) and the NASA Astrophysics Theory Program (M.
M., D. S.). This publication makes use of data products from the
following resources: the Wide-field Infrared Survey Explorer, which is a
joint project of the University of California, Los Angeles, and the Jet
Propulsion Laboratory/California Institute of Technology, funded by the
National Aeronautics and Space Administration; the NASA/IPAC Infrared
Science Archive, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space Administration; the SpeX Prism Spectral Libraries,
maintained by Adam Burgasser at http://www.browndwarfs.org/spexprism;
the M, L, and T dwarf compendium housed at http://DwarfArchives.org and
maintained by Chris Gelino, Davy Kirkpatrick, and Adam Burgasser. The
Center for Exoplanets and Habitable Worlds is supported by the
Pennsylvania State University, the Eberly College of Science, and the
Pennsylvania Space Grant Consortium.; Based on observations made with
the following facilities: the Spitzer Space Telescope, which is operated
by the Jet Propulsion Laboratory, California Institute of Technology
under a contract with NASA; the ESO Telescopes at Paranal Observatory
under program ID 286.C-5042; the 6.5 meter Magellan Telescopes located
at Las Campanas Observatory, Chile.
NR 39
TC 29
Z9 29
U1 0
U2 1
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 JAN 10
PY 2012
VL 744
IS 2
AR 135
DI 10.1088/0004-637X/744/2/135
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 870JW
UT WOS:000298666400055
ER
PT J
AU Nowak, MA
Wilms, J
Pottschmidt, K
Schulz, N
Maitra, D
Miller, J
AF Nowak, Michael A.
Wilms, Joern
Pottschmidt, Katja
Schulz, Norbert
Maitra, Dipankar
Miller, Jon
TI SUZAKU OBSERVATIONS OF 4U 1957+11: POTENTIALLY THE MOST RAPIDLY SPINNING
BLACK HOLE IN (THE HALO OF) THE GALAXY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; radiation mechanisms:
thermal; X-rays: binaries
ID X-RAY BINARY; ACCRETION DISK MODELS; CYGNUS X-1; SOFT STATE; LMC X-3;
ABSORPTION; SPECTRA; LONG; JET
AB We present three Suzaku observations of the black hole candidate 4U 1957+11 (V1408 Aql)-a source that exhibits some of the simplest and cleanest examples of soft, disk-dominated spectra. 4U 1957+11 also presents among the highest peak temperatures found from disk-dominated spectra. Such temperatures may be associated with rapid black hole spin. The 4U 1957+11 spectra also require a very low normalization, which can be explained by a combination of small inner disk radius and a large distance (>10 kpc) which places 4U 1957+11 well into the Galactic halo. We perform joint fits to the Suzaku spectra with both relativistic and Comptonized disk models. Assuming a low-mass black hole and the nearest distance (3 M-circle dot, 10 kpc), the dimensionless spin parameter a* equivalent to Jc/GM(2) greater than or similar to 0.9. Higher masses and farther distances yield a* approximate to 1. Similar conclusions are reached with Comptonization models; they imply a combination of small inner disk radii (or, equivalently, rapid spin) and large distance. Low spin cannot be recovered unless 4U 1957+11 is a low-mass black hole that is at the unusually large distance of greater than or similar to 40 kpc. We speculate whether the suggested maximal spin is related to how the system came to reside in the halo.
C1 [Nowak, Michael A.; Schulz, Norbert] MIT, Kavli Inst Astrophys, Cambridge, MA 02139 USA.
[Wilms, Joern] Univ Erlangen Nurnberg, Dr Karl Remeis Sternwarte & Erlangen Ctr Astropar, D-96049 Bamberg, Germany.
[Pottschmidt, Katja] UMBC, CRESST, Greenbelt, MD 20771 USA.
[Pottschmidt, Katja] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Maitra, Dipankar; Miller, Jon] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
RP Nowak, MA (reprint author), MIT, Kavli Inst Astrophys, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM mnowak@space.mit.edu; joern.wilms@sternwarte.uni-erlangen.de;
katja@milkyway.gsfc.nasa.gov; nss@space.mit.edu; dmaitra@umich.edu;
jonmm@umich.edu
RI Wilms, Joern/C-8116-2013; XRAY, SUZAKU/A-1808-2009
OI Wilms, Joern/0000-0003-2065-5410;
FU NASA [NNX10AR94G, SV3-73016]; European Commission [ITN 215212];
Bundesministerium fur Wirtschaft und Technologie through Deutsches
Zentrum fur Luft-und Raumfahrt [50OR0701, 50OR1005]
FX Michael Nowak was supported by NASA Grants NNX10AR94G and SV3-73016.
Jorn Wilms was partly supported by the European Commission under
contract ITN 215212 "Black Hole Universe" and by the Bundesministerium
fur Wirtschaft und Technologie through Deutsches Zentrum fur Luft-und
Raumfahrt grants 50OR0701 and 50OR1005.
NR 33
TC 15
Z9 15
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JAN 10
PY 2012
VL 744
IS 2
AR 107
DI 10.1088/0004-637X/744/2/107
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 870JW
UT WOS:000298666400027
ER
PT J
AU Ono, Y
Ouchi, M
Mobasher, B
Dickinson, M
Penner, K
Shimasaku, K
Weiner, BJ
Kartaltepe, JS
Nakajima, K
Nayyeri, H
Stern, D
Kashikawa, N
Spinrad, H
AF Ono, Yoshiaki
Ouchi, Masami
Mobasher, Bahram
Dickinson, Mark
Penner, Kyle
Shimasaku, Kazuhiro
Weiner, Benjamin J.
Kartaltepe, Jeyhan S.
Nakajima, Kimihiko
Nayyeri, Hooshang
Stern, Daniel
Kashikawa, Nobunari
Spinrad, Hyron
TI SPECTROSCOPIC CONFIRMATION OF THREE z-DROPOUT GALAXIES AT z=6.844-7.213:
DEMOGRAPHICS OF Ly alpha EMISSION IN z similar to 7 GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; galaxies: evolution; galaxies: formation;
galaxies: high-redshift
ID LYMAN-BREAK GALAXIES; STAR-FORMING GALAXIES; ULTRA-DEEP-FIELD;
HIGH-REDSHIFT GALAXIES; REST-FRAME ULTRAVIOLET; HUBBLE-SPACE-TELESCOPE;
UV LUMINOSITY FUNCTION; STELLAR MASS DENSITY; GOODS-S FIELD;
REIONIZATION EPOCH
AB We present the results of our ultra-deep Keck/DEIMOS spectroscopy of z-dropout galaxies in the Subaru Deep Field and Great Observatories Origins Deep Survey's northern field. For 3 out of 11 objects, we detect an emission line at similar to 1 mu m with a signal-to-noise ratio of similar to 10. The lines show asymmetric profiles with high weighted skewness values, consistent with being Ly alpha, yielding redshifts of z = 7.213, 6.965, and 6.844. Specifically, we confirm the z = 7.213 object in two independent DEIMOS runs with different spectroscopic configurations. The z = 6.965 object is a known Ly alpha emitter, IOK-1, for which our improved spectrum at a higher resolution yields a robust skewness measurement. The three z-dropouts have Ly alpha fluxes of 3x10(-17) erg s(-1) cm(-2) and rest-frame equivalent widths EW0Ly alpha = 33-43 angstrom. Based on the largest spectroscopic sample of 43 z-dropouts, which is the combination of our and previous data, we find that the fraction of Ly alpha-emitting galaxies (EW0Ly alpha > 25 angstrom) is low at z similar to 7; 17% +/- 10% and 24% +/- 12% for bright (M-UV similar or equal to -21) and faint (M-UV similar or equal to -19.5) galaxies, respectively. The fractions of Ly alpha-emitting galaxies drop from z similar to 6 to 7 and the amplitude of the drop is larger for faint galaxies than for bright galaxies. These two pieces of evidence would indicate that the neutral hydrogen fraction of the intergalactic medium increases from z similar to 6 to 7 and that the reionization proceeds from high-to low-density environments, as suggested by an inside-out reionization model.
C1 [Ono, Yoshiaki; Shimasaku, Kazuhiro; Nakajima, Kimihiko] Univ Tokyo, Grad Sch Sci, Dept Astron, Tokyo 1130033, Japan.
[Ouchi, Masami] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan.
[Ouchi, Masami] Univ Tokyo, TODIAS, Inst Phys & Math Univ IPMU, Chiba 2778583, Japan.
[Mobasher, Bahram; Nayyeri, Hooshang] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA.
[Dickinson, Mark; Kartaltepe, Jeyhan S.] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Penner, Kyle] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
[Shimasaku, Kazuhiro] Univ Tokyo, Grad Sch Sci, Res Ctr Early Univ, Tokyo 1130033, Japan.
[Weiner, Benjamin J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Kashikawa, Nobunari] Natl Astron Observ Japan, Div Opt & Infrared Astron, Tokyo 1818588, Japan.
[Spinrad, Hyron] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Ono, Y (reprint author), Univ Tokyo, Grad Sch Sci, Dept Astron, Tokyo 1130033, Japan.
EM ono@astron.s.u-tokyo.ac.jp
RI Ouchi, Masami/A-4490-2011
FU Japan Society for the Promotion of Science (JSPS); NASA; National
Science Foundation
FX We thank the anonymous referee for valuable comments and suggestions
which improved the manuscript. The authors 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. We thank Michael Cooper and Yousuke Utsumi for giving us
helpful advices to reduce DEIMOS spectra. We are also thankful to
Richard Ellis for giving us helpful comments on an early draft of this
paper, and to Mark Dijkstra for providing us with the machine-readable
table of their simulation results. Y.O. acknowledges support from the
Japan Society for the Promotion of Science (JSPS) through the JSPS
Research Fellowship for Young Scientists. The work of D.S. was carried
out at the Jet Propulsion Laboratory, California Institute of
Technology, under a contract with NASA. H. S. acknowledges the support
of the National Science Foundation during the earlier phases of his
spectroscopic program at the Keck Observatory.
NR 111
TC 175
Z9 175
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 JAN 10
PY 2012
VL 744
IS 2
AR 83
DI 10.1088/0004-637X/744/2/83
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 870JW
UT WOS:000298666400003
ER
PT J
AU Pletsch, HJ
Guillemot, L
Allen, B
Kramer, M
Aulbert, C
Fehrmann, H
Ray, PS
Barr, ED
Belfiore, A
Camilo, F
Caraveo, PA
Celik, O
Champion, DJ
Dormody, M
Eatough, RP
Ferrara, EC
Freire, PCC
Hessels, JWT
Keith, M
Kerr, M
de Luca, A
Lyne, AG
Marelli, M
McLaughlin, MA
Parent, D
Ransom, SM
Razzano, M
Reich, W
Parkinson, PMS
Stappers, BW
Wolff, MT
AF Pletsch, H. J.
Guillemot, L.
Allen, B.
Kramer, M.
Aulbert, C.
Fehrmann, H.
Ray, P. S.
Barr, E. D.
Belfiore, A.
Camilo, F.
Caraveo, P. A.
Celik, Oe.
Champion, D. J.
Dormody, M.
Eatough, R. P.
Ferrara, E. C.
Freire, P. C. C.
Hessels, J. W. T.
Keith, M.
Kerr, M.
de Luca, A.
Lyne, A. G.
Marelli, M.
McLaughlin, M. A.
Parent, D.
Ransom, S. M.
Razzano, M.
Reich, W.
Parkinson, P. M. Saz
Stappers, B. W.
Wolff, M. T.
TI DISCOVERY OF NINE GAMMA-RAY PULSARS IN FERMI LARGE AREA TELESCOPE DATA
USING A NEW BLIND SEARCH METHOD
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma rays: stars; pulsars: general; pulsars: individual
ID TIME-DIFFERENCING TECHNIQUE; RADIO-CONTINUUM SURVEY; MILLISECOND
PULSARS; GRAVITATIONAL-WAVES; FREQUENCY SEARCHES; CATALOG; LAT;
SENSITIVITY; ATLAS; SKY
AB We report the discovery of nine previously unknown gamma-ray pulsars in a blind search of data from the Fermi Large Area Telescope (LAT). The pulsars were found with a novel hierarchical search method originally developed for detecting continuous gravitational waves from rapidly rotating neutron stars. Designed to find isolated pulsars spinning at up to kHz frequencies, the new method is computationally efficient and incorporates several advances, including a metric-based gridding of the search parameter space (frequency, frequency derivative, and sky location) and the use of photon probability weights. The nine pulsars have spin frequencies between 3 and 12 Hz, and characteristic ages ranging from 17 kyr to 3 Myr. Two of them, PSRs J1803-2149 and J2111+4606, are young and energetic Galactic-plane pulsars (spin-down power above 6 x 10(35) erg s(-1) and ages below 100 kyr). The seven remaining pulsars, PSRs J0106+4855, J0622+3749, J1620-4927, J1746-3239, J2028+3332, J2030+4415, and J2139+4716, are older and less energetic; two of them are located at higher Galactic latitudes (|b| > 10 degrees). PSR J0106+4855 has the largest characteristic age (3 Myr) and the smallest surface magnetic field (2 x 10(11) G) of all LAT blind-search pulsars. PSR J2139+4716 has the lowest spin-down power (3 x 10(33) erg s(-1)) among all non-recycled gamma-ray pulsars ever found. Despite extensivemulti-frequency observations, only PSR J0106+4855 has detectable pulsations in the radio band. The other eight pulsars belong to the increasing population of radio-quiet gamma-ray pulsars.
C1 [Pletsch, H. J.; Allen, B.; Aulbert, C.; Fehrmann, H.] Albert Einstein Inst, Max Planck Inst Gravitat Phys, D-30167 Hannover, Germany.
[Allen, B.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53211 USA.
[Pletsch, H. J.; Allen, B.; Aulbert, C.; Fehrmann, H.] Leibniz Univ Hannover, Inst Gravitat Phys, D-30167 Hannover, Germany.
[Guillemot, L.; Kramer, M.; Barr, E. D.; Champion, D. J.; Eatough, R. P.; Freire, P. C. C.; Reich, W.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Kramer, M.; Lyne, A. G.; Stappers, B. W.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Ray, P. S.; Wolff, M. T.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Belfiore, A.; Dormody, M.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Belfiore, A.; Dormody, M.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Belfiore, A.] Univ Pavia, Dipartimento Fis Nucl & Teor, I-27100 Pavia, Italy.
[Belfiore, A.; Caraveo, P. A.; de Luca, A.; Marelli, M.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Camilo, F.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Celik, Oe.; Ferrara, E. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Celik, Oe.] Ctr Res & Explorat Space Sci & Technol CRESST, Greenbelt, MD 20771 USA.
[Celik, Oe.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA.
[Celik, Oe.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Hessels, J. W. T.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Hessels, J. W. T.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands.
[Keith, M.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Kerr, M.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Kerr, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[de Luca, A.] Ist Univ Studi Super IUSS, I-27100 Pavia, Italy.
[McLaughlin, M. A.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA.
[Parent, D.] George Mason Univ, Ctr Earth Observing & Space Res, Coll Sci, Fairfax, VA 22030 USA.
[Ransom, S. M.] Natl Radio Astron Observ NRAO, Charlottesville, VA 22903 USA.
[Razzano, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
RP Pletsch, HJ (reprint author), Albert Einstein Inst, Max Planck Inst Gravitat Phys, D-30167 Hannover, Germany.
EM holger.pletsch@aei.mpg.de; guillemo@mpifr-bonn.mpg.de
RI Allen, Bruce/K-2327-2012; Saz Parkinson, Pablo Miguel/I-7980-2013;
OI Allen, Bruce/0000-0003-4285-6256; Champion, David/0000-0003-1361-7723;
Caraveo, Patrizia/0000-0003-2478-8018; De Luca,
Andrea/0000-0001-6739-687X; Ransom, Scott/0000-0001-5799-9714; Ray,
Paul/0000-0002-5297-5278; Marelli, Martino/0000-0002-8017-0338
FU Max Planck Gesellschaft; U.S. National Science Foundation [0555655,
0970074, 1104902]; National Science Foundation
FX This work was partly supported by the Max Planck Gesellschaft and by
U.S. National Science Foundation Grants 0555655, 0970074, and 1104902.;
The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc.
NR 67
TC 56
Z9 57
U1 0
U2 1
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 JAN 10
PY 2012
VL 744
IS 2
AR 105
DI 10.1088/0004-637X/744/2/105
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 870JW
UT WOS:000298666400025
ER
PT J
AU Ragozzine, B
Clowe, D
Markevitch, M
Gonzalez, AH
Bradac, M
AF Ragozzine, B.
Clowe, D.
Markevitch, M.
Gonzalez, A. H.
Bradac, M.
TI WEAK-LENSING RESULTS FOR THE MERGING CLUSTER A1758
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dark matter; galaxies: clusters: general; galaxies: clusters: individual
(A1758); gravitational lensing: weak
ID DARK-MATTER; PHOTOMETRIC REDSHIFTS; GALAXY FORMATION; BULLET CLUSTER;
CROSS-SECTION; MASS; GRAVITY; BARYONS; CHANDRA; COSMOS
AB Here we present the weak-lensing results for A1758, which is known to consist of four subclusters undergoing two separate mergers, A1758N and A1758S. Weak-lensing results for A1758N agree with previous weak-lensing results for clusters 1E0657-558 (Bullet cluster) and MACS J0025.4-1222, whose X-ray gas components were found to be largely separated from their clusters' gravitational potentials. A1758N has a geometry that is different from previously published mergers in that one of its X-ray peaks overlays the corresponding gravitational potential and the other X-ray peak is well separated from its cluster's gravitational potential. The weak-lensing mass peaks of the two northern clusters are separated at the 2.5 sigma level. We estimate the combined mass of the clusters in A1758N to be (2.2 +/- 0.5) x 10(15) M(circle dot) and r(200) = 2300(-130)(+100) kpc. We also detect seven strong-lensing candidates, two of which may provide information that would improve the mass measurements of A1758N.
C1 [Ragozzine, B.; Clowe, D.] Ohio Univ, Dept Phys & Astron, Inst Astrophys, Athens, OH 45701 USA.
[Markevitch, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Bradac, M.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
RP Ragozzine, B (reprint author), Ohio Univ, Dept Phys & Astron, Inst Astrophys, Athens, OH 45701 USA.
EM ragoz@phy.ohiou.edu
FU NASA through Space Telescope Science Institute [HST-GO-11194.01-A]; NASA
[NAS 5-26555, 11194]; Alfred P. Sloan Foundation
FX Support for program HST-GO-11194.01-A was provided by NASA through a
grant from the Space Telescope Science Institute, which is operated by
the Association of Universities for Research in Astronomy, Inc., under
NASA contract NAS 5-26555. D.C. also acknowledges support from the
Alfred P. Sloan Foundation.; Based on observations made with the
NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science
Institute, which is operated by the Association of Universities for
Research in Astronomy, Inc., under NASA contract NAS 5-26555, under
program 11194. Also based on data collected at the Subaru Telescope and
partly obtained from SMOKA, which is operated by the National
Astronomical Observatory of Japan.
NR 42
TC 21
Z9 21
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 JAN 10
PY 2012
VL 744
IS 2
AR 94
DI 10.1088/0004-637X/744/2/94
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 870JW
UT WOS:000298666400014
ER
PT J
AU Zhao, M
Monnier, JD
Swain, MR
Barman, T
Hinkley, S
AF Zhao, Ming
Monnier, John D.
Swain, Mark R.
Barman, Travis
Hinkley, Sasha
TI GROUND-BASED DETECTIONS OF THERMAL EMISSION FROM CoRoT-1b AND WASP-12b
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared: planetary systems; planetary systems; stars: individual
(CoRoT-1, WASP-12)
ID SECONDARY ECLIPSE; TRANSITING EXOPLANETS; EXTRASOLAR PLANET; LIGHT
CURVES; HOT; INVERSION; KS
AB We report a new detection of the H-band thermal emission of CoRoT-1b and two confirmation detections of the Ks-band thermal emission of WASP-12b at secondary eclipses. The H-band measurement of CoRoT-1b shows an eclipse depth of 0.145% +/- 0.049% with a 3 sigma percentile between 0.033% and 0.235%. This depth is consistent with the previous conclusions that the planet has an isothermal region with inefficient heat transport from day side to night side, and has a dayside thermal inversion layer at high altitude. The two Ks-band detections of WASP-12b show a joint eclipse depth of 0.299% +/- 0.065%. This result agrees with the measurement of Croll & collaborators, providing independent confirmation of their measurement. The repeatability of the WASP-12b measurements also validates our data analysis method. Our measurements, in addition to a number of previous results made with other telescopes, demonstrate that ground-based observations are becoming widely available for characterization of atmospheres of hot Jupiters.
C1 [Zhao, Ming; Swain, Mark R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Monnier, John D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48104 USA.
[Barman, Travis] Lowell Observ, Flagstaff, AZ 86001 USA.
[Hinkley, Sasha] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
RP Zhao, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM ming.zhao@psu.edu
FU National Aeronautics and Space Administration; NASA through the NASA
Advanced Supercomputing Division; OSU; MDM consortium; NSF [AST-9605012]
FX We thank the anonymous referee for valuable comments and suggestions for
the paper. We thank John Tolbin, Zhaohuan Zhu, and the Palomar
supporting staff for their help with the observations. Part of this
research was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with the National Aeronautics
and Space Administration. M.Z. is supported by the NASA Postdoctoral
Program at JPL. T.B. acknowledges support from NASA Origins grants to
Lowell Observatory and support from the NASA High-End Computing Program
through the NASA Advanced Supercomputing Division. S.H. is supported by
NASA's Sagan Fellowship at California Institute of Technology. TIFKAM
was funded by OSU and the MDM consortium, and NSF grant AST-9605012. The
Palomar Hale Telescope is operated by Caltech, JPL, and the Cornell
University.
NR 23
TC 27
Z9 27
U1 1
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 JAN 10
PY 2012
VL 744
IS 2
AR 122
DI 10.1088/0004-637X/744/2/122
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 870JW
UT WOS:000298666400042
ER
PT J
AU Zheng, M
Chen, XM
Bae, IT
Ke, CH
Park, C
Smith, MW
Jordan, K
AF Zheng, Meng
Chen, Xiaoming
Bae, In-Tae
Ke, Changhong
Park, Cheol
Smith, Michael W.
Jordan, Kevin
TI Radial Mechanical Properties of Single-Walled Boron Nitride Nanotubes
SO SMALL
LA English
DT Article
DE atomic force microscopy; boron nitride; elastic modulus; mechanical
properties; nanotubes
ID CARBON NANOTUBES; ELASTIC PROPERTIES; FORCE MICROSCOPY; DEFORMATION;
COMPOSITES; NANOWIRES
AB The radial mechanical properties of single-walled boron nitride nanotubes (SW-BNNTs) are investigated by atomic force microscopy. Nanomechanical measurements reveal the radial deformation of individual SW-BNNTs in both elastic and plastic regimes. The measured effective radial elastic moduli of SW-BNNTs are found to follow a decreasing trend with an increase in tube diameter, ranging from 40.78 to 1.85 GPa for tube diameters of 0.58 to 2.38 nm. The results show that SW-BNNTs have relatively lower effective radial elastic moduli than single-walled carbon nanotubes (SWCNTs). The axially strong, but radially supple characteristics suggest that SW-BNNTs may be superior to SWCNTs as reinforcing additives for nanocomposite applications.
C1 [Zheng, Meng; Chen, Xiaoming; Ke, Changhong] SUNY Binghamton, Dept Mech Engn, Binghamton, NY 13902 USA.
[Bae, In-Tae] SUNY Binghamton, Small Scale Syst Integrat & Packaging Ctr, Binghamton, NY 13902 USA.
[Park, Cheol] Natl Inst Aerosp, Hampton, VA 23666 USA.
[Park, Cheol] Univ Virginia, Dept Mech & Aerosp Engn, Charlottesville, VA 22904 USA.
[Smith, Michael W.] NASA Langley Res Ctr, Hampton, VA 23681 USA.
[Jordan, Kevin] Thomas Jefferson Natl Accelerator Facil, Newport News, VA 23606 USA.
RP Ke, CH (reprint author), SUNY Binghamton, Dept Mech Engn, Binghamton, NY 13902 USA.
EM cke@binghamton.edu
RI Zheng, Meng/D-3985-2011; Ke, Changhong/C-4064-2008; CHEN,
XIAOMING/A-1377-2016
OI Zheng, Meng/0000-0002-6769-3054;
FU US Air Force Office of Scientific Research [FA9550-11-1-0042,
FA9550-10-1-0451]; American Chemistry Society
FX This work was funded by the US Air Force Office of Scientific Research
Low Density Materials Program under Grant Nos. FA9550-11-1-0042 and
FA9550-10-1-0451. This work was also partially supported by the American
Chemistry Society-Petroleum Research Fund. The HRTEM imaging work was
performed using the facilities in the Analytical and Diagnostics
Laboratory at Binghamton University's Small Scale Systems Integration
and Packaging Center (S3IP).
NR 43
TC 22
Z9 22
U1 0
U2 19
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1613-6810
J9 SMALL
JI Small
PD JAN 9
PY 2012
VL 8
IS 1
BP 116
EP 121
DI 10.1002/smll.201100946
PG 6
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 872DP
UT WOS:000298788800016
PM 22081558
ER
PT J
AU Galley, CR
AF Galley, Chad R.
TI A nonlinear scalar model of extreme mass ratio inspirals in effective
field theory: II. Scalar perturbations and a master source
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article
AB The motion of a small compact object (SCO) in a background spacetime is investigated further in the context of a class of model nonlinear scalar field theories that have a perturbative structure analogous to the general relativistic description of extreme mass ratio inspirals. We derive regular expressions for the scalar perturbations generated by the motion of the compact object that are valid through third order in e the size of the SCO to the background curvature length scale. Our results for the field perturbations are compared to those calculated through second order in e by Rosenthal (2005 Class. Quantum Grav. 22 S859) and found to agree. However, our procedure for regularizing the scalar perturbations is considerably simpler. Following the Detweiler-Whiting scheme, we use our results for the regular expressions for the field and derive the regular self-force corrections through third order. We find agreement with our previous derivation based on a variational principle of an effective action for the worldline associated with the SCO thereby demonstrating the internal consistency of our formalism. This also explicitly demonstrates that the Detweiler-Whiting decomposition of Green's functions is a valid and practical method of self-force computation at higher orders in perturbation theory and more generally, at all orders in perturbation theory, as we show in an appendix. Finally, we identify a central quantity, which we call a master source, from which all other physically relevant quantities are derivable. Specifically, knowing the master source through some order in e allows one to construct the waveform measured by an observer, the regular part of the field and its derivative on the worldline, the regular part of the self-force and various orbital quantities such as shifts of the innermost stable circular orbit, etc when restricting to conservative dynamics. The existence of a master source together with the regularization methods implemented in this series should be indispensable for derivations of higher order gravitational self-force corrections in the future.
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 chad.r.galley@jpl.nasa.gov
FU NASA
FX We thank Tanja Hinderer for providing valuable feedback and comments on
a previous draft. This work 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. Copyright 2011. All rights reserved.
NR 14
TC 8
Z9 8
U1 0
U2 2
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 JAN 7
PY 2012
VL 29
IS 1
AR 015011
DI 10.1088/0264-9381/29/1/015011
PG 25
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA 866SV
UT WOS:000298404200011
ER
PT J
AU Galley, CR
AF Galley, Chad R.
TI A nonlinear scalar model of extreme mass ratio inspirals in effective
field theory: I. Self-force through third order
SO CLASSICAL AND QUANTUM GRAVITY
LA English
DT Article
ID GRAVITATIONAL-RADIATION REACTION; GENERAL-RELATIVITY; WHITE-DWARFS;
BLACK-HOLES; PARTICLE; MOTION; WAVE
AB The motion of a small compact object in a background spacetime is investigated in the context of a model nonlinear scalar field theory. This model is constructed to have a perturbative structure analogous to the general relativistic description of extreme mass ratio inspirals (EMRIs). We apply the effective field theory approach to this model and calculate the finite part of the self-force on the small compact object through third order in the ratio of the size of the compact object to the curvature scale of the background (e. g. black hole) spacetime. We use well-known renormalization methods and demonstrate the consistency of the formalism in rendering the self-force finite at higher orders within a point particle prescription for the small compact object. This nonlinear scalar model should be useful for studying various aspects of higher-order self-force effects in EMRIs but within a comparatively simpler context than the full gravitational case. These aspects include developing practical schemes for higher-order self-force numerical computations, quantifying the effects of transient resonances on EMRI waveforms and accurately modeling the small compact object's motion for precise determinations of the parameters of detected EMRI sources.
C1 [Galley, Chad R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Galley, Chad R.] Univ Maryland, Dept Phys, Ctr Fundamental Phys, College Pk, MD 20742 USA.
[Galley, Chad R.] Univ Maryland, Ctr Sci Computat & Math Modeling, College Pk, MD 20742 USA.
RP Galley, CR (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM chad.r.galley@jpl.nasa.gov
FU NASA; National Science Foundation [PHY0801213, PHY0908457]
FX We thank Tanja Hinderer, Michele Vallisneri, Ian Vega and Steven
Detweiler for very helpful comments and discussions. This work 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 National
Science Foundation grants PHY0801213 and PHY0908457.
NR 76
TC 9
Z9 9
U1 0
U2 1
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 JAN 7
PY 2012
VL 29
IS 1
AR 015010
DI 10.1088/0264-9381/29/1/015010
PG 37
WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles
& Fields
SC Astronomy & Astrophysics; Physics
GA 866SV
UT WOS:000298404200010
ER
PT J
AU Dong, CM
Lin, XY
Liu, Y
Nencioli, F
Chao, Y
Guan, YP
Chen, D
Dickey, T
McWilliams, JC
AF Dong, Changming
Lin, Xiayan
Liu, Yu
Nencioli, Francesco
Chao, Yi
Guan, Yuping
Chen, Dake
Dickey, Tommy
McWilliams, James C.
TI Three-dimensional oceanic eddy analysis in the Southern California Bight
from a numerical product
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID SANTA-BARBARA CHANNEL; HIGH-FREQUENCY RADAR; DATA ASSIMILATION ANALYSIS;
SURFACE CIRCULATION; CURRENT SYSTEM; ISLAND WAKES; MODEL; EDDIES;
VORTICES; PATTERNS
AB With eight islands, complex coastlines and bottom topography, strong wind curls, and frequent upwelling fronts, the Southern California Bight (SCB) is an area with strong eddy activity. By applying an automated eddy detection scheme to a 12 year high-resolution numerical product of the oceanic circulation in the SCB, a three-dimensional eddy data set is developed. It includes information for each eddy's location, polarity, intensity, size, boundary, and moving path at nine vertical levels. Through a series of statistical analyses applied to the eddy data set, three-dimensional statistical characteristics of mesoscale and submeoscale eddy variations in the SCB are elucidated; these shed light on how eddies are generated, evolve, and terminate. A significant percentage of eddies is found to be generated around islands and headlands along the coastline, which indicates that islands in the SCB play a vital role in eddy generation. Three types of eddies, based on shape, are identified from the numerical product: bowl, lens, and cone. A dynamic analysis shows that some submesoscale eddies with finite local Rossby numbers tend to be ageostrophic balanced while mesoscale eddies are in geostrophic balance. The present research results are useful for the interpretation of data sets obtained during the interdisciplinary Santa Barbara Channel Radiance in a Dynamic Ocean (RaDyo) field experiment conducted on September 3-25, 2008.
C1 [Dong, Changming; McWilliams, James C.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
[Lin, Xiayan; Liu, Yu; Guan, Yuping] Chinese Acad Sci, State Key Lab Trop Oceanog, S China Sea Inst Oceanol, Guangzhou 510301, Guangdong, Peoples R China.
[Lin, Xiayan; Liu, Yu] Chinese Acad Sci, Grad Univ, Beijing, Peoples R China.
[Nencioli, Francesco] Univ Aix Marseille 2, Lab Oceanog Phys & Biogeochim, UMR CNRS IRD 6535, Ctr Oceanol Marseille, F-13288 Marseille 9, France.
[Chao, Yi] CALTECH, NASA Jet Prop Lab, Pasadena, CA 91109 USA.
[Chao, Yi] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Los Angeles, CA 90095 USA.
[Chen, Dake] SIO SOA, State Key Lab Satellite Ocean Environm Dynam, Hangzhou 310012, Zhejiang, Peoples R China.
[Dickey, Tommy] Univ Calif Santa Barbara, Dept Geog, Santa Barbara, CA 93106 USA.
RP Dong, CM (reprint author), Univ Calif Los Angeles, Inst Geophys & Planetary Phys, 405 Hilgard Ave, Los Angeles, CA 90095 USA.
EM cdong@atmos.ucla.edu
RI Guan, Yuping /A-1119-2015; Chen, Dake/E-7082-2011
OI Guan, Yuping /0000-0003-2744-136X;
FU NASA [NNX08AI84G]; ONR [N00014-10-1-0564]; State Key Laboratory of
Satellite Ocean Environment Dynamics, China; Chinese Academy of Sciences
[KZCX1-YW-12-4]; National Basic Research Program of China
[2007CB411801]; Ministry of Science and Technology [2008GR1335,
2007CB816005]; National Science Foundation of China [40730843]; ONR
RaDyO [N00014-07-1-0732, N000140811178]; NASA through the NASA Advanced
Supercomputing (NAS) Division at Ames Research Center; NOAA Integrated
Ocean Observing System (IOOS) through the Southern California Coastal
Ocean Observing System (SCCOOS)
FX C.D. appreciates the support from his NASA grant NNX08AI84G and ONR
grant N00014-10-1-0564. C. D. is also supported by a visiting scholar
grant from State Key Laboratory of Satellite Ocean Environment Dynamics,
China. X. L., Y.L., and Y.P.G. are grateful for support from the
Knowledge Innovation Program of the Chinese Academy of Sciences (grant
KZCX1-YW-12-4) and National Basic Research Program of China
(2007CB411801). D. C. is supported by research grants from Ministry of
Science and Technology (2008GR1335,2007CB816005) and National Science
Foundation of China (40730843). T. D. acknowledges support from ONR
RaDyO contract N00014-07-1-0732 and grant N000140811178 for his ONR
Secretary of the Navy/Chief of Naval Operations Chair in Oceanographic
Sciences for Francesco Nencioli, Songnian Jiang, Derek Manov, and
himself. Y. P. G. thanks Joint Institute for Regional Earth System of
UCLA for the host of Y. P. G.' s visit at UCLA. All authors thank
Chunyan Li for his comments, which help improve the manuscript.
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. Y. C. acknowledges support from the
NOAA Integrated Ocean Observing System (IOOS) program through the
Southern California Coastal Ocean Observing System (SCCOOS). This study
was carried out in part by the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with NASA. We thank two
anonymous reviewers for their comments.
NR 37
TC 23
Z9 28
U1 0
U2 26
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 JAN 7
PY 2012
VL 117
AR C00H14
DI 10.1029/2011JC007354
PG 17
WC Oceanography
SC Oceanography
GA 874CG
UT WOS:000298932000002
ER
PT J
AU Gladstone, GR
Retherford, KD
Egan, AF
Kaufmann, DE
Miles, PF
Parker, JW
Horvath, D
Rojas, PM
Versteeg, MH
Davis, MW
Greathouse, TK
Slater, DC
Mukherjee, J
Steffl, AJ
Feldman, PD
Hurley, DM
Pryor, WR
Hendrix, AR
Mazarico, E
Stern, SA
AF Gladstone, G. Randall
Retherford, Kurt D.
Egan, Anthony F.
Kaufmann, David E.
Miles, Paul F.
Parker, Joel W.
Horvath, David
Rojas, Paul M.
Versteeg, Maarten H.
Davis, Michael W.
Greathouse, Thomas K.
Slater, David C.
Mukherjee, Joey
Steffl, Andrew J.
Feldman, Paul D.
Hurley, Dana M.
Pryor, Wayne R.
Hendrix, Amanda R.
Mazarico, Erwan
Stern, S. Alan
TI Far-ultraviolet reflectance properties of the Moon's permanently
shadowed regions
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID LUNAR RADIOMETER OBSERVATIONS; LYMAN-ALPHA; BIDIRECTIONAL REFLECTANCE;
OPTICAL-PROPERTIES; LCROSS IMPACT; WATER ICE; MISSION; ALBEDO;
PHOTODESORPTION; INSTRUMENT
AB Although of great interest for science and resource utilization, the Moon's permanently shadowed regions (PSRs) near each pole present difficult targets for remote sensing. The Lyman Alpha Mapping Project (LAMP) instrument on the Lunar Reconnaissance Orbiter (LRO) mission is able to map PSRs at far-ultraviolet (FUV) wavelengths using two faint sources of illumination from the night sky: the all-sky Ly alpha glow produced as interplanetary medium (IPM) H atoms scatter the Sun's Ly alpha emissions, and the much fainter source from UV-bright stars. The reflected light from these two sources produces only a few hundred events per second in the photon-counting LAMP instrument, so building maps with useful signal-to-noise (SNR) ratios requires the careful accumulation of the observations from thousands of individual LRO orbits. In this paper we present the first FUV albedo maps obtained by LAMP of the Moon's southern and northern polar regions. The results show that (1) most PSR regions are darker at all FUV wavelengths, consistent with their surface soils having much larger porosities than non-PSR regions (e.g., similar to 70% compared to similar to 40% or so), and (2) most PSRs are somewhat "redder" (i.e., more reflective at the longer FUV wavelengths) than non-PSR regions, consistent with the presence of similar to 1-2% water frost at the surface.
C1 [Gladstone, G. Randall; Retherford, Kurt D.; Miles, Paul F.; Horvath, David; Rojas, Paul M.; Versteeg, Maarten H.; Davis, Michael W.; Greathouse, Thomas K.; Slater, David C.; Mukherjee, Joey] SW Res Inst, San Antonio, TX 78238 USA.
[Egan, Anthony F.; Kaufmann, David E.; Parker, Joel W.; Steffl, Andrew J.; Stern, S. Alan] SW Res Inst, Boulder, CO 80302 USA.
[Feldman, Paul D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Hurley, Dana M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Pryor, Wayne R.] Cent Arizona Coll, Div Sci, Coolidge, AZ 85128 USA.
[Hendrix, Amanda R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Mazarico, Erwan] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
RP Gladstone, GR (reprint author), SW Res Inst, 6220 Culebra Rd, San Antonio, TX 78238 USA.
EM rgladstone@swri.org
RI Hurley, Dana/F-4488-2015; Mazarico, Erwan/N-6034-2014;
OI Hurley, Dana/0000-0003-1052-1494; Mazarico, Erwan/0000-0003-3456-427X;
Retherford, Kurt/0000-0001-9470-150X
FU NASA [NNG05EC87C]; LRO
FX We thank the LRO project for support of the LAMP observations reported
here. In particular we thank C. Tooley, D. Everett, M. Houghton, A.
Bartels, C. Baker, R. Saylor, R. Vondrak, G. Chin, J. Keller, T.
Johnson, and S. Odendahl for making LRO work so well. LAMP is funded by
NASA under contract NNG05EC87C, whose financial support we gratefully
acknowledge.
NR 38
TC 27
Z9 27
U1 4
U2 26
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 JAN 7
PY 2012
VL 117
AR E00H04
DI 10.1029/2011JE003913
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 874BW
UT WOS:000298931000001
ER
PT J
AU Farrell, SL
McAdoo, DC
Laxon, SW
Zwally, HJ
Yi, DH
Ridout, A
Giles, K
AF Farrell, Sinead Louise
McAdoo, David C.
Laxon, Seymour W.
Zwally, H. Jay
Yi, Donghui
Ridout, Andy
Giles, Katharine
TI Mean dynamic topography of the Arctic Ocean
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID ALTIMETER MEASUREMENTS; AIRBORNE LASER; SEA-ICE; CIRCULATION; RADAR
AB ICESat and Envisat altimetry data provide measurements of the instantaneous sea surface height (SSH) across the Arctic Ocean, using lead and open water elevation within the sea ice pack. First, these data were used to derive two independent mean sea surface (MSS) models by stacking and averaging along-track SSH profiles gathered between 2003 and 2009. The ICESat and Envisat MSS data were combined to construct the high-resolution ICEn MSS. Second, we estimate the 5.5-year mean dynamic topography (MDT) of the Arctic Ocean by differencing the ICEn MSS with the new GOCO02S geoid model, derived from GRACE and GOCE gravity. Using these satellite-only data we map the major features of Arctic Ocean dynamical height that are consistent with in situ observations, including the topographical highs and lows of the Beaufort and Greenland Gyres, respectively. Smaller-scale MDT structures remain largely unresolved due to uncertainties in the geoid at short wavelengths. Citation: Farrell, S. L., D. C. McAdoo, S. W. Laxon, H. J. Zwally, D. Yi, A. Ridout, and K. Giles (2012), Mean dynamic topography of the Arctic Ocean, Geophys. Res. Lett., 39, L01601, doi:10.1029/2011GL050052.
C1 [Farrell, Sinead Louise] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20740 USA.
[Farrell, Sinead Louise; McAdoo, David C.] NOAA, Lab Satellite Altimetry, Silver Spring, MD 20910 USA.
[Farrell, Sinead Louise; Zwally, H. Jay; Yi, Donghui] NASA, Cryospher Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Laxon, Seymour W.; Ridout, Andy; Giles, Katharine] UCL, Ctr Polar Observat & Modelling, Natl Ctr Earth Observat, London WC1E 6BT, England.
RP Farrell, SL (reprint author), Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, 5825 Univ Res Ct,Ste 4001, College Pk, MD 20740 USA.
EM sineadf@umd.edu
RI Farrell, Sinead/F-5586-2010; Giles, Katharine/G-3837-2010; McAdoo,
Dave/F-5612-2010
OI Farrell, Sinead/0000-0003-3222-2751; McAdoo, Dave/0000-0002-7533-5564
FU NASA [NNX10AG17G]; United Kingdom Natural Environment Research Council
FX We acknowledge NASA's ICESat Science Project and the NSIDC for
distribution of the ICESat data (see http://nsidc.org/data/icesat/), and
ESA for the distribution of Envisat data. We thank three anonymous
reviewers for their comments and suggestions, which helped to improve
this note. Support for SLF has been provided by the NASA Cryosphere
Program under NASA grant NNX10AG17G. Support for ALR, KAG, and SWL is
provided by the United Kingdom Natural Environment Research Council. The
views, opinions, and findings contained in this report are those of the
authors and should not be construed as an official National Oceanic and
Atmospheric Administration or U.S. Government position, policy, or
decision.
NR 18
TC 16
Z9 19
U1 2
U2 15
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN 6
PY 2012
VL 39
AR L01601
DI 10.1029/2011GL050052
PG 5
WC Geosciences, Multidisciplinary
SC Geology
GA 874BV
UT WOS:000298930900003
ER
PT J
AU Lasue, J
Wiens, RC
Clegg, SM
Vaniman, DT
Joy, KH
Humphries, S
Mezzacappa, A
Melikechi, N
McInroy, RE
Bender, S
AF Lasue, J.
Wiens, R. C.
Clegg, S. M.
Vaniman, D. T.
Joy, K. H.
Humphries, S.
Mezzacappa, A.
Melikechi, N.
McInroy, R. E.
Bender, S.
TI Remote laser-induced breakdown spectroscopy (LIBS) for lunar exploration
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
ID IMPACT-MELT BRECCIAS; APOLLO-16 REGOLITH BRECCIAS; POLE-AITKEN BASIN;
WATER ICE; PECORA ESCARPMENT-02007; THORIUM ABUNDANCES; SPACE
EXPLORATION; CENTRAL-HIGHLANDS; MOON; METEORITES
AB Laser-induced breakdown spectroscopy (LIBS) is an active analytical technique that makes use of a laser pulse to analyze materials of interest at a distance by creating a plasma, which emits photons at characteristic emission line wavelengths. We validate the technique for planetary exploration under vacuum conditions. We review the capability and advantages of the LIBS technique for lunar regolith analysis at 1.5 m distance from a lunar rover, and we characterize its potential for the detection of resources for future exploration, such as the determination of regolith water content. The limits of detection determined for the major elements (typically <1 wt %) help to determine regolith parent material such as feldspathic highland rocks, rocks from the ancient magmatic high magnesian suite (Mg-suite), Fe-rich mare basalts or potassium, rare earth element, and phosphorus-rich (KREEP-rich) samples. Compositional parameters commonly used to classify lunar regoliths such as TiO2, Al2O3, and K2O abundances are readily determined by LIBS. Certain elements support regolith analysis: For example, Ba and Zr can be used to confirm KREEP-like composition, while quantifying the Ni and Co content can be used to infer the amount of meteoritic material. Finally, it is shown that the ice content of lunar soil produces strong H emissions with the LIBS techniques at the 25 wt % H2O level, while measurements on altered basalts give a limit of detection of about 1 wt % for H2O content. This demonstrates that the 5.6 wt % water content detected by the recent LCROSS experiment should be easily detectable and quantifiable by LIBS analysis.
C1 [Lasue, J.; Wiens, R. C.; Bender, S.] Los Alamos Natl Lab, ISR, Los Alamos, NM 87545 USA.
[Clegg, S. M.; Humphries, S.; McInroy, R. E.] Los Alamos Natl Lab, C PCS, Los Alamos, NM 87545 USA.
[Lasue, J.; Joy, K. H.] Lunar & Planetary Inst, Houston, TX 77058 USA.
[Mezzacappa, A.; Melikechi, N.] Delaware State Univ, Appl Opt Ctr, Dover, DE 19901 USA.
[Vaniman, D. T.] Los Alamos Natl Lab, EES 14, Los Alamos, NM 87545 USA.
[Joy, K. H.] NASA Ames Res Ctr, NASA Lunar Sci Inst, Moffett Field, CA USA.
RP Lasue, J (reprint author), Los Alamos Natl Lab, ISR, MS D466, Los Alamos, NM 87545 USA.
EM lasue@lanl.gov
OI Joy, Katherine/0000-0003-4992-8750; Clegg, Sam/0000-0002-0338-0948
FU Los Alamos National Laboratory (LANL) Laboratory Directed Research and
Development (LDRD); NASA URC [NNX09AU90A]
FX The authors thank K. Ishibashi and F. Rull for useful comments that
helped improve the manuscript. The authors thank J. Ranke for helpful
discussion and for providing the chemCal R package to the community.
This work was made possible by Los Alamos National Laboratory (LANL)
Laboratory Directed Research and Development (LDRD) funding and the NASA
URC grant NNX09AU90A. This is JL and KHJ LPI contribution 1634.
NR 105
TC 14
Z9 14
U1 2
U2 38
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9097
EI 2169-9100
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD JAN 6
PY 2012
VL 117
AR E01002
DI 10.1029/2011JE003898
PG 18
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 874BU
UT WOS:000298930800001
ER
PT J
AU Davies, AG
Veeder, GJ
Matson, DL
Johnson, TV
AF Davies, A. G.
Veeder, G. J.
Matson, D. L.
Johnson, T. V.
TI Io: Charting thermal emission variability with the Galileo NIMS Io
Thermal Emission Database (NITED): Loki Patera
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID INFRARED MAPPING SPECTROMETER; VOLCANIC ACTIVITY; HOT-SPOTS; HEAT-FLOW;
TEMPERATURE
AB We have calculated the approximate to 5-mu m radiant flux for every volcanic hot spot in every one of the 190 Galileo Near-Infrared Mapping Spectrometer (NIMS) tube observations of Io obtained between 28 June 1996 and 16 October 2001 in order to determine the variability of thermal emission from Io's volcanoes at local, regional and global scales, and to identify individual eruption episodes where thermal emission waxes and wanes. The resulting NIMS Io Thermal Emission Database (NITED) allows the comparison of activity at individual volcanoes and different regions of Io. The database contains over 1000 measurements of radiant flux at approximately 5 mu m, corrected for emission angle, range to target and incident sunlight (where necessary). We examine the data for Loki Patera, Io's most powerful volcano. For data acquired in local darkness we use two-temperature fits to nighttime spectra and prior knowledge of emitting area to determine total radiated thermal emission. For other data we use the constancy of the integrated thermal emission spectrum to determine total thermal emission from measurements of radiant flux at 5 mu m. As seen by NIMS, total thermal emission from Loki Patera varies between 7600 GW and 17000 GW. We revise upwards previous estimates of thermal emission from NIMS data. NIMS 3.5-mu m radiant fluxes (both measured and estimated) are consistent with measurements from ground-based telescopes. This work highlights the value of NITED as a research tool. Citation: Davies, A. G., G. J. Veeder, D. L. Matson, and T. V. Johnson (2012), Io: Charting thermal emission variability with the Galileo NIMS Io Thermal Emission Database (NITED): Loki Patera, Geophys. Res. Lett., 39, L01201, doi:10.1029/2011GL049999.
C1 [Davies, A. G.; Matson, D. L.; Johnson, T. V.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Veeder, G. J.] Bear Fight Inst, Winthrop, WA 98862 USA.
RP Davies, AG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Ashley.Davies@jpl.nasa.gov
FU NASA; NASA OPR
FX This work was conducted at the Jet Propulsion Laboratory, California
Institute of Technology, under contract with NASA, and is supported by
the NASA OPR Program.
NR 23
TC 11
Z9 11
U1 0
U2 2
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 JAN 5
PY 2012
VL 39
AR L01201
DI 10.1029/2011GL049999
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 874BT
UT WOS:000298930700003
ER
PT J
AU Marubashi, K
Cho, KS
Kim, YH
Park, YD
Park, SH
AF Marubashi, Katsuhide
Cho, Kyung-Suk
Kim, Yeon-Han
Park, Yong-Deuk
Park, Sung-Hong
TI Geometry of the 20 November 2003 magnetic cloud
SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS
LA English
DT Article
ID CORONAL MASS EJECTION; SOLAR-WIND; FLUX ROPES; HELICITY; MODEL;
ORIENTATION; FILAMENTS; REGIONS
AB This study is an attempt to find a coherent interpretation of the link between the 20 November 2003 magnetic cloud (MC) and its solar source. Most previous studies agree on the orientation of the MC, but the orientation is nearly perpendicular to the axis of the post-eruption arcade (PEA) or the orientation of the neutral line in the solar source region. We first determine the geometry of this MC by fitting methods with both torus and cylinder models. Three possible geometries are obtained, which can reproduce the observed magnetic field variations associated with the MC, one from the cylinder fit and two from the torus fit. The cylinder fit gives the MC orientation with a tilt of a large angle (similar to 60 degrees) from the ecliptic plane and nearly perpendicular to the PEA axis, being similar to those from previous studies. In contrast, two torus fit results give the MC axis with tilt angles less than 20 from the ecliptic plane. The two torus results correspond to the spacecraft encounter with the eastern flank of the flux rope loop (model A) and the western flank of the loop (model B), respectively. In either case, the orientation of the loop around the apex is nearly parallel to the PEA as observed by the SOHO/extreme ultraviolet imaging telescope instrument in the most plausible solar source region of a halo coronal mass ejection (CME), which appeared in the field of view of Large Angle and Spectrometric Coronagraph (LASCO) C2 at 08:50 UT, 18 November 2003. The magnetic helicity of the PEA region is positive in agreement with the helicity of the MC. The 3-D reconstruction from the Solar Mass Ejection Imager data shows that the main part of the ejected plasma expands mainly to the west of the Sun-Earth line. Thus, we reach the most straightforward interpretation of the link between the MC and its solar source as follows. The MC was created in association with the launch of the CME that was first observed by the LASCO C2 at 08:50 UT, 18 November 2003, and propagated through interplanetary space with its orientation almost unchanged. The spacecraft encountered the eastern flank of the loop as described by model A.
C1 [Marubashi, Katsuhide; Cho, Kyung-Suk; Kim, Yeon-Han; Park, Yong-Deuk; Park, Sung-Hong] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
[Cho, Kyung-Suk] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Cho, Kyung-Suk] Catholic Univ Amer, Washington, DC 20064 USA.
RP Marubashi, K (reprint author), Korea Astron & Space Sci Inst, 61-1 Whaam Dong, Taejon 305348, South Korea.
EM kmaru@kasi.re.kr
RI Park, Sung-Hong/K-1578-2014
OI Park, Sung-Hong/0000-0001-9149-6547
FU Development of Korean Space Weather Center; KASI
FX We thank the ACE/MAG and SWEPAM teams and the ACE Science Center for
providing the solar wind data. We also gratefully acknowledge the use of
data from the Wind/MFI and SWE instruments. The authors' special
gratitude is directed to Bernard V. Jackson of UCSD for providing newly
analyzed images from the SMEI, which is a collaborative project of the
U. S. Air Force Research Laboratory; NASA; the University of California
at San Diego; the University of Birmingham, UK; Boston College; and
Boston University. This work was supported by the Development of Korean
Space Weather Center, the project of KASI, and the KASI basic research
fund.
NR 30
TC 9
Z9 9
U1 0
U2 7
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 JAN 5
PY 2012
VL 117
AR A01101
DI 10.1029/2011JA016802
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 874GR
UT WOS:000298943900002
ER
PT J
AU Beck, PG
Montalban, J
Kallinger, T
De Ridder, J
Aerts, C
Garcia, RA
Hekker, S
Dupret, MA
Mosser, B
Eggenberger, P
Stello, D
Elsworth, Y
Frandsen, S
Carrier, F
Hillen, M
Gruberbauer, M
Christensen-Dalsgaard, J
Miglio, A
Valentini, M
Bedding, TR
Kjeldsen, H
Girouard, FR
Hall, JR
Ibrahim, KA
AF Beck, Paul G.
Montalban, Josefina
Kallinger, Thomas
De Ridder, Joris
Aerts, Conny
Garcia, Rafael A.
Hekker, Saskia
Dupret, Marc-Antoine
Mosser, Benoit
Eggenberger, Patrick
Stello, Dennis
Elsworth, Yvonne
Frandsen, Soren
Carrier, Fabien
Hillen, Michel
Gruberbauer, Michael
Christensen-Dalsgaard, Jorgen
Miglio, Andrea
Valentini, Marica
Bedding, Timothy R.
Kjeldsen, Hans
Girouard, Forrest R.
Hall, Jennifer R.
Ibrahim, Khadeejah A.
TI Fast core rotation in red-giant stars as revealed by gravity-dominated
mixed modes
SO NATURE
LA English
DT Article
ID SOLAR-LIKE OSCILLATIONS; ASTEROSEISMOLOGY; KEPLER; CIRCULATION
AB When the core hydrogen is exhausted during stellar evolution, the central region of a star contracts and the outer envelope expands and cools, giving rise to a red giant. Convection takes place overmuch of the star's radius. Conservation of angular momentum requires that the cores of these stars rotate faster than their envelopes; indirect evidence supports this(1,2). Information about the angular-momentum distribution is inaccessible to direct observations, but it can be extracted from the effect of rotation on oscillation modes that probe the stellar interior. Here we report an increasing rotation rate from the surface of the star to the stellar core in the interiors of red giants, obtained using the rotational frequency splitting of recently detected 'mixed modes'(3,4). By comparison with theoretical stellar models, we conclude that the core must rotate at least ten times faster than the surface. This observational result confirms the theoretical prediction of a steep gradient in the rotation profile towards the deep stellar interior(1,5,6).
C1 [Beck, Paul G.; Kallinger, Thomas; De Ridder, Joris; Aerts, Conny; Carrier, Fabien; Hillen, Michel] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
[Montalban, Josefina; Dupret, Marc-Antoine; Valentini, Marica] Univ Liege, Inst Astrophys Geophys, B-4000 Liege, Belgium.
[Kallinger, Thomas] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Aerts, Conny] Radboud Univ Nijmegen, IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Garcia, Rafael A.] Univ Paris Diderot, CNRS, IRFU Sap, Ctr Saclay,CEA DSM,Lab Astrophys Instrumentat & M, F-91191 Gif Sur Yvette, France.
[Hekker, Saskia] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
[Hekker, Saskia; Elsworth, Yvonne; Miglio, Andrea] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Mosser, Benoit] Univ Paris 07, Univ Paris 06, CNRS, Observ Paris,Lab Etudes Spatiales & Instrumentat, F-92195 Meudon, France.
[Eggenberger, Patrick] Univ Geneva, Observ Geneve, CH-1290 Sauverny, Switzerland.
[Stello, Dennis; Bedding, Timothy R.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
[Frandsen, Soren; Christensen-Dalsgaard, Jorgen; Kjeldsen, Hans] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Gruberbauer, Michael] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada.
[Girouard, Forrest R.; Hall, Jennifer R.; Ibrahim, Khadeejah A.] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
RP Beck, PG (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium.
EM paul.beck@ster.kuleuven.be
OI Kallinger, Thomas/0000-0003-3627-2561; Hillen,
Michel/0000-0001-9086-4766; Bedding, Timothy/0000-0001-5943-1460;
Bedding, Tim/0000-0001-5222-4661; Garcia, Rafael/0000-0002-8854-3776
FU NASA's Science Mission Directorate; European Community; Fund for
Scientific Research, Flanders; Netherlands Organisation for Scientific
Research; Belgian Science Policy Office
FX We acknowledge the work of the team behind Kepler. Funding for the
Kepler Mission is provided by NASA's Science Mission Directorate. P. G.
B. and C. A. were supported by the European Community's Seventh
Framework Programme (ERC grant PROSPERITY); J.D.R. and T.K. were
supported by the Fund for Scientific Research, Flanders. S. H. was
supported by the Netherlands Organisation for Scientific Research. J.M.
and M. V. were supported by the Belgian Science Policy Office. The work
is partly based on observations with the High Efficiency and Resolution
Mercator Echelle Spectrograph at the Mercator Telescope, which is
operated at La Palma in Spain by the Flemish Community.
NR 24
TC 183
Z9 183
U1 32
U2 183
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD JAN 5
PY 2012
VL 481
IS 7379
BP 55
EP 57
DI 10.1038/nature10612
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 872VD
UT WOS:000298836900027
PM 22158105
ER
PT J
AU Morison, J
Kwok, R
Peralta-Ferriz, C
Alkire, M
Rigor, I
Andersen, R
Steele, M
AF Morison, James
Kwok, Ron
Peralta-Ferriz, Cecilia
Alkire, Matt
Rigor, Ignatius
Andersen, Roger
Steele, Mike
TI Changing Arctic Ocean freshwater pathways
SO NATURE
LA English
DT Article
ID BEAUFORT GYRE; ICE; TEMPERATURE; VARIABILITY; RUNOFF; MODEL
AB Freshening in the Canada basin of the Arctic Ocean began in the 1990s(1,2) and continued(3) to at least the end of 2008. By then, the Arctic Ocean might have gained four times as much fresh water as comprised the Great Salinity Anomaly(4,5) of the 1970s, raising the spectre of slowing global ocean circulation(6). Freshening has been attributed to increased sea ice melting(1) and contributions from runoff(7), but a leading explanation has been a strengthening of the Beaufort High-a characteristic peak in sea level atmospheric pressure(2,8)-which tends to accelerate an anticyclonic (clockwise) wind pattern causing convergence of fresh surface water. Limited observations have made this explanation difficult to verify, and observations of increasing freshwater content under a weakened Beaufort High suggest that other factors(2) must be affecting freshwater content. Here we use observations to show that during a time of record reductions in ice extent from 2005 to 2008, the dominant freshwater content changes were an increase in the Canada basin balanced by a decrease in the Eurasian basin. Observations are drawn from satellite data (sea surface height and ocean-bottom pressure) and in situ data. The freshwater changes were due to a cyclonic (anticlockwise) shift in the ocean pathway of Eurasian runoff forced by strengthening of the west-to-east Northern Hemisphere atmospheric circulation characterized by an increased Arctic Oscillation(9) index. Our results confirm that runoff is an important influence on the Arctic Ocean and establish that the spatial and temporal manifestations of the runoff pathways are modulated by the Arctic Oscillation, rather than the strength of the wind-driven Beaufort Gyre circulation.
C1 [Morison, James; Peralta-Ferriz, Cecilia; Alkire, Matt; Rigor, Ignatius; Andersen, Roger; Steele, Mike] Univ Washington, Appl Phys Lab, Polar Sci Ctr, Seattle, WA 98105 USA.
[Kwok, Ron] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Morison, J (reprint author), Univ Washington, Appl Phys Lab, Polar Sci Ctr, 1013 NE 40th St, Seattle, WA 98105 USA.
EM morison@apl.washington.edu
RI Kwok, Ron/A-9762-2008
OI Kwok, Ron/0000-0003-4051-5896
FU NSF [OPP 0352754]; NASA [NNX08AH62G]; Jet Propulsion Laboratory,
California Institute of Technology; NASA MEASURES; [ARC-0634226];
[ARC-0856330]
FX This work was supported chiefly by NSF grants OPP 0352754, ARC-0634226,
ARC-0856330 and NASA grant NNX08AH62G. R. K. was supported at the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with NASA. GRACE ocean data were processed by D. P. Chambers,
supported by the NASA MEASURES Program. We thank the NASA ICESat and
GRACE programmes, K. Falkner, R. Collier, M. McPhee, W. Ermold, L. de
Steur, A. Proshutinsky and the Beaufort Gyre Exploration Project, J.
Toole and R. Krishfield and the Ice Tethered Profiler project at WHOI,
and W. Smethie of the Switchyard project for the observations that made
this work possible.
NR 31
TC 121
Z9 124
U1 5
U2 84
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
EI 1476-4687
J9 NATURE
JI Nature
PD JAN 5
PY 2012
VL 481
IS 7379
BP 66
EP 70
DI 10.1038/nature10705
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 872VD
UT WOS:000298836900030
PM 22222749
ER
PT J
AU Abadie, J
Abbott, BP
Abbott, R
Abbott, TD
Abernathy, M
Accadia, T
Acernese, F
Adams, C
Adhikari, R
Affeldt, C
Ajith, P
Allen, B
Allen, GS
Ceron, EA
Amariutei, D
Amin, RS
Anderson, SB
Anderson, WG
Arai, K
Arain, MA
Araya, MC
Aston, SM
Astone, P
Atkinson, D
Aufmuth, P
Aulbert, C
Aylott, BE
Babak, S
Baker, P
Ballardin, G
Ballmer, S
Barker, D
Barone, F
Barr, B
Barriga, P
Barsotti, L
Barsuglia, M
Barton, MA
Bartos, I
Bassiri, R
Bastarrika, M
Basti, A
Batch, J
Bauchrowitz, J
Bauer, TS
Bebronne, M
Behnke, B
Beker, MG
Bell, AS
Belletoile, A
Belopolski, I
Benacquista, M
Berliner, JM
Bertolini, A
Betzwieser, J
Beveridge, N
Beyersdorf, PT
Bilenko, IA
Billingsley, G
Birch, J
Biswas, R
Bitossi, M
Bizouard, MA
Black, E
Blackburn, JK
Blackburn, L
Blair, D
Bland, B
Blom, M
Bock, O
Bodiya, TP
Bogan, C
Bondarescu, R
Bondu, F
Bonelli, L
Bonnand, R
Bork, R
Born, M
Boschi, V
Bose, S
Bosi, L
Bouhou, B
Braccini, S
Bradaschia, C
Brady, PR
Braginsky, VB
Branchesi, M
Brau, JE
Breyer, J
Briant, T
Bridges, DO
Brillet, A
Brinkmann, M
Brisson, V
Britzger, M
Brooks, AF
Brown, DA
Brummit, A
Bulik, T
Bulten, HJ
Buonanno, A
Burguet-Castell, J
Burmeister, O
Buskulic, D
Buy, C
Byer, RL
Cadonati, L
Cagnoli, G
Calloni, E
Camp, JB
Campsie, P
Cannizzo, J
Cannon, K
Canuel, B
Cao, J
Capano, CD
Carbognani, F
Caride, S
Caudill, S
Cavaglia, M
Cavalier, F
Cavalieri, R
Cella, G
Cepeda, C
Cesarini, E
Chaibi, O
Chalermsongsak, T
Chalkley, E
Charlton, P
Chassande-Mottin, E
Chelkowski, S
Chen, Y
Chincarini, A
Chiummo, A
Cho, H
Christensen, N
Chua, SSY
Chung, CTY
Chung, S
Ciani, G
Clara, F
Clark, DE
Clark, J
Clayton, JH
Cleva, F
Coccia, E
Cohadon, PF
Colacino, CN
Colas, J
Colla, A
Colombini, M
Conte, A
Conte, R
Cook, D
Corbitt, TR
Cordier, M
Cornish, N
Corsi, A
Costa, CA
Coughlin, M
Coulon, JP
Couvares, P
Coward, DM
Coyne, DC
Creighton, JDE
Creighton, TD
Cruise, AM
Cumming, A
Cunningham, L
Cuoco, E
Cutler, RM
Dahl, K
Danilishin, SL
Dannenberg, R
D'Antonio, S
Danzmann, K
Dattilo, V
Daudert, B
Daveloza, H
Davier, M
Davies, G
Daw, EJ
Day, R
Dayanga, T
De Rosa, R
Debra, D
Debreczeni, G
Degallaix, J
Del Pozzo, W
del Prete, M
Dent, T
Dergachev, V
DeRosa, R
DeSalvo, R
Dhurandhar, S
Di Fiore, L
DiGuglielmo, J
Di Lieto, A
Di Palma, I
Emilio, MDP
Di Virgilio, A
Diaz, M
Dietz, A
Donovan, F
Dooley, KL
Dorsher, S
Drago, M
Drever, RWP
Driggers, JC
Du, Z
Dumas, JC
Dwyer, S
Eberle, T
Edgar, M
Edwards, M
Effler, A
Ehrens, P
Endroczi, G
Engel, R
Etzel, T
Evans, K
Evans, M
Evans, T
Factourovich, M
Fafone, V
Fairhurst, S
Fan, Y
Farr, BF
Farr, W
Fazi, D
Fehrmann, H
Feldbaum, D
Ferrante, I
Fidecaro, F
Finn, LS
Fiori, I
Fisher, RP
Flaminio, R
Flanigan, M
Foley, S
Forsi, E
Forte, LA
Fotopoulos, N
Fournier, JD
Franc, J
Frasca, S
Frasconi, F
Frede, M
Frei, M
Frei, Z
Freise, A
Frey, R
Fricke, TT
Friedrich, D
Fritschel, P
Frolov, VV
Fulda, PJ
Fyffe, M
Galimberti, M
Gammaitoni, L
Ganija, MR
Garcia, J
Garofoli, JA
Garufi, F
Gaspar, ME
Gemme, G
Geng, R
Genin, E
Gennai, A
Gergely, LA
Ghosh, S
Giaime, JA
Giampanis, S
Giardina, KD
Giazotto, A
Gill, C
Goetz, E
Goggin, LM
Gonzalez, G
Gorodetsky, ML
Gossler, S
Gouaty, R
Graef, C
Granata, M
Grant, A
Gras, S
Gray, C
Gray, N
Greenhalgh, RJS
Gretarsson, AM
Greverie, C
Grosso, R
Grote, H
Grunewald, S
Guidi, GM
Guido, C
Gupta, R
Gustafson, EK
Gustafson, R
Ha, T
Hage, B
Hallam, JM
Hammer, D
Hammond, G
Hanks, J
Hanna, C
Hanson, J
Harms, J
Harry, GM
Harry, IW
Harstad, ED
Hartman, MT
Haughian, K
Hayama, K
Hayau, JF
Hayler, T
Heefner, J
Heidmann, A
Heintze, MC
Heitmann, H
Hello, P
Hendry, MA
Heng, IS
Heptonstall, AW
Herrera, V
Hewitson, M
Hild, S
Hoak, D
Hodge, KA
Holt, K
Hong, T
Hooper, S
Hosken, DJ
Hough, J
Howell, EJ
Hughey, B
Husa, S
Huttner, SH
Huynh-Dinh, T
Ingram, DR
Inta, R
Isogai, T
Ivanov, A
Izumi, K
Jacobson, M
Jang, H
Jaranowski, P
Johnson, WW
Jones, DI
Jones, G
Jones, R
Ju, L
Kalmus, P
Kalogera, V
Kamaretsos, I
Kandhasamy, S
Kang, G
Kanner, JB
Katsavounidis, E
Katzman, W
Kaufer, H
Kawabe, K
Kawamura, S
Kawazoe, F
Kells, W
Keppel, DG
Keresztes, Z
Khalaidovski, A
Khalili, FY
Khazanov, EA
Kim, B
Kim, C
Kim, D
Kim, H
Kim, K
Kim, N
Kim, YM
King, PJ
Kinsey, M
Kinzel, DL
Kissel, JS
Klimenko, S
Kokeyama, K
Kondrashov, V
Kopparapu, R
Koranda, S
Korth, WZ
Kowalska, I
Kozak, D
Kringel, V
Krishnamurthy, S
Krishnan, B
Krolak, A
Kuehn, G
Kumar, R
Kwee, P
Lam, PK
Landry, M
Lang, M
Lantz, B
Lastzka, N
Lawrie, C
Lazzarini, A
Leaci, P
Lee, CH
Lee, HM
Leindecker, N
Leong, JR
Leonor, I
Leroy, N
Letendre, N
Li, J
Li, TGF
Liguori, N
Lindquist, PE
Lockerbie, NA
Lodhia, D
Lorenzini, M
Loriette, V
Lormand, M
Losurdo, G
Luan, J
Lubinski, M
Luck, H
Lundgren, AP
Macdonald, E
Machenschalk, B
MacInnis, M
Macleod, DM
Mageswaran, M
Mailand, K
Majorana, E
Maksimovic, I
Man, N
Mandel, I
Mandic, V
Mantovani, M
Marandi, A
Marchesoni, F
Marion, F
Marka, S
Marka, Z
Markosyan, A
Maros, E
Marque, J
Martelli, F
Martin, IW
Martin, RM
Marx, JN
Mason, K
Masserot, A
Matichard, F
Matone, L
Matzner, RA
Mavalvala, N
Mazzolo, G
McCarthy, R
McClelland, DE
McGuire, SC
McIntyre, G
McIver, J
McKechan, DJA
Meadors, GD
Mehmet, M
Meier, T
Melatos, A
Melissinos, AC
Mendell, G
Menendez, D
Mercer, RA
Meshkov, S
Messenger, C
Meyer, MS
Miao, H
Michel, C
Milano, L
Miller, J
Minenkov, Y
Mitrofanov, VP
Mitselmakher, G
Mittleman, R
Miyakawa, O
Moe, B
Moesta, P
Mohan, M
Mohanty, SD
Mohapatra, SRP
Moraru, D
Moreno, G
Morgado, N
Morgia, A
Mori, T
Mosca, S
Mossavi, K
Mours, B
Mow-Lowry, CM
Mueller, CL
Mueller, G
Mukherjee, S
Mullavey, A
Muller-Ebhardt, H
Munch, J
Murphy, D
Murray, PG
Mytidis, A
Nash, T
Naticchioni, L
Nawrodt, R
Necula, V
Nelson, J
Newton, G
Nishizawa, A
Nocera, F
Nolting, D
Nuttall, L
Ochsner, E
O'Dell, J
Oelker, E
Ogin, GH
Oh, JJ
Oh, SH
Oldenburg, RG
O'Reilly, B
O'Shaughnessy, R
Osthelder, C
Ott, CD
Ottaway, DJ
Ottens, RS
Overmier, H
Owen, BJ
Page, A
Pagliaroli, G
Palladino, L
Palomba, C
Pan, Y
Pankow, C
Paoletti, F
Papa, MA
Parisi, M
Pasqualetti, A
Passaquieti, R
Passuello, D
Patel, P
Pedraza, M
Peiris, P
Pekowsky, L
Penn, S
Peralta, C
Perreca, A
Persichetti, G
Phelps, M
Pickenpack, M
Piergiovanni, F
Pietka, M
Pinard, L
Pinto, IM
Pitkin, M
Pletsch, HJ
Plissi, MV
Poggiani, R
Pold, J
Postiglione, F
Prato, M
Predoi, V
Price, LR
Prijatelj, M
Principe, M
Privitera, S
Prix, R
Prodi, GA
Prokhorov, L
Puncken, O
Punturo, M
Puppo, P
Quetschke, V
Raab, FJ
Rabeling, DS
Racz, I
Radkins, H
Raffai, P
Rakhmanov, M
Ramet, CR
Rankins, B
Rapagnani, P
Raymond, V
Re, V
Redwine, K
Reed, CM
Reed, T
Regimbau, T
Reid, S
Reitze, DH
Ricci, F
Riesen, R
Riles, K
Robertson, NA
Robinet, F
Robinson, C
Robinson, EL
Rocchi, A
Roddy, S
Rodriguez, C
Rodruck, M
Rolland, L
Rollins, J
Romano, JD
Romano, R
Romie, JH
Rosinska, D
Rover, C
Rowan, S
Rudiger, A
Ruggi, P
Ryan, K
Ryll, H
Sainathan, P
Sakosky, M
Salemi, F
Samblowski, A
Sammut, L
de la Jordana, LS
Sandberg, V
Sankar, S
Sannibale, V
Santamaria, L
Santiago-Prieto, I
Santostasi, G
Sassolas, B
Sathyaprakash, BS
Sato, S
Saulson, PR
Savage, RL
Schilling, R
Schlamminger, S
Schnabel, R
Schofield, RMS
Schulz, B
Schutz, BF
Schwinberg, P
Scott, J
Scott, SM
Searle, AC
Seifert, F
Sellers, D
Sengupta, AS
Sentenac, D
Sergeev, A
Shaddock, DA
Shaltev, M
Shapiro, B
Shawhan, P
Shoemaker, DH
Sibley, A
Siemens, X
Sigg, D
Singer, A
Singer, L
Sintes, AM
Skelton, G
Slagmolen, BJJ
Slutsky, J
Smith, JR
Smith, MR
Smith, ND
Smith, RJE
Somiya, K
Sorazu, B
Soto, J
Speirits, FC
Sperandio, L
Stefszky, M
Stein, AJ
Steinert, E
Steinlechner, J
Steinlechner, S
Steplewski, S
Stochino, A
Stone, R
Strain, KA
Strigin, S
Stroeer, AS
Sturani, R
Stuver, AL
Summerscales, TZ
Sung, M
Susmithan, S
Sutton, PJ
Swinkels, B
Tacca, M
Taffarello, L
Talukder, D
Tanner, DB
Tarabrin, SP
Taylor, JR
Taylor, R
Thomas, P
Thorne, KA
Thorne, KS
Thrane, E
Thuring, A
Titsler, C
Tokmakov, KV
Toncelli, A
Tonelli, M
Torre, O
Torres, C
Torrie, CI
Tournefier, E
Travasso, F
Traylor, G
Trias, M
Tseng, K
Ugolini, D
Urbanek, K
Vahlbruch, H
Vajente, G
Vallisneri, M
van den Brand, JFJ
Van Den Broeck, C
van der Putten, S
van Veggel, AA
Vass, S
Vasuth, M
Vaulin, R
Vavoulidis, M
Vecchio, A
Vedovato, G
Veitch, J
Veitch, PJ
Veltkamp, C
Verkindt, D
Vetrano, F
Vicere, A
Villar, AE
Vinet, JY
Vitale, S
Vitale, S
Vocca, H
Vorvick, C
Vyatchanin, SP
Wade, A
Waldman, SJ
Wallace, L
Wan, Y
Wang, X
Wang, Z
Wanner, A
Ward, RL
Was, M
Wei, P
Weinert, M
Weinstein, AJ
Weiss, R
Wen, L
Wen, S
Wessels, P
West, M
Westphal, T
Wette, K
Whelan, JT
Whitcomb, SE
White, D
Whiting, BF
Wilkinson, C
Willems, PA
Williams, HR
Williams, L
Willke, B
Winkelmann, L
Winkler, W
Wipf, CC
Wiseman, AG
Wittel, H
Woan, G
Wooley, R
Worden, J
Yablon, J
Yakushin, I
Yamamoto, H
Yamamoto, K
Yang, H
Yeaton-Massey, D
Yoshida, S
Yu, P
Yvert, M
Zadrozny, A
Zanolin, M
Zendri, JP
Zhang, F
Zhang, L
Zhang, W
Zhang, Z
Zhao, C
Zotov, N
Zucker, ME
Zweizig
AF Abadie, J.
Abbott, B. P.
Abbott, R.
Abbott, T. D.
Abernathy, M.
Accadia, T.
Acernese, F.
Adams, C.
Adhikari, R.
Affeldt, C.
Ajith, P.
Allen, B.
Allen, G. S.
Ceron, E. Amador
Amariutei, D.
Amin, R. S.
Anderson, S. B.
Anderson, W. G.
Arai, K.
Arain, M. A.
Araya, M. C.
Aston, S. M.
Astone, P.
Atkinson, D.
Aufmuth, P.
Aulbert, C.
Aylott, B. E.
Babak, S.
Baker, P.
Ballardin, G.
Ballmer, S.
Barker, D.
Barone, F.
Barr, B.
Barriga, P.
Barsotti, L.
Barsuglia, M.
Barton, M. A.
Bartos, I.
Bassiri, R.
Bastarrika, M.
Basti, A.
Batch, J.
Bauchrowitz, J.
Bauer, Th S.
Bebronne, M.
Behnke, B.
Beker, M. G.
Bell, A. S.
Belletoile, A.
Belopolski, I.
Benacquista, M.
Berliner, J. M.
Bertolini, A.
Betzwieser, J.
Beveridge, N.
Beyersdorf, P. T.
Bilenko, I. A.
Billingsley, G.
Birch, J.
Biswas, R.
Bitossi, M.
Bizouard, M. A.
Black, E.
Blackburn, J. K.
Blackburn, L.
Blair, D.
Bland, B.
Blom, M.
Bock, O.
Bodiya, T. P.
Bogan, C.
Bondarescu, R.
Bondu, F.
Bonelli, L.
Bonnand, R.
Bork, R.
Born, M.
Boschi, V.
Bose, S.
Bosi, L.
Bouhou, B.
Braccini, S.
Bradaschia, C.
Brady, P. R.
Braginsky, V. B.
Branchesi, M.
Brau, J. E.
Breyer, J.
Briant, T.
Bridges, D. O.
Brillet, A.
Brinkmann, M.
Brisson, V.
Britzger, M.
Brooks, A. F.
Brown, D. A.
Brummit, A.
Bulik, T.
Bulten, H. J.
Buonanno, A.
Burguet-Castell, J.
Burmeister, O.
Buskulic, D.
Buy, C.
Byer, R. L.
Cadonati, L.
Cagnoli, G.
Calloni, E.
Camp, J. B.
Campsie, P.
Cannizzo, J.
Cannon, K.
Canuel, B.
Cao, J.
Capano, C. D.
Carbognani, F.
Caride, S.
Caudill, S.
Cavaglia, M.
Cavalier, F.
Cavalieri, R.
Cella, G.
Cepeda, C.
Cesarini, E.
Chaibi, O.
Chalermsongsak, T.
Chalkley, E.
Charlton, P.
Chassande-Mottin, E.
Chelkowski, S.
Chen, Y.
Chincarini, A.
Chiummo, A.
Cho, H.
Christensen, N.
Chua, S. S. Y.
Chung, C. T. Y.
Chung, S.
Ciani, G.
Clara, F.
Clark, D. E.
Clark, J.
Clayton, J. H.
Cleva, F.
Coccia, E.
Cohadon, P. -F.
Colacino, C. N.
Colas, J.
Colla, A.
Colombini, M.
Conte, A.
Conte, R.
Cook, D.
Corbitt, T. R.
Cordier, M.
Cornish, N.
Corsi, A.
Costa, C. A.
Coughlin, M.
Coulon, J. -P.
Couvares, P.
Coward, D. M.
Coyne, D. C.
Creighton, J. D. E.
Creighton, T. D.
Cruise, A. M.
Cumming, A.
Cunningham, L.
Cuoco, E.
Cutler, R. M.
Dahl, K.
Danilishin, S. L.
Dannenberg, R.
D'Antonio, S.
Danzmann, K.
Dattilo, V.
Daudert, B.
Daveloza, H.
Davier, M.
Davies, G.
Daw, E. J.
Day, R.
Dayanga, T.
De Rosa, R.
Debra, D.
Debreczeni, G.
Degallaix, J.
Del Pozzo, W.
del Prete, M.
Dent, T.
Dergachev, V.
DeRosa, R.
DeSalvo, R.
Dhurandhar, S.
Di Fiore, L.
DiGuglielmo, J.
Di Lieto, A.
Di Palma, I.
Di Paolo Emilio, M.
Di Virgilio, A.
Diaz, M.
Dietz, A.
Donovan, F.
Dooley, K. L.
Dorsher, S.
Drago, M.
Drever, R. W. P.
Driggers, J. C.
Du, Z.
Dumas, J. -C.
Dwyer, S.
Eberle, T.
Edgar, M.
Edwards, M.
Effler, A.
Ehrens, P.
Endroczi, G.
Engel, R.
Etzel, T.
Evans, K.
Evans, M.
Evans, T.
Factourovich, M.
Fafone, V.
Fairhurst, S.
Fan, Y.
Farr, B. F.
Farr, W.
Fazi, D.
Fehrmann, H.
Feldbaum, D.
Ferrante, I.
Fidecaro, F.
Finn, L. S.
Fiori, I.
Fisher, R. P.
Flaminio, R.
Flanigan, M.
Foley, S.
Forsi, E.
Forte, L. A.
Fotopoulos, N.
Fournier, J. -D.
Franc, J.
Frasca, S.
Frasconi, F.
Frede, M.
Frei, M.
Frei, Z.
Freise, A.
Frey, R.
Fricke, T. T.
Friedrich, D.
Fritschel, P.
Frolov, V. V.
Fulda, P. J.
Fyffe, M.
Galimberti, M.
Gammaitoni, L.
Ganija, M. R.
Garcia, J.
Garofoli, J. A.
Garufi, F.
Gaspar, M. E.
Gemme, G.
Geng, R.
Genin, E.
Gennai, A.
Gergely, L. A.
Ghosh, S.
Giaime, J. A.
Giampanis, S.
Giardina, K. D.
Giazotto, A.
Gill, C.
Goetz, E.
Goggin, L. M.
Gonzalez, G.
Gorodetsky, M. L.
Gossler, S.
Gouaty, R.
Graef, C.
Granata, M.
Grant, A.
Gras, S.
Gray, C.
Gray, N.
Greenhalgh, R. J. S.
Gretarsson, A. M.
Greverie, C.
Grosso, R.
Grote, H.
Grunewald, S.
Guidi, G. M.
Guido, C.
Gupta, R.
Gustafson, E. K.
Gustafson, R.
Ha, T.
Hage, B.
Hallam, J. M.
Hammer, D.
Hammond, G.
Hanks, J.
Hanna, C.
Hanson, J.
Harms, J.
Harry, G. M.
Harry, I. W.
Harstad, E. D.
Hartman, M. T.
Haughian, K.
Hayama, K.
Hayau, J. -F.
Hayler, T.
Heefner, J.
Heidmann, A.
Heintze, M. C.
Heitmann, H.
Hello, P.
Hendry, M. A.
Heng, I. S.
Heptonstall, A. W.
Herrera, V.
Hewitson, M.
Hild, S.
Hoak, D.
Hodge, K. A.
Holt, K.
Hong, T.
Hooper, S.
Hosken, D. J.
Hough, J.
Howell, E. J.
Hughey, B.
Husa, S.
Huttner, S. H.
Huynh-Dinh, T.
Ingram, D. R.
Inta, R.
Isogai, T.
Ivanov, A.
Izumi, K.
Jacobson, M.
Jang, H.
Jaranowski, P.
Johnson, W. W.
Jones, D. I.
Jones, G.
Jones, R.
Ju, L.
Kalmus, P.
Kalogera, V.
Kamaretsos, I.
Kandhasamy, S.
Kang, G.
Kanner, J. B.
Katsavounidis, E.
Katzman, W.
Kaufer, H.
Kawabe, K.
Kawamura, S.
Kawazoe, F.
Kells, W.
Keppel, D. G.
Keresztes, Z.
Khalaidovski, A.
Khalili, F. Y.
Khazanov, E. A.
Kim, B.
Kim, C.
Kim, D.
Kim, H.
Kim, K.
Kim, N.
Kim, Y. -M.
King, P. J.
Kinsey, M.
Kinzel, D. L.
Kissel, J. S.
Klimenko, S.
Kokeyama, K.
Kondrashov, V.
Kopparapu, R.
Koranda, S.
Korth, W. Z.
Kowalska, I.
Kozak, D.
Kringel, V.
Krishnamurthy, S.
Krishnan, B.
Krolak, A.
Kuehn, G.
Kumar, R.
Kwee, P.
Lam, P. K.
Landry, M.
Lang, M.
Lantz, B.
Lastzka, N.
Lawrie, C.
Lazzarini, A.
Leaci, P.
Lee, C. H.
Lee, H. M.
Leindecker, N.
Leong, J. R.
Leonor, I.
Leroy, N.
Letendre, N.
Li, J.
Li, T. G. F.
Liguori, N.
Lindquist, P. E.
Lockerbie, N. A.
Lodhia, D.
Lorenzini, M.
Loriette, V.
Lormand, M.
Losurdo, G.
Luan, J.
Lubinski, M.
Lueck, H.
Lundgren, A. P.
Macdonald, E.
Machenschalk, B.
MacInnis, M.
Macleod, D. M.
Mageswaran, M.
Mailand, K.
Majorana, E.
Maksimovic, I.
Man, N.
Mandel, I.
Mandic, V.
Mantovani, M.
Marandi, A.
Marchesoni, F.
Marion, F.
Marka, S.
Marka, Z.
Markosyan, A.
Maros, E.
Marque, J.
Martelli, F.
Martin, I. W.
Martin, R. M.
Marx, J. N.
Mason, K.
Masserot, A.
Matichard, F.
Matone, L.
Matzner, R. A.
Mavalvala, N.
Mazzolo, G.
McCarthy, R.
McClelland, D. E.
McGuire, S. C.
McIntyre, G.
McIver, J.
McKechan, D. J. A.
Meadors, G. D.
Mehmet, M.
Meier, T.
Melatos, A.
Melissinos, A. C.
Mendell, G.
Menendez, D.
Mercer, R. A.
Meshkov, S.
Messenger, C.
Meyer, M. S.
Miao, H.
Michel, C.
Milano, L.
Miller, J.
Minenkov, Y.
Mitrofanov, V. P.
Mitselmakher, G.
Mittleman, R.
Miyakawa, O.
Moe, B.
Moesta, P.
Mohan, M.
Mohanty, S. D.
Mohapatra, S. R. P.
Moraru, D.
Moreno, G.
Morgado, N.
Morgia, A.
Mori, T.
Mosca, S.
Mossavi, K.
Mours, B.
Mow-Lowry, C. M.
Mueller, C. L.
Mueller, G.
Mukherjee, S.
Mullavey, A.
Mueller-Ebhardt, H.
Munch, J.
Murphy, D.
Murray, P. G.
Mytidis, A.
Nash, T.
Naticchioni, L.
Nawrodt, R.
Necula, V.
Nelson, J.
Newton, G.
Nishizawa, A.
Nocera, F.
Nolting, D.
Nuttall, L.
Ochsner, E.
O'Dell, J.
Oelker, E.
Ogin, G. H.
Oh, J. J.
Oh, S. H.
Oldenburg, R. G.
O'Reilly, B.
O'Shaughnessy, R.
Osthelder, C.
Ott, C. D.
Ottaway, D. J.
Ottens, R. S.
Overmier, H.
Owen, B. J.
Page, A.
Pagliaroli, G.
Palladino, L.
Palomba, C.
Pan, Y.
Pankow, C.
Paoletti, F.
Papa, M. A.
Parisi, M.
Pasqualetti, A.
Passaquieti, R.
Passuello, D.
Patel, P.
Pedraza, M.
Peiris, P.
Pekowsky, L.
Penn, S.
Peralta, C.
Perreca, A.
Persichetti, G.
Phelps, M.
Pickenpack, M.
Piergiovanni, F.
Pietka, M.
Pinard, L.
Pinto, I. M.
Pitkin, M.
Pletsch, H. J.
Plissi, M. V.
Poggiani, R.
Poeld, J.
Postiglione, F.
Prato, M.
Predoi, V.
Price, L. R.
Prijatelj, M.
Principe, M.
Privitera, S.
Prix, R.
Prodi, G. A.
Prokhorov, L.
Puncken, O.
Punturo, M.
Puppo, P.
Quetschke, V.
Raab, F. J.
Rabeling, D. S.
Racz, I.
Radkins, H.
Raffai, P.
Rakhmanov, M.
Ramet, C. R.
Rankins, B.
Rapagnani, P.
Raymond, V.
Re, V.
Redwine, K.
Reed, C. M.
Reed, T.
Regimbau, T.
Reid, S.
Reitze, D. H.
Ricci, F.
Riesen, R.
Riles, K.
Robertson, N. A.
Robinet, F.
Robinson, C.
Robinson, E. L.
Rocchi, A.
Roddy, S.
Rodriguez, C.
Rodruck, M.
Rolland, L.
Rollins, J.
Romano, J. D.
Romano, R.
Romie, J. H.
Rosinska, D.
Roever, C.
Rowan, S.
Ruediger, A.
Ruggi, P.
Ryan, K.
Ryll, H.
Sainathan, P.
Sakosky, M.
Salemi, F.
Samblowski, A.
Sammut, L.
Sancho de la Jordana, L.
Sandberg, V.
Sankar, S.
Sannibale, V.
Santamaria, L.
Santiago-Prieto, I.
Santostasi, G.
Sassolas, B.
Sathyaprakash, B. S.
Sato, S.
Saulson, P. R.
Savage, R. L.
Schilling, R.
Schlamminger, S.
Schnabel, R.
Schofield, R. M. S.
Schulz, B.
Schutz, B. F.
Schwinberg, P.
Scott, J.
Scott, S. M.
Searle, A. C.
Seifert, F.
Sellers, D.
Sengupta, A. S.
Sentenac, D.
Sergeev, A.
Shaddock, D. A.
Shaltev, M.
Shapiro, B.
Shawhan, P.
Shoemaker, D. H.
Sibley, A.
Siemens, X.
Sigg, D.
Singer, A.
Singer, L.
Sintes, A. M.
Skelton, G.
Slagmolen, B. J. J.
Slutsky, J.
Smith, J. R.
Smith, M. R.
Smith, N. D.
Smith, R. J. E.
Somiya, K.
Sorazu, B.
Soto, J.
Speirits, F. C.
Sperandio, L.
Stefszky, M.
Stein, A. J.
Steinert, E.
Steinlechner, J.
Steinlechner, S.
Steplewski, S.
Stochino, A.
Stone, R.
Strain, K. A.
Strigin, S.
Stroeer, A. S.
Sturani, R.
Stuver, A. L.
Summerscales, T. Z.
Sung, M.
Susmithan, S.
Sutton, P. J.
Swinkels, B.
Tacca, M.
Taffarello, L.
Talukder, D.
Tanner, D. B.
Tarabrin, S. P.
Taylor, J. R.
Taylor, R.
Thomas, P.
Thorne, K. A.
Thorne, K. S.
Thrane, E.
Thuering, A.
Titsler, C.
Tokmakov, K. V.
Toncelli, A.
Tonelli, M.
Torre, O.
Torres, C.
Torrie, C. I.
Tournefier, E.
Travasso, F.
Traylor, G.
Trias, M.
Tseng, K.
Ugolini, D.
Urbanek, K.
Vahlbruch, H.
Vajente, G.
Vallisneri, M.
van den Brand, J. F. J.
Van Den Broeck, C.
van der Putten, S.
van Veggel, A. A.
Vass, S.
Vasuth, M.
Vaulin, R.
Vavoulidis, M.
Vecchio, A.
Vedovato, G.
Veitch, J.
Veitch, P. J.
Veltkamp, C.
Verkindt, D.
Vetrano, F.
Vicere, A.
Villar, A. E.
Vinet, J. -Y.
Vitale, S.
Vitale, S.
Vocca, H.
Vorvick, C.
Vyatchanin, S. P.
Wade, A.
Waldman, S. J.
Wallace, L.
Wan, Y.
Wang, X.
Wang, Z.
Wanner, A.
Ward, R. L.
Was, M.
Wei, P.
Weinert, M.
Weinstein, A. J.
Weiss, R.
Wen, L.
Wen, S.
Wessels, P.
West, M.
Westphal, T.
Wette, K.
Whelan, J. T.
Whitcomb, S. E.
White, D.
Whiting, B. F.
Wilkinson, C.
Willems, P. A.
Williams, H. R.
Williams, L.
Willke, B.
Winkelmann, L.
Winkler, W.
Wipf, C. C.
Wiseman, A. G.
Wittel, H.
Woan, G.
Wooley, R.
Worden, J.
Yablon, J.
Yakushin, I.
Yamamoto, H.
Yamamoto, K.
Yang, H.
Yeaton-Massey, D.
Yoshida, S.
Yu, P.
Yvert, M.
Zadrozny, A.
Zanolin, M.
Zendri, J. -P.
Zhang, F.
Zhang, L.
Zhang, W.
Zhang, Z.
Zhao, C.
Zotov, N.
Zucker, M. E.
Zweizig
CA LIGO Sci Collaboration
Virgo Collaboration
TI All-sky search for periodic gravitational waves in the full S5 LIGO data
SO PHYSICAL REVIEW D
LA English
DT Article
ID SCIENCE RUN; LIMIT
AB We report on an all-sky search for periodic gravitational waves in the frequency band 50-800 Hz and with the frequency time derivative in the range of 0 through -6 x 10(-9) Hz/s. Such a signal could be produced by a nearby spinning and slightly nonaxisymmetric isolated neutron star in our Galaxy. After recent improvements in the search program that yielded a 10x increase in computational efficiency, we have searched in two years of data collected during LIGO's fifth science run and have obtained the most sensitive all-sky upper limits on gravitational-wave strain to date. Near 150 Hz our upper limit on worst-case linearly polarized strain amplitude h(0) is 1 x 10(-24), while at the high end of our frequency range we achieve a worst-case upper limit of 3.8 x 10(-24) for all polarizations and sky locations. These results constitute a factor of 2 improvement upon previously published data. A new detection pipeline utilizing a loosely coherent algorithm was able to follow up weaker outliers, increasing the volume of space where signals can be detected by a factor of 10, but has not revealed any gravitational-wave signals. The pipeline has been tested for robustness with respect to deviations from the model of an isolated neutron star, such as caused by a low-mass or long-period binary companion.
C1 [Abadie, J.; Abbott, B. P.; Abbott, R.; Adhikari, R.; Ajith, P.; Anderson, S. B.; Arai, K.; Araya, M. C.; Betzwieser, J.; Billingsley, G.; Black, E.; Blackburn, J. K.; Bork, R.; Brooks, A. F.; Cepeda, C.; Chalermsongsak, T.; Corsi, A.; Coyne, D. C.; Dannenberg, R.; Daudert, B.; Dergachev, V.; DeSalvo, R.; Driggers, J. C.; Ehrens, P.; Engel, R.; Etzel, T.; Flanigan, M.; Fotopoulos, N.; Gustafson, E. K.; Hanna, C.; Heefner, J.; Heptonstall, A. W.; Hodge, K. A.; Ivanov, A.; Jacobson, M.; Kalmus, P.; Kells, W.; Keppel, D. G.; King, P. J.; Kondrashov, V.; Korth, W. Z.; Kozak, D.; Lazzarini, A.; Lindquist, P. E.; Mageswaran, M.; Mailand, K.; Maros, E.; Marx, J. N.; McIntyre, G.; Meshkov, S.; Nash, T.; Ogin, G. H.; Osthelder, C.; Patel, P.; Pedraza, M.; Phelps, M.; Price, L. R.; Privitera, S.; Robertson, N. A.; Sannibale, V.; Santamaria, L.; Searle, A. C.; Seifert, F.; Sengupta, A. S.; Singer, A.; Singer, L.; Smith, M. R.; Stochino, A.; Taylor, R.; Torrie, C. I.; Vass, S.; Villar, A. E.; Wallace, L.; Wei, P.; Weinstein, A. J.; Whitcomb, S. E.; Willems, P. A.; Yamamoto, H.; Yeaton-Massey, D.; Zhang, L.; Zweizig] LIGO Calif Inst Technol, Pasadena, CA 91125 USA.
[Abbott, T. D.; Smith, J. R.] Calif State Univ Fullerton, Fullerton, CA 92831 USA.
[Abernathy, M.; Barr, B.; Bassiri, R.; Bastarrika, M.; Bell, A. S.; Beveridge, N.; Campsie, P.; Cumming, A.; Cunningham, L.; Edgar, M.; Evans, K.; Gill, C.; Grant, A.; Gray, N.; Hammond, G.; Haughian, K.; Hendry, M. A.; Heng, I. S.; Hild, S.; Hough, J.; Huttner, S. H.; Jones, R.; Kumar, R.; Lawrie, C.; Macdonald, E.; Martin, I. W.; Murray, P. G.; Nawrodt, R.; Nelson, J.; Newton, G.; Pitkin, M.; Plissi, M. V.; Reid, S.; Robertson, N. A.; Rowan, S.; Santiago-Prieto, I.; Scott, J.; Sorazu, B.; Speirits, F. C.; Strain, K. A.; Torrie, C. I.; van Veggel, A. A.; Woan, G.] Univ Glasgow, SUPA, Glasgow G12 8QQ, Lanark, Scotland.
[Accadia, T.; Bebronne, M.; Belletoile, A.; Buskulic, D.; Dietz, A.; Gouaty, R.; Letendre, N.; Marion, F.; Masserot, A.; Mours, B.; Rolland, L.; Tournefier, E.; Verkindt, D.; Yvert, M.] Univ Savoie, Lab Annecy Le Vieux Phys Particules LAPP, CNRS IN2P3, F-74941 Annecy Le Vieux, France.
[Acernese, F.; Barone, F.; Calloni, E.; Conte, R.; Di Fiore, L.; Di Paolo Emilio, M.; Forte, L. A.; Milano, L.; Parisi, M.; Persichetti, G.; Pinto, I. M.; Postiglione, F.; Principe, M.; Romano, R.] Ist Nazl Fis Nucl, Sez Napoli, Naples, Italy.
[Calloni, E.; Milano, L.; Parisi, M.; Persichetti, G.] Univ Naples Federico II, Naples, Italy.
[Acernese, F.; Barone, F.; Romano, R.] Complesso Univ Monte S Angelo, I-80126 Naples, Italy.
[Acernese, F.; Barone, F.; Romano, R.] Univ Salerno, I-84084 Salerno, Italy.
[Adams, C.; Basti, A.; Birch, J.; Bridges, D. O.; Evans, T.; Forsi, E.; Frolov, V. V.; Fyffe, M.; Giaime, J. A.; Giardina, K. D.; Guido, C.; Hanson, J.; Holt, K.; Huynh-Dinh, T.; Katzman, W.; Kinzel, D. L.; Lormand, M.; Meyer, M. S.; Nolting, D.; O'Reilly, B.; Overmier, H.; Ramet, C. R.; Riesen, R.; Roddy, S.; Romie, J. H.; Sellers, D.; Sibley, A.; Stuver, A. L.; Thorne, K. A.; Torres, C.; Traylor, G.; Wen, S.; Wooley, R.; Yakushin, I.] LIGO Livingston Observ, Livingston, LA 70754 USA.
[Affeldt, C.; Allen, B.; Aufmuth, P.; Aulbert, C.; Bauchrowitz, J.; Bertolini, A.; Bock, O.; Bogan, C.; Born, M.; Breyer, J.; Brinkmann, M.; Britzger, M.; Burmeister, O.; Dahl, K.; Danzmann, K.; Degallaix, J.; DiGuglielmo, J.; Di Palma, I.; Eberle, T.; Fehrmann, H.; Frede, M.; Friedrich, D.; Goetz, E.; Gossler, S.; Graef, C.; Grote, H.; Hage, B.; Hewitson, M.; Kaufer, H.; Kawazoe, F.; Khalaidovski, A.; Kim, H.; Kringel, V.; Kuehn, G.; Kwee, P.; Lastzka, N.; Leong, J. R.; Lueck, H.; Machenschalk, B.; Mazzolo, G.; Mehmet, M.; Meier, T.; Mossavi, K.; Mueller-Ebhardt, H.; Pickenpack, M.; Pletsch, H. J.; Poeld, J.; Prijatelj, M.; Prix, R.; Puncken, O.; Roever, C.; Ruediger, A.; Ryll, H.; Salemi, F.; Samblowski, A.; Schilling, R.; Schnabel, R.; Schulz, B.; Shaltev, M.; Steinlechner, J.; Steinlechner, S.; Tarabrin, S. P.; Taylor, J. R.; Thuering, A.; Vahlbruch, H.; Veltkamp, C.; Wanner, A.; Weinert, M.; Wessels, P.; Westphal, T.; Wette, K.; Willke, B.; Winkelmann, L.; Winkler, W.; Wittel, H.; Yamamoto, K.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany.
[Affeldt, C.; Allen, B.; Aufmuth, P.; Aulbert, C.; Bauchrowitz, J.; Bertolini, A.; Bock, O.; Bogan, C.; Born, M.; Breyer, J.; Brinkmann, M.; Britzger, M.; Burmeister, O.; Dahl, K.; Danzmann, K.; Degallaix, J.; DiGuglielmo, J.; Di Palma, I.; Eberle, T.; Fehrmann, H.; Frede, M.; Friedrich, D.; Goetz, E.; Gossler, S.; Graef, C.; Grote, H.; Hage, B.; Hewitson, M.; Kaufer, H.; Kawazoe, F.; Khalaidovski, A.; Kim, H.; Kringel, V.; Kuehn, G.; Kwee, P.; Lastzka, N.; Leong, J. R.; Lueck, H.; Machenschalk, B.; Mazzolo, G.; Mehmet, M.; Meier, T.; Mossavi, K.; Mueller-Ebhardt, H.; Pickenpack, M.; Pletsch, H. J.; Poeld, J.; Prijatelj, M.; Prix, R.; Puncken, O.; Roever, C.; Ruediger, A.; Ryll, H.; Salemi, F.; Samblowski, A.; Schilling, R.; Schnabel, R.; Schulz, B.; Shaltev, M.; Steinlechner, J.; Steinlechner, S.; Tarabrin, S. P.; Taylor, J. R.; Thuering, A.; Vahlbruch, H.; Veltkamp, C.; Wanner, A.; Weinert, M.; Wessels, P.; Westphal, T.; Wette, K.; Willke, B.; Winkelmann, L.; Winkler, W.; Wittel, H.; Yamamoto, K.] Leibniz Univ Hannover, D-30167 Hannover, Germany.
[Allen, B.; Ceron, E. Amador; Anderson, W. G.; Brady, P. R.; Burguet-Castell, J.; Clayton, J. H.; Creighton, J. D. E.; Giampanis, S.; Goggin, L. M.; Hammer, D.; Hughey, B.; Koranda, S.; Mercer, R. A.; Moe, B.; Oldenburg, R. G.; O'Shaughnessy, R.; Papa, M. A.; Siemens, X.; Skelton, G.; Wiseman, A. G.; Yu, P.] Univ Wisconsin, Milwaukee, WI 53201 USA.
[Allen, G. S.; Byer, R. L.; Clark, D. E.; Debra, D.; Herrera, V.; Kim, N.; Lantz, B.; Leindecker, N.; Marandi, A.; Markosyan, A.; Tseng, K.; Urbanek, K.] Stanford Univ, Stanford, CA 94305 USA.
[Amariutei, D.; Arain, M. A.; Ciani, G.; Dooley, K. L.; Feldbaum, D.; Hartman, M. T.; Heintze, M. C.; Klimenko, S.; Martin, R. M.; Mitselmakher, G.; Mueller, C. L.; Mueller, G.; Mytidis, A.; Necula, V.; Ottens, R. S.; Pankow, C.; Reitze, D. H.; Sainathan, P.; Tanner, D. B.; Whiting, B. F.; Williams, L.] Univ Florida, Gainesville, FL 32611 USA.
[Amin, R. S.; Caudill, S.; Costa, C. A.; DeRosa, R.; Effler, A.; Fricke, T. T.; Giaime, J. A.; Gonzalez, G.; Johnson, W. W.; Slutsky, J.; Sung, M.] Louisiana State Univ, Baton Rouge, LA 70803 USA.
[Aston, S. M.; Aylott, B. E.; Chalkley, E.; Chelkowski, S.; Cruise, A. M.; Cutler, R. M.; Freise, A.; Fulda, P. J.; Hallam, J. M.; Kokeyama, K.; Lodhia, D.; Page, A.; Smith, R. J. E.; Vecchio, A.] Univ Birmingham, Birmingham B15 2TT, W Midlands, England.
[Astone, P.; Colla, A.; Colombini, M.; Conte, A.; Frasca, S.; Majorana, E.; Naticchioni, L.; Palomba, C.; Puppo, P.; Rapagnani, P.; Ricci, F.] Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy.
[Colla, A.; Colombini, M.; Conte, A.; Frasca, S.; Naticchioni, L.; Rapagnani, P.; Ricci, F.] Univ Roma La Sapienza, I-00185 Rome, Italy.
[Atkinson, D.; Barker, D.; Barton, M. A.; Batch, J.; Berliner, J. M.; Bland, B.; Clara, F.; Cook, D.; Flanigan, M.; Garcia, J.; Gray, C.; Hanks, J.; Ingram, D. R.; Kawabe, K.; Landry, M.; Lubinski, M.; McCarthy, R.; Mendell, G.; Moraru, D.; Moreno, G.; Raab, F. J.; Radkins, H.; Reed, C. M.; Rodruck, M.; Ryan, K.; Sakosky, M.; Sandberg, V.; Savage, R. L.; Schwinberg, P.; Sigg, D.; Steinert, E.; Thomas, P.; Vorvick, C.; Wilkinson, C.; Worden, J.] LIGO Hanford Observ, Richland, WA 99352 USA.
[Babak, S.; Behnke, B.; Grunewald, S.; Krishnan, B.; Leaci, P.; Moesta, P.; Papa, M. A.; Peralta, C.; Robinson, E. L.; Schutz, B. F.] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany.
[Baker, P.; Cornish, N.] Montana State Univ, Bozeman, MT 59717 USA.
[Ballardin, G.; Canuel, B.; Carbognani, F.; Cavalieri, R.; Chiummo, A.; Colas, J.; Cuoco, E.; Dattilo, V.; Day, R.; Fiori, I.; Genin, E.; Marque, J.; Mohan, M.; Nocera, F.; Paoletti, F.; Pasqualetti, A.; Ruggi, P.; Sentenac, D.; Swinkels, B.; Tacca, M.] European Gravitat Observ, I-56021 Cascina, PI, Italy.
[Ballmer, S.; Brown, D. A.; Capano, C. D.; Couvares, P.; Garofoli, J. A.; Pekowsky, L.; Perreca, A.; Saulson, P. R.; Wei, P.; West, M.] Syracuse Univ, Syracuse, NY 13244 USA.
[Barriga, P.; Blair, D.; Chung, S.; Coward, D. M.; Dumas, J. -C.; Fan, Y.; Gras, S.; Hooper, S.; Howell, E. J.; Ju, L.; Kim, D.; Miao, H.; Susmithan, S.; Wen, L.; Whitcomb, S. E.; Zhang, Z.; Zhao, C.] Univ Western Australia, Crawley, WA 6009, Australia.
[Barsotti, L.; Bodiya, T. P.; Corbitt, T. R.; Donovan, F.; Dwyer, S.; Evans, M.; Foley, S.; Fritschel, P.; Harry, G. M.; Katsavounidis, E.; Kissel, J. S.; MacInnis, M.; Mandel, I.; Mason, K.; Matichard, F.; Mavalvala, N.; Mittleman, R.; Oelker, E.; Sankar, S.; Shapiro, B.; Shoemaker, D. H.; Smith, N. D.; Soto, J.; Stein, A. J.; Vaulin, R.; Waldman, S. J.; Weiss, R.; Wipf, C. C.; Zucker, M. E.] LIGO Massachusetts Inst Technol, Cambridge, MA 02139 USA.
[Barsuglia, M.; Bouhou, B.; Buy, C.; Chassande-Mottin, E.; Granata, M.; Ward, R. L.] Univ Paris Diderot, Lab AstroParticule & Cosmol APC, CNRS IN2P3, CEA DSM IRFU,Observ Paris, F-75013 Paris, France.
[Bartos, I.; Belopolski, I.; Factourovich, M.; Marka, S.; Marka, Z.; Matone, L.; Murphy, D.; Redwine, K.; Rollins, J.] Columbia Univ, New York, NY 10027 USA.
[Basti, A.; Bitossi, M.; Bonelli, L.; Boschi, V.; Braccini, S.; Bradaschia, C.; Cella, G.; Colacino, C. N.; Di Lieto, A.; Di Virgilio, A.; Ferrante, I.; Fidecaro, F.; Frasconi, F.; Gennai, A.; Giazotto, A.; Mantovani, M.; Paoletti, F.; Passaquieti, R.; Passuello, D.; Poggiani, R.; Toncelli, A.; Tonelli, M.; Torre, O.; Vajente, G.] Ist Nazl Fis Nucl, Sez Pisa, Pisa, Italy.
[Basti, A.; Bonelli, L.; Colacino, C. N.; Di Lieto, A.; Ferrante, I.; Fidecaro, F.; Passaquieti, R.; Poggiani, R.; Toncelli, A.; Tonelli, M.; Vajente, G.] Univ Pisa, I-56100 Pisa, Italy.
[Mantovani, M.; Torre, O.] Univ Siena, I-53100 Siena, Italy.
[Bauer, Th S.; Beker, M. G.; Blom, M.; Bulten, H. J.; Del Pozzo, W.; Li, T. G. F.; Rabeling, D. S.; van den Brand, J. F. J.; Van Den Broeck, C.; van der Putten, S.; Vitale, S.] Nikhef, Amsterdam, Netherlands.
[Bulten, H. J.; Rabeling, D. S.; van den Brand, J. F. J.] Vrije Univ Amsterdam, NL-1081 HV Amsterdam, Netherlands.
[Benacquista, M.; Biswas, R.; Creighton, T. D.; Daveloza, H.; Diaz, M.; Grosso, R.; Mohanty, S. D.; Mukherjee, S.; Quetschke, V.; Rakhmanov, M.; Romano, J. D.; Stone, R.; Stroeer, A. S.] Univ Texas Brownsville & Texas Southmost Coll, Brownsville, TX 78520 USA.
[Beyersdorf, P. T.; Cordier, M.] San Jose State Univ, San Jose, CA 95192 USA.
[Bilenko, I. A.; Braginsky, V. B.; Danilishin, S. L.; Gorodetsky, M. L.; Khalili, F. Y.; Mitrofanov, V. P.; Prokhorov, L.; Strigin, S.; Vyatchanin, S. P.] Moscow MV Lomonosov State Univ, Moscow 119992, Russia.
[Bizouard, M. A.; Brisson, V.; Cavalier, F.; Davier, M.; Hello, P.; Robinet, F.; Vavoulidis, M.; Was, M.] Univ Paris 11, LAL, IN2P3, CNRS, F-91898 Orsay, France.
[Loriette, V.; Maksimovic, I.] CNRS, ESPCI, F-75005 Paris, France.
[Blackburn, L.; Camp, J. B.; Cannizzo, J.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Bondarescu, R.; Finn, L. S.; Fisher, R. P.; Kinsey, M.; Kopparapu, R.; Lang, M.; Lundgren, A. P.; Menendez, D.; Owen, B. J.; Titsler, C.; Williams, H. R.] Penn State Univ, University Pk, PA 16802 USA.
[Brillet, A.; Chaibi, O.; Cleva, F.; Coulon, J. -P.; Fournier, J. -D.; Greverie, C.; Heitmann, H.; Man, N.; Regimbau, T.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-06304 Nice, France.
[Bondu, F.; Hayau, J. -F.] Univ Rennes 1, Inst Phys Rennes, CNRS, F-35042 Rennes, France.
[Bonnand, R.; Flaminio, R.; Franc, J.; Galimberti, M.; Michel, C.; Morgado, N.; Pinard, L.; Sassolas, B.] Univ Lyon 1, CNRS, IN2P3, LMA, F-69622 Lyon, France.
[Bose, S.; Dayanga, T.; Ghosh, S.; Steplewski, S.; Talukder, D.] Washington State Univ, Pullman, WA 99164 USA.
[Basti, A.; Bosi, L.; Gammaitoni, L.; Marchesoni, F.; Punturo, M.; Travasso, F.; Vocca, H.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Gammaitoni, L.; Travasso, F.] Univ Perugia, I-06123 Perugia, Italy.
[Branchesi, M.; Cagnoli, G.; Guidi, G. M.; Lorenzini, M.; Losurdo, G.; Martelli, F.; Piergiovanni, F.; Sturani, R.; Vetrano, F.; Vicere, A.] Ist Nazl Fis Nucl, Sez Firenze, I-50019 Sesto Fiorentino, Italy.
[Branchesi, M.; Cesarini, E.; Guidi, G. M.; Martelli, F.; Piergiovanni, F.; Sturani, R.; Vetrano, F.; Vicere, A.] Univ Urbino Carlo Bo, I-61029 Urbino, Italy.
[Brau, J. E.; Frey, R.; Harstad, E. D.; Leonor, I.; Schofield, R. M. S.] Univ Oregon, Eugene, OR 97403 USA.
[Briant, T.; Cohadon, P. -F.; Heidmann, A.] Univ Paris 06, Lab Kastler Brossel, ENS, CNRS, F-75005 Paris, France.
[Brummit, A.; Greenhalgh, R. J. S.; Hayler, T.; O'Dell, J.] Rutherford Appleton Lab, HSIC, Didcot OX11 0QX, Oxon, England.
[Krolak, A.] IM PAN, PL-00956 Warsaw, Poland.
[Bulik, T.] Warsaw Univ, Astron Observ, PL-00478 Warsaw, Poland.
[Bulik, T.; Rosinska, D.] CAMK PAN, PL-716 Warsaw, Poland.
[Jaranowski, P.; Pietka, M.] Bialystok Univ, PL-15424 Bialystok, Poland.
[Krolak, A.; Zadrozny, A.] IPJ, PL-05400 Otwock, Poland.
[Rosinska, D.] Inst Astron, PL-65265 Zielona Gora, Poland.
[Buonanno, A.; Kanner, J. B.; Ochsner, E.; Pan, Y.; Shawhan, P.] Univ Maryland, College Pk, MD 20742 USA.
[Cadonati, L.; Hoak, D.; McIver, J.; Mohapatra, S. R. P.] Univ Massachusetts, Amherst, MA 01003 USA.
[Cavaglia, M.; Rankins, B.] Univ Mississippi, University, MS 38677 USA.
[Cannon, K.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Cao, J.; Du, Z.; Geng, R.; Li, J.; Wan, Y.; Wang, X.; Wang, Z.; Zhang, F.; Zhang, W.] Tsinghua Univ, Beijing 100084, Peoples R China.
[Caride, S.; Gustafson, R.; Meadors, G. D.; Riles, K.] Univ Michigan, Ann Arbor, MI 48109 USA.
[Charlton, P.] Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia.
[Basti, A.; Chen, Y.; Hong, T.; Luan, J.; Ott, C. D.; Somiya, K.; Thorne, K. S.; Vallisneri, M.; Wen, L.; Yang, H.] Caltech CaRT, Pasadena, CA 91125 USA.
[Chincarini, A.; Gemme, G.; Prato, M.] Ist Nazl Fis Nucl, Sez Genova, I-16146 Genoa, Italy.
[Cho, H.; Kim, Y. -M.; Lee, C. H.] Pusan Natl Univ, Pusan 609735, South Korea.
[Christensen, N.; Coughlin, M.; Isogai, T.] Carleton Coll, Northfield, MN 55057 USA.
[Chua, S. S. Y.; Inta, R.; Lam, P. K.; McClelland, D. E.; Miller, J.; Mow-Lowry, C. M.; Mullavey, A.; Scott, S. M.; Shaddock, D. A.; Slagmolen, B. J. J.; Stefszky, M.; Wade, A.] Australian Natl Univ, Canberra, ACT 0200, Australia.
[Chung, C. T. Y.; Melatos, A.; Sammut, L.] Univ Melbourne, Parkville, Vic 3010, Australia.
[Clark, J.; Davies, G.; Dent, T.; Edwards, M.; Fairhurst, S.; Harry, I. W.; Jones, G.; Kamaretsos, I.; Macleod, D. M.; McKechan, D. J. A.; Messenger, C.; Nuttall, L.; Predoi, V.; Robinson, C.; Sathyaprakash, B. S.; Schutz, B. F.; Sutton, P. J.; Veitch, J.] Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales.
[Coccia, E.; D'Antonio, S.; Fafone, V.; Minenkov, Y.; Morgia, A.; Pagliaroli, G.; Palladino, L.; Re, V.; Rocchi, A.; Sperandio, L.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, Rome, Italy.
[Coccia, E.; Fafone, V.; Morgia, A.; Re, V.; Sperandio, L.] Univ Roma Tor Vergata, I-00133 Rome, Italy.
[Di Paolo Emilio, M.; Pagliaroli, G.; Palladino, L.] Univ Aquila, I-67100 Laquila, Italy.
[Conte, R.; Postiglione, F.] Univ Salerno, I-84084 Salerno, Italy.
[Daw, E. J.; White, D.] Univ Sheffield, Sheffield S10 2TN, S Yorkshire, England.
[Debreczeni, G.; Endroczi, G.; Gaspar, M. E.; Racz, I.; Vasuth, M.] RMKI, H-1121 Budapest, Hungary.
[Drago, M.; Liguori, N.; Prodi, G. A.] Ist Nazl Fis Nucl, Grp Collegato Trento, Trento, Italy.
[del Prete, M.; Drago, M.; Liguori, N.; Prodi, G. A.] Univ Trento, I-38050 Povo, Trento, Italy.
[Taffarello, L.; Vedovato, G.; Zendri, J. -P.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Dhurandhar, S.; Gupta, R.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India.
[Dorsher, S.; Kandhasamy, S.; Mandic, V.; Thrane, E.] Univ Minnesota, Minneapolis, MN 55455 USA.
[Drever, R. W. P.; Harms, J.] CALTECH, Pasadena, CA 91125 USA.
[Farr, B. F.; Farr, W.; Fazi, D.; Kalogera, V.; Krishnamurthy, S.; Raymond, V.; Rodriguez, C.; Yablon, J.] Northwestern Univ, Evanston, IL 60208 USA.
[Frei, M.; Matzner, R. A.] Univ Texas Austin, Austin, TX 78712 USA.
[Frei, Z.; Raffai, P.] Eotvos Lorand Univ, H-1117 Budapest, Hungary.
[Ganija, M. R.; Hosken, D. J.; Munch, J.; Ottaway, D. J.; Veitch, P. J.] Univ Adelaide, Adelaide, SA 5005, Australia.
[Gergely, L. A.; Keresztes, Z.] Univ Szeged, H-6720 Szeged, Hungary.
[Gretarsson, A. M.; Vitale, S.; Zanolin, M.] Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA.
[Ha, T.; Oh, J. J.; Oh, S. H.] Natl Inst Math Sci, Taejon 305390, South Korea.
[Hanna, C.] Perimeter Inst Theoret Phys, Toronto, ON N2L 2Y5, Canada.
[Hayama, K.; Izumi, K.; Kawamura, S.; Miyakawa, O.; Mori, T.; Nishizawa, A.; Sato, S.] Natl Astron Observ Japan, Tokyo 1818588, Japan.
[Husa, S.; Sancho de la Jordana, L.; Sintes, A. M.; Trias, M.] Univ Illes Balears, E-07122 Palma De Mallorca, Spain.
[Jang, H.; Kang, G.; Kim, B.] Korea Inst Sci & Technol Informat, Taejon 305806, South Korea.
[Jones, D. I.] Univ Southampton, Southampton SO17 1BJ, Hants, England.
[Khazanov, E. A.; Sergeev, A.] Inst Appl Phys, Nizhnii Novgorod 603950, Russia.
[Kim, C.] Lund Observ, SE-22100 Lund, Sweden.
[Kim, K.] Hanyang Univ, Seoul 133791, South Korea.
[Lee, H. M.] Seoul Natl Univ, Seoul 151742, South Korea.
[Lockerbie, N. A.; Tokmakov, K. V.] Univ Strathclyde, Glasgow G1 1XQ, Lanark, Scotland.
[McGuire, S. C.] Southern Univ, Baton Rouge, LA 70813 USA.
[McGuire, S. C.] A&M Coll, Baton Rouge, LA 70813 USA.
[Melissinos, A. C.] Univ Rochester, Rochester, NY 14627 USA.
[Peiris, P.; Whelan, J. T.] Rochester Inst Technol, Rochester, NY 14623 USA.
[Penn, S.] Hobart & William Smith Coll, Geneva, NY 14456 USA.
[Pinto, I. M.; Principe, M.] Univ Sannio Benevento, I-82100 Benevento, Italy.
[Reed, T.; Zotov, N.] Louisiana Tech Univ, Ruston, LA 71272 USA.
[Santostasi, G.] McNeese State Univ, Lake Charles, LA 70609 USA.
[Schlamminger, S.] Univ Washington, Seattle, WA 98195 USA.
[Summerscales, T. Z.] Andrews Univ, Berrien Springs, MI 49104 USA.
[Ugolini, D.] Trinity Univ, San Antonio, TX 78212 USA.
[Yoshida, S.] SE Louisiana Univ, Hammond, LA 70402 USA.
RP Abadie, J (reprint author), LIGO Calif Inst Technol, Pasadena, CA 91125 USA.
RI Ward, Robert/I-8032-2014; Howell, Eric/H-5072-2014; Ott,
Christian/G-2651-2011; mosca, simona/I-7116-2012; Frasconi,
Franco/K-1068-2016; Pinto, Innocenzo/L-3520-2016; Harms,
Jan/J-4359-2012; Ferrante, Isidoro/F-1017-2012; Travasso,
Flavio/J-9595-2016; Bartos, Imre/A-2592-2017; Cella,
Giancarlo/A-9946-2012; Cesarini, Elisabetta/C-4507-2017; Frey,
Raymond/E-2830-2016; Di Virgilio, Angela Dora Vittoria/E-9078-2015;
Sergeev, Alexander/F-3027-2017; Finn, Lee Samuel/A-3452-2009; Sigg,
Daniel/I-4308-2015; Tacca, Matteo/J-1599-2015; Graef,
Christian/J-3167-2015; Ottaway, David/J-5908-2015; Garufi,
Fabio/K-3263-2015; Shaddock, Daniel/A-7534-2011; Postiglione,
Fabio/O-4744-2015; Rocchi, Alessio/O-9499-2015; Martelli,
Filippo/P-4041-2015; Branchesi, Marica/P-2296-2015; Gehring,
Tobias/A-8596-2016; Heidmann, Antoine/G-4295-2016; Pitkin,
Matthew/I-3802-2013; Miao, Haixing/O-1300-2013; Khazanov,
Efim/B-6643-2014; Salemi, Francesco/F-6988-2014; Nelson,
John/H-7215-2014; Losurdo, Giovanni/K-1241-2014; Lam, Ping
Koy/A-5276-2008; Danilishin, Stefan/K-7262-2012; Canuel,
Benjamin/C-7459-2014; Lee, Chang-Hwan/B-3096-2015; McClelland,
David/E-6765-2010; Vecchio, Alberto/F-8310-2015; Mow-Lowry,
Conor/F-8843-2015; Rapagnani, Piero/J-4783-2012; CONTE,
ANDREA/J-6667-2012; Gemme, Gianluca/C-7233-2008; Bilenko,
Igor/D-5172-2012; Allen, Bruce/K-2327-2012; Chen, Yanbei/A-2604-2013;
Zhao, Chunnong/C-2403-2013; Ju, Li/C-2623-2013; Parisi,
Maria/D-2817-2013; Steinlechner, Sebastian/D-5781-2013; Drago,
Marco/E-7134-2013; Re, Virginia /F-6403-2013; Martin, Iain/A-2445-2010;
Santamaria, Lucia/A-7269-2012; Costa, Cesar/G-7588-2012; Prokhorov,
Leonid/I-2953-2012; Gorodetsky, Michael/C-5938-2008; Punturo,
Michele/I-3995-2012; Strigin, Sergey/I-8337-2012; Cuoco,
Elena/I-8789-2012; Vicere, Andrea/J-1742-2012; Ciani,
Giacomo/G-1036-2011; Mitrofanov, Valery/D-8501-2012; Vyatchanin,
Sergey/J-2238-2012; Puppo, Paola/J-4250-2012; Colla,
Alberto/J-4694-2012; Vocca, Helios/F-1444-2010; Bell, Angus/E-7312-2011;
Acernese, Fausto/E-4989-2010; Toncelli, Alessandra/A-5352-2012;
Gammaitoni, Luca/B-5375-2009; Khalili, Farit/D-8113-2012; Prato,
Mirko/D-8531-2012; Hild, Stefan/A-3864-2010; prodi,
giovanni/B-4398-2010; Hammond, Giles/A-8168-2012; Freise,
Andreas/F-8892-2011; Marchesoni, Fabio/A-1920-2008; Strain,
Kenneth/D-5236-2011;
OI Del Pozzo, Walter/0000-0003-3978-2030; O'Shaughnessy,
Richard/0000-0001-5832-8517; Gray, Norman/0000-0002-1941-9202;
Fairhurst, Stephen/0000-0001-8480-1961; Granata,
Massimo/0000-0003-3275-1186; Aulbert, Carsten/0000-0002-1481-8319; Husa,
Sascha/0000-0002-0445-1971; Di Paolo Emilio,
Maurizio/0000-0002-9558-3610; Vitale, Salvatore/0000-0003-2700-0767;
Guidi, Gianluca/0000-0002-3061-9870; Santamaria,
Lucia/0000-0002-5986-0449; Coccia, Eugenio/0000-0002-6669-5787; Hallam,
Jonathan Mark/0000-0002-7087-0461; Vetrano, Flavio/0000-0002-7523-4296;
Naticchioni, Luca/0000-0003-2918-0730; Nishizawa,
Atsushi/0000-0003-3562-0990; calloni, enrico/0000-0003-4819-3297;
Sorazu, Borja/0000-0002-6178-3198; Stuver, Amber/0000-0003-0324-5735;
Bondu, Francois/0000-0001-6487-5197; Zweizig, John/0000-0002-1521-3397;
Swinkels, Bas/0000-0002-3066-3601; Drago, Marco/0000-0002-3738-2431;
Ward, Robert/0000-0001-5503-5241; Ricci, Fulvio/0000-0001-5475-4447;
Whelan, John/0000-0001-5710-6576; Vedovato,
Gabriele/0000-0001-7226-1320; Howell, Eric/0000-0001-7891-2817; Boschi,
Valerio/0000-0001-8665-2293; Matichard, Fabrice/0000-0001-8982-8418;
Pinto, Innocenzo M./0000-0002-2679-4457; Farr, Ben/0000-0002-2916-9200;
Ott, Christian/0000-0003-4993-2055; mosca, simona/0000-0001-7869-8275;
Frasconi, Franco/0000-0003-4204-6587; Ferrante,
Isidoro/0000-0002-0083-7228; Travasso, Flavio/0000-0002-4653-6156;
Cella, Giancarlo/0000-0002-0752-0338; Cesarini,
Elisabetta/0000-0001-9127-3167; Frey, Raymond/0000-0003-0341-2636; Di
Virgilio, Angela Dora Vittoria/0000-0002-2237-7533; Milano,
Leopoldo/0000-0001-9487-5876; Finn, Lee Samuel/0000-0002-3937-0688;
Sigg, Daniel/0000-0003-4606-6526; Tacca, Matteo/0000-0003-1353-0441;
Graef, Christian/0000-0002-4535-2603; Garufi, Fabio/0000-0003-1391-6168;
Shaddock, Daniel/0000-0002-6885-3494; Postiglione,
Fabio/0000-0003-0628-3796; Rocchi, Alessio/0000-0002-1382-9016;
Martelli, Filippo/0000-0003-3761-8616; Gehring,
Tobias/0000-0002-4311-2593; Heidmann, Antoine/0000-0002-0784-5175;
Pitkin, Matthew/0000-0003-4548-526X; Miao, Haixing/0000-0003-4101-9958;
Nelson, John/0000-0002-6928-617X; Losurdo, Giovanni/0000-0003-0452-746X;
Lam, Ping Koy/0000-0002-4421-601X; Danilishin,
Stefan/0000-0001-7758-7493; Lee, Chang-Hwan/0000-0003-3221-1171;
McClelland, David/0000-0001-6210-5842; Vecchio,
Alberto/0000-0002-6254-1617; Gemme, Gianluca/0000-0002-1127-7406; Allen,
Bruce/0000-0003-4285-6256; Zhao, Chunnong/0000-0001-5825-2401;
Steinlechner, Sebastian/0000-0003-4710-8548; Gorodetsky,
Michael/0000-0002-5159-2742; Punturo, Michele/0000-0001-8722-4485;
Vicere, Andrea/0000-0003-0624-6231; Ciani, Giacomo/0000-0003-4258-9338;
Puppo, Paola/0000-0003-4677-5015; Vocca, Helios/0000-0002-1200-3917;
Bell, Angus/0000-0003-1523-0821; Acernese, Fausto/0000-0003-3103-3473;
Toncelli, Alessandra/0000-0003-4400-8808; Gammaitoni,
Luca/0000-0002-4972-7062; Prato, Mirko/0000-0002-2188-8059; prodi,
giovanni/0000-0001-5256-915X; Marchesoni, Fabio/0000-0001-9240-6793;
Strain, Kenneth/0000-0002-2066-5355; Kanner, Jonah/0000-0001-8115-0577;
PERSICHETTI, GIANLUCA/0000-0001-8424-9791; Freise,
Andreas/0000-0001-6586-9901; Mandel, Ilya/0000-0002-6134-8946; Whiting,
Bernard F/0000-0002-8501-8669; Veitch, John/0000-0002-6508-0713;
Principe, Maria/0000-0002-6327-0628; Papa,
M.Alessandra/0000-0002-1007-5298
FU Australian Research Council; Commonwealth of Australia; Council of
Scientific and Industrial Research of India; Istituto Nazionale di
Fisica Nucleare of Italy; Spanish Ministerio de Educacion y Ciencia;
Conselleria d'Economia Hisenda i Innovacio of the Govern de les Illes
Balears; Netherlands Organisation for Scientific Research; Polish
Ministry of Science and Higher Education; Foundation for Polish Science;
Royal Society; Scottish Funding Council; Scottish Universities Physics
Alliance; The National Aeronautics and Space Administration; Carnegie
Trust; Leverhulme Trust; David and Lucile Packard Foundation; Research
Corporation; Alfred P. Sloan Foundation
FX The authors gratefully acknowledge the support of the United States
National Science Foundation for the construction and operation of the
LIGO Laboratory, the Science and Technology Facilities Council of the
United Kingdom, the Max-Planck-Society, the State of
Niedersachsen/Germany for support of the construction and operation of
the GEO600 detector, and the Italian Istituto Nazionale di Fisica
Nucleare and the French Centre National de la Recherche Scientifique for
the construction and operation of the Virgo detector. The authors also
gratefully acknowledge the support of the research by these agencies and
by the Australian Research Council, the International Science Linkages
program of the Commonwealth of Australia, the Council of Scientific and
Industrial Research of India, the Istituto Nazionale di Fisica Nucleare
of Italy, the Spanish Ministerio de Educacion y Ciencia, the Conselleria
d'Economia Hisenda i Innovacio of the Govern de les Illes Balears, the
Foundation for Fundamental Research on Matter supported by the
Netherlands Organisation for Scientific Research, the Polish Ministry of
Science and Higher Education, the FOCUS Programme of Foundation for
Polish Science, the Royal Society, the Scottish Funding Council, the
Scottish Universities Physics Alliance, The National Aeronautics and
Space Administration, the Carnegie Trust, the Leverhulme Trust, the
David and Lucile Packard Foundation, the Research Corporation, and the
Alfred P. Sloan Foundation. This document has been assigned LIGO
Laboratory Document No. LIGO-P1100029-v36.
NR 24
TC 44
Z9 44
U1 3
U2 33
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1550-7998
EI 1550-2368
J9 PHYS REV D
JI Phys. Rev. D
PD JAN 5
PY 2012
VL 85
IS 2
AR 022001
DI 10.1103/PhysRevD.85.022001
PG 19
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 874WV
UT WOS:000298989700001
ER
PT J
AU Ackermann, M
Ajello, M
Allafort, A
Atwood, WB
Baldini, L
Barbiellini, G
Bastieri, D
Bechtol, K
Bellazzini, R
Berenji, B
Blandford, RD
Bloom, ED
Bonamente, E
Borgland, AW
Bouvier, A
Bregeon, J
Brigida, M
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Caraveo, PA
Casandjian, JM
Cecchi, C
Charles, E
Chekhtman, A
Cheung, CC
Chiang, J
Ciprini, S
Claus, R
Cohen-Tanugi, J
Conrad, J
Cutini, S
de Angelis, A
de Palma, F
Dermer, CD
Digel, SW
Silva, EDE
Drell, PS
Drlica-Wagner, A
Favuzzi, C
Fegan, SJ
Ferrara, EC
Focke, WB
Fortin, P
Fukazawa, Y
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Germani, S
Giglietto, N
Giommi, P
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Grove, JE
Guiriec, S
Gustafsson, M
Hadasch, D
Harding, AK
Hayashida, M
Hughes, RE
Johannesson, G
Johnson, AS
Kamae, T
Katagiri, H
Kataoka, J
Knodlseder, J
Kuss, M
Lande, J
Latronico, L
Lemoine-Goumard, M
Garde, ML
Longo, F
Loparco, F
Lovellette, MN
Lubrano, P
Madejski, GM
Mazziotta, MN
McEnery, JE
Michelson, PF
Mitthumsiri, W
Mizuno, T
Moiseev, AA
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Nakamori, T
Nolan, PL
Norris, JP
Nuss, E
Ohno, M
Ohsugi, T
Okumura, A
Omodei, N
Orlando, E
Ormes, JF
Ozaki, M
Paneque, D
Parent, D
Pesce-Rollins, M
Pierbattista, M
Piron, F
Pivato, G
Porter, TA
Raino, S
Rando, R
Razzano, M
Razzaque, S
Reimer, A
Reimer, O
Reposeur, T
Ritz, S
Romani, RW
Roth, M
Sadrozinski, HFW
Sbarra, C
Schalk, TL
Sgro, C
Siskind, EJ
Spandre, G
Spinelli, P
Strong, AW
Takahashi, H
Takahashi, T
Tanaka, T
Thayer, JG
Thayer, JB
Tibaldo, L
Tinivella, M
Torres, DF
Tosti, G
Troja, E
Uchiyama, Y
Usher, TL
Vandenbroucke, J
Vasileiou, V
Vianello, G
Vitale, V
Waite, AP
Winer, BL
Wood, KS
Wood, M
Yang, Z
Zimmer, S
AF Ackermann, M.
Ajello, M.
Allafort, A.
Atwood, W. B.
Baldini, L.
Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Berenji, B.
Blandford, R. D.
Bloom, E. D.
Bonamente, E.
Borgland, A. W.
Bouvier, A.
Bregeon, J.
Brigida, M.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Caraveo, P. A.
Casandjian, J. M.
Cecchi, C.
Charles, E.
Chekhtman, A.
Cheung, C. C.
Chiang, J.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Conrad, J.
Cutini, S.
de Angelis, A.
de Palma, F.
Dermer, C. D.
Digel, S. W.
do Couto e Silva, E.
Drell, P. S.
Drlica-Wagner, A.
Favuzzi, C.
Fegan, S. J.
Ferrara, E. C.
Focke, W. B.
Fortin, P.
Fukazawa, Y.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Germani, S.
Giglietto, N.
Giommi, P.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Grove, J. E.
Guiriec, S.
Gustafsson, M.
Hadasch, D.
Harding, A. K.
Hayashida, M.
Hughes, R. E.
Johannesson, G.
Johnson, A. S.
Kamae, T.
Katagiri, H.
Kataoka, J.
Knoedlseder, J.
Kuss, M.
Lande, J.
Latronico, L.
Lemoine-Goumard, M.
Garde, M. Llena
Longo, F.
Loparco, F.
Lovellette, M. N.
Lubrano, P.
Madejski, G. M.
Mazziotta, M. N.
McEnery, J. E.
Michelson, P. F.
Mitthumsiri, W.
Mizuno, T.
Moiseev, A. A.
Monte, C.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Nakamori, T.
Nolan, P. L.
Norris, J. P.
Nuss, E.
Ohno, M.
Ohsugi, T.
Okumura, A.
Omodei, N.
Orlando, E.
Ormes, J. F.
Ozaki, M.
Paneque, D.
Parent, D.
Pesce-Rollins, M.
Pierbattista, M.
Piron, F.
Pivato, G.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Razzaque, S.
Reimer, A.
Reimer, O.
Reposeur, T.
Ritz, S.
Romani, R. W.
Roth, M.
Sadrozinski, H. F. -W.
Sbarra, C.
Schalk, T. L.
Sgro, C.
Siskind, E. J.
Spandre, G.
Spinelli, P.
Strong, A. W.
Takahashi, H.
Takahashi, T.
Tanaka, T.
Thayer, J. G.
Thayer, J. B.
Tibaldo, L.
Tinivella, M.
Torres, D. F.
Tosti, G.
Troja, E.
Uchiyama, Y.
Usher, T. L.
Vandenbroucke, J.
Vasileiou, V.
Vianello, G.
Vitale, V.
Waite, A. P.
Winer, B. L.
Wood, K. S.
Wood, M.
Yang, Z.
Zimmer, S.
CA Fermi LAT Collaboration
TI Measurement of Separate Cosmic-Ray Electron and Positron Spectra with
the Fermi Large Area Telescope
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID RADIATION; ENERGIES; RATIO; SPECTROMETER; ASYMMETRY; COMPONENT;
FRACTION; FLIGHT
AB We measured separate cosmic-ray electron and positron spectra with the Fermi Large Area Telescope. Because the instrument does not have an onboard magnet, we distinguish the two species by exploiting Earth's shadow, which is offset in opposite directions for opposite charges due to Earth's magnetic field. We estimate and subtract the cosmic-ray proton background using two different methods that produce consistent results. We report the electron-only spectrum, the positron-only spectrum, and the positron fraction between 20 and 200 GeV. We confirm that the fraction rises with energy in the 20-100 GeV range. The three new spectral points between 100 and 200 GeVare consistent with a fraction that is continuing to rise with energy.
C1 [Ackermann, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wood, M.] Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Porter, T. A.; Reimer, A.; Reimer, O.; Romani, R. W.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Atwood, W. B.; Bouvier, A.; Razzano, M.; Ritz, S.; Sadrozinski, H. F. -W.; Schalk, T. L.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Atwood, W. B.; Bouvier, A.; Razzano, M.; Ritz, S.; Sadrozinski, H. F. -W.; Schalk, T. L.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Buson, S.; Gustafsson, M.; Rando, R.; Sbarra, C.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Pivato, G.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Bruel, P.; Fegan, S. J.; Fortin, P.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Caliandro, G. A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEE CSIC, Barcelona 08193, Spain.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
[Casandjian, J. M.; Grenier, I. A.; Pierbattista, M.] Univ Paris Diderot, CNRS, IRFU, CEA,Lab AIM,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France.
[Chekhtman, A.] Artep Inc, Ellicott City, MD 21042 USA.
[Cheung, C. C.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA.
[Ciprini, S.] ASI Sci Data Ctr, I-00044 Frascati, Roma, Italy.
[Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, Lab Univers & Particules Montpellier, CNRS, IN2P3, Montpellier, France.
[Conrad, J.; Garde, M. Llena; Yang, Z.; Zimmer, S.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden.
[Conrad, J.; Garde, M. Llena; Yang, Z.; Zimmer, S.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Cutini, S.; Gasparrini, D.; Giommi, P.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Frascati, Roma, Italy.
[de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy.
[de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy.
[Dermer, C. D.; Grove, J. E.; Lovellette, M. N.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Ferrara, E. C.; Harding, A. K.; McEnery, J. E.; Moiseev, A. A.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Fukazawa, Y.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan.
[Giroletti, M.; Lemoine-Goumard, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
[Guiriec, S.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan.
[Hughes, R. E.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA.
[Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland.
[Katagiri, H.] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan.
[Kataoka, J.; Nakamori, T.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan.
[Knoedlseder, J.] IRAP, CNRS, F-31028 Toulouse 4, France.
[Knoedlseder, J.] Univ Toulouse, GAHEC, UPS, OMP,IRAP, Toulouse, France.
[Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Lemoine-Goumard, M.; Reposeur, T.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
[McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Moiseev, A. A.] CRESST, Greenbelt, MD 20771 USA.
[Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy.
[Norris, J. P.] Boise State Univ, Dept Phys, Boise, ID 83725 USA.
[Ohno, M.; Okumura, A.; Ozaki, M.; Takahashi, T.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan.
[Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan.
[Orlando, E.; Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA.
[Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
[Parent, D.; Razzaque, S.] George Mason Univ, Ctr Earth Observing & Space Res, Coll Sci, Fairfax, VA 22030 USA.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA.
[Torres, D. F.] ICREA, Barcelona, Spain.
[Vianello, G.] CIFS, I-10133 Turin, Italy.
[Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
EM markus.ackermann@desy.de; funk@slac.stanford.edu;
warit@slac.stanford.edu; carmelo.sgro@pi.infn.it; justinv@stanford.edu
RI Rando, Riccardo/M-7179-2013; Funk, Stefan/B-7629-2015; Loparco,
Francesco/O-8847-2015; Johannesson, Gudlaugur/O-8741-2015; Gargano,
Fabio/O-8934-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario
/O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016;
Orlando, E/R-5594-2016; lubrano, pasquale/F-7269-2012; Morselli,
Aldo/G-6769-2011; Harding, Alice/D-3160-2012; McEnery,
Julie/D-6612-2012; Baldini, Luca/E-5396-2012; Kuss, Michael/H-8959-2012;
giglietto, nicola/I-8951-2012; Reimer, Olaf/A-3117-2013; Tosti,
Gino/E-9976-2013; Ozaki, Masanobu/K-1165-2013
OI Berenji, Bijan/0000-0002-4551-772X; Gasparrini,
Dario/0000-0002-5064-9495; Baldini, Luca/0000-0002-9785-7726; Sgro',
Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Rando,
Riccardo/0000-0001-6992-818X; Zimmer, Stephan/0000-0002-5735-0082;
Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577;
Pesce-Rollins, Melissa/0000-0003-1790-8018; Giroletti,
Marcello/0000-0002-8657-8852; Cutini, Sara/0000-0002-1271-2924; Funk,
Stefan/0000-0002-2012-0080; Loparco, Francesco/0000-0002-1173-5673;
Johannesson, Gudlaugur/0000-0003-1458-7036; Gargano,
Fabio/0000-0002-5055-6395; Moskalenko, Igor/0000-0001-6141-458X;
Mazziotta, Mario /0000-0001-9325-4672; Torres,
Diego/0000-0002-1522-9065; Giordano, Francesco/0000-0002-8651-2394;
giommi, paolo/0000-0002-2265-5003; De Angelis,
Alessandro/0000-0002-3288-2517; Caraveo, Patrizia/0000-0003-2478-8018;
lubrano, pasquale/0000-0003-0221-4806; Morselli,
Aldo/0000-0002-7704-9553; giglietto, nicola/0000-0002-9021-2888; Reimer,
Olaf/0000-0001-6953-1385;
FU European Community [ERC-StG-259391]; K. A. Wallenberg Foundation
FX The Fermi LAT Collaboration acknowledges support from a number of
agencies and institutes for both development and the operation of the
LAT as well as scientific data analysis. These include NASA and DOE in
the United States, CEA/Irfu and IN2P3/CNRS in France, ASI and INFN in
Italy, MEXT, KEK, and JAXA in Japan, and the K. A. Wallenberg
Foundation, the Swedish Research Council and the National Space Board in
Sweden. Additional support from INAF in Italy and CNES in France for
science analysis during the operations phase is also gratefully
acknowledged. M. Lemoine-Goumard is funded by contract ERC-StG-259391
from the European Community. J. Conrad is a Royal Swedish Academy of
Sciences Research Fellow, funded by a grant from the K. A. Wallenberg
Foundation. E. Troja is a NASA Postdoctoral Program Fellow.
NR 39
TC 278
Z9 282
U1 10
U2 31
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
EI 1079-7114
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD JAN 5
PY 2012
VL 108
IS 1
AR 011103
DI 10.1103/PhysRevLett.108.011103
PG 7
WC Physics, Multidisciplinary
SC Physics
GA 874AX
UT WOS:000298928500005
PM 22304252
ER
PT J
AU Poppe, AR
Halekas, JS
Delory, GT
Farrell, WM
Angelopoulos, V
McFadden, JP
Bonnell, JW
Ergun, RE
AF Poppe, A. R.
Halekas, J. S.
Delory, G. T.
Farrell, W. M.
Angelopoulos, V.
McFadden, J. P.
Bonnell, J. W.
Ergun, R. E.
TI A comparison of ARTEMIS observations and particle-in-cell modeling of
the lunar photoelectron sheath in the terrestrial magnetotail
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID SURFACE; PLASMA; THEMIS; MAGNETOSPHERE; ENVIRONMENT; INSTRUMENT;
EMISSIONS; SHADOW; WAVES; PLATE
AB As an airless body in space with no global magnetic field, the Moon is exposed to both solar ultraviolet radiation and ambient plasmas. Photoemission from solar UV radiation and collection of ambient plasma are typically opposing charging currents and simple charging current balance predicts that the lunar dayside surface should charge positively; however, the two ARTEMIS probes have observed energy-dependent loss cones and high-energy, surface-originating electron beams above the dayside lunar surface for extended periods in the magnetosphere, which are indicative of negative surface potentials. In this paper, we compare observations by the ARTEMIS P1 spacecraft with a one-dimensional particle-in-cell simulation and show that the energy-dependent loss cones and electron beams are due to the presence of stable, non-monotonic, negative potentials above the lunar surface. The simulations also show that while the magnitude of the non-monotonic potential is mainly driven by the incoming electron temperature, the incoming ion temperature can alter this magnitude, especially for periods in the plasma sheet when the ion temperature is more than twenty times the electron temperature. Finally, we note several other plasma phenomena associated with these non-monotonic potentials, such as broadband electrostatic noise and electron cyclotron harmonic emissions, and offer possible generation mechanisms for these phenomena. Citation: Poppe, A. R., J. S. Halekas, G. T. Delory, W. M. Farrell, V. Angelopoulos, J. P. McFadden, J. W. Bonnell, and R. E. Ergun (2012), A comparison of ARTEMIS observations and particle-in-cell modeling of the lunar photoelectron sheath in the terrestrial magnetotail, Geophys. Res. Lett., 39, L01102, doi: 10.1029/2011GL050321.
C1 [Poppe, A. R.; Halekas, J. S.; Delory, G. T.; McFadden, J. P.; Bonnell, J. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Angelopoulos, V.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Ergun, R. E.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80303 USA.
[Farrell, W. M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Poppe, A. R.; Halekas, J. S.; Delory, G. T.; Farrell, W. M.] NASA, Lunar Sci Inst, Ames Res Ctr, Mountain View, CA USA.
[Angelopoulos, V.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA.
RP Poppe, AR (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA.
EM poppe@ssl.berkeley.edu
RI Farrell, William/I-4865-2013;
OI Poppe, Andrew/0000-0001-8137-8176; Halekas, Jasper/0000-0001-5258-6128
FU NASA's Lunar Science Institute; NASA [NAS5-02099]
FX The authors gratefully acknowledge support from NASA's Lunar Science
Institute. The ARTEMIS mission was funded and is operated under NASA
grant NAS5-02099. The authors thank E. M. Harnett and another anonymous
reviewer for helpful and constructive comments.
NR 26
TC 18
Z9 18
U1 0
U2 7
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD JAN 4
PY 2012
VL 39
AR L01102
DI 10.1029/2011GL050321
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 874BQ
UT WOS:000298930400005
ER
PT J
AU Swatantran, A
Dubayah, R
Goetz, S
Hofton, M
Betts, MG
Sun, M
Simard, M
Holmes, R
AF Swatantran, Anu
Dubayah, Ralph
Goetz, Scott
Hofton, Michelle
Betts, Matthew G.
Sun, Mindy
Simard, Marc
Holmes, Richard
TI Mapping Migratory Bird Prevalence Using Remote Sensing Data Fusion
SO PLOS ONE
LA English
DT Article
ID SMALL-FOOTPRINT LIDAR; VEGETATION STRUCTURE; QUANTILE REGRESSION;
FOLIAGE STRUCTURE; DECIDUOUS FOREST; HUBBARD-BROOK; NEW-HAMPSHIRE;
HABITAT; CLASSIFICATION; LANDSCAPE
AB Background: Improved maps of species distributions are important for effective management of wildlife under increasing anthropogenic pressures. Recent advances in lidar and radar remote sensing have shown considerable potential for mapping forest structure and habitat characteristics across landscapes. However, their relative efficacies and integrated use in habitat mapping remain largely unexplored. We evaluated the use of lidar, radar and multispectral remote sensing data in predicting multi-year bird detections or prevalence for 8 migratory songbird species in the unfragmented temperate deciduous forests of New Hampshire, USA.
Methodology and Principal Findings: A set of 104 predictor variables describing vegetation vertical structure and variability from lidar, phenology from multispectral data and backscatter properties from radar data were derived. We tested the accuracies of these variables in predicting prevalence using Random Forests regression models. All data sets showed more than 30% predictive power with radar models having the lowest and multi-sensor synergy ("fusion'') models having highest accuracies. Fusion explained between 54% and 75% variance in prevalence for all the birds considered. Stem density from discrete return lidar and phenology from multispectral data were among the best predictors. Further analysis revealed different relationships between the remote sensing metrics and bird prevalence. Spatial maps of prevalence were consistent with known habitat preferences for the bird species.
Conclusion and Significance: Our results highlight the potential of integrating multiple remote sensing data sets using machine-learning methods to improve habitat mapping. Multi-dimensional habitat structure maps such as those generated from this study can significantly advance forest management and ecological research by facilitating fine-scale studies at both stand and landscape level.
C1 [Swatantran, Anu; Dubayah, Ralph; Hofton, Michelle] Univ Maryland, College Pk, MD 20742 USA.
[Goetz, Scott; Sun, Mindy] Woods Hole Res Ctr, Falmouth, MA USA.
[Betts, Matthew G.] Oregon State Univ, Dept Forest Ecosyst & Soc, Corvallis, OR 97331 USA.
[Simard, Marc] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Holmes, Richard] Dartmouth Coll, Hanover, NH 03755 USA.
RP Swatantran, A (reprint author), Univ Maryland, College Pk, MD 20742 USA.
EM aswatan@umd.edu
RI Simard, Marc/H-3516-2013; Goetz, Scott/A-3393-2015; Swatantran,
Anu/B-8786-2016
OI Simard, Marc/0000-0002-9442-4562; Goetz, Scott/0000-0002-6326-4308;
FU NASA [NNX08AP55G, NNX09AK20G]; National Science Foundation
FX The avian ecology research at HBEF has been supported primarily by
multiple grants from the National Science Foundation. Dr. Swatantran,
Dr. Dubayah, Dr. Goetz and Dr. Simard were supported by grants from
NASA's Terrestrial Ecology and Biodiversity Programs (NASA Grants
http://www.nasa.gov/ NNX08AP55G; NNX09AK20G). The funders had no role in
study design, data collection and analysis, decision to publish, or
preparation of the manuscript.
NR 59
TC 30
Z9 30
U1 6
U2 47
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD JAN 3
PY 2012
VL 7
IS 1
AR e28922
DI 10.1371/journal.pone.0028922
PG 11
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 903NK
UT WOS:000301123400015
PM 22235254
ER
PT J
AU Baaklini, GY
AF Baaklini, George Y.
BE Paipetis, AS
Matikas, TE
Aggelis, DG
VanHemelrijck, D
TI Nondestructive evaluation, structural health monitoring and optical
diagnostics at NASA Glenn: A summary
SO EMERGING TECHNOLOGIES IN NON-DESTRUCTIVE TESTING V
LA English
DT Proceedings Paper
CT 5th International Conference on Emerging Technologies in Non-Destructive
Testing (NDT)
CY SEP 19-21, 2011
CL Ioannina, GREECE
SP Univ Ioannina, Dept Mat Sci & Engn
AB The Optical Instrumentation and NDE branch's mission is to compete to be the customer's first choice within the National Aeronautics and Space Administration (NASA) for innovative instrumentation and cost effective solutions in the following research and development challenges: optical flow diagnostics, optical surface diagnostics, space and airborne flight electronics and mobile sensor platforms, nondestructive evaluation and propulsion health monitoring methods, and photonic devices and measurement systems. Our data leads to improved designs, validation and verification of systems performance, increased safety and security and reduced design cycle times for core technologies developed at the Glenn Research Center (GRC) & NASA. For ETNDT5, the focus is on NDE methods development, propulsion health monitoring, optical flow diagnostics, optical surface diagnostics, and thermal barrier coatings (TBCs) for damage assessment in materials and components. The selected accomplishments that are highlighted include technologies pertinent to ETNDT5 with some emphasis on seedling ideas that progressed from the development in the lab to real time aerospace applications.
C1 NASA, Optic Instrumentat & NDE Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Baaklini, GY (reprint author), NASA, Optic Instrumentat & NDE Branch, Glenn Res Ctr, Cleveland, OH 44135 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU CRC PRESS-TAYLOR & FRANCIS GROUP
PI BOCA RATON
PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA
BN 978-0-415-62131-1
PY 2012
BP 3
EP 5
PG 3
WC Materials Science, Multidisciplinary; Materials Science,
Characterization & Testing
SC Materials Science
GA BIF19
UT WOS:000327989800001
ER
PT J
AU Turbiner, D
Young, LE
Meehan, TK
AF Turbiner, Dmitry
Young, Larry E.
Meehan, Tom K.
GP ION
TI PHASED ARRAY GNSS ANTENNA FOR THE FORMOSAT-7/COSMIC-2 RADIO OCCULTATION
MISSION
SO PROCEEDINGS OF THE 25TH INTERNATIONAL TECHNICAL MEETING OF THE SATELLITE
DIVISION OF THE INSTITUTE OF NAVIGATION (ION GNSS 2012)
LA English
DT Proceedings Paper
CT 25th International Technical Meeting of the Satellite-Division of the
Institute-of-Navigation
CY SEP 17-21, 2012
CL Nashville, TN
SP Inst Nav, Satellite Div
AB Future GNSS remote sensing instruments such as the TriG receiver require more capable antennas than those flown on missions such as COSMIC. To maximize the number of ionospheric and atmospheric profiles, the TriG receiver will be capable of tracking legacy and new GPS signals such as L5, L2C and L1C; GLONASS CDMA and Galileo E1 and E5a. There has been an in-house effort at JPL to develop a set of antennas that would provide excellent Radio Occultations performance as well as navigation and ionospheric profiling. This effort is ongoing but near completion for the manufacture and delivery of a set of flight antennas for the FORMOSAT-7/COSMIC-2 mission.
We will present aspects of the design and performance figures of an electronically steerable 12-element phased array to accompany the TriG instrument on COSMIC-2, the next RO mission. We will discuss specific features that help ensure the maximum scientific return. In particular, we designed custom helical elements and a low-loss broadband combiner networks. Also, each individual element is electrically phased in a way that synthesizes a final directivity pattern whose peak gains are distributed along the limb of the Earth.
According to HFSS simulations, we anticipate a realized peak gain of 18dBic and 16dBic at GPS L1 and L2/L5 respectively. This gain drops by 6dB at 55 degree azimuth.
C1 [Turbiner, Dmitry; Young, Larry E.; Meehan, Tom K.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Turbiner, D (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
NR 2
TC 0
Z9 0
U1 0
U2 0
PU INST NAVIGATION
PI WASHINGTON
PA 815 15TH ST NW, STE 832, WASHINGTON, DC 20005 USA
PY 2012
BP 915
EP 916
PG 2
WC Remote Sensing
SC Remote Sensing
GA BIA71
UT WOS:000327163300088
ER
PT J
AU Pi, XQ
Meyer, FJ
Chotoo, K
Freeman, A
Caton, RG
Bridgwood, CT
AF Pi, Xiaoqing
Meyer, Franz J.
Chotoo, Kancham
Freeman, Anthony
Caton, Ronald G.
Bridgwood, Christopher T.
GP ION
TI Impact of Ionospheric Scintillation on Spaceborne SAR Observations
Studied Using GNSS
SO PROCEEDINGS OF THE 25TH INTERNATIONAL TECHNICAL MEETING OF THE SATELLITE
DIVISION OF THE INSTITUTE OF NAVIGATION (ION GNSS 2012)
LA English
DT Proceedings Paper
CT 25th International Technical Meeting of the Satellite-Division of the
Institute-of-Navigation
CY SEP 17-21, 2012
CL Nashville, TN
SP Inst Nav, Satellite Div
AB A survey of artifacts seen in JAXA's Phase Array type L-band Synthetic Aperture Radar (PALSAR) data over South America is reported in this paper. A significant impact on the radar data during a low solar activity year is revealed: about 14% of the surveyed PALSAR images (totally 2779) are affected by the artifacts during a month and the artifacts occur on 74.2% of the surveyed days. The characteristics of the artifacts have led to a consideration that the artifacts are a consequence of ionospheric scintillation. This raises not only a concern about scintillation effects on radar but also a question about active scintillation conditions during a low solar activity year. To assess and verify the scintillation conditions, GPS data collected from the constellation of FORMOSAT-3/COSMIC satellites and three ground-based GPS networks are processed and analyzed. The space and ground GPS data provides a global context and regional dense coverage, respectively, of ionospheric scintillation measurements. It is concluded that even during a low solar activity year, L-band scintillation at low latitudes can occur frequently and affect L-band SAR significantly.
C1 [Pi, Xiaoqing; Freeman, Anthony] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Pi, XQ (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
NR 11
TC 2
Z9 2
U1 0
U2 1
PU INST NAVIGATION
PI WASHINGTON
PA 815 15TH ST NW, STE 832, WASHINGTON, DC 20005 USA
PY 2012
BP 1998
EP 2006
PG 9
WC Remote Sensing
SC Remote Sensing
GA BIA71
UT WOS:000327163302003
ER
PT S
AU Bloem, M
Huang, HY
Bambos, N
AF Bloem, Michael
Huang, Haiyun
Bambos, Nicholas
GP IEEE
TI Approximating the Likelihood of Historical Airline Actions to Evaluate
Airline Delay Cost Functions
SO 2012 IEEE 51ST ANNUAL CONFERENCE ON DECISION AND CONTROL (CDC)
SE IEEE Conference on Decision and Control
LA English
DT Proceedings Paper
CT 51st IEEE Annual Conference on Decision and Control (CDC)
CY DEC 10-13, 2012
CL HI
SP IEEE, Soc Ind & Appl Math, Inst Operat Res Management Sci, Japanese Soc Instrument & Control Engineers, European Union Control Assoc, Int Federat Automat Control, Elsevier, GE Global Res, MathWorks, Springer, Univ Hawaii Manoa, Coll Engn, Univ Texas Dallas, Journal Franklin Inst, Engn & Appl Math, Taylor & Francis Grp, Visual Solut, Wolfram Res
AB Delay cost functions that quantify the cost of delay to airlines are essential to air traffic management research. Seventeen delay cost functions from previous research are evaluated with airline actions in Airspace Flow Programs. Airlines are assumed to solve a minimum cost perfect matching problem when matching flights to slots. Unobserved aspects of airline costs are accounted for by adding a noise term to the cost functions. The goal of this research is to find the cost function and corresponding noise parameters that maximize the likelihood of airline actions during 32 Airspace Flow Programs in the summer of 2006. A heuristic is developed that finds cost noise parameters that maximize an approximation of the log-likelihood of the airline actions. When applied to sample estimation problem instances generated by solving linear programming problems with known noise parameters, the heuristic can more accurately estimate noise parameters than a simple simulation-based approach. Validation efforts based on synthetic airline action data generated with known delay cost functions and noise parameters demonstrate that the heuristic is in many cases able to correctly identify as most likely the delay cost function that was in fact used to generate the synthetic data. However, the heuristic also under-estimates the magnitude of the cost noise variance on these estimation problem instances. Delay costs that are proportional to the length of delay, but with larger proportionality constants for flights bound for hub airports, maximize the approximation of the log-likelihood of the historical airline actions. The estimated standard deviations of the cost noise, expressed as a fraction of the average assignment cost for the historical matchings, ranged from 0.1 to 0.7 for cost functions that achieved relatively large approximate log-likelihoods.
C1 [Bloem, Michael] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Bloem, M (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM michael.bloem@nasa.gov; h.huang@student.tudelft.nl; bambos@stanford.edu
NR 12
TC 0
Z9 0
U1 1
U2 2
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 0191-2216
BN 978-1-4673-2066-5
J9 IEEE DECIS CONTR P
PY 2012
BP 508
EP 513
PG 6
WC Automation & Control Systems; Computer Science, Artificial Intelligence;
Engineering, Electrical & Electronic
SC Automation & Control Systems; Computer Science; Engineering
GA BIB20
UT WOS:000327200400084
ER
PT S
AU Kuwata, Y
Pavone, M
Balaram, J
AF Kuwata, Yoshiaki
Pavone, Marco
Balaram, J. (Bob)
GP IEEE
TI A Risk-Constrained Multi-Stage Decision Making Approach to the
Architectural Analysis of Planetary Missions
SO 2012 IEEE 51ST ANNUAL CONFERENCE ON DECISION AND CONTROL (CDC)
SE IEEE Conference on Decision and Control
LA English
DT Proceedings Paper
CT 51st IEEE Annual Conference on Decision and Control (CDC)
CY DEC 10-13, 2012
CL HI
SP IEEE, Soc Ind & Appl Math, Inst Operat Res Management Sci, Japanese Soc Instrument & Control Engineers, European Union Control Assoc, Int Federat Automat Control, Elsevier, GE Global Res, MathWorks, Springer, Univ Hawaii Manoa, Coll Engn, Univ Texas Dallas, Journal Franklin Inst, Engn & Appl Math, Taylor & Francis Grp, Visual Solut, Wolfram Res
ID MARS
AB This paper presents a novel risk-constrained multi-stage decision making approach to the architectural analysis of planetary rover missions. In particular, focusing on a 2018 Mars rover concept, which was considered as part of a potential Mars Sample Return campaign, we model the entry, descent, and landing (EDL) phase and the rover traverse phase as four sequential decision-making stages. The problem is to find a sequence of divert and driving maneuvers so that the rover drive is minimized and the probability of a mission failure (e. g., due to a failed landing) is below a user-specified bound. By solving this problem for several different values of the model parameters (e. g., divert authority), this approach enables rigorous, accurate and systematic trade-offs for the EDL system vs. the mobility system, and, more in general, cross-domain trade-offs for the different phases of a space mission. The overall optimization problem can be seen as a chance-constrained dynamic programming problem, with the additional complexity that 1) in some stages the disturbances do not have any probabilistic characterization, and 2) the state space is extremely large (i.e, hundreds of millions of states for trade-offs with high-resolution Martian maps). To this purpose, we solve the problem by performing an unconventional combination of average and minimax cost analysis and by leveraging high efficient computation tools from the image processing community. Preliminary trade-off results are presented.
C1 [Kuwata, Yoshiaki; Balaram, J. (Bob)] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Kuwata, Y (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM Yoshiaki.Kuwata@jpl.nasa.gov; pavone@stanford.edu;
J.Balaram@jpl.nasa.gov
NR 11
TC 1
Z9 1
U1 0
U2 3
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 0191-2216
BN 978-1-4673-2066-5
J9 IEEE DECIS CONTR P
PY 2012
BP 2102
EP 2109
PG 8
WC Automation & Control Systems; Computer Science, Artificial Intelligence;
Engineering, Electrical & Electronic
SC Automation & Control Systems; Computer Science; Engineering
GA BIB20
UT WOS:000327200402078
ER
PT S
AU Stepanyan, V
Krishnakumar, K
AF Stepanyan, Vahram
Krishnakumar, Kalmanje
GP IEEE
TI Certainty Equivalence M-MRAC for Systems with Unmatched Uncertainties
SO 2012 IEEE 51ST ANNUAL CONFERENCE ON DECISION AND CONTROL (CDC)
SE IEEE Conference on Decision and Control
LA English
DT Proceedings Paper
CT 51st IEEE Annual Conference on Decision and Control (CDC)
CY DEC 10-13, 2012
CL HI
SP IEEE, Soc Ind & Appl Math, Inst Operat Res Management Sci, Japanese Soc Instrument & Control Engineers, European Union Control Assoc, Int Federat Automat Control, Elsevier, GE Global Res, MathWorks, Springer, Univ Hawaii Manoa, Coll Engn, Univ Texas Dallas, Journal Franklin Inst, Engn & Appl Math, Taylor & Francis Grp, Visual Solut, Wolfram Res
AB The paper presents a certainty equivalence state feedback indirect adaptive control design method for the systems of any relative degree with unmatched uncertainties. The approach is based on the parameter identification (estimation) model, which is completely separated from the control design and is capable of producing parameter estimates as fast as the computing power allows without generating high frequency oscillations. It is shown that the system's input and output tracking errors can be systematically decreased by the proper choice of the design parameters.
C1 [Stepanyan, Vahram] NASA, Ames Res Ctr, Mission Crit Technol Inc, Moffett Field, CA 94035 USA.
RP Stepanyan, V (reprint author), NASA, Ames Res Ctr, Mission Crit Technol Inc, Moffett Field, CA 94035 USA.
EM vahram.stepanyan@nasa.gov; kalmanje.krishnakumar@nasa.gov
NR 5
TC 2
Z9 2
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 0191-2216
BN 978-1-4673-2066-5
J9 IEEE DECIS CONTR P
PY 2012
BP 4152
EP 4157
PG 6
WC Automation & Control Systems; Computer Science, Artificial Intelligence;
Engineering, Electrical & Electronic
SC Automation & Control Systems; Computer Science; Engineering
GA BIB20
UT WOS:000327200404079
ER
PT S
AU Li, SR
De Geronimo, G
Chen, W
D' Anadragora, A
Fried, J
Li, Z
Pinelli, DA
Smith, GC
Gaskin, JA
Ramsey, BD
AF Li, Shaorui
De Geronimo, Gianluigi
Chen, Wei
D' Anadragora, Alessio
Fried, Jack
Li, Zheng
Pinelli, Donald A.
Smith, Graham C.
Gaskin, Jessica A.
Ramsey, Brian D.
BE Yu, B
TI A Low-Power, Radiation-Resistant ASIC for SDD-Based X-Ray Spectrometers
SO 2012 IEEE NUCLEAR SCIENCE SYMPOSIUM AND MEDICAL IMAGING CONFERENCE
RECORD (NSS/MIC)
SE IEEE Nuclear Science Symposium Conference Record
LA English
DT Proceedings Paper
CT IEEE Nuclear Science Symposium / Medical Imaging Conference Record
(NSS/MIC) / 19th Room-Temperature Semiconductor X-ray and Gamma-ray
Detector Workshop
CY OCT 29-NOV 03, 2012
CL Anaheim, CA
SP IEEE, IEEE Nucl & Plasma Sci Soc
ID CMOS TECHNOLOGIES
AB We present an Application Specific Integrated Circuit (ASIC) for high resolution x-ray spectrometers (XRS) in radiation harsh environment (such as Jovian system). The ASIC was designed to read out signals from low resistivity pixelated Silicon-Drift- Detectors (SDD) to ensure radiation hardness. The readout is done by wire-bonding the anodes to the inputs of the ASIC. The ASIC dissipates 32 mW and provides 16 channels of low-noise charge amplification, high-order shaping with baseline stabilization, discrimination, pile-up rejection, and peak detection with analog memory. The readout is sparse and based on a custom low-power tristatable low-voltage differential signaling. A unit of 64 SDD pixels, read out by four ASICs, covers an area of 12.8 cm(2), and dissipates less than 20 mW/cm(2.) The ASICs were powered on and irradiated using a beam line with 200 MeV protons, to doses ranging from 0.25 Mrad to 12 Mrad. Performance degradation due to radiation-induced leakage current was observed to peak around 2 Mrad dose. Critical contributors to the degradation were identified through simulation and measurements, and corresponding circuitry was modified to address the issues. Measurements on the radiation-resistant design have shown excellent radiation resistance at doses from 1 to 8 Mrad.
C1 [Li, Shaorui; De Geronimo, Gianluigi; Chen, Wei; D' Anadragora, Alessio; Fried, Jack; Li, Zheng; Pinelli, Donald A.; Smith, Graham C.] Brookhaven Natl Lab, Upton, NY 11973 USA.
[Gaskin, Jessica A.; Ramsey, Brian D.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Li, SR (reprint author), Brookhaven Natl Lab, Upton, NY 11973 USA.
EM shaoruili@bnl.gov
FU U.S. Department of Energy [DE-AC02-98CH10886]; NASA Research
Opportunities in Space and Earth Science, Planetary Instrument
Definition and Development Program
FX This work was supported in part by the U.S. Department of Energy under
Contract DE-AC02-98CH10886, and in part by the NASA Research
Opportunities in Space and Earth Science, Planetary Instrument
Definition and Development Program.
NR 7
TC 1
Z9 1
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 1082-3654
BN 978-1-4673-2030-6; 978-1-4673-2028-3
J9 IEEE NUCL SCI CONF R
PY 2012
BP 371
EP 375
PG 5
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA BHW16
UT WOS:000326814200081
ER
PT S
AU Chen, W
De Geronimo, G
Gaskin, JA
Li, S
Li, Z
Ramsey, BD
Smith, G
AF Chen, W.
De Geronimo, G.
Gaskin, J. A.
Li, S.
Li, Z.
Ramsey, B. D.
Smith, G.
BE Yu, B
TI Development of Low-resistivity Silicon Drift Detector Arrays for Soft
X-rays
SO 2012 IEEE NUCLEAR SCIENCE SYMPOSIUM AND MEDICAL IMAGING CONFERENCE
RECORD (NSS/MIC)
SE IEEE Nuclear Science Symposium Conference Record
LA English
DT Proceedings Paper
CT IEEE Nuclear Science Symposium / Medical Imaging Conference Record
(NSS/MIC) / 19th Room-Temperature Semiconductor X-ray and Gamma-ray
Detector Workshop
CY OCT 29-NOV 03, 2012
CL Anaheim, CA
SP IEEE, IEEE Nucl & Plasma Sci Soc
ID SPECTROMETERS
AB New silicon drift detector (SDD) arrays are being developed for use as extraterrestrial X-ray spectrometers. For the first time these SDDs have been produced on low resistivity, n-type silicon, with a thinner thickness than normal, effectively ensuring their radiation hardness in anticipation of operation in potentially harsh radiation environments (such as those found around Jupiter). To achieve low-energy X-ray response, a thin entrance window was produced using a double implantation technology. The design, fabrication and performance of these detectors are presented here.
C1 [Chen, W.; De Geronimo, G.; Li, S.; Li, Z.; Smith, G.] Brookhaven Natl Lab, Upton, NY 11973 USA.
[Gaskin, J. A.; Ramsey, B. D.] NASA, MSFC, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA.
RP Chen, W (reprint author), Brookhaven Natl Lab, Upton, NY 11973 USA.
EM weichen@bnl.gov
FU U.S. Department of Energy [DE-AC02-98CHI0886]; NASA
FX This work was supported in part by the U.S. Department of Energy under
Contract No. DE-AC02-98CHI0886 and also was funded in part by the NASA
Research Opportunities in Space and Earth Science, Planetary Instrument
Defmition and Development Program.
NR 13
TC 2
Z9 2
U1 0
U2 1
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 1082-3654
BN 978-1-4673-2030-6; 978-1-4673-2028-3
J9 IEEE NUCL SCI CONF R
PY 2012
BP 931
EP 935
PG 5
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA BHW16
UT WOS:000326814201014
ER
PT S
AU Hong, J
Allen, B
Grindlay, J
Rodrigues, B
Ellis, JR
Baker, R
Barthelmy, S
Mao, P
Miyasaka, H
Apple, J
AF Hong, Jaesub
Allen, Branden
Grindlay, Jonathan
Rodrigues, Barbara
Ellis, Jon Robert
Baker, Robert
Barthelmy, Scott
Mao, Peter
Miyasaka, Hiromasa
Apple, Jeff
BE Yu, B
TI Tiled Array of Pixelated CZT Imaging Detectors for ProtoEXIST2 and
MIRAX-HXI
SO 2012 IEEE NUCLEAR SCIENCE SYMPOSIUM AND MEDICAL IMAGING CONFERENCE
RECORD (NSS/MIC)
SE IEEE Nuclear Science Symposium Conference Record
LA English
DT Proceedings Paper
CT IEEE Nuclear Science Symposium / Medical Imaging Conference Record
(NSS/MIC) / 19th Room-Temperature Semiconductor X-ray and Gamma-ray
Detector Workshop
CY OCT 29-NOV 03, 2012
CL Anaheim, CA
SP IEEE, IEEE Nucl & Plasma Sci Soc
AB We have assembled a tiled array (220 cm(2)) of fine pixel (0.6 mm) imaging CZT detectors for a balloon borne wide-field hard X-ray telescope, ProtoEXIST2. ProtoEXIST2 is a prototype experiment for a next generation hard X-ray imager MIRAX-HXI on board Lattes, a spacecraft from the Agencia Espacial Brasilieira. MIRAX will survey the 5 to 200 keV sky of Galactic bulge, adjoining southern Galactic plane and the extragalactic sky with 6' angular resolution. This survey will open a vast discovery space in timing studies of accretion neutron stars and black holes. The ProtoEXIST2 CZT detector plane consists of 64 of 5 mm thick 2 cm x 2 cm CZT crystals tiled with a minimal gap. MIRAX will consist of 4 such detector planes, each of which will be imaged with its own coded-aperture mask. We present the packaging architecture and assembly procedure of the ProtoEXIST2 detector. On 2012, Oct 10, we conducted a successful high altitude balloon experiment of the ProtoEXIST1 and 2 telescopes, which demonstrates their technology readiness for space application. Both telescopes performed flawlessly during the flight as well as on the ground. We report the results of pre-flight ground calibration and the preliminary results for the detector performance in the balloon flight.
C1 [Hong, Jaesub; Allen, Branden; Grindlay, Jonathan; Ellis, Jon Robert] Harvard Smithsonian Ctr Astrophys CfA, 60 Garden St, Cambridge, MA 02138 USA.
[Rodrigues, Barbara] Inst Nacl Pesquisas Espaciais, Sao Jose Dos Campos, SP, Brazil.
[Baker, Robert; Barthelmy, Scott] Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Mao, Peter; Miyasaka, Hiromasa] CALTECH, Pasadena, CA 91125 USA.
[Apple, Jeff] Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
RP Hong, J (reprint author), Harvard Smithsonian Ctr Astrophys CfA, 60 Garden St, Cambridge, MA 02138 USA.
EM jaesub@head.cfa.harvard.edu
FU NASA [NNX09AD96G, NNX11AF35G]
FX This work was supported by NASA grants NNX09AD96G and NNX11AF35G.
NR 10
TC 0
Z9 0
U1 0
U2 1
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 1082-3654
BN 978-1-4673-2030-6; 978-1-4673-2028-3
J9 IEEE NUCL SCI CONF R
PY 2012
BP 4205
EP 4211
PG 7
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA BHW16
UT WOS:000326814204063
ER
PT J
AU Gunapala, SD
Rafol, SB
Ting, DZ
Soibel, A
Liu, JK
Khoshakhlagh, A
Keo, SA
Mumolo, JM
AF Gunapala, S. D.
Rafol, S. B.
Ting, D. Z.
Soibel, A.
Liu, J. K.
Khoshakhlagh, A.
Keo, S. A.
Mumolo, J. M.
GP IEEE
TI High Performance GaSb/InAs Superlattice Long-Wave Infrared Focal Plane
Array
SO 2012 PHOTONICS GLOBAL CONFERENCE (PGC)
LA English
DT Proceedings Paper
CT Photonics Global Conference (PGC)
CY DEC 13-16, 2012
CL Singapore, SINGAPORE
DE superlattices; infrared detectors; focal plane arrays
AB We describe the demonstration of a 1/4 VGA format long-wavelength infrared focal plane array based on an InAs/GaSb superlattice absorber surrounded by an electron-blocking and a hole-blocking unipolar barrier. An 8.8 mu m cutoff focal plane without antireflection coating based on this complementary barrier infrared detector design has yielded noise equivalent differential temperature of 18.6 mK at operating temperature of 80 K, with 300 K background and f/2 cold-stop.
C1 [Gunapala, S. D.; Rafol, S. B.; Ting, D. Z.; Soibel, A.; Liu, J. K.; Khoshakhlagh, A.; Keo, S. A.; Mumolo, J. M.] CALTECH, Jet Prop Lab, Ctr Infrared Sensors, Pasadena, CA 91109 USA.
RP Gunapala, SD (reprint author), CALTECH, Jet Prop Lab, Ctr Infrared Sensors, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 10
TC 0
Z9 0
U1 0
U2 1
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4673-2516-5
PY 2012
PG 4
WC Engineering, Electrical & Electronic; Optics; Imaging Science &
Photographic Technology
SC Engineering; Optics; Imaging Science & Photographic Technology
GA BHE75
UT WOS:000325203600106
ER
PT S
AU Aumann, HH
Elliott, D
Strow, LL
AF Aumann, H. H.
Elliott, D.
Strow, L. L.
BE Butler, JJ
Xiong, X
Gu, X
TI Validation of the Radiometric Stability of the Atmospheric Infrared
Sounder
SO EARTH OBSERVING SYSTEMS XVII
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Earth Observing Systems XVII
CY AUG 13-16, 2012
CL San Diego, CA
SP SPIE
DE Climate; CO2; N2O; Calibration; hyper-spectral; infrared
AB It has been widely accepted that an infrared sounder in low polar orbit is capable of producing climate quality data, if the spectral brightness temperatures have instrumental trends of less than 10 mK/yr. Achieving measurement stability at this level is not only very demanding of the design of the instrument, it is also pushes the state of art of measuring on orbit what stability is actually achieved. We discuss this using Atmospheric Infrared Sounder (AIRS) L1B data collected between 2002 and 2011. We compare the L1B brightness temperature observed in cloud filtered night tropical ocean spectra (obs) to the brightness temperature calculated based on the known surface emissivity, temperature and water vapor profiles from the ECMWF ReAnalysis (ERA) and the growth rates of CO2, N2O and Ozone. The trend in (obs-calc) is a powerful tool for the evaluation of the stability of the 2378 AIRS channels. We divided the channels into seven classes: All channels which sound in the stratosphere (at pressure levels below 150 hPa), 14 um CO2 sounding, 4 um CO2 P-branch sounding, 4um CO2 R-branch sounding, water vapor sounding, shortwave surface sounding and longwave surface sounding. The peak in the weighting function at 1050 hPa separates sounding and surface channels. The boundary between shortwave and longwave is 5 mu m. Except for the stratosphere sounding channels, the remaining six groups have (obs-calc) trends of less than 20 mK/yr. The longwave surface channels have trends of 2 mK/yr, significantly less than the 8 mK/yr trend seem in the shortwave window channels. Based on the design of the instrument, trends within a group of channels should be the same. While the longwave and shortwave trends are less than the canonical 10 mK/yr, the larger trend in the shortwave channels could be an artifact of using the pre-launch determined calibration coefficients. This is currently under evaluation. The trend in (obs-calc) for the non-surface sounding channels, in particular for stratosphere sounding and upper tropospheric water channels, is dominated by artifacts created in calc, most likely due to changes in the ERA Ozone and water vapor. Based on this argument the best estimate of the trend for the channels within a channel group is given by the surface sensitive channels within the group. Based on this consideration we estimated the trend of all AIRS longwave channels as 2 mK/yr, while the shortwave channels have a trend of 8 mK/yr.
C1 [Aumann, H. H.; Elliott, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Aumann, HH (reprint author), CALTECH, Jet Prop Lab, 4900 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Aumann@jpl.nasa.gov
NR 5
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-9227-2
J9 PROC SPIE
PY 2012
VL 8510
AR 85100T
DI 10.1117/12.929979
PG 8
WC Instruments & Instrumentation; Remote Sensing; Optics
SC Instruments & Instrumentation; Remote Sensing; Optics
GA BHU72
UT WOS:000326699000028
ER
PT S
AU Butler, JJ
Xiong, XX
Barnes, RA
Patt, FS
Sun, JQ
Chiang, KF
AF Butler, James J.
Xiong, Xiaoxiong
Barnes, Robert A.
Patt, Frederick S.
Sun, Junqiang
Chiang, Kwofu
BE Butler, JJ
Xiong, X
Gu, X
TI An overview of Suomi NPP VIIRS calibration maneuvers
SO EARTH OBSERVING SYSTEMS XVII
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Earth Observing Systems XVII
CY AUG 13-16, 2012
CL San Diego, CA
SP SPIE
DE VIIRS; SNPP; maneuvers; on-orbit calibration; characterization
ID MODIS; ORBIT; SEAWIFS; MOON
AB The first Visible Infrared Imager Radiometer Suite (VIIRS) instrument was successfully launched on-board the Suomi National Polar-orbiting Partnership (SNPP) spacecraft on October 28, 2011. Suomi NPP VIIRS observations are made in 22 spectral bands, from the visible (VIS) to the long-wave infrared (LWIR), and are used to produce 22 Environmental Data Records (EDRs) with a broad range of scientific applications. The quality of these VIIRS EDRs strongly depends on the quality of its calibrated and geo-located Sensor Date Records (SDRs). Built with a strong heritage to the NASA's EOS MODerate resolution Imaging Spectroradiometer (MODIS) instrument, the VIIRS is calibrated on-orbit using a similar set of on-board calibrators (OBC), including a solar diffuser (SD) and solar diffuser stability monitor (SDSM) system for the reflective solar bands (RSB) and a blackbody (BB) for the thermal emissive bands (TEB). On-orbit maneuvers of the SNPP spacecraft provide additional calibration and characterization data from the VIIRS instrument which cannot be obtained pre-launch and are required to produce the highest quality SDRs. These include multi-orbit yaw maneuvers for the characterization of SD and SDSM screen transmission, quasi-monthly roll maneuvers to acquire lunar observations to track sensor degradation in the visible through shortwave infrared, and a driven pitch-over maneuver to acquire multiple scans of deep space to determine TEB response versus scan angle (RVS). This paper provides an overview of these three SNPP calibration maneuvers. Discussions are focused on their potential calibration and science benefits, pre-launch planning activities, and on-orbit scheduling and implementation strategies. Results from calibration maneuvers performed during the Intensive Calibration and Validation (ICV) period for the VIIRS sensor are illustrated. Also presented in this paper are lessons learned regarding the implementation of calibration spacecraft maneuvers on follow-on missions.
C1 [Butler, James J.] NASA Goddard Space Flight Ctr, Div Earth Sci, Biospher Sci Lab, Greenbelt, MD 20661 USA.
RP Butler, JJ (reprint author), NASA Goddard Space Flight Ctr, Div Earth Sci, Biospher Sci Lab, Code 618, Greenbelt, MD 20661 USA.
EM James.J.Butler@nasa.gov
RI Butler, James/D-4188-2013
NR 18
TC 7
Z9 7
U1 1
U2 5
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-9227-2
J9 PROC SPIE
PY 2012
VL 8510
AR 85101J
DI 10.1117/12.930993
PG 13
WC Instruments & Instrumentation; Remote Sensing; Optics
SC Instruments & Instrumentation; Remote Sensing; Optics
GA BHU72
UT WOS:000326699000051
ER
PT S
AU Elliott, DA
Aumann, HH
AF Elliott, Denis A.
Aumann, H. H.
BE Butler, JJ
Xiong, X
Gu, X
TI Relative trends of AIRS and IASI radiometric calibrations
SO EARTH OBSERVING SYSTEMS XVII
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Earth Observing Systems XVII
CY AUG 13-16, 2012
CL San Diego, CA
SP SPIE
DE hyperspectral; infrared; sounder; calibration; AIRS; IASI
AB This study examines relative trends in the radiometric calibrations of AIRS and IASI. The stability of the AIRS calibration in window channels over tropical oceans has been shown to be 5 mK/yr or better using 9 years of data. IASI data have been available for five years, and during IASI's time in operation there have been significant El Nino and La Nina events. Those events introduce uncertainty into trend determinations that are more significant for IASI because of its shorter time in operation. When IASI and AIRS are directly compared in a double difference, the El Nino / La Nina effects cancel, allowing for an improved measurement of any instrumental trends in IASI over what can be done using IASI data alone. We find no significant relative trend between the two instruments. We do, however, find some data incompleteness effects for IASI that could introduce spurious trends over certain areas if ignored.
C1 [Elliott, Denis A.; Aumann, H. H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Elliott, DA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 6
TC 0
Z9 0
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-9227-2
J9 PROC SPIE
PY 2012
VL 8510
AR 85100S
DI 10.1117/12.930045
PG 9
WC Instruments & Instrumentation; Remote Sensing; Optics
SC Instruments & Instrumentation; Remote Sensing; Optics
GA BHU72
UT WOS:000326699000027
ER
PT S
AU Iona, G
Butler, J
Guenther, B
Graziani, L
Johnson, E
Kennedy, B
Kent, C
Lambeck, R
Waluschka, E
Xiong, XX
AF Iona, Glenn
Butler, James
Guenther, Bruce
Graziani, Larissa
Johnson, Eric
Kennedy, Brian
Kent, Craig
Lambeck, Robert
Waluschka, Eugene
Xiong, Xiaoxiong
BE Butler, JJ
Xiong, X
Gu, X
TI VIIRS on-orbit optical anomaly - Investigation, analysis, root cause
determination and lessons learned
SO EARTH OBSERVING SYSTEMS XVII
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Earth Observing Systems XVII
CY AUG 13-16, 2012
CL San Diego, CA
SP SPIE
DE NPP; VIIRS; Degradation; MODIS; Tungsten; Radiation; Contamination;
lessons learned
ID MODIS; PERFORMANCE
AB A gradual, but persistent, decrease in the optical throughput was detected during the early commissioning phase for the Suomi National Polar-Orbiting Partnership (SNPP) Visible Infrared Imager Radiometer Suite (VIIRS) Near Infrared (NIR) bands. Its initial rate and unknown cause were coincidently coupled with a decrease in sensitivity in the same spectral wavelength of the Solar Diffuser Stability Monitor (SDSM) raising concerns about contamination or the possibility of a system-level satellite problem.
An anomaly team was formed to investigate and provide recommendations before commissioning could resume. With few hard facts in hand, there was much speculation about possible causes and consequences of the degradation. Two different causes were determined as will be explained in this paper. This paper will describe the build and test history of VIIRS, why there were no indicators, even with hindsight, of an on-orbit problem, the appearance of the on-orbit anomaly, the initial work attempting to understand and determine the cause, the discovery of the root cause and what Test-As-You-Fly (TAYF) activities, can be done in the future to greatly reduce the likelihood of similar optical anomalies. These TAYF activities are captured in the "lessons learned" section of this paper.
C1 [Iona, Glenn; Butler, James; Waluschka, Eugene; Xiong, Xiaoxiong] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Iona, G (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RI Butler, James/D-4188-2013
NR 17
TC 5
Z9 5
U1 0
U2 2
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-9227-2
J9 PROC SPIE
PY 2012
VL 8510
AR 85101C
DI 10.1117/12.933863
PG 15
WC Instruments & Instrumentation; Remote Sensing; Optics
SC Instruments & Instrumentation; Remote Sensing; Optics
GA BHU72
UT WOS:000326699000044
ER
PT S
AU Manning, EM
Jiang, YB
Aumann, HH
Elliott, DA
Hannon, S
AF Manning, Evan M.
Jiang, Yibo
Aumann, Hartmut H.
Elliott, Denis A.
Hannon, Scott
BE Butler, JJ
Xiong, X
Gu, X
TI Level-1C Product from AIRS: Principal Component Filtering
SO EARTH OBSERVING SYSTEMS XVII
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Earth Observing Systems XVII
CY AUG 13-16, 2012
CL San Diego, CA
SP SPIE
DE AIRS; Level-1C; Principal Components; NEdT; infrared sounder; grating
array; cross-calibration
AB The Atmospheric Infrared Sounder (AIRS), launched on the EOS Aqua spacecraft on May 4, 2002, is a grating spectrometer with 2378 channels in the range 3.7 to 15.4 microns. In a grating spectrometer each individual radiance measurement is largely independent of all others. Most measurements are extremely accurate and have very low noise levels. However, some channels exhibit high noise levels or other anomalous behavior, complicating applications needing radiances throughout a band, such as cross-calibration with other instruments and regression retrieval algorithms. The AIRS Level-1C product is similar to Level-1B but with instrument artifacts removed. This paper focuses on the "cleaning" portion of Level-1C, which identifies bad radiance values within spectra and produces substitute radiances using redundant information from other channels. The substitution is done in two passes, first with a simple combination of values from neighboring channels, then with principal components. After results of the substitution are shown, differences between principal component reconstructed values and observed radiances are used to investigate detailed noise characteristics and spatial misalignment in other channels.
C1 [Manning, Evan M.; Jiang, Yibo; Aumann, Hartmut H.; Elliott, Denis A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Manning, EM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM evan.m.manning@jpl.nasa.gov
NR 5
TC 1
Z9 1
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-9227-2
J9 PROC SPIE
PY 2012
VL 8510
AR 85100V
DI 10.1117/12.928546
PG 16
WC Instruments & Instrumentation; Remote Sensing; Optics
SC Instruments & Instrumentation; Remote Sensing; Optics
GA BHU72
UT WOS:000326699000030
ER
PT S
AU McCorkel, J
Thome, K
Hair, J
McAndrew, B
Jennings, D
Rabin, D
Daw, A
Lunsford, A
AF McCorkel, J.
Thome, K.
Hair, J.
McAndrew, B.
Jennings, D.
Rabin, D.
Daw, A.
Lunsford, A.
BE Butler, JJ
Xiong, X
Gu, X
TI Instrumentation and first results of the reflected solar demonstration
system for the Climate Absolute Radiance and Refractivity Observatory
SO EARTH OBSERVING SYSTEMS XVII
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Earth Observing Systems XVII
CY AUG 13-16, 2012
CL San Diego, CA
SP SPIE
DE CLARREO; imaging spectrometer; SIRCUS; calibration
AB The Climate Absolute Radiance and Refractivity Observatory (CLARREO) mission key goals include enabling observation of high accuracy long-term climate change trends, use of these observations to test and improve climate forecasts, and calibration of operational and research sensors. The spaceborne instrument suites include a reflected solar (RS) spectroradiometer, emitted infrared spectroradiometer, and radio occultation receivers. The requirement for the RS instrument is that derived reflectance must be traceable to SI standards with an absolute uncertainty of <0.3% and the error budget that achieves this requirement is described in previous work. This work describes the Solar/Lunar Absolute Reflectance Imaging Spectroradiometer (SOLARIS), a calibration demonstration system for RS instrument, and presents initial calibration and characterization methods and results. SOLARIS is an Offner spectrometer with two separate focal planes each with its own entrance aperture and grating covering spectral ranges of 320-640, 600-2300 nm over a full field-of-view of 10 degrees with 0.27 milliradian sampling. Results from laboratory measurements including use of integrating spheres, transfer radiometers and spectral standards combined with field-based solar and lunar acquisitions are presented.
C1 [McCorkel, J.; Thome, K.; Hair, J.; McAndrew, B.; Jennings, D.; Rabin, D.; Daw, A.; Lunsford, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP McCorkel, J (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
EM joel.mccorkel@nasa.gov
RI Thome, Kurtis/D-7251-2012; McCorkel, Joel/D-4454-2012; Richards,
Amber/K-8203-2015
OI McCorkel, Joel/0000-0003-2853-2036;
NR 8
TC 3
Z9 3
U1 2
U2 2
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-9227-2
J9 PROC SPIE
PY 2012
VL 8510
AR 85100B
DI 10.1117/12.930950
PG 9
WC Instruments & Instrumentation; Remote Sensing; Optics
SC Instruments & Instrumentation; Remote Sensing; Optics
GA BHU72
UT WOS:000326699000010
ER
PT S
AU Susskind, J
Blaisdell, J
Iredell, L
AF Susskind, Joel
Blaisdell, John
Iredell, Lena
BE Butler, JJ
Xiong, X
Gu, X
TI Significant Advances in the AIRS Science Team Version-6 Retrieval
Algorithm
SO EARTH OBSERVING SYSTEMS XVII
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Earth Observing Systems XVII
CY AUG 13-16, 2012
CL San Diego, CA
SP SPIE
DE AIRS/AMSU; high spectral resolution IR sounders; retrieval methodology;
IR sounding in cloudy conditions; cloud cleared radiances; Quality
Control
ID CLOUDY ATMOSPHERES
AB The Goddard DISC generated products derived from AIRS/AMSU-A observations, starting from September 2002 when the AIRS instrument became stable, using the AIRS Science Team Version-5 retrieval algorithm. The AIRS Science Team Version-6 retrieval algorithm became operational at the Goddard DISC in late 2012. This paper describes some of the significant improvements in retrieval methodology contained in the Version-6 retrieval algorithm, compared to that used in Version-5. In particular, the Science Team made major changes with regard to the algorithms used to 1) derive surface skin temperature and surface spectral emissivity; 2) generate the initial state used to start the cloud clearing and retrieval procedures; and 3) determine Quality Control. This paper describes these advances found in the AIRS Version-6 retrieval algorithm and demonstrates the improvements of some AIRS Version-6 products compared to those obtained using Version-5.
C1 [Susskind, Joel] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Susskind, J (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
NR 7
TC 4
Z9 4
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-9227-2
J9 PROC SPIE
PY 2012
VL 8510
AR 85100U
DI 10.1117/12.929953
PG 12
WC Instruments & Instrumentation; Remote Sensing; Optics
SC Instruments & Instrumentation; Remote Sensing; Optics
GA BHU72
UT WOS:000326699000029
ER
PT S
AU Thome, K
McCorkel, J
AF Thome, Kurtis
McCorkel, Joel
BE Butler, JJ
Xiong, X
Gu, X
TI CROSS-CALIBRATION OF IMAGING SENSORS USING MODEL-BASED, SI-TRACEABLE
PREDICTIONS OF AT-SENSOR RADIANCE
SO EARTH OBSERVING SYSTEMS XVII
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Earth Observing Systems XVII
CY AUG 13-16, 2012
CL San Diego, CA
SP SPIE
DE Cross-calibration; radiometric calibration; SI-traceable
ID SPECTRORADIOMETER MODIS; VICARIOUS CALIBRATION; ABSOLUTE CALIBRATION;
AVHRR; BAND; ASTER; ETM+
AB Many inter-consistency efforts force empirical agreement between sensors viewing a source nearly coincident in time and geometry that ensures consistency between sensors rather than obtain an SI-traceable calibration with documented error budgets. The method described here provides inter-consistency via absolute radiometric calibration with defensible error budget avoiding systematic errors through prediction of at-sensor radiance for a site viewed by multiple sensors but not necessarily viewed at coincident times. The method predicts spectral radiance over a given surface site for arbitrary view and illumination angles and for any date dominated by clear-sky conditions. The foundation is a model-based, SI-traceable prediction of at-sensor radiance over selected sites based on physical understanding of the surface and atmosphere. The calibration of the ground site will include spatial, spectral, and sun-view geometric effects based on satellite and ground-based data. The result is an interconsistency of hyperspectral and multispectral sensors spanning spatial resolutions from meters to kilometers all relative to the surface site rather than a single sensor. The source-centric philosophy of calibrating the site inherently accounts for footprint size mismatch, spectral band mismatch, and temporal and spatial sampling effects. The method for characterizing the test site allows its use for SI-traceable calibration of any sensor that can view the calibrated test site. Interconsistency is obtained through the traceability and error budget rather than coincident views. Such an approach to inter-consistency provides better understanding of biases between sensors as well producing more accurate results with documented SI-traceability that reduces the need for overlapping data sets.
C1 [Thome, Kurtis; McCorkel, Joel] NASA GSFC, Greenbelt, MD 20771 USA.
RP Thome, K (reprint author), NASA GSFC, Greenbelt, MD 20771 USA.
EM kurtis.thome@nasa.gov
RI Thome, Kurtis/D-7251-2012; McCorkel, Joel/D-4454-2012
OI McCorkel, Joel/0000-0003-2853-2036
NR 28
TC 1
Z9 1
U1 2
U2 7
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-9227-2
J9 PROC SPIE
PY 2012
VL 8510
AR 85100N
DI 10.1117/12.930309
PG 10
WC Instruments & Instrumentation; Remote Sensing; Optics
SC Instruments & Instrumentation; Remote Sensing; Optics
GA BHU72
UT WOS:000326699000022
ER
PT S
AU Wolfe, RE
Lin, GQ
Nishihama, M
Tewari, KP
Montano, E
AF Wolfe, Robert E.
Lin, Guoqing
Nishihama, Masahiro
Tewari, Krishna P.
Montano, Enrique
BE Butler, JJ
Xiong, X
Gu, X
TI NPP VIIRS Early On-Orbit Geometric Performance
SO EARTH OBSERVING SYSTEMS XVII
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Earth Observing Systems XVII
CY AUG 13-16, 2012
CL San Diego, CA
SP SPIE
DE Suomi NPP; VIIRS; pointing; BBR; LSF; geolocation; error trends
ID GEOLOCATION ACCURACY; RESOLUTION
AB The NASA/NOAA Visible Infrared Imager Radiometer Suite (VIIRS) instrument on-board the Suomi National Polar-orbiting Partnership satellite was launched in October 2011. Assessment of VIIRS' geometric performance includes measurements of the sensor's spatial response, band-to-band co-registration (BBR), and geolocation accuracy and precision.
The instrument sensor (detector) spatial response is estimated by line spread functions (LSFs) in the scan and track directions. The LSFs are parameterized by dynamic field of view in the scan direction and instantaneous FOV in the track direction, modulation transfer function for the 16 moderate resolution bands (M-bands), and horizontal spatial resolution for the five imagery bands (I-bands). VIIRS BBR for the M and I bands is defined as the overlapped fractional area of angular pixel sizes from the corresponding detectors in a band pair, including nested I-bands into M-bands, and measured on-orbit using lunar and earth data. VIIRS geolocation accuracy and precision are affected by instrument parameters, ancillary data (i.e., ephemeris and attitude), and thermally induced pointing variations with respect to orbital position. These are being tracked by a ground control point matching program and corrected in geolocation parameter lookup tables in the ground data processing software.
This on-orbit geometric performance assessment is an important aspect of the VIIRS sensor data record calibration and validation process. In this paper, we will discuss VIIRS' geometric performance based on the first seven-month of VIIRS' on-orbit earth and lunar data, and compare these results with the at-launch performance based on ground test data and numerical modeling results. Overall, VIIRS' on-orbit geometric performance is very good and matches the prelaunch performance, and is thus expected to meet the needs of both the long-term monitoring and operational communities.
C1 [Wolfe, Robert E.; Lin, Guoqing; Nishihama, Masahiro; Tewari, Krishna P.; Montano, Enrique] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Wolfe, RE (reprint author), NASA, Goddard Space Flight Ctr, Code 619,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
EM gary.lin@nasa.gov
RI Wolfe, Robert/E-1485-2012
OI Wolfe, Robert/0000-0002-0915-1855
NR 12
TC 11
Z9 11
U1 1
U2 3
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-9227-2
J9 PROC SPIE
PY 2012
VL 8510
AR 851013
DI 10.1117/12.929925
PG 13
WC Instruments & Instrumentation; Remote Sensing; Optics
SC Instruments & Instrumentation; Remote Sensing; Optics
GA BHU72
UT WOS:000326699000035
ER
PT S
AU Xiong, XX
Angal, A
Choi, T
Sun, JQ
Johnson, E
AF Xiong, Xiaoxiong (Jack)
Angal, Amit
Choi, Taeyoung (Jason)
Sun, Junqiang
Johnson, Eric
BE Butler, JJ
Xiong, X
Gu, X
TI On-orbit Performance of MODIS Solar Diffuser Stability Monitor
SO EARTH OBSERVING SYSTEMS XVII
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Earth Observing Systems XVII
CY AUG 13-16, 2012
CL San Diego, CA
SP SPIE
DE MODIS; VIIRS; radiometer; calibration; solar diffuser; solar diffuser
stability monitor
AB MODIS reflective solar bands (RSB) calibration is provided by an on-board solar diffuser (SD). On-orbit changes in the SD bi-directional reflectance factor (BRF) are tracked by a solar diffuser stability monitor (SDSM). The SDSM consists of a solar integration sphere (SIS) with nine detectors covering wavelengths from 0.41 to 0.94 mu m. It functions as a ratioing radiometer, making alternate observations of the sunlight through a fixed attenuation screen and the sunlight diffusely reflected from the SD during each scheduled SD/SDSM calibration event. Since launch, Terra and Aqua MODIS SD/SDSM systems have been operated regularly to support the RSB on-orbit calibration. This paper provides an overview of MODIS SDSM design functions, its operation and calibration strategies, and on-orbit performance. Changes in SDSM detector responses over time and their potential impact on tracking SD on-orbit degradation are examined. Also presented in this paper are lessons learned from MODIS SD/SDSM calibration system and improvements made to the VIIRS SD/SDSM system, including preliminary comparisons of MODIS and VIIRS SDSM on-orbit performance.
C1 [Xiong, Xiaoxiong (Jack)] NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
RP Xiong, XX (reprint author), NASA, Goddard Space Flight Ctr, Sci & Explorat Directorate, Greenbelt, MD 20771 USA.
NR 11
TC 8
Z9 8
U1 1
U2 2
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-9227-2
J9 PROC SPIE
PY 2012
VL 8510
AR 85100H
DI 10.1117/12.930963
PG 9
WC Instruments & Instrumentation; Remote Sensing; Optics
SC Instruments & Instrumentation; Remote Sensing; Optics
GA BHU72
UT WOS:000326699000016
ER
PT S
AU Daniels, JL
Thomas, S
Smith, GL
Priestley, KJ
AF Daniels, Janet L.
Thomas, Susan
Smith, G. Louis
Priestley, Kory J.
BE Shen, SS
Lewis, PE
TI The point response functions of CERES instruments aboard the Terra and
Aqua spacecrafts over the mission-to-date
SO IMAGING SPECTROMETRY XVII
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Imaging Spectrometry XVII
CY AUG 13-14, 2012
CL San Diego, CA
SP SPIE
DE CERES; Calibration; Radiometry; EOS; Terra; Aqua; Earth Radiation
Budget; point response function
ID ENERGY SYSTEM CERES; CLOUDS
AB The point response function (PRF) describes the response of an instrument to radiance from a point within its field of view. The Clouds and Earth Radiant Energy System (CERES) PRF is used together with measurements from the Moderate Resolution Imaging Spectro-radiometer (MODIS) to compute cloud information for each CERES pixel. Knowledge of the point response function (PRF) of CERES is essential to accurately align these data sets. The PRF has been measured for each CERES instrument during ground calibrations. Using in-orbit lunar calibrations, over ten years of data have been compiled for the Flight Models-1 and -2 aboard the Terra satellite and over eight years have been recorded for Flight Models-3 and -4 aboard the Aqua satellite. These data are used to examine the stability of the PRF of these instruments over the duration of their operations-to-date. In-orbit calibrations are taken at a lower scanning rate when compared to ground testing. As a result, these lunar scans provide more precise detector mapping capability due to a higher data sampling rate. Additional instrument performance measurements which can be gleaned are detector sensitivity stability and pointing accuracy.
C1 [Daniels, Janet L.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Daniels, JL (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
EM Janet.l.Daniels@nasa.gov
NR 8
TC 3
Z9 3
U1 0
U2 2
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-9232-6
J9 PROC SPIE
PY 2012
VL 8515
AR 85150O
DI 10.1117/12.928499
PG 13
WC Optics; Imaging Science & Photographic Technology; Spectroscopy
SC Optics; Imaging Science & Photographic Technology; Spectroscopy
GA BHV24
UT WOS:000326729000019
ER
PT S
AU Key, R
Sander, S
Eldering, A
Blavier, JF
Bekker, D
Manatt, K
Rider, D
Wu, YH
AF Key, Richard
Sander, Stanley
Eldering, Annmarie
Blavier, Jean-Francois
Bekker, Dmitriy
Manatt, Ken
Rider, David
Wu, Yen-Hung
BE Shen, SS
Lewis, PE
TI The Geostationary Fourier Transform Spectrometer
SO IMAGING SPECTROMETRY XVII
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Imaging Spectrometry XVII
CY AUG 13-14, 2012
CL San Diego, CA
SP SPIE
DE Fourier Transform Spectrometer; atmospheric trace gases; diurnal
land-atmosphere carbon exchange; geostationary orbit; hosted payload
ID GASES OBSERVING SATELLITE
AB The Geostationary Fourier Transform Spectrometer (GeoFTS) is an imaging spectrometer designed for a geostationary orbit (GEO) earth science mission to measure key atmospheric trace gases and process tracers related to climate change and human activity. GEO allows GeoFTS to continuously stare at a region of the earth for frequent sampling to capture the variability of biogenic fluxes and anthropogenic emissions from city to continental spatial scales and temporal scales from diurnal, synoptic, seasonal to interannual. The measurement strategy provides a process based understanding of the carbon cycle from contiguous maps of carbon dioxide (CO2), methane (CH4), carbon monoxide (CO), and chlorophyll fluorescence (CF) collected many times per day at high spatial resolution (similar to 2.7kmx2.7km at nadir). The CO2/CH4/CO/CF measurement suite in the near infrared spectral region provides the information needed to disentangle natural and anthropogenic contributions to atmospheric carbon concentrations and to minimize uncertainties in the flow of carbon between the atmosphere and surface. The half meter cube size GeoFTS instrument is based on a Michelson interferometer design that uses all high TRL components in a modular configuration to reduce complexity and cost. It is self-contained and as independent of the spacecraft as possible with simple spacecraft interfaces, making it ideal to be a "hosted" payload on a commercial communications satellite mission. The hosted payload approach for measuring the major carbon-containing gases in the atmosphere from the geostationary vantage point will affordably advance the scientific understating of carbon cycle processes and climate change.
C1 [Key, Richard; Sander, Stanley; Eldering, Annmarie; Blavier, Jean-Francois; Bekker, Dmitriy; Manatt, Ken; Rider, David; Wu, Yen-Hung] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Key, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Richard.Key@jpl.nasa.gov
NR 21
TC 2
Z9 2
U1 1
U2 3
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-9232-6
J9 PROC SPIE
PY 2012
VL 8515
AR 851506
DI 10.1117/12.930257
PG 22
WC Optics; Imaging Science & Photographic Technology; Spectroscopy
SC Optics; Imaging Science & Photographic Technology; Spectroscopy
GA BHV24
UT WOS:000326729000003
ER
PT S
AU Mouroulis, P
Van Gorp, B
Green, RO
Eastwood, M
Boardman, J
Richardson, BS
Rodriguez, JI
Urquiza, E
Franklin, BD
Gao, BC
AF Mouroulis, Pantazis
Van Gorp, Byron
Green, Robert O.
Eastwood, Michael
Boardman, Joseph
Richardson, Brandon S.
Rodriguez, Jose I.
Urquiza, Eugenio
Franklin, Brian D.
Gao, Bo-Cai
BE Shen, SS
Lewis, PE
TI Portable Remote Imaging Spectrometer (PRISM): laboratory and field
calibration
SO IMAGING SPECTROMETRY XVII
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Imaging Spectrometry XVII
CY AUG 13-14, 2012
CL San Diego, CA
SP SPIE
DE Imaging spectroscopy; coastal ocean; imaging spectrometer
AB We report the characteristics of the Portable Remote Imaging Spectrometer, an airborne sensor specifically designed for the challenges of coastal ocean research. PRISM has high signal to noise ratio and uniformity, as well as low polarization sensitivity. Acquisition of high quality data has been demonstrated with the first engineering flight.
C1 [Mouroulis, Pantazis; Van Gorp, Byron; Green, Robert O.; Eastwood, Michael; Richardson, Brandon S.; Rodriguez, Jose I.; Urquiza, Eugenio; Franklin, Brian D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mouroulis, P (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM pantazis.mouroulis@jpl.nasa.gov
NR 4
TC 1
Z9 1
U1 1
U2 6
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-9232-6
J9 PROC SPIE
PY 2012
VL 8515
AR 85150F
DI 10.1117/12.933939
PG 10
WC Optics; Imaging Science & Photographic Technology; Spectroscopy
SC Optics; Imaging Science & Photographic Technology; Spectroscopy
GA BHV24
UT WOS:000326729000010
ER
PT S
AU Pagano, TS
Olsen, ET
Nguyen, H
AF Pagano, Thomas S.
Olsen, Edward T.
Hai Nguyen
BE Shen, SS
Lewis, PE
TI Global and regional seasonal variability of mid-tropospheric CO2 as
measured by the Atmospheric Infrared Sounder (AIRS)
SO IMAGING SPECTROMETRY XVII
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Imaging Spectrometry XVII
CY AUG 13-14, 2012
CL San Diego, CA
SP SPIE
DE NASA; Satellite; Hyperspectral; Atmosphere; Carbon Dioxide
ID GASES
AB The Atmospheric Infrared Sounder (AIRS) is a hyperspectral infrared instrument on the Earth Observing System (EOS) Aqua Spacecraft, launched on May 4, 2002 into a near polar sun-synchronous orbit. AIRS has 2378 infrared channels ranging from 3.7 mu m to 15.4 mu m and a 13.5 km footprint at nadir. AIRS, in conjunction with the Advanced Microwave Sounding Unit (AMSU), produces temperature profiles with 1K/km accuracy on a global scale, as well as water vapor profiles and trace gas amounts for CO2, CO, SO2, O-3 and CH4. AIRS CO2 climatologies have been shown to be useful for identifying anomalies associated with geophysical events such as El Nino-Southern Oscillation or Madden-Julian oscillation. In this study, monthly representations of mid-tropospheric CO2 are constructed from 10 years of AIRS Version 5 monthly Level 3 data. We compare the AIRS mid-tropospheric CO2 representations to ground-based measurements from the Scripps and National Oceanic and Atmospheric Administration Climate Modeling and Diagnostics Laboratory (NOAA CMDL) ground networks to better understand the phase lag of the CO2 seasonal cycle between the surface and middle troposphere. Results show only a small phase lag in the tropics that grows to approximately two months in the northern latitudes.
C1 [Pagano, Thomas S.; Olsen, Edward T.; Hai Nguyen] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Pagano, TS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 7
TC 0
Z9 0
U1 2
U2 4
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-9232-6
J9 PROC SPIE
PY 2012
VL 8515
AR 851507
DI 10.1117/12.929197
PG 5
WC Optics; Imaging Science & Photographic Technology; Spectroscopy
SC Optics; Imaging Science & Photographic Technology; Spectroscopy
GA BHV24
UT WOS:000326729000004
ER
PT S
AU Thompson, PL
Hill, PC
AF Thompson, Patrick L.
Hill, Peter C.
BE Shen, SS
Lewis, PE
TI Conceptual optical design and system engineering of the CLARREO/RS
(Reflected Solar) instrument suite
SO IMAGING SPECTROMETRY XVII
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Imaging Spectrometry XVII
CY AUG 13-14, 2012
CL San Diego, CA
SP SPIE
DE imaging spectrometer; hyperspectral; absolute; radiometer; JUICE;
Jupiter; Europa; planet; moon; asteroid
AB The Climate Absolute Radiance and Refractivity Observatory (CLARREO) program objectives are recommended by the NRC as a Tier-1 mission in its January 15, 2007 Earth Science Decadal Survey to be the key component of a future decade-scale, global climate change observing system. The purpose of CLARREO is to make SI-traceable absolute observations sensitive to the most critical, but least understood climate forcing phenomena, responses, and feedbacks. NASA / LaRC is the mission lead as well as the Infrared (IR) instrument suite development lead. The Reflected Solar (RS) instrument lead center has been assigned to GSFC where engineering risk reduction and science calibration demonstration studies are being conducted on flight-like ETUs in anticipation of entry into Phase A.
The RS instrument suite (SOLARIS) is composed of multiple all-aluminum, slit-based, push-broom imaging spectr-oradiometers of nearly identical construction. Each 'box' will be optimized to provide better than 8nm spectral resolution (using multiple detector elements) over a specific spectral band covering the 320-2300nm total range with significant overlaps to aid calibration. Optical design, fabrication, and alignment will provide for 500m nadir resolutions over a full slit field of 100km from an approximately 600km polar orbit greater than 90% of the time. SNRs are likewise required to exceed 33 for lambda < 900nm and 25 for lambda > 900nm. The maximum radiometric sensitivity to any naturally-occurring polarized scene elements is expected to be between 0.5% - 0.75% for lambda < 1000nm and lambda > 1000nm respectively. The RS suite system will be capable of demonstrating a long-term, spectrally- & spatially-averaged, systematic radiometric error of less than 0.3% (k=2).
Coupled with measurements from on-board GPS radio occultation receivers and inherent inter-calibration compatibility with existing and future Earth science and operational missions, these measurements will provide a long-term benchmarking data record for the detection, projection, and attribution of changes to our planet's climate system. The CLARREO Project team successfully completed its Mission Concept Review (MCR) on November 17, 2010 at LaRC with high marks and remains dedicated to the mission and its instruments. However, the launch readiness date (LRD) is yet to be determined pending budget directive updates from the White House along with review of the IR and RS calibration demonstration efforts (extended pre-Phase A).
C1 [Thompson, Patrick L.; Hill, Peter C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Thompson, PL (reprint author), NASA, Goddard Space Flight Ctr, Code 551,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
RI Richards, Amber/K-8203-2015
NR 2
TC 3
Z9 3
U1 2
U2 2
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-9232-6
J9 PROC SPIE
PY 2012
VL 8515
AR UNSP 85150N
DI 10.1117/12.929849
PG 9
WC Optics; Imaging Science & Photographic Technology; Spectroscopy
SC Optics; Imaging Science & Photographic Technology; Spectroscopy
GA BHV24
UT WOS:000326729000018
ER
PT S
AU Van Gorp, B
Mouroulis, P
Green, RO
Rodriguez, JI
Blaney, D
Wilson, DW
Sellar, RG
Richardson, BS
AF Van Gorp, Byron
Mouroulis, Pantazis
Green, Robert O.
Rodriguez, Jose I.
Blaney, Diana
Wilson, Daniel W.
Sellar, R. Glenn
Richardson, Brandon S.
BE Shen, SS
Lewis, PE
TI Ultra-compact Imaging Spectrometer (UCIS) for in-situ planetary
mineralogy: laboratory and field calibration
SO IMAGING SPECTROMETRY XVII
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Imaging Spectrometry XVII
CY AUG 13-14, 2012
CL San Diego, CA
SP SPIE
DE Imaging spectroscopy; imaging spectrometer
AB The Ultra-Compact Imaging Spectrometer (UCIS) is a miniature telescope and spectrometer system intended for mapping terrain mineralogy over distances from 1.5 m to infinity with spatial sampling of 1.35 mrad over a 30 degrees field, and spectral sampling of 10 nm in the 600-2500 nm range. The core of the system has been designed for operation in a Martian environment, but can also be used in a terrestrial environment when placed inside a vacuum vessel. We report the laboratory and field calibration data that include spatial and spectral calibration, and demonstrate the use of the system.
C1 [Van Gorp, Byron; Mouroulis, Pantazis; Green, Robert O.; Rodriguez, Jose I.; Blaney, Diana; Wilson, Daniel W.; Sellar, R. Glenn; Richardson, Brandon S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Van Gorp, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM byron.vangorp@jpl.nasa.gov
NR 3
TC 3
Z9 3
U1 2
U2 3
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-9232-6
J9 PROC SPIE
PY 2012
VL 8515
AR 85150G
DI 10.1117/12.939475
PG 8
WC Optics; Imaging Science & Photographic Technology; Spectroscopy
SC Optics; Imaging Science & Photographic Technology; Spectroscopy
GA BHV24
UT WOS:000326729000011
ER
PT J
AU Ou, SC
Liou, KN
Hsu, C
Tsay, SC
AF Ou, S. C.
Liou, K. N.
Hsu, C.
Tsay, S. C.
TI Satellite remote sensing of dust aerosol indirect effects on cloud
formation over Eastern Asia
SO INTERNATIONAL JOURNAL OF REMOTE SENSING
LA English
DT Article
ID ICE CLOUDS; MODIS; CLIMATE; PRODUCTS; MODELS; STORMS; PARAMETERS; WATER
AB The dust aerosol indirect effect of the first kind on ice and liquid water cloud formation has been investigated using available MODIS cloud and aerosol products on the basis of correlation analysis. The variability in the correlation between cloud parameters, including optical depth, effective particle size, cloud water path and cloud particle number concentration, and aerosol variables, including optical depth and number concentration, over Eastern Asia has been studied. Three MODIS scenes that contain a significant presence of local and transported dust and clouds have been selected for comprehensive analysis. For all cases studied, we demonstrate that there is a negative trend regarding the correlation between cloud particle size and aerosol optical depth, which is statistically significant. These results represent a strong evidence of dust and cloud interactions that are consistent with the hypothesis of the Twomey effect for clouds.
C1 [Ou, S. C.; Liou, K. N.] Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA.
[Hsu, C.; Tsay, S. C.] NASA, Goddard Space Flight Ctr, Climate & Radiat Branch, Greenbelt, MD 20771 USA.
RP Ou, SC (reprint author), Univ Calif Los Angeles, Joint Inst Reg Earth Syst Sci & Engn, Dept Atmospher & Ocean Sci, Los Angeles, CA 90095 USA.
EM ssou@atmos.ucla.edu
RI Tsay, Si-Chee/J-1147-2014
FU NASA/Goddard Grant [NNX09AR42G]
FX This work was supported in part by the NASA/Goddard Grant NNX09AR42G.
NR 37
TC 5
Z9 5
U1 0
U2 6
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 0143-1161
EI 1366-5901
J9 INT J REMOTE SENS
JI Int. J. Remote Sens.
PY 2012
VL 33
IS 22
BP 7257
EP 7272
DI 10.1080/01431161.2012.700135
PG 16
WC Remote Sensing; Imaging Science & Photographic Technology
SC Remote Sensing; Imaging Science & Photographic Technology
GA 249WW
UT WOS:000326812500002
ER
PT J
AU Tayon, WA
Domack, MS
Hales, SJ
AF Tayon, Wesley A.
Domack, Marcia S.
Hales, Stephen J.
BE Weiland, H
Rollett, AD
Cassada, WA
TI CORRELATION OF FRACTURE BEHAVIOR WITH MICROSTRUCTURE IN FRICTION STIR
WELDED, AND SPIN-FORMED AL-LI 2195 DOMES
SO PROCEEDINGS OF THE 13TH INTERNATIONAL CONFERENCE ON ALUMINUM ALLOYS
(ICAA13)
LA English
DT Proceedings Paper
CT 13th International Conference on Aluminum Alloys (ICAA)
CY JUN 03-07, 2012
CL Carnegie Mellon Univ, Pittsburgh, PA
SP TMS
HO Carnegie Mellon Univ
DE friction stir welding; Al-Li 2195; spin forming; texture; TMAZ;
fracture; EBSD
ID TEXTURE
AB Single-piece, spin-formed domes manufactured from friction stir welded (FSW) plates of Al-Li alloy 2195 have the potential to reduce the cost of fabricating cryogenic propellant tanks. Mechanical properties in the completed domes can be related directly to the final material condition and the microstructures developed. However, these new fabrication techniques have resulted in unexpected material challenges, such as abnormal grain growth in the weld nugget and the propensity for fracture in the adjacent thermo-mechanically affected zone (TMAZ). In this study, the microstructure and texture transformations within the TMAZ are related to fracture location in the vicinity of the weldment. The texture variations in the TMAZ are caused primarily by the varying amounts of shear deformation introduced during the FSW process. Grain morphology and microtexture characteristics are examined as a function of location in the TMAZ via electron backscatter diffraction (EBSD). A strong correlation between fracture location and the presence of texture banding in the TMAZ is observed. The fracture path tends to follow a distinct region of low Taylor Factor (TF) grains.
C1 [Tayon, Wesley A.; Domack, Marcia S.; Hales, Stephen J.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Tayon, WA (reprint author), NASA, Langley Res Ctr, 8 West Taylor St,MS 188A, Hampton, VA 23681 USA.
NR 6
TC 0
Z9 0
U1 0
U2 2
PU JOHN WILEY & SONS
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER, W SUSSEX PO 19 8SQ, ENGLAND
BN 978-1-11845-804-4
PY 2012
BP 623
EP 628
PG 6
WC Metallurgy & Metallurgical Engineering
SC Metallurgy & Metallurgical Engineering
GA BHI12
UT WOS:000325479800090
ER
PT J
AU Singh, UN
Bai, YX
Yu, JR
Petros, M
AF Singh, Upendra N.
Bai, Yingxin
Yu, Jirong
Petros, Mulugeta
GP IEEE
TI Efficient Tm:Fiber Pumped Solid-State Ho:YLF 2-mu m Laser for Remote
Sensing Applications
SO 2012 INTERNATIONAL CONFERENCE ON FIBER OPTICS AND PHOTONICS (PHOTONICS)
LA English
DT Proceedings Paper
CT International Conference on Fiber Optics and Photonics (PHOTONICS)
CY DEC 09-12, 2012
CL Chennai, INDIA
AB An efficient 19 W, TEM00 mode, Ho:YLF laser pumped by continuous wave Tm:fiber laser has been demonstrated at the room temperature. The slope efficiency and optical-to-optical efficiency are 65% and 55%, respectively.
C1 [Singh, Upendra N.; Yu, Jirong; Petros, Mulugeta] NASA, Langley Res Ctr, Hampton, VA USA.
RP Singh, UN (reprint author), NASA, Langley Res Ctr, Hampton, VA USA.
EM Upendra.N.Singh@nasa.gov
NR 5
TC 0
Z9 0
U1 0
U2 2
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4673-4718-1
PY 2012
PG 3
WC Engineering, Electrical & Electronic; Optics
SC Engineering; Optics
GA BHQ22
UT WOS:000326324000218
ER
PT S
AU Forgione, JB
Grose, JR
Myers, JS
Sorenson, CE
Vogler, RG
AF Forgione, Joshua B.
Grose, Jeffrey R.
Myers, Jeffrey S.
Sorenson, Carl E.
Vogler, Roy G.
BE Ardanuy, PE
Puschell, JJ
Bloom, HJ
TI The EIP: A Standard Experimenter Interface Panel for NASA Airborne
Science
SO REMOTE SENSING SYSTEM ENGINEERING IV
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Remote Sensing System Engineering IV
CY AUG 12-13, 2012
CL San Diego, CA
SP SPIE
DE airborne science; sensor webs; instrumentation; data systems; power;
Ethernet; avionics
AB NASA operates a fleet of piloted and UAV aircraft to perform a variety of Earth Science and emergency observation [1]. NASA's recent move toward sensor-web mission architectures requires a corresponding upgrade to its payload systems. NASA Airborne Science payloads will now interface to a new standard Experimenter Interface Panel (EIP), presented here.
This discussion will cover the standard interface from the payload perspective. Details are provided on payload interface, cockpit control (for manned aircraft), technical design, network physical layer, qualification, and maintenance. Analyses are provided to support high-altitude design 'rules of thumb' and design decisions.
C1 [Forgione, Joshua B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Forgione, JB (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
NR 22
TC 1
Z9 1
U1 0
U2 0
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-9233-3
J9 PROC SPIE
PY 2012
VL 8516
AR UNSP 85160A
DI 10.1117/12.928380
PG 13
WC Remote Sensing; Optics
SC Remote Sensing; Optics
GA BHU08
UT WOS:000326658800008
ER
PT S
AU Thome, K
McCorkel, J
Hair, J
McAndrew, B
Daw, A
Jennings, D
Rabin, D
AF Thome, Kurtis
McCorkel, Joel
Hair, Jason
McAndrew, Brendan
Daw, Adrian
Jennings, Donald
Rabin, Douglas
BE Ardanuy, PE
Puschell, JJ
Bloom, HJ
TI TEST PLAN FOR A CALIBRATION DEMONSTRATION SYSTEM FOR THE REFLECTED SOLAR
INSTRUMENT FOR THE CLIMATE ABSOLUTE RADIANCE AND REFRACTIVITY
OBSERVATORY
SO REMOTE SENSING SYSTEM ENGINEERING IV
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Remote Sensing System Engineering IV
CY AUG 12-13, 2012
CL San Diego, CA
SP SPIE
DE CLARREO; preflight calibration; radiometric calibration; SI-traceable
AB The Climate Absolute Radiance and Refractivity Observatory (CLARREO) mission addresses the need to observe high-accuracy, long-term climate change trends and to use decadal change observations as the most critical method to determine the accuracy of climate change. One of the major objectives of CLARREO is to advance the accuracy of SI traceable absolute calibration at infrared and reflected solar wavelengths. This advance is required to reach the on-orbit absolute accuracy required to allow climate change observations to survive data gaps while remaining sufficiently accurate to observe climate change to within the uncertainty of the limit of natural variability. While these capabilities exist at NIST in the laboratory, there is a need to demonstrate that it can move successfully from NIST to NASA and/or instrument vendor capabilities for future spaceborne instruments. The current work describes the test plan for the Solar, Lunar for Absolute Reflectance Imaging Spectroradiometer (SOLARIS) which is the calibration demonstration system (CDS) for the reflected solar portion of CLARREO. The goal of the CDS is to allow the testing and evaluation of calibration approaches, alternate design and/or implementation approaches and components for the CLARREO mission. SOLARIS also provides a test-bed for detector technologies, non-linearity determination and uncertainties, and application of future technology developments and suggested spacecraft instrument design modifications. The end result of efforts with the SOLARIS CDS will be an SI-traceable error budget for reflectance retrieval using solar irradiance as a reference and methods for laboratory-based, absolute calibration suitable for climate-quality data collections.
C1 [Thome, Kurtis; McCorkel, Joel; Hair, Jason; McAndrew, Brendan; Daw, Adrian; Jennings, Donald; Rabin, Douglas] NASA, GSFC, Greenbelt, MD 20771 USA.
RP Thome, K (reprint author), NASA, GSFC, Greenbelt, MD 20771 USA.
EM kurtis.thome@nasa.gov
RI Thome, Kurtis/D-7251-2012; McCorkel, Joel/D-4454-2012; Richards,
Amber/K-8203-2015
OI McCorkel, Joel/0000-0003-2853-2036;
NR 7
TC 1
Z9 1
U1 2
U2 3
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-9233-3
J9 PROC SPIE
PY 2012
VL 8516
AR UNSP 851602
DI 10.1117/12.930337
PG 11
WC Remote Sensing; Optics
SC Remote Sensing; Optics
GA BHU08
UT WOS:000326658800002
ER
PT S
AU Norbury, JW
AF Norbury, John W.
BE Freeman, S
Andreyev, A
Bruce, A
Deacon, A
Jenkins, D
Joss, D
MacGregor, D
Regan, P
Simpson, J
Tungate, G
Wadsworth, R
Watts, D
TI Nuclear physics and space radiation
SO RUTHERFORD CENTENNIAL CONFERENCE ON NUCLEAR PHYSICS, 2011
SE Journal of Physics Conference Series
LA English
DT Proceedings Paper
CT Rutherford Centennial Conference on Nuclear Physics
CY AUG 08-12, 2011
CL Univ Manchester, Manchester, ENGLAND
HO Univ Manchester
ID VALIDATION; TRANSPORT; HZETRN
AB Nuclear fragmentation reactions induced by alpha particle projectiles are an important component of the space radiation problem. Inclusive isotopic spectral distributions and double differential cross sections are used as input to the Boltzmann transport equation, which is often solved in many space radiation applications. For alpha particle projectiles, it is found that most of the available experimental data are below the pion threshold. This is a significant validation gap because the important energy range for galactic cosmic rays extends up to 10 GeV/n and above.
C1 NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Norbury, JW (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
EM john.w.norbury@nasa.gov
NR 11
TC 0
Z9 0
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 1742-6588
J9 J PHYS CONF SER
PY 2012
VL 381
AR 012117
DI 10.1088/1742-6596/381/1/012117
PG 4
WC Physics, Particles & Fields
SC Physics
GA BEE76
UT WOS:000316303200118
ER
PT B
AU Maxwell, T
AF Maxwell, Thomas
GP IEEE
TI Exploratory Climate Data Visualization and Analysis Using DV3D and
UVCDAT
SO 2012 SC COMPANION: HIGH PERFORMANCE COMPUTING, NETWORKING, STORAGE AND
ANALYSIS (SCC)
LA English
DT Proceedings Paper
CT 25th ACM/IEEE International Conference for High Performance Computing,
Networking, Storage and Analysis (SC)
CY NOV 10-16, 2012
CL Salt Lake City, UT
SP IEEE Comp Soc, Assoc Comp Machinery (ACM), IEEE
DE climate; visualization; analysis; simulation
AB Earth system scientists are being inundated by an explosion of data generated by ever-increasing resolution in both global models and remote sensors. Advanced tools for accessing, analyzing, and visualizing very large and complex climate data are required to maintain rapid progress in Earth system research. To meet this need, NASA, in collaboration with the Ultra-scale Visualization Climate Data Analysis Tools (UV-CDAT) consortium, is developing exploratory climate data analysis and visualization tools which provide data analysis capabilities for the Earth System Grid (ESG).
This paper describes DV3D, a UV-CDAT package that enables exploratory analysis of climate simulation and observation datasets. DV3D provides user-friendly interfaces for visualization and analysis of climate data at a level appropriate for scientists. It features workflow interfaces, interactive 4D data exploration, hyperwall and stereo visualization, automated provenance generation, and parallel task execution. DV3D's integration with CDAT's climate data management system (CDMS) and other climate data analysis tools provides a wide range of high performance climate data analysis operations. DV3D expands the scientists' toolbox by incorporating a suite of rich new exploratory visualization and analysis methods for addressing the complexity of climate datasets.
C1 NASA, Goddard Space Flight Ctr, Ctr Climate Simulat, Greenbelt, MD USA.
RP Maxwell, T (reprint author), NASA, Goddard Space Flight Ctr, Ctr Climate Simulat, Greenbelt, MD USA.
EM thomas.maxwell@nasa.gov
NR 7
TC 0
Z9 0
U1 0
U2 2
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-0-7695-4956-9; 978-1-4673-6218-4
PY 2012
BP 483
EP 487
DI 10.1109/SC.Companion.2012.69
PG 5
WC Computer Science, Hardware & Architecture; Computer Science, Theory &
Methods; Engineering, Electrical & Electronic
SC Computer Science; Engineering
GA BFO96
UT WOS:000320824300059
ER
PT B
AU Putman, W
AF Putman, William
GP IEEE
TI A Dynamic Portrait of Global Aerosols
SO 2012 SC COMPANION: HIGH PERFORMANCE COMPUTING, NETWORKING, STORAGE AND
ANALYSIS (SCC)
LA English
DT Proceedings Paper
CT 25th ACM/IEEE International Conference for High Performance Computing,
Networking, Storage and Analysis (SC)
CY NOV 10-16, 2012
CL Salt Lake City, UT
SP IEEE Comp Soc, Assoc Comp Machinery (ACM), IEEE
AB Through numerical experiments that simulate our current knowledge of the dynamical and physical processes that govern weather and climate variability of Earth's atmosphere, models create a dynamic portrait of our planet. The simulation visualized here captures how winds lift up aerosols from the Earth's surface and transport them around the globe. Such simulations allow scientists to identify the source and pathway of these tiny particulates that influence weather and climate. Each frame covers a 30-minute interval, from September 1, 2006 to January 31, 2007.
C1 [Putman, William] NASA Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
RP Putman, W (reprint author), NASA Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
NR 8
TC 2
Z9 2
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-0-7695-4956-9; 978-1-4673-6218-4
PY 2012
BP 1583
EP 1588
PG 6
WC Computer Science, Hardware & Architecture; Computer Science, Theory &
Methods; Engineering, Electrical & Electronic
SC Computer Science; Engineering
GA BFO96
UT WOS:000320824300324
ER
PT B
AU Krantz, TL
AF Krantz, Timothy L.
GP ASME
TI ON CALCULATION METHODS AND RESULTS FOR STRAIGHT CYLINDRICAL ROLLER
BEARING DEFLECTION, STIFFNESS, AND STRESS
SO PROCEEDINGS OF THE ASME INTERNATIONAL DESIGN ENGINEERING TECHNICAL
CONFERENCES AND COMPUTERS AND INFORMATION IN ENGINEERING CONFERENCE,
2011, VOL 8
LA English
DT Proceedings Paper
CT ASME Internationl Design Engineering Technical Conferences / Computers
and Information in Engineering Conference (IDETC/CIE)
CY AUG 28-31, 2011
CL Washington, DC
SP Amer Soc Mech Engineers, Design Engn Div, Amer Soc Mech Engineers, Comp & Informat Engn Div
ID CONTACT
AB The purpose of this study was to assess some calculation methods for quantifying the relationships of bearing geometry, material properties, load, deflection, stiffness, and stress. The scope of the work was limited to two-dimensional modeling of straight cylindrical roller bearings. Preparations for studies of dynamic response of bearings with damaged surfaces motivated this work. Studies were selected to exercise and build confidence in the numerical tools. Three calculation methods were used in this work. Two of the methods were numerical solutions of the Hertz contact approach. The third method used was a combined finite element surface integral method. Example calculations were done for a single roller loaded between an inner and outer raceway for code verification. Next, a bearing with 13 rollers and all-steel construction was used as an example to do additional code verification, including an assessment of the leading order of accuracy of the finite element and surface integral method. Results from that study show that the method is at least first-order accurate. Those results also show that the contact grid refinement has a more significant influence on precision as compared to the finite element grid refinement. To explore the influence of material properties, the 13-roller bearing was modeled as made from Nitinol 60, a material with very different properties from steel and showing some potential for bearing applications. The codes were exercised to compare contact areas and stress levels for steel and Nitinol 60 bearings operating at equivalent power density. As a step toward modeling the dynamic response of bearings having surface damage, static analyses were completed to simulate a bearing with a spall or similar damage.
C1 NASA, Cleveland, OH USA.
RP Krantz, TL (reprint author), NASA, Cleveland, OH USA.
NR 29
TC 0
Z9 0
U1 0
U2 2
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-5485-3
PY 2012
BP 25
EP 36
PG 12
WC Engineering, Manufacturing; Engineering, Electrical & Electronic;
Engineering, Mechanical; Transportation Science & Technology
SC Engineering; Transportation
GA BGW27
UT WOS:000324349100003
ER
PT S
AU Arpin, CYP
Stoltzfus, J
AF Arpin, Christina Y. Pina
Stoltzfus, Joel
BE Davis, SE
Steinberg, TA
TI Rudimentary Cleaning Compared to Level 300A
SO FLAMMABILITY AND SENSITIVITY OF MATERIALS IN OXYGEN-ENRICHED
ATMOSPHERES, VOL 13
SE American Society for Testing and Materials Special Technical
Publications
LA English
DT Proceedings Paper
CT 13th International Conference on Flammability and Sensitivity of
Materials in Oxygen-Enriched Atmospheres
CY SEP 19-21, 2012
CL Montreal, CANADA
SP ASTM Int Comm G04 Compatibil & Sensitiv Mat Oxygen Enriched Atmospheres
DE precision cleaning; rudimentary cleaning; Level 300; oxygen systems;
hardware cleaning procedures; process; non-cleanroom; field shop
environment
AB A study was performed to characterize the cleanliness level achievable when using a rudimentary cleaning process, and results were compared to JPR 5322.1G Level 300A. While it is not ideal to clean in a shop environment, some situations (e. g., field combat operations) require oxygen system hardware to be maintained and cleaned to prevent a fire hazard, even though it cannot be sent back to a precision cleaning facility. This study measured the effectiveness of basic shop cleaning. Initially, three items representing parts of an oxygen system with maximum operating pressure of 2000 psi were contaminated: a metal plate, valve body, and metal oxygen bottle. The contaminants chosen were representative of materials that could contaminate the system during normal use: oil, lubricant, metal shavings/powder, sand, fingerprints, tape, lip balm, and hand lotion. The cleaning process used hot water, soap, various brushes, gaseous nitrogen, a water nozzle, plastic trays, scouring pads, and a controlled shop environment. Test subjects were classified into three groups: technical professionals having an appreciation for oxygen hazards; professional precision cleaners; and a group with no previous professional knowledge of oxygen or precision cleaning. Three test subjects were in each group, and each was provided with standard cleaning equipment, a cleaning procedure, and one of each of the three test items to clean. The results indicated that the achievable cleanliness level was independent of the technical knowledge or proficiency of the personnel cleaning the items. Results also showed that achieving a Level 300 particle count was more difficult than achieving a Level A nonvolatile residue amount.
C1 [Arpin, Christina Y. Pina] NASA, Tech Serv Off, Johnson Space Ctr White Sands Test Facil, Las Cruces, NM 88012 USA.
RP Arpin, CYP (reprint author), NASA, Tech Serv Off, Johnson Space Ctr White Sands Test Facil, Las Cruces, NM 88012 USA.
NR 4
TC 0
Z9 0
U1 2
U2 3
PU ASTM INTERNATIONAL
PI WEST CONSHOHOCKEN
PA 100 BARR HARBOR DRIVE, PO BOX C700, WEST CONSHOHOCKEN, PA 19428-2959 USA
SN 0066-0558
BN 978-0-8031-7547-1
J9 AM SOC TEST MATER
PY 2012
VL 1561
DI 10.1520/STP20120015
PG 15
WC Materials Science, Characterization & Testing
SC Materials Science
GA BHH73
UT WOS:000325463400004
ER
PT S
AU Davis, SE
AF Davis, Samuel Edgar
BE Davis, SE
Steinberg, TA
TI An Elementary Overview of the Selection of Materials for Service in
Oxygen-enriched Environments
SO FLAMMABILITY AND SENSITIVITY OF MATERIALS IN OXYGEN-ENRICHED
ATMOSPHERES, VOL 13
SE American Society for Testing and Materials Special Technical
Publications
LA English
DT Proceedings Paper
CT 13th International Conference on Flammability and Sensitivity of
Materials in Oxygen-Enriched Atmospheres
CY SEP 19-21, 2012
CL Montreal, CANADA
SP ASTM Int Comm G04 Compatibil & Sensitiv Mat Oxygen Enriched Atmospheres
AB The process of selecting materials for use in oxygen or oxygen-enriched environments is one that continues to be investigated by many industries because of the importance to those industries of oxygen systems. There are several excellent resources available to assist oxygen systems design engineers and end-users, with the most comprehensive being the second edition of ASTM MNL-36, Safe Use of Oxygen and Oxygen Systems: Handbook for Design, Operation and Maintenance. ASTM also makes available several standards for oxygen systems. However, the ASTM publications are extremely detailed and typically are designed for professionals who already possess a working knowledge of oxygen systems. No notable resource exists, whether an ASTM publication or that of some other organization, that can be used to educate engineers or technicians who have no prior knowledge of the nuances of oxygen system design and safety. This paper will fill the void for information needed by organizations that design or operate oxygen systems. The information in this paper is not new, but it provides a concise and easily understood summary of the selection of materials for oxygen systems. This paper will serve well as an employee's first introduction to oxygen system materials selection, and probably as the employee's first introduction to ASTM.
C1 NASA, George C Marshall Space Flight Ctr, Mat & Proc Lab, Huntsville, AL 35812 USA.
RP Davis, SE (reprint author), NASA, George C Marshall Space Flight Ctr, Mat & Proc Lab, Huntsville, AL 35812 USA.
NR 17
TC 0
Z9 0
U1 0
U2 0
PU ASTM INTERNATIONAL
PI WEST CONSHOHOCKEN
PA 100 BARR HARBOR DRIVE, PO BOX C700, WEST CONSHOHOCKEN, PA 19428-2959 USA
SN 0066-0558
BN 978-0-8031-7547-1
J9 AM SOC TEST MATER
PY 2012
VL 1561
DI 10.1520/STP20120001
PG 27
WC Materials Science, Characterization & Testing
SC Materials Science
GA BHH73
UT WOS:000325463400002
ER
PT S
AU Davis, SE
Steinberg, TA
AF Davis, Samuel Edgar
Steinberg, Theodore A.
BE Davis, SE
Steinberg, TA
TI Selected Technical Papers STP1561 Flammability and Sensitivity of
Materials in Oxygen-Enriched Atmospheres: 13th Volume
SO FLAMMABILITY AND SENSITIVITY OF MATERIALS IN OXYGEN-ENRICHED
ATMOSPHERES, VOL 13
SE American Society for Testing and Materials Special Technical
Publications
LA English
DT Proceedings Paper
CT 13th International Conference on Flammability and Sensitivity of
Materials in Oxygen-Enriched Atmospheres
CY SEP 19-21, 2012
CL Montreal, CANADA
SP ASTM Int Comm G04 Compatibil & Sensitiv Mat Oxygen Enriched Atmospheres
C1 [Davis, Samuel Edgar] NASA, George C Marshall Space Flight Ctr, Mat & Proc Lab, Huntsville, AL 35812 USA.
RP Davis, SE (reprint author), NASA, George C Marshall Space Flight Ctr, Mat & Proc Lab, Huntsville, AL 35812 USA.
NR 0
TC 0
Z9 0
U1 1
U2 1
PU ASTM INTERNATIONAL
PI WEST CONSHOHOCKEN
PA 100 BARR HARBOR DRIVE, PO BOX C700, WEST CONSHOHOCKEN, PA 19428-2959 USA
SN 0066-0558
BN 978-0-8031-7547-1
J9 AM SOC TEST MATER
PY 2012
VL 1561
PG 3
WC Materials Science, Characterization & Testing
SC Materials Science
GA BHH73
UT WOS:000325463400001
ER
PT S
AU Stoltzfus, JM
Jeffers, N
Gallus, TD
AF Stoltzfus, Joel M.
Jeffers, Nathan
Gallus, Timothy D.
BE Davis, SE
Steinberg, TA
TI Burning of CP Titanium (Grade 2) in Oxygen-Enriched Atmospheres
SO FLAMMABILITY AND SENSITIVITY OF MATERIALS IN OXYGEN-ENRICHED
ATMOSPHERES, VOL 13
SE American Society for Testing and Materials Special Technical
Publications
LA English
DT Proceedings Paper
CT 13th International Conference on Flammability and Sensitivity of
Materials in Oxygen-Enriched Atmospheres
CY SEP 19-21, 2012
CL Montreal, CANADA
SP ASTM Int Comm G04 Compatibil & Sensitiv Mat Oxygen Enriched Atmospheres
DE flammability; oxygen; titanium; RRMI
ID COMBUSTION; IGNITION
AB The flammability in oxygen-enriched atmospheres of commercially pure (CP) titanium rods as a function of diameter and test gas pressure was determined. Test samples of varying diameters were ignited at the bottom and burned upward in 70 % O-2/balance N-2 and in 99.5 +/-% O-2 at various pressures. The burning rate of each ignited sample was determined by observing the apparent regression rate of the melting interface (RRMI) of the burning samples. The burning rate or RRMI increased with decreasing test sample diameter and with increasing test gas pressure and oxygen concentration. The oxygen concentration had a much more marked affect on the burning rate than oxygen pressure.
C1 [Stoltzfus, Joel M.] NASA, Mat & Components Labs Off, Johnson Space Ctr White Sands Test Facil, Las Cruces, NM 88012 USA.
RP Stoltzfus, JM (reprint author), NASA, Mat & Components Labs Off, Johnson Space Ctr White Sands Test Facil, Las Cruces, NM 88012 USA.
NR 7
TC 0
Z9 0
U1 0
U2 1
PU ASTM INTERNATIONAL
PI WEST CONSHOHOCKEN
PA 100 BARR HARBOR DRIVE, PO BOX C700, WEST CONSHOHOCKEN, PA 19428-2959 USA
SN 0066-0558
BN 978-0-8031-7547-1
J9 AM SOC TEST MATER
PY 2012
VL 1561
DI 10.1520/STP20120017
PG 16
WC Materials Science, Characterization & Testing
SC Materials Science
GA BHH73
UT WOS:000325463400012
ER
PT S
AU Stoltzfus, JM
Gallus, TD
Sparks, K
AF Stoltzfus, Joel M.
Gallus, Timothy D.
Sparks, Kyle
BE Davis, SE
Steinberg, TA
TI Flow Friction or Spontaneous Ignition?
SO FLAMMABILITY AND SENSITIVITY OF MATERIALS IN OXYGEN-ENRICHED
ATMOSPHERES, VOL 13
SE American Society for Testing and Materials Special Technical
Publications
LA English
DT Proceedings Paper
CT 13th International Conference on Flammability and Sensitivity of
Materials in Oxygen-Enriched Atmospheres
CY SEP 19-21, 2012
CL Montreal, CANADA
SP ASTM Int Comm G04 Compatibil & Sensitiv Mat Oxygen Enriched Atmospheres
DE flow friction; spontaneous combustion; ignition mechanism; pressurized
oxygen-enriched systems
AB "Flow friction," a proposed ignition mechanism in oxygen systems, has proved elusive in attempts at experimental verification. In this paper, the literature regarding flow friction is reviewed and the experimental verification attempts are briefly discussed. Another ignition mechanism, a form of spontaneous combustion, is proposed as an explanation for at least some of the fire events that have been attributed to flow friction in the literature. In addition, the results of a failure analysis performed at NASA Johnson Space Center White Sands Test Facility are presented, and the observations indicate that spontaneous combustion was the most likely cause of the fire in this 2000 psig (14 MPa) oxygen-enriched system.
C1 [Stoltzfus, Joel M.] NASA, Mat & Components Labs Off, Johnson Space Ctr White Sands Test Facil, Las Cruces, NM 88004 USA.
RP Stoltzfus, JM (reprint author), NASA, Mat & Components Labs Off, Johnson Space Ctr White Sands Test Facil, Las Cruces, NM 88004 USA.
NR 12
TC 1
Z9 1
U1 0
U2 1
PU ASTM INTERNATIONAL
PI WEST CONSHOHOCKEN
PA 100 BARR HARBOR DRIVE, PO BOX C700, WEST CONSHOHOCKEN, PA 19428-2959 USA
SN 0066-0558
BN 978-0-8031-7547-1
J9 AM SOC TEST MATER
PY 2012
VL 1561
DI 10.1520/STP20120016
PG 19
WC Materials Science, Characterization & Testing
SC Materials Science
GA BHH73
UT WOS:000325463400005
ER
PT S
AU Hah, C
AF Hah, Chunill
GP ASME
TI INVESTIGATION OF TURBULENT TIP LEAKAGE VORTEX IN AN AXIAL WATER JET PUMP
WITH LARGE EDDY SIMULATION
SO PROCEEDINGS OF THE ASME FLUIDS ENGINEERING DIVISION SUMMER MEETING,
2012, VOL 1, PTS A AND B, SYMPOSIA
SE ASME Fluids Engineering Division Summer Meeting
LA English
DT Proceedings Paper
CT ASME Fluids Engineering Division Summer Meeting (FEDSM)
CY JUL 08-12, 2012
CL Rio Grande, PR
SP ASME, Fluids Engn Div
AB Detailed steady and unsteady numerical studies were performed to investigate tip clearance flow in an axial water jet pump. The primary objective is to understand physics of unsteady tip clearance flow, unsteady tip leakage vortex, and cavitation inception in an axial water jet pump. Steady pressure field and resulting steady tip leakage vortex from a steady flow analysis do not seem to explain measured cavitation inception correctly. The measured flow field near the tip is unsteady and measured cavitation inception is highly transient. Flow visualization with cavitation bubbles shows that the leakage vortex is oscillating significantly and many intermittent vortex ropes are present between the suction side of the blade and the tip leakage core vortex. Although the flow field is highly transient, the overall flow structure is stable and a characteristic frequency seems to exist. To capture relevant flow physics as much as possible, a Reynolds-averaged Navier-Stokes (RANS) calculation and a Large Eddy Simulation (LES) were applied for the current investigation. The present study reveals that several vortices from the tip leakage vortex system cross the tip gap of the adjacent blade periodically. Sudden changes in local pressure field inside tip gap due to these vortices create vortex ropes. The instantaneous pressure filed inside the tip gap is drastically different from that of the steady flow simulation. Unsteady flow simulation which can calculate unsteady vortex motion is necessary to calculate cavitation inception accurately even at design flow condition in such a water jet pump.
C1 NASA, Glenn Res Ctr, Cleveland, OH USA.
RP Hah, C (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA.
NR 12
TC 0
Z9 3
U1 1
U2 2
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
SN 1093-4928
BN 978-0-7918-4475-5
J9 ASME FLUID ENG DIV
PY 2012
BP 135
EP 142
PG 8
WC Engineering, Mechanical; Transportation Science & Technology
SC Engineering; Transportation
GA BGX48
UT WOS:000324506700014
ER
PT B
AU Prassinos, PG
Lyver, JW
Bui, CT
AF Prassinos, Peter G.
Lyver, John W.
Bui, Chinh T.
GP ASME
TI RISK ASSESSMENT OVERVIEW
SO PROCEEDINGS OF THE ASME INTERNATIONAL MECHANICAL ENGINEERING CONGRESS
AND EXPOSITION, 2011, VOL 1
LA English
DT Proceedings Paper
CT ASME International Mechanical Engineering Congress and Exposition
(IMECE)
CY NOV 11-17, 2011
CL Denver, CO
SP Amer Soc Mech Engn
AB Risk assessment is used in many industries to identify and manage risks. Initially developed for use on aeronautical and nuclear systems, risk assessment has been applied to transportation, chemical, computer, financial, and security systems among others. It is used to gain an understanding of the weaknesses or vulnerabilities in a system so modification can be made to increase operability, efficiency, and safety and to reduce failure and down-time. Risk assessment results are primary inputs to risk-informed decision making; where risk information including uncertainty is used along with other pertinent information to assist management in the decision-making process. Therefore, to be useful, a risk assessment must be directed at specific objectives.
As the world embraces the globalization of trade and manufacturing, understanding the associated risk become important to decision making. Applying risk assessment techniques to a global system of development, manufacturing, and transportation can provide insight into how the system can fail, the likelihood of system failure and the consequences of system failure. The risk assessment can identify those elements that contribute most to risk and identify measures to prevent and mitigate failures, disruptions, and damaging outcomes. In addition, risk associated with public and environment impact can be identified. The risk insights gained can be applied to making decisions concerning suitable development and manufacturing locations, supply chains, and transportation strategies. While risk assessment has been mostly applied to mechanical and electrical systems, the concepts and techniques can be applied across other systems and activities. This paper provides a basic overview of the development of a risk assessment.
C1 [Prassinos, Peter G.; Lyver, John W.] NASA, Washington, DC 20546 USA.
RP Prassinos, PG (reprint author), NASA, Washington, DC 20546 USA.
NR 3
TC 0
Z9 0
U1 0
U2 2
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-5487-7
PY 2012
BP 673
EP 677
PG 5
WC Engineering, Aerospace; Energy & Fuels; Engineering, Mechanical
SC Engineering; Energy & Fuels
GA BHD13
UT WOS:000325040500073
ER
PT B
AU Schiller, NH
Perey, DF
Cabell, RH
AF Schiller, Noah H.
Perey, Daniel F.
Cabell, Randolph H.
GP ASME
TI DEVELOPMENT OF A PRACTICAL BROADBAND ACTIVE VIBRATION CONTROL SYSTEM
SO PROCEEDINGS OF THE ASME INTERNATIONAL MECHANICAL ENGINEERING CONGRESS
AND EXPOSITION, 2011, VOL 8
LA English
DT Proceedings Paper
CT ASME International Mechanical Engineering Congress and Exposition
(IMECE)
CY NOV 11-17, 2011
CL Denver, CO
SP Amer Soc Mech Engn
AB The goal of this work is to develop robust, lightweight, and low-power control units that can be used to suppress structural vibration in flexible aerospace structures. In particular, this paper focuses on active damping, which is implemented using compact decentralized control units distributed over the structure. Each control unit consists of a diamond-shaped piezoelectric patch actuator, three miniature accelerometers, and analog electronics. The responses from the accelerometers are added together and then integrated to give a signal proportional to velocity. The signal is then inverted, amplified, and applied to the actuator, which generates a control force that is out of phase with the measured velocity.
This paper describes the development of the control system, including a detailed description of the control and power electronics. The paper also presents experimental results acquired on a Plexiglas window blank. Five identical control units installed around the perimeter of the window achieved
dB peak reductions and a 2.4 dB integrated reduction of the spatially averaged velocity of the window between 500 and 3000 Hz.
C1 [Schiller, Noah H.; Perey, Daniel F.; Cabell, Randolph H.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
RP Schiller, NH (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
NR 12
TC 0
Z9 0
U1 0
U2 0
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-5494-5
PY 2012
BP 683
EP 690
PG 8
WC Acoustics; Engineering, Mechanical
SC Acoustics; Engineering
GA BHC47
UT WOS:000324956000088
ER
PT S
AU DellaCorte, C
Noebe, RD
Stanford, MK
Padula, SA
AF DellaCorte, Christopher
Noebe, Ronald D.
Stanford, Malcolm K.
Padula, Santo A.
BE Takeuchi, YR
Mandler, WF
TI Resilient and Corrosion-proof Rolling Element Bearings Made from
Superelastic Ni-Ti Alloys for Aerospace Mechanism Applications
SO ROLLING ELEMENT BEARINGS, 9TH VOL
SE American Society for Testing and Materials Special Technical
Publications
LA English
DT Proceedings Paper
CT 7th ASTM International Symposium on Rolling Element Bearings
CY APR 13-14, 2011
CL Anaheim, CA
SP ASTM Int, ASTM Int Comm F34 Rolling Element Bearings
DE materials; tribology; bearings; shock load resistance; mechanical
components; superelastic materials
AB Mechanical components (bearings, gears, mechanisms) typically utilize hard materials to minimize wear and attain long life. In such components, heavily loaded contact points (e.g., meshing gear teeth, bearing ball-raceway contacts) experience high contact stresses. The combination of high hardness, heavy loads, and high elastic modulus often leads to damaging contact stress. In addition, mechanical component materials such as tool steel or silicon nitride exhibit limited recoverable strain (typically less than 1 %). These material attributes can lead to Brinell damage (e.g., denting), particularly during transient overload events such as shock impacts that occur during the launching of space vehicles or the landing of aircraft. In this paper, a superelastic alloy, 60NiTi, is considered for rolling element bearing applications. A series of Rockwell and Brinell hardness, compressive strength, fatigue, and tribology tests have been conducted and are reported. The combination of high hardness, moderate elastic modulus, large recoverable strain, low density, and intrinsic corrosion immunity provides a path to the creation of bearings largely impervious to shock load damage. It is anticipated that bearings and components made from alloys with such attributes might alleviate many problems encountered in advanced aerospace applications.
C1 [DellaCorte, Christopher; Noebe, Ronald D.; Stanford, Malcolm K.; Padula, Santo A.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP DellaCorte, C (reprint author), NASA, Glenn Res Ctr, 21000 Brookpark Rd, Cleveland, OH 44135 USA.
NR 15
TC 2
Z9 2
U1 1
U2 3
PU ASTM INTERNATIONAL
PI WEST CONSHOHOCKEN
PA 100 BARR HARBOR DRIVE, PO BOX C700, WEST CONSHOHOCKEN, PA 19428-2959 USA
SN 0066-0558
BN 978-0-8031-7528-0
J9 AM SOC TEST MATER
PY 2012
VL 1542
BP 143
EP 166
DI 10.1520/STP103887
PG 24
WC Engineering, Mechanical; Materials Science, Characterization & Testing
SC Engineering; Materials Science
GA BHL09
UT WOS:000325761000007
ER
PT J
AU Richardson, IG
Cane, HV
AF Richardson, Ian G.
Cane, Hilary V.
TI Near-earth solar wind flows and related geomagnetic activity during more
than four solar cycles (1963-2011)
SO JOURNAL OF SPACE WEATHER AND SPACE CLIMATE
LA English
DT Article
DE Stream; Solar cycle; Interplanetary Coronal Mass Ejection (CME);
Interplanetary medium
ID CORONAL MASS EJECTIONS; INTERPLANETARY MAGNETIC-FIELD; COSMIC-RAY
DECREASES; COROTATING INTERACTION REGIONS; LONG-TERM AVERAGES; ENERGETIC
PARTICLES; AA INDEXES; STORMS; INTENSITY; STREAMS
AB In past studies, we classified the near-Earth solar wind into three basic flow types based on inspection of solar wind plasma and magnetic field parameters in the OMNI database and additional data (e.g., geomagnetic indices, energetic particle, and cosmic ray observations). These flow types are: (1) High-speed streams associated with coronal holes at the Sun, (2) Slow, interstream solar wind, and (3) Transient flows originating with coronal mass ejections at the Sun, including interplanetary coronal mass ejections and the associated upstream shocks and post-shock regions. The solar wind classification in these previous studies commenced with observations in 1972. In the present study, as well as updating this classification to the end of 2011, we have extended the classification back to 1963, the beginning of near-Earth solar wind observations, thereby encompassing the complete solar cycles 20 to 23 and the ascending phase of cycle 24. We discuss the cycle-to-cycle variations in near-Earth solar wind structures and the related geomagnetic activity over more than four solar cycles, updating some of the results of our earlier studies.
C1 [Richardson, Ian G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Richardson, Ian G.] Univ Maryland, CRESST, College Pk, MD 20742 USA.
[Richardson, Ian G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Cane, Hilary V.] Univ Tasmania, Sch Math & Phys, Hobart, Tas, Australia.
RP Richardson, IG (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA.
EM ian.g.richardson@nasa.gov
OI Richardson, Ian/0000-0002-3855-3634
FU University of Delaware; Bartol Research Institute
FX We thank the many researchers who have made available near-Earth
magnetic field, plasma and energetic particle data that have contributed
to the solar wind identifications, and to J. King and colleagues at the
Space Physics Data Facility at GSFC for compiling the OMNI database. The
Thule neutron monitor (P.I. John Bieber) is supported by the University
of Delaware and the Bartol Research Institute. Data were obtained from
the Bartol web site (http://neutronm.bartol.udel.edu/). We acknowledge
discussions with E.W. Cliver that prompted extending the solar wind
classification back through cycle 20.
NR 84
TC 30
Z9 30
U1 0
U2 7
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 2115-7251
J9 J SPACE WEATHER SPAC
JI J. Space Weather Space Clim.
PY 2012
VL 2
AR UNSP A02
DI 10.1051/swsc/2012003
PG 10
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA 226AY
UT WOS:000325007800002
ER
PT J
AU Richardson, IG
Cane, HV
AF Richardson, Ian G.
Cane, Hilary V.
TI Solar wind drivers of geomagnetic storms during more than four solar
cycles
SO JOURNAL OF SPACE WEATHER AND SPACE CLIMATE
LA English
DT Article
DE Solar wind; Interplanetary Coronal Mass Ejection (CME); Storm; Stream;
Solar cycle
ID CORONAL MASS EJECTIONS; CATALOG; INDEXES; STREAMS; SIGNATURES; MINIMUM;
HOLES; NT
AB Using a classification of the near-Earth solar wind into three basic flow types: (1) High-speed streams associated with coronal holes at the Sun; (2) Slow, interstream solar wind; and (3) Transient flows originating with coronal mass ejections (CMEs) at the Sun, including interplanetary CMEs and the associated upstream shocks and post-shock regions, we determine the drivers of geomagnetic storms of various size ranges based on the Kp index and the NOAA "G'' criteria since 1964, close to the beginning of the space era, to 2011, encompassing more than four solar cycles (20-23). We also briefly discuss the occurrence of storms since the beginning of the Kp index in 1932, in the minimum before cycle 17. We note that the extended low level of storm activity during the minimum following cycle 23 is without precedent in this 80-year interval. Furthermore, the "typical'' numbers of storm days/cycle quoted in the standard NOAA G storm table appear to be significantly higher than those obtained from our analysis, except for the strongest (G5) storms, suggesting that they should be revised downward.
C1 [Richardson, Ian G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Richardson, Ian G.] Univ Maryland, CRESST, College Pk, MD 20742 USA.
[Richardson, Ian G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Cane, Hilary V.] Univ Tasmania, Sch Math & Phys, Hobart, Tas, Australia.
RP Richardson, IG (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA.
EM ian.g.richardson@nasa.gov
OI Richardson, Ian/0000-0002-3855-3634
NR 34
TC 21
Z9 21
U1 0
U2 5
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 2115-7251
J9 J SPACE WEATHER SPAC
JI J. Space Weather Space Clim.
PY 2012
VL 2
AR UNSP A01
DI 10.1051/swsc/2012001
PG 9
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA 226AY
UT WOS:000325007800001
ER
PT J
AU Tsurutani, BT
Verkhoglyadova, OP
Mannucci, AJ
Lakhina, GS
Huba, JD
AF Tsurutani, Bruce T.
Verkhoglyadova, Olga P.
Mannucci, Anthony J.
Lakhina, Gurbax S.
Huba, Joseph D.
TI Extreme changes in the dayside ionosphere during a Carrington-type
magnetic storm
SO JOURNAL OF SPACE WEATHER AND SPACE CLIMATE
LA English
DT Article
DE ionosphere (equatorial); ionosphere (mid latitude); electric field;
coronal mass ejection (CME); flares
ID LOW-LATITUDE IONOSPHERE; ELECTRIC-FIELDS; PENETRATION; SYSTEM; ORIGIN;
SECTOR; MODEL; SAMI2
AB It is shown that during the 30 October 2003 superstorm, dayside O+ ions were uplifted to DMSP altitudes (similar to 850 km). Peak densities were similar to 9 x 10(5) cm(-3) during the magnetic storm main phase (peak Dst = -390 nT). By comparison the 1-2 September 1859 Carrington magnetic storm (peak Dst estimated at -1760 nT) was considerably stronger. We investigate the impact of this storm on the low- to mid-latitude ionosphere using a modified version of the NRL SAMI2 ionospheric code. It is found that the equatorial region (LAT = 0 degrees +/- 15 degrees) is swept free of plasma within 15 min (or less) of storm onset. The plasma is swept to higher altitudes and higher latitudes due to E x B convection associated with the prompt penetration electric field. Equatorial Ionization Anomaly (EIA) O+ density enhancements are found to be located within the broad range of latitudes similar to +/- (25 degrees-40 degrees) at similar to 500-900 km altitudes. Densities within these peaks are similar to 6 x 10(6) oxygen ions-cm(-3) at similar to 700 km altitude, approximately +600% quiet time values. The oxygen ions at the top portions (850-1000 km) of uplifted EIAs will cause strong low-altitude satellite drag. Calculations are currently being performed on possible uplift of oxygen neutrals by ion-neutral coupling to understand if there might be further significant satellite drag forces present.
C1 [Tsurutani, Bruce T.; Verkhoglyadova, Olga P.; Mannucci, Anthony J.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Verkhoglyadova, Olga P.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA.
[Lakhina, Gurbax S.] Indian Inst Geomagnetism, Navi Mumbai, Maharashtra, India.
[Huba, Joseph D.] Naval Res Lab, Washington, DC USA.
RP Tsurutani, BT (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
EM bruce.tsurutani@jpl.nasa.gov
OI Lakhina, Gurbax /0000-0002-8956-486X; Verkhoglyadova,
Olga/0000-0002-9295-9539
FU NASA; Indian National Science Academy, New Delhi; NRL 6.1 Base Funds
FX Portions of this research effort were performed at the Jet Propulsion
Laboratory, California Institute of Technology under contract with the
NASA. GSL thanks the Indian National Science Academy, New Delhi for
support under the Senior Scientist Scheme. JDH thanks NRL 6.1 Base Funds
for support of this research. We gratefully acknowledge the Center for
Space Sciences at the University of Texas at Dallas and the U. S. Air
Force for providing the DMSP thermal plasma data.
NR 39
TC 13
Z9 13
U1 0
U2 5
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 2115-7251
J9 J SPACE WEATHER SPAC
JI J. Space Weather Space Clim.
PY 2012
VL 2
AR UNSP A05
DI 10.1051/swsc/2012004
PG 7
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA 226AY
UT WOS:000325007800005
ER
PT S
AU Prasad, NS
AF Prasad, Narasimha S.
BE Taylor, EW
Cardimona, DA
TI Performance testing of lidar components subjected to exposure in space
via MISSE 7 mission
SO NANOPHOTONICS AND MACROPHOTONICS FOR SPACE ENVIRONMENTS VI
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Nanophotonics and Macrophotonics for Space Environments VI
CY AUG 13-14, 2012
CL San Diego, CA
SP SPIE
DE MISSE 7; Space Qualification; Lidar components; International Space
Station (ISS); STS-129; STS-134
AB The objective of the Materials International Space Station Experiment (MISSE) is to study the performance of novel materials when subjected to the synergistic effects of the harsh space environment for several months. MISSE missions provide an opportunity for developing space qualifiable materials. Several laser and lidar components were sent by NASA Langley Research Center (LaRC) as a part of the MISSE 7 mission. The MISSE 7 module was transported to the international space station (ISS) via STS 129 mission that was launched on Nov 16, 2009. Later, the MISSE 7 module was brought back to the earth via the STS 134 that landed on June 1, 2011. The MISSE 7 module that was subjected to exposure in space environment for more than one and a half year included fiber laser, solid-state laser gain materials, detectors, and semiconductor laser diode. Performance testing of these components is now progressing. In this paper, the current progress on post-flight performance testing of a high-speed photodetector and a balanced receiver is discussed. Preliminary findings show that detector characteristics did not undergo any significant degradation.
C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Prasad, NS (reprint author), NASA, Langley Res Ctr, 5 N Dryden St,MS 468, Hampton, VA 23681 USA.
EM narasimha.s.prasad@nasa.gov
NR 3
TC 0
Z9 0
U1 1
U2 2
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-9236-4
J9 PROC SPIE
PY 2012
VL 8519
AR 85190O
DI 10.1117/12.933275
PG 8
WC Nanoscience & Nanotechnology; Optics; Physics, Applied
SC Science & Technology - Other Topics; Optics; Physics
GA BHG04
UT WOS:000325297900019
ER
PT B
AU Lorenzo, CF
Malti, R
Hartley, TT
AF Lorenzo, Carl F.
Malti, Rachid
Hartley, Tom T.
GP ASME
TI THE SOLUTION OF LINEAR FRACTIONAL DIFFERENTIAL EQUATIONS USING THE
FRACTIONAL META-TRIGONOMETRIC FUNCTIONS
SO PROCEEDINGS OF THE ASME INTERNATIONAL DESIGN ENGINEERING TECHNICAL
CONFERENCES AND COMPUTERS AND INFORMATION IN ENGINEERING CONFERENCE,
2011, VOL 3, PTS A AND B
LA English
DT Proceedings Paper
CT ASME Internationl Design Engineering Technical Conferences / Computers
and Information in Engineering Conference (IDETC/CIE)
CY AUG 28-31, 2011
CL Washington, DC
SP Amer Soc Mech Engineers, Design Engn Div, Amer Soc Mech Engineers, Comp & Informat Engn Div
DE Fractional Differential Equations; Fractional Meta-Trigonometric
Functions; R-Function
AB A new method for the solution of linear constant coefficient fractional differential equations of any commensurate order based on the Laplace transforms of the fractional meta-trigonometric functions and the R-function is presented. The new method simplifies the solution of such equations. A simplifying characterization that reduces the number of parameters in the fractional meta-trigonometric functions is introduced.
C1 [Lorenzo, Carl F.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Lorenzo, CF (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM Carl.F.Lorenzo@nasa.gov; rachid.malti@ims-bordeaux.fr;
thartley@uakron.edu
NR 17
TC 0
Z9 0
U1 0
U2 0
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-5479-2
PY 2012
BP 155
EP 161
PG 7
WC Engineering, Electrical & Electronic; Engineering, Mechanical
SC Engineering
GA BGU93
UT WOS:000324221300021
ER
PT B
AU Lorenzo, CF
Hartley, TT
AF Lorenzo, Carl F.
Hartley, Tom T.
GP ASME
TI TIME-VARYING INITIALIZATION AND LAPLACE TRANSFORM OF THE CAPUTO
DERIVATIVE: WITH ORDER BETWEEN ZERO AND ONE
SO PROCEEDINGS OF THE ASME INTERNATIONAL DESIGN ENGINEERING TECHNICAL
CONFERENCES AND COMPUTERS AND INFORMATION IN ENGINEERING CONFERENCE,
2011, VOL 3, PTS A AND B
LA English
DT Proceedings Paper
CT ASME Internationl Design Engineering Technical Conferences / Computers
and Information in Engineering Conference (IDETC/CIE)
CY AUG 28-31, 2011
CL Washington, DC
SP Amer Soc Mech Engineers, Design Engn Div, Amer Soc Mech Engineers, Comp & Informat Engn Div
DE Initialization function; Caputo derivative; Laplace transform
AB This paper derives the time-varying initialization function for the Caputo derivative with order between zero and one. The derivative is redefined to include this initialization function. Then, the Laplace transform for the redefined Caputo derivative is determined which corrects (supplants) that given for the derivative in the literature and properly accounts for time-varying initialization effects.
C1 [Lorenzo, Carl F.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Lorenzo, CF (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
EM Carl.F.Lorenzo@nasa.gov; thartley@uakron.edu
NR 11
TC 0
Z9 0
U1 0
U2 0
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-5479-2
PY 2012
BP 163
EP 168
PG 6
WC Engineering, Electrical & Electronic; Engineering, Mechanical
SC Engineering
GA BGU93
UT WOS:000324221300022
ER
PT B
AU Lyver, JW
Prassinos, PG
Bui, CT
AF Lyver, John W.
Prassinos, Peter G.
Bui, Chinh T.
GP ASME
TI DESIGNING IN SAFETY THROUGH EARLY SAFETY REQUIREMENTS MANAGEMENT
SO PROCEEDINGS OF THE ASME INTERNATIONAL MECHANICAL ENGINEERING CONGRESS
AND EXPOSITION, 2011, VOL 9
LA English
DT Proceedings Paper
CT ASME International Mechanical Engineering Congress and Exposition
(IMECE)
CY NOV 11-17, 2011
CL Denver, CO
SP Amer Soc Mech Engn
AB The National Aeronautics and Space Administration (NASA) has developed a set of Agency-level requirements which cover the risk areas associated with the safety, reliability, maintainability and quality assurance disciplines. This set of requirements applies to NASA activities ranging from space exploration to aeronautics research to product quality to the protection of the NASA family. With the establishment of NASA's new human exploration programs, NASA realized that it needed to develop a methodology for sorting through the wide variety of knowledge captured in the Agency requirements and identify how those requirements are applicable to each emerging program. This paper will highlight the process used by NASA to filter the thousands of requirements into a concise set which would reduce overall programmatic risk without overburdening the program.
C1 [Lyver, John W.; Prassinos, Peter G.] NASA, Washington, DC 20546 USA.
RP Lyver, JW (reprint author), NASA, Washington, DC 20546 USA.
NR 2
TC 0
Z9 0
U1 0
U2 0
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-5495-2
PY 2012
BP 697
EP 701
PG 5
WC Engineering, Mechanical; Transportation Science & Technology
SC Engineering; Transportation
GA BGZ58
UT WOS:000324716700075
ER
PT S
AU Bryant, N
Bunch, W
Fretz, R
Kim, P
Logan, T
Smyth, M
Zobrist, A
AF Bryant, N.
Bunch, W.
Fretz, R.
Kim, P.
Logan, T.
Smyth, M.
Zobrist, A.
GP IEEE
TI Obtaining Accurate Change Detection Results From High-Resolution
Satellite Sensors
SO 2012 IEEE APPLIED IMAGERY PATTERN RECOGNITION WORKSHOP (AIPR)
SE IEEE Applied Imagery Pattern Recognition Workshop
LA English
DT Proceedings Paper
CT IEEE Applied Imagery Pattern Recognition Workshop (AIPR)
CY OCT 09-11, 2012
CL Washington, DC
SP IEEE
ID MISREGISTRATION; CLASSIFICATION
AB Multi-date acquisitions of high-resolution imaging satellites (e.g. GeoEye and WorldView), can display local changes of current economic interest. However, their large data volume precludes effective manual analysis, requiring image co-registration followed by image-to-image change detection, preferably with minimal analyst attention. We have recently developed an automatic change detection procedure that minimizes false-positives. The processing steps include: (a) Conversion of both the pre- and post-images to reflectance values (this step is of critical importance when different sensors are involved); reflectance values can be either top-of-atmosphere units or have full aerosol optical depth calibration applied using bi-directional reflectance knowledge. (b) Panchromatic band image-to-image co-registration, using an orthorectified base reference image (e.g. Digital Orthophoto Quadrangle) and a digital elevation model; this step can be improved if a stereo-pair of images have been acquired on one of the image dates. (c) Pan-sharpening of the multispectral data to assure recognition of change objects at the highest resolution. (d) Characterization of multispectral data in the post-image (i.e. the background) using unsupervised cluster analysis. (e) Band ratio selection in the post-image to separate surface materials of interest from the background. (f) Preparing a pre-to-post change image. (g) Identifying locations where change has occurred involving materials of interest.
C1 [Bryant, N.; Bunch, W.; Fretz, R.; Kim, P.; Logan, T.; Smyth, M.; Zobrist, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Bryant, N (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 38
TC 0
Z9 0
U1 2
U2 3
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 1550-5219
BN 978-1-4673-4558-3; 978-1-4673-4556-9
J9 IEEE APP IMG PAT
PY 2012
PG 5
WC Computer Science, Artificial Intelligence; Engineering, Electrical &
Electronic
SC Computer Science; Engineering
GA BGV67
UT WOS:000324312300011
ER
PT S
AU Li, J
Hylton, A
Budinger, J
Nappier, J
Downey, J
Raible, D
AF Li (Tiffany), Jing
Hylton, Alan
Budinger, James
Nappier, Jennifer
Downey, Joseph
Raible, Daniel
GP IEEE
TI Dual-pulse Pulse Position Modulation (DPPM) for Deep-Space Optical
Communications: Performance and Practicality Analysis
SO 2012 INTERNATIONAL CONFERENCE ON WIRELESS COMMUNICATIONS AND SIGNAL
PROCESSING (WCSP 2012)
SE International Conference on Wireless Communications and Signal
Processing
LA English
DT Proceedings Paper
CT 4th International Conference on Wireless Communications and Signal
Processing (WCSP)
CY OCT 25-27, 2012
CL Huangshan, PEOPLES R CHINA
SP IEEE, IEEE Commun Soc, SE Univ, IEEE Commun Soc Nanjing Chapter, IEEE Signal Proc Soc Nanjing Chapter, Univ Sci & Technol China, Huawei Technologies Co Ltd
DE dual-pulse pulse position modulation (DPPM); strong turbulence;
negative-exponential fading; bit/symbol error rate; energy efficiency;
bandwidth efficiency; channel capacity
ID ATMOSPHERIC-TURBULENCE; PPM; CHANNELS; SYSTEMS
AB Due to its simplicity and robustness against wave-front distortion, pulse position modulation (PPM) with photon counting detector has been seriously considered for long-haul optical wireless systems. This paper evaluates the dual-pulse case and compares it with the conventional single-pulse case. Analytical expressions for symbol error rate and bit error rate are first derived and numerically evaluated, for the strong, negative-exponential turbulent atmosphere. The capacity of the turbulent FSO channel modeled as a Z-channel is evaluated, and throughput, bandwidth efficiency and energy efficiency of Dual-pulse and single-pulse PPM are subsequently assessed. It is shown that, under a set of practical constraints including pulse width and pulse repetition frequency (PRF), dual-pulse PPM enables a better channel utilization and hence a higher throughput than its single-pulse counterpart. This result is new and different from the previous idealistic studies that showed multi-pulse PPM provided no essential information-theoretic gains over single-pulse PPM.
C1 [Li (Tiffany), Jing] Lehigh Univ, Dept Elect & Comp Engn, Bethlehem, PA 18015 USA.
[Hylton, Alan; Budinger, James; Nappier, Jennifer; Downey, Joseph; Raible, Daniel] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Li, J (reprint author), Lehigh Univ, Dept Elect & Comp Engn, Bethlehem, PA 18015 USA.
EM jingli@ece.lehigh.edu; alan.g.hylton@nasa.gov;
james.m.budinger@nasa.gov; jennifer.m.nappier@nasa.gov;
joseph.a.downey@nasa.gov; daniel.e.raible@nasa.gov
FU NASA under Glenn Faculty Fellowship; NSF [CMMI-0928092, CCF-0829888,
OCI-1122027]
FX Lis work is supported by NASA under Glenn Faculty Fellowship. Her work
also received partial support from NSF under Grants No. CMMI-0928092,
CCF-0829888 and OCI-1122027
NR 15
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 2325-3746
BN 978-1-4673-5829-3; 978-1-4673-5830-9
J9 INT CONF WIRE COMMUN
PY 2012
PG 7
WC Engineering, Electrical & Electronic; Telecommunications
SC Engineering; Telecommunications
GA BGZ71
UT WOS:000324751500094
ER
PT S
AU Davis, DO
Friedlander, DJ
Saunders, JD
Frate, FC
Foster, LE
AF Davis, David O.
Friedlander, David J.
Saunders, J. David
Frate, Franco C.
Foster, Lancert E.
GP ASME
TI CALIBRATION OF THE NASA GRC 16 '' MASS-FLOW PLUG
SO PROCEEDINGS OF THE ASME FLUIDS ENGINEERING DIVISION SUMMER MEETING, VOL
2: FORA
SE ASME Fluids Engineering Division Summer Meeting
LA English
DT Proceedings Paper
CT ASME Fluids Engineering Division Summer Meeting (FEDSM)
CY JUL 08-12, 2012
CL Rio Grande, PR
SP ASME, Fluids Engn Div
AB The results of an experimental calibration of the NASA Glenn Research Center 16 '' Mass-Flow Plug (MFP) are presented and compared to a previously obtained calibration of a 15 '' Mass-Flow Plug. An ASME low-beta, long-radius nozzle was used as the calibration reference. The discharge coefficient for the ASME nozzle was obtained by numerically simulating the flow through the nozzle from the WIND-US code. The results showed agreement between the 15 '' and 16 '' MFPs for area ratios (MFP to pipe area ratio) greater than 0.6 but deviate at area ratios below this value for reasons that are not fully understood. A general uncertainty analysis was also performed and indicates that large uncertainties in the calibration are present for low MFP area ratios.
C1 [Davis, David O.; Friedlander, David J.; Saunders, J. David; Foster, Lancert E.] NASA, Glenn Res Ctr, Cleveland, OH USA.
RP Davis, DO (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA.
NR 16
TC 0
Z9 0
U1 0
U2 0
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
SN 1093-4928
BN 978-0-7918-4476-2
J9 ASME FLUID ENG DIV
PY 2012
BP 269
EP 277
PG 9
WC Engineering, Mechanical
SC Engineering
GA BGX51
UT WOS:000324507600031
ER
PT B
AU Mukherjee, RM
Houlihan, R
AF Mukherjee, Rudranarayan M.
Houlihan, Ryan
GP ASME
TI MASSIVELY PARALLEL GRANULAR MEDIA MODELING OF ROBOT-TERRAIN INTERACTIONS
SO PROCEEDINGS OF THE ASME INTERNATIONAL DESIGN ENGINEERING TECHNICAL
CONFERENCES AND COMPUTERS AND INFORMATION IN ENGINEERING CONFERENCE, VOL
6
LA English
DT Proceedings Paper
CT ASME International Design Engineering Technical Conferences and
Computers and Information in Engineering Conference
CY AUG 12-15, 2012
CL Chicago, IL
SP ASME, Design Engn Div, ASME, Comp & Informat Engn Div
ID CONTACT DETECTION ALGORITHM
AB This paper presents select results that demonstrate the feasibility of modeling the interactions of robotic systems with granular terrain through Discrete Element Modeling (DEM) using massively parallel computing systems. We report numerical simulation results of full 3D DEM simulations with the granular material modeled as a deformable bed of spherical granules. The mobility systems of the robots retain their CAD geometry and are represented as triangular meshes. The inter-granular interactions and the interactions between the CAD mesh triangles with the granules are modeled explicitly using a deformation-damping force field. The parameters of the force field are derived from physically measurable properties. We model friction, cohesion, and shearing and other interactions among the granules, and between the CAD mesh and the granules. The simulations involve granular beds with number of granules in the order of several hundred thousand to several millions. Temporally, we report simulations in the order of several seconds. These simulations were run on parallel clusters with number of processors ranging from 100 to 256. We present the findings from a number of simulations ranging including wheeled and legged mobility systems, and robotic tools in micro-gravity environments.
C1 [Mukherjee, Rudranarayan M.] CALTECH, Jet Prop Lab, NASA, Mobil & Robot Syst Sect, Pasadena, CA 91109 USA.
RP Mukherjee, RM (reprint author), CALTECH, Jet Prop Lab, NASA, Mobil & Robot Syst Sect, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Rudranarayan.M.Mukherjee@jpl.nasa.gov; ryan.houlihan90@gmail.com
NR 17
TC 1
Z9 1
U1 0
U2 0
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-4505-9
PY 2012
BP 71
EP 78
PG 8
WC Engineering, Manufacturing; Engineering, Mechanical; Transportation
Science & Technology
SC Engineering; Transportation
GA BGW22
UT WOS:000324346500009
ER
PT J
AU Gabb, TP
Kantzos, PT
Palsa, B
Telesman, J
Gayda, J
Sudbrack, CK
AF Gabb, Tim P.
Kantzos, Pete T.
Palsa, Bonny
Telesman, Jack
Gayda, John
Sudbrack, Chantal K.
BE Huron, ES
Reed, RC
Hardy, MC
Mills, MJ
Montero, RE
Portella, PD
Telesman, J
TI FATIGUE FAILURE MODES OF THE GRAIN SIZE TRANSITION ZONE IN A DUAL
MICROSTRUCTURE DISK
SO SUPERALLOYS 2012
LA English
DT Proceedings Paper
CT 12th International Symposium on Superalloys
CY SEP 09-13, 2012
CL Seven Springs, PA
SP TMS
DE dual microstructure; transition zone; fatigue
ID SUPERALLOY
AB Mechanical property requirements vary with location in nickel-based superalloy disks. In order to maximize the associated mechanical properties, heat treatment methods have been developed for producing tailored grain microstructures. In this study, fatigue failure modes of a grain size transition zone in a dual microstructure disk were evaluated. A specialized heat treatment method was applied to produce varying grain microstructure in the bore to rim portions of a powder metallurgy processed nickel-based superalloy disk. The transition in grain size was concentrated in a zone of the disk web, between the bore and rim. Specimens were extracted parallel and transversely across this transition zone, and multiple fatigue tests were performed at 427 degrees C and 704 degrees C. Grain size distributions were characterized in the specimens, and related to operative failure initiation modes. Mean fatigue life decreased with increasing maximum grain size, going out through the transition zone. The scatter in limited tests of replicates was comparable for failures of uniform gage specimens in all transition zone locations examined.
C1 [Gabb, Tim P.; Palsa, Bonny; Telesman, Jack; Gayda, John; Sudbrack, Chantal K.] NASA Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
[Kantzos, Pete T.] Honeywell Engine Syst, Cleveland, OH USA.
RP Gabb, TP (reprint author), NASA Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
FU NASA Aviation Safety program
FX The authors wish to acknowledge the support of the NASA Aviation Safety
program. Disk forging was performed at PCC WymanGordon Forgings under
the direction of Ian Dempster. Disk heat treatments were performed at
Ladish Forgings, Inc. under the direction of Joe Lemsky, and David
Furrer, now at Rolls-Royce Aircraft Engines.
NR 20
TC 0
Z9 0
U1 0
U2 0
PU JOHN WILEY & SONS
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER, W SUSSEX PO 19 8SQ, ENGLAND
BN 978-0-470-94320-5
PY 2012
BP 63
EP 72
PG 10
WC Metallurgy & Metallurgical Engineering
SC Metallurgy & Metallurgical Engineering
GA BGX57
UT WOS:000324518300007
ER
PT J
AU Telesman, J
Gabb, TP
Yamada, Y
Ghosn, LJ
Hombach, D
Jayaraman, N
AF Telesman, J.
Gabb, T. P.
Yamada, Y.
Ghosn, L. J.
Hombach, D.
Jayaraman, N.
BE Huron, ES
Reed, RC
Hardy, MC
Mills, MJ
Montero, RE
Portella, PD
Telesman, J
TI DWELL NOTCH LOW CYCLE FATIGUE BEHAVIOR OF A POWDER METALLURGY NICKEL
DISK ALLOY
SO SUPERALLOYS 2012
LA English
DT Proceedings Paper
CT 12th International Symposium on Superalloys
CY SEP 09-13, 2012
CL Seven Springs, PA
SP TMS
DE Notch Low Cycle Fatigue; Dwells; Oxidation; Vacuum; Alloy ME3
AB A study was conducted to determine the processes which govern dwell notch low cycle fatigue (NLCF) behavior of a powder metallurgy (P/M) ME3 disk superalloy. The emphasis was placed on the environmentally driven mechanisms which may embrittle the highly stressed notch surface regions and reduce NLCF life. In conjunction with the environmentally driven notch surface degradation processes, the visco-plastic driven mechanisms which can significantly change the notch root stresses were also considered.
Dwell notch low cycle fatigue testing was performed in air and vacuum on a ME3 P/M disk alloy specimens heat treated using either a fast or a slow cooling rate from the solutioning treatment. It was shown that dwells at the minimum stress typically produced a greater life debit than the dwells applied at the maximum stress, especially for the slow cooled heat treatment. Two different environmentally driven failure mechanisms were identified as the root cause of early crack initiation in the min dwell tests. Both of these failure mechanisms produced mostly a transgranular crack initiation failure mode and yet still resulted in low NLCF fatigue lives. The lack of stress relaxation during the min dwell tests produced higher notch root stresses which caused early crack initiation and premature failure when combined with the environmentally driven surface degradation mechanisms.
The importance of environmental degradation mechanisms was further highlighted by vacuum dwell NLCF tests which resulted in considerably longer NLCF lives, especially for the min dwell tests.
C1 [Telesman, J.; Gabb, T. P.; Ghosn, L. J.] NASA, Glenn Res Ctr, Cleveland, OH USA.
[Yamada, Y.] Ohio Aerosp Inst, Brookpark, OH USA.
[Jayaraman, N.] Lambda Res Inc, Cincinnati, OH USA.
RP Telesman, J (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA.
FU NASA Aviation Safety program
FX The authors wish to acknowledge the support of the NASA Aviation Safety
program. The assistance of Dr. Rick Rogers and Mr. David Hull in
performing x-ray diffraction analysis and the FIB-SEM microscopy work is
gratefully acknowledged. The authors are particularly grateful for
advice and assistance of Ms. Sue Draper, Dr. Chantal Sudbrack and Mr.
Pete Kantzos.
NR 5
TC 4
Z9 4
U1 0
U2 0
PU JOHN WILEY & SONS
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER, W SUSSEX PO 19 8SQ, ENGLAND
BN 978-0-470-94320-5
PY 2012
BP 853
EP 862
PG 10
WC Metallurgy & Metallurgical Engineering
SC Metallurgy & Metallurgical Engineering
GA BGX57
UT WOS:000324518300094
ER
PT J
AU Sudbrack, CK
Draper, SL
Gorman, TT
Telesman, J
Gabb, TP
Hull, DR
AF Sudbrack, Chantal K.
Draper, Susan L.
Gorman, Timothy T.
Telesman, Jack
Gabb, Timothy P.
Hull, David R.
BE Huron, ES
Reed, RC
Hardy, MC
Mills, MJ
Montero, RE
Portella, PD
Telesman, J
TI OXIDATION AND THE EFFECTS OF HIGH TEMPERATURE EXPOSURES ON NOTCHED
FATIGUE LIFE OF AN ADVANCED POWDER METALLURGY DISK SUPERALLOY
SO SUPERALLOYS 2012
LA English
DT Proceedings Paper
CT 12th International Symposium on Superalloys
CY SEP 09-13, 2012
CL Seven Springs, PA
SP TMS
DE disk; superalloys; oxidation; low cycle fatigue; environment
ID GROWTH
AB Oxidation and the effects of high temperature exposures on notched fatigue life were considered for a powder metallurgy processed supersolvus heat-treated ME3 disk superalloy. The isothermal static oxidation response at 704 degrees C, 760 degrees C, and 815 degrees C was consistent with other chromia forming nickel-based superalloys: TiO2-Cr2O3 external oxide formed with a branched Al2O3 internal subscale that extended into a recrystallized gamma'-dissolution layer. These surface changes can potentially impact disk durability, making layer growth rates important. Growth of the external scales and gamma' dissolution layers followed a cubic rate law, while Al2O3 subscales followed a parabolic rate law. Cr- rich M23C6 carbides at the grain boundaries dissolved to help sustain Cr2O3 growth to depths about 12 times thicker than the scale.
The effect of prior exposures was examined through notched low cycle fatigue tests performed to failure in air at 704 degrees C. Prior exposures led to pronounced debits of up to 99 % in fatigue life, where fatigue life decreased inversely with exposure time. Exposures that produced roughly equivalent 1 mu m thick external scales at the various isotherms showed statistically equivalent fatigue lives, establishing that surface damage drives fatigue debit, not exposure temperature. Fractographic evaluation indicated the failure mode for the pre-exposed specimens involved surface crack initiations that shifted with exposure from predominately single intergranular initiations with transgranular propagation to multi-initiations from the cracked external oxide with intergranular propagation. Weakened grain boundaries at the surface resulting from the M23C6 carbide dissolution are partially responsible for the intergranular cracking. Removing the scale and subscale while leaving a layer where M23C6 carbides were dissolved did not lead to a significant fatigue life improvement, however, also removing the M23C6 carbide dissolution layer led to nearly full recovery of life, with a transgranular initiation typical to that observed in unexposed specimens.
C1 [Sudbrack, Chantal K.; Draper, Susan L.; Gorman, Timothy T.; Telesman, Jack; Gabb, Timothy P.; Hull, David R.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Sudbrack, CK (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA.
NR 14
TC 10
Z9 10
U1 1
U2 2
PU JOHN WILEY & SONS
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER, W SUSSEX PO 19 8SQ, ENGLAND
BN 978-0-470-94320-5
PY 2012
BP 863
EP 872
PG 10
WC Metallurgy & Metallurgical Engineering
SC Metallurgy & Metallurgical Engineering
GA BGX57
UT WOS:000324518300095
ER
PT S
AU Liang, XM
Ignatov, A
Liu, QH
Chen, Y
Groff, D
Xiong, XX
Cao, CY
Borbas, E
Hook, S
AF Liang, XingMing
Ignatov, Alexander
Liu, Quanhua
Chen, Yong
Groff, David
Xiong, Xiaoxiong
Cao, Changyong
Borbas, Eva
Hook, Simon
BE Shimoda, H
Xiong, X
TI Improvements to radiometric consistency between AVHRR, MODIS, and VIIRS
in SST bands using MICROS online near-real time system
SO EARTH OBSERVING MISSIONS AND SENSORS: DEVELOPMENT, IMPLEMENTATION, AND
CHARACTERIZATION II
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Earth Observing Missions and Sensors - Development,
Implementation, and Characterization II
CY OCT 30-NOV 01, 2012
CL Kyoto, JAPAN
SP SPIE, Japan Aerosp Explorat Agcy (JAXA), Natl Aeronaut & Space Adm (NASA), Natl Inst Informat & Commun Technol, Commemorat Org Japan World Exposit, Indian Space Res Org (ISRO), State Key Lab Remote Sensing Sci
DE MICROS; Double Differences; Cross-platform consistency; M-O bias; CRTM;
AVHRR; MODIS; VIIRS
ID SEA-SURFACE TEMPERATURE; RADIANCES; VALIDATION; SATELLITE; OCEANS;
MODEL; AIRS
AB Monitoring of IR Clear-Sky Radiances over Oceans for SST (MICROS; www.star.nesdis.noaa.gov/sod/sst/micros) near-real time web-based system has been established in July 2008. It analyzes Model (Community Radiative Transfer Model, CRTM) minus Observation (M-O) biases in clear-sky ocean brightness temperatures (BT) in AVHRR bands 3.7 (IR37), 11 (IR11), and 12 mu m (IR12) onboard NOAA-16, -17, -18, -19 and Metop-A. In January 2012, AVHRR-like bands of VIIRS onboard the Suomi National Polar Partnership (S-NPP; launched in October 2012), and two MODIS instruments onboard Terra and Aqua, were included in MICROS. Double-differences are employed to check various sensors for radiometric consistency. The VIIRS and AVHRR have been in-family, and the consistency further improved after the VIIRS IR calibration was fine-tuned on 7 March 2012. However, MODIS M-O biases have been out of family (by -0.6K in IR 11, and -0.3K in IR12). Analyses have shown that these anomalies in MODIS M-O biases are caused by the "M" term, i.e., incorrect MODIS transmittance coefficients in CRTM v2.02. Based on feedback from NESDIS SST and U. Wisconsin Teams, CRTM Team updated transmittance coefficients in CRTM v2.10. As a result, MODIS M-O biases are now in agreement with AVHRR/VIIRS. However, cross-platform Terra/Aqua bias of similar to 0.3 K in Ch20 (3.9 mu m) remains, likely due to calibration uncertainties in MODIS L1b product. This paper documents the joint effort by the SST, MODIS Characterization Support and CRTM Teams towards identifying and resolving observed cross-platform inconsistencies.
C1 [Liang, XingMing; Ignatov, Alexander; Liu, Quanhua; Chen, Yong; Cao, Changyong] NOAA, NESDIS, Ctr Satellite Applicat & Res STAR, College Pk, MD 20740 USA.
[Liang, XingMing; Chen, Yong] Colorado State Univ, CIRA, Ft Collins, CO 80523 USA.
[Liu, Quanhua] IMSG Inc, Rockville, MD USA.
[Groff, David] Natl Centers Environm Predict, College Pk, MD 20746 USA.
[Xiong, Xiaoxiong; Cao, Changyong] NASA, GSFC, Sci Explorat Directorate, Greenbelt, MD 20771 USA.
[Borbas, Eva] Univ Wisconsin Madison, Madison, WI 53706 USA.
[Hook, Simon] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Hook, Simon] NASA, Jet Prop Lab, Washington, DC USA.
RP Liang, XM (reprint author), NOAA, NESDIS, Ctr Satellite Applicat & Res STAR, College Pk, MD 20740 USA.
RI Cao, Changyong/F-5578-2010; Liu, Quanhua/B-6608-2008; Liang,
Xingming/H-7368-2014; Ignatov, Alexander/F-5594-2010; Chen,
Yong/E-4321-2010
OI Liu, Quanhua/0000-0002-3616-351X; Liang, Xingming/0000-0001-5641-0509;
Ignatov, Alexander/0000-0002-7463-5944; Chen, Yong/0000-0002-0279-9405
FU JPSS and GOES-R Program Offices; NOAA PSDI and Ocean Remote Sensing
Programs
FX This work is supported by the JPSS and GOES-R Program Offices, and NOAA
PSDI and Ocean Remote Sensing Programs. CRTM is provided by the NESDIS
Joint Center for Satellite Data Assimilation. XL and YC acknowledge the
CSU/CIRA visiting scientist fellowship. Thanks to John Sapper, Yury
Kihai, John Stroup, Boris Petrenko, and Korak Saha of NESDIS for
contributions to ACSPO and MICROS development, and data collection and
processing. Thanks also to Fred Wu, Fangfang Yu, Paul Van Delst, and
Fuzhong Weng of NESDIS and Tim Hewison of EUMETSAT for helpful
discussions. 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.
NR 23
TC 0
Z9 0
U1 0
U2 3
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-9267-8
J9 PROC SPIE
PY 2012
VL 8528
AR 85280I
DI 10.1117/12.979597
PG 12
WC Remote Sensing; Optics
SC Remote Sensing; Optics
GA BDH77
UT WOS:000313295300013
ER
PT S
AU Barbee, BW
Alfano, S
Pinon, E
Gold, K
Gaylor, D
AF Barbee, Brent W.
Alfano, Salvatore
Pinon, Elfego
Gold, Kenn
Gaylor, David
BE Osborne, ML
TI DESIGN OF SPACECRAFT MISSIONS TO REMOVE MULTIPLE ORBITAL DEBRIS OBJECTS
SO GUIDANCE AND CONTROL 2012
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 35th Annual AAS Rocky Mountain Section Guidance and Control Conference
CY FEB 03-08, 2012
CL Breckenridge, CO
SP AAS, Rocky Mt Sect
AB The amount of hazardous debris in Earth orbit has been increasing, posing an ever-greater danger to space assets and human missions. In January of 2007, a Chinese ASAT test produced approximately 2600 pieces of orbital debris. In February of 2009, Iridium 33 collided with an inactive Russian satellite, yielding approximately 1300 pieces of debris. These recent disastrous events and the sheer size of the Earth orbiting population make clear the necessity of removing orbital debris. In fact, experts from both NASA and ESA have stated that 10 to 20 pieces of orbital debris need to be removed per year to stabilize the orbital debris environment. However, no spacecraft trajectories have yet been designed for removing multiple debris objects and the size of the debris population makes the design of such trajectories a daunting task. Designing an efficient spacecraft trajectory to rendezvous with each of a large number of orbital debris pieces is akin to the famous Traveling Salesman problem, an NP-complete combinatorial optimization problem in which a number of cities are to be visited in turn. The goal is to choose the order in which the cities are visited so as to minimize the total path distance traveled. In the case of orbital debris, the pieces of debris to be visited must be selected and ordered such that spacecraft propellant consumption is minimized or at least kept low enough to be feasible. Emergent Space Technologies, Inc. has developed specialized algorithms for designing efficient tour missions for near-Earth asteroids that may be applied to the design of efficient spacecraft missions capable of visiting large numbers of orbital debris pieces. The first step is to identify a list of high priority debris targets using the Analytical Graphics, Inc. SOCRATES website and then obtain their state information from Celestrak. The tour trajectory design algorithms will then be used to determine the itinerary of objects and Delta v requirements. These results will shed light on how many debris pieces can be visited for various amounts of propellant, which launch vehicles can accommodate such missions, and how much margin is available for debris removal system payloads.
C1 [Barbee, Brent W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Barbee, BW (reprint author), NASA, Goddard Space Flight Ctr, Code 595,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
NR 11
TC 1
Z9 1
U1 0
U2 3
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-585-5
J9 ADV ASTRONAUT SCI
PY 2012
VL 144
BP 93
EP 110
PG 18
WC Engineering, Aerospace
SC Engineering
GA BFX61
UT WOS:000321807500006
ER
PT S
AU Sparks, L
AF Sparks, Lawrence
BE Osborne, ML
TI ADDRESSING THE INFLUENCE OF SPACE WEATHER ON AIRLINE NAVIGATION
SO GUIDANCE AND CONTROL 2012
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 35th Annual AAS Rocky Mountain Section Guidance and Control Conference
CY FEB 03-08, 2012
CL Breckenridge, CO
SP AAS, Rocky Mt Sect
AB The advent of satellite-based augmentation systems has made it possible to navigate aircraft safely using radio signals emitted by global navigation satellite systems (GNSS) such as the Global Positioning System. As a signal propagates through the earth's ionosphere, it suffers delay that is proportional to the total electron content encountered along the raypath. Since the magnitude of this total electron content is strongly influenced by space weather, the safety and reliability of GNSS for airline navigation requires continual monitoring of the state of the ionosphere and calibration of ionospheric delay. This paper examines the impact of space weather on GNSS-based navigation and provides an overview of how the Wide Area Augmentation System protects its users from positioning error due to ionospheric disturbances.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Sparks, L (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 6
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-585-5
J9 ADV ASTRONAUT SCI
PY 2012
VL 144
BP 131
EP 144
PG 14
WC Engineering, Aerospace
SC Engineering
GA BFX61
UT WOS:000321807500009
ER
PT S
AU Fitzpatrick, H
DeWeese, K
AF Fitzpatrick, Henry
DeWeese, Keith
BE Osborne, ML
TI SAFEHOLD ATTITUDE DETERMINATION APPROACH FOR GPM
SO GUIDANCE AND CONTROL 2012
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 35th Annual AAS Rocky Mountain Section Guidance and Control Conference
CY FEB 03-08, 2012
CL Breckenridge, CO
SP AAS, Rocky Mt Sect
AB Spacecraft sating designs generally have minimal goals with loose pointing requirements. Safe pointing orientations for three-axis stabilized spacecraft are usually chosen to put the spacecraft into a thermally safe and power-positive orientation. In addition, safe mode designs are required to be simple and reliable. This simplicity lends itself to the usage of analog sun sensors, because digital sun sensors will add unwanted complexity to the safe hold mode.
The Global Precipitation Measurement (GPM) Mission Core Observatory will launch into lower earth orbit (LEO) at an inclination of 65 degrees. The GPM instrument suite consists of an active radar system and a passive microwave imager to provide the next-generation global observations of rain and snow. The complexity and precision of these instruments along with the operational constraints of the mission result in tight pointing requirements during all phases of the mission. To ensure the instruments are not damaged during spacecraft safing, thermal constraints dictate that the solar pointing orientation must be maintained to better than 6.5 degrees. This requirement is outside the capabilities of a typical analog sun sensor suite, primarily due to the effects of Earth's albedo. To ensure mission success, a new analog sensor, along with the appropriate algorithms, is needed.
This paper discusses the design issues involving albedo effects on spacecraft pointing and the development of a simple, low-cost analog sensor and algorithm that will address the needs of the GPM mission. In addition, the algorithms are designed to be easily integrated into the existing attitude determination software by using common interfaces. The sensor design is based on a heritage, commercial off-the-shelf analog sun sensors with a limited field-of-view to reduce the effects of Earth's albedo. High fidelity simulation results are presented that demonstrate the efficacy of the design.
C1 [Fitzpatrick, Henry; DeWeese, Keith] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Fitzpatrick, H (reprint author), NASA, Goddard Space Flight Ctr, Code 591, Greenbelt, MD 20771 USA.
NR 2
TC 1
Z9 1
U1 0
U2 1
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-585-5
J9 ADV ASTRONAUT SCI
PY 2012
VL 144
BP 213
EP 222
PG 10
WC Engineering, Aerospace
SC Engineering
GA BFX61
UT WOS:000321807500015
ER
PT S
AU Welter, G
Liu, KC
Blaurock, C
AF Welter, Gary
Liu, Kuo Chia (Alice)
Blaurock, Carl
BE Osborne, ML
TI GIMBAL CONTROL ALGORITHMS FOR THE GLOBAL PRECIPITATION MEASUREMENT CORE
OBSERVATORY
SO GUIDANCE AND CONTROL 2012
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 35th Annual AAS Rocky Mountain Section Guidance and Control Conference
CY FEB 03-08, 2012
CL Breckenridge, CO
SP AAS, Rocky Mt Sect
AB There are two gimbaled systems on the Global Precipitation Measurement Core Observatory: two single-degree-of-freedom solar arrays (SAs) and one two-degree-of-freedom high gain antenna (HGA). The guidance, navigation, and control analysis team was presented with the following challenges regarding SA orientation control during periods of normal mission science: (1) maximize solar flux on the SAs during orbit day, subject to battery charging limits, (2) minimize atmospheric drag during orbit night to reduce frequency of orbit maintenance thruster usage, (3) minimize atmospheric drag during orbits for which solar flux is nearly independent of SA orientation, and (4) keep array-induced spacecraft attitude disturbances within allocated tolerances. The team was presented with the following challenges regarding HGA control during mission science periods: (1) while tracking a ground-selected Tracking Data and Relay Satellite (TDRS), keep HGA control error below about 4', (2) keep array-induced spacecraft attitude disturbances small, and (3) minimize transition time between TDRSs subject to constraints imposed by item 2. This paper describes the control algorithms developed to achieve these goals and certain analysis done as part of that work.
C1 [Welter, Gary] NASA, Goddard Space Flight Ctr, Software Engn Div, Greenbelt, MD 20771 USA.
RP Welter, G (reprint author), NASA, Goddard Space Flight Ctr, Software Engn Div, Greenbelt, MD 20771 USA.
NR 6
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-585-5
J9 ADV ASTRONAUT SCI
PY 2012
VL 144
BP 317
EP 331
PG 15
WC Engineering, Aerospace
SC Engineering
GA BFX61
UT WOS:000321807500022
ER
PT S
AU Dennehy, CJ
AF Dennehy, Cornelius J.
BE Osborne, ML
TI TECHNICAL CHALLENGES AND FUTURE TECHNOLOGY NEEDS FOR NASA'S GUIDANCE,
NAVIGATION AND CONTROL ENGINEERING DISCIPLINE
SO GUIDANCE AND CONTROL 2012
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 35th Annual AAS Rocky Mountain Section Guidance and Control Conference
CY FEB 03-08, 2012
CL Breckenridge, CO
SP AAS, Rocky Mt Sect
AB Currently the United States (U.S.) National Aeronautics and Space Administration (NASA) is experiencing some significant changes, particularly in the human exploration arena. Notable among the changes that have recently occurred within NASA is the retirement of the space shuttle, the emergence of commercial crew transport to the International Space Station (ISS), the development of architectures for human exploration beyond low-Earth orbit (LEO), affordability constraints on robotic spaceflight missions, and a renewed emphasis on and commitment to space technology development/demonstration. These new changes within the Agency will have impacts on the Guidance, Navigation and Control (GN&C) discipline. This paper will summarize an independent NASA Engineering and Safety Center (NESC) assessment of the GN&C technical challenges and barriers currently faced by the three NASA Mission Directorates. Technical challenges and future technological need for NASA's GN&C engineering discipline will be summarized. In particular, three key GN&C challenge areas will be discussed in this paper. The first challenge concerns the fact that advanced GN&C capabilities (e.g., the application of robust/optimal or adaptive control) are not being exploited as much as they could be due to perceived risk of implementation. The second challenge addresses the need for meaningful investments in the next generation of GN&C component-level technologies. The third challenge arises from the lack of consistent NASA-wide top-level guidelines for GN&C system Design, Development, Test and Evaluation (DDT&E). Specific steps, many involving the efforts of the NESC GN&C Technical Discipline Team (TDT), to mitigate these three challenges will be identified and described. This paper will also discuss the need for sustained investments to sufficiently mature the several classes of GN&C technologies required to implement NASA crewed exploration missions beyond LEO, to address future aeronautical system needs, and to conduct robotic spaceflight missions for attaining Earth and Space scientific goals.
C1 NASA, Engn & Safety Ctr, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Dennehy, CJ (reprint author), NASA, Engn & Safety Ctr, Goddard Space Flight Ctr, 8800 Greenbelt Rd,Mail Code 590, Greenbelt, MD 20771 USA.
EM cornelius.j.dennehy@nasa.gov
NR 10
TC 0
Z9 0
U1 0
U2 1
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-585-5
J9 ADV ASTRONAUT SCI
PY 2012
VL 144
BP 335
EP 355
PG 21
WC Engineering, Aerospace
SC Engineering
GA BFX61
UT WOS:000321807500023
ER
PT S
AU Naasz, BJ
Moreau, MC
AF Naasz, Bo J.
Moreau, Michael C.
BE Osborne, ML
TI AUTONOMOUS RPOD TECHNOLOGY CHALLENGES FOR THE COMING DECADE
SO GUIDANCE AND CONTROL 2012
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 35th Annual AAS Rocky Mountain Section Guidance and Control Conference
CY FEB 03-08, 2012
CL Breckenridge, CO
SP AAS, Rocky Mt Sect
AB Rendezvous Proximity Operations and Docking (RPOD) technologies are important to a wide range of future space endeavors. This paper will review some of the recent and ongoing activities related to autonomous RPOD capabilities and summarize the current state of the art. Gaps are identified where future investments are necessary to successfully execute some of the missions likely to be conducted within the next ten years. A proposed RPOD technology roadmap that meets the broad needs of NASA's future missions will be outlined, and ongoing activities at GSFC in support of a future satellite servicing mission are presented. The case presented shows that an evolutionary, stair-step technology development program, including a robust campaign of coordinated ground tests and space-based system-level technology demonstration missions, will ultimately yield a multi-use mainstream autonomous RPOD capability suite with cross-cutting benefits across a wide range of future applications.
C1 [Naasz, Bo J.; Moreau, Michael C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Naasz, BJ (reprint author), NASA, Goddard Space Flight Ctr, Code 595,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
NR 54
TC 1
Z9 1
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-585-5
J9 ADV ASTRONAUT SCI
PY 2012
VL 144
BP 403
EP 425
PG 23
WC Engineering, Aerospace
SC Engineering
GA BFX61
UT WOS:000321807500027
ER
PT S
AU Montgomery, JF
Bodie, JH
Brown, JD
Chen, A
Chen, CW
Essmiller, JC
Fisher, CD
Goldberg, HR
Lee, SW
Shaffer, SJ
AF Montgomery, James F.
Bodie, James H.
Brown, Joseph D.
Chen, Allen
Chen, Curtis W.
Essmiller, John C.
Fisher, Charles D.
Goldberg, Hannah R.
Lee, Steven W.
Shaffer, Scott J.
BE Osborne, ML
TI IMPLEMENTING THE MARS SCIENCE LABORATORY TERMINAL DESCENT SENSOR FIELD
TEST CAMPAIGN
SO GUIDANCE AND CONTROL 2012
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 35th Annual AAS Rocky Mountain Section Guidance and Control Conference
CY FEB 03-08, 2012
CL Breckenridge, CO
SP AAS, Rocky Mt Sect
AB The Mars Science Laboratory (MSL) will deliver a 900 kg rover to the surface of Mars in August 2012. MSL will utilize a new pulse-Doppler landing radar, the Terminal Descent Sensor (TDS). The TDS employs six narrow-beam antennas to provide unprecedented slant range and velocity performance at Mars to enable soft touchdown of the MSL rover using a unique sky crane Entry, Descent, and Landing (EDL) technique. Prior to use on MSL, the TDS was put through a rigorous verification and validation (V&V) process. A key element of this V&V was operating the TDS over a series of field tests, using flight-like profiles expected during the descent and landing of MSL over Mars-like terrain on Earth. Limits of TDS performance were characterized with additional testing meant to stress operational modes outside of the expected EDL flight profiles. The flight envelope over which the TDS must operate on Mars encompasses such a large range of altitudes and velocities that a variety of venues were necessary to cover the test space. These venues included an F/A-18 high performance aircraft, a Eurocopter AS350 AStar helicopter and 100-meter tall Echo Towers at the China Lake Naval Air Warfare Center. Testing was carried out over a five year period from July 2006 to June 2011. TDS performance was shown, in general, to be excellent over all venues. This paper describes the planning, design, and implementation of the field test campaign plus results and lessons learned.
C1 [Montgomery, James F.; Bodie, James H.; Brown, Joseph D.; Chen, Allen; Chen, Curtis W.; Essmiller, John C.; Fisher, Charles D.; Lee, Steven W.; Shaffer, Scott J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Montgomery, JF (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM james.f.montgomery@jpl.nasa.gov; James.h.bodie@jpl.nasa.gov;
joseph.d.brown@jpl.nasa.gov; Allen.chen@jpl.nasa.gov;
Curtis.w.chen@jpl.nasa.gov; John.c.essmiller@jpl.nasa.gov;
hannah@arkyd.com; steven.w.lee@jpl.nasa.gov; scott.j.shaffer@jpinasa.gov
NR 4
TC 5
Z9 5
U1 0
U2 1
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-585-5
J9 ADV ASTRONAUT SCI
PY 2012
VL 144
BP 647
EP 664
PG 18
WC Engineering, Aerospace
SC Engineering
GA BFX61
UT WOS:000321807500041
ER
PT S
AU Smith, BA
Vanelli, CA
Lee, AY
AF Smith, Brett A.
Vanelli, C. Anthony
Lee, Allan Y.
BE Osborne, ML
TI UNDERSTANDING SPACECRAFT AGILITY FOR ORBIT TRANSFERS ON THE DAWN
LOW-THRUST MISSION
SO GUIDANCE AND CONTROL 2012
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 35th Annual AAS Rocky Mountain Section Guidance and Control Conference
CY FEB 03-08, 2012
CL Breckenridge, CO
SP AAS, Rocky Mt Sect
AB Dawn is a low-thrust interplanetary spacecraft currently orbiting the asteroid Vesta. The spacecraft launched in September 2007 on a mission to better understand the early creation of the solar system, and recently arrived at Vesta in May of 2011. Three solar electric ion-propulsion engines provide the primary thrust for the Dawn spacecraft. Ion engines very efficiently produce a small thrust magnitude, and therefore must thrust almost continuously for long periods to realize the necessary change in velocity to reach Vesta, and eventually Ceres.
The amount of time that must be spent thrusting presents unique challenges to executing orbit transfers on low-thrust missions. The necessary delta-V cannot be easily decomposed into a subset of fixed inertial attitudes, leading to the need to use time-varying thrust attitudes. Changing spacecraft orientation while thrusting imposes dynamic constraints on orbit transfer thrust designs, in addition to geometric pointing constraints. The dynamic constraints increase the coupling between the navigation design and the attitude control system, further challenging the design of flyable orbit transfers. Additionally, software commanding limitations and the need to maintain positive solar array power made developing simplified constraints for the navigation team a very non-linear problem. Post-launch development of new tools and processes was necessary to aid in the design of flyable orbit transfer trajectories.
This paper briefly discusses the general attitude control issues with orbit transfers on a low thrust mission, and details their specific resolution on the Dawn mission. The discussion presents the tools and strategies developed to ensure successful design of orbit transfer thrust trajectories that remain safely within the capabilities of the Dawn attitude control system. With Dawn having recently completed a significant percentage of the orbit transfers at Vesta, this paper compares predicted performance and capabilities with actual spacecraft performance during orbit transfers. Being NASA's first ion-propulsion mission to orbit an asteroid provided numerous lessons that will be beneficial to all future low thrust missions.
C1 [Smith, Brett A.; Vanelli, C. Anthony; Lee, Allan Y.] CALTECH, Jet Prop Lab, Tech Staff Guidance & Control Sect, Pasadena, CA 91109 USA.
RP Smith, BA (reprint author), CALTECH, Jet Prop Lab, Tech Staff Guidance & Control Sect, M-S 264-853,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Brett.A.Smith@jpl.nasa.gov; Tony.Vanelli@jpl.nasa.gov;
Allan.Y.Lee@jpl.nasa.gov
NR 6
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-585-5
J9 ADV ASTRONAUT SCI
PY 2012
VL 144
BP 753
EP 770
PG 18
WC Engineering, Aerospace
SC Engineering
GA BFX61
UT WOS:000321807500047
ER
PT S
AU Wolf, AA
Larson, T
Thompson, P
McElrath, T
Bhaskaran, S
Chesley, S
Klaasen, KP
Cheuvront, A
AF Wolf, Aron A.
Larson, Timothy
Thompson, Paul
McElrath, Timothy
Bhaskaran, Shyam
Chesley, Steven
Klaasen, Kenneth P.
Cheuvront, Allan
BE Osborne, ML
TI STARDUST-NEXT: LESSONS LEARNED FROM A COMET FLYBY MISSION
SO GUIDANCE AND CONTROL 2012
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 35th Annual AAS Rocky Mountain Section Guidance and Control Conference
CY FEB 03-08, 2012
CL Breckenridge, CO
SP AAS, Rocky Mt Sect
AB The Stardust-NExT (New Exploration of Tempel) mission, a follow-on to the Stardust prime mission, successfully completed a flyby of comet Tempel-1 on 2/14/11. However there were many challenges along the way, most significantly low propellant margin and detection of the comet in imagery later than anticipated. These challenges and their ramifications forced the project to respond with flexibility and ingenuity. As a result, the flyby at an altitude of 178 km was nearly flawless, accomplishing all its science objectives. Lessons learned on Stardust-NExT may have relevance to other spacecraft missions.
C1 [Wolf, Aron A.] CALTECH, GNC Sect, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Wolf, AA (reprint author), CALTECH, GNC Sect, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 8
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-585-5
J9 ADV ASTRONAUT SCI
PY 2012
VL 144
BP 771
EP 785
PG 15
WC Engineering, Aerospace
SC Engineering
GA BFX61
UT WOS:000321807500048
ER
PT S
AU Mandic, M
Acikmese, B
Bayard, DS
Blackmore, L
AF Mandic, Milan
Acikmese, Behcet
Bayard, David S.
Blackmore, Lars
BE Osborne, ML
TI ANALYSIS OF THE TOUCH-AND-GO SURFACE SAMPLING CONCEPT FOR COMET SAMPLE
RETURN MISSIONS
SO GUIDANCE AND CONTROL 2012
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 35th Annual AAS Rocky Mountain Section Guidance and Control Conference
CY FEB 03-08, 2012
CL Breckenridge, CO
SP AAS, Rocky Mt Sect
AB This paper studies the Touch-and-Go (TAG) concept for enabling a spacecraft to take a sample from the surface of a small primitive body, such as an asteroid or comet. The idea behind the TAG concept is to let the spacecraft descend to the surface, make contact with the surface for several seconds, and then ascend to a safe location. Sampling would be accomplished by an end-effector that is active during the few seconds of surface contact. The TAG event is one of the most critical events in a primitive body sample-return mission. The purpose of this study is to evaluate the dynamic behavior of a representative spacecraft during the TAG event, i.e., immediately prior, during, and after surface contact of the sampler. The study evaluates the sample-collection performance of the proposed sampling end-effector, in this case a brushwheel sampler, while acquiring material from the surface during the contact. A main result of the study is a guidance and control (G&C) validation of the overall TAG concept, in addition to specific contributions to demonstrating the effectiveness of using nonlinear clutch mechanisms in the sampling arm joints, and increasing the length of the sampling arms to improve robustness.
C1 [Mandic, Milan; Acikmese, Behcet; Bayard, David S.; Blackmore, Lars] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Mandic, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM mandic@jpl.nasa.gov; acikmese@jpl.nasa.gov; bayard@jpl.nasa.gov;
larsb@mit.edu
NR 13
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-585-5
J9 ADV ASTRONAUT SCI
PY 2012
VL 144
BP 841
EP 855
PG 15
WC Engineering, Aerospace
SC Engineering
GA BFX61
UT WOS:000321807500053
ER
PT J
AU Reynolds, JR
Rooney, SC
Heifetz, J
Greene, HG
Norcross, BL
Shotwell, SK
AF Reynolds, Jennifer R.
Rooney, Sean C.
Heifetz, Jonathan
Greene, H. Gary
Norcross, Brenda L.
Shotwell, S. Kalei
BE Harris, PT
Baker, EK
TI Habitats and Demersal Fish Communities in the Vicinity of Albatross
Bank, Gulf of Alaska
SO SEAFLOOR GEOMORPHOLOGY AS BENTHIC HABITAT: GEOHAB ATLAS OF SEAFLOOR
GEOMORPHIC FEATURES AND BENTHIC HABITATS
SE Elsevier Insights
LA English
DT Article; Book Chapter
DE shelf; bank; pinnacle; moraine; glacial; till; pavement;
macroinvertebrate; fish community; rockfish
AB The outer shelf and upper slope in the vicinity of Albatross Bank, Gulf of Alaska, have been shaped by glaciation, recent sedimentation, and mass wasting. A series of flat sedimentary bedrock banks in about 50-100 m water depth are variably covered by glacial deposits and modern sediment. Sediment redistribution and pavement formation reflect the energy of bottom currents. Three sites, Snakehead fishing ground, 8-Fathom Pinnacle, and 49-Fathom Bank, were surveyed using a multibeam echosounder mapping system to 800m and by manned submersible diving between 15 and 360m. Habitat maps produced from these surveys emphasize seafloor physiography and geological substrate. Twenty-three fish species were observed, dominated by rockfishes (Sebastes spp. and Sebastolobus spp., 69% of fishes observed). Macroinvertebrate distribution was also characterized. At a scale of tens to hundreds of meters, seven fish communities associated with different depth zones and substrate characteristics were identified.
C1 [Reynolds, Jennifer R.; Rooney, Sean C.; Norcross, Brenda L.] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Fairbanks, AK 99775 USA.
[Heifetz, Jonathan; Shotwell, S. Kalei] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Auke Bay Labs, Juneau, AK USA.
[Greene, H. Gary] Tombolo Habitat Inst, Eastsound, WA USA.
RP Reynolds, JR (reprint author), Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Fairbanks, AK 99775 USA.
NR 9
TC 1
Z9 1
U1 0
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
BN 978-0-12-385141-3
J9 ELSEV INSIGHT
PY 2012
BP 539
EP 553
DI 10.1016/B978-0-12-385140-6.00038-4
PG 15
WC Geosciences, Multidisciplinary
SC Geology
GA BGC23
UT WOS:000322237000040
ER
PT J
AU Pope, AT
Stephens, CL
AF Pope, Alan T.
Stephens, Chad L.
GP ACM
TI Interpersonal Biocybernetics: Connecting through Social Psychophysiology
SO ICMI '12: PROCEEDINGS OF THE ACM INTERNATIONAL CONFERENCE ON MULTIMODAL
INTERACTION
LA English
DT Proceedings Paper
CT 14th ACM International Conference on Multimodal Interaction (ICMI)
CY OCT 22-26, 2012
CL Santa Monica, CA
SP ACM, SIGCHI
DE Physiological modulation; biofeedback
AB One embodiment of biocybernetic adaptation is a human-computer interaction system designed such that physiological signals modulate the effect that control of a task by other means, usually manual control, has on performance of the task. Such a modulation system enables a variety of human-human interactions based upon physiological self-regulation performance. These interpersonal interactions may be mixes of competition and cooperation for simulation training and/or videogame entertainment.
C1 [Pope, Alan T.; Stephens, Chad L.] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Pope, AT (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
EM alan.t.pope@nasa.gov; chad.l.stephens@nasa.gov
NR 11
TC 1
Z9 1
U1 0
U2 2
PU ASSOC COMPUTING MACHINERY
PI NEW YORK
PA 1515 BROADWAY, NEW YORK, NY 10036-9998 USA
BN 978-1-4503-1467-1
PY 2012
BP 561
EP 565
PG 5
WC Computer Science, Artificial Intelligence; Computer Science, Theory &
Methods; Engineering, Electrical & Electronic
SC Computer Science; Engineering
GA BFY85
UT WOS:000321926300100
ER
PT J
AU Yoshida, N
Hosokawa, T
Omukai, K
AF Yoshida, Naoki
Hosokawa, Takashi
Omukai, Kazuyuki
TI Formation of the first stars in the universe
SO PROGRESS OF THEORETICAL AND EXPERIMENTAL PHYSICS
LA English
DT Article
ID POPULATION-III-STARS; FAR-ULTRAVIOLET RADIATION; SUPERMASSIVE
BLACK-HOLES; PRIMORDIAL GAS CLOUDS; DARK-MATTER COSMOLOGY; GAMMA-RAY
BURST; SUPERNOVA EXPLOSIONS; HIGH-REDSHIFT; HII-REGIONS;
PHOTODISSOCIATION FEEDBACK
AB The standard theory of cosmic structure formation posits that the present-day rich structure of the universe developed through gravitational amplification of tiny matter density fluctuations left over from the Big Bang. Recent observations of the cosmic microwave background, large-scale structure, and distant supernovae determined the energy content of the universe and the basic statistics of the initial density field with great accuracy. It has become possible to make accurate predictions for the formation and nonlinear growth of structure through early to the present epochs. We review recent progress in the theory of structure formation in the early universe. Results from state-of-the-art computer simulations are presented. Finally, we discuss prospects for future observations of the first generation of stars, black holes, and galaxies.
C1 [Yoshida, Naoki] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan.
[Yoshida, Naoki] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan.
[Hosokawa, Takashi] CALTECH, Jet Prop Lab, Pasadena, CA 91198 USA.
[Omukai, Kazuyuki] Kyoto Univ, Dept Phys, Kyoto 6068502, Japan.
RP Yoshida, N (reprint author), Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan.
EM naoki.yoshida@ipmu.jp
FU Ministry of Education, Culture, Sports, Science and Technology of Japan
[2168407, 21244021, 20674003]; Japan Society for the Promotion of
Science for Research Abroad; National Aeronautics and Space
Administration (NASA)
FX The present work is supported in part by Grants-in-Aid from the Ministry
of Education, Culture, Sports, Science and Technology of Japan (2168407,
21244021:KO, 20674003:NY). T. H. acknowledges support by Fellowship of
the Japan Society for the Promotion of Science for Research Abroad.
Portions of this research were conducted at the Jet Propulsion
Laboratory, California Institute of Technology, which is supported by
the National Aeronautics and Space Administration (NASA).
NR 145
TC 2
Z9 2
U1 1
U2 4
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 2050-3911
J9 PROG THEOR EXP PHYS
JI Prog. Theor. Exp. Phys.
PY 2012
IS 1
AR 01A305
DI 10.1093/ptep/pts022
PG 22
WC Physics, Multidisciplinary; Physics, Particles & Fields
SC Physics
GA 190CD
UT WOS:000322314000025
ER
PT S
AU Folta, DC
Woodard, M
Pavlak, T
Haapala, A
Howell, KC
AF Folta, David C.
Woodard, Mark
Pavlak, Tom
Haapala, Amanda
Howell, Kathleen C.
BE Guerman, AD
Bainum, PM
Contant, JM
TI EARTH-MOON LIBRATION STATIONKEEPING: THEORY, MODELING, AND OPERATIONS
SO FIRST IAA CONFERENCE ON DYNAMICS AND CONTROL OF SPACE SYSTEMS 2012, PTS
I AND II
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT 1st International-Academy-of-Astronautics Conference on Dynamics and
Control of Space Systems (DyCoSS)
CY MAR 19-21, 2012
CL Porto, PORTUGAL
SP Int Acad Astronaut
ID RESTRICTED 3-BODY PROBLEM; PERIODIC-ORBITS; ENVIRONMENTS; TRANSITIONS;
POINTS
AB Collinear Earth-Moon libration points have emerged as locations with immediate applications. These libration point orbits are inherently unstable and must be controlled at a rapid frequency which constrains operations and maneuver locations. Stationkeeping is challenging due to short time scales of divergence, effects of large orbital eccentricity of the secondary body, and third-body perturbations. Using the Acceleration Reconnection and Turbulence and Electrodynamics of the Moon's Interaction with the Sun (ARTEMIS) mission orbit as our platform (hypothesis), we contrast and compare promising stationkeeping strategies including Optimal Continuation and Mode Analysis that achieved consistent and reasonable operational stationkeeping costs. Background on the fundamental structure and the dynamical models to achieve these demonstrated results are discussed along with their mathematical development.
C1 [Folta, David C.; Woodard, Mark] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Folta, DC (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
NR 27
TC 0
Z9 0
U1 0
U2 1
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-587-9
J9 ADV ASTRONAUT SCI
PY 2012
VL 145
BP 489
EP 507
PG 19
WC Engineering, Aerospace
SC Engineering
GA BFX62
UT WOS:000321808100035
ER
PT S
AU Saini, S
Rappleye, J
Chang, J
Barker, D
Mehrotra, P
Biswas, R
AF Saini, Subhash
Rappleye, Jason
Chang, Johnny
Barker, David
Mehrotra, Piyush
Biswas, Rupak
GP IEEE
TI I/O Performance Characterization of Lustre and NASA Applications on
Pleiades
SO 2012 19TH INTERNATIONAL CONFERENCE ON HIGH PERFORMANCE COMPUTING (HIPC)
SE Proceedings-International Conference on High Performance Computing
LA English
DT Proceedings Paper
CT 19th International Conference on High Performance Computing (HiPC)
CY DEC 18-22, 2012
CL Pune, INDIA
DE Lustre file system; I/O performance evaluation; benchmarking;
computational fluid dynamics; climate modeling; Read and Write Policy;
I/O cache effect; I/O latency
AB In this paper we study the performance of the Lustre file system using five scientific and engineering applications representative of NASA workload on large-scale supercomputing systems such as NASA's Pleiades. In order to facilitate the collection of Lustre performance metrics, we have developed a software tool that exports a wide variety of client and server-side metrics using SGI's Performance Co-Pilot (PCP), and generates a human readable report on key metrics at the end of a batch job. These performance metrics are (a) amount of data read and written, (b) number of files opened and closed, and (c) remote procedure call (RPC) size distribution (4 KB to 1024 KB, in powers of 2) for I/O operations. RPC size distribution measures the efficiency of the Lustre client and can pinpoint problems such as small write sizes, disk fragmentation, etc. These extracted statistics are useful in determining the I/O pattern of the application and can assist in identifying possible improvements for users' applications. Information on the number of file operations enables a scientist to optimize the I/O performance of their applications. Amount of I/O data helps users choose the optimal stripe size and stripe count to enhance I/O performance. In this paper, we demonstrate the usefulness of this tool on Pleiades for five production quality NASA scientific and engineering applications. We compare the latency of read and write operations under Lustre to that with NFS by tracing system calls and signals. We also investigate the read and write policies and study the effect of page cache size on I/O operations. We examine the performance impact of Lustre stripe size and stripe count along with performance evaluation of file per process and single shared file accessed by all the processes for NASA workload using parameterized IOR benchmark.
C1 [Saini, Subhash; Rappleye, Jason; Chang, Johnny; Barker, David; Mehrotra, Piyush; Biswas, Rupak] NASA, Ames Res Ctr, Adv Supercomp NAS Div, Moffett Field, CA 94035 USA.
RP Saini, S (reprint author), NASA, Ames Res Ctr, Adv Supercomp NAS Div, Moffett Field, CA 94035 USA.
EM subhash.saini@nasa.gov; jason.rappleye@nasa.gov; johnny.chang@nasa.gov;
david.p.barker@nasa.gov; piyush.mehrotra@nasa.gov; rupak.biswas@nasa.gov
NR 7
TC 0
Z9 0
U1 1
U2 1
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 1094-7256
BN 978-1-4673-2370-3
J9 P INT C HIGH PERFORM
PY 2012
PG 10
WC Computer Science, Hardware & Architecture; Computer Science, Theory &
Methods
SC Computer Science
GA BGC51
UT WOS:000322311400034
ER
PT B
AU Hilbe, JM
AF Hilbe, Joseph M.
BA Miner, G
Delen, D
Elder, J
Fast, A
Hill, T
Nisbet, RA
BF Miner, G
Delen, D
Elder, J
Fast, A
Hill, T
Nisbet, RA
TI Practical Text Mining and Statistical Analysis for Non-structured Text
Data Applications Foreword 2
SO PRACTICAL TEXT MINING AND STATISTICAL ANALYSIS FOR NON-STRUCTURED TEXT
DATA APPLICATIONS
LA English
DT Editorial Material; Book Chapter
C1 [Hilbe, Joseph M.] Arizona State Univ, Tempe, AZ 85287 USA.
[Hilbe, Joseph M.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA.
RP Hilbe, JM (reprint author), Arizona State Univ, Tempe, AZ 85287 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER ACADEMIC PRESS INC
PI SAN DIEGO
PA 525 B STREET, SUITE 1900, SAN DIEGO, CA 92101-4495 USA
BN 978-0-12-387011-7
PY 2012
BP XVII
EP XVIII
PG 2
WC Mathematics, Applied; Statistics & Probability
SC Mathematics
GA BFX72
UT WOS:000321819300002
ER
PT S
AU Ting, DZ
Soibel, A
Hill, CJ
Keo, SA
Mumolo, JM
Gunapala, SD
AF Ting, David Z.
Soibel, Alexander
Hill, Cory J.
Keo, Sam A.
Mumolo, Jason M.
Gunapala, Sarath D.
BE Andresen, BF
Fulop, GF
Norton, PR
TI High operating temperature midwave quantum dot barrier infrared detector
(QD-BIRD)
SO INFRARED TECHNOLOGY AND APPLICATIONS XXXVIII, PTS 1 AND 2
SE Proceedings of SPIE
LA English
DT Proceedings Paper
CT Conference on Infrared Technology and Applications XXXVIII
CY APR 23-27, 2012
CL Baltimore, MD
SP SPIE
DE midwave infrared; high operating temperature; infrared detector; quantum
dot; unipolar barrier
ID PHOTODETECTORS
AB The nBn or XBn barrier infrared detector has the advantage of reduced dark current resulting from suppressed Shockley-Read-Hall (SRH) recombination and surface leakage. High performance detectors and focal plane arrays (FPAs) based on InAsSb absorber lattice matched to GaSb substrate, with a matching AlAsSb unipolar electron barrier, have been demonstrated. The band gap of lattice-matched InAsSb yields a detector cutoff wavelength of approximately 4.2 mu m when operating at similar to 150K. We report results on extending the cutoff wavelength of midwave barrier infrared detectors by incorporating self-assembled InSb quantum dots into the active area of the detector. Using this approach, we were able to extend the detector cutoff wavelength to similar to 6 mu m, allowing the coverage of the full midwave infrared (MWIR) transmission window. The quantum dot barrier infrared detector (QD-BIRD) shows infrared response at temperatures up to 225 K.
C1 [Ting, David Z.; Soibel, Alexander; Hill, Cory J.; Keo, Sam A.; Mumolo, Jason M.; Gunapala, Sarath D.] CALTECH, Jet Prop Lab, Ctr Infrared Sensors, Pasadena, CA 91109 USA.
RP Ting, DZ (reprint author), CALTECH, Jet Prop Lab, Ctr Infrared Sensors, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM David.Z.Ting@jpl.nasa.gov
NR 26
TC 9
Z9 9
U1 0
U2 6
PU SPIE-INT SOC OPTICAL ENGINEERING
PI BELLINGHAM
PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA
SN 0277-786X
BN 978-0-8194-9031-5
J9 PROC SPIE
PY 2012
VL 8353
AR 835332
DI 10.1117/12.920685
PG 8
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA BBE01
UT WOS:000306604400109
ER
PT S
AU Bellerose, J
Burns, KJ
Marchis, F
AF Bellerose, Julie
Burns, Keaton J.
Marchis, Franck
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI DYNAMICS AND STABILITY IN A TRIPLE ASTEROID SYSTEM: APPLICATIONS TO
MISSION DESIGN
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
ID 1999 KW4; MUTUAL ORBITS
AB We now count two triple asteroid systems in the NEA population. To enable exploration of such systems, we look at the dynamics of triple systems, starting from a two-body and a restricted three body dynamical models. The dynamics of an augmented system is inevitably rich, and we show spacecraft applications for rendezvous and proximity operations at these systems. Finally, we numerically investigate the perturbations and the stability within such systems to show and quantify fate of particles.
C1 [Bellerose, Julie] Carnegie Mellon Univ Silicon Valley, NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
RP Bellerose, J (reprint author), Carnegie Mellon Univ Silicon Valley, NASA, Ames Res Ctr, MS-202-3,Bldg 202,Room 200B, Moffett Field, CA 94035 USA.
NR 20
TC 0
Z9 0
U1 0
U2 1
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 53
EP 68
PG 16
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400004
ER
PT S
AU Anderson, RL
Parker, JS
AF Anderson, Rodney L.
Parker, Jeffrey S.
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI COMPARISON OF LOW-ENERGY LUNAR TRANSFER TRAJECTORIES TO INVARIANT
MANIFOLDS
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
ID RESTRICTED 3-BODY PROBLEM; LIBRATION POINT ORBITS; FAMILIES; EARTH; MOON
AB In this study, transfer trajectories from the Earth to the Moon that encounter the Moon at various flight path angles are examined, and lunar approach trajectories are compared to the invariant manifolds of selected unstable orbits in the circular restricted three-body problem. Previous work focused on lunar impact and landing trajectories encountering the Moon normal to the surface, and this research extends the problem with different flight path angles in three dimensions. The lunar landing geometry for a range of Jacobi constants are computed, and approaches to the Moon via invariant manifolds from unstable orbits are analyzed for different energy levels.
C1 [Anderson, Rodney L.; Parker, Jeffrey S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Anderson, RL (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 301-121, Pasadena, CA 91109 USA.
OI Anderson, Rodney/0000-0001-5336-2775
NR 27
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 333
EP 352
PG 20
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400021
ER
PT S
AU Campagnola, S
Skerritt, P
Russell, RP
AF Campagnola, Stefano
Skerritt, Paul
Russell, Ryan P.
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI FLYBYS IN THE PLANAR, CIRCULAR, RESTRICTED, THREE-BODY PROBLEM
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
ID TRAJECTORY DESIGN; KEPLERIAN MAP; MISSIONS; ORBITER; GRAPH
AB This paper presents an analysis of gravity assisted flybys in the planar, circular, restricted three-body problem that is inspired by the Keplerian map and by the Tisserand-Poincare graph. The Flyby map is defined and used to give new insight on the flyby dynamics and on the accuracy of the linked-conics model. The first main result of this work is using the Flyby map to extend the functionality of the Tisserand graph to low energies beyond the validity of linked conics. Two families of flybys are identified: Type I (direct) flybys and Type II (retrograde) flybys. The second main result of this work is showing that Type I flybys exist at all energies and are more efficient than Type II flybys, when both exist. The third main result of this work is an example trajectory that consists of Type I flybys only, all outside the linked-conics domain of applicability. The trajectory is computed with the patched-cr3bp, and connects an initial orbit around Jupiter intersecting the Callisto orbit, to a 200-km circular orbit around Europa. The trajectory saves up to 30% in Delta v (endgame and orbit insertion) compared to the current baseline for Europa orbiters computed in patched conics, without any significant increase to the time of flight nor the radiation dose.
C1 [Campagnola, Stefano] CALTECH, Jet Prop Lab, Outer Planet Mission Anal Grp, Pasadena, CA 91109 USA.
RP Campagnola, S (reprint author), CALTECH, Jet Prop Lab, Outer Planet Mission Anal Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM stefano.campagnola@jpl.nasa.gov; sker-ritt@caltech.edu;
ryan.russell@utexas.edu
NR 30
TC 0
Z9 0
U1 1
U2 1
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 373
EP 392
PG 20
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400023
ER
PT S
AU Grebow, DJ
Petropoulos, AE
Finlayson, PA
AF Grebow, Daniel J.
Petropoulos, Anastassios E.
Finlayson, Paul A.
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI MULTI-BODY CAPTURE TO LOW-ALTITUDE CIRCULAR ORBITS AT EUROPA
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
ID PERIODIC-ORBITS; GRAPH
AB For capture to a 200-km circular orbit around Europa, millions of different starting points on the orbit are propagated in the Jupiter-Europa Restricted 3-Body Problem. The transfers exist as members of families of trajectories, where certain families consistently outperform the others. The trajectories are not sensitive to changes in inclination for the final circular orbit. The top-performing trajectories appear to follow the invariant manifolds of L-2 Lyapunov orbits for capture into a retrograde orbit, and in some cases save up to 40% of the Delta v from the patched 2-body problem. Transfers are attached to the current nominal mission for NASA's Jupiter-Europa Orbiter, where the total cost is roughly 100 m/s less than the baseline mission.
C1 [Grebow, Daniel J.; Petropoulos, Anastassios E.; Finlayson, Paul A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Grebow, DJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 16
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 413
EP 432
PG 20
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400025
ER
PT S
AU Prince, JLH
Powell, RW
Murri, D
AF Prince, Jill L. H.
Powell, Richard W.
Murri, Dan
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI AUTONOMOUS AEROBRAKING: A DESIGN, DEVELOPMENT, AND FEASIBILITY STUDY
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
AB Aerobraking has been used four times to decrease the apoapsis of a spacecraft in a captured orbit around a planetary body with a significant atmosphere utilizing atmospheric drag to decelerate the spacecraft. While aerobraking requires minimum fuel, the long time required for aerobraking requires both a large operations staff, and large Deep Space Network resources. A study to automate aerobraking has been sponsored by the NASA Engineering and Safety Center to determine initial feasibility of equipping a spacecraft with the onboard capability for autonomous aerobraking, thus saving millions of dollars incurred by a large aerobraking operations workforce and continuous DSN coverage. This paper describes the need for autonomous aerobraking, the development of the Autonomous Aerobraking Development Software that includes an ephemeris estimator, an atmospheric density estimator, and maneuver calculation, and the plan forward for continuation of this study.
C1 [Prince, Jill L. H.] NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, Hampton, VA 23681 USA.
RP Prince, JLH (reprint author), NASA, Langley Res Ctr, Atmospher Flight & Entry Syst Branch, MS 489, Hampton, VA 23681 USA.
NR 18
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 475
EP 481
PG 7
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400028
ER
PT S
AU Dec, JA
Thornblom, MN
AF Dec, John A.
Thornblom, Mark N.
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI AUTONOMOUS AEROBRAKING: THERMAL ANALYSIS AND RESPONSE SURFACE
DEVELOPMENT
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
AB A high-fidelity thermal model of the Mars Reconnaissance Orbiter was developed for use in an autonomous aerobraking simulation study. Response surface equations were derived from the high-fidelity thermal model and integrated into the autonomous aerobraking simulation software. The high-fidelity thermal model was developed using the Thermal Desktop software and used in all phases of the analysis. The use of Thermal Desktop exclusively, represented a change from previously developed aerobraking thermal analysis methodologies. Comparisons were made between the Thermal Desktop solutions and those developed for the previous aerobraking thermal analyses performed on the Mars Reconnaissance Orbiter during aerobraking operations. A variable sensitivity screening study was performed to reduce the number of variables carried in the response surface equations. Thermal analysis and response surface equation development were performed for autonomous aerobraking missions at Mars and Venus.
C1 [Dec, John A.; Thornblom, Mark N.] NASA, Langley Res Ctr, Struct & Thermal Syst Branch, Washington, DC 20546 USA.
RP Dec, JA (reprint author), NASA, Langley Res Ctr, Struct & Thermal Syst Branch, MS 431, Washington, DC 20546 USA.
NR 14
TC 1
Z9 1
U1 0
U2 1
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 483
EP 497
PG 15
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400029
ER
PT S
AU Maddock, RW
Cianciolo, AD
Bowes, A
Prince, JLH
Powell, RW
AF Maddock, Robert W.
Cianciolo, Alicia Dwyer
Bowes, Angela
Prince, Jill L. H.
Powell, Richard W.
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI IMPLEMENTATION AND SIMULATION RESULTS USING AUTONOMOUS AEROBRAKING
DEVELOPMENT SOFTWARE
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
AB An autonomous aerobraking software system is currently under development with support from the NASA Engineering and Safety Center (NESC) that would move typically ground-based aerobraking operations functions to onboard a spacecraft, reducing mission risk and cost. The software suite that will enable autonomous aerobraking is the Autonomous Aerobraking Development Software (AADS) and consists of an ephemeris model, onboard atmosphere estimator, temperature and loads prediction, and a maneuver calculation. The software calculates the maneuver time, magnitude and direction commands to maintain the spacecraft periapsis parameters within the desired design structural load and/or thermal constraints. The AADS is currently tested in simulations at Mars, with plans to also evaluate feasibility and performance at Venus and Titan.
C1 [Maddock, Robert W.; Cianciolo, Alicia Dwyer; Bowes, Angela; Prince, Jill L. H.] NASA, Langley Res Ctr, Engn Directorate, Hampton, VA 23681 USA.
RP Maddock, RW (reprint author), NASA, Langley Res Ctr, Engn Directorate, MS 489, Hampton, VA 23681 USA.
NR 13
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 499
EP 512
PG 14
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400030
ER
PT S
AU Tolson, RH
Prince, JLH
AF Tolson, Robert H.
Prince, Jill L. H.
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI ONBOARD ATMOSPHERIC MODELING AND PREDICTION FOR AUTONOMOUS AEROBRAKING
MISSIONS
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
ID MARS GLOBAL SURVEYOR
AB For capture to a 200-km circular orbit around Europa, millions of different starting points on the orbit are propagated in the Jupiter-Europa Restricted 3-Body Problem. The transfers exist as members of families of trajectories, where certain families consistently outperform the others. The trajectories are not sensitive to changes in inclination for the final circular orbit. The top-performing trajectories appear to follow the invariant manifolds of L-2 Lyapunov orbits for capture into a retrograde orbit, and in some cases save up to 40% of the Delta upsilon from the patched 2-body problem. Transfers are attached to the current nominal mission for NASA's Jupiter-Europa Orbiter, where the total cost is roughly 100 m/s less than the baseline mission.
C1 [Tolson, Robert H.; Prince, Jill L. H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Tolson, RH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 21
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 513
EP 532
PG 20
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400031
ER
PT S
AU Justh, HL
Justus, CG
Ramey, HS
AF Justh, Hilary L.
Justus, Carl G.
Ramey, Holly S.
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI THE NEXT GENERATION OF MARS-GRAM AND ITS ROLE IN THE AUTONOMOUS
AEROBRAKING DEVELOPMENT PLAN
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
ID CIRCULATION; DYNAMICS
AB The Mars Global Reference Atmospheric Model (Mars-GRAM) is an engineering-level atmospheric model widely used for diverse mission applications. Mars-GRAM 2010 is currently being used to develop the onboard atmospheric density estimator that is part of the Autonomous Aerobraking Development Plan. In previous versions, Mars-GRAM was less than realistic when used for sensitivity studies for Thermal Emission Spectrometer (TES) Map Year=0 and large optical depth values, such as tau=3. A comparison analysis has been completed between Mars-GRAM, TES and data from the Planetary Data System (PDS) resulting in updated coefficients for the functions relating density, latitude, and longitude of the sun. The adjustment factors are expressed as a function of height (z), Latitude (Lat) and areocentric solar longitude (Ls). The latest release of Mars-GRAM 2010 includes these adjustment factors that alter the input data from MGCM and MTGCM for the Mapping Year 0 (user-controlled dust) case. The greatest adjustment occurs at large optical depths such as tau >1. The addition of the adjustment factors has led to better correspondence to TES Limb data from 0-60 km as well as better agreement with MGS, ODY and MRO data at approximately 90-135 km. Improved simulations utilizing Mars-GRAM 2010 are vital to developing the onboard atmospheric density estimator for the Autonomous Aerobraking Development Plan. Mars-GRAM 2010 was not the only planetary GRAM utilized during phase 1 of this plan; Titan-GRAM and Venus-GRAM were used to generate density data sets for Aerobraking Design Reference Missions. These data sets included altitude profiles (both vertical and along a trajectory), GRAM perturbations (tides, gravity waves, etc.) and provided density and scale height values for analysis by other Autonomous Aerobraking team members.
C1 [Justh, Hilary L.] NASA, George C Marshall Space Flight Ctr, Nat Environm Branch, Huntsville, AL 35812 USA.
RP Justh, HL (reprint author), NASA, George C Marshall Space Flight Ctr, Nat Environm Branch, Mail Code EV44, Huntsville, AL 35812 USA.
NR 5
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 533
EP 540
PG 8
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400032
ER
PT S
AU Barbee, BW
Mink, RG
Adamo, DR
Alberding, CM
AF Barbee, Brent W.
Mink, Ronald G.
Adamo, Daniel R.
Alberding, Cassandra M.
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI METHODOLOGY AND RESULTS OF THE NEAR-EARTH OBJECT (NEO) HUMAN SPACE
FLIGHT (HSF) ACCESSIBLE TARGETS STUDY (NHATS)
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
AB Near-Earth Asteroids (NEAs) have been identified by the Administration as potential destinations for human explorers during the mid-2020s. Planning such ambitious missions requires selecting potentially accessible targets from the growing known population of 8,008 NEAs. NASA is therefore conducting the Near-Earth Object (NEO) Human Space Flight (HSF) Accessible Targets Study (NHATS), in which the trajectory opportunities to all known NEAs are being systematically evaluated with respect to a set of defined constraints. While the NHATS algorithms have identified hundreds of NEAs which satisfy purposely inclusive trajectory constraints, only a handful of them offer truly attractive mission opportunities in the time frame of greatest interest. In this paper we will describe the structure of the NHATS algorithms and the constraints utilized in the study, present current study results, and discuss various mission design considerations for future human space flight missions to NEAs.
C1 [Barbee, Brent W.; Mink, Ronald G.; Alberding, Cassandra M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Barbee, BW (reprint author), NASA, Goddard Space Flight Ctr, Code 595,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
NR 5
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 595
EP 614
PG 20
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400036
ER
PT S
AU Landau, D
Strange, N
AF Landau, Damon
Strange, Nathan
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI NEAR-EARTH ASTEROIDS ACCESSIBLE TO HUMAN EXPLORATION WITH HIGH-POWER
ELECTRIC PROPULSION
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
ID 99942 APOPHIS; MISSION; TARGETS; OBJECTS
AB The diverse physical and orbital characteristics of near-Earth asteroids provide progressive stepping stones on a flexible path to Mars. Beginning with cislunar exploration capability, the variety of accessible asteroid targets steadily increases as technology is developed for eventual missions to Mars. Noting the potential for solar electric propulsion to dramatically reduce launch mass for Mars exploration, we apply this technology to expand the range of candidate asteroid missions. The variety of mission options offers flexibility to adapt to shifting exploration objectives and development schedules. A robust and efficient exploration program emerges where a potential mission is available once per year (on average) with technology levels that span cislunar to Mars-orbital capabilities. Examples range from a six-month mission that encounters a 10-m object with 65 kW to a two-year mission that reaches a 2-km asteroid with a 350-kW system.
C1 [Landau, Damon] CALTECH, Jet Prop Lab, Outer Planet Mission Anal Grp, Pasadena, CA 91125 USA.
RP Landau, D (reprint author), CALTECH, Jet Prop Lab, Outer Planet Mission Anal Grp, M-S 301-121, Pasadena, CA 91125 USA.
NR 61
TC 1
Z9 1
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 635
EP 654
PG 20
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400038
ER
PT S
AU Plice, L
Craychee, T
AF Plice, Laura
Craychee, Tim
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI A DESIGN METHOD FOR LOW ALTITUDE, NEAR-EQUATORIAL LUNAR ORBITS
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
AB In 2013 the Lunar Atmosphere & Dust Environment Explorer (LADEE) mission will return to an orbital regime not visited since Apollo. The lunar orbit required for LADEE poses unique challenges to the mission designer: low, retrograde, near circular, near equatorial, 100 days duration, with the line of apsides aligned near the solar terminator. Due to the close proximity to the surface, the lunar gravity creates havoc on the LADEE orbit, perturbing the eccentricity and line of apsides while the semi-major axis remains largely unchanged. LADEE uses a novel, visual approach to allow the orbit designer to predict altitude decay and shifts in argument of periapsis and to plan orbit maintenance maneuvers.
C1 [Plice, Laura] NASA, Ames Res Ctr, Logyx LLC, Moffett Field, CA 94035 USA.
RP Plice, L (reprint author), NASA, Ames Res Ctr, Logyx LLC, MS 240-5, Moffett Field, CA 94035 USA.
NR 6
TC 0
Z9 0
U1 0
U2 1
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 733
EP 751
PG 19
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400043
ER
PT S
AU Parker, JS
Anderson, RL
AF Parker, Jeffrey S.
Anderson, Rodney L.
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI TARGETING LOW-ENERGY TRANSFERS TO LOW LUNAR ORBIT
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
ID MOON; TRAJECTORIES; MISSION
AB A targeting scheme is presented to build trajectories from a specified Earth parking orbit to a specified low lunar orbit via a low-energy transfer and up to two maneuvers. The total transfer Delta V is characterized as a function of the Earth parking orbit inclination and the departure date for transfers to each given low lunar orbit. The transfer Delta V cost is characterized for transfers constructed to low lunar polar orbits with any longitude of ascending node and for transfers that arrive at the Moon at any given time during a month.
C1 [Parker, Jeffrey S.; Anderson, Rodney L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Parker, JS (reprint author), CALTECH, Jet Prop Lab, M-S 301-101,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
OI Anderson, Rodney/0000-0001-5336-2775
NR 30
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 847
EP 866
PG 20
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400049
ER
PT S
AU Carpenter, JR
Markley, FL
Alfriend, KT
Wright, C
Arcido, J
AF Carpenter, J. R.
Markley, F. L.
Alfriend, K. T.
Wright, C.
Arcido, J.
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI SEQUENTIAL PROBABILITY RATIO TEST FOR COLLISION AVOIDANCE MANEUVER
DECISIONS BASED ON A BANK OF NORM-INEQUALITY-CONSTRAINED EPOCH-STATE
FILTERS
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
ID ORBIT
AB Sequential probability ratio tests explicitly allow decision makers to incorporate false alarm and missed detection risks, and are potentially less sensitive to modeling errors than a procedure that relies solely on a probability of collision threshold. Recent work on constrained Kalman filtering has suggested an approach to formulating such a test for collision avoidance maneuver decisions: a filter bank with two norm-inequality-constrained epoch-state extended Kalman filters. One filter models the null hypothesis that the miss distance is inside the combined hard body radius at the predicted time of closest approach, and one filter models the alternative hypothesis. The epoch-state filter developed for this method explicitly accounts for any process noise present in the system. The method appears to work well using a realistic example based on an upcoming highly-elliptical orbit formation flying mission.
C1 [Carpenter, J. R.] NASA GSFC, Nav & Mission Design Branch, Greenbelt, MD 20771 USA.
RP Carpenter, JR (reprint author), NASA GSFC, Nav & Mission Design Branch, Greenbelt, MD 20771 USA.
NR 11
TC 1
Z9 1
U1 0
U2 2
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 1105
EP 1124
PG 20
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400064
ER
PT S
AU Chung, MKJ
Bhaskaran, S
Chesley, SR
Halsell, CA
Helfrich, CE
Jefferson, DC
McElrath, TP
Rush, BP
Wang, TCM
Yen, CWL
AF Chung, Min-Kun J.
Bhaskaran, Shyamkumar
Chesley, Steven R.
Halsell, C. Allen
Helfrich, Clifford E.
Jefferson, David C.
McElrath, Timothy P.
Rush, Brian P.
Wang, Tseng-Chan M.
Yen, Chen-wan L.
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI EPOXI TRAJECTORY AND MANEUVER ANALYSES
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
ID MISSION
AB The EPOXI mission is a NASA Discovery Mission of Opportunity combining two separate investigations: Extrasolar Planet Observation and Characterization (EPOCh) and Deep Impact eXtended Investigation (DIXI). Both investigations reused the DI instruments and spacecraft that successfully flew by the comet Tempel-1 (4 July 2005). For EPOCh, the goal was to find exoplanets with the high resolution imager, while for DIXI it was to fly by the comet Hartley 2 (4 Nov 2010). This paper documents the navigation experience of the earlier maneuver analyses critical for the EPOXI mission including statistical Delta V analyses and other useful analyses in designing maneuvers. It also recounts the trajectory design leading up to the final reference trajectory to Hartley 2.
C1 [Chung, Min-Kun J.; Bhaskaran, Shyamkumar; Chesley, Steven R.; Halsell, C. Allen; Helfrich, Clifford E.; Jefferson, David C.; McElrath, Timothy P.; Rush, Brian P.; Wang, Tseng-Chan M.; Yen, Chen-wan L.] CALTECH, Jet Prop Lab, Mission Design & Nav Sect, Pasadena, CA 91109 USA.
RP Chung, MKJ (reprint author), CALTECH, Jet Prop Lab, Mission Design & Nav Sect, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 9
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 1213
EP 1226
PG 14
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400070
ER
PT S
AU Gillam, SD
Riedel, JE
Owen, WM
Wang, TCM
Werner, RA
Bhaskaran, S
Chesley, SR
Thompson, PF
Wolf, AA
AF Gillam, Stephen D.
Riedel, J. Ed.
Owen, William M., Jr.
Wang, Tseng-Chan Mike
Werner, Robert A.
Bhaskaran, Shyam
Chesley, Steven R.
Thompson, Paul F.
Wolf, Aron A.
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI GROUND OPTICAL NAVIGATION FOR THE STARDUST-NEXT MISSION TO COMET
9P/TEMPEL 1
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
AB Ground-based optical navigation (OpNav) using pictures taken by the Navigation camera on the Stardust spacecraft provided the target-relative information needed to design maneuvers during its approach to comet Tempel 1. Hardware problems, limited downlink bandwidth, and changes in the flight profile affected the OpNav picture schedule, sometimes in near-real time. The Stardust navigation camera and attitude control presented challenges. Picture-processing techniques were developed during approach that included background estimation, co-addition, and co-registration. These techniques, along with adaptive picture scheduling, successfully addressed the challenges.
C1 [Gillam, Stephen D.; Riedel, J. Ed.; Owen, William M., Jr.; Wang, Tseng-Chan Mike; Werner, Robert A.; Bhaskaran, Shyam; Chesley, Steven R.; Thompson, Paul F.; Wolf, Aron A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Gillam, SD (reprint author), CALTECH, Jet Prop Lab, MS 301-121,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 14
TC 0
Z9 0
U1 1
U2 2
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 1227
EP 1246
PG 20
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400071
ER
PT S
AU Haw, RJ
Bhaskaran, S
Strauss, W
Sklyanskiy, E
Graat, EJ
Smith, JJ
Menon, P
Ardalan, S
Ballard, C
Williams, P
Kawaguchi, J
Makoto, Y
Ohnishi, T
AF Haw, Robert J.
Bhaskaran, S.
Strauss, W.
Sklyanskiy, E.
Graat, E. J.
Smith, J. J.
Menon, P.
Ardalan, S.
Ballard, C.
Williams, P.
Kawaguchi, J.
Makoto, Y.
Ohnishi, T.
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI HAYABUSA: NAVIGATION CHALLENGES FOR EARTH RETURN
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
AB Hayabusa was a JAXA sample-return mission to Itokawa navigated, in part, by JPL personnel. The spacecraft survived several near mission-ending failures at Itokawa yet returned to Earth with an asteroid regolith sample on June 13, 2010. This paper describes NASA/JPL's participation in the Hayabusa mission during the last 100 days of its mission, wherein JPL provided tracking data and orbit determination, plus verification of maneuver design and entry, descent and landing.
C1 [Haw, Robert J.; Bhaskaran, S.; Smith, J. J.; Ardalan, S.] CALTECH, Jet Prop Lab, Outer Planet Nav Mission Design & Nav Sect, Pasadena, CA 91109 USA.
RP Haw, RJ (reprint author), CALTECH, Jet Prop Lab, Outer Planet Nav Mission Design & Nav Sect, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 4
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 1247
EP 1261
PG 15
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400072
ER
PT S
AU Bhaskaran, S
Abrahamson, M
Chesley, S
Chung, MK
Halsell, A
Haw, R
Helfrich, C
Jefferson, D
Kennedy, B
McElrath, T
Owen, W
Rush, B
Smith, J
Wang, TC
Yen, CW
AF Bhaskaran, Shyam
Abrahamson, Matt
Chesley, Steven
Chung, Min-Kun
Halsell, Allen
Haw, Robert
Helfrich, Cliff
Jefferson, David
Kennedy, Brian
McElrath, Tim
Owen, William
Rush, Brian
Smith, Jonathon
Wang, Tseng-Chan
Yen, Chen-Wan
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI NAVIGATION OF THE EPOXI SPACECRAFT TO COMET HARTLEY 2
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
AB On November 4, 2010, the EPOXI spacecraft flew by the comet Hartley 2, marking the fourth time that a NASA spacecraft successfully captured high resolution images of a cometary nucleus. EPOXI is the extended mission of the Deep Impact mission, which delivered an impactor on comet Tempel-1 on July 4, 2005. EPOXI officially started in September 2007 and eventually took over 3 years of flight time and had 3 Earth gravity assists to achieve the proper encounter conditions. In the process, the mission was redesigned to accommodate a new comet as the target and changes in the trajectory to achieve better imaging conditions at encounter. Challenges in navigation of the spacecraft included precision targeting of several Earth flybys and the comet encounter, uncertainties in determining the ephemeris of the comet relative to the spacecraft, and the high accuracy trajectory knowledge needed to image the comet during the encounter. This paper presents an overview of the navigation process used for the mission.
C1 [Bhaskaran, Shyam; Abrahamson, Matt; Chesley, Steven; Chung, Min-Kun; Halsell, Allen; Haw, Robert; Helfrich, Cliff; Jefferson, David; Kennedy, Brian; McElrath, Tim; Owen, William; Rush, Brian; Smith, Jonathon; Wang, Tseng-Chan; Yen, Chen-Wan] CALTECH, Jet Prop Lab, Nav & Mission Design Sect, Pasadena, CA 91109 USA.
RP Bhaskaran, S (reprint author), CALTECH, Jet Prop Lab, Nav & Mission Design Sect, MS 301-820,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 9
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 1283
EP 1299
PG 17
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400074
ER
PT S
AU Broschart, SB
Sweetser, TH
Angelopoulos, V
Folta, DC
Woodard, MA
AF Broschart, Stephen B.
Sweetser, Theodore H.
Angelopoulos, Vassilis
Folta, David C.
Woodard, Mark A.
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI ARTEMIS LUNAR ORBIT INSERTION AND SCIENCE ORBIT DESIGN THROUGH 2013
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
ID MISSION
AB As of late-July 2011, the ARTEMIS mission is transferring two spacecraft from Lissajous orbits around Earth-Moon Lagrange Point #1 into highly-eccentric lunar science orbits. This paper presents the trajectory design for the transfer from Lissajous orbit to lunar orbit insertion, the period reduction maneuvers, and the science orbits through 2013. The design accommodates large perturbations from Earth's gravity and restrictive spacecraft capabilities to enable opportunities for a range of heliophysics and planetary science measurements. The process used to design the highly-eccentric ARTEMIS science orbits is outlined. The approach may inform the design of future eccentric orbiter missions at planetary moons.
C1 [Broschart, Stephen B.; Sweetser, Theodore H.; Angelopoulos, Vassilis] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Broschart, SB (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
NR 18
TC 0
Z9 0
U1 0
U2 1
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 1609
EP 1627
PG 19
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400093
ER
PT S
AU Folta, D
Sweetser, T
AF Folta, David
Sweetser, Theodore
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI ARTEMIS MISSION OVERVIEW: FROM CONCEPT TO OPERATIONS
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
ID DESIGN
AB ARTEMIS (Acceleration, Reconnection, Turbulence and Electrodynamics of the Moon's Interaction with the Sun) repurposed two spacecraft to extend their useful science (Angelopoulos, 2010) by moving them via lunar gravity assists from elliptical Earth orbits to L-1 and L-2 Earth-Moon libration orbits and then to lunar orbits by exploiting the Earth-Moon-Sun dynamical environment. This paper describes the complete design from conceptual plans using weak stability transfer options and lunar gravity assist to the implementation and operational support of the Earth-Moon libration and lunar orbits. The two spacecraft of the ARTEMIS mission will have just entered lunar orbit at this paper's presentation.
C1 [Folta, David] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Folta, D (reprint author), NASA, Goddard Space Flight Ctr, Code 595, Greenbelt, MD 20771 USA.
EM david.c.folta@nasa.gov; Theodore.h.sweetser@jpl.nasa.gov
NR 17
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 1629
EP 1645
PG 17
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400094
ER
PT S
AU Folta, D
Woodard, M
Sweetser, T
Broschart, SB
Cosgrove, D
AF Folta, David
Woodard, Mark
Sweetser, Theodore
Broschart, Stephen B.
Cosgrove, Daniel
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI DESIGN AND IMPLEMENTATION OF THE ARTEMIS LUNAR TRANSFER USING MULTI-BODY
DYNAMICS
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
ID LIBRATION POINTS; EARTH; TRANSITIONS; ORBITS; L-1
AB The use of multi-body dynamics to design the transfer of spacecraft from Earth elliptical orbits to the Earth-Moon libration (L-1 and L-2) orbits has been successfully demonstrated by the Acceleration Reconnection and Turbulence and Electrodynamics of the Moon's Interaction with the Sun (ARTEMIS) mission. Operational support of the two ARTEMIS spacecraft is a final step in the realization of a design process that can be used to transfer spacecraft with restrictive operational constraints and fuel limitations. The focus of this paper is to describe in detail the processes and implementation of this successful approach.
C1 [Folta, David; Woodard, Mark] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Folta, D (reprint author), NASA, Goddard Space Flight Ctr, Bldg 11,Room S116, Greenbelt, MD 20771 USA.
NR 19
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 1647
EP 1665
PG 19
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400095
ER
PT S
AU Woodard, M
Cosgrove, D
Morinelli, P
Marchese, J
Owens, B
Folta, D
AF Woodard, Mark
Cosgrove, Daniel
Morinelli, Patrick
Marchese, Jeffrey
Owens, Brandon
Folta, David
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI ORBIT DETERMINATION OF SPACECRAFT IN EARTH-MOON L1 AND L2 LIBRATION
POINT ORBITS
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
AB The ARTEMIS mission, part of the THEMIS extended mission is the first to fly spacecraft in the Earth-Moon Lissajous regions. In order to effectively perform lunar Lissajous station-keeping maneuvers, the ARTEMIS operations team has provided orbit determination solutions with typical accuracies on the order of 0.1 km in position and 0.1 cm/s in velocity. The ARTEMIS team utilizes the Goddard Trajectory Determination System (GTDS), using a batch least squares method, to process range and Doppler tracking measurements from the NASA Deep Space Network (DSN), Berkeley Ground Station (BGS), Merritt Island (MILA) station, and United Space Network (USN). The team has also investigated processing of the same tracking data measurements using the Orbit Determination Tool Kit (ODTK) software, which uses an extended Kalman filter and recursive smoother to estimate the orbit. The orbit determination results from each of these methods will be presented and we will discuss the advantages and disadvantages associated with using each method in the lunar Lissajous regions. In addition, we used the Orbit Determination Error Analysis System (ODEAS) to perform covariance analyses using various tracking data schedules. From this analysis, it was determined that 3.5 hours of DSN TRK-2-34 range and Doppler tracking data every other day would suffice to meet the predictive orbit knowledge accuracies in the Lissajous region.
C1 [Woodard, Mark] NASA GSFC, Nav & Miss Design Branch, Greenbelt, MD USA.
RP Woodard, M (reprint author), NASA GSFC, Nav & Miss Design Branch, Greenbelt, MD USA.
NR 8
TC 0
Z9 0
U1 1
U2 2
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 1683
EP 1696
PG 14
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400097
ER
PT S
AU Folta, DC
Woodard, MA
Cosgrove, D
AF Folta, David C.
Woodard, Mark A.
Cosgrove, Daniel
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI STATIONKEEPING OF THE FIRST EARTH-MOON LIBRATION ORBITERS: THE ARTEMIS
MISSION
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
ID POINT ORBITS; KEEPING STRATEGIES
AB Libration point orbits near collinear locations are inherently unstable and must be controlled. For Acceleration Reconnection and Turbulence and Electrodynamics of the Moon's Interaction with the Sun (ARTEMIS) Earth-Moon Lissajous orbit operations, stationkeeping is challenging because of short time scales, large orbital eccentricity of the secondary, and solar gravitational and radiation pressure perturbations. ARTEMIS is the first NASA mission continuously controlled at both Earth-Moon L-1 and L-2 locations and uses a balance of optimization, spacecraft implementation and constraints, and multi-body dynamics. Stationkeeping results are compared to pre-mission research including mode directions.
C1 [Folta, David C.; Woodard, Mark A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Folta, DC (reprint author), NASA, Goddard Space Flight Ctr, Bldg 11,Room S116, Greenbelt, MD 20771 USA.
NR 23
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 1697
EP 1715
PG 19
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400098
ER
PT S
AU Woolley, RC
Mattingly, RL
Riedel, JE
Sturm, EJ
AF Woolley, Ryan C.
Mattingly, Richard L.
Riedel, Joseph E.
Sturm, Erick J.
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI MARS SAMPLE RETURN: LAUNCH AND DETECTION STRATEGIES FOR ORBITAL
RENDEZVOUS
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
AB This study sets forth conceptual mission design strategies for the ascent and rendezvous phase of the proposed NASA/ESA joint Mars Sample Return Campaign. The current notional mission architecture calls for the launch of an acquisition/caching rover in 2018, an Earth return orbiter in 2022, and a fetch rover with ascent vehicle in 2024. Strategies are presented to launch the sample into a nearly coplanar orbit with the Orbiter which would facilitate robust optical detection, orbit determination, and rendezvous. Repeating ground track orbits exist at 457 and 572 km which would provide multiple launch opportunities with similar geometries for detection and rendezvous.
C1 [Woolley, Ryan C.] CALTECH, Jet Prop Lab, Planetary & Lunar Miss Concepts Grp, Pasadena, CA 91109 USA.
RP Woolley, RC (reprint author), CALTECH, Jet Prop Lab, Planetary & Lunar Miss Concepts Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 6
TC 0
Z9 0
U1 1
U2 1
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 1773
EP 1790
PG 18
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400102
ER
PT S
AU Ryne, MS
Mottinger, NA
Broschart, SB
You, TH
Higa, E
Helfrich, C
Berry, D
AF Ryne, Mark S.
Mottinger, Neil A.
Broschart, Stephen B.
You, Tung-Han
Higa, Earl
Helfrich, Cliff
Berry, David
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI NAVIGATION SUPPORT AT JPL FOR THE JAXA AKATSUKI (PLANET-C) VENUS ORBITER
MISSION
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
AB This paper details the orbit determination activities undertaken at JPL in support of the Japanese Aerospace Exploration Agency's (JAXA) Akatsuki (a.k.a. Planet-C and/or Venus Climate Orbiter) mission. The JPL navigation team's role was to provide independent navigation support as a point of comparison with the JAXA generated orbit determination solutions. Topics covered include a mission and spacecraft overview, dynamic forces modeling, cruise and approach orbit determination results, and the international teaming arrangement. Significant discussion is dedicated to the events surrounding recovery from the unsuccessful Venus orbit insertion maneuver.
C1 [Ryne, Mark S.; Mottinger, Neil A.; Broschart, Stephen B.; Higa, Earl; Helfrich, Cliff; Berry, David] CALTECH, Jet Prop Lab, Miss Design & Nav Sect, Pasadena, CA 91109 USA.
RP Ryne, MS (reprint author), CALTECH, Jet Prop Lab, Miss Design & Nav Sect, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 6
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 1799
EP 1818
PG 20
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400104
ER
PT S
AU Sklyanskiy, E
You, TH
Cheatwood, N
Cianciolo, AD
Bowes, A
AF Sklyanskiy, Evgeniy
You, Tung-Han
Cheatwood, Neil
Cianciolo, Alicia Dwyer
Bowes, Angela
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI PASSIVE AEROGRAVITY ASSISTED TRAJECTORIES FOR A MARS ATMOSPHERIC SAMPLE
RETURN MISSION
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
ID INTERPLANETARY TRAJECTORIES; DESIGN
AB A number of studies have demonstrated that aerodynamic lift during a planetary low-altitude atmospheric flyby can increase the V-infinity bending angle and the total Delta V achievable from gravity assist. Aero-Gravity Assist (AGA) trajectories of this type require a significantly high spacecraft L/D (lift-to-drag) ratio and a fairly robust closed-loop guidance algorithm capable of providing a desired control authority for level, nearly constant-altitude atmospheric flight. The AGA concept has been described in some previous publications as one of the techniques for Mars and Venus atmospheric sample return mission design strategies. Recent analysis has demonstrated that passive, ballistic (zero-lift) aeropass trajectories could equally satisfy potential future sample return mission objectives and provide quite robust and simple alternatives to a complex guided AGA lifting trajectory design.
C1 [Sklyanskiy, Evgeniy] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Sklyanskiy, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 21
TC 0
Z9 0
U1 0
U2 1
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 1819
EP 1833
PG 15
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400105
ER
PT S
AU Parker, JJK
Hughes, SP
AF Parker, Joel J. K.
Hughes, Steven P.
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI A GENERAL EVENT LOCATION ALGORITHM WITH APPLICATIONS TO ECLIPSE AND
STATION LINE-OF-SIGHT
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
AB A general-purpose algorithm for the detection and location of orbital events is developed. The proposed algorithm reduces the problem to a global root-finding problem by mapping events of interest (such as eclipses, station access events, etc.) to continuous, differentiable event functions. A stepping algorithm and a bracketing algorithm are used to detect and locate the roots. Examples of event functions and the stepping/bracketing algorithms are discussed, along with results indicating performance and accuracy in comparison to commercial tools across a variety of trajectories.
C1 [Parker, Joel J. K.; Hughes, Steven P.] NASA, Goddard Space Flight Ctr, Nav & Mission Design Branch, Greenbelt, MD 20771 USA.
RP Parker, JJK (reprint author), NASA, Goddard Space Flight Ctr, Nav & Mission Design Branch, Code 595,8800 Greenbelt Rd, Greenbelt, MD 20771 USA.
NR 6
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 1885
EP 1898
PG 14
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400109
ER
PT S
AU Wagner, SV
Arrieta, J
Ballard, CG
Hahn, Y
Stumpf, PW
Valerino, PN
AF Wagner, Sean V.
Arrieta, Juan
Ballard, Christopher G.
Hahn, Yungsun
Stumpf, Paul W.
Valerino, Powtawche N.
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI CASSINI SOLSTICE MISSION MANEUVER EXPERIENCE: YEAR ONE
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
AB The Cassini-Huygens spacecraft began its four-year Prime Mission to study Saturn's system in July 2004. Two tour extensions followed: a two-year Equinox Mission beginning in July 2008 and a seven-year Solstice Mission starting in September 2010. This paper highlights Cassini maneuver activities from June 2010 through June 2011, covering the transition from the Equinox to Solstice Mission. This interval included 38 scheduled maneuvers, eight targeted Titan flybys, three targeted Enceladus flybys, and one close Rhea flyby. In addition, beyond the demanding nominal navigation schedule, numerous unforeseen challenges further complicated maneuver operations. These challenges will be discussed in detail.
RP Wagner, SV (reprint author), CALTECH, Jet Prop Lab, Mail Stop 230-205,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Sean.V.Wagner@jpl.nasa.gov
NR 25
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 1899
EP 1917
PG 19
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400110
ER
PT S
AU Ballard, CG
Ionasescu, R
AF Ballard, Christopher G.
Ionasescu, Rodica
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI FLIGHT PATH CONTROL DESIGN FOR THE CASSINI SOLSTICE MISSION
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
AB The Cassini spacecraft has been in orbit around Saturn for just over 7 years, with a planned 7-year extension, called the Solstice Mission, which started on September 27, 2010. The Solstice Mission includes 205 maneuvers and 70 flybys which consist of the moons Titan, Enceladus, Dione, and Rhea. This mission is designed to use all available propellant with a statistical margin averaging 0.6 m/s per encounter, and the work done to prove and ensure the viability of this margin is highlighted in this paper.
C1 [Ballard, Christopher G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Ballard, CG (reprint author), CALTECH, Jet Prop Lab, Mail Stop 230-205,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Christo-pher.G.Ballard@jpl.nasa.gov
NR 17
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 1933
EP 1949
PG 17
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400112
ER
PT S
AU Ely, TA
Chau, AH
AF Ely, Todd A.
Chau, Alexandra H.
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI RADAR ALTIMETRY AND VELOCIMETRY FOR INERTIAL NAVIGATION: A LUNAR LANDING
EXAMPLE
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
AB The traditional role that altimetry and velocimetry have played in spacecraft landings is to provide a direct measure of the spacecraft's surface altitude and surface relative velocity; however, their role in determining an inertial position and velocity has seen limited investigation. In this study, inertially sensitive measurement models for altimetry and velocimetry are formulated and include relevant instrument and environment error models. These models are applied and simulated for a realistic lunar landing scenario that is based on recent work for NASA's Altair lander. The preliminary results indicate that an inertial landing accuracy of several meters is possible.
C1 [Ely, Todd A.] CALTECH, Jet Prop Lab, Mission Design & Nav Sect, Pasadena, CA 91109 USA.
RP Ely, TA (reprint author), CALTECH, Jet Prop Lab, Mission Design & Nav Sect, MS 301-121,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Todd.A.Ely@jpl.nasa.gov; Alexandra.H.Chau@jpl.nasa.gov
NR 12
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 2023
EP 2042
PG 20
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933400117
ER
PT S
AU Abilleira, F
AF Abilleira, Fernando
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI 2011 MARS SCIENCE LABORATORY LAUNCH PERIOD DESIGN
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
AB The Mars Science Laboratory mission, set to launch in the fall of 2011, has the primary objective of landing the most advanced rover to date to the surface of Mars to assess whether Mars ever was, or still is today, able to sustain carbon-based life. Arriving at Mars in August 2012, the Mars Science Laboratory will also demonstrate the ability to deliver large payloads to the surface of Mars, land more accurately (than previous missions) in a 20-km by 25-km ellipse, and traverse up to 20 km. Following guided entry and parachute deployment, the spacecraft will descend on a parachute and a Powered Descent Vehicle to safely land the rover on the surface of Mars. The launch/arrival strategy is driven by several key requirements, which include: launch vehicle capability, atmosphere-relative entry speed, communications coverage during Entry, Descent and Landing, latitude accessibility, and dust storm season avoidance. Notable among these requirements is maintaining a telecommunications link from atmospheric entry to landing plus one minute, via a Direct-To-Earth X-band link and via orbital assets using an UHF link, to ensure that any failure during Entry, Descent and Landing can be reconstructed in case of a mission anomaly. Due to concerns related to the lifetime of the relay orbiters, two additional launch/arrival strategies have been developed to improve Entry, Descent, and Landing communications. This paper discusses the final launch/arrival strategy selected prior to the launch period down-selection that is scheduled to occur in August 2011. It is also important to note that this paper is an update to Ref. 1 in that it includes two new Type 1 launch periods and drops the Type 2 launch period that is no longer considered.
C1 CALTECH, Jet Prop Lab, Inner Planets Mission Anal Grp, Pasadena, CA 91109 USA.
RP Abilleira, F (reprint author), CALTECH, Jet Prop Lab, Inner Planets Mission Anal Grp, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Fernando.Abilleira@jpl.nasa.gov
NR 11
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 2345
EP 2364
PG 20
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933401017
ER
PT S
AU Senent, JS
Garcia, J
AF Senent, Juan S.
Garcia, Jaume
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI CLOSED-FORM AND NUMERICALLY-STABLE SOLUTIONS TO PROBLEMS RELATED TO THE
OPTIMAL TWO-IMPULSE TRANSFER BETWEEN SPECIFIED TERMINAL STATES OF
KEPLERIAN ORBITS
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
ID REVOLUTION LAMBERT SOLUTIONS
AB The first part of the paper presents some closed-form solutions to the optimal two-impulse transfer between fixed position and velocity vectors on Keplerian orbits when some constraints are imposed on the magnitude of the initial and final impulses. Additionally, a numerically-stable gradient-free algorithm with guaranteed convergence is presented for the minimum delta-v two-impulse transfer. In the second part of the paper, cooperative bargaining theory is used to solve some two-impulse transfer problems when the initial and final impulses are carried by different vehicles or when the goal is to minimize the delta-v and the time-of-flight at the same time.
C1 [Senent, Juan S.] NASA, Johnson Space Ctr, Flight Mech & Trajectory Design Branch, Houston, TX 77058 USA.
RP Senent, JS (reprint author), NASA, Johnson Space Ctr, Flight Mech & Trajectory Design Branch, EG5, Houston, TX 77058 USA.
NR 16
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 2385
EP 2404
PG 20
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933401019
ER
PT S
AU Scott, JR
AF Scott, James R.
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI TAYLOR SERIES TRAJECTORY CALCULATIONS INCLUDING OBLATENESS EFFECTS AND
VARIABLE ATMOSPHERIC DENSITY
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
AB Taylor series integration is implemented in NASA Glenn's Spacecraft N-body Analysis Program, and compared head-to-head with the code's existing 8th-order Runge-Kutta Fehlberg time integration scheme. This paper focuses on trajectory problems that include oblateness and/or variable atmospheric density. Taylor series is shown to be significantly faster and more accurate for oblateness problems up through a 4x4 field, with speedups ranging from a factor of 2 to 13. For problems with variable atmospheric density, speedups average 24 for atmospheric density alone, and average 1.6 to 8.2 when density and oblateness are combined.
C1 NASA, Glenn Res Ctr, Syst Engn & Anal Div, Cleveland, OH 44135 USA.
RP Scott, JR (reprint author), NASA, Glenn Res Ctr, Syst Engn & Anal Div, 21000 Brookpk Rd,Mail Stop 86-1, Cleveland, OH 44135 USA.
NR 9
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 2499
EP 2512
PG 14
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933401025
ER
PT S
AU Brown, AJ
AF Brown, Aaron J.
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI A MINIMUM Delta V ORBIT MAINTENANCE STRATEGY FOR LOW-ALTITUDE MISSIONS
USING BURN PARAMETER OPTIMIZATION
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
AB Orbit maintenance is the series of burns performed during a mission to ensure the orbit satisfies mission constraints. Low-altitude missions often require non-trivial orbit maintenance Delta V due to sizable orbital perturbations and minimum altitude thresholds. A strategy is presented for minimizing this Delta V using impulsive burn parameter optimization. An initial estimate for the burn parameters is generated by considering a feasible solution to the orbit maintenance problem. An low-lunar orbit example demonstrates the Delta V savings from the feasible solution to the optimal solution. The strategy's extensibility to more complex missions is discussed, as well as the limitations of its use.
C1 NASA, Flight Dynam Div, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Brown, AJ (reprint author), NASA, Flight Dynam Div, Lyndon B Johnson Space Ctr, Mail Code DM34,2101 NASA Pkwy, Houston, TX 77058 USA.
NR 8
TC 0
Z9 0
U1 0
U2 2
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 3581
EP 3596
PG 16
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933401088
ER
PT S
AU Dannemiller, DP
AF Dannemiller, David P.
BE Schaub, H
Gunter, BC
Russell, RP
Cerven, WT
TI MULTI-MANEUVER CLOHESSY-WILTSHIRE TARGETING
SO ASTRODYNAMICS 2011, PTS I - IV
SE Advances in the Astronautical Sciences
LA English
DT Proceedings Paper
CT AAS/AIAA Astrodynamics Specialist Conference
CY JUL 31-AUG 04, 2011
CL AK
SP AAS, AIAA
AB A non-iterative method is presented for targeting a rendezvous scenario that includes a sequence of maneuvers and relative constraints. This method is referred to as Multi-Maneuver Clohessy-Wiltshire Targeting (MM_CW_TGT). When a single maneuver is targeted to a single relative position, the classic CW targeting solution is obtained. The MM_CW_TGT method involves manipulation of the CW state transition matrix to form a linear system. Solution of the linear system includes the straight-forward inverse of a square matrix. Example solutions are presented for several rendezvous scenarios to illustrate the utility of the method.
C1 NASA, Flight Dynam Div, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
RP Dannemiller, DP (reprint author), NASA, Flight Dynam Div, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA.
EM David.P.Dannemiller@nasa.gov
NR 1
TC 0
Z9 0
U1 0
U2 0
PU UNIVELT INC
PI SAN DIEGO
PA PO BOX 28130, SAN DIEGO, CA 92128 USA
SN 1081-6003
BN 978-0-87703-577-0
J9 ADV ASTRONAUT SCI
PY 2012
VL 142
BP 3767
EP 3780
PG 14
WC Engineering, Aerospace
SC Engineering
GA BFY99
UT WOS:000321933401099
ER
PT S
AU Kessel, RL
AF Kessel, R. L.
BE Summers, D
Mann, IR
Baker, DN
Schulz, M
TI NASA's Radiation Belt Storm Probes Mission: From Concept to Reality
SO DYNAMICS OF THE EARTH'S RADIATION BELTS AND INNER MAGNETOSPHERE
SE Geophysical Monograph Series
LA English
DT Proceedings Paper
CT AGU Chapman Conference Dynamics of the Earth's Radiation Belts and Inner
Magnetosphere
CY JUL 17-22, 2011
CL St Johns, CANADA
ID RELATIVISTIC ELECTRON MICROBURSTS; LOSSES; CHORUS
AB NASA's Radiation Belt Storm Probes (RBSP) mission is a two-satellite mission designed to measure charged particle populations, fields, and waves in the Van Allen radiation belts in order to provide understanding of how these change in response to variable inputs of energy from the Sun. This paper tracks the progress of the mission from formulation and the development of science objectives through instrument selection to mission design, integration, and testing, with an emphasis on how the chosen measurements address the science objectives. At the start of normal operations (similar to 60 days after launch), the spacecraft will be positioned to address a number of science questions such as the nature of whistler mode interactions and their roles in electron energization and loss, the large-scale dynamics and structure of the magnetosphere during geomagnetic storms, and the source, structure, and dynamics of the inner (L < 2) ion and electron belts. Collaborations with other missions such as Time History of Events and Macroscale Interactions during Substorrns and Balloon Array for Radiation-belt Relativistic Electron Losses will enable studies of dawn-dusk differences in magnetospheric particle populations and will quantify particle losses through the magnetopause for comparison with losses by precipitation into the ionosphere. A real-time space weather broadcast will enable nowcasting of radiation belt conditions. The RBSP Key Messages summarize the high-level impacts expected from the mission.
C1 NASA, Washington, DC 20546 USA.
RP Kessel, RL (reprint author), NASA, 300 E St,SW, Washington, DC 20546 USA.
EM mona.kessel@nasa.gov
NR 15
TC 7
Z9 7
U1 1
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0065-8448
BN 978-0-87590-489-4
J9 GEOPHYS MONOGR SER
PY 2012
VL 199
BP 93
EP 101
DI 10.1029/2012GM001312
PG 9
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Geosciences,
Multidisciplinary
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Geology
GA BFZ10
UT WOS:000321935300007
ER
PT S
AU Baker, K
Epperson, D
Goldstein, H
Skrupky, K
Smith, B
Gitschlag, G
Lewandowski, J
Turk, T
AF Baker, Kyle
Epperson, Deborah
Goldstein, Howard
Skrupky, Kimberly
Smith, Brad
Gitschlag, Gregg
Lewandowski, Jill
Turk, Teresa
BE Popper, AN
Hawkins, A
TI Standardizing Protected Species Observer Requirements in the United
States
SO EFFECTS OF NOISE ON AQUATIC LIFE
SE Advances in Experimental Medicine and Biology
LA English
DT Article
C1 [Baker, Kyle] NOAA, Natl Marine Fisheries Serv, St Petersburg, FL 33701 USA.
[Epperson, Deborah] Bur Ocean Energy Management Regulat & Enforcement, New Orleans, LA 70123 USA.
[Goldstein, Howard; Turk, Teresa] NOAA, Natl Marine Fisheries Serv, Silver Spring, MD 20910 USA.
[Skrupky, Kimberly; Lewandowski, Jill] Bur Ocean Energy Management Regulat & Enforcement, Herndon, VA 20170 USA.
[Smith, Brad] NOAA, Natl Marine Fisheries Serv, Anchorage, AK 99513 USA.
[Gitschlag, Gregg] NOAA, Natl Marine Fisheries Serv, Galveston, TX 77551 USA.
RP Baker, K (reprint author), NOAA, Natl Marine Fisheries Serv, St Petersburg, FL 33701 USA.
EM kyle.baker@noaa.gov; deborah.epperson@boemre.gov;
howard.goldstein@noaa.gov; kimberly.skrupky@boemre.gov;
brad.smith@noaa.gov; gregg.gitschlag@noaa.gov;
jill.lewandowski@boemre.gov; teresa.turk@nooa.gov
NR 0
TC 0
Z9 0
U1 0
U2 1
PU SPRINGER
PI NEW YORK
PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES
SN 0065-2598
BN 978-1-4419-7310-8
J9 ADV EXP MED BIOL
JI Adv.Exp.Med.Biol.
PY 2012
VL 730
BP 637
EP 639
DI 10.1007/978-1-4419-7311-5_145
PG 3
WC Biology; Medicine, Research & Experimental
SC Life Sciences & Biomedicine - Other Topics; Research & Experimental
Medicine
GA BFV95
UT WOS:000321592700145
PM 22278582
ER
PT S
AU Goldstein, H
Epperson, D
Baker, K
Skrupky, K
Smith, B
Gitschlag, G
Lewandowski, J
Turk, T
AF Goldstein, Howard
Epperson, Deborah
Baker, Kyle
Skrupky, Kimberly
Smith, Brad
Gitschlag, Gregg
Lewandowski, Jill
Turk, Teresa
BE Popper, AN
Hawkins, A
TI Development of a National Database and Standards for Protected Species
Observer Data in the United States
SO EFFECTS OF NOISE ON AQUATIC LIFE
SE Advances in Experimental Medicine and Biology
LA English
DT Article
C1 [Goldstein, Howard; Turk, Teresa] NOAA, Natl Marine Fisheries Serv, Silver Spring, MD 20910 USA.
[Epperson, Deborah] Bur Ocean Energy Management Regulat & Enforcement, New Orleans, LA 70123 USA.
[Baker, Kyle] NOAA, Natl Marine Fisheries Serv, St Petersburg, FL 33701 USA.
[Skrupky, Kimberly; Lewandowski, Jill] Bur Ocean Energy Management Regulat & Enforcement, Herndon, VA 20170 USA.
[Smith, Brad] NOAA, Natl Marine Fisheries Serv, Anchorage, AK 99513 USA.
[Gitschlag, Gregg] NOAA, Natl Marine Fisheries Serv, Galveston, TX 77551 USA.
RP Goldstein, H (reprint author), NOAA, Natl Marine Fisheries Serv, Silver Spring, MD 20910 USA.
EM Howard.Goldstein@noaa.gov; Deborah.Epperson@boemre.gov;
Kyle.Baker@noaa.gov; Kimberly.Skrupky@boemre.gov; Brad.Smith@noaa.gov;
Gregg.Gitschlag@noaa.gov; Jill.Lewankowski@boemre.gov;
Teresa.Turk@noaa.gov
NR 0
TC 0
Z9 0
U1 0
U2 0
PU SPRINGER
PI NEW YORK
PA 233 SPRING STREET, NEW YORK, NY 10013, UNITED STATES
SN 0065-2598
BN 978-1-4419-7310-8
J9 ADV EXP MED BIOL
JI Adv.Exp.Med.Biol.
PY 2012
VL 730
BP 645
EP 647
DI 10.1007/978-1-4419-7311-5_147
PG 3
WC Biology; Medicine, Research & Experimental
SC Life Sciences & Biomedicine - Other Topics; Research & Experimental
Medicine
GA BFV95
UT WOS:000321592700147
PM 22278584
ER
PT S
AU Chow, E
Vatan, F
Paloulian, G
Frisbie, S
Srostlik, Z
Kalomiris, V
Apgar, D
AF Chow, Edward
Vatan, Farrokh
Paloulian, George
Frisbie, Steve
Srostlik, Zuzana
Kalomiris, Vasilios
Apgar, Daniel
GP IEEE
TI Dynamic Communication Resource Negotiations
SO 2012 IEEE MILITARY COMMUNICATIONS CONFERENCE (MILCOM 2012)
SE IEEE Military Communications Conference
LA English
DT Proceedings Paper
CT IEEE Military Communications Conference (MILCOM)
CY OCT 29-NOV 01, 2012
CL Orlando, FL
SP IEEE, AFCEA Int, IEEE Commun Soc
DE Policy-Based Management; Policy Negotiation; Network Management
AB Today's advanced network management systems can automate many aspects of the tactical networking operations within a military domain. However, automation of joint and coalition tactical networking across multiple domains remains challenging. Due to potentially conflicting goals and priorities, human agreement is often required before implementation into the network operations. This is further complicated by incompatible network management systems and security policies, rendering it difficult to implement automatic network management, thus requiring manual human intervention to the communication protocols used at various network routers and endpoints. This process of manual human intervention is tedious, error-prone, and slow. In order to facilitate a better solution, we are pursuing a technology which makes network management automated, reliable, and fast. Automating the negotiation of the common network communication parameters between different parties is the subject of this paper. We present the technology that enables inter-force dynamic communication resource negotiations to enable ad-hoc inter-operation in the field between force domains, without pre-planning. It also will enable a dynamic response to changing conditions within the area of operations. Our solution enables the rapid blending of intra-domain policies so that the forces involved are able to inter-operate effectively without overwhelming each other's networks with in-appropriate or un-warranted traffic. It will evaluate the policy rules and configuration data for each of the domains, then generate a compatible inter-domain policy and configuration that will update the gateway systems between the two domains.
C1 [Chow, Edward; Vatan, Farrokh; Paloulian, George] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
[Frisbie, Steve; Srostlik, Zuzana] SPAWAR Syst Ctr Pacific, San Diego, CA USA.
[Kalomiris, Vasilios; Apgar, Daniel] US Army, CERDEC S& TCD, Aberdeen Proving Ground, MD USA.
RP Chow, E (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
NR 9
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 2155-7578
BN 978-1-4673-1729-0; 978-1-4673-1730-6
J9 IEEE MILIT COMMUN C
PY 2012
PG 6
WC Telecommunications
SC Telecommunications
GA BEY60
UT WOS:000318702900212
ER
PT B
AU Chamis, CC
Murthy, PLN
AF Chamis, Christos C.
Murthy, Pappu L. N.
GP ASME
TI VIBRATION OF FIBER REINFORCED ANISOTROPIC COMPOSITE PLATES WITH
NANOFIBER REINFORCED MATRICES
SO PROCEEDINGS OF THE ASME INTERNATIONAL MECHANICAL ENGINEERING CONGRESS
AND EXPOSITION - 2010, VOL 8, PTS A AND B
LA English
DT Proceedings Paper
CT ASME International Mechanical Engineering Congress and Exposition
(IMECE)
CY NOV 12-18, 2010
CL Vancouver, CANADA
SP Amer Soc Mech Engineers
AB Anisotropic composite plates were evaluated with nanofiber reinforced matrices (NFRM). The nanofiber reinforcement volumes ratio in the matrix was 0.01. The plate dimensions were 20 by 10 by 1.0 in. (508 by 254 by 25.4 mm). Seven different loading condition cases were evaluated: three for uniaxial loading, three for pairs of combined loading, and one with three combined loadings. The anisotropy arose from the unidirectional plates having been at 30 degrees from the structural axis. The anisotropy had a full 6 by 6 rigidities matrix which were satisfied and solved by a Galerkin buckling algorithm. The buckling results showed that the NFRM plates buckled at about twice those with conventional matrix.
C1 [Chamis, Christos C.; Murthy, Pappu L. N.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Chamis, CC (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
NR 5
TC 0
Z9 0
U1 0
U2 1
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-4445-8
PY 2012
BP 513
EP 528
PG 16
WC Automation & Control Systems; Engineering, Mechanical
SC Automation & Control Systems; Engineering
GA BFQ45
UT WOS:000320970700065
ER
PT J
AU Chattopadhyay, G
AF Chattopadhyay, Goutam
GP IEEE
TI Terahertz Science, Technology, and Communication
SO 2012 5TH INTERNATIONAL CONFERENCE ON COMPUTERS AND DEVICES FOR
COMMUNICATION (CODEC)
LA English
DT Proceedings Paper
CT 5th International Conference on Computers and Devices for Communication
(CODEC)
CY DEC 17-19, 2012
CL Kolkata, INDIA
SP Univ Calcutta, Inst Radio Phys Elect
AB The term "terahertz" has been ubiquitous in the arena of technology over the past couple of years. New applications are emerging every day which are exploiting the promises of terahertz - its small wavelength; capability of penetrating dust, clouds, and fog; and possibility of having large instantaneous bandwidth for high-speed communication channels. Until very recently, space-based instruments for astrophysics, planetary science, and Earth science missions have been the primary motivator for the development of terahertz sensors, sources, and systems. However, in recent years the emerging areas such as imaging from space platforms, surveillance of person-borne hidden weapons or contraband from a safe stand-off distance and reconnaissance, medical imaging and DNA sequencing, and in the world high speed communications have been the driving force for this area of research.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Chattopadhyay, G (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 6
TC 0
Z9 0
U1 0
U2 4
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4673-2620-9
PY 2012
PG 4
WC Engineering, Electrical & Electronic; Telecommunications
SC Engineering; Telecommunications
GA BFL44
UT WOS:000320383100077
ER
PT B
AU Datta, CR
Datta, A
Gupta, D
Chakravarty, SK
AF Datta, C. R.
Datta, Abhirup
Gupta, Dola
Chakravarty, S. K.
GP IEEE
TI y Performance Analysis of Adaptive Power Control Algorithm For Varying
Target SIR
SO 2012 5TH INTERNATIONAL CONFERENCE ON COMPUTERS AND DEVICES FOR
COMMUNICATION (CODEC)
LA English
DT Proceedings Paper
CT 5th International Conference on Computers and Devices for Communication
(CODEC)
CY DEC 17-19, 2012
CL Kolkata, INDIA
SP Univ Calcutta, Inst Radio Phys Elect
DE Cellular networks; Mobile communication; Quality of service; Radio
transceivers
AB In this paper we study the performance of two Power Control algorithms: the Adaptive Standard Power Control (ASPC) and the Standard Power Control (PCA) algorithms. Simulation of both algorithms is being done under three different network conditions including the case with varying SIR target. The results from our simulations are shown graphically. These results show that the performance ASPC is be better than PCA under the different network conditions considered in this paper. All simulations are done in MATLAB.
C1 [Datta, C. R.] Govt West Bengal, Sch Educ Dept, Kolkata, India.
[Datta, Abhirup] Univ Colorado, NASA, Boulder, CO 80309 USA.
[Gupta, Dola] Narula Inst Technol, Kolkata, India.
[Chakravarty, S. K.] Govt West Bengal, Dept Educ, Kolkata, W Bengal, India.
RP Datta, CR (reprint author), Govt West Bengal, Sch Educ Dept, Kolkata, India.
EM crdatta@gmail.com; Abhirup.Datta@colorado.edu; dola.ju@gmail.com;
skchakravarty@gmail.com
NR 10
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4673-2620-9; 978-1-4673-2619-3
PY 2012
PG 4
WC Engineering, Electrical & Electronic; Telecommunications
SC Engineering; Telecommunications
GA BFL44
UT WOS:000320383100154
ER
PT B
AU Simon, DL
Armstrong, JB
Garg, S
AF Simon, Donald L.
Armstrong, Jeffrey B.
Garg, Sanjay
GP ASME
TI APPLICATION OF AN OPTIMAL TUNER SELECTION APPROACH FOR ON-BOARD
SELF-TUNING ENGINE MODELS
SO PROCEEDINGS OF THE ASME TURBO EXPO 2011, VOL 3
LA English
DT Proceedings Paper
CT ASME Turbo Expo 2011
CY JUN 06-10, 2011
CL Vancouver, CANADA
SP ASME, Int Gas Turbine Inst
AB An enhanced design methodology for minimizing the error in on-line Kalman filter-based aircraft engine performance estimation applications is presented in this paper. It specifically addresses the underdetermined estimation problem, in which there are more unknown parameters than available sensor measurements. This work builds upon an existing technique for systematically selecting a model tuning parameter vector of appropriate dimension to enable estimation by a Kalman filter, while minimizing the estimation error in the parameters of interest. While the existing technique was optimized for open-loop engine operation at a fixed design point, in this paper an alternative formulation is presented that enables the technique to be optimized for an engine operating under closed-loop control throughout the flight envelope. The theoretical Kalman filter mean squared estimation error at a steady-state closed-loop operating point is derived, and the tuner selection approach applied to minimize this error is discussed. A technique for constructing a globally optimal tuning parameter vector, which enables full-envelope application of the technology, is also presented, along with design steps for adjusting the dynamic response of the Kalman filter state estimates. Results from the application of the technique to linear and nonlinear aircraft engine simulations are presented and compared to the conventional approach of tuner selection. The new methodology is shown to yield a significant improvement in on-line Kalman filter estimation accuracy.
C1 [Simon, Donald L.; Garg, Sanjay] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA.
RP Simon, DL (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,MS 77-1, Cleveland, OH 44135 USA.
NR 11
TC 0
Z9 0
U1 0
U2 0
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-5463-1
PY 2012
BP 361
EP 373
PG 13
WC Engineering, Mechanical
SC Engineering
GA BFQ42
UT WOS:000320967100035
ER
PT B
AU Thurman, DR
El-Gabry, LA
Poinsatte, PE
Heidmann, JD
AF Thurman, Douglas R.
El-Gabry, Lamyaa A.
Poinsatte, Philip E.
Heidmann, James D.
GP ASME
TI TURBULENCE AND HEAT TRANSFER MEASUREMENTS IN AN INCLINED LARGE SCALE
FILM COOLING ARRAY - PART II, TEMPERATURE AND HEAT TRANSFER MEASUREMENTS
SO PROCEEDINGS OF THE ASME TURBO EXPO 2011, VOL 5, PTS A AND B
LA English
DT Proceedings Paper
CT ASME Turbo Expo 2011
CY JUN 06-10, 2011
CL Vancouver, CANADA
SP ASME, Int Gas Turbine Inst
ID STREAMWISE ANGLES; CROSS-FLOW; HOLES; ROW; DOWNSTREAM; INJECTION; RATIO
AB The second of a two-part paper, this study focuses on the temperature field and surface heat transfer measurements on a large-scale models of an inclined row of film cooling holes. Detailed surface and flow field measurements were taken and presented in Part I. The model consists of three holes of 1.9-cm diameter that are spaced 3 hole diameters apart and inclined 30 degrees from the surface. Additionally, another model with an anti-vortex adaptation to the film cooling holes is also tested. The coolant stream is metered and cooled to 20 degrees C below the mainstream temperature. A thermocouple is used to obtain the flow temperatures along the jet centerline and at various streamwise locations. Steady state liquid crystal thermography is used to obtain surface heat transfer coefficients. Results are obtained for blowing ratios of up to 2 in order to capture off-design conditions in which the jet is lifted. Film cooling effectiveness values of 0.4 and 0.15 were found along the centerline for blowing ratios of 1 and 2 respectively. In addition, an anti-vortex design was tested and found to have improved film effectiveness. This paper presents the detailed temperature contours showing the extent of mixing between the coolant and freestream and the local heat transfer results.
C1 [Thurman, Douglas R.] US Army, Res Lab, Glenn Res Ctr, Cleveland, OH USA.
RP Thurman, DR (reprint author), US Army, Res Lab, Glenn Res Ctr, Cleveland, OH USA.
NR 16
TC 0
Z9 0
U1 0
U2 1
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-5465-5
PY 2012
BP 551
EP 558
PG 8
WC Engineering, Mechanical
SC Engineering
GA BFR71
UT WOS:000321076300049
ER
PT B
AU Bonacuse, PJ
Mital, S
Goldberg, R
AF Bonacuse, Peter J.
Mital, Subodh
Goldberg, Robert
GP ASME
TI CHARACTERIZATION OF THE AS MANUFACTURED VARIABILITY IN A CVI SIC/SIC
WOVEN COMPOSITE
SO PROCEEDINGS OF THE ASME TURBO EXPO 2011, VOL 6, PTS A AND B
LA English
DT Proceedings Paper
CT ASME Turbo Expo 2011
CY JUN 06-10, 2011
CL Vancouver, CANADA
SP ASME, Int Gas Turbine Inst
AB The microstructure of a 2D woven ceramic matrix composite displays significant variability and irregularity. For example, a chemical vapor infiltrated (CVI) SiC/SiC composite exhibits significant amount of porosity arranged in irregular patterns. Furthermore, the fiber tows within a ply frequently have irregular shape and spacing, and the stacked plies are often misaligned and nested within each other. The goal of an ongoing project at NASA Glenn is to investigate the effects of the complex microstructure and its variability on the properties and the durability of the material. One key requirement for this effort is the development of methods to characterize the distribution in as-fabricated ceramic matrix composite (CMC) microstructures with the objective of correlating microstructural distribution parameters with mechanical performance. An initial task in this effort was to perform quantitative image analysis of polished cross sections of CVI SiC/SiC composite specimens. This analysis provided sample distributions of various microstructural composite features, including: inter-tow pore sizes and shapes, transverse sectioned tow sizes and shapes, and within ply tow spacing. This information can then be used to quantify the effect of extreme values of these features on the local stress state with the goal of determining the likelihood of matrix cracking at a given external load.
C1 [Bonacuse, Peter J.; Goldberg, Robert] NASA, Glenn Res Ctr, Cleveland, OH USA.
RP Bonacuse, PJ (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA.
NR 5
TC 0
Z9 0
U1 0
U2 2
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-5466-2
PY 2012
BP 741
EP 746
PG 6
WC Engineering, Mechanical
SC Engineering
GA BFS59
UT WOS:000321160200076
ER
PT B
AU Provenza, AJ
Morrison, CR
AF Provenza, Andrew J.
Morrison, Carlos R.
GP ASME
TI CONTROL OF FAN BLADE VIBRATIONS USING PIEZOELECTRICS AND BI-DIRECTIONAL
TELEMETRY
SO PROCEEDINGS OF THE ASME TURBO EXPO 2011, VOL 6, PTS A AND B
LA English
DT Proceedings Paper
CT ASME Turbo Expo 2011
CY JUN 06-10, 2011
CL Vancouver, CANADA
SP ASME, Int Gas Turbine Inst
AB A novel wireless device which transfers supply power through induction to rotating operational amplifiers and transmits low voltage AC signals to and from a rotating body by way of radio telemetry has been successfully demonstrated in the NASA Glenn Research Center (GRC) Dynamic Spin Test Facility.
In the demonstration described herein, a rotating operational amplifier provides controllable AC power to a piezoelectric patch epoxied to the surface of a rotating Ti plate. The amplitude and phase of the sinusoidal voltage command signal, transmitted wirelessly to the amplifier, was tuned to completely suppress the 3rd bending resonant vibration of the plate.
The plate's 3rd bending resonance was excited using rotating magnetic bearing excitation while it spun at slow speed in a vacuum chamber. A second patch on the opposite side of the plate was used as a sensor.
This paper discusses the characteristics of this novel device, the details of a spin test, results from a preliminary demonstration, and future plans.
C1 [Provenza, Andrew J.; Morrison, Carlos R.] NASA, Glenn Res Ctr, Cleveland, OH USA.
RP Provenza, AJ (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA.
NR 18
TC 0
Z9 0
U1 0
U2 1
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-5466-2
PY 2012
BP 923
EP 930
PG 8
WC Engineering, Mechanical
SC Engineering
GA BFS59
UT WOS:000321160200094
ER
PT B
AU Shyam, V
Ameri, A
AF Shyam, Vikram
Ameri, Ali
GP ASME
TI Comparison of Various Supersonic Turbine Tip Designs to Minimize
Aerodynamic Loss and Tip Heating
SO PROCEEDINGS OF THE ASME TURBO EXPO 2011, VOL 7, PTS A-C
LA English
DT Proceedings Paper
CT ASME Turbo Expo 2011
CY JUN 06-10, 2011
CL Vancouver, CANADA
SP ASME, Int Gas Turbine Inst
AB The rotor tips of axial turbines experience high heat flux and are the cause of aerodynamic losses due to tip clearance flows, and in the case of supersonic tips, shocks. As stage loadings increase, the flow in the tip gap approaches and exceeds sonic conditions. This introduces effects such as shock-boundary layer interactions and choked flow that are not observed for subsonic tip flows that have been studied extensively in literature. This work simulates the tip clearance flow for a flat tip, a diverging tip gap and several contoured tips to assess the possibility of minimizing tip heat flux while maintaining a constant massflow from the pressure side to the suction side of the rotor, through the tip clearance. The CFD code GlennHT was used for the simulations. Due to the strong favorable pressure gradients the simulations assumed laminar conditions in the tip gap. The nominal tip gap width to height ratio for this study is 6.0. The Reynolds number of the flow is 2.4x10(5) based on nominal tip width and exit velocity. A wavy wall design was found to reduce heat flux by 5% but suffered from an additional 6% in aerodynamic loss coefficient. Conventional tip recesses are found to perform far worse than a flat tip due to severe shock heating. Overall, the baseline flat tip was the second best performer. A diverging converging tip gap with a hole was found to be the best choice. Average tip heat flux was reduced by 37% and aerodynamic losses were cut by 2.84%.
C1 [Shyam, Vikram] NASA Glenn Res Ctr, Cleveland, OH USA.
RP Shyam, V (reprint author), NASA Glenn Res Ctr, Cleveland, OH USA.
NR 13
TC 0
Z9 0
U1 0
U2 0
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-5467-9
PY 2012
BP 887
EP 895
PG 9
WC Engineering, Mechanical
SC Engineering
GA BFS60
UT WOS:000321160300075
ER
PT S
AU Bradley, AT
Fowler, J
Yavoich, B
Jennings, S
AF Bradley, Arthur T.
Fowler, Jennine
Yavoich, Brian
Jennings, Stephen
GP IEEE
TI Reducing Printed Circuit Board Emissions with Low-Noise Design Practices
SO 2012 ASIA-PACIFIC INTERNATIONAL SYMPOSIUM ON ELECTROMAGNETIC
COMPATIBILITY (APEMC)
SE Asia-Pacific International Symposium on Electromagnetic Compatibility
LA English
DT Proceedings Paper
CT Asia-Pacific International Symposium on Electromagnetic Compatibility
(APEMC)
CY MAY 21-24, 2012
CL Singapore, SINGAPORE
SP IEEE, EMC Soc
AB This paper presents the results of an experiment designed to determine the effectiveness of adopting several low-noise printed circuit board (PCB) design practices. Two boards were designed and fabricated, each consisting of identical mixed-signal circuitry. Several important differences were introduced between the board layouts: one board was constructed using recommended low-noise practices and the other constructed without such attention. The emissions from the two boards were then measured and compared, demonstrating an improvement in radiated emissions of up to 22 dB.
C1 [Bradley, Arthur T.; Fowler, Jennine; Yavoich, Brian; Jennings, Stephen] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Bradley, AT (reprint author), NASA, Langley Res Ctr, 5 North Dryden,MS488, Hampton, VA 23681 USA.
EM arthur.t.bradley@nasa.gov; jfowler12391@gmail.com; byavoich@gmail.com;
stephen.a.jennings@nasa.gov
NR 5
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 2162-7673
BN 978-1-4577-1558-7
J9 ASIA-PAC INT SYM ELE
PY 2012
BP 613
EP 616
PG 4
WC Engineering, Electrical & Electronic
SC Engineering
GA BFN56
UT WOS:000320645900148
ER
PT B
AU Bar-Cohen, Y
AF Bar-Cohen, Y.
GP ASME
TI ELECTROACTIVE POLYMER (EAP) AS ACTUATORS FOR BIOMIMETIC APPLICATIONS
SO PROCEEDINGS OF THE ASME INTERNATIONAL MECHANICAL ENGINEERING CONGRESS
AND EXPOSITION (IMECE 2010), VOL 9
LA English
DT Proceedings Paper
CT ASME International Mechanical Engineering Congress and Exposition
(IMECE)
CY NOV 12-18, 2010
CL Vancouver, CANADA
SP Amer Soc Mech Engineers
ID ARTIFICIAL MUSCLES; PIEZOELECTRICITY; ELASTOMERS; FLUORIDE
AB Many polymers are known to vary their shape or size when subjected to electric, chemical, pneumatic, optical, or magnetic field. Electrical excitation is one of the most attractive methods for causing elastic deformation. The convenience and practicality of electrical stimulation and the recent advances in electroactive polymers (EAP) make them the most preferred among the responsive polymers. An added benefit of some of the EAP materials is their having the reverse effect of converting mechanical strain to electrical signal making them useful for sensors and energy harvesting mechanisms. To bring these materials to use in daily use products will necessitate finding niche that addresses critical needs. One of the main applications that are being considered for biologically inspired capabilities, also known as biomimetics, which were previously imaginable only in science fiction concepts. Some of the applications that are considered include Refreshable Braille Display, Robotic Fish, Fish-like Blimp, Humanlike Robots and many others. In the paper, the latest development in EAP materials and their applications will be reviewed and discussed.
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Bar-Cohen, Y (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 67-119, Pasadena, CA 91109 USA.
EM yosi@jpl.nasa.gov
NR 30
TC 1
Z9 1
U1 1
U2 10
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-4446-5
PY 2012
BP 655
EP 660
PG 6
WC Engineering, Mechanical; Mechanics
SC Engineering; Mechanics
GA BFM23
UT WOS:000320481000078
ER
PT B
AU Lall, P
Gupta, P
Goebel, K
AF Lall, Pradeep
Gupta, Prashant
Goebel, Kai
GP ASME
TI KL TRANSFORM AND NEURAL-NET BASED FRAMEWORK FOR FAILURE MODES
CLASSIFICATION IN ELECTRONICS SUBJECTED TO MECHANICAL-SHOCK
SO PROCEEDINGS OF THE ASME PACIFIC RIM TECHNICAL CONFERENCE AND EXHIBITION
ON PACKAGING AND INTEGRATION OF ELECTRONIC AND PHOTONIC SYSTEMS, MEMS
AND NEMS 2011, VOL 1
LA English
DT Proceedings Paper
CT ASME Pacific Rim Technical Conference and Exhibition on Packaging and
Integration of Electronic and Photonic Systems, MEMS and NEMS
CY JUL 06-08, 2011
CL Portland, OR
SP ASME, Japan Soc Mech Engineers
ID TIME-FREQUENCY-DISTRIBUTIONS; FINE-PITCH BGAS; DROP-IMPACT; RELIABILITY;
PREDICTION; NETWORKS; CSPS
AB Electronic systems under extreme shock and vibration environments including shock and vibration may sustain several failure modes simultaneously. Previous experience of the authors indicates that the dominant failure modes experienced by packages in a drop and shock frame work are in the solder interconnects including cracks at the package and the board interface, pad cratering, copper trace fatigue, and bulk-failure in the solder joint. In this paper, a method has been presented for failure mode classification using a combination of Karhunen Loeve transform with parity-based stepwise supervised training of a perceptrons. Early classification of multiple failure modes in the pre-failure space using supervised neural networks in conjunction with Karhunen Loeve transform is new. Feature space has been formed by joint time frequency analysis. Since the cumulative damage may be accrued under repetitive loading with exposure to multiple shock events, the area array assemblies have been exposed to shock and feature vectors constructed to track damage initiation and progression. Error Back propagation learning algorithm has been used for stepwise parity of each particular failure mode. The classified failure modes and failure regions belonging to each particular failure modes in the feature space are also validated by simulation of the designed neural network used for parity of feature space. Statistical similarity and validation of different classified dominant failure modes is performed by multivariate analysis of variance and Hoteling's T-square. The results of different classified dominant failure modes are also correlated with the experimental cross sections of the failed test assemblies. The methodology adopted in this paper can perform real-time fault monitoring with identification of specific dominant failure mode and is scalable to system level reliability.
C1 [Lall, Pradeep; Gupta, Prashant] Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA.
[Lall, Pradeep; Gupta, Prashant] NSF Ctr Adv Vehicle & Extreme Environm Elect, Auburn, AL 36849 USA.
[Goebel, Kai] NASA Ames Res Ctr, Moffett Field, CA USA.
RP Lall, P (reprint author), Auburn Univ, Dept Mech Engn, Auburn, AL 36849 USA.
EM lall@auburn.edu
FU NASA-IVHM Program Grant from the National Aeronautics and Space
Administration [NNA08BA21C]
FX The research presented in this paper has been supported by NASA-IVHM
Program Grant NNA08BA21C from the National Aeronautics and Space
Administration.
NR 39
TC 0
Z9 0
U1 0
U2 1
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-4461-8
PY 2012
BP 563
EP +
PG 3
WC Engineering, Electrical & Electronic; Engineering, Mechanical
SC Engineering
GA BFJ69
UT WOS:000320140300068
ER
PT S
AU Kaeppler, SR
Kletzing, CA
Bounds, SR
Gjerloev, JW
Anderson, BJ
Korth, H
LaBelle, JW
Dombrowski, MP
Lessard, M
Pfaff, RF
Rowland, DE
Jones, S
Heinselman, CJ
AF Kaeppler, S. R.
Kletzing, C. A.
Bounds, S. R.
Gjerloev, J. W.
Anderson, B. J.
Korth, H.
LaBelle, J. W.
Dombrowski, M. P.
Lessard, M.
Pfaff, R. F.
Rowland, D. E.
Jones, S.
Heinselman, C. J.
BE Keiling, A
Donovan, E
Bagenal, F
Karlsson, T
TI Current Closure in the Auroral Ionosphere: Results From the Auroral
Current and Electrodynamics Structure Rocket Mission
SO AURORAL PHENOMENOLOGY AND MAGNETOSPHERIC PROCESSES: EARTH AND OTHER
PLANETS
SE Geophysical Monograph Book Series
LA English
DT Proceedings Paper
CT Chapman Conference on the Relationship Between Auroral Phenomenology and
Magnetospheric Processes
CY FEB 27-MAR 04, 2011
CL Fairbanks, AK
SP Natl Sci Fdn (NSF), Univ Calgary
ID ELECTRIC-FIELD; PARTICLE PRECIPITATION; BLACK AURORA; ARC; ENERGY
AB The Auroral Current and Electrodynamics Structure mission consisted of two sounding rockets launched nearly simultaneously from Poker Flat Research Range, Alaska, on 29 January 2009 into a dynamic multiple-arc aurora. The two well-instrumented payloads were flown along very similar magnetic field footprints, at different altitudes, with small temporal separation to measure electrodynamic and plasma parameters above and within the ionospheric current closure region. The higher-altitude payload (360 km apogee) acquired in situ measurements of electrodynamic and plasma parameters above the current closure region to determine the magnetospheric input signature. The low-altitude payload (130 km apogee) made conjugate observations within the current closure region. Results are presented comparing observations of the electric fields, magnetic fields, and the electron differential energy flux at magnetic foot points common to both payloads. In situ data is compared to ground-based all-sky imager data, which recorded the evolution of the auroral event as the payloads traversed through magnetically conjugate regions. Current measurements derived from the magnetometers on the high-altitude payload observed upward and downward field-aligned currents. The effect of collisions with the neutral atmosphere is investigated to determine if it is a significant mechanism to explain differences in the low-energy electron flux. A calculation of ionospheric conductivity is performed to explain attenuation in electric field observations between the two payloads. The electric fields and magnetic fields of the first auroral crossing are examined in detail and found to have results consistent with the model of an auroral arc.
C1 [Kaeppler, S. R.; Kletzing, C. A.; Bounds, S. R.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Gjerloev, J. W.] Univ Bergen, Dept Phys & Technol, Bergen, Norway.
[Anderson, B. J.; Korth, H.] Johns Hopkins Univ, Appl Phys Lab, Baltimore, MD USA.
[LaBelle, J. W.; Dombrowski, M. P.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH USA.
[Lessard, M.] Univ New Hampshire, Ctr Space Sci, Durham, NH USA.
[Pfaff, R. F.; Rowland, D. E.; Jones, S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
[Heinselman, C. J.] SRI Int, Ctr Geospace Studies, Menlo Pk, CA USA.
RP Kaeppler, SR (reprint author), Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
EM stephen-kaeppler@uiowa.edu
RI Rowland, Douglas/F-5589-2012; Jones, Sarah/D-5293-2012;
OI Rowland, Douglas/0000-0003-0948-6257; Jones, Sarah/0000-0002-3816-4954;
Kletzing, Craig/0000-0002-4136-3348
NR 23
TC 3
Z9 3
U1 0
U2 3
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0065-8448
BN 978-0-87590-487-0
J9 GEOPHYS MONOGR SER
PY 2012
VL 197
BP 183
EP +
DI 10.1029/2011GM001177
PG 2
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Physics,
Applied
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Physics
GA BFJ22
UT WOS:000320090100015
ER
PT S
AU Keiling, A
Shiokawa, K
Uritsky, V
Sergeev, V
Zesta, E
Kepko, L
Ostgaard, N
AF Keiling, A.
Shiokawa, K.
Uritsky, V.
Sergeev, V.
Zesta, E.
Kepko, L.
Ostgaard, N.
BE Keiling, A
Donovan, E
Bagenal, F
Karlsson, T
TI Auroral Signatures of the Dynamic Plasma Sheet
SO AURORAL PHENOMENOLOGY AND MAGNETOSPHERIC PROCESSES: EARTH AND OTHER
PLANETS
SE Geophysical Monograph Book Series
LA English
DT Proceedings Paper
CT Chapman Conference on the Relationship Between Auroral Phenomenology and
Magnetospheric Processes
CY FEB 27-MAR 04, 2011
CL Fairbanks, AK
SP Natl Sci Fdn (NSF), Univ Calgary
ID EARTHWARD FLOW BURSTS; POLEWARD BOUNDARY INTENSIFICATIONS; WESTWARD
TRAVELING SURGE; SUBSTORM BRIGHTENING ARC; THIN CURRENT SHEET;
BALLOONING INSTABILITY; CURRENT DISRUPTION; EXPANSION PHASE; BULK FLOWS;
ONSET
AB Understanding the physical connections of the coupled magnetosphere-ionosphere system will result in a more complete explanation of the aurora and will further the goal of being able to interpret the global auroral distributions as a dynamic map of the magnetosphere. Significant advances have been made in recent years toward this goal. In this chapter, we briefly review, while focusing on recent observations, selected auroral phenomena that are driven by magnetospheric processes. These include expansion of substorm aurora, plasma sheet waves and auroral modulations, ballooning instability and auroral beads, dipolarization/plasma injections and the auroral bulge, poleward boundary intensifications and auroral streamers, vortical flows and auroral spirals, and plasma flows prior to auroral onset. In addition, other auroral phenomena, such as auroral arcs, diffuse auroras, auroral asymmetry/conjugacy in the conjugate hemispheres, and auroral magneto spheric currents, are highlighted here but expanded in other chapters of this monograph for in-depth reviews.
C1 [Keiling, A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Shiokawa, K.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi, Japan.
[Uritsky, V.; Kepko, L.] Goddard Space Flight Ctr, Greenbelt, MD USA.
[Sergeev, V.] St Petersburg State Univ, Inst Phys, St Petersburg, Russia.
[Zesta, E.] Air Force Res Lab RVBXP, Kirtland AFB, NM USA.
[Ostgaard, N.] Univ Bergen, Dept Phys & Technol, Bergen, Norway.
RP Keiling, A (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
EM keiling@ssl.berkeley.edu
FU NASA [NNX08AF29G]; STEL visiting professor program at Nagoya University
FX We congratulate the entire THEMIS team (science and operation) for a
successful mission, which has given auroral researchers a powerful tool
for their daily work. Furthermore, Andreas Keiling thanks the members of
the science program committee for their help in organizing the Aurora
Chapman conference in Fairbanks, including writing the conference
proposal, parts of which have been used for this chapter. This work was
supported by the NASA grant NNX08AF29G and by the STEL visiting
professor program at Nagoya University.
NR 101
TC 7
Z9 7
U1 0
U2 8
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0065-8448
BN 978-0-87590-487-0
J9 GEOPHYS MONOGR SER
PY 2012
VL 197
BP 317
EP +
DI 10.1029/2012GM001231
PG 6
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Physics,
Applied
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Physics
GA BFJ22
UT WOS:000320090100028
ER
PT S
AU Birn, J
Schindler, K
Hesse, M
AF Birn, J.
Schindler, K.
Hesse, M.
BE Keiling, A
Donovan, E
Bagenal, F
Karlsson, T
TI Magnetotail Aurora Connection: The Role of Thin Current Sheets
SO AURORAL PHENOMENOLOGY AND MAGNETOSPHERIC PROCESSES: EARTH AND OTHER
PLANETS
SE Geophysical Monograph Book Series
LA English
DT Proceedings Paper
CT Chapman Conference on the Relationship Between Auroral Phenomenology and
Magnetospheric Processes
CY FEB 27-MAR 04, 2011
CL Fairbanks, AK
SP Natl Sci Fdn (NSF), Univ Calgary
ID INTENSE ELECTRIC-FIELDS; PLASMA SHEET; PARTICLE-ACCELERATION; MAGNETIC
RECONNECTION; CLUSTER; EQUILIBRIUM; CONVECTION; LOCATION; MODELS; REGION
AB Connections between magnetotail structure and dynamics and auroral forms are investigated on the basis of fluid and particle simulations, as well as Vlasov theory. Our focus is on possible mechanisms to generate or enhance perpendicular electric fields associated with quasistatic electric potentials of "U" shape or "S" shape, relevant for auroral arcs. At small scales (less than 10 km), such electric fields are associated with Hall currents and electron E x B drift rather than plasma flow shear, indicating the relevance of thin current sheets as possible source regions. Two-dimensional and 3-D MHD theory and simulations demonstrate that moderate deformations of the magnetotail may lead to critical states characterized by the loss of neighboring equilibrium and the formation of thin current sheets embedded in the wider plasma sheet. This provides a suitable scenario for the onset of reconnection in the tail, as well as a potential mechanism to generate or intensify auroral arcs, even prior to the onset of reconnection. Particle-in-cell simulations confirm this mechanism and further demonstrate that thin embedded electron current sheets may form from moderate compression, as well as expansion, of a thicker current sheet. This suggests that such structures might be more typical for the tail current sheet than a smooth solution and may represent a possible source region for quiescent arcs within the plasma sheet footpoint region and at the plasma sheet/polar cap boundary. One-dimensional Vlasov models of such structures indicate association with either S- or U-shaped potentials (and intermediate structures), depending on the magnitude of the magnetic field jump and the plasma beta.
C1 [Birn, J.] Space Sci Inst, Boulder, CO 80301 USA.
[Birn, J.] Los Alamos Natl Lab, Los Alamos, NM USA.
[Schindler, K.] Ruhr Univ Bochum, Inst Theoret Phys, Bochum, Germany.
[Hesse, M.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Birn, J (reprint author), Space Sci Inst, Boulder, CO 80301 USA.
EM jbirn@spacescience.org
RI NASA MMS, Science Team/J-5393-2013
OI NASA MMS, Science Team/0000-0002-9504-5214
FU US Depanment of Energy; NASA's MMS/SMART Theory; Modeling and SRT
Programs
FX This work was performed under the auspices of the US Depanment of
Energy, supported by NASA's MMS/SMART Theory and Modeling and SR&T
Programs.
NR 44
TC 3
Z9 3
U1 1
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0065-8448
BN 978-0-87590-487-0
J9 GEOPHYS MONOGR SER
PY 2012
VL 197
BP 337
EP +
DI 10.1029/2011GM001182
PG 3
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Physics,
Applied
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Physics
GA BFJ22
UT WOS:000320090100029
ER
PT B
AU Schiller, NH
Cabell, RH
Quinones, JD
Wier, NC
AF Schiller, Noah H.
Cabell, Randolph H.
Quinones, Juan D.
Wier, Nathan C.
GP ASME
TI ACTIVE DAMPING USING DISTRIBUTED ANISOTROPIC ACTUATORS
SO PROCEEDINGS OF THE ASME INTERNATIONAL MECHANICAL ENGINEERING CONGRESS
AND EXPOSITION 2010, VOL 13
LA English
DT Proceedings Paper
CT ASME International Mechanical Engineering Congress and Exposition
(IMECE)
CY NOV 12-18, 2010
CL Vancouver, CANADA
SP Amer Soc Mech Engineers
AB A helicopter structure experiences substantial high-frequency mechanical excitation from powertrain components such as gearboxes and drive shafts. The resulting structure-borne vibration excites the windows which then radiate sound into the passenger cabin. In many cases the radiated sound power can be reduced by adding damping. This can be accomplished using passive or active approaches. Passive treatments such as constrained layer damping tend to reduce window transparency. Therefore this paper focuses on an active approach utilizing compact decentralized control units distributed around the perimeter of the window Each control unit consists of a triangularly shaped piezoelectric actuator, a miniature accelerometer, and analog electronics. Earlier work has shown that this type of system can increase damping up to approximately 1 kHz. However at higher frequencies the mismatch between the distributed actuator and the point sensor caused control spillover.
This paper describes new anisotropic actuators that can be used to improve the bandwidth of the control system. The anisotropic actuators are composed of piezoelectric material sandwiched between interdigitated electrodes, which enables the application of the electric field in a preferred in-plane direction. When shaped correctly the anisotropic actuators outperform traditional isotropic actuators by reducing the mismatch between the distributed actuator and point sensor at high frequencies. Testing performed on a Plexiglas panel, representative of a helicopter window, shows that the control units can increase damping at low frequencies. However high frequency performance was still limited due to the flexible boundary conditions present on the test structure.
C1 [Schiller, Noah H.; Cabell, Randolph H.] NASA, Langley Res Ctr, Hampton, VA 23665 USA.
[Quinones, Juan D.] Univ Puerto Rico, Mayaguez, PR 00708 USA.
[Wier, Nathan C.] Michigan Technol Univ, Houghton, MI 49931 USA.
RP Schiller, NH (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA.
NR 9
TC 0
Z9 0
U1 0
U2 0
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-4450-2
PY 2012
BP 73
EP +
PG 3
WC Engineering, Mechanical
SC Engineering
GA BFJ73
UT WOS:000320140700010
ER
PT B
AU DellaCorte, C
Stanford, MK
Manco, RA
Thomas, F
AF DellaCorte, Christopher
Stanford, Malcolm K.
Manco, Richard A., II
Thomas, Fransua
GP ASME
TI DESIGN CONSIDERATIONS FOR RESILIENT ROLLING ELEMENT BEARINGS MADE FROM
LOW MODULUS SUPERELASTIC MATERIALS
SO PROCEEDINGS OF THE ASME/STLE INTERNATIONAL JOINT TRIBOLOGY CONFERENCE -
2011
LA English
DT Proceedings Paper
CT ASME/STLE International Joint Tribology Conference
CY OCT 24-26, 2011
CL Los Angeles, CA
SP ASME, Tribol Div, Soc Tribologists & Lubricat Engineers
AB Nickel-titanium based superelastic materials are emerging as candidates for rolling element-bearing applications [1]. When properly prepared, these unique intermetallics are hard, exhibit excellent tribological properties and are intrinsically corrosion immune [2]. In addition, recent investigations have revealed that, unlike traditional bearing steels, superelastics can endure much higher levels of recoverable elastic strain during compressive deformation [3]. This behavior enables bearings that are more resilient to load induced damage such as raceway denting and from the ingestion of hard particles. Despite these positive attributes, these alloys differ significantly from conventional steels and these differences must be carefully considered to achieve successful applications. These differences include reduced elastic modulus, high hardness and enhanced resistance to indentation loads. The current paper introduces nickel-titanium based superelastic bearing materials and compares their properties to current bearing materials. General bearing design practices and manufacturing processes are also examined to identify and explore the challenges and opportunities for making resilient rolling element bearings utilizing this new class of superelastic materials.
C1 [DellaCorte, Christopher; Stanford, Malcolm K.; Thomas, Fransua] NASA, Glenn Res Ctr, Cleveland, OH USA.
RP DellaCorte, C (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA.
NR 5
TC 0
Z9 0
U1 0
U2 0
PU AMER SOC MECHANICAL ENGINEERS
PI NEW YORK
PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA
BN 978-0-7918-5474-7
PY 2012
BP 223
EP 224
PG 2
WC Engineering, Mechanical
SC Engineering
GA BFI64
UT WOS:000320008100055
ER
PT J
AU Bolonkin, A
AF Bolonkin, Alexander
BA Bolonkin, A
BF Bolonkin, A
TI Macro World
SO UNIVERSE, HUMAN IMMORTALITY AND FUTURE HUMAN EVALUATION
SE Elsevier Insights
LA English
DT Article; Book Chapter
C1 [Bolonkin, Alexander] NASA, Washington, DC 20546 USA.
RP Bolonkin, A (reprint author), NASA, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
BN 978-0-12-415810-8
J9 ELSEV INSIGHT
PY 2012
BP 3
EP 20
DI 10.1016/B978-0-12-415801-6.00001-3
PG 18
WC Computer Science, Artificial Intelligence; Engineering,
Multidisciplinary
SC Computer Science; Engineering
GA BFK57
UT WOS:000320247100002
ER
PT J
AU Bolonkin, A
AF Bolonkin, Alexander
BA Bolonkin, A
BF Bolonkin, A
TI Universe, Human Immortality and Future Human Evaluation Preface
SO UNIVERSE, HUMAN IMMORTALITY AND FUTURE HUMAN EVALUATION
SE Elsevier Insights
LA English
DT Editorial Material; Book Chapter
C1 [Bolonkin, Alexander] NASA, Washington, DC 20546 USA.
RP Bolonkin, A (reprint author), NASA, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 1
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
BN 978-0-12-415810-8
J9 ELSEV INSIGHT
PY 2012
BP IX
EP +
PG 3
WC Computer Science, Artificial Intelligence; Engineering,
Multidisciplinary
SC Computer Science; Engineering
GA BFK57
UT WOS:000320247100001
ER
PT J
AU Bolonkin, A
AF Bolonkin, Alexander
BA Bolonkin, A
BF Bolonkin, A
TI Micro World
SO UNIVERSE, HUMAN IMMORTALITY AND FUTURE HUMAN EVALUATION
SE Elsevier Insights
LA English
DT Article; Book Chapter
C1 [Bolonkin, Alexander] NASA, Washington, DC 20546 USA.
RP Bolonkin, A (reprint author), NASA, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
BN 978-0-12-415810-8
J9 ELSEV INSIGHT
PY 2012
BP 21
EP 27
DI 10.1016/B978-0-12-415801-6.00002-5
PG 7
WC Computer Science, Artificial Intelligence; Engineering,
Multidisciplinary
SC Computer Science; Engineering
GA BFK57
UT WOS:000320247100003
ER
PT J
AU Bolonkin, A
AF Bolonkin, Alexander
BA Bolonkin, A
BF Bolonkin, A
TI Surprising Properties of Our Universe
SO UNIVERSE, HUMAN IMMORTALITY AND FUTURE HUMAN EVALUATION
SE Elsevier Insights
LA English
DT Article; Book Chapter
C1 [Bolonkin, Alexander] NASA, Washington, DC 20546 USA.
RP Bolonkin, A (reprint author), NASA, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
BN 978-0-12-415810-8
J9 ELSEV INSIGHT
PY 2012
BP 29
EP 34
DI 10.1016/B978-0-12-415801-6.00003-7
PG 6
WC Computer Science, Artificial Intelligence; Engineering,
Multidisciplinary
SC Computer Science; Engineering
GA BFK57
UT WOS:000320247100004
ER
PT J
AU Bolonkin, A
AF Bolonkin, Alexander
BA Bolonkin, A
BF Bolonkin, A
TI What Is God?
SO UNIVERSE, HUMAN IMMORTALITY AND FUTURE HUMAN EVALUATION
SE Elsevier Insights
LA English
DT Article; Book Chapter
C1 [Bolonkin, Alexander] NASA, Washington, DC 20546 USA.
RP Bolonkin, A (reprint author), NASA, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
BN 978-0-12-415810-8
J9 ELSEV INSIGHT
PY 2012
BP 35
EP 37
DI 10.1016/B978-0-12-415801-6.00004-9
PG 3
WC Computer Science, Artificial Intelligence; Engineering,
Multidisciplinary
SC Computer Science; Engineering
GA BFK57
UT WOS:000320247100005
ER
PT J
AU Bolonkin, A
AF Bolonkin, Alexander
BA Bolonkin, A
BF Bolonkin, A
TI What Is the Human Soul?
SO UNIVERSE, HUMAN IMMORTALITY AND FUTURE HUMAN EVALUATION
SE Elsevier Insights
LA English
DT Article; Book Chapter
C1 [Bolonkin, Alexander] NASA, Washington, DC 20546 USA.
RP Bolonkin, A (reprint author), NASA, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
BN 978-0-12-415810-8
J9 ELSEV INSIGHT
PY 2012
BP 39
EP 41
DI 10.1016/B978-0-12-415801-6.00005-0
PG 3
WC Computer Science, Artificial Intelligence; Engineering,
Multidisciplinary
SC Computer Science; Engineering
GA BFK57
UT WOS:000320247100006
ER
PT J
AU Bolonkin, A
AF Bolonkin, Alexander
BA Bolonkin, A
BF Bolonkin, A
TI What Is "I"? What Are "We"?
SO UNIVERSE, HUMAN IMMORTALITY AND FUTURE HUMAN EVALUATION
SE Elsevier Insights
LA English
DT Article; Book Chapter
C1 [Bolonkin, Alexander] NASA, Washington, DC 20546 USA.
RP Bolonkin, A (reprint author), NASA, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
BN 978-0-12-415810-8
J9 ELSEV INSIGHT
PY 2012
BP 43
EP 51
DI 10.1016/B978-0-12-415801-6.00006-2
PG 9
WC Computer Science, Artificial Intelligence; Engineering,
Multidisciplinary
SC Computer Science; Engineering
GA BFK57
UT WOS:000320247100007
ER
PT J
AU Bolonkin, A
AF Bolonkin, Alexander
BA Bolonkin, A
BF Bolonkin, A
TI Human Emotions, Happiness, and Pleasure
SO UNIVERSE, HUMAN IMMORTALITY AND FUTURE HUMAN EVALUATION
SE Elsevier Insights
LA English
DT Article; Book Chapter
C1 [Bolonkin, Alexander] NASA, Washington, DC 20546 USA.
RP Bolonkin, A (reprint author), NASA, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
BN 978-0-12-415810-8
J9 ELSEV INSIGHT
PY 2012
BP 53
EP 57
DI 10.1016/B978-0-12-415801-6.00007-4
PG 5
WC Computer Science, Artificial Intelligence; Engineering,
Multidisciplinary
SC Computer Science; Engineering
GA BFK57
UT WOS:000320247100008
ER
PT J
AU Bolonkin, A
AF Bolonkin, Alexander
BA Bolonkin, A
BF Bolonkin, A
TI The Advent of the Non-Biological Civilization
SO UNIVERSE, HUMAN IMMORTALITY AND FUTURE HUMAN EVALUATION
SE Elsevier Insights
LA English
DT Article; Book Chapter
C1 [Bolonkin, Alexander] NASA, Washington, DC 20546 USA.
RP Bolonkin, A (reprint author), NASA, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
BN 978-0-12-415810-8
J9 ELSEV INSIGHT
PY 2012
BP 61
EP 71
DI 10.1016/B978-0-12-415801-6.00008-6
PG 11
WC Computer Science, Artificial Intelligence; Engineering,
Multidisciplinary
SC Computer Science; Engineering
GA BFK57
UT WOS:000320247100009
ER
PT J
AU Bolonkin, A
AF Bolonkin, Alexander
BA Bolonkin, A
BF Bolonkin, A
TI The Beginning of Human Immortality
SO UNIVERSE, HUMAN IMMORTALITY AND FUTURE HUMAN EVALUATION
SE Elsevier Insights
LA English
DT Article; Book Chapter
C1 [Bolonkin, Alexander] NASA, Washington, DC 20546 USA.
RP Bolonkin, A (reprint author), NASA, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
BN 978-0-12-415810-8
J9 ELSEV INSIGHT
PY 2012
BP 73
EP 80
DI 10.1016/B978-0-12-415801-6.00009-8
PG 8
WC Computer Science, Artificial Intelligence; Engineering,
Multidisciplinary
SC Computer Science; Engineering
GA BFK57
UT WOS:000320247100010
ER
PT J
AU Bolonkin, A
AF Bolonkin, Alexander
BA Bolonkin, A
BF Bolonkin, A
TI What are Science, Soul, Paradise, and Artificial Intelligence?
SO UNIVERSE, HUMAN IMMORTALITY AND FUTURE HUMAN EVALUATION
SE Elsevier Insights
LA English
DT Article; Book Chapter
C1 [Bolonkin, Alexander] NASA, Washington, DC 20546 USA.
RP Bolonkin, A (reprint author), NASA, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
BN 978-0-12-415810-8
J9 ELSEV INSIGHT
PY 2012
BP 81
EP 90
DI 10.1016/B978-0-12-415801-6.00010-4
PG 10
WC Computer Science, Artificial Intelligence; Engineering,
Multidisciplinary
SC Computer Science; Engineering
GA BFK57
UT WOS:000320247100011
ER
PT J
AU Bolonkin, A
AF Bolonkin, Alexander
BA Bolonkin, A
BF Bolonkin, A
TI Real Breakthrough to Immortality
SO UNIVERSE, HUMAN IMMORTALITY AND FUTURE HUMAN EVALUATION
SE Elsevier Insights
LA English
DT Article; Book Chapter
C1 [Bolonkin, Alexander] NASA, Washington, DC 20546 USA.
RP Bolonkin, A (reprint author), NASA, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
BN 978-0-12-415810-8
J9 ELSEV INSIGHT
PY 2012
BP 91
EP 101
DI 10.1016/B978-0-12-415801-6.00011-6
PG 11
WC Computer Science, Artificial Intelligence; Engineering,
Multidisciplinary
SC Computer Science; Engineering
GA BFK57
UT WOS:000320247100012
ER
PT J
AU Bolonkin, A
AF Bolonkin, Alexander
BA Bolonkin, A
BF Bolonkin, A
TI The Natural Purpose of Humankind Is to Become God
SO UNIVERSE, HUMAN IMMORTALITY AND FUTURE HUMAN EVALUATION
SE Elsevier Insights
LA English
DT Article; Book Chapter
C1 [Bolonkin, Alexander] NASA, Washington, DC 20546 USA.
RP Bolonkin, A (reprint author), NASA, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
BN 978-0-12-415810-8
J9 ELSEV INSIGHT
PY 2012
BP 103
EP 114
DI 10.1016/B978-0-12-415801-6.00012-8
PG 12
WC Computer Science, Artificial Intelligence; Engineering,
Multidisciplinary
SC Computer Science; Engineering
GA BFK57
UT WOS:000320247100013
ER
PT J
AU Bolonkin, A
AF Bolonkin, Alexander
BA Bolonkin, A
BF Bolonkin, A
TI Setting God in a Computer-Internet Net
SO UNIVERSE, HUMAN IMMORTALITY AND FUTURE HUMAN EVALUATION
SE Elsevier Insights
LA English
DT Article; Book Chapter
C1 [Bolonkin, Alexander] NASA, Washington, DC 20546 USA.
RP Bolonkin, A (reprint author), NASA, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
BN 978-0-12-415810-8
J9 ELSEV INSIGHT
PY 2012
BP 115
EP 122
DI 10.1016/B978-0-12-415801-6.00013-X
PG 8
WC Computer Science, Artificial Intelligence; Engineering,
Multidisciplinary
SC Computer Science; Engineering
GA BFK57
UT WOS:000320247100014
ER
PT J
AU Bolonkin, A
AF Bolonkin, Alexander
BA Bolonkin, A
BF Bolonkin, A
TI Immortality Becomes a Reality
SO UNIVERSE, HUMAN IMMORTALITY AND FUTURE HUMAN EVALUATION
SE Elsevier Insights
LA English
DT Article; Book Chapter
C1 [Bolonkin, Alexander] NASA, Washington, DC 20546 USA.
RP Bolonkin, A (reprint author), NASA, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
BN 978-0-12-415810-8
J9 ELSEV INSIGHT
PY 2012
BP 123
EP 125
DI 10.1016/B978-0-12-415801-6.00014-1
PG 3
WC Computer Science, Artificial Intelligence; Engineering,
Multidisciplinary
SC Computer Science; Engineering
GA BFK57
UT WOS:000320247100015
ER
PT J
AU Bolonkin, A
AF Bolonkin, Alexander
BA Bolonkin, A
BF Bolonkin, A
TI Personhood: Three Prerequisites or Laws of E-beings
SO UNIVERSE, HUMAN IMMORTALITY AND FUTURE HUMAN EVALUATION
SE Elsevier Insights
LA English
DT Article; Book Chapter
C1 [Bolonkin, Alexander] NASA, Washington, DC 20546 USA.
RP Bolonkin, A (reprint author), NASA, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
BN 978-0-12-415810-8
J9 ELSEV INSIGHT
PY 2012
BP 127
EP 130
DI 10.1016/B978-0-12-415801-6.00015-3
PG 4
WC Computer Science, Artificial Intelligence; Engineering,
Multidisciplinary
SC Computer Science; Engineering
GA BFK57
UT WOS:000320247100016
ER
PT J
AU Bolonkin, A
AF Bolonkin, Alexander
BA Bolonkin, A
BF Bolonkin, A
TI General Summary for Chapters 8-15
SO UNIVERSE, HUMAN IMMORTALITY AND FUTURE HUMAN EVALUATION
SE Elsevier Insights
LA English
DT Article; Book Chapter
C1 [Bolonkin, Alexander] NASA, Washington, DC 20546 USA.
RP Bolonkin, A (reprint author), NASA, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
BN 978-0-12-415810-8
J9 ELSEV INSIGHT
PY 2012
BP 131
EP 136
DI 10.1016/B978-0-12-415801-6.00016-5
PG 6
WC Computer Science, Artificial Intelligence; Engineering,
Multidisciplinary
SC Computer Science; Engineering
GA BFK57
UT WOS:000320247100017
ER
PT J
AU Bolonkin, A
AF Bolonkin, Alexander
BA Bolonkin, A
BF Bolonkin, A
TI An Open Statement to the President of the United States of America and
to the Presidents and Prime Ministers of All Countries About a
Scientific and Technology Jump in the Twenty-First Century
SO UNIVERSE, HUMAN IMMORTALITY AND FUTURE HUMAN EVALUATION
SE Elsevier Insights
LA English
DT Article; Book Chapter
C1 [Bolonkin, Alexander] NASA, Washington, DC 20546 USA.
RP Bolonkin, A (reprint author), NASA, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
BN 978-0-12-415810-8
J9 ELSEV INSIGHT
PY 2012
BP 137
EP 139
PG 3
WC Computer Science, Artificial Intelligence; Engineering,
Multidisciplinary
SC Computer Science; Engineering
GA BFK57
UT WOS:000320247100018
ER
PT J
AU Bolonkin, A
AF Bolonkin, Alexander
BA Bolonkin, A
BF Bolonkin, A
TI Current Artificial Intelligence
SO UNIVERSE, HUMAN IMMORTALITY AND FUTURE HUMAN EVALUATION
SE Elsevier Insights
LA English
DT Article; Book Chapter
C1 [Bolonkin, Alexander] NASA, Washington, DC 20546 USA.
RP Bolonkin, A (reprint author), NASA, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
BN 978-0-12-415810-8
J9 ELSEV INSIGHT
PY 2012
BP 141
EP 149
PG 9
WC Computer Science, Artificial Intelligence; Engineering,
Multidisciplinary
SC Computer Science; Engineering
GA BFK57
UT WOS:000320247100019
ER
PT J
AU Bolonkin, A
AF Bolonkin, Alexander
BA Bolonkin, A
BF Bolonkin, A
TI Current Supercomputers
SO UNIVERSE, HUMAN IMMORTALITY AND FUTURE HUMAN EVALUATION
SE Elsevier Insights
LA English
DT Article; Book Chapter
C1 [Bolonkin, Alexander] NASA, Washington, DC 20546 USA.
RP Bolonkin, A (reprint author), NASA, Washington, DC 20546 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
BN 978-0-12-415810-8
J9 ELSEV INSIGHT
PY 2012
BP 151
EP 154
PG 4
WC Computer Science, Artificial Intelligence; Engineering,
Multidisciplinary
SC Computer Science; Engineering
GA BFK57
UT WOS:000320247100020
ER
PT S
AU Dennison, JR
Evans, A
Wilson, G
Dekany, J
Bowers, CW
Meloy, R
AF Dennison, J. R.
Evans, Amberly
Wilson, Gregory
Dekany, Justin
Bowers, Charles W.
Meloy, Robert
GP IEEE
TI Electron Beam Induced Luminescence of SiO2 Optical Coatings
SO 2012 ANNUAL REPORT CONFERENCE ON ELECTRICAL INSULATION AND DIELECTRIC
PHENOMENA (CEIDP)
SE Conference on Electrical Insulation and Dielectric Phenomena Annual
Report
LA English
DT Proceedings Paper
CT IEEE Conference on Electrical Insulation and Dielectric Phenomena
(CEIDP)
CY OCT 14-17, 2012
CL Montreal, CANADA
SP IEEE
ID SILICA
AB Optical coatings of disordered thin film SiO2/SiOx dielectric samples on reflective metal substrates exhibited cathodoluminescence under electron beam irradiation. Measurements of the absolute radiance and emission spectra as functions of incident electron energy, flux and power over a range of sample temperatures are reported. Radiance reached a saturation plateau at high incident electron power. Well below saturation radiance scaled with deposited power, that is linearly with incident power for lower-energy non-penetrating electrons and decreasing with increasing energy for penetrating radiation. Four bands were observed in spectral measurements from 300 nm to 1000 nm. Changes in peak intensity and shifts in peak energies as functions of temperature are described. The observations are explained in terms of a simple disordered band theory model and the transitions that take place between electrons in extended conduction states and localized trapped states associated with structural or compositional defects in the highly disordered insulating materials; this provides a fundamental basis for understanding the dependence of cathodoluminescence on irradiation time, incident flux and energy, and sample thickness and temperature.
C1 [Dennison, J. R.; Evans, Amberly; Wilson, Gregory; Dekany, Justin] Utah State Univ, Mat Phys Grp, 4415 Old Main Hill, Logan, UT 84322 USA.
[Bowers, Charles W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Meloy, Robert] MEI Technol Inc, NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
RP Dennison, JR (reprint author), Utah State Univ, Mat Phys Grp, 4415 Old Main Hill, Logan, UT 84322 USA.
OI Dennison, JR/0000-0002-5504-3353
NR 12
TC 4
Z9 4
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 0084-9162
BN 978-1-4673-1252-3
J9 C ELECT INSUL DIEL P
PY 2012
BP 479
EP 482
PG 4
WC Engineering, Electrical & Electronic
SC Engineering
GA BEJ40
UT WOS:000316899800113
ER
PT S
AU Denison, DR
Kotrba, LM
Castano, N
AF Denison, Daniel R.
Kotrba, Lindsey M.
Castano, Nathalie
BE Moblely, WH
Wang, Y
Li, M
TI A CROSS-CULTURAL PERSPECTIVE ON LEADERSHIP ASSESSMENT: COMPARING
360-DEGREE FEEDBACK RESULTS FROM AROUND THE WORLD
SO ADVANCES IN GLOBAL LEADERSHIP, VOL 7
SE Advances in Global Leadership
LA English
DT Article; Book Chapter
ID PSYCHOMETRIC PROPERTIES; ORGANIZATIONAL CULTURE; SUBORDINATE; RATINGS;
METAANALYSIS; PERFORMANCE; INSTRUMENTS; INVENTORY; VALIDITY; PEER
AB How generalizable are 360-degree feedback instruments in different cultures? Research investigating the validity and utility of these instruments across the globe is scarce, yet, extraordinarily important. This chapter investigates the utility of a 360-degree feedback instrument across the globe, as well as how different raters from various cultures perceive leaders.
C1 [Denison, Daniel R.] IMD, Lausanne, Switzerland.
[Kotrba, Lindsey M.] Denison Consulting, Res & Dev, Ann Arbor, MI USA.
[Castano, Nathalie] Wayne State Univ, NASA, Kennedy Space Ctr, Brevard, FL USA.
RP Denison, DR (reprint author), IMD, Lausanne, Switzerland.
NR 44
TC 5
Z9 5
U1 1
U2 5
PU EMERALD GROUP PUBLISHING LTD
PI BINGLEY
PA HOWARD HOUSE, WAGON LANE, BINGLEY, W YORKSHIRE BD16 1WA, ENGLAND
SN 1535-1203
BN 978-1-78052-002-5
J9 ADV GLOB LEADERSHIP
PY 2012
VL 7
BP 205
EP 228
DI 10.1108/S1535-1203(2012)0000007013
PG 24
WC Business; Management
SC Business & Economics
GA BFE62
UT WOS:000319502400011
ER
PT B
AU Hill, S
AF Hill, Steele
BE Bolt, M
Case, S
TI The Sun as Art
SO ENGAGING THE HEAVENS: INSPIRATION OF ASTRONOMICAL PHENOMENA V
SE Astronomical Society of the Pacific Conference Series
LA English
DT Proceedings Paper
CT Conference on Engaging the Heavens: Inspiration of Astronomical
Phenomena
CY JUN 26-JUL 01, 2005
CL Adler Planetarium, Chicago, IL
HO Adler Planetarium
AB This exhibit presents a new way of looking at the Sun. Its goal is to feature the variety and beauty that can be derived from very little or sometimes no manipulation of SOHO (Solar and Heliospheric Observatory) images. Somewhere near the meeting point of art and science, the show reveals the best of SOHO in inventive and engaging displays.
C1 [Hill, Steele] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU ASTRONOMICAL SOC PACIFIC
PI SAN FRANCISCO
PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA
BN 978-1-58381-818-3
J9 ASTR SOC P
PY 2012
VL 468
BP 27
EP 30
PG 4
WC Art; Astronomy & Astrophysics; Literature
SC Art; Astronomy & Astrophysics; Literature
GA BFJ28
UT WOS:000320096200005
ER
PT B
AU Bailey, S
Raffaelle, R
AF Bailey, Sheila
Raffaelle, Ryne
BE McEvoy, A
Markvart, T
Castaner, L
TI Operation of Solar Cells in a Space Environment
SO PRACTICAL HANDBOOK OF PHOTOVOLTAICS: FUNDAMENTALS AND APPLICATIONS, 2ND
EDITION
LA English
DT Article; Book Chapter
C1 [Bailey, Sheila] NASA Glenn Res Ctr, Photovolta & Space Environm Branch, Cleveland, OH 44135 USA.
[Raffaelle, Ryne] Natl Ctr Photovolta, NREL, Golden, CO 80401 USA.
RP Bailey, S (reprint author), NASA Glenn Res Ctr, Photovolta & Space Environm Branch, Cleveland, OH 44135 USA.
EM Sheila.Bailey@grc.nasa.gov; ryne_raffaelle@nrel.gov
NR 26
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA SARA BURGERHARTSTRAAT 25, PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
BN 978-0-12-385935-8
PY 2012
BP 863
EP 880
PG 18
WC Energy & Fuels; Engineering, Electrical & Electronic
SC Energy & Fuels; Engineering
GA BFD40
UT WOS:000319259600030
ER
PT B
AU Mehdi, I
Chattopadhyay, G
Lee, C
Reck, T
Jung, C
Siles, J
Cooper, K
Llombart, N
AF Mehdi, Imran
Chattopadhyay, Goutam
Lee, Choonsup
Reck, Theodore
Jung, Cecile
Siles, Jose
Cooper, Ken
Llombart, Nuria
GP IEEE
TI Wafer-Level Technology for Sub-mm Wave Focal Plane Arrays
SO 2012 7TH EUROPEAN MICROWAVE INTEGRATED CIRCUITS CONFERENCE (EUMIC)
SE European Microwave Integrated Circuits Conference - Proceedings
LA English
DT Proceedings Paper
CT 15th European Microwave Week - Space for Microwaves Conference
Proceedings
CY OCT 28-NOV 02, 2012
CL Amsterdam, NETHERLANDS
DE Focal plane arrays; submillimeter imaging arrays; Schottky diodes;
receiver front ends
AB A robust and compact scheme for building Submm-wave array receivers will be presented in this paper. By utilizing wafer-level integration the scheme enables compact multi-pixel modules. Bulk Silicon Deep Reactive Ion Etching techniques are used to build waveguides that allow the RF signals to be routed in the third dimension. Finally, a novel micro-lens antenna has been designed; fabricated and characterized that allows the antenna array to be fabricated via standard photolithography thus making it possible to build a beam-forming array. Preliminary work has focused on demonstrating a single pixel 500-600 GHz receiver front end and the characterization of the micro-lens.
C1 [Mehdi, Imran; Chattopadhyay, Goutam; Lee, Choonsup; Reck, Theodore; Jung, Cecile; Siles, Jose; Cooper, Ken] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
[Llombart, Nuria] Univ Complutense Madrid, Madrid, Spain.
RP Mehdi, I (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
NR 10
TC 0
Z9 0
U1 0
U2 1
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-2-87487-028-6; 978-1-4673-2302-4
J9 EUR MICROW INTEGRAT
PY 2012
BP 230
EP 233
PG 4
WC Engineering, Electrical & Electronic
SC Engineering
GA BEY23
UT WOS:000318630900059
ER
PT B
AU Burrage, D
Wesson, J
Wang, D
Garrison, J
Quindara, N
Ganoe, G
Katzberg, S
AF Burrage, Derek
Wesson, Joel
Wang, David
Garrison, James
Quindara, Nicole
Ganoe, George
Katzberg, Stephen
GP IEEE
TI Airborne Observation of Ocean Surface Roughness Variations Using a
Combination of Microwave Radiometer and Reflectometer Systems The Second
Virginia Offshore (Virgo II) Experiment
SO 2012 WORKSHOP ON REFLECTOMETRY USING GNSS AND OTHER SIGNALS OF
OPPORTUNITY (GNSS+R)
LA English
DT Proceedings Paper
CT Workshop on Reflectometry Using GNSS and Other Signals of Opportunity
(GNSS+R)
CY OCT 10-11, 2012
CL Purdue Univ, West Lafayette, IN
SP Natl Aeronaut & Space Adm (NASA), Inst Elect & Elect Engineers-Geoscience & Remote Sensing Soc (IEEE-GRSS), Int Assoc Geodesy (IAG) Sub-Commiss 4.6
HO Purdue Univ
DE sea surface salinity; sea surface roughness; microwave radiometry and
reflectometry; brightness temperatures; bi-static radar; delay Doppler
map
ID SALINITY; WATER; MODEL
AB Airborne and satellite retrieval of Sea Surface Salinity (SSS) using L-band microwave radiometers requires accurate corrections for the influence of wind-induced Sea Surface Roughness (SSR) on the retrievals. We describe an airborne experiment, Virgo II, that combined an L-band microwave radiometer for retrieving SSS, with L- and S-band reflectometer systems for retrieving SSR descriptors including Mean Square Slope (MSS) and Wind Speed (WS) under a range of surface wind and wave conditions. The research objective is to use the SSR descriptors derived from the reflectometers to correct the brightness temperatures observed by the L-band radiometer, and produce more accurate SSS retrievals. Here we describe our experimental investigations to assess the feasibility of this approach. Preliminary comparisons of WS data retrieved from the reflectometers with coincident WS data from in situ platforms and an atmospheric circulation model indicate that after correcting for apparent biases, the reflectometry-derived SSR descriptors could, indeed, provide reliable corrections for the L- band radiometer salinity retrieval.
C1 [Burrage, Derek; Wesson, Joel; Wang, David] USN, Res Lab, Div Oceanog, Stennis Space Ctr, MS 39529 USA.
[Garrison, James; Quindara, Nicole] Purdue Univ, Radio Nav Lab, W Lafayette, IN USA.
[Ganoe, George; Katzberg, Stephen] NASA, Langley Res Ctr, Hampton, VA USA.
RP Burrage, D (reprint author), USN, Res Lab, Div Oceanog, Stennis Space Ctr, MS 39529 USA.
EM derek.burrage@nrlssc.navy.mil; jgarriso@ecn.purdue.edu;
Stephen.j.katzberg@nasa.gov
FU Rick Aviation Inc. (Newport News, VA)
FX The expert support of Rick Aviation Inc. (Newport News, VA) for aircraft
operations is gratefully acknowledged. Philip Chu of NRL provided COAMPS
data.
NR 14
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
BN 978-1-4673-2883-8; 978-1-4673-2884-5
PY 2012
PG 6
WC Engineering, Electrical & Electronic
SC Engineering
GA BEZ72
UT WOS:000318915700008
ER
PT J
AU Siegel, PH
Alberti, S
Williams, DF
Shaw, S
Beigang, R
Davies, AG
East, J
Gallerano, GP
Grossman, EN
Jepsen, PU
Kawase, K
Koch, M
Llombart, N
Mehdi, I
Park, GS
Walker, C
AF Siegel, Peter H.
Alberti, Stefano
Williams, Dylan F.
Shaw, Sharri
Beigang, Rene
Davies, A. Giles
East, Jack
Gallerano, Gian Piero
Grossman, Erich N.
Jepsen, Peter Uhd
Kawase, Kodo
Koch, Martin
Llombart, Nuria
Mehdi, Imran
Park, Gun-Sik
Walker, Christopher
TI Untitled
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Editorial Material
C1 [Siegel, Peter H.] Columbia Univ, New York, NY 10027 USA.
[Alberti, Stefano] Ecole Polytech Fed Lausanne, Lausanne, Switzerland.
[Williams, Dylan F.] NIST, Electromagnet Fields Div, Boulder, CO USA.
[Shaw, Sharri] Aquinas Coll, Grand Rapids, MI USA.
[Beigang, Rene] Univ Kaiserslautern, D-67663 Kaiserslautern, Germany.
[Davies, A. Giles] Univ Leeds, Leeds, W Yorkshire, England.
[East, Jack] Univ Michigan, Elect Engn & Comp Sci Dept, Ann Arbor, MI 48109 USA.
[Gallerano, Gian Piero] Leibniz Univ Hannover, Hannover, Germany.
[Grossman, Erich N.] Univ Texas Austin, Austin, TX USA.
[Jepsen, Peter Uhd] Univ Freiburg, Freiburg, Germany.
[Kawase, Kodo] RIKEN, Wako, Saitama, Japan.
[Mehdi, Imran] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Park, Gun-Sik] USN, Res Lab, Washington, DC 20375 USA.
RP Siegel, PH (reprint author), Columbia Univ, New York, NY 10027 USA.
NR 0
TC 0
Z9 0
U1 1
U2 5
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD JAN
PY 2012
VL 2
IS 1
BP 1
EP 4
DI 10.1109/TTHZ.2011.2178650
PG 4
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 141ZP
UT WOS:000318765500001
ER
PT J
AU Siegel, PH
AF Siegel, Peter H.
TI Terahertz Pioneers A Series of Interviews With Significant Contributors
to Terahertz Science and Technology
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Editorial Material
C1 [Siegel, Peter H.] CALTECH, Dept Biol, Pasadena, CA 91125 USA.
[Siegel, Peter H.] CALTECH, Dept Elect Engn, Pasadena, CA 91125 USA.
[Siegel, Peter H.] NASA, Jet Prop Lab, SWAT, Pasadena, CA 91125 USA.
RP Siegel, PH (reprint author), CALTECH, Dept Biol, Pasadena, CA 91125 USA.
NR 0
TC 2
Z9 2
U1 0
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD JAN
PY 2012
VL 2
IS 1
BP 5
EP 5
DI 10.1109/TTHZ.2011.2178652
PG 1
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 141ZP
UT WOS:000318765500002
ER
PT J
AU Siegel, PH
AF Siegel, Peter H.
TI Terahertz Pioneer: Maurice F. Kimmitt "A Person Who Makes Things Work"
SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY
LA English
DT Biographical-Item
C1 [Siegel, Peter H.] CALTECH, Dept Biol, Pasadena, CA 91125 USA.
[Siegel, Peter H.] CALTECH, Dept Elect Engn, Pasadena, CA 91125 USA.
[Siegel, Peter H.] CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA.
RP Siegel, PH (reprint author), CALTECH, Dept Biol, Pasadena, CA 91125 USA.
EM phs@caltech.edu
NR 1
TC 2
Z9 2
U1 1
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 2156-342X
J9 IEEE T THZ SCI TECHN
JI IEEE Trans. Terahertz Sci. Technol.
PD JAN
PY 2012
VL 2
IS 1
BP 6
EP 9
DI 10.1109/TTHZ.2011.2178654
PG 4
WC Engineering, Electrical & Electronic; Optics; Physics, Applied
SC Engineering; Optics; Physics
GA 141ZP
UT WOS:000318765500003
ER
PT B
AU Dick, SJ
AF Dick, Steven J.
BE Geppert, ACT
TI Space, Time and Aliens: The Role of Imagination in Outer Space
SO IMAGINING OUTER SPACE: EUROPEAN ASTROCULTURE IN THE TWENTIETH CENTURY
LA English
DT Article; Book Chapter
C1 [Dick, Steven J.] NASA, Washington, DC USA.
[Dick, Steven J.] Amer Astron Soc, Hist Astron Div, Washington, DC USA.
[Dick, Steven J.] Int Astron Union, Hist Astron Commiss, Paris, France.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU PALGRAVE
PI BASINGSTOKE
PA HOUNDMILLS, BASINGSTOKE RG21 6XS, ENGLAND
BN 978-0-230-36136-2
PY 2012
BP 27
EP 44
D2 10.1057/9780230361362
PG 18
WC History & Philosophy Of Science
SC History & Philosophy of Science
GA BEI92
UT WOS:000316763100002
ER
PT J
AU Esterhuizen, S
Turbiner, D
Stowers, D
Young, L
AF Esterhuizen, Stephan
Turbiner, Dmitry
Stowers, Dave
Young, Lawrence
GP ION
TI Testing High Precision Space Receivers versus LightSquared Interference
SO PROCEEDINGS OF THE 2012 INTERNATIONAL TECHNICAL MEETING OF THE INSTITUTE
OF NAVIGATION
LA English
DT Proceedings Paper
CT International Technical Meeting (ITM) of the Institute-of-Navigation
(ION)
CY JAN 30-FEB 01, 2012
CL Newport Beach, CA
SP Inst Nav (ION)
AB This paper describes various tests held to document the impact of LightSquared signals on JPLs high performance GPS receivers, and will emphasize test design. The first test was done at the Jet Propulsion Laboratory, where interference was introduced into the receiver under test using a directional coupler, that is, it was a conducted test as opposed to a radiated test [GARMIN2011]. We will describe the methods of generating the simulated GNSS and LightSquared signals, as well as the careful calibration of the system noise realized in the test setup.
A brief account will be given of two radiated tests consisting of anechoic chamber and live-sky testing held at White Sands Missile Range and at Holloman Air Force Base.
We will describe the strengths and weaknesses of each test type, and a summary of results will be presented.
C1 [Esterhuizen, Stephan; Turbiner, Dmitry; Stowers, Dave; Young, Lawrence] CALTECH, JPL, NASA, Pasadena, CA 91125 USA.
RP Esterhuizen, S (reprint author), CALTECH, JPL, NASA, Pasadena, CA 91125 USA.
NR 5
TC 0
Z9 0
U1 0
U2 2
PU INST NAVIGATION
PI WASHINGTON
PA 815 15TH ST NW, STE 832, WASHINGTON, DC 20005 USA
PY 2012
BP 669
EP 675
PG 7
WC Remote Sensing
SC Remote Sensing
GA BER53
UT WOS:000317865600032
ER
PT J
AU Tien, JY
Okihiro, BB
Esterhuizen, SX
Franklin, GW
Meehan, TK
Munson, TN
Robison, DE
Turbiner, D
Young, LE
AF Tien, Jeffrey Y.
Okihiro, Brian Bachman
Esterhuizen, Stephan X.
Franklin, Garth W.
Meehan, Thomas K.
Munson, Timothy N.
Robison, David E.
Turbiner, Dmitry
Young, Lawrence E.
GP ION
TI Next Generation Scalable Spaceborne GNSS Science Receiver
SO PROCEEDINGS OF THE 2012 INTERNATIONAL TECHNICAL MEETING OF THE INSTITUTE
OF NAVIGATION
LA English
DT Proceedings Paper
CT International Technical Meeting (ITM) of the Institute-of-Navigation
(ION)
CY JAN 30-FEB 01, 2012
CL Newport Beach, CA
SP Inst Nav (ION)
ID OCEAN ALTIMETRY; SYSTEM
AB Several upcoming NASA and NOAA missions require an advanced science-quality GNSS receiver as a mission-critical payload for cm-level precise orbit determination and/or Radio Occultation (RO) observations to meet their science objectives. The science and navigation requirements dictate that GNSS receivers track signals from GPS, GLONASS, and other GNSS systems as they become available.
JPL is developing the next generation GNSS receiver for flight called the TriG Receiver enabling continued access of precision orbit determination for remote sensing missions and the application of GNSS signals for the technically demanding RO and surface reflections observations. Derived from the NASA/JPL BlackJack receiver design, which has flown on over 16 spacecraft with over 115 years of successful operations, the TriG offers significantly enhanced capability to track more GNSS signals with higher SNR. The TriG receiver will track both the legacy and new signals from GPS as well as new GNSS signals from Galileo and GLONASS. The ability to track multiple GNSS satellite signals will improve both precision orbit determination and the quality and quantity of the RO measurements.
The TriG receiver features several innovations including digital beam steering to produce multiple simultaneous high-gain beams, wideband open loop tracking, and an advanced "time delayed" signal processing algorithm. These innovations improve precision for RO in the upper atmosphere while also supporting the wider range in delay and Doppler shift necessary for full RO retrieval in the lower troposphere. The TriG receiver is implemented in scalable 3U architecture and is fully reconfigurable enabling optimization to meet specific mission requirements and spacecraft resource constraints.
This paper will describe the TriG architecture, and how the new features will benefit the next-generation of global network instruments, as well as current test results.
C1 [Tien, Jeffrey Y.; Okihiro, Brian Bachman; Esterhuizen, Stephan X.; Franklin, Garth W.; Meehan, Thomas K.; Munson, Timothy N.; Robison, David E.; Turbiner, Dmitry; Young, Lawrence E.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RP Tien, JY (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
NR 12
TC 0
Z9 0
U1 0
U2 0
PU INST NAVIGATION
PI WASHINGTON
PA 815 15TH ST NW, STE 832, WASHINGTON, DC 20005 USA
PY 2012
BP 882
EP 890
PG 9
WC Remote Sensing
SC Remote Sensing
GA BER53
UT WOS:000317865600042
ER
PT J
AU van den Hurk, B
Doblas-Reyes, F
Balsamo, G
Koster, RD
Seneviratne, SI
Camargo, H
AF van den Hurk, Bart
Doblas-Reyes, Francisco
Balsamo, Gianpaolo
Koster, Randal D.
Seneviratne, Sonia I.
Camargo, Helio, Jr.
TI Soil moisture effects on seasonal temperature and precipitation forecast
scores in Europe
SO CLIMATE DYNAMICS
LA English
DT Article
DE Soil moisture initialization; Seasonal forecasting; Potential
predictability; Europe
ID UNITED-STATES; LAND-SURFACE; PREDICTION; RANGE
AB The Second Global Land Atmosphere Coupling Experiment (GLACE2) is designed to explore the improvement of forecast skill of summertime temperature and precipitation up to 8 weeks ahead by using realistic soil moisture initialization. For the European continent, we show in this study that for temperature the skill does indeed increase up to 6 weeks, but areas with (statistically significant) lower skill also exist at longer lead times. The skill improvement is smaller than shown earlier for the US, partly because of a lower potential predictability of the European climate at seasonal time scales. Selection of extreme soil moisture conditions or a subset of models with similar initial soil moisture conditions does improve the forecast skill, and sporadic positive effects are also demonstrated for precipitation. Using realistic initial soil moisture data increases the interannual variability of temperature compared to the control simulations in the South-Central European area at longer lead times. This leads to better temperature forecasts in a remote area in Western Europe. However, the covered range of forecast dates (1986-1995) is too short to isolate a clear physical mechanism for this remote correlation.
C1 [van den Hurk, Bart; Camargo, Helio, Jr.] Royal Netherlands Meteorol Inst, KNMI, NL-3730 AE De Bilt, Netherlands.
[Doblas-Reyes, Francisco] Catalan Inst Climate Sci IC3, Barcelona 08005, Spain.
[Doblas-Reyes, Francisco; Balsamo, Gianpaolo] European Ctr Medium Range Weather Forecasts ECMWF, Reading RG2 9AX, Berks, England.
[Koster, Randal D.] NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA.
[Seneviratne, Sonia I.] ETH, Inst Atmospher & Climate Sci, Zurich, Switzerland.
RP van den Hurk, B (reprint author), Royal Netherlands Meteorol Inst, KNMI, POB 201, NL-3730 AE De Bilt, Netherlands.
EM hurkvd@knmi.nl
RI Balsamo, Gianpaolo/I-3362-2013; Koster, Randal/F-5881-2012; Seneviratne,
Sonia/G-8761-2011; Doblas-Reyes, Francisco/C-1228-2016
OI Balsamo, Gianpaolo/0000-0002-1745-3634; Koster,
Randal/0000-0001-6418-6383; Seneviratne, Sonia/0000-0001-9528-2917;
Doblas-Reyes, Francisco/0000-0002-6622-4280
NR 22
TC 37
Z9 37
U1 0
U2 23
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0930-7575
EI 1432-0894
J9 CLIM DYNAM
JI Clim. Dyn.
PD JAN
PY 2012
VL 38
IS 1-2
BP 349
EP 362
DI 10.1007/s00382-010-0956-2
PG 14
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 871QQ
UT WOS:000298753200020
ER
PT S
AU Barmore, B
Smith, C
Palmer, S
Abbott, T
AF Barmore, Bryan
Smith, Colin
Palmer, Susan
Abbott, Terence
GP IEEE
TI A COMPARATIVE STUDY OF INTERVAL MANAGEMENT CONTROL LAW CAPABILITIES
SO 2012 IEEE/AIAA 31ST DIGITAL AVIONICS SYSTEMS CONFERENCE (DASC)
SE IEEE-AIAA Digital Avionics Systems Conference
LA English
DT Proceedings Paper
CT IEEE/AIAA 31st Digital Avionics Systems Conference (DASC)
CY OCT 14-18, 2012
CL Williamsburg, VA
SP IEEE, AIAA, Avionics, AESS, DATC, Boeing
C1 [Barmore, Bryan; Smith, Colin; Palmer, Susan] NASA, Langley Res Ctr, Hampton, VA 23681 USA.
RP Barmore, B (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU IEEE
PI NEW YORK
PA 345 E 47TH ST, NEW YORK, NY 10017 USA
SN 2155-7195
BN 978-1-4673-1700-9
J9 IEEEAAIA DIGIT AVION
PY 2012
PG 25
WC Engineering, Aerospace
SC Engineering
GA BEJ49
UT WOS:000316917202045
ER
EF